Author: "Mignoli M" / Database: OpenAIRE - Searchworks@Jio Institute Digital Library Search Results

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255 results on '"Mignoli M"'

1. Identifying Ly{\alpha} emitter candidates with Random Forest: learning from galaxies in CANDELS survey

Author: Napolitano, L., Pentericci, L., Calabrò, A., Santini, P., Castellano, M., Cassata, P., Fynbo, J. P. U., Jung, I., Kashino, D., Mascia, S., and Mignoli, M.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The physical processes which make a galaxy a Lyman Alpha Emitter have been extensively studied for the past 25 years. However, the correlations between physical and morphological properties of galaxies and the strength of the Ly$\alpha$ emission line are still highly debated. Therefore, we investigate the correlations between the rest-frame Ly$\alpha$ equivalent width and stellar mass, star formation rate, dust reddening, metallicity, age, half-light semi-major axis, S\'ersic index and projected axis ratio in a sample of 1578 galaxies in the redshift range $2 \leq z \leq 7.9$ from the GOODS-S, UDS and COSMOS fields. From the large sample of Ly$\alpha$ emitters (LAEs) in the dataset we find that LAEs are typically common main sequence star forming galaxies which show stellar mass $ \leq 10^9 \text{M}_{\odot}$, star formation rate $ \leq 10^{0.5} \text{M}_{\odot}/\text{yr}$, $E(B-V) \leq 0.2$ and half-light semi-major axis $\leq 1 \text{kpc}$. Building on these findings we develop a new method based on Random Forest (i.e. a Machine Learning classifier) in order to select galaxies which have the highest probability of being Ly$\alpha$ emitters. When applied to a population in the redshift range $z \in [2.5, 4.5]$, our classifier holds a $(80 \pm 2)\%$ accuracy and $(73 \pm 4)\%$ precision. At higher redshifts ($z \in [4.5, 6]$), we obtain a $73\%$ accuracy and a $80\%$ precision. These results highlight it is possible to overcome the current limitations in assembling large samples of LAEs by making informed predictions that can be used for planning future large scale spectroscopic surveys., Comment: Accepted for publication in the 4. Extragalactic astronomy section of Astronomy & Astrophysics, 13 pages, 13 figures
Published: 2023

2. An extremely metal poor star complex in the reionization era: Approaching Population III stars with JWST

Author: Vanzella, E., Loiacono, F., Bergamini, P., Mestric, U., Castellano, M., Rosati, P., Meneghetti, M., Grillo, C., Calura, F., Mignoli, M., Bradac, M., Adamo, A., Rihtarsic, G., Dickinson, M., Gronke, M., Zanella, A., Annibali, F., Willott, C., Messa, M., Sani, E., Acebron, A., Bolamperti, A., Comastri, A., Gilli, R., Caputi, K. I., Ricotti, M., Gruppioni, C., Ravindranath, S., Mercurio, A., Strait, V., Martis, N., Pascale, R., Caminha, G. B., and Annunziatella, M.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract: We present JWST/NIRSpec integral field spectroscopy (IFS) of a lensed Population III candidate stellar complex (dubbed Lensed And Pristine 1, LAP1), with a lensing-corrected stellar mass ~ -11.2 (m_UV > 35.6), confirmed at redshift 6.639 +/- 0.004. The system is strongly amplified (μ>~ 100) by straddling a critical line of the Hubble Frontier Field galaxy cluster MACS J0416. Despite the stellar continuum is currently not detected in the Hubble and JWST/NIRCam and NIRISS imaging, arclet-like shapes of Lyman and Balmer lines, Lya, Hg, Hb and Ha are detected with NIRSpec IFS with signal-to-noise ratios SNR=5-13 and large equivalent widths (>300-2000A), along with a remarkably weak [OIII]4959-5007 at SNR ~ 4. LAP1 shows a large ionizing photon production efficiency, log(ξ_{ion}[erg~Hz^{-1}])>26. From the metallicity indexes R23 = ([OIII]4959-5007 + [OII]3727) / Hb ~< 0.74 and R3 = ([OIII]5007 / Hb) = 0.55 +/- 0.14, we derive an oxygen abundance 12+log(O/H) ~< 6.3. Intriguingly, the Ha emission is also measured in mirrored sub-components where no [OIII] is detected, providing even more stringent upper limits on the metallicity if in-situ star formation is ongoing in this region (12+log(O/H) < 6, or Z < 0.002 Zsun). The formal stellar mass limit of the sub-components would correspond to ~10^{3} Msun or M_UV fainter than -10. Alternatively, such a metal-free pure line emitting region could be the first case of a fluorescing HI gas region, induced by transverse escaping ionizing radiation from a nearby star-complex. The presence of large equivalent-width hydrogen lines and the deficiency of metal lines in such a small region, make LAP1 the most metal poor star-forming region currently known in the reionization era and a promising site that may host isolated, pristine stars., 15 pages, 10 figures, 1 table. Submitted to A&A. Comments welcome
Published: 2023

3. Optical and mid-infrared line emission in nearby Seyfert galaxies

Author: Feltre, A., Gruppioni, C., Marchetti, L., Mahoro, A., Salvestrini, F., Mignoli, M., Bisigello, L., Calura, F., Charlot, S., Chevallard, J., Romero-Colmenero, E., Curtis-Lake, E., Delvecchio, I., Dors, O. L., Hirschmann, M., Jarrett, T., Marchesi, S., Moloko, M. E., Plat, A., Pozzi, F., Sefako, R., Traina, A., Vaccari, M., Väisänen, P., Vallini, L., Vidal-García, A., and Vignali, C.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract: Line ratio diagnostics provide valuable clues on the source of ionizing radiation in galaxies with intense black hole accretion and starbursting events, such as local Seyfert or galaxies at the peak of the star formation history. We aim to provide a reference joint optical and mid-IR analysis for studying AGN identification via line ratios and testing predictions from photoionization models. We obtained homogenous optical spectra with the Southern Africa Large Telescope for 42 Seyfert galaxies with Spitzer/IRS spectroscopy and X-ray to mid-IR multiband data available. After confirming the power of the main optical ([OIII]) and mid-IR ([NeV], [OIV], [NeIII]) emission lines in tracing AGN activity, we explore diagrams based on ratios of optical and mid-IR lines by exploiting photoionization models of different ionizing sources (AGN, star formation and shocks). We find that pure AGN photoionization models are good at reproducing observations of Seyfert galaxies with an AGN fractional contribution to the mid-IR (5-40 micron) emission larger than 50 per cent. For targets with a lower AGN contribution these same models do not fully reproduce the observed mid-IR line ratios. Mid-IR ratios like [NeV]/[NeII], [OIV]/[NeII] and [NeIII]/[NeII] show a dependence on the AGN fractional contribution to the mid-IR unlike optical line ratios. An additional source of ionization, either from star formation or radiative shocks, can help explain the observations in the mid-IR. Among combinations of optical and mid-IR diagnostics in line ratio diagrams, only those involving the [OI]/Halpha ratio are promising diagnostics for simultaneously unraveling the relative role of AGN, star formation and, shocks. A proper identification of the dominant ionizing source would require the exploitation of analysis tools based on advanced statistical techniques as well as spatially resolved data., 31 pages, 15 figures, 2 tables. Accepted for publication in A&A
Published: 2023

4. The ionizing photon production efficiency of bright z$\sim$2-5 galaxies

Author: Castellano, M., Belfiori, D., Pentericci, L., Calabrò, A., Mascia, S., Napolitano, L., Caro, F., Charlot, S., Chevallard, J., Curtis-Lake, E., Talia, M., Bongiorno, A., Fontana, A., Fynbo, J. P. U., Garilli, B., Guaita, L., McLure, R. J., Merlin, E., Mignoli, M., Moresco, M., Pompei, E., Pozzetti, L., Lopez, A. Saldana, Saxena, A., Santini, P., Schaerer, D., Schreiber, C., Shapley, A. E., Vanzella, E., and Zamorani, G.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract: We investigate the production efficiency of ionizing photons ($\xi_{ion}^*$) of 1174 galaxies with secure redshift at z=2-5 from the VANDELS survey to determine the relation between ionizing emission and physical properties of bright and massive sources. We constrain $\xi_{ion}^*$ and galaxy physical parameters by means of spectro-photometric fits performed with the BEAGLE code. The analysis exploits the multi-band photometry in the VANDELS fields, and the measurement of UV rest-frame emission lines (CIII]$\lambda 1909$, HeII$\lambda 1640$, OIII]$\lambda 1666$) from deep VIMOS spectra. We find no clear evolution of $\xi_{ion}^*$ with redshift within the probed range. The ionizing efficiency slightly increases at fainter $M_{UV}$, and bluer UV slopes, but these trends are less evident when restricting the analysis to a complete subsample at log(M$_{star}$/M$_{\odot}$)$>$9.5. We find a significant trend of increasing $\xi_{ion}^*$ with increasing EW(Ly$\alpha$), with an average log($\xi_{ion}^*$/Hz erg$^{-1}$)$>$25 at EW$>$50\AA, and a higher ionizing efficiency for high-EW CIII]$\lambda 1909$ and OIII]$\lambda 1666$ emitters. The most significant correlations are found with respect to stellar mass, specific star-formation rate (sSFR) and SFR surface density ($\Sigma_{SFR}$). The relation between $\xi_{ion}^*$ and sSFR shows a monotonic increase from log($\xi_{ion}^*$/Hz erg$^{-1}$) $\sim$24.5 at log(sSFR)$\sim$-9.5$yr^{-1}$ to $\sim$25.5 at log(sSFR)$\sim$-7.5$yr^{-1}$, a low scatter and little dependence on mass. The objects above the main-sequence of star-formation consistently have higher-than-average $\xi_{ion}^*$. A clear increase of $\xi_{ion}^*$ with $\Sigma_{SFR}$ is also found, with log($\xi_{ion}^*$/Hz erg$^{-1}$)$>$25 for objects at $\Sigma_{SFR}>$10 M$_{\odot}/yr/kpc^2$.(Abridged), Comment: 11 pages, 9 figures, accepted for publication in A&A
Published: 2023
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5. The VANDELS ESO public spectroscopic survey: Final data release of 2087 spectra and spectroscopic measurements

