Untitled - Osservatorio Astronomico di Bologna

INAF
Osservatorio Astronomico di Bologna
Annual Report 2009
Osservatorio Astronomico di Bologna
Via Ranzani 1, I-40127 Bologna, ITALY
Tel.: +39-051-2095701 ; Fax: +39-051-2095700
http://www.bo.astro.it/
Cover: XMM-Newton image of the cluster Abell 2028, from Gastaldello
et al., 2010, A&A, 522, A34
Introduction
The Osservatorio Astronomico di Bologna is one of the twenty research
structures of the Italian National Institute for Astrophysics (INAF), operating under the supervision of the Ministry for Education, University and
Research (MIUR). The Ministry provides most of the financial resources
which make our activity possible.
This Report gives an overview of our scientific research, covering a wide
range of astrophysical topics, as well as operational and educational activities. OAB astronomers are mostly involved in:
• studies of stellar populations and galactic evolution and their cosmological implications;
• studies of the structure, evolution and distribution of galaxies, clusters and AGNs, and their contribution to the cosmological backgrounds;
• numerical studies in the field of gas hydrodynamics and turbulence
simulations;
• management and upgrading of the two telescopes in Loiano (152 and
60 cm) and development of astronomical instruments in the framework of national and international programs.
• outreach and educational initiatives, through exhibitions, lectures and
workshops.
Most of these studies are based on an intensive use of the most advanced
ground-based and space instruments available today at all wavelengths.
They are carried out in collaboration with many international and national institutes and, locally, with the Università di Bologna, Dipartimento
di Astronomia and with two other research structures of INAF, Istituto
di Radioastronomia and Istituto di Astrofisica Spaziale e Fisica CosmicaBologna. A large fraction of the staff is involved in international long-term
projects, at the forefront of astronomical research.
This report was edited by Alberto Buzzoni, Alberto Cappi, Antonio De
Blasi, Roberto Bedogni, Emiliano Diolaiti, Silvia Galleti, Monica Marra,
Roberto Merighi, Giovanna Stirpe, and Valentina Zitelli.
Flavio Fusi Pecci
(Director)
Osservatorio Astronomico di Bologna:
2009
• Director: Flavio Fusi Pecci
• Deputy Director: Monica Tosi
Staff
• Scientific Staff: Bardelli, Sandro; Bedogni, Roberto; Bellazzini, Michele;
Bolzonella, Micol; Bragaglia, Angela; Buzzoni, Alberto; Cacciari,
Carla; Cappi, Alberto; Carretta, Eugenio; Ciliegi, Paolo; Clementini, Gisella; Comastri, Andrea; D’ Ercole, Annibale; De Ruiter,
Hans Rudolf (transferred, May 1); Diolaiti, Emiliano; Ettori, Stefano;
Federici, Luciana; Finelli, Fabio (transferred, Aug. 1); Fusi Pecci,
Flavio; Gilli, Roberto; Gruppioni, Carlotta; Londrillo, Pasquale (retired, Aug. 1); Meneghetti, Massimo; Merighi, Roberto; Mignoli,
Marco; Montegriffo, Paolo; Origlia, Livia; Pancino, Elena; Pozzetti,
Lucia; Stanghellini, Letizia; Stirpe, Giovanna Maria; Tosi, Monica;
Zamorani, Giovanni; Zitelli, Valentina; Zucca, Elena
• Computer Centre: Di Luca, Roberto; Gatti, Michele; Lolli, Marco;
Policastro, Rocco
• Laboratory: Bregoli, Giovanni
• Logistic Support: Ravaglia, Maurizio
• Loiano Staff: Bernabei, Stefano; Bruni, Ivan; De Blasi, Antonio; Gualandi, Roberto; Muzi, Ivo
• Administration: Abicca, Renata; Caddeo, Sandra; Diodato, Olga;
Orlandi, Marco; Piccioni, Annalia; Polastri, Tiziana; Venturini, Adele
• Library: Marra, Monica
• Reception: Caputo, Silvana; Iuso, Annalisa
PhD, fellows and contracts:
• PhD grants funded by INAF–OAB: Contreras Ramos, Rodrigo; Coppa,
Graziano; Lombini, Matteo; Lusso, Elisabeta; Macario, Giulia; Maruccia, Ylenia; Perina, Sibilla.
• PhD students with OAB supervisors: Bellagamba, Fabio; Correnti,
Matteo; De Boni, Cristiano; Donnarumma, Annamaria; Fabbri, Sara;
Guido, Vincenzo; Marinoni, Silvia; Moresco, Michele; Moretti, Maria
Ida; Morgan, John; Verma, Rashmi.
• Post-grad: Altavilla, Giuseppe; Cocozza, Gabriele; Dominguez Sanchez,
Helena; Galleti, Silvia; Merten, Julian; Poppi, Francesco; Ragaini,
Silvia; Rossetti, Emanuel.
• Post-doc: Cignoni, Michele; Gitti, Myriam; Iwasawa, Kazushi; Nair,
Preethi; Ranalli, Piero; Roche, Nathan; Romano, Donatella; Vergani,
Daniela.
• Contracts: Georgantopoulos, Ioannis
Contents
1 Stars and Stellar Populations
1.1 The Galaxy . . . . . . . . .
1.2 Globular Clusters . . . . . .
1.3 Nearby Galaxies . . . . . .
1.4 Pulsating variable stars . .
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2 Extragalactic Astronomy and Cosmology
2.1 Active galactic nuclei and star-forming galaxies . . . . . . .
2.2 Surveys and observational cosmology . . . . . . . . . . . . .
2.3 Galaxy clusters and large-scale structure . . . . . . . . . . .
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3 Hydrodynamics
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4 Instruments and Technology
4.1 The GAIA project . . . . . . . . . . . . . . . . . . . .
4.2 GIANO: an ultra-stable IR spectrometer for TNG . .
4.3 Site testing . . . . . . . . . . . . . . . . . . . . . . . .
4.4 LINC-NIRVANA . . . . . . . . . . . . . . . . . . . . .
4.5 MAORY: an adaptive optics module for E-ELT . . . .
4.6 SIMPLE: a high resolution IR spectrograph for E-ELT
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5 Loiano Observing Site
5.1 Operations and use of the 152 cm telescope . . . . .
5.2 Loiano computer station . . . . . . . . . . . . . . . .
5.3 Applications to the 152cm telescope . . . . . . . . .
5.4 Loiano cooperation . . . . . . . . . . . . . . . . . . .
5.5 Scientific production involving the 152 cm Telescope
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6 Computer Centre and Computer Network
6.1 General Description . . . . . . . . . . . . .
6.2 Computer centre improvements . . . . . .
6.3 Web applications . . . . . . . . . . . . . . .
6.4 Routine activities . . . . . . . . . . . . . . .
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7 Library
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8 Outreach and Educational Activities
8.1 Outreach Activities . . . . . . . . . . . . . . . . . . . . . . .
8.2 Educational Activities . . . . . . . . . . . . . . . . . . . . .
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8.3
Educational and Public Outreach . . . . . . . . . . . . . . .
9 List of Publications
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10 Observing Campaigns
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11 National and International Appointments,
working-group memberships & policy committees
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12 Organization of Workshops
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13 Seminars
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14 “Laurea” thesis
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15 PhD theses
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16 Post-Doctoral, Post-Laurea fellowships and Contracts
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1
Stars and Stellar Populations
V-band mosaic (through the F606W filter) of eleven globular clusters in M31
studied by Perina et al. (2009, A&A, 507, 1375). As labelled on the different
panels, all pictures have been obtained either through the Wide Field Channel
(WFC) or High Resolution Channel (HRC) of the Advanced Camera for Survey
(ACS) onboard the Hubble Space Telescope. Each field is 2000 × 2000 across. North
is up and East to the left.
People involved at OAB:
• Scientific staff: M. Bellazzini, A. Bragaglia, A. Buzzoni, C. Cacciari,
E. Carretta, G. Clementini, L. Federici, F. Fusi Pecci, P. Montegriffo,
L. Origlia, E. Pancino, G. Parmeggiani, M. Tosi;
• Technical staff: M. Lolli;
• Fellows and contracts: G. Altavilla, M. Cignoni, R. Contreras, M.
Correnti, S. Galleti, S. Perina, S. Ragaini, D. Romano, E. Rossetti;
The study of stellar populations and stellar systems is a very active research
field at the OAB since its foundation. Interests range from the evolution of
galaxies to Galactic and extragalactic star clusters, from chemical evolution
to variable stars, covering the whole range of astronomical wavelengths.
The present description of the activity of 2009 has been organized, as usual,
in a few main Sections to provide a very general overview: 1. The Galaxy,
2. Globular clusters, 3. Nearby galaxies, 4. Pulsating variable stars.
1.1
1.1.1
The Galaxy
A census of the Galaxy with Gaia
People involved at OAB: Altavilla, Bellazzini, Bragaglia, Cacciari, Clementini, Cocozza, Federici, Marinoni, Montegriffo, Pancino, Ragaini
GREAT (Gaia Research for European Astronomy Training) is a pan-European science driven research infrastructure which will facilitate, through
focussed interaction on a European scale, the fullest exploitation of the Gaia
mission. A GREAT kickoff meeting was held in Cambridge on 26–27 March
2009, and a plenary meeting was held in Nice in autumn 2009. OAB personnel is involved in several working groups of the following areas: WGA2:
Census of Supporting Surveys; WGA3: Chemical Tagging; WGA4: Local Group, Dwarf Spheroidals and Tidal Streams; WGA5: Alerts; WGA8:
Distance Scales (with a leading role by OAB); WGB1: Open Clusters and
Young Associations. In particular, a Conference on the Distance Scales,
to be held in May 2011 at the Capodimonte Observatory (Naples), has
been approved and funded by the European Science Fundation within the
GREAT programme.
A Ph.D. student, C. Lardo, joined the OAB activities on WGA3: Chemical
Tagging in November 2009.
2
Figure 1: The radial metallicity gradient as defined by the open clusters. (a)
We show the clusters in the Dias et al. (2002) catalogue, with the three clusters
analysed in Andreuzzi et al. (2010: Be 20, Be 66, and To 2) indicated by filled,
red symbols. (b) We show here only clusters for which [Fe/H] has been derived
using high resolution spectroscopy. The BOCCE clusters are indicated by filled
symbols, with the last three clusters analysed shown with larger, filled symbols.
Technical details on the Gaia mission and on the involvement of OAB
personnel in the fields of absolute photometric calibration and of variable
stars are given in the Instruments and Technology chapter.
1.1.2
Open clusters as tracers of the evolution of the abundance
gradients
People involved at OAB: Bragaglia, Carretta, Cignoni, Pancino, Tosi
Open clusters are very useful tracers of the properties of the Galactic disk.
In the context of the BOCCE project (the Bologna Open Cluster Chemical
Evolution project) Bragaglia and Tosi continued the analysis of photometric data collected at ESO and TNG (Andreuzzi et al. 2010) or LBT (paper
in preparation); see Fig. 1 and the web page http://www.bo.astro.it/
~angela/bocce.html. Bragaglia, Carretta and Tosi continued the study
of SARG@TNG spectra of clusters in collaboration with Gratton (INAF3
OAPd). Bragaglia and Carretta, in collaboration with Sneden (Univ. Austin), Gratton and Lucatello (INAF-OAPd) obtained and analysed Hydra@WIYN spectra of NGC6791, to see whether the Na-O anticorrelation
is really seen exclusively in globular clusters. Bragaglia and Pancino joined
the working group on open clusters and associations, which is part of the
GREAT network and participated in a successful FP7 ITN grant request
(PI N. Walton, Cambridge).
This research is in collaboration with Cignoni (Univ. Bologna), Gratton,
Lucatello (INAF-Padova Obs.), Marconi (ESO, Chile), Andreuzzi (INAFRoma Obs., TNG), Beccari (ESO, Garching), Sneden (Univ. Texas, USA).
A set of 13 open clusters was observed with [email protected] m and
UVES@VLT for abundance analysis. The first paper, concerning Cr 110,
M 67, NGC 2099, NGC 2420, and NGC 7789, has been submitted and
published (Pancino et al. 2010). A second paper focussed on Berkeley 32,
NGC 752, Hyades, and Praesepe is in preparation (Carrera et al., in preparation).
This research is in collaboration with C. Gallart and R. Carrera (IAC Tenerife, Spain).
1.1.3
The structure of the Galactic halo
People involved at OAB: Bragaglia, Cacciari
RR Lyrae (RRL) variables and blue horizontal branch (BHB) stars have
been used to trace the old stellar population in the Galactic halo as far
as 10–12 kpc in the direction of the Anticentre. The space motion vectors
UVW have been derived from photometric data, radial velocities and proper
motions. The presence of sub-structure, retrograde rotation and downstreaming motion by BHB (typical of old halo population) stars has been
revealed. These results were presented at the meeting The Milky Way and
the Local Group – Now and in the Gaia Era, Heidelberg, August 31 –
September 4, 2009. A paper is in preparation.
This work is in collaboration with A. Spagna and R. Smart (INAF-OA
Torino) and T.D. Kinman (NOAO)
4
1.1.4
The accreted component of the Galactic Halo:
The Sagittarius Dwarf Spheroidal and other large
structures
People involved at OAB: Bellazzini, Correnti
There is now a growing body of observational evidence in favour of an inhomogeneous halo, where the traces of the slow building up by hierarchical
merging of sub-units should be still observable (Bell et al. 2007). The Sagittarius dwarf Spheroidal Galaxy (Sgr dSph; Ibata et al. 1994) is the most
evident and striking example of a real time accretion event occurring in the
Galactic Halo. The main body of Sgr dSph orbits well within the Galactic
spheroid (RGC ' 16 kpc) and shows clear signs of being disrupted by the
Galactic tidal field. Thus, the Sgr dSph is (and has been) one of the major
contributors to the stellar content of the whole Galactic Halo.
Our research on the Sagittarius galaxy and its Stream is continuously ongoing with a constant production of new published results (Monaco et al.
2002, 2003, 2004, 2005a,b, 2007; Bellazzini et al. 1999a,b, 2003a,b, 2006a,b,
2008; Correnti et al. 2007, 2008). A high-resolution spectroscopy survey of
stars in the various branches of the Sgr Stream is also ongoing and is providing the first interesting results (Monaco et al. 2007).
As a follow-up of the huge kinematical study of the nucleus of Sgr and of
the giant cluster M54 (Bellazzini et al. 2008) we obtained high resolution 2dimensional spectra of 51 overlapping VLT-ARGUS tiles in the central 0.60
of M54. ARGUS is an Integral Field Unit that can obtain 22 × 14 spectra
simultaneously on a rectangular raster, covering a field of 11.400 ×7.700 . With
these data we were able to identify a central cusp in the velocity dispersion
curve of M54 (see Fig. 2), that is not consistent with an isotropic King
model. The observed kinematics are consistent with the presence of a
central Black Hole of mass ∼ 9400 solar masses. However, the observations
can alternatively be explained if the cusp stars possess moderate radial
anisotropy. A Jeans analysis of the Sgr nucleus reveals a strong tangential
anisotropy, probably a relic from the formation of the system.
M. Correnti is using SDSS data to take accurate measures of the northern
branch of the Sgr tidal Stream. Preliminary results of this study were
presented in Correnti et al. (2007, 2008). The final results are presented in
the PhD thesis and in a paper to be published on the Astrophysical Journal
(Correnti 2010; Correnti et al. 2010).
This research is in collaboration with F. Ferraro (Univ. of Bologna), L.
5
Figure 2: σ profile measured from ARGUS spectra coadded in annuli (black triangles
and squares) rises rapidly toward the cluster centre. Be00
yond ∼ 20 , the MEDUSA
and ARGUS spectra can be
used to measure the velocities
of individual stars, uncontaminated by neighbours.
The
blue and red points show the
corresponding profiles for the
M54 and Sgr samples, respectively.
For comparison, we
show the earlier Bellazzini et
al. (2008) results. The line
shows the kinematic behavior
of a best fit King model plus an
Intermediate-Mass Black Hole.
From Ibata et al. (2009).
Monaco (ESO, Chile), R. Ibata (Obs. Strasbourg, France), N. Martin (MPI,
Germany), M. Irwin (Cambridge, UK), D. Mackey (Edinburgh Univ., UK),
and S. Chapman (Caltech, USA). Matteo Correnti’s PhD project is focussed
on the study of galactic relics, including Sgr. This research was partly
supported by INAF-PRIN07 grant n. CRA 1.06.10.04 (PI: M. Bellazzini,
The local route to galaxy formation. Tracing the relics of the hierarchical
merging process in the Milky Way and in other nearby galaxies).
1.1.5
Chemical evolution models
People involved at OAB: Romano, Tosi
Models of Galactic chemical evolution can nowadays reproduce the vast
majority of the observed characteristics of our Galaxy. Yet, there are a
number of open questions which require further studies. In 2009, to better
understand the evolution of the Galaxy, we have worked on the combination
of our detailed chemical evolution code with a more appropriate treatment
of star and gas dynamics. We have also proceeded towards a complete and
accurate comparison of the various stellar nucleosynthesis yields available
in literature and their capability (or lack thereof) of reproducing all the
major observed chemical properties of Galactic objects. Finally, we have
6
studied the chemical evolution of ω Cen, assuming it to be both a real
globular cluster and the fossil nucleus of an accreted galaxy.
These studies are in collaboration with F. Matteucci (Trieste Univ.), L.
Ciotti (Bologna Univ.), V. Hill (Nice Obs., France), C. Charbonnel (Geneva
Univ., CH).
1.2
1.2.1
Globular Clusters
Observational tests of theoretical stellar models
People involved at OAB: Bellazzini, Cacciari, Fusi Pecci, Origlia, Pancino
Stellar evolutionary models are often used to derive relevant properties
of globular star clusters (GCs) and galaxies, such as their age and metal
content. The Luminosity Function of the stellar sequences in the CMDs,
from the Main Sequence Turn Off (MS-TO) up to the termination of the
Asymptotic Giant Branch (AGB), has been recognized as the most powerful
tool for testing stellar evolutionary models (with particular regard to the
accuracy of the input physics, the reliability of canonical assumptions, etc.).
A fully fruitful test requires that the observations be a) complete, b) statistically significant, and c) accurate and adequate for each specific evolutionary
sequence. Point (a) means that virtually all of the stars in a given area of
the cluster are measured down to a given magnitude level, and that reliable
corrections for incompleteness can be applied below that level. Point (b)
means that observations should cover most of the cluster extension. Point
(c) requires infrared observations to measure the cool Red Giant Branch
(RGB) stars and UV observations to properly study the blue sequences
such as the Horizontal Branch and the Blue Stragglers.
1.2.2
The Blue Straggler Star Population in Globular Clusters
People involved at OAB: Bellazzini, Fusi Pecci
It is now generally accepted that Blue Straggler Stars (BSS) are more massive than the normal MS stars, and are the result of mass transfer between
binary companions (MT-BSS), possibly up to the coalescence of the binary
system, or merger of two single or binary stars driven by stellar collisions
(COL-BSS).
To finally unveil their nature and their formation mechanisms, we are using
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several different and complementary approaches, including high-resolution
and multi-wavelength photometric observations, deep high-resolution spectroscopy, and Monte-Carlo dynamical simulations.
This line of research has received a remarkable boost in the last year thanks
to the availability of the wide-field camera LBC on the part-Italian 2 × 8 m
LBT telescope. This instrument is ideal to obtain the very efficient multiwavelength radial coverage of GCs required for the detailed analyses of the
BSS populations which we are performing. In particular we have recently
completed a thorough study of M53 (Beccari et al. 2008), of NGC2419 (Dalessandro et al. 2008), NGC5466 (Beccari et al. 2009) and M2 (Dalessandro
et al. 2009)
This work is in collaboration with F. Ferraro, E. Dalessandro, B. Lanzoni,
A. Sollima (Univ. Bologna), G. Beccari (ESTEC, NL), R. Rood, R. Schiavon (Univ. of Virginia, USA), M. Mapelli (Zurich Univ., Switzerland), S.
Sigurdsson (Pennsylvania State Univ., USA), E. Sanna (Univ. Roma Tor
Vergata), A. Sills (McMaster Univ., Canada), C. Mancini (Univ. Firenze).
1.2.3
Multiple stellar populations in Globular Clusters
People involved at OAB: Bragaglia, Carretta, Bellazzini, Pancino
Our group was fundamental in providing the chemical evidence that GCs
are not simple stellar populations.
While the metallicity (i.e., [Fe/H]) is remarkably homogeneous in each GC,
the large star-to-star variations in light elements (see e.g. the Na-O and MgAl anticorrelations) are explained by the formation of (at least) a second
generation of stars from material polluted by a previous population. All
GCs studied so far support this vision; in particular we have analysed
about 2000 RGB stars in 20 GCs, observed with FLAMES@VLT. We are
now extending the project adding other elements, like Li, and observing
other GCs (e.g., in P84 we obtained X-shooter spectra of two MS stars in
NGC 2808, under the Italian GTO programme).
The results have been presented in a series of papers: Carretta et al. 2009a,
2009b on the ubiquitous Na-O anticorrelation (see Fig. 3); Carretta et al.
2009c on a new [Fe/H] scale for GCs; Bragaglia et al. 2010a on the He
content of RGB stars (see Fig. 4); Gratton et al. 2010 on the relation
between the anticorrelations, He and the HB; Carretta et al. 2010a on the
Ca abundance; Carretta et al. 2009b on the properties of GCs; Carretta
8
Figure 3: The Na-O anticorrelation in 20 GCs (adapted from Carretta et al.
2009a, 2010d): the universality of this feature is the confirmation of the existence
of multiple populations in GCs.
et al. 2010c on the high-mass GC M54 and its similarities with ω Cen
(see Fig. 5); Bragaglia et al. 2010b on the abundances of two MS stars in
NGC 2808; Carretta et al. 2010d on NGC 1851.
This work is in collaboration with R. Gratton, S. Lucatello, Y. Momany, V.
D’Orazi (INAF-Padova Obs.), G. Piotto (Univ. of Padova), F. D’Antona
(INAF-Roma Obs.), F. Leone (Univ. Catania), G. Catanzaro (INAFCatania Obs.), S. Cassisi (INAF-Teramo Obs.), P. François (Obs. Paris),
A. Recio-Blanco (Obs. Nice) and many more. This project received funding
by INAF-PRIN 2005 and by the PRIN-MIUR 2007.
1.2.4
Mass loss in RGB stars
People involved at OAB: Bragaglia, Cacciari, Carretta, Fusi Pecci, Origlia
The IR spectral range is also particularly suitable to study the mass loss
process in giant stars. Mass loss is a crucial parameter in any stellar evolu-
9
Figure 4: He-rich (i.e., Na-rich, second generation) and He-poor (i.e., Na-poor, first generation) stars have different luminosities at the
RGB bump. We show here the results from our
survey (Bragaglia et al. 2010a).
tion modelling. The late evolutionary stages of low- and intermediate-mass
giant stars are strongly influenced by mass loss processes. Yet, our lack of
empirical estimates on mass loss in low-mass RGB and AGB stars remains
one of the most serious stumbling blocks for a comprehensive understanding
of stellar evolution. A pilot survey of GCs performed with ISOCAM in the
10 µm spectral region (Origlia et al. 2002) has placed the whole problem
into a new perspective that we can explore in deeper detail now, thanks
to the powerful capabilities of the NASA Spitzer Space Telescope. Followup Spitzer observations have been obtained, aimed at studying mass loss
along the entire RGB in 17 globular clusters with different metallicities.
Data analysis has been completed, mass loss rates and duty cycles have
been derived for most of the clusters. First results on 47 Tuc have been
published in Origlia et al. (2007; 2010). The results for the other clusters
are ready for publication. A relevant fraction of giant stars show an excess
of mid-IR light above that expected from their photospheric emission. This
is plausibly due to dust formation in mass flowing from these stars. This
mass loss extends down to the level of the horizontal branch and increases
with luminosity. The mass loss is episodic, occurring in only a fraction
of stars at a given luminosity. Using the DUSTY code and our observations we derive mass-loss rates for these stars. Finally, we obtain the first
empirical mass-loss formula calibrated with observations of Population II
stars. The dependence on luminosity of our mass-loss rate is considerably
shallower than the widely used Reimers law.
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Figure 5: M54 and ω Cen show interesting similarities. We show here the Na-O
anticorrelations we found in M54 (Carretta et al. 2010c) compared to literature
data on ω Cen. In both cases the leftmost panels show the whole samples, the
intermediate the metal-rich components, and the rightmost panels the metal-poor
populations. It is clear that the extension of the anticorrelation is different in the
two sub-samples in both stellar systems.
This work is in collaboration with F. Ferraro, S. Fabbri, E. Dalessandro
(Univ. of Bologna), E. Valenti (ESO, Chile), R.T. Rood (Univ. of Virginia,
USA), R.M. Rich (UCLA, USA).
Velocity fields in the atmosphere of red giant stars, that may lead to mass
loss, can be studied by comparing the CaII K and Hα lines from high resolution spectra with accurate chromospheric models. This type of analysis
has been performed on several bright red giant stars in the stellar system
Omega Cen, selected on the basis of their luminosity and metallicity. Mass
loss rates have been estimated, in general agreement with the requirements
of stellar evolution. A paper is in press.
This work is in collaboration with P. Mauas and M. Vieytes (Univ. of
Buenos Aires, Argentina).
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1.2.5
Clusters and field stars in the Galactic bulge: an infrared
view
People involved at OAB: Origlia
Bulge GCs are a fundamental stellar population of our Galaxy and it is
most interesting to compare their detailed chemical abundances with the
Galactic halo populations. For most of the bulge population, foreground
extinction is so large as to preclude any photometric and spectroscopic
optical study. In the last few years we have undertaken a long-term project
devoted to study the Galactic bulge in the infrared, to minimize the effects
of extinction.
Using the SOFI medium-resolution imager/spectrograph at the ESO NTT
and the NIRSPEC high-resolution echelle spectrograph at Keck II, we are
performing a systematic survey of M giant stars in bulge GCs as well as
in several fields at different distances from the Galactic centre. From a
detailed analysis of the IR colour-magnitude diagrams we construct a catalogue of 24 Galactic GCs toward the bulge. An additional sample of 12
clusters in the innermost region is under analysis. The compilation includes
measurements of the cluster reddening, distance, photometric metallicity,
horizontal branch/red clump, and red giant branch morphological (e.g.,
mean ridge lines) and evolutionary (e.g., bump and tip) features.
From the analysis of the high resolution spectra, we measured several single
roto-vibrational OH lines and CO bandheads to derive accurate oxygen
and carbon abundances. Other metal abundances can be derived from the
atomic lines of Fe I, Mg I, Si I, Ti I, Ca I and Al I. Abundance analysis is
performed by using full spectral synthesis techniques and equivalent width
measurements of representative lines. Results have been already published
for 10 GCs and two fields, the Baade window and an inner field at l = 0,
b = −1. Other fields in the inner bulge at different distances from the
Galactic Centre are under analysis. We find an overall [α/Fe] enhancement
up to about solar metallicities, both in the cluster and field populations,
that is consistent with a scenario in which the bulge formed early, with
rapid enrichment.
Finally, we started an IR spectroscopic screening of the young populations
of red supergiants in the central bar/bulge (Scutum) and in the Galactic
centre. First results have been recently published (Davies et al. 2009a,b).
This work is in collaboration with F. Ferraro, (Univ. of Bologna), E. Valenti
(ESO, Chile), R.M. Rich (UCLA, USA), B. Davies (University of Leeds,
12
Figure 6: Best MAD image obtained in the K band (the image size is 10 × 10 ,
north is up, east is left). The measured full-width at half-maximum (FWHM)
of stars is 0.100 , the Strehl ratio ranges between 15% and 24% over the entire
field of view. The quality of the J image is slightly worse (FWHM = 0.2400 and
Strehl ratio < 10%), but still much better than normally obtained with groundbased observations. A small (1600 × 1600 ) portion of the K image sampling the very
central region of Terzan 5 is shown magnified.
UK).
This work is in collaboration with F. Ferraro, B. Lanzoni, A. Mucciarelli,
E. Dalessandro (Univ. of Bologna), E. Valenti (ESO), G. Beccari (ESA),
R.M. Rich (UCLA, USA), R.T. Rood (Univ. of Virginia, USA).
1.2.6
Terzan 5
People involved at OAB: Bellazzini, Origlia
We have used exceptionally high resolution image from the Multi-Conjugate
Adaptive optics module MAD, mounted on the VLT, to obtain an extremely
accurate CMD of the highly obscured Bulge globular cluster Terzan 5 (see
Fig. 6).
The derived CMD revealed the presence of a double Red Clump, revealing
the presence of multiple stellar populations in this system (Fig 7). Followup Keck-NIRSPEC spectroscopy of showed that the stars in the two different Red Clumps have widely different metallicities: the faint RC has
[Fe/H] = −0.2, the bright RC has [Fe/H] = +0.3. This is the first time that
a cluster with a metallicity spread has been found in the Galactic Bulge. All
the available evidence suggest that Terzan 5 is the remnant of a larger system, that possibly took part in the assembly of the Bulge. These exciting re13
Figure 7: MAD (K, J − K)
CMD of the central region of
Terzan 5. Inset: magnified
view of the horizontal branch
region, with the two horizontal branch clumps marked
with red arrows. The effect
of reddening on the K magnitude and the J − K colour
is indicated by the reddening
vector plotted in the main
panel.
sults have been published in Nature (Ferraro et al 2009.) and were the subject of a press release (see http://www.bo.astro.it/ter5/ter5page.html).
This work is in collaboration with F. Ferraro, (Univ. of Bologna), E. Valenti
(ESO, Chile), R.M. Rich (UCLA, USA), R.T. Rood (Univ. Virginia), G.
Beccari (ESA), E. Dalessandro (Univ. of Bologna), B. Lanzoni (Univ. of
Bologna).
1.2.7
ω Centauri
People involved at OAB: Bellazzini, Cacciari, Pancino, Romano, Tosi
ω Centauri is the largest (M = 2.9 106 M , Merrit et al. 1997), brightest
cluster in the Galactic Halo, and surely the most peculiar one in terms of
structure, kinematics and stellar contents. It is in fact the only GC which
shows undisputed variations in the chemical content of its stars. From this
point of view, ω Cen could be considered a bridge system between genuine
globulars, which are unable to retain the gas ejected by their former massive
stars, and dwarf galaxies, which are the least massive self-enriching stellar
systems known.
Our group started working on this fascinating cluster years ago (Pancino et
al. 2000) producing results on many aspects such as photometry, kinematics, chemistry, in a series of 15 papers in international journals. In 2009,
we focussed mainly on the few following topics: (a) a very large kinematic
survey (radial velocities for ∼ 2600 stars from FLAMES spectra) to study
14
Figure 8: Comparison between the best-fitting Wilson (1975) model (solid lines)
and (a) the projected surface brightness (from Trager et al. 1995), (b) the ellipticity profile (from Geyer et al. 1983), (c) the rotation curve and (d) the velocity
dispersion profile presented in this paper. In panel (c), the 1σ, 2σ and 3σ contours
predicted by the model are also shown as dashed lines.
the velocity dispersion curve at very large distances from the cluster centre
(Sollima et al. 2009, see Fig. 8); (b) a more detailed modelling of the chemical evolution of the system: the first paper dealing with the helium content
has been published (Romano et al. 2010); (c) a dedicated search for the
tidal debris of ω Cen in the solar neighbourhood, using both kinematical
and chemical information, for which we have acquired most of the needed
spectra with UVES@VLT and SARG@TNG. This research is in collaboration with A. Sollima (IAC tenerife), R. Smart (OATO), and F.R. Ferraro
(UniBO).
1.2.8
The Globular Cluster System of the Andromeda galaxy
People involved at OAB: Bellazzini, Buzzoni, Cacciari, Federici, Fusi Pecci,
Perina, Galleti
The M31 globular cluster system is the largest found in the Local Group,
sufficiently close to allow detailed observations and little affected by red15
dening, at least for a large outer sub-set. Since the intrinsic depth of the
spheroid is small compared to the distance to M31, in the study of the basic
properties and comparisons one can remove the degeneracies introduced by
the uncertain knowledge of the individual distances. In practice, M31 offers
the unique opportunity of studying in very good detail the GC system of
a spiral galaxy that is similar to the MW, without some of the limitations
that affect the Galactic GC system.
The study of the M31 GC system is a long-term project started at the OAB
in the early 1980s, and recently revived by new observational programmes
(Galleti et al. 2004, 2005, 2006a,b, 2007; Federici et al. 2007; Fusi Pecci
et al. 2005). The OAB M31 team, in collaboration with scientists of other
Italian and foreign institutions, is carrying out the exhaustive systematic
census of M31 GC candidates using both photometry (from the UV to
the IR bands) and spectroscopy. The purpose of the project is to use the
globular cluster system to improve our knowledge of the mass, dynamics
and chemical evolution of the parent galaxy.
The main ongoing programmes are summarized in the following:
1. Our continuously updated on-line catalogue (Revised Bologna Catalogue of M31 globular clusters–RBC, Galleti et al. 2004) has become
the most complete and widely used reference in the field. The RBC
web site (http://www.bo.astro.it/M31/) scores more than 600 contacts per year from all over the world. A thorough analysis to add
spectroscopic metallicities to as many RBC clusters as possible is
currently ongoing (Galleti et al. 2009).
2. The study of a sample of 63 M31 GC candidates using HST/ACS
archive data has been completed. We derived sufficiently accurate
CMDs for 17 such objects, namely 11 old GCs and 6 luminous young
clusters. For the 11 old GCs, estimates of metallicity, reddening and
distance could be obtained by comparison with template Galactic
GCs. The age of the young clusters was estimated by fitting with
theoretical isochrones. This work brings to 44+11 the total number of
M31 old+young GCs with usable CMD. A paper has been published
(Perina et al. 2009b; see the cover figure of this chapter).
3. The presence in M31 of stellar systems similar to the MW globulars in
luminosity and shape, but with integrated colours significantly bluer
than the bluest MW counterparts, is well known and documented.
As a follow-up of our recent study (Fusi Pecci et al. 2005) on these
young and bright clusters, a large HST survey in collaboration with
16
scientists of foreign institutions (HST cycle 15, PI Cohen; PhD thesis
of Sibilla Perina) is in progress, to check the real nature of these
objects that seem to have no counterpart in the Milky Way. Twenty
candidates were imaged with WFPC2. The data reduction is now
complete and four papers have been published (Huchra et al. 2009,
Barmby et al. 2009, Perina et al. 2009a, 2010).
This work is in collaboration with J. Cohen (Caltech, USA), P. Hodge
(Univ. Washington, USA), P. Barmby (Univ. Ontario, Canada), M. Rich
(Caltech, USA), C. Corsi (INAF-OAR) and many others.
1.3
1.3.1
Nearby Galaxies
The Magellanic Clouds: field and cluster populations
People involved at OAB: Carretta, Cignoni, Fusi Pecci, Origlia, Tosi
At OAB several studies are being performed on the Magellanic Clouds,
using both their clusters and field populations to trace galaxy and stellar
evolution.
As major players in the international collaboration aimed at studying the
evolution of the SMC as a prototype of dwarf irregular galaxies, in 2009 we
completed the data reduction (Sabbi et al. 2009) of 6 fields in key galactic
locations (three HST/ACS fields in the SMC central region, two in the wing
toward the LMC, and one in the SMC halo) and started the analysis of their
star formation histories (SFH). We also derived the SFH of our HST/ACS
fields in and around the young SMC clusters NGC 346 and NGC 602, using
the synthetic CMD method (Cignoni et al. 2009, Cignoni et al. 2010).
This collaboration includes, among others, A. Nota, E. Sabbi, (STScI,
USA), J. Gallagher (Univ. of Wisconsin, USA) and E. Grebel (ARI, Heidelberg, Germany). The work has been partially supported by ASI-COFIS2007.
The spectral evolution of a Simple Stellar Population (SSP) and its most
evident colour glitches are ideal clocks for dating primeval galaxies and deriving a suitable, empirical relation between look-back time and redshift.
The empirical calibration of the clock which determines the spectral evolution of SSPs and its readability are the primary goals of our project. The
globular cluster system of the Magellanic Clouds (MC) provides a unique
opportunity to investigate the integrated spectrophotometric behavior of
17
stellar populations as a function of both age and chemical composition.
We are tackling these major astrophysical objectives by means of a coordinated spectrophotometric survey on a representative sample of MC clusters,
aimed at determining with great accuracy and in a homogeneous way their
age, metallicity and overall integrated spectral properties.
During a number of successful observing runs with SOFI@NTT, our group
secured high quality J, H, K photometry of 20 LMC and a few SMC clusters spanning the age range between 50 Myr and a few Gyr. We have also
obtained mid-IR photometry during Cycle 1 observations with the NASA
Spitzer Space Telescope. Populous and complete near-IR CMDs covering
the entire RGB extension have been obtained. The mid-IR data are under
analysis. The high quality and homogeneity of such an IR database provided the most accurate empirical determination of the occurrence of the
so-called AGB and RGB phase transitions. The results for the intermediate
age clusters in the LMC have been published in the past years, those for
the 4 intermediate age clusters in the SMC have been published in Mucciarelli et al. 2009. Accurate ages for individual clusters based on deep
ACS@HST photometry and updated models of stellar evolution have also
been obtained. Results for 2 intermediate-age clusters, namely NGC 1978
and NGC 1783, were already published in the past years; other clusters are
under analysis.
The correct reading of the age from a SSP requires the accurate knowledge
of the global metallicity. This major piece of information, namely a selfconsistent metallicity scale and a detailed description of the abundance
patterns of MC clusters, is still lacking. In order to fill such a gap, we
undertook a medium-term project to provide a homogeneous metallicity
scale based on high resolution optical (using UVES+GIRAFFE at the ESOVLT) and IR spectroscopy (using CRIRES@ESO-VLT) for a representative
sample of MC clusters. The detailed chemical abundance analysis of 4
intermediate age LMC clusters was published in the past years. Recently,
we published the chemical abundances of three old LMC clusters, namely
NGC 1786, 2210, and 2257 (Mucciarelli et al. 2009), finding significant
inhomogeneities for the [Na/Fe], [Al/Fe], [O/Fe], and [Mg/Fe] abundance
ratios, with evidence of [O/Fe] versus [Na/Fe] and [Mg/Fe] versus [Al/Fe]
anticorrelations. The trends detected agree nicely with those observed in
Galactic GCs, suggesting that such abundance anomalies are ubiquitous
features of old stellar systems and do not depend on the parent galaxy
environment. In NGC 1786 we also detected two extreme O-poor, Narich stars. This is the first time that a firm signature of extreme chemical
18
abundance anomalies has been found in an extragalactic stellar cluster.
This research is in collaboration with F. Ferraro, A. Mucciarelli (Univ. of
Bologna), V. Testa (INAF-Roma Obs.), C. Maraston (Univ. of Portsmouth,
UK).
1.3.2
Star formation histories and evolution of resolved
galaxies
People involved at OAB: Cignoni, Romano, Tosi
The importance of deriving the SFHs of galaxies from their resolved stellar populations, the relative intrinsic uncertainties in the synthetic CMD
method have been described in invited review papers (Tosi 2009; Cignoni &
Tosi 2009). Our current understanding of dwarf galaxy evolution as resulting from the SFH combined with the results with chemical and kinematical
analyses has been summarized in an Annual Review article (Tolstoy, Hill
& Tosi 2009). We are applying the method developed at the Bologna Observatory to infer the star formation history (SFH) from the CMDs of their
resolved stellar populations to a number of galaxies of different morphological type, mass and metallicity. In 2009 we have analysed the stellar
populations of metal-poor late-type dwarf galaxies located both inside and
outside the Local Group. In particular we have studied resolved stars and
star clusters in NGC 1705 and derived its SFH (Annibali et al. 2009) with
proprietary ACS and WFPC2 HST data. As mentioned in Sect. 1.3.1 we
are also studying the SFH of the SMC fields observed with ACS@HST.
These studies are in collaboration with, among others, A. Aloisi, A. Nota
and E. Sabbi (STScI, USA), F. Annibali, (INAF-Padova Obs.), J. Gallagher (Wisconsin Univ., USA). This research was partly supported by
ASI-COFIS-2007.
1.4
Pulsating variable stars
People involved at OAB: Bellazzini, Cacciari, Clementini, Contreras, Federici, Fusi Pecci, Tosi
The role played by pulsating variable stars in establishing the astronomical
distance scale and in tracing different stellar generations in galaxies (see
e.g. Smith, Catelan & Clementini 2009, and Clementini 2010) are major
fields of study at the INAF-OAB.
19
1.4.1
Variable stars in the remote Galactic globular cluster
NGC 2419
People involved at OAB: Clementini, Federici
NGC 2419, one of the brightest and most distant clusters in the MW halo,
is a metal-poor Oosterhoff type II system suspected to be the relic of an
extragalactic system accreted by the MW. We have completed the study
of the variable stars in this cluster and published the paper presenting the
catalogue of multi-band light curves and the distance to the cluster derived
with different techniques based on the cluster variables (Di Crescienzo et
al. 2010, AJ, in press).
This work is in collaboration with M. Marconi, I. Musella, V. Ripepi, M.
Dall’Ora (INAF-Napoli Obs.), R. Di Crescienzo (INAF-Roma Obs.), L.
Di Fabrizio (INAF-TNG), C. Greco (UniGe). This research was partly
supported by PRIN MIUR 2007 (PI: G. Piotto).
1.4.2
Variable stars in the globular cluster M54
People involved at OAB: Bellazzini, Cacciari
New BVI time series photometry has allowed us to nearly double the number of pulsating variable stars in M54 for which ephemerides are known.
The large majority of the RR Lyrae variables likely belong to M54. The
pulsation properties of the M54 RR Lyrae variables are close to those of
Oosterhoff I clusters, but a significant number of long-period ab type RR
Lyrae are present. Reddening, distance and metallicity have been estimated both for the cluster variables and for those likely belonging to the
field. The M54 metallicity distribution has a symmetric bell shape, with
a mean of [Fe/H] = −1.65 and a standard deviation of about 0.15 dex,
whereas the supposed members of the Sagittarius galaxy indicate a wide
range of metallicities. The paper Sollima et al. (2010) presents these results.
This work is in collaboration with A. Sollima (IAC, Spain) and is based on
the Master Thesis work by S. Colucci.
1.4.3
Variable stars in nearby galaxies
People involved at OAB: Clementini, Contreras, Federici, Tosi
The detection and study of the pulsating variables in a number of LG
20
galaxies (Fornax, Ursa Minor, Small Magellanic Cloud, M31), as well as
in several of the new ultra-faint satellites recently discovered around the
Milky Way and Andromeda galaxies, and in most distant systems like the
blue compact galaxy (BCD) IZw18, is being carried out in collaboration
with E. Held, M. Gullieuszik and L. Rizzi (INAF-Padova Obs.), E. Poretti
(INAF-Brera Obs.), M. Moretti (Univ. Bologna), M. Marconi, I. Musella,
V. Ripepi, M. Dall’Ora (INAF-Napoli Obs.), L. Di Fabrizio (INAF-TNG),
C. Greco (UniGe), G. Fiorentino (Groningen), H. Smith (MSU, USA), M.
Catelan (PUC, Chile), B. Pritzl (Macalester Univ., USA), A. Nota (STScI,
USA), J. Gallagher (Univ. Wisconsin, USA), E. Grebel (ARI, Heidelberg,
Germany), K. Kinemuchi (Univ. of Florida, USA), T. Beers (MSU, USA),
A. Aloisi, R. van der Marel (STSci, USA), F. Annibali (INAF-Padova Obs.),
A. Saha (NOAO, USA).
The Fornax Project
The Fornax project (Clementini et al. 2007) is an international collaboration set up to make a comprehensive and deep (V ≤ 26 mag) study of
the variable star population in the field and globular clusters of the Fornax dSph. To this end we have carried out a wide-area (∼ 1 deg2 ) time
series photometric survey of the galaxy field, as well as obtaining high spatial resolution photometry of the Fornax GCs. In 2009 we have published
results from the study of the variable stars in cluster Fornax 5 (Greco et
al. 2009). A paper presenting the study of the variable star population in
cluster Fornax 3 is in preparation (Clementini et al. 2010, in preparation).
According to the pulsation properties of the RR Lyrae stars, the Fornax
GCs have been found to belong to an Oosterhoff-intermediate class and to
fill the Oosterhoff-gap defined by the Galactic GCs.
This study is in collaboration with E. Held, M. Gullieuszik (INAF-Padova
Obs.), E. Poretti (INAF-Brera Obs.), M. Catelan (PUC, Chile), H. Smith
(MSU, USA), B. Pritzl (Macalester Univ., USA). This research was partly
supported by MIUR-PRIN04 grant n. CRA 1.06.02.03, and by PRININAF06 grant n. CRA 1.06.09.15.
The “Small Magellanic Cloud in Space and Time” and “The
VISTA near-infrared Y JKs survey of the Magellanic System, VMC”
As part of large international collaborations we are making a detailed and
comprehensive study of the field and cluster stellar populations, structure and evolution of the entire Magellanic Cloud System (MCS, see also
Sect. 1.3.1). The MCS pulsating variable stars are key tools of these studies (see Clementini 2009). In 2009 we published the structural parameters
of six SMC clusters (Glatt et al. 2009) among which the only globular in
21
the SMC: NGC121. Study of the NGC121 variable stars is in progress.
Guaranteed time observations to study constant and variable star populations of the SMC body, Bridge and Stream down to the turn-off of the
oldest stars, are planned for OmegaCAM@VST (the STEP@VST survey,
PI: V. Ripepi, CoIs: members of the OAB; Ripepi et al. 2006). The MC
project was extended to the near-infrared in the framework of the approved
VMC@VISTA (The VISTA near-infrared Y JKs survey of the Magellanic
System, PI: M. Cioni, CoIs: members of the OAB) ESO public survey (see
Cioni et al. 2008). The VMC observations started in fall 2009 and are now
complete for a number of LMC fields. A full description of the survey and
results from these first data have been published in Cioni et al. (2010, A&A
submitted).
This study is part of the PhD Thesis of M. Moretti (Univ. Bologna), and
is in collaboration with V. Ripepi, M. Marconi, I. Musella, E. Cappellaro
(INAF-Napoli Obs.), A. Nota, M. Sirianni (STSCI, USA), J. Gallagher
(Univ. Wisconsin, USA), M.R. Cioni (Univ. Hertfordshire, UK), and E.
Grebel (ARI, Heidelberg, Germany). This research is partially supported
by the PRIN INAF 2008.
Stellar Archeology in the Milky Way halo: variable stars and
stellar populations in the newly discovered Milky Way satellites
Our team is systematically studying the variable star content as well as
the stellar populations of the ultra-faint dwarf (UFDs) satellites recently
discovered around the Milky Way and M31. In 2009 we published results for
3 Milky Way UFDs, namely: Coma (Musella et al. 2009), Leo IV (Moretti
et al. 2009) and UMa II (Dall’Ora et al. 2010, submitted), while analysis
is in progress on Hercules, UMa I, Leo T, and for the M31 UFDs And XI,
XII, XIII, and And XXI. Figure 9 shows the CMDs and maps of the Coma
dSph from our study published in Musella et al. (2009).
This study is part of the PhD Thesis of M. Moretti, and of the Master
Thesis of A. Garofalo, and is in collaboration with, V. Ripepi, M. Marconi,
I. Musella, M. Dall’Ora (INAF-Napoli Obs.), L. Di Fabrizio (INAF-TNG),
H. Smith (MSU, USA), M. Catelan (PUC, Chile), B. Pritzl (Macalester
Univ., USA), K. Kinemuchi (Univ. of Florida, USA), T. Beers (MSU, USA).
IZw18
Variable stars were identified for the first time in the very metal-poor BCD
IZw18, using proprietary ACS@HST time-series photometry (Aloisi et al.
2007). They include two long-period variables and 3 Classical Cepheids,
the lowest metallicity ones found so far. We have studied these variable
22
stars in detail and derived from the Classical Cepheids a new distance to
IZw18 (19 Mpc), which is much more reliable than that obtained from
other indicators (Fiorentino et al. 2010). We have exploited the unique
value of this metal-poor sample of Cepheids to constrain theoretical models for pulsation (Marconi et al. 2010) and extend the calibration of the
Cepheid extragalactic distance scale to low metallicity regimes. This study
is in collaboration with G. Fiorentino (Groningen, NL), M. Marconi and I.
Musella (INAF-Napoli Obs.), F. Annibali (INAF-Padova Obs.), A. Aloisi
and R. van der Marel (STScI, USA), A. Saha (NOAO, USA) and is partially
funded by ASI-Cofis-2007.
1.4.4
Variable stars in the Andromeda galaxy
People involved at OAB: Bellazzini, Cacciari, Clementini, Contreras, Federici, Fusi Pecci, Tosi
Our team is studying the pulsation characteristics of short and intermediate
period pulsating variable stars in the M31 halo, in its giant tidal stream,
in the M31 GCs and in the new M31 dSph satellites. Observing time with
the Large Binocular Telescope (LBC@LBT) was awarded to the project in
2009 (see Clementini et al. 2010, AJ submitted). In addition, 78 orbits with
WFPC2 on board of the HST had been awarded in HST Cycle 15 (PI G.
Clementini) to study the variable star population of six properly selected
globular clusters of M31. Data reduction has been completed for all 6
clusters (see Contreras 2010, PhD Thesis work). Results on the variable
star population in B514 were published in Clementini et al. (2009); analysis
is in progress for the other five clusters.
The study is in collaboration with M. Marconi, V. Ripepi (INAF-Napoli
Obs.), H. Smith (MSU, USA), M. Catelan (PUC, Chile), B. Pritzl (Macalester Univ., USA), K. Kinemuchi (Univ. of Florida, USA). This research is
partially supported by ASI-Cofis-2007.
23
Figure 9: Upper panels: V, B −V (left) and V, V −I(right) CMDs of the ultra-faint
Milky Way dwarf spheroidal satellite Coma (Musella et al. 2009). Solid (blue) and
dashed (black) lines are the ridgelines of the Galactic globular clusters M68 and
M3, respectively. Red and cyan dots are stars respectively within ± 0.06 mag
in B − V and ± 0.05 mag in V − I, and from ± 0.05/0.06 to ± 0.1 mag from
the ridgelines of M68. Blue dots are nonvariable stars on the galaxy HB, green
dots are stars in the blue stragglers’ region. Variable stars are marked by filled
triangles, cyan: RRc star, magenta: RRab star, blue: short period variable. Open
circles mark 24 spectroscopically confirmed members of the Coma dSph. Black
dots are galaxies of cluster MaxBCG J 186.85861+2380004. Lower panels: maps
of objects most likely belonging to the Coma dSph, colour-coded and with the
same symbols as in the top panels of the figure. HB stars are outlined by squares.
The large circles show the galaxy half-light radius rh (exponential) = 5.9 arcmin.
The dashed circles show the position of the galaxy cluster.
24
2
Extragalactic Astronomy and Cosmology
XMM X-ray image of RXCJ 1314.4 −2515 with superimposed 610 MHz radio
contours. The white line indicates the approximate position of the shock
People involved at OAB:
• Scientific staff: S. Bardelli, M. Bolzonella, A. Cappi, P. Ciliegi, A. Comastri, H.R. de Ruiter (transferred, May 1), S. Ettori, R. Gilli,
C. Gruppioni, M. Meneghetti, R. Merighi, M. Mignoli, L. Pozzetti,
G.M. Stirpe, G. Zamorani, V. Zitelli, E. Zucca;
• Fellows and contracts: A. Baldi, H. Dominguez Sanchez, I. Georgantopoulos, M. Gitti, K. Iwasawa, J. Merten, P. Nair, P. Ranalli,
N. Roche, D. Vergani.
Observational extragalactic astronomy has traditionally been one of the
main themes of research at the Bologna Observatory. It includes a wide
range of subjects, from the structure and evolution of “normal” galaxies, to
the physical properties of active galactic nuclei (AGN) and galaxy clusters,
to large-scale structures and observational cosmology.
The extragalactic research at the Bologna Observatory is characterized by
a multi-wavelength (radio, infrared, optical, X-ray) study of galaxies, AGN
and clusters of galaxies. Much of this research is based on an intensive use
of the most advanced instruments available today: the ESO optical/NIR
telescopes (including VLT), the Hubble Space Telescope, the X-ray satellites Chandra and XMM-Newton, the IR satellite Herschel, the Westerbork,
VLA and ATCA radio-telescopes.
2.1
2.1.1
Active galactic nuclei and star-forming galaxies
Optical studies
People involved at OAB: de Ruiter, Stirpe, Zitelli
Continuum variability In 2009 Zitelli and Stirpe, in collaboration with
Trevese (Univ. Roma La Sapienza) and Vagnetti (Univ. Roma Tor Vergata), continued a study of a composite sample of AGN candidates selected
in SA57 following different searching techniques, to identify low luminosity AGN (LLAGN), and break down the sample into different classes of
objects. Analysis continued on observations obtained at the TNG.
Emission lines in AGN G. Stirpe, in collaboration with P. Marziani, M.
Calvani (INAF–Padova Observatory), D. Dultzin-Hacyan (UAM, Mexico
26
City), J. Sulentic (IAA, Univ. Granada), and S. Zamfir (Univ. of Alabama),
has continued the study of the broad-emission line characteristics of a sample of high-z QSOs. New observations of the Hβ region of were obtained
at the VLT/ISAAC, extending the existing sample to radio-loud sources.
They are undergoing analysis within the framework of the Boroson-Green
Eigenvector 1 (E1), which correlates various measured properties of the
optical emission lines of AGN, extending it to the high-luminosity domain.
HST images of B2 radio galaxies H.R. de Ruiter, in collaboration with
P.Parma (INAF-IRA), and D. Bettoni and R. Falomo (INAF-OAPd) has
continued the study of B2 radio galaxies, as discussed in Bettoni et al.
(2009, A&A, 508, 1253).
2.1.2
X-ray studies of nearby objects
People involved at OAB: Comastri, Gilli, Iwasawa, Ranalli
The analysis of Suzaku observations of a small (5 objects), but representative sample of hard X-ray selected (> 10keV) candidate Compton Thick
AGN was finalized in 2009. The results indicate a variety of spectral shapes.
Three out of the five sources are Compton Thick and two of them reflection
dominated. The remaining two sources are heavily obscured (NH ∼ a few
1023 ), but Compton thin. The covering fraction of the X-ray absorber is
also very different among the sources. In one object the lack of X-ray emission below ∼ 4 keV suggest that the nuclear source may be fully covered by
the obscuring material. The shape of the soft X-ray continuum is best fitted
by a blend of emission lines arising by photoionization of circumnuclear gas
by the nuclear continuum radiation. The results, published in ApJ in 2010,
clearly highlight the complexity of the X-ray emission in Type 2 obscured
AGN and the need for further, longer exposures. Further observations with
XMM–Newton and Suzaku are being proposed for the next announcements
of opportunity.
This research is in collaboration with C. Vignali (Astronomy Dept., Univ.
of Bologna)
27
2.2
2.2.1
Surveys and observational cosmology
The VIMOS/VLT Deep Survey (VVDS)
People involved at OAB: Bardelli, Bolzonella, Cappi, Ciliegi, Merighi, Pozzetti, Vergani, Zamorani, Zucca
The VVDS consists in a Deep sample (IAB ≤ 24 objects over 1 deg2 ), a
Wide sample (IAB ≤ 22.5 objects over 8.6 deg2 ) and an Ultra-Deep sample
(IAB ≤ 24.75 objects over 0.16 deg2 ) for a total of about 50,000 measured
redshifts. The data reduction process has been completed in 2009. The
results of the survey have been published in the last few years in about
50 refereed papers. A few of the main issues which have been addressed
with these data are the estimate of the Luminosity and Mass Functions of
galaxies and their star formation history up to z ∼ 2, the comparison with
models of galaxy evolution, the study of the effect of the environment on
galaxy evolution, the analysis of spectroscopic features and their evolution
(mass-metallicity relation), the estimate of the merger rate from the number
of galaxy pairs, the Luminosity Function of type-1 AGN and the relation
between black hole mass (or Eddington ratio) and bolometric luminosity,
the properties and evolution of clustering and the relation between the
spatial distribution of luminous and dark matter (bias). Moreover, parallel
studies, joining VVDS data with surveys at different wavelengths, have
produced other interesting results, e.g. the VVDS-VLA (see the Section on
Radio Surveys) and the VVDS-SWIRE, with the estimate of the mid- and
far-infrared Luminosity Functions.
In 2009, the main contributions to the VVDS survey by the researchers at
the Bologna Observatory were the study of:
1. the history of the galaxy mass assembly and the environmental effects
on galaxy evolution up to z ' 1.4;
2. the evolution of the major merger rate via galaxy pairs since z ∼ 1;
3. the evolution with redshift of the average metallicity and its dependency on the stellar mass;
4. the luminosity function of the VVDS data up to z ∼ 4.5 and a comparison with simulations.
1. We studied how the large-scale environment affects galaxy evolution
using the galaxy number density contrast on scales of 8 Mpc. Studying a
28
sample of galaxies in the redshift range 0.2 < z < 1.4, we observed a significant mass and optical colour segregation, with redder galaxies populating
regions of higher density. When we consider only galaxies in narrow bins of
stellar mass, i.e. excluding the effects of stellar mass segregation on galaxy
properties, the colour segregation disappears, showing that the colour segregation is only a mirror of the more fundamental stellar mass segregation,
in its turn connected to the halo mass. The environmental effects on galaxy
properties, therefore, should mainly be the result of the dark matter halo
mass segregation (Scodeggio et al. 2009).