Author: Garilli, B., McLure, R., Pentericci, L., Franzetti, P., Gargiulo, A., Carnall, A., Cucciati, O., Iovino, A., Amorin, R., Bolzonella, M., Bongiorno, A., Castellano, M., Cimatti, A., Cirasuolo, M., Cullen, F., Dunlop, J., Elbaz, D., Finkelstein, S., Fontana, A., Fontanot, F., Fumana, M., Guaita, L., Hartley, W., Jarvis, M., Juneau, S., Maccagni, D., McLeod, D., Nandra, K., Pompei, E., Pozzetti, L., Scodeggio, M., Talia, M., Cresci, G., Fynbo, J. P. U., Hathi, N. P., Hibon, P., Koekemoer, A. M., Magliocchetti, M., Salvato, M., Vietri, G., Zamorani, G., Almaini, O., Balestra, I., Bardelli, S., Begley, R., Brammer, G., Bell, E. F., Bowler, R. A. A., Brusa, M., Buitrago, F., Caputi, C., Cassata, P., Charlot, S., Citro, A., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G., Ferguson, H. C., Fiore, F., Franco, M., Georgakakis, A., Giavalisco, M., Grazian, A., Hamadouche, M., Jung, I., Kim, S., Khusanova, Y., Longhetti, M., Lotz, J., Mannucci, F., Maltby, D., Matsuoka, K., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Roberts-Borsani, G., Rosario, D. J., Saldana-Lopez, A., Santini, P., Saxena, A., Schaerer, D., Schreiber, C., Stark, D., Tasca, L. A. M., Thomas, R., Vanzella, E., Wild, V., Williams, C., and Zucca, E.
Subjects: Space and Planetary Science, Astronomy and Astrophysics
Published: 2021

6. The VANDELS ESO public spectroscopic survey

Author: Garilli, B., Mclure, R., Pentericci, L., Franzetti, P., Gargiulo, A., Carnall, A., Cucciati, O., Iovino, A., Amorin, R., Bolzonella, M., Bongiorno, A., Castellano, M., Cimatti, A., Cirasuolo, M., Cullen, F., Dunlop, J., Elbaz, D., Finkelstein, S., Fontana, A., Fontanot, F., Fumana, M., Guaita, L., Hartley, W., Jarvis, M., Juneau, S., Maccagni, D., Mcleod, D., Nandra, K., Pompei, E., Pozzetti, L., Scodeggio, M., Talia, M., Calabrò, A., Cresci, G., Fynbo, J., Hathi, N., Hibon, P., Koekemoer, A., Magliocchetti, M., Salvato, M., Vietri, G., Zamorani, G., Almaini, O., Balestra, I., Bardelli, S., Begley, R., Brammer, G., Bell, E., Bowler, R., Brusa, M., Buitrago, F., Caputi, C., Cassata, P., Charlot, S., Citro, A., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G., Ferguson, H., Fiore, F., Franco, M., Georgakakis, A., Giavalisco, M., Grazian, A., Hamadouche, M., Jung, I., Kim, S., Khusanova, Y., Le Fèvre, O., Longhetti, M., Lotz, J., Mannucci, F., Maltby, D., Matsuoka, K., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Roberts-Borsani, G., Rosario, D., Saldana-Lopez, A., Santini, P., Saxena, A., Schaerer, D., Schreiber, C., Stark, D., Tasca, L., Thomas, R., Vanzella, E., Wild, V., Williams, C., Zucca, E., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS]Physics [physics], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], surveys, cosmology: observations, galaxies: fundamental parameters, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: distances and redshifts, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: statistics, catalogs, Astrophysics::Galaxy Astrophysics
Abstract: International audience; VANDELS is an ESO Public Spectroscopic Survey designed to build a sample of high-signal-to-noise ratio, medium-resolution spectra of galaxies at redshifts between 1 and 6.5. Here we present the final Public Data Release of the VANDELS Survey, comprising 2087 redshift measurements. We provide a detailed description of sample selection, observations, and data reduction procedures. The final catalogue reaches a target selection completeness of 40% at i AB = 25. The high signal-to-noise ratio of the spectra (above 7 in 80% of the spectra) and the dispersion of 2.5 Å allowed us to measure redshifts with high precision, the redshift measurement success rate reaching almost 100%. Together with the redshift catalogue and the reduced spectra, we also provide optical mid-infrared photometry and physical parameters derived through fitting the spectral energy distribution. The observed galaxy sample comprises both passive and star forming galaxies covering a stellar mass range of 8.3 < Log( M * / M ⊙ ) < 11.7.
Published: 2021
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7. The MUSE Deep Lensed Field on the Hubble Frontier Field MACS~J0416

Author: Vanzella, E., Caminha, G. B., Rosati, P., Mercurio, A., Castellano, M., Meneghetti, M., Grillo, C., Sani, E., Bergamini, P., Calura, F., Caputi, K., Cristiani, S., Cupani, G., Fontana, A., Gilli, R., Grazian, A., Gronke, M., Mignoli, M., Nonino, M., Pentericci, L., Tozzi, P., Treu, T., Balestra, I., and Dijkstra, M.
Subjects: Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: Context: A census of faint and tiny star forming complexes at high redshift is key to improving our understanding of reionizing sources, galaxy growth and the formation of globular clusters. Aims: We present the MUSE Deep Lensed Field (MDLF) program. Methods: We describe Deep MUSE observations of 17.1 hours integration on a single pointing over the Hubble Frontier Field galaxy cluster MACS~J0416. Results: We confirm spectroscopic redshifts for all 136 multiple images of 48 source galaxies at 0.910 for individual objects down to de-lensed magnitude 28-30 suggesting that they are common in such faint sources. Conclusions:Deep MUSE observations, in combination with existing HST imaging, allowed us to:(1) confirm redshifts for extremely faint high-z sources;(2) peer into their internal clumps (down to 100-200 pc scale);(3) in some cases break down such clumps into bound star clusters (, Comment: 43 pages total (17 pages main body); 5 appendices. Accepted for publication in A&A on October 26
Published: 2020

8. Obscured AGN at 1.5 < z < 3.0 from the zCOSMOS-deep Survey

Author: Mignoli, M., Feltre, A., Bongiorno, A., Calura, F., Gilli, R., Vignali, C., Zamorani, G., Lilly, S. J., Le Fèvre, O., Bardelli, S., Bolzonella, M., Bordoloi, R., Le Brun, V., Caputi, K. I., Cimatti, A., Diener, C., Garilli, B., Koekemoer, A. M., Maier, C., Mainieri, V., Peng, Y., Pérez Montero, E., Silverman, J. D., Zucca, E., Mignoli, M., Feltre, A., Bongiorno, A., Calura, F., Gilli, R., Vignali, C., Zamorani, G., Lilly, S. J., Le Fèvre, O., Bardelli, S., Bolzonella, M., Bordoloi, R., Le Brun, V., Caputi, K. I., Cimatti, A., Diener, C., Garilli, B., Koekemoer, A. M., Maier, C., Mainieri, V., Peng, Y., Pérez Montero, E., Silverman, J. D., and Zucca, E.
Subjects: galaxies: active, line: formation, galaxies: evolution, galaxies: fundamental parameter, quasars: emission line, X-rays: galaxie
Abstract: Context. The physics and demographics of high-redshift obscured active galactic nuclei (AGN) is still scarcely investigated. New samples of such objects, selected with different techniques, can provide useful insights into their physical properties.Aims. With the goal to determine the properties of the gas in the emitting region of type 2 AGN, in particular, the gas metal content, we exploit predictions from photoionization models, including new parameterizations for the distance of gas distribution from the central source and internal microturbulence in the emitting clouds, to interpret rest-frame UV spectral data.Methods. We selected a sample of 90 obscured (type 2) AGN with 1.45
Published: 2019

9. The deep Chandra survey in the SDSS J1030+0524 field

Author: Nanni, R., Gilli, R., Vignali, Cristian, Mignoli, M., Peca, A., Marchesi, Stefano, Annunziatella, M., Brusa, M., Calura, F., Cappelluti, N., Chiaberge, Marco, Comastri, A., Iwasawa, K., Lanzuisi, G., Liuzzo, E., Marchesini, D., Prandoni, I., Zamorani, G., Norman, Colin, National Aeronautics and Space Administration (US), Tufts University, and Comisión Nacional de Investigación Científica y Tecnológica (Chile)
Subjects: Supermassive black holes, X-rays, High-redshift, Surveys, Catalogues, Galaxies, General, Quasars
Abstract: We present the X-ray source catalog for the ∼479 ks Chandra exposure of the SDSS J1030+0524 field, which is centered on a region that shows the best evidence to date of an overdensity around a z > 6 quasar, and also includes a galaxy overdensity around a Compton-thick Fanaroff-Riley type II (FRII) radio galaxy at z = 1.7. Using wavdetect for initial source detection and ACIS Extract for source photometry and significance assessment, we create preliminary catalogs of sources that are detected in the full (0.5-7.0 keV), soft (0.5-2.0 keV), and hard (2-7 keV) bands, respectively. We produce X-ray simulations that mirror our Chandra observation to filter our preliminary catalogs and achieve a completeness level of > 91% and a reliability level of ∼95% in each band. The catalogs in the three bands are then matched into a final main catalog of 256 unique sources. Among them, 244, 193, and 208 are detected in the full, soft, and hard bands, respectively. The Chandra observation covers a total area of 335 arcmin2 and reaches flux limits over the central few square arcmins of ∼3 × 10-16, 6 × 10-17, and 2 × 10-16 erg cm-2 s-1 in the full, soft, and hard bands, respectively This makes J1030 field the fifth deepest extragalactic X-ray survey to date. The field is part of the Multiwavelength Survey by Yale-Chile (MUSYC), and is also covered by optical imaging data from the Large Binocular Camera (LBC) at the Large Binocular Telescope (LBT), near-infrared imaging data from the Canada France Hawaii Telescope WIRCam (CFHT/WIRCam), and Spitzer IRAC. Thanks to its dense multi-wavelength coverage, J1030 represents a legacy field for the study of large-scale structures around distant accreting supermassive black holes. Using a likelihood ratio analysis, we associate multi-band (r, z, J, and 4.5 μm) counterparts for 252 (98.4%) of the 256 Chandra sources, with an estimated reliability of 95%. Finally, we compute the cumulative number of sources in each X-ray band, finding that they are in general agreement with the results from the Chandra Deep Fields. We acknowledge the referee for a prompt and constructive report. We acknowledge financial contribution from the agreement ASI-INAF n. 2017-14-H.O. We thank P. Broos for providing great support for the analysis of our simulations with AE, and H. M. Günther for the support provided for using MARX. We also thank B. Luo for providing us the log(N)–log(S) of the 7Ms CDF-S. FV acknowledges financial support from CONICYT and CASSACA through the Fourth call for tenders of the CAS-CONICYT Fund, and CONICYT grants Basal-CATA AFB-170002. DM and MA acknowledge support by grant number NNX16AN49G issued through the NASA Astrophysics Data Analysis Program (ADAP). Further support was provided by the Faculty Research Fund (FRF) of Tufts University.
Published: 2020

10. Discovery of molecular gas fueling galaxy growth in a protocluster at z=1.7

Author: D'Amato, Q., Gilli, R., Prandoni, I., Vignali, C., Massardi, M., Mignoli, M., Cucciati, O., Morishita, T., Decarli, R., Brusa, M., Calura, F., Balmaverde, B., Chiaberge, M., Liuzzo, E., Nanni, R., Peca, A., Pensabene, A., Tozzi, P., and Norman, C.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: Based on ALMA Band 3 observations of the CO(2-1) line transition, we report the discovery of three new gas-rich (M_H2 ~ 1.5-4.8 x 10^10 M_sun, SFRs in the range ~5-100 M_sun/yr) galaxies in an overdense region at z=1.7, that already contains eight spectroscopically confirmed members. This leads to a total of 11 confirmed overdensity members, within a projected distance of ~ 1.15 Mpc and in a redshift range of Dz = 0.012. Under simple assumptions, we estimate that the system has a total mass of >= 3-6 x 10^13 M_sun, and show that it will likely evolve into a >~ 10^14 M_sun cluster at z = 0. The overdensity includes a powerful Compton-thick Fanaroff-Riley type II (FRII) radio-galaxy, around which we discovered a large molecular gas reservoir (M_H2 ~ 2 x 10^11 M_sun). We fitted the FRII resolved CO emission with a 2-D Gaussian model with major (minor) axis of ~ 27 (~ 17) kpc, that is a factor of ~3 larger than the optical rest-frame emission. Under the assumption of a simple edge-on disk morphology, we find that the galaxy interstellar medium produces a column density towards the nucleus of ~ 5.5 x 10^23 cm^-2. Such a dense ISM may then contribute significantly to the total nuclear obscuration measured in the X-rays (N_(H,X) ~ 1.5 x 10^24 cm^-2) in addition to a small, pc-scale absorber around the central engine. The velocity map of this source unveils a rotational motion of the gas that is perpendicular to the radio-jets. The FRII is located at the center of the projected spatial distribution of the structure members, and its velocity offset from the peak of the redshift distribution is well within the structure's velocity dispersion. All this, coupled with the large amount of gas around the FRII, its stellar mass of ~ 3 x 10^11 M_sun, SFR of ~ 200-600 M_sun/yr, and powerful radio-to-X-ray emission, suggests that this source is the likely progenitor of the future brightest cluster galaxy., 7 pages, 4 figures, 2 tables. Accepted for publication as a Letter in A&A
Published: 2020
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11. Obscured AGN at 1.5 < z < 3.0 from the zCOSMOS-deep Survey I. Properties of the emitting gas in the Narrow Line Region

Author: Mignoli, M., Feltre, A., Bongiorno, A., Calura, F., Gilli, R., Vignali, C., Zamorani, G., Lilly, S. J., Fevre, O. Le, Bardelli, S., Bolzonella, M., Bordoloi, R., Brun, V. Le, Caputi, K. I., Cimatti, A., Diener, C., Garilli, B., Koekemoer, A. M., Maier, C., Mainieri, V., Peng, Y., Montero, E. Perez, Silverman, J. D., and Zucca, E.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences
Abstract: We select a sample of 90 obscured (type2) AGN with 1.45, 14 pages, 7 figures. Paper accepted in Astronomy and Astrophysics, electronic data will be available on CDS
Published: 2019
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12. The X-Ray Properties Of Z~6 Quasars

Author: Nanni, Riccardo, Gilli, R., Vignali, C., Mignoli, M., Balmaverde, B., and Vito, F.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, X-rays, Active Galactic Nuclei, Astrophysics::Cosmology and Extragalactic Astrophysics, AGN, high-redshift quasars, Astrophysics::Galaxy Astrophysics
Abstract: More than 200 quasars (QSOs) with spectroscopic redshift z > 6 have been discovered so far. Multi-wavelength observations showed that these QSOs are evolved systems with large black hole masses (108−10M⊙), and their broad-band spectral energy distributions (SEDs) and rest-frame NIR/optical/UV spectra have not significantly evolved over cosmic time. The formation of their Super Massive Black Holes in less than 1 Gyr is still a challenge for theory, with many simulations claiming they formed at the center of primordial overdense regions. I report the study of all the 29 z∼6 QSOs observed so far with X-rays, in which our group concluded that the X-ray spectral properties of high-z QSOs do not differ significantly from those of QSOs at lower-z. We also obtained a deep 500 ks Chandra observation to study the environment around the QSO J1030+0524, which shows the best evidence of an overdense region around a z∼6 QSO. This is the deepest X-ray observation ever achieved for a z∼6 QSO. Comparing our results with those from previous XMM observation we found a hardening of the X-ray spectrum and a decrease of the flux by a factor 2.5. This is the first evidence of a variable QSO at such high redshift. I also report the discovery of a diffuse X-ray emission southward the QSO, that could be linked to the feedback of the AGN.
Published: 2018
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13. Obscured Agn In The Field Of J1030: The X-Ray And Optical/Infrared Perspective

Author: Peca, Alessandro, Vignali, C., Gilli, R., and Mignoli, M.
Subjects: X-ray, Astrophysics::High Energy Astrophysical Phenomena, Active Galactic Nuclei, Astrophysics::Cosmology and Extragalactic Astrophysics, AGN, Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: Deep X surveys are an essential tool for the study of obscured AGN. These objects are very faint even in the X-ray band, due to the large column densities responsible for the obscuration. We studied obscured AGN candidates in the deep field around the z=6.31 QSO SDSS J1030+0524. The goal of this project is the selection and characterization of obscured AGN using a multi-wavelength approach. We used X-ray spectral features such as 6.4 keV Fe line or Fe absorption edge to estimate the still unknown redshift of these sources from the X-ray band, and compared the results with the outcomes of a standard SED-fitting procedure (hyperz code, Bolzonella+00) using optical/NIR/MIR photometry. The obtained results show the possibility to use X-ray spectra in support in the search for redshift of obscured AGN.
Published: 2018
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14. The J1030 deep survey