2. The evolution of the fraction of galaxies in pairs and the merging rate
since redshift ∼ 1 have been measured to understand the main phases of
galaxy evolution. The merger rate of galaxies with MB (z) ≤ −18 − 1.11 × z
has significantly evolved since z ∼ 1 and is strongly dependent on the
luminosity and spectral type of galaxies with a faster (slower) evolution for
fainter (brighter) luminosities and more frequent events in the present days
for early-type systems. We estimated that major mergers have contributed
with a fraction of about 20% to the growth in stellar mass density of bright
galaxies (de Ravel et al. 2009).
3. We reported an evolution with redshift of the average metallicity of
galaxies in agreement with the results reported in the literature. Galaxies
at redshift ∼ 1 have an average metallicity 0.3 dex lower than local galaxies
for a given stellar mass (Lamareille et al. 2009, Pérez-Montero et al. 2009).
We obtained a flattening of the mass-metallicity relation at low redshift
compared to the local Universe, but no significant metallicity evolution of
the slope between redshifts 0.7 (Lamareille et al. 2009) and 1.0 (PérezMontero et al. 2009).
4. The study of the observed luminosity function up to redshift ∼ 4.5 on
the Ultra-Deep sample (IAB ≤ 24.75) and the comparison with hierarchical
model predictions from the Millennium simulation is ongoing (Cucciati et
al. in prep.).
2.2.2
MASSIV (Mass Assembly Survey with SINFONI in VVDS)
People involved at OAB: Bardelli, Vergani, Zucca
A spin-off of the VVDS is the survey MASSIV (Mass Assembly Survey with
SINFONI In the VVDS), an ESO Large Programme started in 2007 with
300h of observation time with SINFONI, to sample a hundred star-forming
galaxies at 1 < z < 2. So far half of the sample has been observed, fully re29
duced, and analysed. The modelling of the SINFONI integral field dynamics allows us to obtain a robust measurement of the maximum rotational
velocity and other kinematic properties to properly assess the dynamical
vs baryonic mass budget. This has implications on the gas fraction, the
evolution of fundamental relations, and the relative contributions of merging and other processes (i.e., continuous gas accretion or feedback) in the
early assembly of massive galaxies. First results based on a pilot sample
have already been published (Epinat et al. 2009, Queyrel et al. 2009).
2.2.3
The VImos Public Extragalactic Redshift Survey: VIPERS
People involved at OAB: Bolzonella, Cappi, Vergani, Zamorani
VIPERS (PI Guzzo) is the widest ESO Large Programme approved so
far, started in 2008, aiming at mapping the spatial distribution of galaxies
up to z ∼ 1. This spectroscopic survey will measure 100,000 redshifts of
IAB ≤ 22.5 galaxies using the VIMOS@VLT spectrograph over an area of
24 square degrees with a sampling of ∼ 50%. It will represent the high
redshift analogue of local surveys like the 2dFGRS.
The main goal of the survey is the study of the large scale structures, their
cosmological implications, and the evolution of bright galaxies in different
environments with a high statistical accuracy and low influence from the
cosmic variance. Observations started during summer 2008 and the redshift
measurements of the first 10,000 galaxies have been already achieved.
2.2.4
The Herschel guaranteed time extragalactic survey: PACS
Evolutionary Probe (PEP)
People involved at OAB: Gruppioni
The PACS Evolutionary Probe (PEP) is a Herschel guaranteed time key
programme survey of the extragalactic sky, aimed at studying the restframe far-infrared emission of galaxies up to redshift ∼ 3, as a function of
environment. The survey is shedding new light on the constituents of the
cosmic IR background and their nature, as well as on the co-evolution of
AGN and starbursts.
The PEP survey is driven by science goals addressing a number of key open
topics in galaxy evolution.
• Resolve the Cosmic Infrared Background and determine the nature
30
of its constituents
• Determine the cosmic evolution of dusty star formation and of the
infrared luminosity function
• Elucidate the relation of far-infrared emission and environment, and
determine clustering properties
• Determine the contribution of AGN
• Determine the infrared emission and energetics of known galaxy populations
The Science Demonstration Phase (SDP) PEP data in the GOODS-North
Field have been released to the consortium at the end of November 2009.
C. Gruppioni is the PI of one of the main scientific projects with PEP data,
titled: “Luminosity function of FIR galaxies and AGN and its evolution
with redshift”. The work on the PEP Luminosity Function with the SDP
data in the GOODS-North field has been published by Gruppioni et al.
(2010) in the A&A Special Issue dedicated to the first results of Herschel .
2.2.5
X-ray Surveys
People involved at OAB: Comastri, Georgantopoulos, Gilli, Iwasawa, Mignoli, Ranalli, Zamorani
This research is in collaboration with C. Vignali, E. Lusso (Astronomy
Dept., Univ. of Bologna).
The OAB team is deeply involved in the exploitation of the X-ray and
multiwavelength follow-up observations of both the ultra deep CDFS and
the large area COSMOS surveys.
The Chandra Deep Field South (CDFS) is, by far, the most extensively
studied extragalactic field. The deepest surveys at virtually all wavelengths
are carried out in the CDFS. In the X-ray band it was targeted by Chandra
with a long (almost 4 Ms) exposure in the central 0.1 sq. degree, complemented by 4 shallower (250 ksec) flanking fields (the Extended CDFS)
bringing the covered area to about 0.25 square degrees. An ultradeep (∼ 3
Ms) XMM–Newton exposure providing the most sensitive view of the hard
X-ray sky is currently ongoing (PI A. Comastri). This is the largest ever
approved XMM programme. The most important scientific issues which
will be addressed include: the search for and the detailed spectroscopic
study of obscured and Compton-Thick AGN at the redshift peak of their
31
activity (z ∼ 1–2), and, thanks to the excellent multiwavelength coverage,
the study of the role of accreting SMBHs in the context of galaxy evolution.
This project, targeting a “new” unexplored discovery space, will create an
XMM legacy and a pathfinder for future X-ray missions.
In 2009, the first part (about 1.5 Ms) of the XMM–Newton observations
were received and combined with archival data in the same field. We devised
a multi-step strategy to perform data analysis and reduction which turned
out to challenge the available software requiring the developement of new
tools and utilities. A sophisticated X-ray simulator has been developed
and tested. The spectra of a representative sample of candidate Compton
Thick AGN (from Chandra observations) were extracted and analyzed.
The COSMOS survey is by now a mature project. The vast majority of
the data were already fully reduced and analysed, especially with regard
to the XMM–Newton and Chandra X-ray surveys. In 2009 the Chandra
X-ray catalogue and a paper describing the data analysis techniques were
published. A major effort was put in the identification of the Chandra
source counterparts using the excellent quality COSMOS multiwavelength
database. The photometric redshift catalogue of all the XMM sources was
also published in 2009, providing for the first time a redshift accuracy
comparable to that of “normal galaxy” samples. A major effort was put in
the compilation of a truly multiwavelength catalogue of the > 1800 sources
of the XMM sample, including, whenever available, higher level products
such as black hole masses, host galaxy masses, star formation rates and so
on.
Among the various AGN science projects aimed to exploit the powerful
multiwavelength COSMOS archive, a few of them deserve to be mentioned
due to the significant contribution of the OAB team. More specifically:
the study of the optical to X-ray flux ratio distribution for a large sample
(≈ 500) of Type 1 AGN, the first determination of the space density of
high redshift (z > 3) X-ray selected AGN, and a detailed analysis of the
broad-band Spectral Energy Distribution of optically and X-ray obscured
Type 2 AGN.
2.2.6
The zCOSMOS survey
People involved at OAB: Bardelli, Bolzonella, Cappi, Ciliegi, Coppa, Mignoli,
Nair, Pozzetti, Vergani, Zamorani, Zucca.
The zCOSMOS project (600 hours with VIMOS, approved in 2004 and
32
started on April 2005; PI: S. Lilly) is a major treasury redshift survey in
the COSMOS field. The zCOSMOS collaboration involves a significant
number of researchers of the Bologna Observatory and other institutes in
Zurich, Milano, Marseille, Toulouse and Garching.
This project consists of two parallel surveys: (1) the bright survey, aiming
at observing ∼ 20,000 magnitude-selected galaxies with IAB ≤ 22.5 and
0.1 ≤ z ≤ 1.2 over 1.7 deg2 ; (2) the deep survey, with ∼ 10,000 galaxies
selected through colour-selection criteria to be at 1.4 < z < 3.0, within
the central 1 deg2 . The observations of zCOSMOS-bright were completed
in 2008 (20K sample) and the analysis on this data set is ongoing. The
completion of the zCOSMOS-deep observations is expected in 2010.
The main goal of the spectroscopic survey zCOSMOS is to characterize
galactic environments throughout the COSMOS volume out to redshifts
z ∼ 3, in particular: (1) the study of large-scale structures by means of
the evolution of correlation functions, the measure of the density field and
galaxy groups, (2) the study of diagnostics derived from spectra to determine star-formation rates of galaxies, active galactic nuclei (AGN) classification, reddening by dust, stellar population ages, and metallicities, (3)
the description of the galaxy population by means of various distribution
functions, such as the Luminosity and Galaxy Stellar Mass Functions, as
a function of different galaxy types and environments. The analysis of the
first half of the bright sample (10K sample) already produced more than 10
published papers in 2009 and a similar number of papers are in preparation,
or submitted to refereed journals.
Our group is mainly involved in the classification of galaxy types from the
spectral analysis, the study of the evolution of stellar mass and luminosity
functions, for different photometric and spectroscopic types, morphology
and environment, as well as the study of the processes driven the quenching
of the star formation activity in galaxies.
The Bologna node has led the work on the galaxy classification of Cosmos
data (ACS morphology and Subaru photometry) and the first 1K bright
zCOSMOS spectra. Applying a simple parametric classification that uses
spectral, photometric, and morphological properties, we characterized the
bimodality distribution of the galaxy population out to z ∼ 1 (Mignoli et
al. 2009). A very good agreement exists between the different estimators
resulting in 85% of the galaxies being either quiescent, red, bulge-dominated
galaxies (∼ 20%) or star-forming, blue, disk-dominated galaxies (∼ 65%).
We are currently exploring a new statistical classification based on the
33
Principal Component Analysis on the larger 10K zCOSMOS sample to
investigate the twofold nature of galaxies (Coppa et al. 2009, in prep.).
Using the spectroscopic 10k sample, we have estimated the luminosity and
stellar mass content of each galaxy, through the SED fitting of the extensive
and deep available multi-band photometry from the U to the Mid-IR bands.
Thus, we have derived the galaxy luminosity and stellar mass function up to
z ∼ 1, for the global population and for sub-classes of galaxies in different
environments (Bolzonella et al. subm. Pozzetti et al. subm., Zucca et al.
2009).
At low z, late types dominate the luminosity function at faint magnitudes,
while the bright end is populated mainly by early types. At higher z, latetype galaxies evolve significantly and, at z ∼ 1, the contribution from the
various types to the bright end of the luminosity function is comparable.
The evolution for early types is in both luminosity and normalization. A
similar behaviour is exhibited by late types, but with an opposite trend
for the normalization. Blue galaxies are the main contributors to the luminosity function in low-density environments, while red galaxies contribute
mostly to the bright end in high-density environments. This result fits in a
scenario where some of the blue galaxies are transformed into red galaxies
with increasing cosmic time, without significant changes in the fraction of
intermediate-type galaxies. The bulk of this tranformation in overdense
regions probably happened before z ∼ 1, while it is still ongoing at lower z
in underdense environments (Zucca et al. 2009).
We found a galaxy bimodality in the global mass function at 0.1 < z < 0.5,
which is explained by the different populations of late/early type galaxies at different masses. We observed a different behaviour of the number
densities of galaxies as a function of stellar mass and of galaxy type. This
result can be interpreted as the combination of a transformation with cosmic time from blue active spiral galaxies of intermediate mass into red
passive early ones, followed by a transformation on longer time scales into
spheroidal galaxies, and a continuous replacement by blue active low-mass
spirals growing in stellar mass (Pozzetti et al. subm.).
The environmental effect in the mass function is visible both in its shape,
with the afore-mentioned bimodality more evident in denser regions, and in
the population of galaxies inhabiting the extreme environments: the transformation of intermediate-mass late-type galaxies, contributing most of the
mass functions in low-density regions, into early-type galaxies, which dominate the mass function in dense environments, seems to act more rapidly
34
in dense regions from z ∼ 1 to z ∼ 0.1 (Bolzonella et al. subm.).
To understand this transformation of galaxies observed in the luminosity and mass functions, we studied the class of post-starburst galaxies in
the COSMOS field at z = 0.48–1.2, identified thanks to their k+a spectral features. These galaxies are affected by a sudden quenching of their
star-formation activity over timescales shorter than 1Gyr. We characterized their multiwavelength properties and number density, concluding that
the contribution to the mass assembly of the red-sequence due to a fast
quenching of the star formation is of the order of 10%. The star-formation
quenching is usually a smooth mode process (Vergani et al. 2009).
In collaboration with a PhD student of Bologna University (M. Moresco),
we have estimated the ages of the stellar populations of ETGs using the
SEDs. The aim is to attempt to place constraints on the equation of state
parameter for Dark Energy (w). We have also explored the mass and
environment dependence in photometric and spectral properties of ETGs.
We confirm the low-redshift results in the SDSS, finding that the colour
distribution of ETGs is not strongly dependent on the environment for
all the mass bins. On the other hand, the dependence on the mass is
much more significant, in both high- and low-redshift environments. The
spectral analysis we have performed (using the D4000 and Hδ features) is
in agreement with our photometric results (Moresco et al. 2009, in prep.).
2.2.7
The VLA-COSMOS survey
People involved at OAB: Ciliegi, Bardelli, Zamorani.
This work is carried out in collaboration with M. Bondi (INAF-IRA Bologna), E. Schinnerer, V. Smolcic, K. Jahnke (Max Plank Institute, Heidelberg, Germany), C. Carilli (NRAO, Socorro, USA), and S. Giodini (MPE).
The VLA-COSMOS survey (Schinnerer et al. 2007) is a deep radio survey
performed at the VLA on a 2 deg2 field centred on the COSMOS area.
Additional VLA A array observations at 1.4GHz were obtained for the
central degree of the COSMOS field and combined with the existing data.
In 2009, a newly constructed Deep mosaic with a resolution of 2.5 arcsec was
used to search for sources down to a radio flux of 48µJy in the central 50×50
arcmin field. This new source list has been combined with the catalogue
from the Large project to construct a new Joint catalogue, published by
Schinnerer et al. (2010) and available for download by the public at the
35
Figure 10: HST image of the dominant galaxy of a COSMOS group with superimposed the VLA 1.4 GHz radioisophotes.
36
COSMOS archive at IPAC/IRSA (http://irsa.ipac.caltech.edu/
data/COSMOS/tables/vla).
We studied the properties and environment of radio galaxies in the combined VLA-zCOSMOS sample, deriving a new method to distinguish AGN
from star-forming galaxies. We found that only AGN hosted in passive
galaxies reside in higher densities than a control sample of similar nonactive galaxies, while AGN, whose galaxy host forms stars, do not show
any environment dependence. Moreover, the radio luminosity of the AGN
is correlated to the stellar mass of the host galaxy in a low density environment. In high densities, the relation is lost, because in this case the feeding
of the black hole is due to the cooling of the gas of the hosting group or
cluster (Bardelli et al., 2010)
Using a sample selected jointly at IR and radio wavelengths in order to
reduce selection biases, we provide firm support for previous findings that
the IR-radio relation remains unchanged out to at least z ∼ 1.4. Moreover,
based on data from ∼ 150 objects we also find that the local relation likely
still holds at z ∈ [2.5, 5] (Sargent et al., 2010).
Giodini et al. (2010), studying radio AGN, which show extended emission
at the centre of galaxy groups, found that the mechanical energy released
by the black hole activity is comparable or larger than the potential energy
of the group. This means that some baryons of the intra group medium
can be lost and the baryon-to-mass fraction lowered.
2.2.8
The EUCLID project
People involved at OAB: Zamorani, Bardelli, Buzzoni, Cappi, Ettori, Gruppioni, Meneghetti, Mignoli, Pozzetti, Vergani, Zucca
In 2009, we continued the preparatory work for the ESA EUCLID mission,
whose primary task is to investigate Dark Energy and constrain its cosmological parameters with a number of cosmological probes (e.g. weak lensing
and Baryonic-Acoustic-Oscillations). This will be achieved through high
quality optical and NIR imaging and NIR spectroscopy, over 20,000 square
degrees of the sky.
EUCLID is a space telescope with a primary mirror of 1.2m diameter
equipped with 1) an optical imaging channel, which will be used to measure the shapes of galaxies and extract the lensing signal by the large-scale
structures in the universe. The PSF will be ∼ 0.1800 , and the observations
37
will be carried out in a single wide-band covering the wavelength range
of 550–920nm; 2) a near-IR channel, which will perform both photometry in the Y, J, and H bands for photometric redshift determinations and
slitless spectroscopy in the wavelength range 1–2µm at spectral resolution
R = 400, achieving redshift measurements with accuracy dz < 0.001. The
mission is now in phase-B, together with other two missions, and the final
down-selection will be in June 2011.
We are involved in both the imaging and spectroscopic aspects of the mission.
For the imaging channels, we were responsible for the image simulations.
Our primary goal was to assess whether the new design of EUCLID will
match the scientific requirements of the mission. This includes evaluating whether the spatial resolution (PSF) is compatible with precise galaxy
shape measurements, and the sensitivity is high enough to detect a sufficient
number of sources with high signal-to-noise ratio at the planned exposure
time. With this aim, simulated EUCLID observations were created with
SkyLens (Meneghetti et al. 2008), a locally developed software which allows to simulate patches of sky including the instrumental response, realistic
source morphologies, and all relevant observational noises. The simulations
allowed to estimate that EUCLID will observe about 35–50 galaxies/sq. arcmin at the signal-to-noise required for precise shape measurements. The
median redshift of these galaxies will be z ∼ 1.
For the spectroscopic channel, we have continued to work on the science
cases of the mission. In parallel, we have constructed a realistic input galaxy
catalogue to be used for the spectroscopy simulations. This catalogue,
which includes the emission line properties (fluxes and equivalent widths)
of galaxies over the redshift range of interest for EUCLID (0.5 < z < 2.0),
was produced from the existing multi-wavelength data-set in COSMOS and
is now being exploited in extensive and realistic simulations, which will be
used to optimize the final instrument configuration and to test and improve
the methods of data analysis.
2.2.9
The SAFARI instrument for the ESA/JAXA joint mission
SPICA
People involved at OAB: Gruppioni
SPICA is a proposed next generation infrared satellite for cosmology and astrophysics and a candidate mission for the ESA Cosmic Vision. A Japanese38
led, joint JAXA-ESA mission, SPICA will have a single-element, high surface accuracy 3.5m mirror, cooled to ∼ 4.5 K. The combination of large
collecting area, low self-emission and diffraction-limited performance over
a core wavelength range of 5–210µm will provide the basis for a sensitive
and versatile suite of focal plane instruments. These include: a largeformat MIR camera (5–38µm) and MIR spectrometer (R ∼ 30, 000 at 4–
18µm; Rsim3,000 at 16–38µm)), a high contrast (10–6) MIR coronograph
(5–27µm) with photometric and spectroscopic capabilities, a FIR imaging
spectrometer and camera (35–210µm), and a single-pixel high sensitivity,
low-resolution FIR/submm grating spectrometer (40–350µm). The FIR
imaging spectrometer and camera (SpicA FAR-infrared Instrument – SAFARI) is a European-led instrument (PI Bruce Swinyard, UK) which covers
the 30–210µm waveband with a spectral resolution of R ∼ 10 to 10000, and
a field of view of 20 × 20 . The baseline optical configuration of SAFARI is
a Mach-Zehnder imaging Fourier Transform Spectrometer. The principal
advantages of this type of spectrometer for SAFARI are the high mapping
speed of the FTS due to spatial multiplexing, the ability to incorporate
straightforwardly a photometric imaging mode and the operational flexibility to tailor the spectral resolution to the science programme.
SPICA is ideally suited to study star-formation hidden by dust absorption,
by tracing the solid state features of dust further into the past than ever
before. The combination of mid infrared and far infrared spectroscopy on
SPICA will provide, for the first time, the capability to detect the cooling
lines out to the peak of star formation activity in the history of the Universe (z ∼ 1–2) for a wide range of galaxy types. SPICA will enable the
study of interstellar medium conditions in central outbursts, circumnuclear
rings, disks, winds and halos in galaxies of the local Universe, as well as
comprehensively in sources in the distant Universe. SPICA spectroscopic
observations will be unique to address the AGN-Starburst connection at
high redshifts (z > 3). The field of view of the SPICA instruments will
provide a considerable spatial multiplexing advantage both for mapping
local, resolved, galaxies and to perform cosmological surveys. Photometrically, SPICA has the sensitivity to detect high-luminosity objects out to
z > 4 and Milky Way-type populations out to z ∼ 1.
C. Gruppioni is a member of the SAFARI-SPICA Consortium and is actively involved in the Science Working Groups planning ”Deep Extragalactic Photometric Surveys” and ”Spectro-Photometric Observations of High-z
AGNs” with SAFARI.
39
2.3
2.3.1
Galaxy clusters and large-scale structure
Lensing by galaxies and galaxy clusters
People involved at OAB: Meneghetti, Ettori, Donnarumma
Our research focusses on the study of the lensing effects by galaxies and
galaxy clusters, which we use to reconstruct the mass distribution of the
lenses.
Donnarumma et al. (2009) investigated the mass distribution in the famous
gravitational lens MS2137. This galaxy cluster has both a tangential and
a radial arc, which are used to construct a parametric model using the
public software LensTool. The resulting mass profile was compared to that
derived from the X-ray analysis of archival Chandra data. We find a good
agreement between the X-ray and SL mass estimates, which is in contrast
to several other studies where discrepancies of order 100–200% were found.
We also determine an NFW concentration which is lower than previously
measured by other authors, and in better agreement with the predictions
of LCDM. We further discuss the dependency of the reconstruction results
on the modeling of the BCG.
In Maiolino et al. (2009), we report the detection of the [CII]157.74µm finestructure line in the lensed galaxy BRI0952−0115 at z = 4.43, using the
APEX telescope. This is the first detection of the [CII] line in a source with
LFIR < 1013 L at high redshift. The line is much stronger than previous
[CII] detections at high-z (a factor of 5–8 higher in flux), partly due to the
lensing amplification. The L[CII] /LFIR ratio is 10−2.9 , which is higher than
observed in local galaxies with similar infrared luminosities. Together with
previous observations of [CII] at high redshift, our result suggests that
the [CII] emission in high-redshift galaxies is enhanced relative to local
galaxies with the same infrared luminosity. This finding may result from
selection effects of the few current observations of [CII] at high redshift
and, in particular, from non detections that may not have been published
(although the few published upper limits are still consistent with the [CII]
enhancement scenario). If the trend is confirmed with larger samples, it
would indicate that high-z galaxies are characterized by different physical
conditions than for their local counterparts. Regardless of the physical
origin of the trend, this effect would increase the potential of the [CII]158
µm line to search and characterize high-z sources.
In Merten et al. (2009) we present a novel method for combining weak
40
and strong lensing by galaxy clusters for reconstructing their mass distribution in a completely non-parametric way. The robustness of the reconstructions is quantified using numerical simulations which show that the
two-dimensional mass profile is recovered with errors < 10%. The method
is applied to MS2137, allowing to extend the work of Donnarumma et al.
(2009) and drawing the cluster mass profile covering a range of scales from
a few kpc to the virial radius.
2.3.2
The MUSIC project
People involved at OAB: Cappi
A. Cappi is involved in the MUSIC project (MUlti-wavelength Sample of Interacting Clusters), in collaboration with S. Maurogordato (PI), C. Benoist,
A. Bijaoui, C. Ferrari, E. Slezak (Observatoire de la Côte d’Azur), Hervé
Bourdin (Università di Roma), M. Arnaud and J-L. Sauvageot (CEA/CEN,
Saclay). This project is based on optical observations (ESO 3.6m and VLT,
CFHT) and on X-ray observations with XMM-Newton and Chandra, while
complementary radio observations are carried out in collaboration with
L. Feretti (INAF-IRA Bologna). We dispose of a database of clusters in
different evolutionary phases, suited for a systematic statistical study and
a quantitative comparison with theoretical predictions (Maurogordato et
al. 2000; Ferrari et al. 2003; Ferrari et al. 2005). In Maurogordato et al.
(2010), we have reconstructed the merging history of three bimodal clusters (A2933, A2440 and A2384), using optical and X-ray data and merger
simulations.
Our recent work is focussed on the hottest X-ray Abell cluster, A2163, at
z ∼ 0.2, which we observed with VIMOS at the VLT. We have identified
the main components and merger directions and estimated its dynamical
mass (Maurogordato, Cappi, Ferrari et al. 2008). In Bourdin et al. (2010,
in press) we study the gas structure and dynamics by means of spectralimaging analysis of X-ray data obtained from XMM-Newton and Chandra
observations and show that the exceptional properties of A2163 present
various similarities with those of 1E0657−56, the so-called ‘bullet-cluster’,
likely related to a comparable merger scenario. Further work is presently
carried out to study the effect of merging on star formation.
41
2.3.3
Galaxy clusters in the CFHTLS and in the DAFT
People involved at OAB: Cappi
A. Cappi is involved in an ongoing study of galaxy clusters detected in the
Canada French Hawaii Telescope Legacy Survey (CFHTLS), in collaboration with C. Benoist, C. Ferrari, S. Maurogordato, F. Martel, E. Slezak (Observatoire de Nice), C. Adami and A. Mazure (Laboratoire d’Astrophysique
de Marseille, France). At the Observatoire de la Côte d’Azur a database has
been implemented: this database includes the cluster catalogue obtained
through the matched filter technique (Olsen, Benoist, Cappi et al. 2007,
2008), while in Adami et al. 2010, we present a catalogue of clusters detected in deep and wide fields of the CFHTLS using photometric redshifts.
These catalogues will provide cluster samples with a completeness limit in
mass, in order to study cluster evolution and to constrain the cosmological
parameters.
Cappi collaborates also with the DAFT (Dark energy American French
Team) which has started a large project to characterize statistically high
redshift galaxy clusters (at z ≥ 0.4), infer cosmological constraints from
weak lensing tomography, and understand biases relevant for constraining
dark energy and cluster physics in future cluster and cosmological experiments. In 2009 Cappi obtained infrared observations of a subsample of
these clusters at the Galileo National Telescope, and in Guennou et al.
(2010) the technique for the photo-z determination which will be used in
all subsequent papers, including weak lensing tomography studies, is described and tested.
2.3.4
A search for Relics and Halos in the redshift range z = 0.2–
0.4
People involved at OAB: Bardelli, Zucca
This work is carried out in collaboration with T. Venturi, G. Brunetti,
G. Macario (INAF-IRA Bologna), D. Dallacasa, R. Cassano (Astronomy
Dept., Univ. of Bologna), P. Mazzotta (Rome University), P. Rao (Pune,
India), S. Giacintucci (CfA).
This year we analysed the multiwavelength properties of the two clusters
Abell 697 and RXCJ 1314 −2515. Abell 697 has been observed with the
Giant Metrewave Radio Telescope at 325 and 610 MHz and we reanalysed
archival data at 1.4 GHZ. The size of the halo reaches the value of ∼ 1.3
42
Mpc, which is considerably larger than at other frequencies. We derived
an integrated spectral index, finding a value of 1.7. This value indicated
that the spectrum of the radio halos is very steep and belongs to a new
class of clusters recently found (Brunetti et al., 2009). Moreover, from
Chandra ACIS-I we inferred the dynamical state of this cluster (Macario
et al., 2010).
RXCJ1314.4 −2515 is an exceptional cluster showing two radio relics and
one radio halo. We obtained XMM observations in the X-ray band of ∼ 50
ksec. The analysis of the image (see the frontispiece of this chapter) revealed
a shock just under the radio relic, reinforcing the hypothesis that such radio
objects are formed by accelerated electrons during cluster-cluster merging
(Mazzotta et al. 2010, in prep.). Note that only a handful of clusters show
confirmed shock features.
2.3.5
Galaxy clusters in X-rays
People involved at OAB: Ettori, Baldi, Gitti
Our research focusses on the study of the observational properties of X-ray
luminous galaxy clusters and groups and on their evolution.
We analysed Chandra observations of two cool core galaxy clusters in order
to study the physical properties of the intra-cluster medium (ICM) and of
the brightest cluster galaxy (BCG). In particular, we found that in Abell
1664 (z = 0.128) the BCG is unusually blue and is forming stars at a rate
(∼ 20 solar masses per year) of the order of the cooling rate, thus consistent
with fuelling by the cooling flow (Kirkpatrick et al. 2009).
We also examined the metallicity structure near the central galaxy of the
Hydra A cluster (z = 0.055) and along its powerful radio source, showing
that the metallicity of the ICM is enhanced by up to 0.2 dex along the
radio jets and lobes compared to the metallicity of the undisturbed gas (see
Fig. 11). Evidently, Hydra A’s powerful radio source is able to redistribute
metal-enriched, low entropy gas throughout the core of the galaxy cluster
(Kirkpatrick, Gitti, Cavagnolo et al. 2009)
Gastaldello et al. (2009) present a 2D analysis of the bright nearby galaxy
group NGC5044 using the currently available Chandra and XMM data.
For the first time in a low mass relaxed object, sloshing cold fronts have
been detected. In the inner 10 kpc, X-ray cavities and bright filaments,
coincident with Hα and dust emission, are observed. This suggests the
43
Figure 11: Metallicity map showing the central 50 ×50 of Hydra A. Brighter regions
represent a higher metallicity. The 330 MHz radio emission is shown by the white
contours and the 1400 MHz radio emission is shown by the black contours. From
Kirkpatrick, Gitti, Cavagnolo et al. 2009.
presence of dust-aided cooling contributing to form warm (104 K) gas,
emitting Hα radiation.
We have undertaken a study of the metal distribution in nearby clusters
with temperature around 2–4 keV. In Gastaldello, Ettori et al. (2010), we
present the XMM observation of the first object of the sample, A2028,
which reveals a complex structure of the cluster over a scale of ∼ 300 kpc.
We show that the inverse iron-bias is responsable for the measured high
metallicity.
A detailed study of the metal distribution in high redshift clusters observed
with XMM is underway (Baldi, Ettori et al. 2010; see fig. 12).
Ettori & Balestra (2009) study the properties of the X-ray surface brightness profiles in a sample of massive galaxy clusters observed with Chandra
at z > 0.3. We measure a consistent steepening of the Sb (r) profile moving
outward from 0.4R200 and make a firm prediction on its mean value at the
virial radius.
44
Figure 12: Abundance measured by EPIC XMM-Newton as a function of redshift
for the clusters in our sample in different spatial bins (from bottom to top: 0.15–
0.6r500 , 0–0.15r500 , 0.15–0.4r500 , and > 0.4r500 ).
Ettori et al. (2009) present the analysis of the baryonic content of 52 Xray luminous galaxy clusters observed with Chandra in the redshift range
0.3–1.3, providing tight constraints on some cosmological parameters with
a detailed discussion on the systematic uncertainties affecting the results.
In Ettori et al. (2010), we constrain the NFW profiles in a sample of 44
X-ray luminous galaxy clusters observed with XMM-Newton in the redshift
range 0.1–0.3 and set limits on the normalization and shape of the power
spectrum of cosmological mass fluctuations using the distribution of the
measured concentration parameters and total mass.
In collaboration with the University of Bologna, we are realizing and analysing
hydrodynamical simulations in a cosmological contest with different dark
energy components. In De Boni et al. (2010), we investigate how the dark
energy influences the formation of galaxy clusters and the interplay between the different background cosmology and the evolving distribution of
the luminous matter.
45
This work is carried out in collaboration with F. Brighenti, L. Moscardini
(University of Bologna), F. Gastaldello, S. Molendi (INAF-IASF Milano),
S. Borgani (Univ. of Trieste), P. Rosati (ESO), P. Tozzi (INAF-OA Trieste).
46
3
Hydrodynamics
People involved at OAB:
• Scientific staff: R. Bedogni, A. D’Ercole, P. Londrillo.
R. Bedogni extended the evolution of the instabilities for Type I and typeII
SNe to the case of a different cooling curve with an inhomogeneous medium.
The possibility was explored of a variable energy input for the case of energy
injection of SNRs.
In collaboration with C. Melioli and F. Brighenti (Bologna University),
and with Gouveia Dal Pino (S. Paulo University), A. D’Ercole worked out
3D numerical hydrodynamic models of galactic fountains powered by SNe
II belonging to O-B stellar associations with the observed mass distribution. These fountains produce Intermediate Velocity Clouds, but not High
Velocity Clouds; the latter, therefore, must have an extra-galactic origin,
which is consistent with their low metal abundance. The metals delivered
by the SNe II are ejected into the Galactic halo, and then fall back onto the
disk, not far (< 1kpc) from the place where they were produced; thus, the
fountains do not alter the radial chemical gradient of the disk. Moreover,
the simulations show that nearly 10% of the SN energy goes into heating
of the hot Galactic gaseous halo, balancing its radiative losses.
47
4
Instruments and Technology
Multi conjugate Adaptive Optics RelaY (MAORY) for the European Extremely
Large Telescope (E-ELT).
Above. MAORY is located on the E-ELT Nasmyth platform to the right of the
pre-focal station. The client instrument MICADO is shown below the MAORY
bench.
Below, left. Image of a point-like source after the atmospheric turbulence correction performed by MAORY; the image peak is normalized to the peak of the
instrumental response of an ideal instrument limited by pure diffraction, showing
the so called Strehl Ratio (about 0.5 in this case).
Below, right. Strehl Ratio map showing the performance achieved by MAORY
at infrared wavelengths (2.16 µm) over an extended field of view. The adaptive
optics correction is remarkably uniform out to a distance of 60 arcsec from the
field center. The high Strehl Ratio also denotes an excellent energy concentration
in the core of a point-like source image, a property that allows the separation of
sources as close as 10 milli-arcsec or less and improves the detection capability of
faint sources against the sky background.
People involved at OAB:
• Staff: M. Bellazzini, A. Bragaglia, G. Bregoli, C. Cacciari, P. Ciliegi,
G. Clementini, E. Diolaiti, L. Federici, F. Fusi Pecci, M. Lolli, P.
Montegriffo, L. Origlia, E. Pancino, V. Zitelli
• Contracts: G. Altavilla, G. Cocozza, G. Innocenti, M. Lombini, Y.
Maruccia, S. Ragaini, E. Rossetti
The development of advanced instrumentation is carried out at OAB in the
framework of a close collaboration between technical and scientific counterparts. OAB personnel is involved in the space mission GAIA and in
instrumental projects for present and future ground-based facilities such
as Telescopio Nazionale Galileo, Large Binocular Telescope, European Extremely Large Telescope. Astronomical site testing is a traditional field of
activity at OAB. Technological research has received a boost in the last
few years thanks to the setup of a new optical laboratory, dedicated to the
development, prototyping and integration of instrumentation.
4.1
The GAIA project
People involved at OAB: G. Altavilla, M. Bellazzini, A. Bragaglia, C.
Cacciari, G. Clementini, G. Cocozza, L. Federici, F. Fusi Pecci, P. Montegriffo, E. Pancino, S. Ragaini, E. Rossetti
The technical activity for Gaia, within the Data Processing and Analysis
Consortium (DPAC), includes the absolute calibration of the Gaia photometric system and the characterization and treatment of the RR Lyrae and
Cepheid variable stars.
The absolute calibration of the Gaia photometric system requires: i) the use
of a large grid of Spectrophotometric Standard Stars (SPSS) with accurate
flux-calibrated Spectral Energy Distributions (SEDs), that are presently being obtained from a dedicated ground-based observing campaign under the
responsibility of E. Pancino, and ii) a calibration model and Java application classes, presently being derived under the coordination of C. Cacciari.
The observing campaign is more than half way through, and the data reduction is in progress. The calibration model definition, test and optimization
are proceeding, with continuous refining and updating as more detailed information is being provided by the other development units of the project.
51
The activity on variable sources is carried on by G. Clementini, who is responsible for the task Supplementary Observations (i.e. ground-based support to Gaia’s observations of variable sources) and for the specific treatment of RR Lyrae and Cepheid variable stars. In collaboration with staff
members and fellows at the Napoli Observatory software tools are being developed to validate and refine the classification of Cepheids and RR Lyrae
stars and to characterize their properties.
All the above activities are documented in internal reports and in technical notes that are posted on the Wiki-BO and/or GAIA Livelink (see
publication list).
These activities are in collaboration with Italian scientists in Napoli, Roma
and Teramo, and with the Gaia European nodes in Barcelona, Cambridge,
Geneva, Leiden and Groningen.
On the photometric calibration, contributions have been provided also by
a PhD and a Master thesis student:
• Silvia Marinoni, PhD student, thesis title: Calibration plan, Quality Control and optimisation of data analysis for red and infrared
spectroscopic observations from TNG and other ground based telescopes, tutors: B. Marano (Astronomy Dept., Univ. of Bologna) and
E. Pancino (OAB), expected completion beginning of 2011;
• Carmela Lardo, Master student, thesis title: Definition of strategy
and procedures for ground-based data reduction and Gaia absolute flux
calibration, tutors: F.R. Ferraro (Astronomy Dept., Univ. of Bologna)
and E. Pancino (OAB), completed in March 2009.
4.2
GIANO: an ultra-stable IR spectrometer for TNG
People involved at OAB: P. Montegriffo, L. Origlia, E. Rossetti, M. Lolli
The recent development of high sensitivity infrared (IR) spectrometers has
opened a new window in astrophysics. The investigation of the 1 to 2.5
µm band has yielded the discovery of a wealth of diagnostic tools, both
in terms of absorption features and emission lines, which are crucial for a
thorough understanding of several hot topics of modern astrophysics, from
faint solar system objects and extra-solar planets to stellar clusters and
galaxies, up to the highest redshift quasars. The much reduced extinction
at these wavelengths allows IR spectrometers to pierce the dust embedding
52
Figure 13: The GIANO cryostat.
several Galactic and extragalactic objects, which are heavily obscured in the
optical. At high redshift several emission and absorption spectral features,
commonly exploited when studying local galaxies, are shifted into the IR.
These and several other advantages of IR spectroscopy have led to a rapid
growth of the community of astronomers, from essentially any scientific
field, making use of these facilities.
GIANO is an optimized near IR spectrograph which can yield, in one shot,
complete 0.9–2.5µm spectra at high resolution (up to R = 46000 with a
0.5” slit) maintaining a very high stability and throughput throughout the
whole spectral range.
This project is part of the Second Generation Instrumentation Plan of the
Telescopio Nazionale Galileo (TNG) located at Roque de Los Muchachos
Observatory (ORM), La Palma, Spain.
The core of GIANO is the spectrometer unit which uses, in double pass, the
same optical elements (3 aspheric mirrors) as collimator and camera. These
feed, through cross-disperser prisms, a commercial 23.2 ll/mm R2 echelle
53
grating acting as high resolution disperser. All these elements and the 20482
Hawaii-2 array are fixed to an optical bench which will operate in vacuum
at cryogenic and thermostated temperatures. Measurements of circular and
linear polarization can be obtained using a combination of beam splitters
and super-achromatic retarders which can be inserted/rotated in the preslit optical system.
The GIANO team includes several Italian researchers and technicians from
INAF (Bologna, Firenze, Catania Observatories, Fundacion Galileo Galilei)
and has collaborations with the Istituto Nazionale di Ottica Applicata
(Firenze) and a few engineering companies. The project management is
undertaken in a coordinate way by L. Origlia (Bologna) – Principal Investigator – and E. Oliva (Arcetri-FGG) – Project Manager. OAB is providing
the high-level software of the instrument and the off-line data reduction
pipeline.
During 2009 major efforts were devoted to the alignment and test at both
room and cryogenic temperatures, and to the implementation of a fibre
system to feed the spectrometer. Progress has been also made in testing
and optimising the pipeline on simulated echellograms.
More details about the project can be found on the web page:
http://www.bo.astro.it/giano/
4.3
Site testing
People involved at OAB: V. Zitelli, Y. Maruccia
Site characterization is an important task, not only to select the best sites
on which to host new telescopes, but also for existing telescopes. The efficiency of large telescopes is based at present on a new operation model,
which assigns a large fraction of the available time to flexible scheduling. In
this observing mode, astronomers are requested to specify not only the targets to observe, but also the environmental conditions (sky transparency,
seeing, etc.), thus increasing the need to know the atmospheric and astronomical conditions.
In this framework V. Zitelli, in collaboration with several important teams
at University of Padova, Fundacion Galileo Galilei, Instituto de Astrofisica
de Canarias and ESO, is continuing the site analysis in order to produce a
complete synoptic analysis and detail the evolution of the observing conditions during time, over short and long time scales. In the years 2008–2009
54
the programme was funded by the EU Framework Programme 7 (FP7,
WP5000), Preparing for the construction of the European Extremely Large
Telescope. In order to test different climatic conditions, important astronomical sites located in Chile, USA and the Canary Islands were analysed and compared. The results of the comparison between Cerro Paranal
(Chile) and El Roque de Los Muchacos (Canary Islands) were published
in Lombardi et al. (2009). Through the use of a satellite equipped with a
simultaneous multi-band camera, we obtained a good improvement in this
field.
In Della Valle et al. (2010) we show quite a good correlation of the emissivity of two satellite infrared bands (6.7µm water vapour and 10.7µm) with
the ground-based data collected in two analysed sites (La Palma, Canary
Islands and Mt. Graham, USA).
The main difficulties in the analysis of the first satellite data arise from
the spatial resolution of the images and from the interpretation of the measured fluxes in terms of cloud coverage, because they are affected by several
problems (partial pixel coverage by clouds, non homogeneities of the temperature distribution, seasonal albedo variation). Many of these difficulties
are overtaken by introducing a wider average matrix and a 3-Band correlation. Furthermore, the use of a more sophisticated channel correlation
analysis method allowed us to detect more subtle effects due to atmospheric
perturbations, including sudden changes in air mass which imply changes
in seeing, wind and relative humidity. The results of this study have been
described in a paper accepted for publication in MNRAS.
4.4
LINC-NIRVANA
People involved at OAB: G. Bregoli, P. Ciliegi, E. Diolaiti, G. Innocenti,
M. Lombini
LINC-NIRVANA is a near infrared imaging interferometer for the Large
Binocular Telescope (LBT), a double 8.4m diameter telescope located in
Arizona, USA. It is built by a Consortium of German and Italian institutes.
The optical beams collected by the two LBT apertures are corrected for
the effects of the atmospheric turbulence by two multi conjugate adaptive optics systems; they are co-phased in real time and combined inside a
cryogenic camera, where they interfere in the focal plane following an optical scheme known as Fizeau interferometry. LINC-NIRVANA is expected
to have unprecedented imaging performance in the near infrared, both in
55
terms of angular resolution and limiting magnitude, thanks to the interferometric mode and to the large collecting area of the two LBT apertures
combined together.
The full resolution of LINC-NIRVANA will be recovered by multiple exposures of the same object, observed at different baseline orientations of
the interferometer. The algorithms for the image combination and reconstruction play a fundamental role. OAB is involved in the definition of the
science case, of the observational strategies and of the reduction procedures.
Our work on data simulation and analysis was continued all over the year
2009.
Figure 14: Mid-High layer Wavefront Sensor of Linc-Nirvana, after the integration
and testing phase in the optical laboratory of OAB.
OAB is also involved in the design, procurement and integration of the
wavefront sensors of LINC-NIRVANA, i.e. the sub-systems devoted to the
measurement of the effects of the atmospheric turbulence. The second MidHigh layer Wavefront Sensor unit (Figure 14) was integrated in 2009 and,
at the moment of writing, has been already shipped to the Max-Planck
Institut für Astronomie.
56
This work is in collaboration with G. Cosentino, I. Foppiani, B. Marano,
L. Schreiber at the Astronomy Dept., Univ. of Bologna.
A detailed description of the project can be found on the web page:
http://www.bo.astro.it/∼ciliegi/astro/nirvana/Welcome.html
4.5
MAORY: an adaptive optics module for E-ELT
People involved at OAB: M. Bellazzini, G. Bregoli, P. Ciliegi, E. Diolaiti,
G. Innocenti, M. Lombini
MAORY (Multi-conjugate Adaptive Optics RelaY, see figure on the cover
of this chapter) is an adaptive optics module for the future 42 meter European Extremely Large Telescope (E-ELT). The atmospheric turbulence
is corrected by means of three deformable mirrors: one integrated in the
telescope and optically conjugated to the ground layer, and two post-focal
deformable mirrors conjugated to 4 km and 12.7 km in the atmosphere.
This design ensures a remarkably uniform correction across an extended
field of view of up to 2 arcminutes. The real-time measurement of the
turbulence is carried out by means of six laser guide stars, generated by excitation of the Sodium layer in the upper atmosphere. Natural guide stars
are also used to measure some basic perturbations not properly measured
by laser guide stars, as the wavefront tilt associated to the image motion.
MAORY is optimized to operate in the near infrared wavelength range 0.8–
2.4µm. With a seeing of 0.8 arcsec in the visible, the expected Strehl Ratio
averaged over a 1 arcminute field is approximately 0.5 at 2.16µm wavelength over 50% of the sky at the Galactic Pole. MAORY has two output
ports: a gravity invariant port with mechanical field derotation feeding the
high angular resolution camera MICADO and a lateral port to feed a detached instrument on the telescope Nasmyth platform, for instance a single
field spectrograph such as SIMPLE, or a multi-object spectrograph.
A two-year Phase-A study of the module was led by OAB (principal investigator: E. Diolaiti) and was carried out in collaboration with the Astronomy
Dept., Univ. of Bologna (I. Foppiani – system engineer, G. Cosentino, B.
Marano, L. Schreiber), with the INAF astronomical observatories of Padova
and Arcetri, with INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica,
Bologna, and with Office National d’Études et de Recherches Aérospatiales
(ONERA). The study was sponsored by ESO and was assigned to the consortium led by OAB through a single-source procurement process. The
study passed its final design review in December 2009; a proposal for the
57
instrument construction was presented.
The project was also funded by the European Community through the programmes FP6 (contract ELT Design Study) and FP7 (contract Preparing
for the Construction of the European Extremely Large Telescope). In this
context a prototype of a laser guide star wavefront sensor was designed and
built (Figure 15), to study the critical aspects of a crucial sub-system of
MAORY.
Figure 15: Laser Guide Star wavefront sensor prototype installed and operated
in the optical laboratory of OAB.
The European Community FP7 funds allowed to support the research
grants of M. Lombini (OAB, scientific referent: E. Diolaiti), I. Foppiani
and L. Schreiber (Astronomy Dept., Univ. of Bologna, scientific referent:
B. Marano).
Two PhD thesis were developed:
• Laura Schreiber, thesis title MCAO for Extremely Large Telescopes:
the cases of LBT and E-ELT , tutors B. Marano (Astronomy Dept.,
Univ. of Bologna) and E. Diolaiti (OAB), completed in 2009;
• Matteo Lombini, thesis title Laser Guide Star Wave Front sensing
for the European Extremely Large Telescope, tutors B. Marano (Astronomy Dept., Univ. of Bologna) and E. Diolaiti (OAB), expected
completion in 2011.
58
More details about the project can be found on the web page:
http://www.bo.astro.it/maory/
4.6
SIMPLE: a high resolution IR spectrograph for E-ELT
People involved at OAB: L. Origlia, A. Bragaglia, P. Montegriffo, E. Rossetti
SIMPLE is the Phase A study of a high resolution near IR spectrograph
for the European Extremely Large Telescope (E-ELT). The International
Consortium includes the following Institutes: INAF – Bologna, Arcetri and
Roma Observatories, Uppsala University (Sweden), Pontificia Universidad
Catolica de Chile (Chile), Thüringer Landessternwarte Tautenburg (Germany). Within the Consortium, INAF is the leading partner, also providing
the Principal Investigator (L. Origlia, INAF Bologna), the Project Manager
(E. Oliva, INAF Arcetri) and the Instrument Scientist (R. Maiolino, INAF
Roma). In 2008 we answered the Call For Proposal CFP/ESO/08/20579,
Advanced Study of a new Instrument Concept for the European Extremely
Large Telescope (E-ELT) issued by ESO, and late in the year our Consortium was selected to undertake the SIMPLE study.
SIMPLE will be fully complementary to JWST, providing the missing high
spectral resolution, and to ALMA providing the near IR high resolution
spectral counterpart. It will also be fully complementary (in terms of spectral resolution and/or spectral coverage) to the other E-ELT instruments
studied so far. The instrumental concept of SIMPLE is relatively easy
(hence its name) and follows from a detailed study of existing high resolution optical spectrographs. For the technical issues specific to cryogenic IR
instruments, we took advantage of the information available for CRIRES
and of the direct experience we recently gained with the GIANO IR spectrograph for the TNG (described in this report).
As current baseline, the spectrograph is vacuum cooled and thermostated
at cryogenic temperatures and has a fixed position at the telescope. It
achieves a resolving power R = 105 with a spatial sampling of 9 milli-arcsec
per pixel along the slit. It is assisted by adaptive optics both to concentrate
the light in the slit and to achieve spatial resolution along the slit at the
diffraction limit of the telescope. It has two observing modes: single object,
with complete 0.85–2.5 µm spectral coverage in a single exposure, or long (4
arcsec) slit with partial spectral coverage. Spectral dispersion is obtained
by a commercial echelle grating with cross-dispersing prisms. The complete
59
spectrum fits on a 3 × 4 k2 array mosaic.
The core of the cryogenic spectrometer consists of a three-mirror anastigmat
which works in double pass and acts both as collimator and camera. Cross
dispersion is performed by means of 3 prisms in double pass, which provide
a minimum inter-order distance of 60 pixels (0.5”). The detector is a mosaic
of three 4096 × 4096 Hawaii-II RG arrays with 15µm pixels.
Among the unique (i.e. feasible only with an ELT) science that will become
possible with SIMPLE, we mention the physics of exo-planet atmospheres,
early nucleosynthesis and chemical enrichment history of the inner Galaxy,
the chemical and kinematic properties of the stellar populations in extragalactic star clusters out to Virgo, the metal and dust content of the highest
redshift Lyman-α absorption systems, and the physics of exo-planet atmospheres. A near IR high resolution spectrograph is also the ideal tool in
other hot topics of modern astrophysics, as the characterization of planet
atmospheres in the solar system, the search of exo-planets with habitable
conditions, the spectro-astrometry of circumstellar disks, the study of stellar magnetic fields. Having such a spectroscopic facility at an ELT, rather
than on existing 8–10m class telescopes, allows us to pick up and/or resolve objects 3–4 mag fainter and/or at least 5 times more distant, and/or
enlarging the searching volume by at least two orders of magnitude.
More details about the project can be found on the SIMPLE wiki page:
http://simple.bo.astro.it
60
5
Loiano Observing Site
The Cassini telescope seen through the planet.
People involved at OAB:
• Scientific staff: V. Zitelli (person in charge)
• Technical staff: S. Bernabei (on trade-union leave), G. Bregoli, I.
Bruni, A. De Blasi, R. Gualandi, I. Muzi.
• Fellows and contracts: S. Galleti
Loiano, observing site of the INAF–Bologna Observatory, is located at 785m
of altitude above sea level, at a distance of 37km from Bologna. The site,
23 hectares of wood, hosts 3 buildings: the 152cm and 60cm telescopes,
and the guesthouse.
The 152 cm telescope, dedicated to G.D. Cassini, was built by REOSC
and has been operating since 1976. A general description of the Cassini
telescope is given in Table 1.
The most requested focal instrument at the telescope is at present the
BFOSC (Bologna Faint Object Spectrograph and Camera), a spectrograph/
focal reducer based on transmitting optics ranging from 330 to 1100nm,
equipped with an EEV2 1340 × 1300 CCD camera and the possibility to
choose between two sets of filters: a standard Johnson-Kron-Cousins system and a Gunn system. An Hα filter has also been made available.
BFOSC, the multipurpose instrument for spectroscopy and imaging belonging to the xFOSC family of instruments, has been the most scheduled
instrument, with about 90% of the total allocated time, well matching the
seeing and variable meteo conditions of the Loiano site. The user manual
of BFOSC is available linking the web page:
http://www.bo.astro.it/~loiano/TechPage/bfosceng/BFOSC.htm
The telescope was updated with the installing of auto-guiding systems: one
for the telescope and one for the rotation of the dome. The technical reports with the description of these systems are available at the web pages:
http://www.bo.astro.it/bap/files/rep12-2004-02-text.pdf,
http://www.bo.astro.it/bap/files/rep12-2004-03-text.pdf (in Italian).
A description of the Cassini and 60cm telescopes is available in the Loiano
web page: http://www.bo.astro.it/loiano/index.htm
The 60cm telescope was built in 1933 by Zeiss of Jena. It was originally equipped with a photographic camera at the f/3 direct focus, and
around 1960 it was modified to an f/20 Cassegrain system. At present it
63
is equipped with a 5-colour photometer. A new Marconi CCD camera (series 4710, 13µm pixel size, 1055 × 1026 pxs) is mounted at the Cassegrain
focus modified by a focal reducer to f/5.6. This telescope is now permanently used to train undergraduate students and for educational activities.
A user’s technical report can be found at the web page:
http://www.bo.astro.it/~loiano/ManualeCCD60cm/ManualeCCD60cm
.htm
The 60cm telescope, during the summer time, is also used for outreach
activities (see section Outreach and Educational activities for more details).
5.1
Operations and use of the 152 cm telescope
The 152cm telescope is regularly used for scientific observations. The statistics of useful nights for the year 2009 remained stable with respect to the
past years, with about 100 useful nights, 60 partially used night, while
about 120 nights were not used because of bad weather. The seeing had
a median value of ∼ 1.8 arcsec, with several nights at ∼ 1.1 arcsec. More
detailed data are available on the web page:
http://www.bo.astro.it/loiano/report2009/stat2.html
Time is allocated every 6 months, starting in February and August. Three
technicians in turn guarantee the night-time technical assistance.
5.2
Loiano computer station
People involved at OAB: Bruni, Di Luca, Gualandi, Lolli.
After the installation in 2002 of the 2Mbit connection between the Loiano
Observatory and Bologna, a fibre optic link was installed, connecting the
152cm Loiano telescope, the old 60cm telescope and the guesthouse. Images
produced during observation runs can now be immediately downloaded
and made available to the observers. It is also possible to pre-reduce the
observed data with a PC in a local network. IRAF packages are available
and it is possible to implement other software facilities.
5.3
Applications to the 152cm telescope
The main observing programmes of 2009 at the 152cm telescope can be
summarized as follows:
64
• optical counterparts of Gamma Ray Bursts;
• variable stars;
• detection of microlensing events;
• monitoring of variable sources (SNe, Novae, X-ray sources, etc.);
• photometry and spectroscopy of extragalactic objects;
• open clusters and globular clusters in our Galaxy and in nearby galaxies;
• scientific observations coordinated with other projects (satellites,
WET, etc.). An example can be seen on the web page of the WET
(Whole Earth Telescope) Project, where the list of used telescopes is
at the link:
http://www.physics.udel.edu/darc/wet/index.html;
• testing of prototypes and instrumentation for other telescopes (i.e.
the GASP polarimeter designed by M. Redfern, Galway University);
• practical training and workshops for students (Italian and foreign);
• outreach activities during special events.
The pressure factor (nights requested/nights available) is ∼ 2. In total, 273
nights were allocated for observations. Of these, 35 (13%) were spent on
didactic observations by several Universities. Service observing is offered
and 36% of all nights were requested in this mode. Service observations
were conducted during 68 nights in 2009 (∼25% of the scheduled time; this
is made possible by the presence of a resident astronomer).
The approved observing programmes are listed below and included several
long-term programmes.
1. Altavilla G. (INAF–OABologna), et al.: GAIA Calibration Working Group: Monitoring candidate Spectrophotometric Standard Stars
against variability.
2. Bartolini C. (Univ. of Bologna), et al.: Fast Photometry of exoplanets
(X0-5)
3. Bellazzini M. (INAF–OABologna), et al.: Ghostly streams in nearby
unresolved galaxies: a pilot project.
4. Bonfanti C. (Ist. “R. Steiner” di Milano), et al.: Esercitazioni di
fotometria e spettroscopia di oggetti celesti.
65
5. Brunt H. (Observatoire de Paris-Meudon, France), et al.: Mode identification of delta Scuti stars in NGC 6866 in the Kepler field.
6. Calchi Novati S. (Univ. of Salerno), et al.: Probing MACHOs by observation of M31 pixel lensing.
7. Clementini G. (INAF–OABologna), et al.: Stellar archaeology in Milky
Way halo: variable stars and stellar populations in the Uma I dwarf
Spheroidal galaxy (dSph).
8. De Martino D. (INAF–OACapodimonte), et al.: Unveiling the nature
of COROT selected binary candidates.
9. De Martino D. (INAF–OACapodimonte) et al.: X-ray counterparts
of hard X-ray Cataclysmic Variables.
10. Dolci M. (INAF–OATeramo), et al.: A coordinated effort towards a
well-sampled photometric and spectroscopic database of supernovae.
11. Focardi P. (Univ. of Bologna), et al.: The role of environment-activity
relationship on galaxies.
12. Galleti S. (INAF–OABologna), et al.: A survey of remote and peculiar
globular cluster in M31.
13. Gavazzi G. (Univ. of Milano Bicocca), et al.: A complete survey of
LINERS in the Virgo and Coma clusters.
14. Giovannelli F. (INAF–IASF, Roma), et al.: Spectrophotometric and
photometric observations of X-ray binaries and interactions with SNRs.
15. Greco G. (Univ. of Bologna), et al.: Target of Opportunity of Afterglows of GRBs.
16. Maiorano E. (INAF–IASF, Bologna), et al.: Peering at the redshift
of one GRB afterglow in Loiano.
17. Mancini L. (Univ. of Salerno), et al.: Accurate properties of extrasolar
planets via telescope defocussing.