Author: Gilli, Roberto, Mignoli, M., Nanni, R., Balmaverde, B., Brusa, M., Calura, F., Caminha, G. B., Cappelluti, N., Cappi, M., Chiaberge, M., Comastri, A., Costa, T., D'Amato, Q., Decarli, R., Iwasawa, K., Lanzuisi, G., Liuzzo, E., Norman, C., Paolillo, M., Peca, A., Prandoni, I., Risaliti, G., Rosati, P., Sani, E., Tozzi, P., Vanzella, E., Vignali, C., Vito, F., and Zamorani, G.
Subjects: high-redshift Universe, Astrophysics::High Energy Astrophysical Phenomena, Active Galactic Nuclei, Astrophysics::Cosmology and Extragalactic Astrophysics, AGN, deep surveys, Astrophysics::Galaxy Astrophysics
Abstract: We report on the status of on-going, deep multi-band observations inthe field around the z=6.31 QSO SDSS J1030+0524, where an overdensityof candidate Lyman Break Galaxies at the QSO redshift was found. Theobservations include a large program with Chandra, deep JVLAobservations, and a strategic LBT program for opticalspectroscopy.Additional imaging and spectroscopic coverage isprovided, among others, by HST, VLT/MUSE, Keck and Spitzer data. The J1030 field is currently the 4th deepest X-ray survey, one of thefew radio fields observed at microJy depth, and the only deepmulti-bandsurvey in a highly biased region of the early Universe. We are collecting and organizing all multi-band data in a publicdatabase that can be effectively exploited by the AGN community. Examples of preliminary results from these data include: i) the firstspectroscopic confirmation of a few galaxies at the redshift of SDSSJ1030+0524, and ii) the discovery of a proto-cluster at z=1.7 around aCompton-thick FRII radio-galaxy.
Published: 2018
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15. The VANDELS ESO public spectroscopic survey

Author: McLure, R.J., Pentericci, L., Cimatti, A., Dunlop, J.S., Elbaz, D., Fontana, A., Nandra, K., Amorin, R., Bolzonella, M., Bongiorno, A., Carnall, A.C., Castellano, M., Cirasuolo, M., Cucciati, O., Cullen, F., De Barros, S., Finkelstein, S.L., Fontanot, F., Franzetti, P., Fumana, M., Gargiulo, A., Garilli, B., Guaita, L., Hartley, W.G., Iovino, A., Jarvis, M.J., Juneau, S., Karman, W., Maccagni, D., Marchi, F., Pompei, E., Pozzetti, L., Scodeggio, M., Sommariva, V., Talia, M., Almaini, Omar, Balestra, I., Bardelli, S., Bell, E.F., Bourne, N., Bowler, R.A.A., Brusa, M., Buitrago, F., Caputi, K.I., Cassata, P., Charlot, S., Citro, A., Cresci, G., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G.G., Ferguson, H.C., Fiore, F., Franco, M., Fynbo, J P U, Galametz, A., Georgakakis, A., Giavalisco, M., Grazian, A., Hathi, N.P., Jung, I., Kim, S., Koekemoer, A.M., Khusanova, Y., Lotz, J.M., Mannucci, F., Maltby, David T., Matsuoka, K., McLeod, D.J., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Mortlock, A., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Rosario, D.P., Salvato, M., Santini, P., Schaerer, D., Schreiber, C., Stark, D.P., Tasca, L.A.M., Thomas, R., Treu, T., Vanzella, E., Wild, V., Williams, C.C., Zamorani, G., and Zucca, E.
Subjects: surveys, galaxies: high-redshift, galaxies: star formation, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract: VANDELS is a uniquely deep spectroscopic survey of high-redshift galaxies with the VIMOS spectrograph on ESO’s Very Large Telescope (VLT). The survey has obtained ultradeep optical (0.48 < λ < 1.0 μm) spectroscopy of ≃2100 galaxies within the redshift interval 1.0 ≤ z ≤ 7.0, over a total area of ≃0.2 deg2 centred on the CANDELS Ultra Deep Survey and Chandra Deep Field South fields. Based on accurate photometric redshift pre-selection, 85 per cent of the galaxies targeted by VANDELS were selected to be at z ≥ 3. Exploiting the red sensitivity of the refurbished VIMOS spectrograph, the fundamental aim of the survey is to provide the high-signal-to-noise ratio spectra necessary to measure key physical properties such as stellar population ages, masses, metallicities, and outflow velocities from detailed absorption-line studies. Using integration times calculated to produce an approximately constant signal-to-noise ratio (20 < tint< 80 h), the VANDELS survey targeted: (a) bright star-forming galaxies at 2.4 ≤ z ≤ 5.5, (b) massive quiescent galaxies at 1.0 ≤ z ≤ 2.5, (c) fainter star-forming galaxies at 3.0 ≤ z ≤ 7.0, and (d) X-ray/Spitzer-selected active galactic nuclei and Herschel-detected galaxies. By targeting two extragalactic survey fields with superb multiwavelength imaging data, VANDELS will produce a unique legacy data set for exploring the physics underpinning high-redshift galaxy evolution. In this paper, we provide an overview of the VANDELS survey designed to support the science exploitation of the first ESO public data release, focusing on the scientific motivation, survey design, and target selection.
Published: 2018

16. The VANDELS ESO public spectroscopic survey: Observations and first data release

Author: Pentericci, L., McLure, R. J., Garilli, B., Cucciati, O., Franzetti, P., Iovino, A., Amorin, R., Bolzonella, M., Bongiorno, A., Carnall, A. C., Castellano, M., Cimatti, A., Cirasuolo, M., Cullen, F., De Barros, S., Dunlop, J. S., Elbaz, D., Finkelstein, S. L., Fontana, A., Fontanot, F., Fumana, M., Gargiulo, A., Guaita, L., Hartley, W. G., Jarvis, M. J., Juneau, S., Karman, W., Maccagni, D., Marchi, F., Marmol-Queralto, E., Nandra, K., Pompei, E., Pozzetti, L., Scodeggio, M., Sommariva, V., Talia, M., Almaini, O., Balestra, I., Bardelli, S., Bell, E. F., Bourne, N., Bowler, R. A. A., Brusa, M., Buitrago, F., Caputi, K. I., Cassata, P., Charlot, S., Citro, A., Cresci, G., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G. G., Ferguson, H. C., Fiore, F., Franco, M., Fynbo, J. P. U., Galametz, A., Georgakakis, A., Giavalisco, M., Grazian, A., Hathi, N. P., Jung, I., Kim, S., Koekemoer, A. M., Khusanova, Y., Lotz, J. M., Mannucci, F., Maltby, D. T., Matsuoka, K., McLeod, D. J., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Mortlock, A., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Rosario, D. P., Salvato, M., Santini, P., Schaerer, D., Schreiber, C., Stark, D. P., Tasca, L. A. M., Thomas, R., Treu, T., Vanzella, E., Wild, V., Williams, C. C., Zamorani, G., and Zucca, E.
Subjects: surveys – galaxies: general – galaxies: evolution – galaxies: high-redshift – galaxies: fundamental parameters, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: © ESO 2018. This paper describes the observations and the first data release (DR1) of the ESO public spectroscopic survey "VANDELS, a deep VIMOS survey of the CANDELS CDFS and UDS fields". The main targets of VANDELS are star-forming galaxies at redshift 2.4 < z < 5.5, an epoch when the Universe had not yet reached 20% of its current age, and massive passive galaxies in the range 1 < z < 2.5. By adopting a strategy of ultra-long exposure times, ranging from a minimum of 20 h to a maximum of 80 h per source, VANDELS is specifically designed to be the deepest-ever spectroscopic survey of the high-redshift Universe. Exploiting the red sensitivity of the refurbished VIMOS spectrograph, the survey is obtaining ultra-deep optical spectroscopy covering the wavelength range 4800-10 000 Å with a sufficiently high signal-to-noise ratio to investigate the astrophysics of high-redshift galaxy evolution via detailed absorption line studies of well-defined samples of high-redshift galaxies. VANDELS-DR1 is the release of all medium-resolution spectroscopic data obtained during the first season of observations, on a 0.2 square degree area centered around the CANDELS-CDFS (Chandra deep-field south) and CANDELS-UDS (ultra-deep survey) areas. It includes data for all galaxies for which the total (or half of the total) scheduled integration time was completed. The DR1 contains 879 individual objects, approximately half in each of the two fields, that have a measured redshift, with the highest reliable redshifts reaching zspec ∼ 6. In DR1 we include fully wavelength-calibrated and flux-calibrated 1D spectra, the associated error spectrum and sky spectrum, and the associated wavelength-calibrated 2D spectra. We also provide a catalog with the essential galaxy parameters, including spectroscopic redshifts and redshift quality flags measured by the collaboration. We present the survey layout and observations, the data reduction and redshift measurement procedure, and the general properties of the VANDELS-DR1 sample. In particular, we discuss the spectroscopic redshift distribution and the accuracy of the photometricredshifts for each individual target category, and we provide some examples of data products for the various target typesand the different quality flags. All VANDELS-DR1 data are publicly available and can be retrieved from the ESO archive. Two further data releases are foreseen in the next two years, and a final data release is currently scheduled for June 2020, which will include an improved rereduction of the entire spectroscopic data set.
Published: 2018