18. Marano B. (Univ. of Bologna): Corso di strumentazione per astrofisica, Modulo ottico.
19. Masetti N. (INAF–IASF, Bologna), et al.: Testing the extragalactic
origin of INTEGRAL sources.
20. Norci L. (Dunsink Observatory), et al.: The runaway status of late B
stars.
21. Meurs Evert J.A. (Dunsink Observatory), et al.: Nuclear magnitudes
for active galaxies.
66
22. Poggiani R. (Univ. of Pisa), et al.: Intranight variability of gammaray loud blazars.
23. Poggiani R. (Univ. of Pisa), et al.: Post-outburst spectroscopy of novae.
24. Polcaro V.F. (INAF–IASF, Roma), et al.: Study of Very High Mass
Stars in various Evolutionary pahses.
25. Righini A. (Univ. of Firenze), et al.: Esercitazioni studenti Lab Astro
I Firenze.
26. Ripepi V. (INAF–OACapodimonte), et al.: Hα survey of the Kepler
satellite field of view.
27. Romoli M. (Univ. of Firenze), et al.: Attività didattica per i Corsi di
Laurea in Fisica e Astrofisica.
28. Rossi C. (Univ. of Roma La Sapienza), et al.: Absolute luminosities
and distances of late M and AGB stars in the galactic halo.
29. Scelsi L. (INAF–OAPalermo), et al.: Observations of candidate members of the Taurus Molecular Cloud.
30. Silvotti R. (INAF–OATorino), et al.: EXOplanet search with the Timing MEthod (EXOTIME).
31. Tozzi G.P. (INAF–OAArcetri), et al.: Observations of the opposition
effects of the asteroid 64 Angelina at very low phase angles.
32. Vittone A.A. (INAF–OACapodimonte), et al.: Study of protoplanetary symbiotic nebulae.
The Bologna Observatory provides also the support necessary for their
degrees to students in Physics and Astronomy of National and European
Universities.
• List of applications for undergradate students of both Italian and
European degrees in Astrophysics:
1. Bonfanti C. (Milano Steiner): 2 nights
2. Gavazzi G. (Milano Bicocca): 8 nights
3. Marano B. (Bologna Univ.): 12 nights
4. Norci L. (Dunsink Observatory): 5 nights
5. Righini A. (Firenze Univ.): 4 nights
6. Romoli M. (Firenze Univ.): 4 nights
67
5.4
Loiano cooperation
Loiano hosts equipment of the Solid Earth Physics group used to study
the Earth’s crust deformation and mean sea level. This research group is
interested in monitoring and measuring with high accuracy the long-term
vertical crustal motions. Starting with the analysis of the Adriatic coast
and of the Po valley, during the last eight years the group has developed
a permanent GPS network consisting of five stations (Medicina, Bologna,
Porto Corsini, Trieste and Loiano). The fibre link connection provides
continuous information from GPS to the physics group. This allows to
correlate and model the observed seasonal fluctuations with environmental
parameters.
5.5
Scientific production involving
the 152 cm Telescope
5.5.1
International refereed publications
1. Bassani, L., Landi, R., Masetti, N. et al., 2009: On the identification of the Fermi/LAT source 0FGL J2001.0+4352 with a BL Lac,
MNRAS, 397, L55
2. Bernabei, S. et al., 2009: Multisite photometry of the pulsating Herbig
Ae star V346 Ori , A&A, 501, 279
3. Calchi Novati, S. et al., 2009: Candidate Microlensing Events from
M31 Observations with the Loiano Telescope, ApJ, 695, 442
4. Galleti, S. et al., 2009: An updated survey of globular clusters in M 31.
III. A spectroscopic metallicity scale for the Revised Bologna Catalog,
A&A, 508, 1285
5. Landi, R. et al., 2009: The AGN nature of three INTEGRAL sources:
IGR J18249−3243, IGR J19443+2117, and IGR J22292+6647 , A&A,
493, 893
6. Lutz, R. et al., 2009: The planet-hosting subdwarf B star V 391 Pegasi
is a hybrid pulsator , A&A, 496, 469
7. Masetti, N. et al., 2009: Unveiling the nature of INTEGRAL objects
through optical spectroscopy. VII. Identification of 20 Galactic and
extragalactic hard X-ray sources’ , A&A, 495, 121
8. Miroshnichenko, A. S. et al., 2009: Toward Understanding the B[e]
Phenomenon. III. Properties of the Optical Counterpart of IRAS
00470+6429 , ApJ, 700, 209
68
9. Musella, I. et al., 2009: Pulsating Variable Stars in the Coma Berenices
dwarf spheroidal galaxy, 2009, ApJ, 695, 83.
10. Pastorello, A. et al, 2009: SN 2005cs in M51 II. Complete Evolution
in the Optical and the Near-Infrared MNRAS, 394, 2266
11. Parisi, P. et al., 2009: ‘Accurate classification of 17 AGNs detected
with Swift/BAT , A&A, 507, 1345
12. Poggiani R., 2009: The early spectroscopy of V2670 Oph (Nova Oph
2008), AP&SS, 323, 319
13. Poggiani, R., 2009: The spectroscopic evolution of V2362 Cyg (Nova
Cygni 2006) in the first 15 months after the outburst, New Astronomy, 14, 4
14. Poggiani, R., 2009: The spectroscopic evolution of V2467 Cyg (Nova
Cygni 2007) in the first months after the outburst, Astronomische
Nachrichten, 330, 77
15. Skopal, A., Sekeras, M., Gonzalez-Riestra, R., Viotti, R.F., 2009:
The origin of the supersoft X-ray–optical/UV flux anticorrelation in
the symbiotic binary AG Draconis, A&A, 507, 1531
16. Trundle, C. et al., 2009: Possible evidence of asymmetry in SN 2007rt,
a type IIn supernova, A&A, 504, 945
17. Shore, S. N. et al, 2009: The spectroscopic evolution of the symbiotic
star AG Draconis. I. The O VI Raman, Balmer, and helium emission
line variations during the outburst of 2006–2008 , 2009arXiv0912.1890S
18. Tamburini, F., de Martino, D., Bianchini, A., 2009: Analysis of the
white-light flickering of the intermediate polar V709 Cassiopeiae with
wavelets and Hurst analysis A&A, 502, 1
5.5.2
Published conference proceeding and circulars
19. Calchi Novati, S., Candidate microlensing events from M31 observations with the Loiano telescope, Microlensing workshop, Paris, January 19–21, 2009.
20. Collins, P.P., Shehan, B., Redfern, M., Shearer, A., GASP - Galway
Astronomical Stokes Polarimeter , Proceedings of the Conference ”Polarimetry days in Rome: Crab status, theory and prospects”, held in
Rome, 16–17 October 2008, to be published in Proceedings of Science
21. Lutz, R., Schuh, S., Silvotti, R. et al., Long-term EXOTIME photometry and follow-up spectroscopy of the sdB pulsator HS 0702+6043 ,
69
(2009) JENAM 2008 proceedings, to be published in ’Communications in Asteroseismology’, 159
22. Lutz, R., Schuh, S., Silvotti, R., Kruspe, R., Dreizler, S., Long-term
EXOTIME photometry and follow-up spectroscopy of the sdB pulsator
HS 0702+6043 Communications in Asteroseismology, Vol. 159, p. 94.
Proceedings of ”JENAM 2008 Symposium No 4: Asteroseismology
and Stellar Evolution”, held on September 8–12 2008
23. Maiorano, E., Pizzichini, G., Bartolini, C., Greco, G., Guarnieri, A.,
Mantegna, A., Piccioni, A., Nanni, D., Terra, F., Gualandi, R., GRB
090313: optical observations, 2009, GCN, 9606
24. Bonnet-Bidaud, J.M., de Martino, D., Mouchet, M., XSS J0056+4548:
a hard X-ray intermediate polar in the period gap, 2009, ATel, 1895
70
6
Computer Centre and Computer Network
People involved at OAB:
• Scientific staff: R. Merighi;
• Technical staff: R. Di Luca, M. Gatti, M. Lolli, R. Policastro.
6.1
General Description
The Bologna Astronomical Observatory, hereafter OAB, is hosted in two
buildings belonging to the University of Bologna and shares these spaces
with The Department of Astronomy of the Bologna University. The main
network infrastructures belong to the University of Bologna and are managed by CeS.I.A (Centro per lo Sviluppo e la Gestione dei Servizi Informatici di Ateneo).
The computer network is constituted by two class C subnets, with IP addresses belonging to the Bologna University domain. Network lines in
each one of the two building previously mentioned are cabled on two HP
ProCurve 4208 vl network-switches owned by CeS.I.A. These switches are
fiber-connected (gigabit) with a HP Procurve 2824 router-switch, interfaced
with a Fortigate 400 firewall. The output line from the firewall goes to the
frontier-router. Both the firewall and the frontier-router are owned and
managed by CeS.I.A.
A third partitioned class C subnet, connects the Loiano Observatory and
the few offices still remaining in the former Observatory location, in the old
Observatory Tower.
In recent years, due to the lack of space in the main buildings, the OAB
rented some external offices, hosting post-doc students and laboratory.
CeS.I.A. offered a laser bridge and micro-wave bridge to connect these
spaces to the internal network.
The computer centre hardware is formed by some Linux servers, hosting
the general services (dns, print server, IDL license manager, web server)
and intensive-computing facilities (two HP DS-20 and one HP DS-25), by a
HPC Beowulf Linux cluster for parallel computing and about 200 personal
workstations. OAB owns about the 65% of these machines.
About 40 PCs are devoted to academic activity (informatics lab and pregraduates students) and other 15 PCs belong to the administrations of the
two institutions.
71
Workstations are mainly dual boot Linux/Windows PCs. In the last two
years, old HP Alpha workstations have been progressively substituted by
Apple PowerMacs (dual-processor IBM PowerPC or quad-processor Intel
Xeon). Also several obsolete PC-Linux workstations have been replaced by
Apple iMac (Intel Core 2 Duo). Presently the number of Apple Macs is
about 50 units, servers, laptops and iMacs.
Printing facilities, managed by a Linux print server, are represented by
14 B/w laser printers, two color laser printers and one large format color
printer.
The HPC Beowulf cluster, a joint venture between OAB and the Department of Astronomy, is formed by 16 dual-processor Linux computers, connected in a local gigabit network.
6.2
Computer centre improvements
People involved at OAB: Di Luca, Gatti, Lolli, Merighi, Policastro.
Some Apple iMac, biprocessor 2.6 GHz Intel Core-Duo CPU, 500 GB SATA
disk, and 4GB RAM have been chosen to replace Unix computers. The
performances and the integration of these devices have been quite good.
These all-in-one devices were also very much appreciated from the point of
view of noise and temperature dissipation.
A new color laser print Kyocera FS-5300DN has been bought to replace
an Oki C7300N printer. Seven Lexmark T652DN laser printers have been
bought to replace old HP equipment (namely LaserJet 4050 and LaserJet
4100).
6.3
Web applications
People involved at OAB: Gatti, Lolli.
During 2009 the GIANO (http://www.bo.astro.it/giano/) web pages
were continuously updated.
Lolli installed a new version of Loiano Image Archive with web interface at
dbima.bo.astro.it.
Gatti is maintaining and improving the Administration’s web site. Useful
information has been made available, including the staff database, different
sets of forms for internal use and legislative references.
72
6.4
Routine activities
People involved at OAB: Di Luca, Gatti, Lolli, Policastro.
Besides all the activities described above, a large part of the work of the
computer centre staff has been, as usual, devoted to routine activities such
as hardware and software maintenance, failure management and user assistance.
Routine operations include:
• backup and user management on computers dedicated to data-reduction
• supply of consumables (toners, paper for printers, magnetic supports
for backup etc.)
• printer maintenance
• local network management
• administrative management of the computer centre (software and
hardware licenses, guarantees, purchases, maintenance contracts)
• updates and new installations of application software for astronomical
reduction (MIDAS, IRAF etc.)
• management of the Observatory’s WWW server
73
7
Library
A view of the library
People involved at OAB:
• Library staff: M. Marra.
During 2009 the library carried out its routine activities: mainly book loan,
book purchases, journal subscriptions, and document delivery.
The structure and setting of the new version of the cataloguing and book
managing software Sebina, released in late 2008, did not prove to be particularly suitable for OAB’s specific needs regarding book management.
During the Spring, some talks took place among technical and research
personnel of both Institutes locally involved in the library, in order to reach
75
a mutually agreed updated version of the library rules (the talks have since
been suspended).
On April 1st and 2nd, a national meeting of INAF librarians took place in
our working area.
A new software for inventoring was adopted by INAF for all of its goods,
and consequently also for INAF books.
In July, M. Marra joined Alberto Cappi as a local member of INAF’s advisory committee for CRIS, the national database for INAF personnel publications made available in an experimental version by the person in charge
of this project, F. Naldi. By the end of the year, M. Marra prepared an
article about this new project, which was published on AIDA Informazioni,
the journal of the Italian Association for Advanced Documentation.
In September–October, the monthly attendance of a course abroad by the
DA unit of personnel was mostly covered with a temporary change in the
OAB library personnel’s working hours.
By the end of October Prof. Giorgio Palumbo left the direction of the
library, as a consequence of his retirement. His constant commitment to
the library needs has been very helpful. A very good contribution also
came from the library scientific advisor for OAB, M. Bellazzini, as in the
previous years.
Several University part-time students have again been important to cover
all opening hours with a continuously-available book loan service, which is
still far and away the most requested service. The great majority of the
users visiting the library are still students from the local University.
76
8
Outreach and Educational Activities
Inside the Observatory’s digital planetarium
People involved at OAB:
• Scientific staff: S. Bardelli, R. Bedogni, A. Buzzoni, A. Cappi, F. Fusi
Pecci, S. Galleti, R. Merighi, G. Parmeggiani, F. Poppi, V. Zitelli, E.
Zucca.
• Technical staff: I. Bruni, A. De Blasi, R. Di Luca, O. Diodato, R.
Gualandi, M. Orlandi, M. Ravaglia.
The Bologna Astronomical Observatory (OA-BO) spends a large effort to
provide bridges between astronomy and the public, especially primary and
secondary level students, interested individuals, and also with those who are
unfamiliar with astronomy. The outreach activities range from hands-on
labs, to work done directly with students, public astronomical observations,
77
exhibitions, and public lectures. The 2009 was the International Year of
Astronomy (IYA) and the OA-BO have contributed to this global event
with strong effort and a lot of initiatives, all of these under the name of
Boastro2009.
In this programme, the long-term and stable partnership between the Bologna Astronomical Observatory and the Astronomy Department of the University of Bologna is important, as are the collaborations with the Institute
of Radio Astronomy, and with the amateur astronomers of Bologna (Associazione Astrofili Bolognesi) and of San Giovanni in Persiceto (Astrofili
Persicetani) outside Bologna. Particularly notable is the intense collaboration started five years ago with the Marino Golinelli Foundation, that
organizes La Scienza in Piazza, or A Town Square for Science, a format
to bring Science to the people in the places where the people are, the city
squares.
The outreach activities during 2009 were:
• Boastro2009 and the exhibition L’universo in evoluzione;
• Col Favore del Buio;
• Guida al cielo con il laser, Settimana della scienza – Brindisi;
• La Scienza in Piazza;
• the theatre show Il Sistema del mondo.
The educational activities in the same period were:
• Giampietro Puppi Prize;
• The Planetarium;
• Parco delle Stelle;
• Conferenze alla Specola.
8.1
8.1.1
Outreach Activities
Boastro2009
People involved at OAB: S. Bardelli, R. Bedogni, I. Bruni, A. De Blasi, R.
Di Luca, F. Fusi Pecci, S. Galleti, R. Gualandi, R. Merighi, M. Orlandi, G.
Parmeggiani, F. Poppi, M. Ravaglia, V. Zitelli, E. Zucca.
78
Below is a list of all events, targeted to students and also to the general
public. (www.bo.astro.it/universo/boastro/paginab.html)
• 17 January, inauguration ceremony Galileo e la scoperta di un nuovo
mondo by William Shea;
• 18 April, 23 May, 10 September, public conferences in Aula Absidale,
held by Gianni Bignami, Silvia Pellegrini, Riccardo Giacconi;
• Alla scoperta del cosmo, a teachers’ course in 8 lessons from January
to November, in collaboration with the Associazione per lInsegnamento della Fisica (AIF);
• Astro...mania during the Scienza in Piazza Maggiore, 12–22 March,
Palazzo DAccursio, Piazza dei Celestini e Via dAzeglio, in collaboration with the Marino Golinelli Foundation;
• Il Sistema del Mondo, theatre show by Archivio Zeta, at the Parco
delle Stelle and Telescopes in Loiano from April to October;
• Archeologite and Col favore del Buio in collaboration with the Provincia di Bologna;
• several Cinema shows on astronomical subjects in collaboration with
the Cineteca di Bologna and Cinema Lumière.
• the exhibition LUniverso in evoluzione. Dal Big Bang alla vita, from
the beginning of the Big Bang to the stars and galaxies, reaching the
planets and life. An exhibition, but also conferences and workshops
on the science of the Cosmos. The exhibition was divided into several
sections housed in the Library Sala Borsa. A section was dedicated
to the description of the cosmological evolution of the universe since
the Big Bang to the galaxies. A telescope of XIX sec and a satellite
to study the universe from space were exposed at this location. A
second section was dedicated to the formation of the universe, with a
3D video by CINECA. A part was dedicated to Geology and Biology,
describing the search for possible forms of life (past or future) in other
planets of the Solar System and the evolution of life on our planet.
• 15 December, closing ceremony of Boastro2009 ; Gli occhi dell’astronomia and L’Universo: a te scoprirlo, with Giulio Giorello, Vito Mancuso, Gianni Riotta, Giancarlo Setti e Flavio Fusi Pecci.
79
8.1.2
Col Favore del Buio
People involved at OAB: I. Bruni, A. De Blasi, S. Galleti, R. Gualandi, F.
Poppi, V. Zitelli.
Thirteen years ago the collaboration between the OAB and the Council for
Culture of the Province of Bologna led to the creation of the Col Favore del
Buio event. This is a programme to visit the telescopes, radio telescopes,
planetariums and astronomical museums of the Province.
The event is organized by the OAB and proposes guided tours to the Loiano
Observatory, the Radio Astronomy Observatory of Medicina, the Museum
of the Specola, the amateur observatories of San Giovanni in Persiceto and
Monte San Pietro, the Planetarium and the Meteorite Collection of San
Giovanni Persiceto, and the Educational Laboratory of the Planetarium
Didactic Classroom of the Bologna City Council. The visitors, in 2009,
were over 20000.
The event gives people the opportunity to observe through the 60cm telescope of the Loiano Observatory. These sessions are mainly for visual viewing, and an astronomer introduces celestial tourists to stars, planets and
other heavenly bodies. For the year 2009, 52 nights were scheduled and
over 1500 people observed and speculated about the sky.
8.1.3
Guida al cielo con il laser a Brindisi
People involved at OAB: A. de Blasi, R. Gualandi, F. Fusi Pecci.
On 18 April, observations of the night sky with the laser were held from the
centre of the town of Brindisi, during the Settimana della scienza event.
The event was attended by about 500 people and was led by F. Fusi Pecci.
8.1.4
La Scienza in Piazza
People involved at OAB: S. Bardelli, R. Bedogni, I. Bruni, A. De Blasi, R.
Di Luca, F. Fusi Pecci, S. Galleti, R. Gualandi, F. Poppi, M. Ravaglia, V.
Zitelli, E. Zucca.
During 2009 OAB has continued its collaboration with the Marino Golinelli Foundation, that organizes La Scienza in Piazza, A Town Square
for Science. This is an activity addressed to schools, in order to promote a
responsible approach amongst the young generations, with a format whose
80
goal is to carry Science through cities, towns, and villages, transforming
them in open air Science Centres. La Scienza in Piazza wishes to promote a general critical awareness of scientific developments, and a positive
perception of science.
The planetarium, astronomical exhibits such as Potenze di 10 (an exhibition of images from the infinitely small to the infinitely large, from Bologna
to the borders of the universe), hands-on activities, the exhibition titled
Universo a tutto tondo (spherical models of planets and stars made for the
occasion by artisans in Bologna; an intuitive way to deal with the diverse
dimensions of celestial bodies), and public lectures were the main activities
of the event.
Several thousands of visitors actively participated in the activities proposed.
8.1.5
The theatre show Il Sistema del mondo
People involved at OAB: I. Bruni, A. De Blasi, F. Fusi Pecci, S. Galleti, R.
Gualandi, F. Poppi, V. Zitelli.
The astronomical station of Loiano was the setting for a play created by
Archivio Zeta entitled Il Sistema del mondo.The show highlights the transition to the heliocentric view of the world, with the verification through
the telescope by Galileo. Twenty shows took place, each with about 50/70
spectators.
8.2
8.2.1
Educational Activities
Giampietro Puppi Prize
People involved at OAB: R. Di Luca, F. Fusi Pecci, F. Poppi.
In 2007, on the occasion of the 50th anniversary of the launch of the first
satellite, the Marino Golinelli Foundation issued a call for candidates to
the Giampietro Puppi Prize for the best annual PhD Thesis on a topic in
Physics or AstroPhysics. Two years later, on 15 December, the prize-giving
ceremony was held in the Aula Absidale of St. Lucia during the closing of
Boastro2009 . The winner of the cash prize of 3000 euros was Dr. Enrico
Bozzo with a thesis on “Theory and Observations of Neutron Star X-ray
Binaries: from wind to disk accretors”. There will be also a third edition
of the Prize in 2010.
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8.2.2
The Planetarium
People involved at OAB: A. De Blasi, R. Di Luca, F. Fusi Pecci, F. Poppi.
Thanks to a financial grant from MIUR, OAB bought a Digital Planetarium
with inflatable dome, where 25 students can attend a show on the sky, and
also a voyage across the planets and stars and galaxies, thanks to new digital
technology. The Planetarium was brought to schools on several occasions,
and every time all of the shows were full.
8.2.3
Parco delle Stelle
People involved at OAB: I. Bruni, A. De Blasi, S. Galleti, R. Gualandi, V.
Zitelli.
The Parco delle Stelle is an educational park developed by the OAB for
students and the general public. It was built with a grant from the MIUR
in the park surrounding the telescopes at Loiano. Exhibits include:
• Solar system model. In order to understand the dimensions of our
planetary system and the distances to the various planets, the OAB,
in collaboration with the AD, has built a scale model of the Solar
System. It starts from the 152cm telescope building and follows a
path in the forest, reaching the dome that hosts the 60cm telescope.
One metre along this path corresponds to 15 million kilometres. To
give a better idea of the dimensions of the planets and of the Sun,
there is a second unit of measure with one centimetre corresponding
to 7000 kilometres. The model is very useful to give people a better
understanding of the locations and sizes of objects in the Solar system.
• Solar telescope. A Coronado solar telescope allows people to see the
Sun in Hα light and understand its physical characteristics.
• Sundial. A modern sundial has been built to show how the Sun moves
in the sky.
• Cosmic Calendar. In The Dragons of Eden, Carl Sagan proposed
to fit the history of the universe, all 13 billion years of it, into just
one year, with the Big Bang occurring in the first few seconds of
New Year’s Day, and all our known history occurring in the final
seconds before midnight on 31 December. Using this scale of time,
82
each month would equal a little over a billion years. In the Cosmic
Calendar exhibit we have used Sagan’s suggestion and created a path
with a panel for each month of the year along the path that leads
to the 60cm dome. This activity helps students to understand how
human activities fit into the grand scale of cosmic time.
The Parco delle Stelle is always open and, upon reservation, it is possible
to arrange guided tours for schools.
The 60cm telescope can be visited throughout the Col Favore del Buio, and
the 1.52 m telescope (G.D. Cassini) is open to the general public only on
the first Saturday of each month and to schools at any time of the year,
upon reservation.
8.2.4
Conferenze alla Specola
People involved at OAB: S. Bardelli, R. Bedogni, A. Buzzoni, A. Cappi, R.
Di Luca, O. Diodato, M. Orlandi, F. Fusi Pecci, F. Poppi, E. Zucca.
On the first Thursday of every month, at the Specola, the old Observatory
of Bologna in the town centre, a lecture is held on an astronomical subject.
The audience is mainly formed by high-school students. On average 80/90
people attend each lecture. The texts of the lectures are available on the
web page of the Observatory.
8.3
Educational and Public Outreach
Bardelli held public lectures at the cinema Lumière and at the Sala Borsa
in Bologna; also at the public library of Riccione and for the Settimana
Astronomica event in Madonna di Campiglio.
Cappi held public lectures at I.T.C.S. Erasmo, Bollate (MI), public lectures
about cosmology for the Scuola di Formazione Permanente del CNRS, Porquerolles, 20–26 September 2009.
Orlandi held public lectures for La scienza in Piazza in Bologna, at the
public library in Riccione, and at Radio Città Fujiko in Bologna.
Zucca held public lectures for the Astroblues event in Bologna, for the
Settimana astronomica event in Madonna di Campiglio, and for a high
school in Ovada.
83
Cappi, D’Ercole, Bedogni, De Blasi, Lolli, Orlandi, and Poppi reviewed
books for Giornale di Astronomia during 2009.
8.3.1
e-articles and web pages
AA.VV., Eventi & Divulgazione all’Osservatorio,
http://www.bo.astro.it/universo/outreach/
84
9
List of Publications
YEAR 2009
REFEREED PAPERS
1. Akylas, A.; Georgantopoulos, I. XMM-Newton observations of Seyfert galaxies
from the Palomar spectroscopic survey: the X-ray absorption distribution. Astronomy and Astrophysics, Volume 500, Issue 3, 2009, pp.999–1012 (2009)
2. Altavilla, G.; Ruiz-Lapuente, P.; Balastegui, A.; Méndez, J.; Irwin, M.; EspañaBonet, C.; Ellis, R. S.; Folatelli, G.; Goobar, A.; Hillebrandt, W.; McMahon, R.
M.; Nobili, S.; Stanishev, V.; Walton, N. A. Type Ia SNe Along Redshift: The
R(Si II) Ratio and the Expansion Velocities in Intermediate-z Supernovae. The
Astrophysical Journal, Volume 695, Issue 1, pp. 135–148 (2009)
3. Ameglio, S.; Borgani, S.; Pierpaoli, E.; Dolag, K.; Ettori, S.; Morandi, A.
Reconstructing mass profiles of simulated galaxy clusters by combining SunyaevZeldovich and X-ray images. Monthly Notices of the Royal Astronomical Society,
Volume 394, Issue 1, pp. 479–490 (2009)
4. Annibali, F.; Tosi, M.; Monelli, M.; Sirianni, M.; Montegriffo, P.; Aloisi, A.;
Greggio, L. Young Stellar Populations and Star Clusters in NGC 1705. The Astronomical Journal, Volume 138, Issue 1, pp. 169–183 (2009)
5. Armus, L.; Mazzarella, J. M.; Evans, A. S.; Surace, J. A.; Sanders, D. B.; Iwasawa, K.; Frayer, D. T.; Howell, J. H.; Chan, B.; Petric, A.; Vavilkin, T.; Kim, D.
C.; Haan, S.; Inami, H.; Murphy, E. J.; Appleton, P. N.; Barnes, J. E.; Bothun, G.;
Bridge, C. R.; Charmandaris, V.; Jensen, J. B.; Kewley, L. J.; Lord, S.; Madore,
B. F.; Marshall, J. A.; Melbourne, J. E.; Rich, J.; Satyapal, S.; Schulz, B.; Spoon,
H. W. W.; Sturm, E.; U, V.; Veilleux, S.; Xu, K. GOALS: The Great Observatories All-Sky LIRG Survey. Publications of the Astronomical Society of the Pacific,
Volume 121, issue 880, pp.559–576 (2009)
6. Arnaud, Monique; Barcons, Xavier; Barret, Didier; Bautz, Marshall; Bellazzini, Ronaldo; Bleeker, Johan; Böhringer, Hans; Boller, Thomas; Brandt, William
Nielsen; Cappi, Massimo; Carrera, Francisco; Comastri, Andrea; Costa, Enrico;
Courvoisier, Thierry; de Korte, Piet; Dwelly, Tom; Fabian, Andrew; Flanagan,
Kathryn; Gilli, Roberto; Griffiths, Richard; Hasinger, Günther; Kaastra, Jelle;
Kahn, Steve; Kelley, Richard; Kunieda, Hideyo; Makishima, Kazuo; Matt, Giorgio; Mendez, Mariano; Mitsuda, Kazuhisa; Nandra, Kirpal; Ohashi, Takaya; Page,
Mathew; Palumbo, Giorgio; Pavlinsky, Mikhail; Sciortino, Salvatore; Smith, Alan;
Strüder, Lothar; Takahashi, Tadayuki; Türler, Marc; Turner, Martin; Ueda, Yoshihiro; Vignali, Cristian; Vink, Jacco; Warwick, Robert; Watson, Mike; Willingale,
Richard; Zhang, Shuang Nan XEUS: the physics of the hot evolving universe.