17. The VANDELS ESO spectroscopic survey

Author: McLure, R. J., Pentericci, L., Cimatti, A., Dunlop, J. S., Elbaz, D., Fontana, A., Nandra, K., Amorin, R., Bolzonella, M., Bongiorno, A., Carnall, A. C., Castellano, M., Cirasuolo, M., Cucciati, O., Cullen, F., De Barros, S., Finkelstein, S. L., Fontanot, F., Franzetti, P., Fumana, M., Gargiulo, A., Garilli, B., Guaita, L., Hartley, W. G., Iovino, A., Jarvis, M. J., Juneau, S., Karman, W., Maccagni, D., Marchi, F., Mármol-Queraltó, E., Pompei, E., Pozzetti, L., Scodeggio, M., Sommariva, V., Talia, M., Almaini, O., Balestra, I., Bardelli, S., Bell, E. F., Bourne, N., Bowler, R. A. A., Brusa, M., Buitrago, F., Caputi, K. I., Cassata, P., Charlot, S., Citro, A., Cresci, G., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G. G., Ferguson, H. C., Fiore, F., Franco, M., Fynbo, J. P. U., Galametz, A., Georgakakis, A., Giavalisco, M., Grazian, A., Hathi, N. P., Jung, I., Kim, S., Koekemoer, A. M., Khusanova, Y., Le Fèvre, O., Lotz, J. M., Mannucci, F., Maltby, D. T., Matsuoka, K., McLeod, D. J., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Mortlock, A., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Rosario, D. P., Salvato, M., Santini, P., Schaerer, D., Schreiber, C., Stark, D. P., Tasca, L. A. M., Thomas, R., Treu, T., Vanzella, E., Wild, V., Williams, C. C., Zamorani, G., Zucca, E., and University of St Andrews. School of Physics and Astronomy
Subjects: high-redshift [Galaxies], QC Physics, NDAS, Astrophysics::Solar and Stellar Astrophysics, QB Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, evolution [Galaxies], star formation [Galaxies], Astrophysics::Galaxy Astrophysics, QC, QB
Abstract: VANDELS is a uniquely-deep spectroscopic survey of high-redshift galaxies with the VIMOS spectrograph on ESO’s Very Large Telescope (VLT). The survey has obtained ultra-deep optical (0.48 < λ < 1.0 μm) spectroscopy of ≃2100 galaxies within the redshift interval 1.0 ≤ z ≤ 7.0, over a total area of ≃ 0.2 deg2 centred on the CANDELS UDS and CDFS fields. Based on accurate photometric redshift pre-selection, 85% of the galaxies targeted by VANDELS were selected to be at z ≥ 3. Exploiting the red sensitivity of the refurbished VIMOS spectrograph, the fundamental aim of the survey is to provide the high signal-to-noise ratio spectra necessary to measure key physical properties such as stellar population ages, masses, metallicities and outflow velocities from detailed absorption-line studies. Using integration times calculated to produce an approximately constant signal-to-noise ratio (20 < tint < 80 hours), the VANDELS survey targeted: a) bright star-forming galaxies at 2.4 ≤ z ≤ 5.5, b) massive quiescent galaxies at 1.0 ≤ z ≤ 2.5, c) fainter star-forming galaxies at 3.0 ≤ z ≤ 7.0 and d) X-ray/Spitzer-selected active galactic nuclei and Herschel-detected galaxies. By targeting two extragalactic survey fields with superb multi-wavelength imaging data, VANDELS will produce a unique legacy data set for exploring the physics underpinning high-redshift galaxy evolution. In this paper we provide an overview of the VANDELS survey designed to support the science exploitation of the first ESO public data release, focusing on the scientific motivation, survey design and target selection. Postprint
Published: 2018

18. PNe and H II regions in the starburst irregular galaxy NGC 4449 from LBT MODS data

Author: Annibali, F., Tosi, M., Romano, D., Buzzoni, A., Cusano, F., Fumana, M., Marchetti, A., Mignoli, M., Pasquali, A., and Aloisi, A.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract: We present deep 3500$-$10000 $\AA$ spectra of H II regions and planetary nebulae (PNe) in the starburst irregular galaxy NGC 4449, acquired with the Multi Object Double Spectrograph at the Large Binocular Telescope. Using the "direct" method, we derived the abundance of He, N, O, Ne, Ar, and S in six H II regions and in four PNe in NGC 4449. This is the first case of PNe studied in a starburst irregular outside the Local Group. Our H II region and PN sample extends over a galacto-centric distance range of $\approx$2 kpc and spans $\approx$0.2 dex in oxygen abundance, with average values of $12+\log(O/H)=8.37 \pm 0.05$ and $8.3 \pm 0.1$ for H II regions and PNe, respectively. PNe and H II regions exhibit similar oxygen abundances in the galacto-centric distance range of overlap, while PNe appear more than $\sim$1 dex enhanced in nitrogen with respect to H II regions. The latter result is the natural consequence of N being mostly synthesized in intermediate-mass stars and brought to the stellar surface during dredge-up episodes. On the other hand, the similarity in O abundance between H II regions and PNe suggests that NGC 4449' s interstellar medium has been poorly enriched in $\alpha$ elements since the progenitors of the PNe were formed. Finally, our data reveal the presence of a negative oxygen gradient for both H II regions and PNe, whilst nitrogen does not exhibit any significant radial trend. We ascribe the (unexpected) nitrogen behaviour as due to local N enrichment by the conspicuous Wolf-Rayet population in NGC 4449., Comment: Accepted for publication on ApJ
Published: 2017

19. Ultraviolet/optical emission of the ionised gas in AGN: diagnostics of the ionizing source and gas properties

Author: Feltre Anna, Charlot S., Plat A., Curtis-Lake E., Mignoli M., Calura F., Bongiorno A., Chevallard J., and Bacon R.
Subjects: High z, AGN, Quasars, Type 2, NLR
Abstract: High quality spectroscopic study of the NLR properties of high z (1.5-3) type 2 AGN.
Published: 2017
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20. The zCOSMOS survey

Author: Zucca E., Bardelli S., Bolzonella M., Zamorani G., Ilbert O., Pozzetti L., Mignoli M., Kova, #269, Lilly S., Tresse L., Tasca L., Cassata P., 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., 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., Perez Montero E., Ricciardelli E., Silverman J. D., Tanaka M., Abbas U., Bottini D., Cappi A., Guzzo L., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Meme, P., Meneux B., Oesch P., Porciani C., Scaramella R., Arnouts S., Aussel H., Capak P., Kartaltepe J., Salvato M., Sanders D., Scoville N., Taniguchi Y., Thompson D., CUCCIATI, OLGA, CIMATTI, ANDREA, MORESCO, MICHELE ENNIO MARIA, INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Bologna (OABO), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), AUTRES, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), University of Chicago, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), INAF- Milano, Dipartimento di Fisica, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Tokai University, Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Space Telescope Science Institute (STSci), Centre de Physique Théorique - UMR 6207 (CPT), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Materials & Process technology, Boeing Company [Chicago], California Institute of Technology (CALTECH), Sea Mammal Research Unit, St Andrews, Astronomy, Zucca E., Bardelli S., Bolzonella M., Zamorani G., Ilbert O., Pozzetti L., Mignoli M., Kova&#269, K., Lilly S., Tresse L., Tasca L., Cassata P., 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., Perez-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., Meme, 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., Università di Bologna, Dipartimento di Astronomia, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: Normalization (statistics), Cosmology and Nongalactic Astrophysics (astro-ph.CO), High density, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, 01 natural sciences, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], MORPHOLOGICAL CLASSIFICATION, 1ST EPOCH DATA, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Density field, FIELD, 10. No inequality, 010303 astronomy & astrophysics, PHOTOMETRIC REDSHIFTS, Astrophysics::Galaxy Astrophysics, galaxies: statistics, Luminosity function (astronomy), Physics, REDSHIFT SURVEY, LEGACY SURVEY, 010308 nuclear & particles physics, Galaxies: evolution, Galaxies: luminosity function, mass function, Galaxies: statistics, Astronomy and Astrophysics, Space and Planetary Science, VLT DEEP SURVEY, B band, Galaxy, galaxies: luminosity function, mass function, COLOR-DENSITY RELATION, galaxies: luminosity function, mass function, DIGITAL SKY SURVEY, galaxies: evolution, Cosmic time, SURVEY COSMOS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: (Abridged) We studied the evolution in the B band luminosity function to z~1 in the zCOSMOS 10k sample, for which both accurate galaxy classifications and a detailed description of the local density field are available. The global LF exhibits a brightening of ~0.7 mag in M* from z~0.2 to z~0.9. At low z, late types dominate at faint magnitudes, while the bright end is populated mainly by early types. At higher z, late-type galaxies evolve significantly and, at z~1, the contribution from the various types to the bright end of the LF 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. Studying the role of the environment, we find that the global LF of galaxies in overdense regions has always a brighter M* and a flatter slope. In low density environments, the main contribution to the LF is from blue galaxies, while for high density environments there is an important contribution from red galaxies to the bright end. The differences between the global LF in the two environments are not due to only a difference in the relative numbers of red and blue galaxies, but also to their relative luminosity distributions: the value of M* for both types in underdense regions is always fainter than in overdense environments. The "specular" evolution of late- and early-type galaxies is consistent with a scenario where a part of blue galaxies is transformed in 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., Comment: 18 pages, 10 figures, A&A in press
Published: 2009
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21. Passive galaxies as tracers of cluster environments at z similar to 2