Experimental Astronomy, Volume 23, Issue 1, pp.139–168 (2009)
7. Baldi, A.; Forman, W.; Jones, C.; Kraft, R.; Nulsen, P.; Churazov, E.; David,
L.; Giacintucci, S. The Unusual X-Ray Morphology of NGC 4636 Revealed by
Deep Chandra Observations: Cavities and Shocks Created by Past Active Galactic
Nucleus Outbursts. The Astrophysical Journal, Volume 707, Issue 2, pp. 1034–
1043 (2009)
8. Baldi, A.; Forman, W.; Jones, C.; Nulsen, P.; David, L.; Kraft, R.; Simionescu,
A. Chandra Observations of the Galaxy Group AWM 5: Cool Core Reheating and
Thermal Conduction Suppression. The Astrophysical Journal, Volume 694, Issue
1, pp. 479–491 (2009)
85
9. Bardelli, S.; Zucca, E.; Bolzonella, M.; Ciliegi, P.; Gregorini, L.; Zamorani, G.; Bondi, M.; Zanichelli, A.; Tresse, L.; Vergani, D.; Gavignaud, I.; Bongiorno, A.; Bottini, D.; Garilli, B.; Le Brun, V.; Le Fèvre, O.; Maccagni, D.;
Scaramella, R.; Scodeggio, M.; Vettolani, G.; Adami, C.; Arnouts, S.; Cappi,
A.; Charlot, S.; Contini, T.; Foucaud, S.; Franzetti, P.; Guzzo, L.; Ilbert, O.;
Iovino, A.; Lamareille, F.; McCracken, H. J.; Marano, B.; Marinoni, C.; Mazure,
A.; Meneux, B.; Merighi, R.; Paltani, S.; Pellò, R.; Pollo, A.; Pozzetti, L.;
Radovich, M.; Abbas, U.; Brinchmann, J.; Cucciati, O.; de La Torre, S.; de Ravel,
L.; Memeo, P.; Perez-Montero, E.; Mellier, Y.; Merluzzi, P.; Temporin, S.; de
Ruiter, H. R.; Parma, P. The VVDS-VLA deep field. IV. Radio-optical properties.
Astronomy and Astrophysics, Volume 495, Issue 2, 2009, pp.431–446 (2009)
10. Barmby, P.; Perina, S.; Bellazzini, M.; Cohen, J. G.; Hodge, P. W.; Huchra, J.
P.; Kissler-Patig, M.; Puzia, T. H.; Strader, J. A Hubble Space Telescope/WFPC2
Survey of Bright Young Clusters in M31. III. Structural Parameters. The Astronomical Journal, Volume 138, Issue 6, pp. 1667–1680 (2009)
11. Benedetti, C.; Londrillo, P.; Petrillo, V.; Serafini, L.; Sgattoni, A.; Tomassini, P.;
Turchetti, G. PIC simulations of the production of high-quality electron beams via
laser-plasma interaction. Nuclear Instruments and Methods in Physics Research
Section A, Volume 608, Issue 1, p. S94–S98 (2009)
12. Benedetti, C.; Londrillo, P.; Liseykina, T. V.; Macchi, A.; Sgattoni, A.; Turchetti,
G. Ion acceleration by petawatt class laser pulses and pellet compression in a fast
ignition scenario. Nuclear Instruments and Methods in Physics Research Section
A, Volume 606, Issue 1-2, p. 89–93 (2009)
13. Bernabei, S.; Ripepi, V.; Ruoppo, A.; Marconi, M.; Monteiro, M. J. P. F. G.;
Rodriguez, E.; Oswalt, T. D.; Leccia, S.; Palla, F.; Catanzaro, G.; Amado, P.
J.; Lopez-Gonzalez, M. J.; Aceituno, F. J. Multi-site photometry of the pulsating
Herbig Ae star V346 Ori. Astronomy and Astrophysics, Volume 501, Issue 1,
2009, pp.279–289 (2009)
14. Bettarini, L.; Landi, S.; Velli, M.; Londrillo, P. Magnetic and Velocity Shear
Driven Instabilities in the Heliospheric Plasma. Earth, Moon, and Planets, Volume 104, Issue 1-4, pp. 135–137 (2009)
15. Bettarini, Lapo; Landi, Simone; Velli, Marco; Londrillo, Pasquale Three-dimensional evolution of magnetic and velocity shear driven instabilities in a compressible magnetized jet. Physics of Plasmas, Volume 16, Issue 6, pp. 062302–062302-12
(2009)
16. Brusa, M.; Comastri, A.; Gilli, R.; Hasinger, G.; Iwasawa, K.; Mainieri,
V.; Mignoli, M.; Salvato, M.; Zamorani, G.; Bongiorno, A.; Cappelluti, N.;
Civano, F.; Fiore, F.; Merloni, A.; Silverman, J.; Trump, J.; Vignali, C.; Capak, P.;
Elvis, M.; Ilbert, O.; Impey, C.; Lilly, S. High-Redshift Quasars in the COSMOS
Survey: The Space Density of z > 3 X-Ray Selected QSOs. The Astrophysical
Journal, Volume 693, Issue 1, pp. 8–22 (2009)
17. Brusa, M.; Fiore, F.; Santini, P.; Grazian, A.; Comastri, A.; Zamorani, G.;
Hasinger, G.; Merloni, A.; Civano, F.; Fontana, A.; Mainieri, V. Black hole growth
and starburst activity at z = 0.6–4 in the Chandra Deep Field South. Host galaxies
properties of obscured AGN. Astronomy and Astrophysics, Volume 507, Issue 3,
2009, pp.1277–1289 (2009)
18. Buzzoni, A.; Bertone, E.; Chavez, M. Snapshot Metallicity Estimate of Resolved
Stellar Systems Through Lick Fe5270 Diagnostic. The Astrophysical Journal Letters, Volume 703, Issue 2, pp. L127-L131 (2009)
86
19. Campisi, M. A.; Vignali, C.; Brusa, M.; Daddi, E.; Comastri, A.; Pozzetti,
L.; Alexander, D. M.; Renzini, A.; Arimoto, N.; Kong, X. On the nature of red
galaxies: the Chandra perspective. Astronomy and Astrophysics, Volume 501,
Issue 2, 2009, pp.485–494 (2009)
20. Cappellari, Michele; di Serego Alighieri, S.; Cimatti, A.; Daddi, E.; Renzini, A.;
Kurk, J. D.; Cassata, P.; Dickinson, M.; Franceschini, A.; Mignoli, M.; Pozzetti, L.; Rodighiero, G.; Rosati, P.; Zamorani, G. Dynamical Masses of EarlyType Galaxies at z ∼ 2: Are they Truly Superdense?. The Astrophysical Journal
Letters, Volume 704, Issue 1, pp. L34–L39 (2009)
21. Cappelluti, N.; Brusa, M.; Hasinger, G.; Comastri, A.; Zamorani, G.; Finoguenov, A.; Gilli, R.; Puccetti, S.; Miyaji, T.; Salvato, M.; Vignali, C.; Aldcroft,
T.; Böhringer, H.; Brunner, H.; Civano, F.; Elvis, M.; Fiore, F.; Fruscione, A.;
Griffiths, R. E.; Guzzo, L.; Iovino, A.; Koekemoer, A. M.; Mainieri, V.; Scoville, N.
Z.; Shopbell, P.; Silverman, J.; Urry, C. M. The XMM-Newton wide-field survey
in the COSMOS field. The point-like X-ray source catalogue. Astronomy and
Astrophysics, Volume 497, Issue 2, 2009, pp.635–648 (2009)
22. Caputi, K. I.; Kovac, K.; Bolzonella, M.; Lilly, S. J.; Zamorani, G.; Aussel,
H.; Sanders, D.; Bardelli, S.; Bongiorno, A.; Contini, T.; Coppa, G.; Cucciati,
O.; de la Torre, S.; de Ravel, L.; Franzetti, P.; Frayer, D.; Garilli, B.; Iovino,
A.; Kampczyk, P.; Kneib, J.-P.; Knobel, C.; Lamareille, F.; LeBorgne, J. F.;
LeBrun, V.; LeFèvre, O.; LeFloc’h, E.; Leauthaud, A.; Maier, C.; Mainieri, V.;
Mignoli, M.; Pellò, R.; Peng, Y.; Pérez-Montero, E.; Ricciardelli, E.; Salvato,
M.; Scodeggio, M.; Scoville, N.; Silverman, J.; Surace, J.; Tanaka, M.; Tasca, L.;
Tresse, L.; Vergani, D.; Zucca, E.; Abbas, U.; Bottini, D.; Capak, P.; Cappi,
A.; Carollo, C. M.; Cassata, P.; Cimatti, A.; Fumana, M.; Ilbert, O.; Kartaltepe,
J.; Maccagni, D.; Marinoni, C.; McCracken, H.; Memeo, P.; Meneux, B.; Oesch,
P.; Porciani, C.; Pozzetti, L.; Renzini, A.; Scaramella, R.; Scarlata, C. The
Close Environment of 24 µm Galaxies at 0.6 < z < 1.0 in the Cosmos Field. The
Astrophysical Journal, Volume 691, Issue 1, pp. 91–97 (2009)
23. Caputi, K. I.; Lilly, S. J.; Aussel, H.; Le Floc’h, E.; Sanders, D.; Maier, C.; Frayer,
D.; Carollo, C. M.; Contini, T.; Kneib, J.-P.; Le Fèvre, O.; Mainieri, V.; Renzini,
A.; Scodeggio, M.; Scoville, N.; Zamorani, G.; Bardelli, S.; Bolzonella, M.;
Bongiorno, A.; Coppa, G.; Cucciati, O.; de la Torre, S.; de Ravel, L.; Franzetti,
P.; Garilli, B.; Ilbert, O.; Iovino, A.; Kampczyk, P.; Kartaltepe, J.; Knobel, C.;
Kovač, K.; Lamareille, F.; Le Borgne, J.-F.; Le Brun, V.; Mignoli, M.; Peng, Y.;
Pérez-Montero, E.; Ricciardelli, E.; Salvato, M.; Silverman, J.; Surace, J.; Tanaka,
M.; Tasca, L.; Tresse, L.; Vergani, D.; Zucca, E.; Abbas, U.; Bottini, D.; Capak,
P.; Cappi, A.; Cassata, P.; Cimatti, A.; Elvis, M.; Hasinger, G.; Koekemoer,
A. M.; Leauthaud, A.; Maccagni, D.; Marinoni, C.; McCracken, H.; Memeo, P.;
Meneux, B.; Oesch, P.; Pellò, R.; Porciani, C.; Pozzetti, L.; Scaramella, R.;
Scarlata, C.; Schiminovich, D.; Taniguchi, Y.; Zamojski, M. The Optical Spectra
of Spitzer 24 µm Galaxies in the Cosmic Evolution Survey Field. II. Faint Infrared
Sources in the zCOSMOS-Bright 10k Catalog. The Astrophysical Journal, Volume
707, Issue 2, pp. 1387–1403 (2009)
24. Carretta, E.; Bragaglia, A.; Gratton, R.; Lucatello, S. Na-O anticorrelation
and HB. VIII. Proton-capture elements and metallicities in 17 globular clusters
from UVES spectra. Astronomy and Astrophysics, Volume 505, Issue 1, 2009,
pp.139–155 (2009)
25. Carretta, E.; Bragaglia, A.; Gratton, R. G.; Lucatello, S.; Catanzaro, G.;
Leone, F.; Bellazzini, M.; Claudi, R.; D’Orazi, V.; Momany, Y.; Ortolani, S.;
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26.
27.
28.
29.
30.
31.
32.
Pancino, E.; Piotto, G.; Recio-Blanco, A.; Sabbi, E. Na-O anticorrelation and
HB. VII. The chemical composition of first and second-generation stars in 15
globular clusters from GIRAFFE spectra. Astronomy and Astrophysics, Volume
505, Issue 1, 2009, pp.117–138 (2009)
Carretta, E.; Bragaglia, A.; Gratton, R.; D’Orazi, V.; Lucatello, S. Intrinsic
iron spread and a new metallicity scale for globular clusters. Astronomy and
Astrophysics, Volume 508, Issue 2, 2009, pp.695–706 (2009)
Cignoni, M.; Sabbi, E.; Nota, A.; Tosi, M.; Degl’Innocenti, S.; Moroni, P. G.
Prada; Angeretti, L.; Carlson, Lynn Redding; Gallagher, J.; Meixner, M.; Sirianni,
M.; Smith, L. J. Star Formation History in the Small Magellanic Cloud: The Case
of NGC 602. The Astronomical Journal, Volume 137, Issue 3, pp. 3668–3684
(2009)
Cimatti, A.; Robberto, M.; Baugh, C.; Beckwith, S. V. W.; Content, R.; Daddi, E.;
De Lucia, G.; Garilli, B.; Guzzo, L.; Kauffmann, G.; Lehnert, M.; Maccagni, D.;
Martnez-Sansigre, A.; Pasian, F.; Reid, I. N.; Rosati, P.; Salvaterra, R.; Stiavelli,
M.; Wang, Y.; Osorio, M. Zapatero; Balcells, M.; Bersanelli, M.; Bertoldi, F.;
Blaizot, J.; Bottini, D.; Bower, R.; Bulgarelli, A.; Burgasser, A.; Burigana, C.;
Butler, R. C.; Casertano, S.; Ciardi, B.; Cirasuolo, M.; Clampin, M.; Cole, S.;
Comastri, A.; Cristiani, S.; Cuby, J.-G.; Cuttaia, F.; de Rosa, A.; Sanchez, A.
Diaz; di Capua, M.; Dunlop, J.; Fan, X.; Ferrara, A.; Finelli, F.; Franceschini, A.;
Franx, M.; Franzetti, P.; Frenk, C.; Gardner, Jonathan P.; Gianotti, F.; Grange,
R.; Gruppioni, C.; Gruppuso, A.; Hammer, F.; Hillenbrand, L.; Jacobsen, A.;
Jarvis, M.; Kennicutt, R.; Kimble, R.; Kriek, M.; Kurk, J.; Kneib, J.-P.; Le
Fevre, O.; Macchetto, D.; MacKenty, J.; Madau, P.; Magliocchetti, M.; Maino,
D.; Mandolesi, N.; Masetti, N.; McLure, R.; Mennella, A.; Meyer, M.; Mignoli,
M.; Mobasher, B.; Molinari, E.; Morgante, G.; Morris, S.; Nicastro, L.; Oliva,
E.; Padovani, P.; Palazzi, E.; Paresce, F.; Garrido, A. Perez; Pian, E.; Popa,
L.; Postman, M.; Pozzetti, L.; Rayner, J.; Rebolo, R.; Renzini, A.; Rttgering,
H.; Schinnerer, E.; Scodeggio, M.; Saisse, M.; Shanks, T.; Shapley, A.; Sharples,
R.; Shea, H.; Silk, J.; Smail, I.; Span, P.; Steinacker, J.; Stringhetti, L.; Szalay,
A.; Tresse, L.; Trifoglio, M.; Urry, M.; Valenziano, L.; Villa, F.; Perez, I. Villo;
Walter, F.; Ward, M.; White, R.; White, S.; Wright, E.; Wyse, R.; Zamorani,
G.; Zacchei, A.; Zeilinger, W. W.; Zerbi, F. SPACE: the spectroscopic all-sky
cosmic explorer. Experimental Astronomy, Volume 23, Issue 1, pp.39–66 (2009)
Clementini, Gisella; Contreras, Rodrigo; Federici, Luciana; Cacciari, Carla;
Merighi, Roberto; Smith, Horace A.; Catelan, Márcio; Fusi Pecci, Flavio;
Marconi, Marcella; Kinemuchi, Karen; Pritzl, Barton J. The Variable Star Population of the Globular Cluster B514 in the Andromeda Galaxy. The Astrophysical
Journal Letters, Volume 704, Issue 2, pp. L103–L107 (2009)
Correnti, M.; Bellazzini, M.; Ferraro, F. R. Red Clump stars in the Boötes
III stellar system. Monthly Notices of the Royal Astronomical Society: Letters,
Volume 397, Issue 1, pp. L26–L30 (2009)
Coupon, J.; Ilbert, O.; Kilbinger, M.; McCracken, H. J.; Mellier, Y.; Arnouts,
S.; Bertin, E.; Hudelot, P.; Schultheis, M.; Le Fèvre, O.; Le Brun, V.; Guzzo, L.;
Bardelli, S.; Zucca, E.; Bolzonella, M.; Garilli, B.; Zamorani, G.; Zanichelli,
A.; Tresse, L.; Aussel, H. Photometric redshifts for the CFHTLS T0004 deep and
wide fields. Astronomy and Astrophysics, Volume 500, Issue 3, 2009, pp.981–998
(2009)
Davies, Ben; Origlia, Livia; Kudritzki, Rolf-Peter; Figer, Don F.; Rich, R.
Michael; Najarro, Francisco; Negueruela, Ignacio; Clark, J. Simon Chemical Abun-
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36.
37.
38.
39.
40.
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dance Patterns in the Inner Galaxy: The Scutum Red Supergiant Clusters. The
Astrophysical Journal, Volume 696, Issue 2, pp. 2014–2025 (2009)
Davies, Ben; Origlia, Livia; Kudritzki, Rolf-Peter; Figer, Don F.; Rich, R.
Michael; Najarro, Francisco The Chemical Abundances in the Galactic Center
from the Atmospheres of Red Supergiants. The Astrophysical Journal, Volume
694, Issue 1, pp. 46–55 (2009)
de Marco, B.; Iwasawa, K.; Cappi, M.; Dadina, M.; Tombesi, F.; Ponti, G.;
Celotti, A.; Miniutti, G. Probing variability patterns of the Fe K line complex in
bright nearby AGNs. Astronomy and Astrophysics, Volume 507, Issue 1, 2009,
pp.159–169 (2009)
de Ravel, L.; Le Fèvre, O.; Tresse, L.; Bottini, D.; Garilli, B.; Le Brun, V.;
Maccagni, D.; Scaramella, R.; Scodeggio, M.; Vettolani, G.; Zanichelli, A.; Adami,
C.; Arnouts, S.; Bardelli, S.; Bolzonella, M.; Cappi, A.; Charlot, S.; Ciliegi,
P.; Contini, T.; Foucaud, S.; Franzetti, P.; Gavignaud, I.; Guzzo, L.; Ilbert, O.;
Iovino, A.; Lamareille, F.; McCracken, H. J.; Marano, B.; Marinoni, C.; Mazure,
A.; Meneux, B.; Merighi, R.; Paltani, S.; Pellò, R.; Pollo, A.; Pozzetti, L.;
Radovich, M.; Vergani, D.; Zamorani, G.; Zucca, E.; Bondi, M.; Bongiorno,
A.; Brinchmann, J.; Cucciati, O.; de La Torre, S.; Gregorini, L.; Memeo, P.;
Perez-Montero, E.; Mellier, Y.; Merluzzi, P.; Temporin, S. The VIMOS VLT Deep
Survey. Evolution of the major merger rate since z ∼ 1 from spectroscopically
confirmed galaxy pairs. Astronomy and Astrophysics, Volume 498, Issue 2, 2009,
pp.379–397 (2009)
Del Zanna, L.; Landi, S.; Zanotti, O.; Bucciantini, N.; Londrillo, P. The ECHO
code for astrophysical plasmas: Special and General Relativistic MHD. Il Nuovo
Cimento C, vol. 032, Issue 02, p.109–113 (2009)
Donnarumma, A.; Ettori, S.; Meneghetti, M.; Moscardini, L. X-ray and strong
lensing mass estimate of MS2137.3−2353. (2009)
Elvis, Martin; Civano, Francesca; Vignali, Cristian; Puccetti, Simonetta; Fiore,
Fabrizio; Cappelluti, Nico; Aldcroft, T. L.; Fruscione, Antonella; Zamorani,
G.; Comastri, Andrea; Brusa, Marcella; Gilli, Roberto; Miyaji, Takamitsu;
Damiani, Francesco; Koekemoer, Anton M.; Finoguenov, Alexis; Brunner, Hermann; Urry, C. M.; Silverman, John; Mainieri, Vincenzo; Hasinger, Guenther;
Griffiths, Richard; Carollo, Marcella; Hao, Heng; Guzzo, Luigi; Blain, Andrew;
Calzetti, Daniela; Carilli, C.; Capak, Peter; Ettori, Stefano; Fabbiano, Giuseppina; Impey, Chris; Lilly, Simon; Mobasher, Bahram; Rich, Michael; Salvato,
Mara; Sanders, D. B.; Schinnerer, Eva; Scoville, N.; Shopbell, Patrick; Taylor,
James E.; Taniguchi, Yoshiaki; Volonteri, Marta The Chandra COSMOS Survey.
I. Overview and Point Source Catalog. The Astrophysical Journal Supplement,
Volume 184, Issue 1, pp. 158–171 (2009) (2009)
Epinat, B.; Contini, T.; Le Fèvre, O.; Vergani, D.; Garilli, B.; Amram, P.; Queyrel,
J.; Tasca, L.; Tresse, L. Integral field spectroscopy with SINFONI of VVDS galaxies. I. Galaxy dynamics and mass assembly at 1.2 < z < 1.6. Astronomy and
Astrophysics, Volume 504, Issue 3, 2009, pp.789–805 (2009)
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The Astrophysical Journal, Volume 695, Issue 1, pp. 171–182 (2009)
Smolcic, V.; Zamorani, G.; Schinnerer, E.; Bardelli, S.; Bondi, M.; Brzan, L.;
Carilli, C. L.; Ciliegi, P.; Elvis, M.; Impey, C. D.; Koekemoer, A. M.; Merloni,
A.; Paglione, T.; Salvato, M.; Scodeggio, M.; Scoville, N.; Trump, J. R. Cosmic
Evolution of Radio Selected Active Galactic Nuclei in the Cosmos Field. The
Astrophysical Journal, Volume 696, Issue 1, pp. 24–39 (2009)
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L.; Ciliegi, P.; Mobasher, B.; Paglione, T.; Scodeggio, M.; Scoville, N. The DustUnbiased Cosmic Star-Formation History from the 20 CM Vla-Cosmos Survey.
The Astrophysical Journal, Volume 690, Issue 1, pp. 610–618 (2009)
Sollima, A.; Bellazzini, M.; Smart, R. L.; Correnti, M.; Pancino, E.; Ferraro,
F. R.; Romano, D. The non-peculiar velocity dispersion profile of the stellar system
Centauri. Monthly Notices of the Royal Astronomical Society, Volume 396, Issue
4, pp. 2183–2193 (2009)
Stanghellini, Letizia; Lee, Ting-Hui; Shaw, Richard A.; Balick, Bruce; Villaver,
Eva Carbon Abundance in Small Magellanic Cloud Planetary Nebulae Through
Advanced Camera for Surveys Prism Spectroscopy: Constraining Stellar Evolution
at Low Metallicity. The Astrophysical Journal, Volume 702, Issue 1, pp. 733–744
(2009)
Tasca, L. A. M.; Kneib, J.-P.; Iovino, A.; Le Fèvre, O.; Kovač;, K.; Bolzonella,
M.; Lilly, S. J.; Abraham, R. G.; Cassata, P.; Cucciati, O.; Guzzo, L.; Tresse,
L.; Zamorani, G.; Capak, P.; Garilli, B.; Scodeggio, M.; Sheth, K.; Zucca, E.;
Carollo, C. M.; Contini, T.; Mainieri, V.; Renzini, A.; Bardelli, S.; Bongiorno,
A.; Caputi, K.; Coppa, G.; de La Torre, S.; de Ravel, L.; Franzetti, P.; Kampczyk,
P.; Knobel, C.; Koekemoer, A. M.; Lamareille, F.; Le Borgne, J.-F.; Le Brun, V.;
Maier, C.; Mignoli, M.; Pello, R.; Peng, Y.; Perez Montero, E.; Ricciardelli, E.;
Silverman, J. D.; Vergani, D.; Tanaka, M.; Abbas, U.; Bottini, D.; Cappi, A.;
Cimatti, A.; Ilbert, O.; Leauthaud, A.; Maccagni, D.; Marinoni, C.; McCracken,
H. J.; Memeo, P.; Meneux, B.; Oesch, P.; Porciani, C.; Pozzetti, L.; Scaramella,
R.; Scarlata, C. The zCOSMOS redshift survey: the role of environment and stellar
mass in shaping the rise of the morphology-density relation from z ∼ 1. Astronomy
and Astrophysics, Volume 503, Issue 2, 2009, pp.379–398 (2009)
Tolstoy, Eline; Hill, Vanessa; Tosi, Monica Star-Formation Histories, Abundances, and Kinematics of Dwarf Galaxies in the Local Group. Annual Review of
Astronomy & Astrophysics, vol. 47, Issue 1, pp.371–425 (2009)
Tosi, M. Chemical composition and evolution of irregular and blue compact galaxies. The dawn of a thirty year journey. Commentary on: Lequeux J., Peimbert
M., Rayo J. F., et al., 1979, A&A, 80, 155. Astronomy and Astrophysics, Volume
500, Issue 1, 2009, pp.157–158 (2009)
Trump, Jonathan R.; Impey, Chris D.; Elvis, Martin; McCarthy, Patrick J.;
Huchra, John P.; Brusa, Marcella; Salvato, Mara; Capak, Peter; Cappelluti, Nico;
Civano, Francesca; Comastri, Andrea; Gabor, Jared; Hao, Heng; Hasinger,
Gunther; Jahnke, Knud; Kelly, Brandon C.; Lilly, Simon J.; Schinnerer, Eva;
Scoville, Nick Z.; Smolčić, Vernesa The COSMOS Active Galactic Nucleus Spectroscopic Survey. I. XMM-Newton Counterparts. The Astrophysical Journal, Volume 696, Issue 2, pp. 1195–1212 (2009)
Vignali, C.; Pozzi, F.; Fritz, J.; Comastri, A.; Gruppioni, C.; Bellocchi,
E.; Fiore, F.; Brusa, M.; Maiolino, R.; Mignoli, M.; La Franca, F.; Pozzetti, L.; Zamorani, G.; Merloni, A. The HELLAS2XMM survey - XII. The
infrared/submillimetre view of an X-ray selected type 2 quasar at z ∼ 2. Monthly
Notices of the Royal Astronomical Society, Volume 395, Issue 4, pp. 2189–2195
(2009)
Zoccali, M.; Pancino, E.; Catelan, M.; Hempel, M.; Rejkuba, M.; Carrera, R.
The Radial Extent of the Double Subgiant Branch in NGC 1851. The Astrophysical
Journal Letters, Volume 697, Issue 1, pp. L22–L27 (2009)
Zucca, E.; Bardelli, S.; Bolzonella, M.; Zamorani, G.; Ilbert, O.; Pozzetti, L.; Mignoli, M.; Kovač, K.; Lilly, S.; Tresse, L.; Tasca, L.; Cassata, P.;
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Halliday, C.; Vergani, D.; Caputi, K.; Carollo, C. M.; Contini, T.; Kneib, J.-P.;
Le Fèvre, O.; Mainieri, V.; Renzini, A.; Scodeggio, M.; Bongiorno, A.; Coppa,
G.; Cucciati, O.; de La Torre, S.; de Ravel, L.; Franzetti, P.; Garilli, B.; Iovino,
A.; Kampczyk, P.; Knobel, C.; Lamareille, F.; Le Borgne, J.-F.; Le Brun, V.;
Maier, C.; Pellò, R.; Peng, Y.; Pérez-Montero, E.; Ricciardelli, E.; Silverman,
J. D.; Tanaka, M.; Abbas, U.; Bottini, D.; Cappi, A.; Cimatti, A.; Guzzo, L.;
Koekemoer, A. M.; Leauthaud, A.; Maccagni, D.; Marinoni, C.; McCracken, H.
J.; Memeo, P.; Meneux, B.; Moresco, M.; Oesch, P.; Porciani, C.; Scaramella,
R.; Arnouts, S.; Aussel, H.; Capak, P.; Kartaltepe, J.; Salvato, M.; Sanders, D.;
Scoville, N.; Taniguchi, Y.; Thompson, D. The zCOSMOS survey: the role of the
environment in the evolution of the luminosity function of different galaxy types.