Author: Strazzullo, V, Daddi, E, Gobat, R, Garilli, B, Mignoli, M, Valentino, F, Onodera, M, Renzini, A, Cimatti, A, Finoguenov, A, Arimoto, N, Cappellari, M, Carollo, Cm, Feruglio, C, Le Floc'h, E, Lilly, Sj, Maccagni, D, Mccracken, Hj, Moresco, M, Pozzetti, L, Zamorani, G, Strazzullo, V, Daddi, E, Gobat, R, Garilli, B, Mignoli, M, Valentino, F, Onodera, M, Renzini, A, Cimatti, A, Finoguenov, A, Arimoto, N, Cappellari, M, Carollo, Cm, Feruglio, C, Le Floc'h, E, Lilly, Sj, Maccagni, D, Mccracken, Hj, Moresco, M, Pozzetti, L, and Zamorani, G
Abstract: Even 10 billion years ago, the cores of the first galaxy clusters are often found to host a characteristic population of massive galaxies with already suppressed star formation. Here we search for distant cluster candidates at z similar to 2 using massive passive galaxies as tracers. With a sample of similar to 40 spectroscopically confirmed passive galaxies at 1.3 < z < 2.1, we tuned photometric redshifts of several thousand passive sources in the 2 sq. deg COSMOS field. This allowed us to map their density in redshift slices, probing the largescale structure in the COSMOS field as traced by passive sources. We report here on the three strongest passive galaxy overdensities that we identify in the range 1.5 < z < 2.5. While the actual nature of these concentrations still needs to be confirmed, we discuss their identification procedure and the arguments supporting them as candidate galaxy clusters (probably in the mid-10(13) M-circle dot range). Although this search approach is probably biased toward more evolved structures, it has the potential of selecting still rare, clusterlike environments close to their epoch of first appearance, enabling new investigations of the evolution of galaxies in the context of structure growth.
Published: 2015

22. VizieR Online Data Catalog: COSMOS photometric redshift catalog (Ilbert+, 2009)

Author: Ilbert, O., Capak, P., Salvato, M., Aussel, H., Mccracken, H. J., Sanders, D. B., Scoville, N., Kartaltepe, J., Arnouts, S., Le Floc H, E., Mobasher, B., Taniguchi, Y., Lamareille, F., Leauthaud, A., Sasaki, S., Thompson, D., Zamojski, M., Zamorani, G., Bardelli, S., Bolzonella, M., Angela Bongiorno, Brusa, M., Caputi, K. I., Carollo, C. M., Contini, T., Cook, R., Coppa, G., Cucciati, O., La Torre, S., Ravel, L., Franzetti, P., Garilli, B., Hasinger, G., Iovino, A., Kampczyk, P., Kneib, J. -P, Knobel, C., Kovac, K., Le Borgne, J. F., Le Brun, V., Fevre, O. L., Lilly, S., Looper, D., Maier, C., Mainieri, V., Mellier, Y., Mignoli, M., Murayama, T., Pello, R., Peng, Y., Perez-Montero, E., Renzini, A., Ricciardelli, E., Schiminovich, D., Scodeggio, M., Shioya, Y., Silverman, J., Surace, J., Tanaka, M., Tasca, L., Tresse, L., Vergani, D., Zucca, E., Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Photometry, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Redshifts, Surveys, Galaxy catalogs
Published: 2017

23. Compton-Thick AGN in Multi-Wavelength Surveys

Author: Lanzuisi, Giorgio, Comastri, A., Brusa, M., Vignali, C., Gilli, R., Mignoli, M., Iwasawa, K., Ranalli, P., Georgantopoulos, I., and Akylas, T.
Subjects: active galactic nuclei, AGN
Abstract: I will review the most recent results on the search for CT AGN through multi-wavelength surveys, and on the study of their host properties.
Published: 2016
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24. Nebular Emission from AGN in the Ultraviolet/Optical: Linking Observations and Theory with New Generation Spectral Models

Author: Feltre, Anna, Charlot, S., Gutkin, J., Hirschmann, M., Mignoli, M., Calura, F., Gilli, R., Bongiorno, A., and and the NEOGAL team
Subjects: Astrophysics::High Energy Astrophysical Phenomena, active galactic nuclei, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, AGN, Astrophysics::Galaxy Astrophysics
Abstract: Spectroscopic studies of AGN are powerful means of probing the physical properties of the ionized gas within them. In particular, forthcoming facilities such as JWST and the E-ELT, will provide rest-frame ultraviolet and optical spectra of the very distant AGN. To lay the groundwork for the interpretation of the revolutionary datasets, we have recently computed new photoionization models of the narrow-line emitting regions (NLR) of AGN and combined them with similar models of the nebular emission from star-forming galaxies. In this talk, I will first describe how new ultraviolet and standard optical spectral diagnostics allow one to distinguish between nuclear activity and star formation. I will then present how the nebular emission from both young stars and AGN can be coupled with a new set of cosmological hydrodynamical zoom-in simulations of massive galaxies to achieve a better understanding of black hole growth and galaxy evolution with cosmic time. I will also present an innovative Bayesian fitting code that can help us best interpret current, and future, spectro-photometric data on active galaxies. In particular, the implementation of AGN photoionization calculations within this fitting tool allows us to better understand the physical properties of the AGN NLR gas. I will conclude showing some results from a recent analysis on one of the most comprehensive set of optical spectra (from VIMOS/VLT) sampling the rest-frame ultraviolet range of ~90 type 2 AGN (1.5 < z < 3), drawn from the z-COSMOS deep survey.
Published: 2016
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25. An X-ray/SDSS Sample: Observational Characterization of the Outflowing Gas

Author: Perna, Michele, Brusa, M., Lanzuisi, G., and Mignoli, M.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, active galactic nuclei, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, AGN, Astrophysics::Galaxy Astrophysics
Abstract: Powerful ionised AGN-driven outflows, commonly detected both locally and at high redshift, are invoked to contribute to the co-evolution of SMBH and galaxies through feedback phenomena. Our recent works (Brusa+2015; 2016; Perna+2015a,b) have shown that the XMM-COSMOS targets with evidence of outflows collected so far (~10 sources) appear to be associated with low X‚Äìray kbol corrections (Lbol /LX ‚âà 18), in spite of their spread in obscuration, in the locations on the SFR-Mstar diagram, in their radio emission. A higher statistical significance is required to validate a connection between outflow phenomena and a X-ray loudness. Moreover, in order to validate their binding nature to the galaxy fate, it is crucial to correctly determine the outflow energetics. This requires time consuming integral field spectroscopic (IFS) observations, which are, at present, mostly limited to high luminosity objectsThe study of SDSS data offers a complementary strategy to IFS efforts. I will present physical and demographic characterization of the AGN-galaxy system during the feedback phase obtained studying a sample of ~ 500 X-ray/SDSS AGNs, at z
Published: 2016
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26. The Primordial Environment of SMBHs: the J1030 Field around a Quasar at z = 6.3

Author: Balmaverde, Barbara, Gilli, R., Mignoli, M., Vignali, C., Comastri, A., Sani, E., Vanzella, E., Zamorani, G., Cappelluti, N., and Brusa, M.
Subjects: QSO, SMBH, active galactic nuclei, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, AGN, super-massive black holes, Astrophysics::Galaxy Astrophysics
Abstract: In recent years, with the goal of understanding the large scale structure around high-z QSO, we have obtained deep r,i,z, band imaging at Large Binocular Telescope (LBT) and Y and J band at CFHT Telescope of the field around the quasar SDSSJ1030+0524 (z=6.3). I present here some results, in particular the photometric catalogue of the sources, the selection process of Lyman break galaxies in the QSO halo and the main properties of these galaxies.
Published: 2016
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27. Investigating the relationship between AGN activity and stellar mass in zCOSMOS galaxies at 0

Author: Vitale, M, Mignoli, M, Cimatti, A, Lilly, S, Carollo, C, Contini, T, Kneib, J, Fevre, O, Mainieri, V, Renzini, A, Scodeggio, M, Zamorani, G, Bardelli, S, Barnes, L, Bolzonella, M, Bongiorno, A, Bordoloi, R, Bschorr, T, Cappi, A, Caputi, K, Coppa, G, Cucciati, O, Torre, S, Ravel, L, and Franzetti, P
Abstract: We investigate the link between AGN activity, star-formation and stellar mass of the host galaxy at 010.2 threshold. Moreover, the stellar populations of AGN hosts are found to be older with respect to star-forming and composites galaxies. This could be due to the the tendency of AGN to reside in massive hosts. The dependence of the AGN classification on the stellar mass is in agreement with what has been already found in previous studies. It is consistent with, together with the evidence of older stellar populations inhabiting the AGN-like galaxies, the downsizing scenario. In particular, our evidence points to an evolutionary scenario where the AGN-feedback is capable of quenching the star formation in the most massive galaxies. Therefore, the AGN-feedback is the best candidate for initiating the passive evolutionary phase of galaxies.
Published: 2016

28. The infrared view of luminous X-ray selected Type 2 quasars, and coeval nuclear activity and star formation at z=2

Author: Vignali C, Pozzi F, Fritz J, Comastri A, Gruppioni C, Bellocchi E, Fiore F, Brusa M, Maiolino R, Mignoli M, Pozzetti L, Zamorani G, Gilli R., LA FRANCA, Fabio, J. RODRIGUEZ, P. FERRANDO, Vignali C., Pozzi F., Fritz J., Comastri A., Gruppioni C., Bellocchi E., Fiore G., Brusa M., Maiolino R., Mignoli M., La Franca F., Pozzetti L., Zamorani G., Gilli R., Ferrando P, Rodriguez J, Vignali, C, Pozzi, F, Fritz, J, Comastri, A, Gruppioni, C, Bellocchi, E, Fiore, F, Brusa, M, Maiolino, R, Mignoli, M, LA FRANCA, Fabio, Pozzetti, L, Zamorani, G, and Gilli, R.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Here we present some preliminary results obtained for a sample of X-ray selected, luminous and obscured (Type 2) quasars at z approximate to 1-2 observed in the near- and mid-IR with Spitzer. In particular, adopting a torus configuration for the obscuring (and reprocessing) matter and fitting the quasar Spectral Energy Distributions (SFDs), we estimate some geometric parameters for the torus like tau(9.7 mu m) and full covering angle, and provide AGN bolometric luminosities and corrections. We also present the interesting case of a z approximate to 2 quasar for which the inclusion of sub-mm (SCUBA) data allows us to reveal and parameterize coeval nuclear activity and star formation.
Published: 2009

29. Hubble imaging of the ionizing radiation from a star-forming galaxy at z=3.2 with fesc>50%

Author: Vanzella, E., de Barros, S., Vasei, K., Alavi, A., Giavalisco, M., Siana, B., Grazian, A., Hasinger, G., Suh, H., Cappelluti, N., Vito, F., Amorin, R., Balestra, I., Brusa, M., Calura, F., Castellano, M., Comastri, A., Fontana, A., Gilli, R., Mignoli, M., Pentericci, L., Vignali, C., and Zamorani, G.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Star-forming galaxies are considered to be the leading candidate sources that dominate the cosmic reionization at z>7, and the search for analogs at moderate redshift showing Lyman continuum (LyC) leakage is currently a active line of research. We have observed a star-forming galaxy at z=3.2 with Hubble/WFC3 in the F336W filter, corresponding to the 730-890A rest-frame, and detect LyC emission. This galaxy is very compact and also has large Oxygen ratio [OIII]5007/[OII]3727 (>=10). No nuclear activity is revealed from optical/near-infrared spectroscopy and deep multi-band photometry (including the 6Ms X-ray, Chandra). The measured escape fraction of ionizing radiation spans the range 50-100\%, depending on the IGM attenuation. The LyC emission is detected at S/N=10 with m(F336W)=27.57+/-0.11 and it is spatially unresolved, with effective radius R_e7 allowing a direct comparison with lower redshift LyC emitters, as reported here., 6 pages, 5 figures, ApJ submitted (comments welcome)
Published: 2016
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30. High-resolution spectroscopy of a young, low-metallicity optically-thin L=0.02L* star-forming galaxy at z=3.12

Author: Vanzella, E., De Barros, S., Cupani, G., Karman, W., Gronke, M., Balestra, I., Coe, D., Mignoli, M., Brusa, M., Calura, F., Caminha, G. -B., Caputi, K., Castellano, M., Christensen, L., Comastri, A., Cristiani, S., Dijkstra, M., Fontana, A., Giallongo, E., Giavalisco, M., Gilli, R., Grazian, A., Grillo, C., Koekemoer, A., Meneghetti, M., Nonino, M., Pentericci, L., Rosati, P., Schaerer, D., Verhamme, A., Vignali, C., and Zamorani, G.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract: We present VLT/X-Shooter and MUSE spectroscopy of an faint F814W=28.60+/-0.33 (Muv=-17.0), low mass (~10 ratio. We detect CIV1548,1550 resonant doublet in emission, each component with FWHM ~< 45 km/s, and redshifted by +51(+/-10)km/s relative to the systemic redshift. We interpret this as nebular emission tracing an expanding optically-thin interstellar medium. Both CIV1548,1550 and HeII1640 suggest the presence of hot and massive stars (with a possible faint AGN). The ultraviolet slope is remarkably blue, beta =-2.95 +/- 0.20 (F_lambda=lambda^beta), consistent with a dust-free and young ~, 7 pages, 4 figures and 1 table; ApJL, accepted for publication
Published: 2016
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31. Hubble Imaging of the Ionizing Radiation from a Star-forming Galaxy at Z=3.2 with fesc>50%

Author: Vanzella, E., de Barros, S., Vasei, K., Alavi, A., Giavalisco, M., Siana, B., Grazian, A., Hasinger, G., Suh, H., Cappelluti, N., Vito, F., Amorin, R., Balestra, I., Brusa, M., Calura, F., Castellano, M., Comastri, A., Fontana, A., Gilli, R., Mignoli, M., Pentericci, L., Vignali, C., and Zamorani, G.
Subjects: Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: Star-forming galaxies are considered to be the leading candidate sources that dominate the cosmic reionization at z>7, and the search for analogs at moderate redshift showing Lyman continuum (LyC) leakage is currently a active line of research. We have observed a star-forming galaxy at z=3.2 with Hubble/WFC3 in the F336W filter, corresponding to the 730-890A rest-frame, and detect LyC emission. This galaxy is very compact and also has large Oxygen ratio [OIII]5007/[OII]3727 (>=10). No nuclear activity is revealed from optical/near-infrared spectroscopy and deep multi-band photometry (including the 6Ms X-ray, Chandra). The measured escape fraction of ionizing radiation spans the range 50-100\%, depending on the IGM attenuation. The LyC emission is detected at S/N=10 with m(F336W)=27.57+/-0.11 and it is spatially unresolved, with effective radius R_e7 allowing a direct comparison with lower redshift LyC emitters, as reported here., Comment: 6 pages, 5 figures, ApJ submitted (comments welcome)
Published: 2016

32. The star formation rate cookbook at 1 < z < 3: Extinction-corrected relations for UV & [OII]{\lambda}3727 luminosities

Author: Talia, M., Cimatti, A., Pozzetti, L., Rodighiero, G., Gruppioni, C., Pozzi, F., Daddi, E., Maraston, C., Mignoli, M., and Kurk, J.
Subjects: Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use a spectroscopic sample of 286 star-forming galaxies (SFGs) at 1, Comment: Accepted for publication in A&A; 20 pages, 19 figures, 5 tables
Published: 2015

33. Extreme emission-line galaxies out to z similar to 1 in zCOSMOS I. Sample and characterization of global properties

Author: Amorin, R., Perez-Montero, F., Contini, T., Vilchez, J. M., Bolzonella, M., Tasca, L. A. M., Lamareille, F., Zamorani, G., Maier, C., Carollo, C. M., Kneib, J. -P., Le Fevre, O., Lilly, S., Mainieri, V., Renzinis, A., Scodeggio, M., Bardelli, S., Bongiorno, A., Caputi, K., Cucciati, O., de la Torre, S., de Ravel, L., Franzetti, P., Garilli, B., Iovino, A., Kampczyk, P., Knobel, C., Kovac, K., Le Borgne, J. -F., Le Brun, V., Mignoli, M., Pello, R., Peng, Y., Presotto, V., Ricciardelli, E., Silverman, J. D., Tanaka, M., Tresse, L., Vergani, D., Zucca, E., and Kapteyn Astronomical Institute
Subjects: ACTIVE GALACTIC NUCLEI, galaxies: irregular galaxies: star formation, ULTRA DEEP FIELD, METAL-POOR GALAXIES, galaxies: fundamental parameters, galaxies: starburst, Astrophysics::Cosmology and Extragalactic Astrophysics, LYMAN BREAK GALAXIES, LY-ALPHA EMITTERS, LUMINOSITY-METALLICITY RELATION, COMPACT DWARF GALAXIES, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, DIGITAL SKY SURVEY, galaxies: abundances, Astrophysics::Earth and Planetary Astrophysics, GREEN PEA GALAXIES, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract: Context. The study of large and representative samples of low-metallicity star-forming galaxies at different cosmic epochs is of great interest to the detailed understanding of the assembly history and evolution of low-mass galaxies. Aims. We present a thorough characterization of a large sample of 183 extreme emission-line galaxies (EELGs) at redshift 0.11 Methods. We use multiwavelength COSMOS photometry, HST-ACS I-band imaging, and optical zCOSMOS spectroscopy to derive the main global properties of star-forming EELGs, such as sizes, stellar masses, star formation rates (SFR), and reliable oxygen abundances using both "direct" and "strong-line" methods. Results. The EELGs are extremely compact (r(50) similar to 1.3 kpc), low-mass (M-* similar to 10(7)-10(10) M-circle dot) galaxies forming stars at unusually high specific star formation rates (sSFR equivalent to SFR/M-star up to 10(-7) yr(-1)) compared to main sequence star-forming galaxies of the same stellar mass and redshift. At rest-frame UV wavelengths, the EELGs are luminous and show high surface brightness and include strong Ly alpha emitters, as revealed by GALEX spectroscopy. We show that zCOSMOS EELGs are high-ionization, low-metallicity systems, with median 12+log(O/H) = 8.16 +/- 0.21 (0.2 Z(circle dot)) including a handful of extremely metal-deficient ( Conclusions. The zCOSMOS EELGs are galaxies caught in a transient and probably early period of their evolution, where they are efficiently building up a significant fraction of their present-day stellar mass in an ongoing, galaxy-wide starburst. Therefore, the EELGs constitute an ideal benchmark for comparison studies between low- and high-redshift low-mass star-forming galaxies.
Published: 2015