Astronomy and Astrophysics, Volume 508, Issue 3, 2009, pp.1217–1234 (2009)
NON-REFEREED PAPERS IN JOURNALS
1. Beccari, G.; Ferraro, L. Pulone F. R.; Lanzoni, B.; Fusi Pecci, F.; Rood, R. T.;
Giallongo, E.; Ragazzoni, R.; Grazian, A.; Baruffolo, A.; De Santis, C.; Diolaiti,
E.; Di Paola, A.; Farinato, J.; Fontana, A.; Gallozzi, S.; Gasparo, F.; Gentile, G.;
Green, R.; Hill, J.; Kuhn, O.; Menci, N.; Pasian, F.; Pedichini, F.; Smareglia, R.;
Speziali, R.; Testa, V.; Thompson, D.; Vernet, E.; Wagner, R. M. First results
on resolved stellar population in three Galactic globular cluster from LBC@LBT
imaging. Memorie della Societa Astronomica Italiana, v.80, p.107 (2009)
2. Dalessandro, E.; Lanzoni, B.; Ferraro, F. R.; Vespe, F.; Bellazzini, M.; Tood, R.
T. Another non-segregated Blue Straggler population in a globular cluster: the case
of NGC 2419. Memorie della Societa Astronomica Italiana, v.80, p.121 (2009)
3. Giacconi, R.; Borgani, S.; Rosati, P.; Tozzi, P.; Gilli, R.; Murray, S.; Paolillo,
M.; Pareschi, G.; Tagliaferri, G.; Ptak, A.; Vikhlinin, A.; Flanagan, K.; Weisskopf,
M.; Bignamini, A.; Donahue, M.; Evrard, A.; Forman, W.; Jones, C.; Molendi, S.;
Santos, J.; Voit, G. Galaxy clusters and the cosmic cycle of baryons across cosmic
times. Astro2010: The Astronomy and Astrophysics Decadal Survey, Science
White Papers, no. 90 (2009)
4. Hartmann, D.; Kouveliotou, C.; Piro, L.; den Herder, J.W.; Ohashi, T.; Abel,
T.; Amati, L.; Barthelmy, S.; Beacom, J.; Bloom, J.; Bonamente, M.; Branchini,
E.; Branduardi-Raymont, G.; Bregman, J.; Briggs, M.; Bromm, V.; Burkert, A.;
Burrows, D.; Campana, S.; Carilli, C.; Cen, R.; Coppi, P.; Danforth, C.; Diehl,
R.; Ettori, S.; Fall, M.; Fan, X.; Fishman, G.; Fields, B.; Forman, C.; Ghisellini,
G.; Galeazzi, M.; Gehrels, N.; Ghirlanda, G.; Grindlay, J.; Heger, A.; Henry, P.;
Hermsen, W.; Holland, A.; Hughes, J.; Kaastra, J.; Kawai, N.; Keel, B.; Kelley,
R.; Kippen, M.; Kusenko, A.; Loeb, A.; Madau, P.; Matteucci, F.; Mathews,
G.; Meegan, C.; Meszaros, P.; Mineo, T.; Mitsuda, K.; Molendi, S.; Natalucci,
L.; Nomoto, K.; O’Brien, P.; O’Dell, S.; Paerels, F.; Pareschi, G.; Petrosian, V.;
Prantzos, N.; Primack, J.; Prochaska, J.; Ramirez-Ruiz, E.; Ramsey, B.; Rasmussen, A.; Savaglio, S.; Schaye, J.; Snowden, S.; Springel, V.; Suto, Y.; Tagliaferri, G.; Takei, Y.; Tawara, Y.; Timmes, F.; Townsely, L.; Ubertini, P.; van der
Horst, A.; Vink, J.; Weisskopf, M.; Wijers, R.; Wilson-Hodge, C.; Woosley, S.; Yamasaki, N. Reading the Metal Diaries of the Universe: Tracing Cosmic Chemical
Evolution. Astro2010: The Astronomy and Astrophysics Decadal Survey, Science
White Papers, no. 114 (2009)
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5. Kurk, Jaron; Cimatti, Andrea; Daddi, Emanuele; Mignoli, Marco; Bolzonella,
Micol; Pozzetti, Lucia; Cassata, Paolo; Halliday, Claire; Zamorani, Gianni; Berta, Stefano; Brusa, Marcella; Dickinson, Mark; Franceschini, Alberto;
Rodighiero, Guilia; Rosati, Piero; Renzini, Alvio A VLT Large Programme to
Study Galaxies at z ∼ 2: GMASS - the Galaxy Mass Assembly Ultra-deep Spectroscopic Survey. The Messenger, vol. 135, p. 40–44 (2009)
6. Londrillo, P.; Nipoti, C. N-MODY: a code for collisionless N-body simulations
in modified Newtonian dynamics. Memorie della Societa Astronomica Italiana
Supplement, v.13, p.89 (2009)
7. Moretti, A.; Arcidiacono, C.; Lombini, M.; Piotto, G.; Falomo, R.; Farinato, J.;
Ragazzoni, R.; Baruffolo, A.; Marchetti, E. MAD@VLT observations in Layer
Oriented mode: first results. Memorie della Societa Astronomica Italiana, v.80,
p.139 (2009)
8. Rosati, P.; Kuemmel, M.; Walsh, J.; Franzetti, P.; Cimatti, A.; Garilli, B.; Zamorani, G.; Scodeggio, M.; Rivera, H. Slitless Spectroscopic Simulations for Euclid
with aXeSIM. Space Telescope European Coordinating Facility Newsletter, Volume 46, p.12 (2009)
9. Sulentic, Jack; Marziani, Paola; Stirpe, Giovanna; Zamfir, Sebastian; Dultzin,
Deborah; Calvani, Massimo; Repetto, Paolo; Zamanov, Radoslav Constraining
Quasar Structural Evolution with VLT/ISAAC. The Messenger, vol. 137, p. 30–
33 (2009)
CIRCULARS AND TELEGRAMS
1. Maiorano, E.; Pizzichini, G.; Bartolini, C.; Greco, G.; Guarnieri, A.; Mantegna,
A.; Piccioni, A.; Nanni, D.; Terra, F.; Gualandi, R. GRB 090313: optical observations. GRB Coordinates Network, Circular Service, 9606, 1 (2009)
2. Nichelli, E.; Israel, G. L.; Moretti, A.; Campana, S.; Bernabei, S.; Mason, E.;
Götz, D.; Stella, L. Swift-XRT detection of x-ray pulsations from IGR J18173−2509
and SWIFT J2138.8+5544. The Astronomer’s Telegram, 2354 (2009)
INVITED PAPERS
1. Bellazzini, M. The Red Giant branches and Asymptotic Giant Branches of Simple
Stellar Population. invited talk at the (2009)
2. Cacciari, C. GAIA: the mission and (some of ) its scientific applications. Memorie della Societa Astronomica Italiana, v.80, p.97 (2009)
3. Cacciari, Carla The promise of Gaia and how it will influence stellar ages.
The Ages of Stars, Proceedings of the International Astronomical Union, IAU
Symposium, Volume 258, p. 409–418 (2009)
4. Carretta, Eugenio Observations of chemical evolution along the RGB. Invited
talk, Workshop ”The giant branches”, Lorentz Center, Leiden, 11–15 May 2009
(2009)
5. Clementini, G. Pulsating variable stars in the Magellanic Clouds. The Magellanic System: Stars, Gas, and Galaxies, eds. J. van Loon, & J. Oliveira, Cambridge
University Press, Volume 256, p. 373–384 (2009)
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6. Comastri, A.; Iwasawa, K.; Gilli, R.; Vignali, C.; Ranalli, P. AGN unified
scheme and evolution: a Suzaku view. eprint arXiv:0910.
1025 (2009)
7. Comastri, Andrea; Ranalli, Piero; Gilli, Roberto; Vignali, Cristian; Brusa,
Marcella; Civano, Francesca The high redshift Universe with the International Xray Observatory. Memorie Società Astronomica Italiana, in stampa (2009)
8. Ettori, S. Observations of the intracluster medium. The Wide Field X-ray Telescope workshop, Bologna, 25–26 Nov 2009 (2009)
9. Ettori, S. Cluster outskirts, mass profiles and concentrations. WFXT Workshop,
6–10 July 2009 (2009)
10. Ettori, S. Outskirts and masses in X-ray luminous clusters. International Workshop: CosmoClusters, i.e. Cosmology with Galaxy Clusters, Marseille (2009)
11. Ettori, S. A brief history of the metal accumulation in the ICM. The Chemical
Enrichment of the Intergalactic Medium, Lorentz Center, 25–29 May 2009 (2009)
12. Smith, Horace A.; Catelan, Márcio; Clementini, Gisella RR Lyrae Variables in
Stellar Systems. STELLAR PULSATION: CHALLENGES FOR THEORY AND
OBSERVATION: Proceedings of the International Conference. AIP Conference
Proceedings, Volume 1170, pp. 179–187 (2009)
13. Tosi, Monica Star formation histories of resolved galaxies. The Ages of Stars,
Proceedings of the International Astronomical Union, IAU Symposium, Volume
258, p. 61–72 (2009)
PUBLISHED PROCEEDINGS
1. Arcidiacono, C.; Ragazzoni, R.; Farinato, J.; Gentile, G.; Baruffolo, A.; Dima, M.;
Metti, C.; Viotto, V.; Diolaiti, E. Retrieving High Layer Atmospheric Turbulence
Statistics on E-ELT Scales. OPTICAL TURBULENCE: Astronomy Meets Meteorology, Proceedings of the Optical Turbulence Characterization for Astronomical
Applications Sardinia, Italy, 15–18 September 2008, edited by Elena Masciadri
(Instituto Nazionale di Astrofisica, Italy) & Marc Sarazin (European Southern
Observatory, Germany), pp.128–135 (2009)
2. Baldi, A.; Forman, W.; Jones, C.; Kraft, R.; Nulsen, P.; David, L.; Giacintucci,
S.; Churazov, E. The Unusual X-ray Morphology of NGC 4636 Revealed by Deep
Chandra Observations: Cavities and Shocks Created by Past AGN Outbursts. THE
MONSTER’S FIERY BREATH: FEEDBACK IN GALAXIES, GROUPS, AND
CLUSTERS. AIP Conference Proceedings, Volume 1201, pp. 271–274 (2009)
3. Bertone, E.; Chavez, M.; Buzzoni, A. Age-Metallicity Degeneracy at mid-UV
Wavelengths. A Long Walk Through Astronomy: A Celebration of Luis Carrasco’s
60th Birthday (Eds. E. Recillas, A. Luna, & Y. D. Mayya) Revista Mexicana de
Astronomı́a y Astrofı́sica (Serie de Conferencias) Vol. 37, pp. 147–149 (2009)
(http://www.astroscu.unam.mx/~rmaa/) (2009)
4. Bragaglia, Angela The Bologna Open Cluster Chemical Evolution project: a
large, homogeneous sample of Galactic open clusters. The Ages of Stars, Proceedings of the International Astronomical Union, IAU Symposium, Volume 258, p.
153–160 (2009)
5. Bragaglia, Angela; Carretta, Eugenio; Gratton, Raffaele; Tosi, Monica
Open Clusters as tracers of the Galactic disk: the Bologna Open Clusters Chemical
Evolution project. The Galaxy Disk in Cosmological Context, Proceedings of the
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International Astronomical Union, IAU Symposium, Volume 254. Edited by J.
Andersen, J. Bland-Hawthorn, and B. Nordström, p. 227–232 (2009)
Buson, L. M.; Bettoni, D.; Bianchi, L.; Buzzoni, A.; Marino, A.; Rampazzo,
R. The Impact of Encounters on the Members of Local Group Analogs. A View
from GALEX. New Quests in Stellar Astrophysics. II. Ultraviolet Properties of
Evolved Stellar Populations, Proceedings of the International Conference held in
Puerto Vallarta, Mexico, April 16–20, 2007. Eds.: M. Chavez, E. Bertone, D.
Rosa-Gonzalez, and L. H. Rodriguez-Merino, Springer, p. 105–108 (2009)
Buzzoni, A.; Bertone, E.; Chávez, M.; Rodrguez-Merino, L. H. Population Synthesis at Short Wavelengths and Spectrophotometric Diagnostic Tools for Galaxy
Evolution. New Quests in Stellar Astrophysics. II. Ultraviolet Properties of
Evolved Stellar Populations, Proceedings of the International Conference held in
Puerto Vallarta, Mexico, April 16–20, 2007. Eds.: M. Chavez, E. Bertone, D.
Rosa-Gonzalez, and L. H. Rodriguez-Merino, Springer, p. 263–271 (2009)
Buzzoni, A.; Battistini, C.; Carrasco, L.; Recillas, E. Spectroscopic Gradients in
Early-type Galaxies. A Long Walk Through Astronomy: A Celebration of Luis
Carrasco’s 60th Birthday (Eds. E. Recillas, A. Luna, & Y. D. Mayya) Revista
Mexicana de Astronomı́a y Astrofı́sica (Serie de Conferencias) Vol. 37, pp. 110–
119 (2009) (http://www.astroscu.unam.mx/~rmaa/) (2009)
Carlson, Lynn R.; Romita, K. A.; Sabbi, E.; Meixner, M.; Babler, B.; Block, M.;
Engelbracht, C.; Gallagher, J. S. III; Gordon, K.; Hora, J. L.; Indebetouw, R.;
Kato, D.; Leitherer, C.; Meade, M.; Misselt, K.; Nota, A.; Oey, M. S.; Robitaille,
T.; Sewilo, M.; Sirianni, M.; Smith, L. J.; Tosi, M.; Vijh, U.; Walterbos, R.;
Whitney, B. A Panchromatic View of Clustered Star Formation in the Magellanic
Clouds: Spatial and Temporal Resolution as Revealed through Optical and Infrared
Imaging. American Astronomical Society, AAS Meeting 213, 413.12; Bulletin of
the American Astronomical Society, Vol. 41, p.222; Bulletin of the American
Astronomical Society, Vol. 41, p.222 (2009)
Comastri, Andrea; Gilli, R.; Vignali, C.; Iwasawa, K.; Ranalli, P. The Quest
for Very High Redshift Black Holes. American Astronomical Society, AAS Meeting 213, 454.02; Bulletin of the American Astronomical Society, Vol. 41, p.350;
Bulletin of the American Astronomical Society, Vol. 41, p.350 (2009)
de Gouveia Dal Pino, E. M.; Melioli, C.; D’Ercole, A.; Brighenti, F.; Raga, A.
C. Supernova Explosions and the Triggering of Galactic Fountains and Outflows.
Magnetic Fields in the Universe II: From Laboratory and Stars to the Primordial
Universe (Eds. A. Esquivel, J. Franco, G. Garca-Segura, E. M. de Gouveia Dal
Pino, A. Lazarian, S. Lizano, & A. Raga) Revista Mexicana de Astronoma y
Astrofsica (Serie de Conferencias) Vol. 36, pp. 17–24
(http://www.astroscu.unam.mx/~rmaa/) (2009)
Evans, Aaron S.; Vavilkin, T.; Iwasawa, K.; Armus, L.; Surace, J.; Pizagno, J.;
Mazzarella, J.; Sanders, D.; Petric, A. GOALS Observations of Star Formation
and AGN Activity in the Luminous Infrared Galaxy NGC 2623. American Astronomical Society, AAS Meeting 213, 334.06; Bulletin of the American Astronomical
Society, Vol. 41, p.395; Bulletin of the American Astronomical Society, Vol. 41,
p.395 (2009)
Eyer, L.; Mowlavi, N.; Varadi, M.; Spano, M.; Lecoeur-Taibi, I.; Clementini,
G. The Gaia mission and variable stars. SF2A-2009: Proceedings of the Annual
meeting of the French Society of Astronomy and Astrophysics, held 29 June–4 July
2009 in Besanon, France. Eds.: M. Heydari-Malayeri, C. Reyl and R. Samadi, p.45
(2009)
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14. Fiore, F.; Arnaud, M.; Briel, U.; Cavazzuti, E.; Cledassou, R.; Counil, J. L.;
Comastri, A.; Ferrando, P.; Giommi, P.; Goldwurm, A.; Lamarle, O.; Lanzuisi,
G.; Laurent, P.; Lebrun, F.; Malaguti, G.; Mereghetti, S.; Micela, G.; Pareschi, G.;
Piconcelli, E.; Piermaria, M.; Puccetti, S.; Roques, J.-P.; Tagliaferri, G.; Vignali,
C. Simbol-X Core Science in a Context. SIMBOL-X: FOCUSING ON THE HARD
X-RAY UNIVERSE: Proceedings of the 2nd International Simbol-X Symposium.
AIP Conference Proceedings, Volume 1126, pp. 9–14 (2009)
15. Gaspari, M.; Melioli, C.; Brighenti, F.; D’Ercole, A. 3D Numerical Simulations
of AGN Outflows in Clusters and Groups. THE MONSTER’S FIERY BREATH:
FEEDBACK IN GALAXIES, GROUPS, AND CLUSTERS. AIP Conference Proceedings, Volume 1201, pp. 309–312 (2009)
16. Gastaldello, Fabio; Ettori, Stefano; Balestra, Italo; Brighenti, Fabrizio; Buote,
David; De Grandi, Sabrina; Gitti, Myriam; Tozzi, Paolo The inverse iron-bias in
action in Abell 2028. 34;The Energetic Cosmos: from Suzaku to Astro-H34;, July
2009, Otaru, Hokkaido, Japan (2009)
17. Giacintucci, S.; Vrtilek, J. M.; O’Sullivan, E.; Raychaudhury, S.; David, L. P.;
Venturi, T.; Athreya, R.; Gitti, M. AGN Feedback in Galaxy Groups: A Joint
GMRT/X-ray Study. THE MONSTER’S FIERY BREATH: FEEDBACK IN
GALAXIES, GROUPS, AND CLUSTERS. AIP Conference Proceedings, Volume
1201, pp. 229–232 (2009)
18. Gitti, M.; O’Sullivan, E.; Giacintucci, S.; David, L.; Vrtilek, J.; Raychaudhury,
S.; Nulsen, P. AGN Feedback in the Compact Group of Galaxies HCG 62-as Revealed by Chandra, XMM and GMRT Data. THE MONSTER’S FIERY BREATH:
FEEDBACK IN GALAXIES, GROUPS, AND CLUSTERS. AIP Conference Proceedings, Volume 1201, pp. 233–236 (2009)
19. Gitti, Myriam; O’Sullivan, E.; Giacintucci, S.; David, L.; Vrtilek, J.; Raychaudhury, S.; Jones, C.; Forman, W. AGN feedback in galaxy groups: The case of HCG
62. Chandra’s First Decade of Discovery, Proceedings of the conference held 22–25
September, 2009 in Boston, MA. Edited by Scott Wolk, Antonella Fruscione, and
Douglas Swartz, abstract 30 (2009)
20. González-Lópezlira, R. A.; Buzzoni, A. UV Excess and AGB Evolution in Elliptical-Galaxy Stellar Populations. New Quests in Stellar Astrophysics. II. Ultraviolet
Properties of Evolved Stellar Populations, Proceedings of the International Conference held in Puerto Vallarta, Mexico, April 16–20, 2007. Eds.: M. Chavez,
E. Bertone, D. Rosa-Gonzalez, and L. H. Rodriguez-Merino, Springer, p. 51–57
(2009)
21. Greco, C.; Clementini, G.; Held, E. V.; Poretti, E.; Catelan, M.; Dell’Arciprete,
L.; Gullieuszik, M.; Maio, M.; Rizzi, L.; Smith, H. A.; Pritzl, B. J.; Rest, A.;
de Lee, N. Variable Stars in the Globular Clusters and in the Field of the Fornax
dSph Galaxy. Globular Clusters – Guides to Galaxies, Eso Astrophysics Symposia,
Volume . ISBN 978-3-540-76960-6. Springer Berlin Heidelberg, 2009, p. 163
(2009)
22. Greco, Claudia; Clementini, Gisella; Held, Enrico E.; Poretti, Ennio; Catelan,
Márcio; Federici, Luciana; Gullieuszik, Marco; Maio, Marcella; Ripepi, Vincenzo; Dall’Ora, Massimo; di Fabrizio, Luca; Kinemuchi, Karen; di Criscienzo,
Marcella; Marconi, Marcella; Musella, Ilaria; Rest, Armin; de Lee, Nathan; Pritzl,
Barton J.; Smith, Horace Looking for the Building Blocks of the Galactic Halo:
Variable stars in the Fornax, Bootes I, Canes Venatici II Dwarfs and in NGC2419.
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Proceedings of the International Conference. AIP Conference Proceedings, Volume 1170, pp. 197–199 (2009)
Gruppioni, C.; Pozzi, F.; Spinoglio, L.; Magliocchetti, M.; Isaak, K.; de Zotti, G.
Model Predictions for Deep Cosmological Surveys with SPICA-SAFARI. SPICA
joint European/Japanese Workshop, held 6–8 July, 2009 at Oxford, United Kingdom. Edited by A.M. Heras, B.M. Swinyard, K.G. Isaak, and J.R. Goicoechea.
EDP Sciences, 2009, p.04009 (2009)
Harris, D. E.; Massaro, F.; Axon, D.; Baum, S. A.; Capetti, A.; Chiaberge, M.;
Gilli, R.; Giovannini, G.; Grandi, P.; Macchetto, F. D.; O’Dea, C. P.; Risaliti, G.;
Sparks, W. The Chandra 3C Snapshot Survey for Sources with z < 0.3. Chandra’s
First Decade of Discovery, Proceedings of the conference held 22–25 September,
2009 in Boston, MA. Edited by Scott Wolk, Antonella Fruscione, and Douglas
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Isaak, Kate G.; Sturm, Eckhard; Elbaz, David; Spinoglio, L.; Gruppioni, Carlotta Exploring the Spectroscopic Capabilities of SAFARI for studies of the Distant
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N.; Comastri, A.; Pozzetti, L.; Vignali, C.; Lonsdale, C.; Rowan-Robinson, M.;
Surace, J.; Shupe, D.; Fang, F.; Matute, I.; Berta, S. Erratum: The Contribution
of AGN and Star-forming Galaxies to the Mid-infrared as Revealed by their Spectral
Energy Distributions (2008, ApJ, 684, 136). The Astrophysical Journal, Volume
701, Issue 1, pp. 850–855 (2009)
113
10
Observing Campaigns
OBSERVATIONS IN 2009
ESO TELESCOPES
VLT
1. ESO VLT+CRIRES, Probing the origin of the Na-O anticorrelation in Globular
Clusters through massive Galactic star clusters, PI: S. Lucatello, Co-I: Bragaglia
A., Carretta E., C. Charbonnel, F. D’Antona, R. Gratton, B. Plez, C. Sneden,
10.3 hrs, P83: 1Apr–30Sep 2009, service mode
2. ESO VLT+CRIRES+UVES, Direct measurement of He abundance variations in
Globular Cluster Red Giants, PI: L. Pasquini, Co-I: C. Cacciari, P. Mauas, H.U.
Kaufl, 8 h, Nov 2009 – Jan 2010, service mode
3. VLT+FLAMES, Ground-based observations for Gaia’s calibrations: the Southern
Ecliptic Pole initial calibration field (084.D-0427)., PI: M. Altmann (Heidelberg),
Co-I: Y. Fremat, U. Heiter, G. Jasniewicz, E. PancinoC. Soubiran, F. Thevenin,
A. Vallenari, 20 hours , October 2009 – March 2010, service mode
4. ESO VLT+FLAMES, Formation and evolution of Galactic Globular Clusters: the
first billion years and how they shaped morphology, chemistry and current properties of these old systems., PI: Carretta E., Co-I: Bellazzini M., Bragaglia A.,
& 13 more, 41 hours, P83: 1 Apr–30 Sep 2009, service mode
5. ESO VLT+FLAMES, Unveiling the true nature of Terzan 5: a prompt follow-up
of a MAD discovery, PI: F.R. Ferraro, Co-I: Mucciarelli, Lanzoni, Dalessandro,
Valenti, Beccari,L. Origlia, M. Bellazzini, Rich, Rood, Ransom, 8 hrs, 2009,
service mode
6. ESO VLT+FLAMES, Searching for chemical signatures of the self-enrichment
process in extra-galactic clusters: the LMC, PI: A. Mucciarelli, Co-I: Origlia, Ferraro, Lanzoni, Valenti, 4 nights, November 2009, visitor mode
7. ESO VLT+FORS2, Magnified Weak Lensing Tomography With Massive Rich Clusters of Galaxies, PI: C. Adami, Co-I: Le Brun V., Ilbert O., A. Cappi, et al., 35
hours, October 2009 – March 2010, service mode
8. ESO VLT+FORS2, Chemical abundances as tracers of Galactic substructures:
Searching for ex-Omega Centauri members among solar neighbourhood stars, PI:
D. Romano, Co-I: Bellazzini M., Pancino E., Tosi M.et al, 27 hours, April
2009, service mode
9. ESO VLT+ISAAC, The Hβ Spectral Region of High Redshift Quasars: Searching for Missing Signatures of Quasars’ Structural Evolution, PI: PI: P. Marziani
(INAF/OAPd), Co-I: Co-I: J. W. Sulentic (Univ. Alabama, IAA-Granada), G.M.
Stirpe, D. Dultzin (UNAM-Mexico), S. Zamfir (Univ. Alabama), A. Negrete
(UNAM-Mexico), 22 hours, service mode
10. ESO VLT+SINFONI, Following the mass assembly of galaxies at the key epoch
1.0 < z < 1.8 from a complete sample observed with SINFONI, PI: T. Contini,
Co-I: ..., S. Bardelli, D. Vergani, E. Zucca ..., 50 hours, year 2009, service mode
11. ESO VLT+SINFONI, Caught in the act: the assembly and makeup of the COSMOS most massive galaxies at z ∼ 2 with SINFONI+AO+ LGS, PI: A. Renzini,
Co-I: Daddi, E., Lilly, S., [...], G. Zamorani, D. Vergani, et al., l6.2 hours, 2009,
service mode
114
12. ESO VLT+UVES, The Lyman alpha forest and the galaxy density field at z = 2.5,
PI: S. Lilly, Co-I: ..., S. Bardelli, E. Zucca ..., 31 hours, year 2009, service mode
13. ESO VLT+UVES, Chemical abundances as tracers of Galactic substructures: Searching for ex-Omega Centauri members among solar neighbourhood stars. (083.B0281), PI: D. Romano, Co-I: E. Pancino, M. Bellazzini, M. Tosi, F.R. Ferraro, E. Rossetti, 27 hours, June 2009, service mode
14. ESO VLT+VIMOS, zCOSMOS: The evolutionary links between galaxies, their nuclei, their morphologies and their environments, PI: S. Lilly, Co-I: ..., S. Bardelli,
M. Bolzonella, A. Cappi, M. Mignoli, L.Pozzetti, D.Vergani, G. Zamorani, E. Zucca and the zCOSMOS team, 30 hours, year 2009, service mode
15. ESO VLT+VIMOS, The large-scale structure and growth rate of the Universe at
z ∼ 1 from a survey of 100, 000 galaxy redshifts (VIPERS), PI: L. Guzzo, Co-I: J.
Blaizot, M. Bolzonella, . . . , Large Programme, 75 hours, 2009, run A-B-C-D-E,
service mode
16. ESO VLT+VIMOS, AGN feedback in NGC5044: What is the relation between the
Hα nebula and X-ray cavities, filaments and dust ?, PI: F. Gastaldello, Co-I: S.
Ettori et al., 20 hours, June 2009, service mode
17. ESO VLT+VIMOS, Intragroup light in HCG 90: a nursery for young stars or the
death throes o f a compact group?, PI: E. Pompei, Co-I: A. Buzzoni, P. Focardi,
P. Imperatore, V. Ivanov, I. Saviane,
3 nights, July 2009, visitor mode
18. ESO VLT+VIMOS, Exploring the Universe with a high REsolution Kinematical
Approach, PI: L. Tresse, Co-I: [...], L. Pozzetti et al., 25.5 hrs, 2009, service mode
VISTA
19. VISTA+VIRCAM, Ultra-VISTA: an Ultra Deep Survey with VISTA, PI: J. Dunlop, Co-I: [...], M. Bolzonella, A. Cimatti et al., 100h, 2009, service mode
20. ESO VISTA+VIRCAM, Ultra-VISTA: an Ultra Deep Survey with VISTA, Prog.
ID: 179.A-2005, PI: Dunlop, Co-I: J. Afonso, . . . , M. Bolzonella. . . . , Large
Programme, 12 hours, 2009, run A, service mode
ESO 2.2m
21. ESO 2.2m+WIFI+FEROS, A complete characterization of the bulge Globular
Cluster NGC 6723, PI: M. Zoccali, Co-I: V. Ripepi, G. Clementini, M. Dall’Ora,
A. Grado, M. Marconi, I. Musella, M.I. Moretti, 5.5+2.5 nights, May 2010, June
2010, visitor mode
NTT
22. ESO NTT+EFOSC2, Ground-based observations for Gaia’s calibrations : Establishing the Grid of Spectro-Photometric Standard Stars. (182.D-0287(B)(C)),
PI: E. Pancino (INAF-OA Bologna), Co-I: A. Bragaglia, G. Altavilla, M.
Bellazzini, C. Cacciari, L. Federici, P. Montegriffo (INAF-OA Bologna); S.
Marinoni (Univ. of Bologna, TNG); J.M. Carrasco, C. Fabricius, F. Figueras, C.
Jordi (Univ. Barcelona-IEEC); C. Soubiran (Obs. Bourdeau); S. Trager (Kapteyn
Astr. Inst.), 5+7 nights, April, August 2009, visitor mode
23. NTT+SOFI, Halpha imaging of a forming cluster at z=1.6 in the GMASS field,
PI: J. Kurk, Co-I: A. Cimatti, G. Zamorani, M. Mignoli, L. Pozzetti et al.,
3 nights, Sept 2009, visitor mode
115
APEX
24. APEX+LABOCA, Large-Scale Structure and Submillimeter Galaxies: A LABOCA
Survey of the COSMOS Field, Co-I: F. Bertoldi, F. Menten, E. Schinnere, [...], G.
Zamorani, et al., 1.5 hours, 2009, service mode
REM
25. REM 0.6m+ROSS, GAIA Calibration Working Group: Monitoring candidate Spectrophotometric Standard Stars against variability (16012 AOT18/07B), PI: E.
Pancino(INAF-OA Bologna), Co-I: G. Altavilla, M. Bellazzini, A. Bragaglia,
C. Cacciari, L. Federici (INAF-OA Bologna); S. Marinoni (Univ. Bologna &
TNG); R. Silvotti (INAF-OA Capodimonte); J.M. Carrasco, F. Figueras, C. Jordi,
(Univ. Barcelona); S. Trager (Univ. Groningen), 76 hours, from August 2008 to
January 2009, service mode
26. REM 0.6m+ROSS, GAIA Calibration Working Group: Monitoring candidate Spectrophotometric Standard Stars against variability (19010 AOT19), PI: E. Pancino,
Co-I: G. Altavilla, M. Bellazzini, A. Bragaglia, C. Cacciari, L. Federici,
S. Marinoni, R. Silvotti, J.M. Carrasco, C. Jordi, F. Figueras, S. Trager, 94 hours,
from Feb. to Jul. 2009. Submitted in Oct 2008 , service mode
27. REM 0.6m+ROSS, GAIA Calibration Working Group: Monitoring candidate Spectrophotometric Standard Stars against variability (AOT
20), PI: E. Pancino (INAF-OA Bologna), Co-I: G. Altavilla, M. Bellazzini,
A. Bragaglia, C. Cacciari, L. Federici, G. Cocozza (INAF-OA Bologna); S.
Marinoni (Univ. Bologna & TNG); R. Silvotti (INAF-OA Capodimonte); J.M.
Carrasco, C. Jordi, F. Figueras (Univ. Barcelona); S. Trager (Univ. Groningen),
146 hours, from August 2009 to January 2010, service mode
ITALIAN TELESCOPES AND OTHER TELESCOPES WITH ITALIAN PARTICIPATION
LBT
28. LBT 2x8.4m+Blue+Red, Pulsating variable stars in the halo and stream of Andromeda: hints on the galaxy star formation history and assembling, PI: G. Clementini, Co-I: G. Beccari, M. Bellazzini, C. Cacciari, L. Ciotti, R. Contreras,
E. Diolaiti, L. Federici, F. Fusi Pecci, G. Macario, B. Marano, M. Tosi,
M. Marconi, I. Musella, V. Ripepi, 20 hours, September, Nov–Dec 2009, service
mode
TNG
29. TNG+DOLORES, Spectrophotometric standard stars observations for GAIA’s absolute flux calibration. (TAC 14 AOT19), PI: E. Pancino, Co-I: G. Altavilla,
M. Bellazzini, A. Bragaglia, C. Cacciari, L. Federici, P. Montegriffo, E.
Rossetti, S. Marinoni, C. Lardo, J.M. Carrasco, C. Fabricius, F. Figueras, C.
Jordi, S. Trager, 5+5 nights +3 compensatory nights, March, June, July 2009,
visitor mode
116
30. TNG+DOLORES, Ground based observations for Gaia Calibration: spectrophotometric standards for absolute flux calibration. (TAC 41 AOT20), PI: E. Pancino
(INAF-OA Bologna), Co-I: G. Altavilla, M. Bellazzini, A. Bragaglia, C.
Cacciari, L. Federici, P. Montegriffo, E. Rossetti, S. Marinoni, C. Lardo,
J.M. Carrasco, C. Fabricius, F. Figueras, C. Jordi, S. Trager, 5+5 nights, September, December 2009, visitor mode
31. TNG+DoLores, A survey of kinematically peculiar globular clusters in M31, le of
the program PI: S. Galleti, Co-I: M. Bellazzini, A. Buzzoni, L. Federici, F.
Fusi Pecci, S. Perina, 4 nights, September 2009, visitor mode
32. TNG+LRS, A survey of kinematically peculiar globular clusters in M31, PI: S.
Galleti, Co-I: M. Bellazzini, A. Buzzoni, L. Federici, F. Fusi Pecci, S.
Perina, 4 nights, September 2009, visitor mode
33. TNG+SARG, Open Clusters as tracers of the Galactic disk chemical evolution (the
BOCCE project), PI: Bragaglia A., Co-I: Carretta E., Tosi M., R. Gratton,
G. Andreuzzi, L. Di Fabrizio , 29hr, 31 Dec 2008–4 Jan 2009, visitor mode
34. TNG+SARG, Searching for ex-Omega Centauri members among solar neighbourhood stars, PI: D. Romano (INAF-OA Bologna/Bologna University), Co-I: E.
Pancino, M. Bellazzini, M. Tosi, F.R. Ferraro (Bologna University), E. Rossetti, 2 nights, March 2009, visitor mode
35. TNG+SARG, Searching for ex-Omega Centauri members among solar neighbourhood stars, PI: D. Romano (INAF-OA Bologna/Bologna University), Co-I: E.
PancinoM. Bellazzini, M. Tosi (INAF-Bologna Observatory), F.R. Ferraro (Bologna University), E. Rossetti (INAF-Bologna Observatory), 10.6 hours, Aug–Dec
2009, service mode
Loiano
36. Cassini 1.5m+BFOSC, GAIA Calibration Working Group: Monitoring candidate
Spectrophotometric Standard Stars against variability, PI: G. Altavilla (INAFOA Bologna), Co-I: E. PancinoM. Bellazzini, A. Bragaglia, C. Cacciari,
L. Federici, G. Cocozza, P. Montegriffo, E. Rossetti (INAF-Bologna Obs); S.
Marinoni (Univ. Bologna & TNG); C. Lardo (Univ. Bologna); R. Silvotti (INAFOA Capodimonte, 3+4 nights, February, May 2009, visitor mode
37. Cassini 1.5m+BFOSC, GAIA Calibration Working Group: Monitoring candidate
Spectrophotometric Standard Stars against variability, PI: G. Altavilla (INAFOA Bologna), Co-I: E. PancinoM. Bellazzini, A. Bragaglia, C. Cacciari,
L. Federici, G. Cocozza, P. Montegriffo, E. Rossetti (INAF-Bologna Obs); S.
Marinoni (Univ. Bologna & TNG); R. Silvotti (INAF-OA Capodimonte, 2+2+2
nights, August, November 2009, January 2010, visitor mode
38. Loiano 1.52m+BFOSC+EEV, Stellar Archaeology in the Milky Way halo: variable
stars and stellar populations in the UMaI dwarf Spheroidal galaxy (dSph), PI: G.
Clementini, Co-I: M. Dall’Ora, V. Ripepi, M. Marconi, C. Greco, K. Kinemuchi,
H.A. Smith, 7 nights, March, April 2009, service mode
117
FOREIGN TELESCOPES
Keck
39. KECK+NIRSPEC, Composition and Na-O Anticorrelations in the Galactic bulge
cluster and Fie ld Population, PI: R.M. Rich, Co-I: L. Origlia, E. Valenti, 0.5
nights, July 2009, visitor mode
SPM 1.5m
40. SPM 1.5m+La Ruca, Ground-based photometry for the absolute flux calibration of
Gaia, PI: F. Figueras (Univ. Barcelona), Co-I: William J. Schuster B., Barbara
Pichardo, E. Pancino, S. Trager (Kapteyn Astr. Inst.), 10 nights, January 2009,
visitor mode
WIYN OBSERVATORY
41. WIYN 3.5m+Hydra, Searching for Abundance Anomalies in the Old, Metal-rich
Open Cluster NGC 6791, PI: C. Sneden, Co-I: Bragaglia A., Carretta E., R.
Gratton, S. Lucatello, 2, 6–7 June 2009, visitor mode
CTIO
42. CTIO 1m+Y4KCam, BV I Time-Series photometry of the bright variable stars
of NGC6584, PI: M. Zoccali, Co-I: V. Ripepi, G. ClementiniM. Dall’Ora, M.
Marconi, M.I. Moretti, S. Vasquez, A. Rojas, 7 nights, Jul 2010, visitor mode
SPACE OBSERVATORIES
HST
43. HST+ACS+COS, The difference between neutral and ionized gas metal abundances in local star forming galaxies, PI: A. Aloisi, Co-I: M. Tosi et al, 17 orbits,
January 2009 – May 2010 due to SM4 delay, service mode
44. HST+WFPC2, UV light from old stellar populations: a census of UV sources
in Galactic Globular Clusters, PI: F.R. Ferraro, Co-I: Beccari, A. Buzzoni, C.
CacciariDalessandro, F. Fusi Pecci, B. Lanzoni, Miochi, Mucciarelli, O’Connell,
L. Origlia, Rood, Schiavon, Sigurdsson, Valenti, 177 orbits, 2009
45. HST+WFC3, ACS, PI: F. Mannucci, F., Co-I: G. Cresci, A. Marconi, [...], L.
Pozzetti et al., The LSD project: dynamics, merging and stellar populations of a
sample of well-studied LBGs at z ∼ 3, 18 orbits, November 2009
46. HST+WFC3, Hunting for optical companions to binary MSPS in globular clusters,
PI: F.R. Ferraro, Co-I: Beccari, Cocozza, Dalessandro, Freire, Lanzoni, Lucatello,
Mucciarelli, L. Origlia, Possenti, Ramson, Rood, Sairs, Valenti, 18 orbits, 2009
Herschel
47. Herschel+PACS/SPIRE, The Great Observatories Origin Deep Survey – far-infrared
imaging with Herschel, PI: D. Elbaz, Co-I: R. Gilli et al., 362.6 hours, May–Aug
2009
118
XMM-Newton
48. XMM+pn/MOS, The ultradeep survey in the CDFS: an XMM-Newton legacy, PI:
A. Comastri, Co-I: R. Gilli, G. Zamorani, C. Vignali, K. Iwasawa et al.,
1563 ksec, Observed in 2009, service mode
49. XMM+pn/MOS, Unveiling obscured accretion: The XMM-Newton view of IR
selected SWIRE QSO2s, PI: F. Fiore, Co-I: Comastri A., C. Vignali, et al., 160
ksec, Observed in 2009, service mode
Chandra
50. Chandra+ACIS, Investigating AGN feedback in cool cores detected in Hα, PI: M.
Gitti, Co-I: F. Gastaldello, S. Ettori, L. Feretti, F. Brighenti, 44 ksec, approved
in June 2009, service mode
51. Chandra+ACIS, What are those clusters that do not have a radio halo?, PI: S.
Giacintucci, Co-I: R. Cassano, G. Brunetti, T. Venturi, M. Markevitch, M. Gitti,
S. Ettori, Archival, approved in June 2009, service mode
119
11
National and International
Appointments, working-group
memberships & policy committees
• Bolzonella M.
- PRIN-INAF VIPERS: The large scale structure and growth rate of the Universe
at z ∼ 1 from a survey of 100, 000 galaxy redshifts, PI Luigi Guzzo, funds assigned
with D.P. 21/2009: local PI
- Observatory “Thursday Seminars”: organizer
• Bragaglia A.
- Time Allocation Committee for TNG: member
- SIMPLE Science Team: member
• Buzzoni A.
- Comisión Dictaminadora Externa dell’Instituto Nacional de Astrofı́sica, Optica
y Electrónica (Mexico): member
- RCEA (Registro Evaluadores Acreditados) del CONACyT (Mexico): member
- Visiting Scientist presso l’European Astronomical Observatory (ESO), Chile
Headquarter, Santiago de Chile (Cile)
- Universitá di Bologna, corso di “Evoluzione spettrale nelle galassie” (Laurea
Specialistica in Astrofisica e Cosmologia): Professore a contratto
- CONICET (Buenos Aires, Argentina): Investigador Correspondiente
• Cacciari C.
- Science Committee for the Fondazione Osservatorio Astrofisico di Castelgrande:
member
- Management Team for the GAIA Coordination Unit 5 (CU5): member
- GAIA CU5/DU14 (Instrument absolute response characterisation: definition and
application): manager
• Cappi A.
- Observatoire de la Côte d’Azur: astronome associé
• Ciliegi P.
- Scientific Working Group of ELT/MAORY , the Multi Conjugate Adaptive Optics Module for ELT: member
- Scientific Working Group of LINC-NIRVANA, the near infrared interferometer
for LBT: member
• Clementini G.
- Working group WGA8 Distance Scales within the Gaia Research for European
Astronomy Training (GREAT): coordinator
120
- Supplementary Observations workpackage (CU7/WP 732) and Cepheids/RR
Lyrae of the Specific Object Studies workpackage (CU7/WP 720-03000), within
GAIA Coordination Unit 7 (CU7): manager
- Ground Based Observation for Gaia (GBOG) working group: representative for
CU7
- PRIN-INAF project “The ESO Magellanic Cloud Surveys: tracing the stellar
populations and beyond”: local coordinator
• Comastri A.
- ESA IXO (International X-ray Observatory) Science Definition Team (ISDT):
member
- COSMOS AGN Working Group: chair
- Euro-VO Scientific Advisory Committe: member
- Università di Ferrara, corso di ”Stelle, Galassie e mezzo interstellare” (Laurea
Specialistica in Astrofisica): Professore a contratto
• Diolaiti E.
- ELT Design Study (European Community Framework Programme 6 - Contract
N. 011863) ”Novel Adaptive Optics Concepts”: Task Manager End: June 2009
- Phase A Study of a multi-conjugate adaptive optics module for the European
Extremely Large Telescope, ESO and European Union Framework Programme 7:
Principal Investigator End: December 2009
- Preparing for the construction of the European Extremely Large Telescope
(Grant Agreement, European Community 7th Framework Programme under Contract INFRA-2.2.1.28), ”Multi Conjugate Adaptive Optics performance evaluation”: Deputy Task Manager End: June 2010
• Ettori S.
-
Chandra Cycle 10 TAC panel: member
ESA XMM-Newton Cycle 9 and 10 TAC: member
Contract ASI I/088/06/0: national PI
PRIN-INAF 2006 and contract ASI I/023/05/0: local PI
Observatory “Thursday Seminars”: organizer
• Fusi Pecci F.
-
Director of the Bologna Observatory
INAF Dip.1: member of the Board
Cagliari Astronomical Observatory: member of the Board
Sardinia Radio Telescope: member of the Board
Consiglio Fondazione FOAC (Telescopio Toppo): member
Fondazione Marino Golinelli, Scientific Committee: member
Società Astronomica Italiana (SAIt): member of the Board
• Gitti M.
SAO, Harvard-Smithsonian Center for Astrophysics (MA, USA): Visiting Scientist
121
• Gruppioni C.
- Extragalactic Herschel Open Time Surveys (“PACS Evolutionary Probe (PEP)”)
Consortium: member
- Consorzio per la missione ESA/JAXA SPICA-SAFARI: member
- Programma Finanziato ASI-INAF I/057/08/0
- Partecipazione italiana allo studio di fattibilità dello strumento SPICA SAFARI:
co-PI
Iwasawa
- ESA: XMM-Newton Time Allocation Committee AO8: AGN panel member
• Origlia L.
- GIANO–TNG project: Principal Investigator
- SIMPLE-E-ELT project: Principal Investigator
- ESO Instrument Science Team of X-shooter: member
- LBT Scientific and Technical Committee: member
- TNG-LBT Time Allocation Committee: member
- Collegio dei Docenti di Dottorato del Dipartimento di Astronomia dell’Università
di Bologna, XXIII Ciclo: member
• Pancino E.
- GAIA DPAC (Data Processing and Analysis Consortium) CU5/DU15 (Instrument absolute response characterisation: ground based preparation): manager
- GAIA DPAC GBOG (Ground Based Observations for Gaia) Working Group:
deputy
• Tosi M.
- Deputy Director of the Bologna Observatory
- ESO OPC Nominating Committee: chair
- INAF Scientific Council: member
- European Research Council, Starting Grants selection committee: member
- ESO ELT Standing Review Committee: member
- JWST Science & Technology Advisory Committee (Baltimore, USA): member
- Institute Visiting Committee of the Space Telescope Science Institute (Baltimore
USA): ESA member
- International Space Science Institute (Bern) Science Committee: member
- ASI: member of the Guppo di Lavoro per Cosmologia e Fisica Fondamentale
- IAU Commission 37 Organizing Committee (Open Clusters): member
• Zamorani G.
-
zCOSMOS management team : member
ESA Time Allocation Committee for Herschel : member
EUCLID WG on ”Galaxy and AGN evolution”: co-coordinator
TNG/LBT TAC: member
122
• Zitelli V.
- SUCOSIP (Site Properties Sub-Committee) per i telescopi presenti alle Canarie
- Loiano telescopes: coordinator
- Contract FP7 Science Access: member
• Zucca E.
- ESO Observing Programme Committee Panel A: member
123
12
Organization of Workshops
Bolzonella M., Vergani D.
- LOC of the School of Astrophysics “Francesco Lucchin”, X Cycle, III Course – Bertinoro, May 24–29, 2009
(http://www.bo.astro.it/~school09/): member
Buzzoni A.
- Docente invitato nei seminari di specializzazione su “Globular Clusters: not that simple
stellar populations”, corso di Dottorato di Ricerca in Astronomia presso l’Università di
Bologna
- Relatore di due tesi di Laurea Specialistica in Astrofisica e Cosmologia presso presso
l’Università di Bologna
Cacciari C.
- Meeting of the Gaia CU5 Management Team, Bologna, 16 March 2009: organizer
- Gaia CU5 Review Meeting M07, Bologna, 17–19 March 2009: organizer
- Gaia CU5 PhotPipe Code Review, Bologna, 19–20 March 2009: organizer
Cappi A.
- Committee for the PhD Thesis of Charline Filloux Evolution des trous noirs supermassifs: simulations cosmologiques, Observatoire de la Côte d’Azur, Nice: member
Clementini G.
- Selection board for a Research grant to work on the Gaia pipeline for the classification
and characterization of Cepheids/RR Lyrae at the OAC Naples: member
Comastri A.
International conference X-ray Astronomy 2009: Present status, multi-wavelength approach and future perspectives, held in Bologna, September 7–11, 2009: SOC Chair
Diolaiti E.
SOC of the conference Adaptive Optics for Extremely Large Telescopes, Paris, 22–26 June
2009: member
- Industrial contract for a mechanical design in the framework of the Phase A Study of
a multi-conjugate adaptive optics module for the European Extremely Large Telescope:
responsible
- Examination committee for the research grant Studio avanzato, ottimizzazione e specifica del sensore di fronte d’onda per il modulo di ottica adattiva multi-coniugata del telescopio E-ELT: member
- Examination committee for the research grant System engineering di un modulo di
ottica adattiva per il futuro European Extremely Large Telescope: member
Tosi M.
- SOC of the IAU Symposium 268: Light Elements in the Universe, held in Geneva (CH)
November 2009: co-chair
- SOC of the Science with the Hubble Space Telescope International Meeting, held in
Venice (It) in October 2010: member
124
13
Seminars of the Astronomical Observatory and
Astronomy Department
Organizers: Bolzonella M., Ettori S.
1. January 15, 2009: Betty De Filippis (University of Napoli – IT)
Dark and visible matter in galaxy clusters: let’s take a closer look
2. January 22, 2009: Paolo Saracco (INAF-OA Brera – IT)
The size evolution of early-type galaxies since z=2: new clues on their formation
and evolution
3. January 29, 2009: Adriano Fontana (INAF-OA Roma – IT)
How do galaxies accrete their mass? Star-forming and quiescent galaxies at high
redshift
4. February 05, 2009: Giuseppe Bianco (Centro di Geodesia Spaziale G. Colombo,
ASI – IT)
Geodynamics: networks, techniques and results
5. February 12, 2009: Piergiorgio Picozza (INFN Roma, University “Tor Vergata” –
IT)
Search for antimatter and dark matter by the PAMELA space mission
6. February 19, 2009: Andrea Viceré (University of Urbino – IT)
The Virgo Detector and the quest for gravitational waves
7. February 26, 2009: Maurizio Salaris (Astrophysics Research Inst., Liverpool John
Moores Univ. – UK)
Cluster ages from white dwarf cosmochronology: techniques and uncertainties
8. March 05, 2009: Giusi Micela (INAF-OA Palermo – IT)
PLATO in the context of the extrasolar planet research
9. March 12, 2009: Mario Di Martino (INAF-OA Torino – IT)
Il rischio asteroidi
10. March 26, 2009: Massimo Turatto (INAF-OA Catania – IT)
The fate of massive stars: theory vs observations
11. April 02, 2009: Daniele Fantin (Nottingham University – IT)
Dark matter on department scale
12. April 16, 2009: Susanna Corti (Institute of Atmospheric Sciences and ClimateCNR Bologna – IT)
Riscaldamento globale e previsioni
13. April 17, 2009: Carlo Burigana (INAF-IASF Bologna – IT)
CMB spectrum: recent results from ARCADE
14. April 23, 2009: Eva Noyola (MPE Garching – DE)
IMBHs in star clusters, are they there?
15. April 27, 2009: Martin Elvis (Harvard-Smithsonian Center for Astrophysics, Cambridge – USA)
Eclipsing in AGN: X-ray Absorption and AGN Structure
16. April 28, 2009: Giuseppina (Pepi) Fabbiano (Harvard-Smithsonian Center for
Astrophysics, Cambridge – USA)
High-resolution X-ray observations of galaxies
17. April 30, 2009: Francesco Shankar (MPA Garching – DE)
Constraining Black Hole and Galaxy Evolution
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18. May 07, 2009: Danilo Marchesini (Astronomy Department, Yale University –
USA)
The Evolution of the Stellar Mass Function of Galaxies from z=4 and the First
Comprehensive Analysis of its Uncertainties: Evidence for Mass-Dependent Evolution
19. May 15, 2009: Martin Feix (SUPA, University of St Andrews – UK)
Gravitational lensing in TeVeS - On filaments, voids and the straight arc
20. May 21, 2009: Emilio Migneco (INFN-LNS Catania – IT)
Neutrini astrofisici di alta energia: verso il telescopio km3 nel Mediterraneo
21. June 04, 2009: Marcella Brusa (MPE Garching – DE)
AGN evolution from large area & deep X-ray surveys: results from COSMOS and
CDFS
22. June 11, 2009: Andrea Veronica Ahumada (ESO & Observatorio Astronomico,
OAC-UNC – AR)
Integrated spectroscopy of stellar clusters
23. June 18, 2009: Marco Baldi (MPA Garching – DE)
Structure formation in presence of dark interactions
24. June 19, 2009: Marcio Catelan (Pontificia Universidad Catolica de Chile – CL)
Horizontal Branch Stars as Astrophysical Probes
25. June 25, 2009: Ramin Skibba (MPIA Heidelberg – DE)
On the Dynamical Behavior of Brightest Halo Galaxies
26. July 02, 2009: Chris Sneden (University of Texas Austin – USA)
Chemical Compositions of Low Metallicity Stars: What We REALLY Know; What
We Hope MIGHT be Right
27. September 15, 2009: Ezequiel Treister (Institute for Astronomy - University of
Hawaii)
Heavily Obscured Supermassive Black Holes
28. September 17, 2009: Marco Prevedelli (University of Bologna – IT)
Orologi atomici nello spazio
29. September 24, 2009: Paolo Ventura (INAF-OA Roma – IT)
Self-enrichment and multiple populations in Globular Clusters
30. October 01, 2009: Nathan Roche (INAF-OA Bologna – IT)
The Colour Magnitude Relation and Colour Gradients of E/S0 Galaxies in the
Sloan Digital Sky Survey
31. October 13, 2009: Licia Verde (Institute of Space Sciences, Barcelona – SP)
Cosmological constraints from the SDSS DR7 halo power spectrum
32. October 15, 2009: Raul Jimenez (Institute of Space Sciences, Barcelona – SP)
The Cosmological Evolution of Galaxies
33. October 22, 2009: Anna Nobili (University of Pisa – IT)
Testing the foundations of General Relativity: the “Galileo Galilei”-GG satellite
experiment
34. November 05, 2009: Antonio Stamerra (University of Siena – IT)
Exploring the frontier of High-Energy Astrophysics with the MAGIC Telescope
35. November 12, 2009: Pablo Mauas (University of Buenos Aires – AR)
Solar Activity and Terrestrial Climate
36. November 19, 2009: Tiziano Valentinuzzi (University of Padova – IT)
Superdense massive galaxies in WINGS local clusters
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37. December 03, 2009: Francesca Matteucci (University of Trieste – IT)
From Chemical Abundances to Formation and Evolution of Galaxies
38. December 10, 2009: Leslie Hunt (INAF-Institute for Radioastronomy, Firenze –
IT)
Star formation at low metallicity
14
“Laurea” thesis
1. Felicia Ziparo, Studio multi-banda di galassie estremamente rosse ad alto redshift
(A. Cimatti, C. Gruppioni), Marzo 2009
2. Carmela Lardo, Definition of Strategy and Procedures for Ground Based Data
Reduction and Gaia’s Absolute Calibration, (F. R. Ferraro, E. Pancinoand G. Altavilla), Maggio 2009
3. Alessia Garofalo, Popolazioni stellari e stelle variabili nella galassia sferoidale
nana Ursa Major I (UMaI) (F. Brighenti, G. Clementini, V. Ripepi), Dicembre
2009
15
PhD theses
1. Rodrigo Contreras, Variable stars in the field and globular clusters of the Andromeda galaxy (M31), XXII cycle (Advisors: B. Marano, G. Clementini)
2. Graziano Coppa, The cosmic mass assembly history of galaxies: a multi-dimensional
study bas ed on deep redshift surveys, XXII cycle (advisors: B. Marano, M.
Mignoli, G. Zamorani)
3. Matteo Correnti, Stellar relics of the hierarchical assembly of the Galaxy, XXII
cycle (advisors: F.R. Ferraro, M. Bellazzini)
4. Annamaria Donnarumma, Testing the consistency of lensing and X-ray mass
estimates in galaxy clusters, XXII cycle (advisors: L. Moscardini, S. Ettori, M.
Meneghetti)
5. Sara Fabbri, Studio della perdita di massa nelle stelle giganti di Popolazione II
con osservazioni SPITZER, XXII cycle (advisors: F.R. Ferraro, L. Origlia, F.
Fusi Pecci)
6. Vincenzo Guido, Development and optimization of graphic user interfaces for
infrared spectr ometers at TNG, XXII cycle (advisors: B. Marano, L. Origlia)
7. Silvia Marinoni, Calibration plan, quality control and optimization of data analysis for red and infrared spectroscopic observations from TNG and other groundbased telesco pes, XXII cycle (advisors: B. Marano, E. Pancino)
8. John Morgan, The application of grid technology to radioastronomy data reduction and ana lysis, XXII cycle (advisors: D. Dallacasa, H.R. de Ruiter)
9. Sibilla Perina, Peculiar star clusters in M31: an HST view, XXII cycle (advisors:
F.R. Ferraro, M. Bellazzini, L. Federici )
10. Cristiano De Boni X-ray properties of galaxy clusters in cosmologies with dynamical dark energy, XXIII cycle (advisors: L. Moscardini, S. Ettori)
11. Matteo Lombini Progetto di un modulo di ottica adattiva multiconiugata per il
telescopio E–ELT, XXIII cycle (advisors: B. Marano, E. Diolaiti)
12. Elisabetta Lusso A panchromatic vew of the evolution of supermassive black
holes, XXIII cycle (advisors: L. Ciotti, A. Comastri)
127
13. Giulia Macario Storia della formazione stellare in galassie risolte, XXIII cycle
(advisors: B. Marano, M. Tosi)
14. Michele Moresco Vincoli sull’energia oscura dalle età di galassie ellittiche, XXIII
cycle (advisors: A. Cimatti, L. Pozzetti)
15. Rashmi Verma Software development to carry out sky surveys with a 20 GHz 7–
horns multibeam, XXIII cycle (advisors: L. Gregorini, I. Prandoni, H. de Ruiter)
16. Fabio Bellagamba Simulazioni realistiche di lensing gravitazionale, XXIV cycle
(advisors: L. Moscardini, M. Meneghetti)
17. Ylenia Maruccia Optimizing the science programmes at ground based optical
large telescopes, XXIV cycle (advisors: B. Marano, V. Zitelli)
18. Maria Ida Moretti Pulsating variable stars as tracers of galactic formation and
interaction mechanisms, XXIV cycle (advisors: B. Marano, G. Clementini)
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Post-Doctoral, Post-Laurea fellowships and Contracts
Altavilla, Giuseppe
Baldi, Alessandro
Cignoni, Michele
Cocozza, Gabriele
Contreras, Rodrigo
Dominguez Sanchez, Helena
Galleti, Silvia
Georgantopoulos, Ioannis
Gitti, Myriam
Iwasawa Kazushi
Lombini, Matteo
Maruccia, Ylenia
Merten, Julian
Nair, Preeti
Perina, Sibilla
Poppi, Francesco
Ragaini, Silvia
Ranalli, Piero
Roche, Nathan
Romano, Donatella
Rossetti, Emanuel
Vergani, Daniela
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