34. Extreme emission-line galaxies out to z similar to 1 in zCOSMOS I. Sample and characterization of global properties

Author: Amorín, R., Perez-Montero, F., Contini, T., Vílchez, J. M., Bolzonella, M., Tasca, L. A. M., Lamareille, F., Zamorani, G., Maier, C., Carollo, C. M., Kneib, J. -P., Le Fevre, O., Lilly, S., Mainieri, V., Renzini, A., Scodeggio, M., Bardelli, S., Bongiorno, A., Caputi, K., Cucciati, O., Torre, S., Ravel, L., Franzetti, P., Garilli, B., Iovino, A., Knobel, C., Kovac, K., Le Borgne, J. -F., Le Brun, V., Mignoli, M., Pello, R., Peng, Y., Presotto, V., Ricciardelli, E., Silverman, J. D., Tanaka, M., Tresse, L., Vergani, D., Zucca, E., INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), University of Vienna [Vienna], University of Chicago, Ecole Polytechnique Fédérale de Lausanne (EPFL), European Southern Observatory (ESO), INAF- Milano, INAF - Osservatorio Astronomico di Bologna (OABO), College of Computing (GATECH), Georgia Institute of Technology [Atlanta], Hunan Normal University (HNU), Università degli studi di Trieste = University of Trieste, INAF - Osservatorio Astronomico di Trieste (OAT), INAF - Osservatorio Astrofisico di Arcetri (OAA), Oncology Institute of Southern Switzerland, European Project: 312725,EC:FP7:SPA,FP7-SPACE-2012-1,ASTRODEEP(2013), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Hunan Normal University, and Università degli studi di Trieste
Subjects: Galaxies: fundamental parameters, Galaxies: star formation, Galaxies: abundances, Astrophysics::Solar and Stellar Astrophysics, Galaxies: evolution, Galaxies: irregular, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxies: starburst, Astrophysics::Galaxy Astrophysics
Abstract: International audience; Context. The study of large and representative samples of low-metallicity star-forming galaxies at different cosmic epochs is of great interest to the detailed understanding of the assembly history and evolution of low-mass galaxies. Aims. We present a thorough characterization of a large sample of 183 extreme emission-line galaxies (EELGs) at redshift 0.11 \textless= z \textless= 0.93 selected from the 20k zCOSMOS bright survey because of their unusually large emission line equivalent widths. Methods. We use multiwavelength COSMOS photometry, HST-ACS I-band imaging, and optical zCOSMOS spectroscopy to derive the main global properties of star-forming EELGs, such as sizes, stellar masses, star formation rates (SFR), and reliable oxygen abundances using both “direct” and “strong-line” methods. Results. The EELGs are extremely compact (r(50) similar to 1.3 kpc), low-mass (M-* similar to 10(7)-10(10) M-circle dot) galaxies forming stars at unusually high specific star formation rates (sSFR equivalent to SFR/M-star up to 10(-7) yr(-1)) compared to main sequence star-forming galaxies of the same stellar mass and redshift. At rest-frame UV wavelengths, the EELGs are luminous and show high surface brightness and include strong Ly alpha emitters, as revealed by GALEX spectroscopy. We show that zCOSMOS EELGs are high-ionization, low-metallicity systems, with median 12+log(O/H) = 8.16 +/- 0.21 (0.2 Z(circle dot)) including a handful of extremely metal-deficient (\textless0.1 Z(circle dot)) EELGs. While similar to 80% of the EELGs show non-axisymmetric morphologies, including clumpy and cometary or tadpole galaxies, we find that similar to 29% of them show additional low-surface-brightness features, which strongly suggests recent or ongoing interactions. As star-forming dwarfs in the local Universe, EELGs are most often found in relative isolation. While only very few EELGs belong to compact groups, almost one third of them are found in spectroscopically confirmed loose pairs or triplets. Conclusions. The zCOSMOS EELGs are galaxies caught in a transient and probably early period of their evolution, where they are efficiently building up a significant fraction of their present-day stellar mass in an ongoing, galaxy-wide starburst. Therefore, the EELGs constitute an ideal benchmark for comparison studies between low- and high-redshift low-mass star-forming galaxies.
Published: 2015
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35. Bolometric luminosities and Eddington ratios of X-ray selected active galactic nuclei in the XMM -COSMOS survey

Author: Lusso, E., Comastri, A., Simmons, B. D., Mignoli, M., Zamorani, G., Vignali, C., Brusa, M., Shankar, F., Lutz, D., Trump, J. R., Maiolino, R., Gilli, R., Bolzonella, M., Puccetti, S., Salvato, M., Impey, C. D., Civano, F., Elvis, M., Mainieri, V., Silverman, J. D., Koekemoer, A. M., Bongiorno, A., Merloni, A., Berta, S., Floc'h, E. Le, Magnelli, B., Pozzi, F., Riguccini, L., INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), AUTRES, INAF - Osservatorio Astronomico di Capodimonte (OAC), Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), INAF - Osservatorio Astronomico di Bologna (OABO), Università di Bologna, Dipartimento di Astronomia, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Space Telescope Science Institute (STSci), Max-Planck-Institut für Astrophysik (MPA), Ecosystèmes lagunaires : organisation biologique et fonctionnement (ECOLAG), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Lusso E., Comastri A., Simmons B.D., Mignoli M., Zamorani G., Vignali C., Brusa M., Shankar F., Lutz D., Trump J.R., Maiolino R., Gilli R., Bolzonella M., Puccetti S., Salvato M., Impey C.D., Civano F., Elvis M., Mainieri V., Silverman J.D., Koekemoer A.M., Bongiorno A., A. Merloni, Berta S., Le Floc'h E., Magnelli B., Pozzi F., Riguccini L., Harvard University-Smithsonian Institution, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Galaxies: active, Galaxies: evolution, Methods: statistical, Quasars: general, Astronomy and Astrophysics, Space and Planetary Science, [PHYS]Physics [physics], methods: statistical, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, quasars: general, Astrophysics::Solar and Stellar Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Bolometric luminosities and Eddington ratios of both X-ray selected broad-line (Type-1) and narrow-line (Type-2) AGN from the XMM-Newton survey in the COSMOS field are presented. The sample is composed by 929 AGN (382 Type-1 AGN and 547 Type-2 AGN) and it covers a wide range of redshifts, X-ray luminosities and absorbing column densities. About 65% of the sources are spectroscopically identified as either Type-1 or Type-2 AGN (83% and 52% respectively), while accurate photometric redshifts are available for the rest of the sample. The study of such a large sample of X-ray selected AGN with a high quality multi-wavelength coverage from the far-infrared (now with the inclusion of Herschel data at 100 micron and 160 micron) to the optical-UV allows us to obtain accurate estimates of bolometric luminosities, bolometric corrections and Eddington ratios. The kbol-Lbol relations derived in the present work are calibrated for the first time against a sizable AGN sample, and rely on observed redshifts, X-ray luminosities and column density distributions. We find that kbol is significantly lower at high Lbol with respect to previous estimates by Marconi et al. (2004) and Hopkins et al. (2007). Black hole masses and Eddington ratios are available for 170 Type-1 AGN, while black hole masses for Type-2 AGN are computed for 481 objects using the black hole mass-stellar mass relation and the morphological information. We confirm a trend between kbol and lambda_Edd, with lower hard X-ray bolometric corrections at lower Eddington ratios for both Type-1 and Type-2 AGN. We find that, on average, Eddington ratio increases with redshift for all Types of AGN at any given Mbh, while no clear evolution with redshift is seen at any given Lbol., Comment: 19 pages, 18 figures, accepted to MNRAS
Published: 2012
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36. The COSMOS Density Field: A Reconstruction Using Both Weak Lensing and Galaxy Distributions

Author: Amara, A., Lilly, S., Kovac, K., Rhodes, J., Massey, R., Zamorani, G., Carollo, C. M., Contini, T., Kneib, J-P, Le Fevre, O., Mainieri, V., Renzini, A., Scodeggio, M., Bardelli, S., Bolzonella, M., Bongiorno, A., Caputi, K., Cucciati, O., Torre, S., Ravel, L., Franzetti, P., Garilli, B., Iovino, A., Kampczyk, P., Knobel, C., Lamareille, F., Le Borgne, J-F, Le Brun, V., Maier, C., Mignoli, M., Pello, R., Peng, Y., Perez Montero, E., Presotto, V., Silverman, J., Tanaka, M., Tasca, L., Tresse, L., Vergani, D., Zucca, E., BARNES, L., Bordoloi, R., Cappi, A., Cimatti, Alessandro, Coppa, G., Koekoemoer, A., Lopez-Sanjuan, C., McCracken, H. J., Moresco, M., Nair, P., Pozzetti, L., Welikala, N., Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Amara A., Lilly S., Kovač K., Rhodes J., Massey R., Zamorani G., Carollo C. M., Contini T., Kneib J.-P., Le Fevre O., Mainieri V., Renzini A., Scodeggio M., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., 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., Mignoli M., Pello R., Peng Y., Montero E. Perez, Presotto V., Silverman J., Tanaka M., Tasca L., Tresse L., Vergani D., Zucca E., Barnes L., Bordoloi R., Cappi A., Cimatti A., Coppa G., Koekoemoer A., López-Sanjuan C., McCracken H. J., Moresco M., Nair P., Pozzetti L., Welikala N., Astronomy, and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: SAMPLE, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], DEEP, DATA RELEASE, FOS: Physical sciences, HUBBLE-SPACE-TELESCOPE, Astrophysics::Cosmology and Extragalactic Astrophysics, dark matter, ADVANCED CAMERA, Large-scale structure of Universe, LARGE-SCALE STRUCTURE, DARK-MATTER, Dark matter, DIGITAL SKY SURVEY, dark matter, large-scale structure of Universe, large-scale structure of Universe, CLUSTERS, ZCOSMOS GALAXIES, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The COSMOS field has been the subject of a wide range of observations, with a number of studies focusing on reconstructing the 3D dark matter density field. Typically, these studies have focused on one given method or tracer. In this paper, we reconstruct the distribution of mass in the COSMOS field out to a redshift z=1 by combining Hubble Space Telescope weak lensing measurements with zCOSMOS spectroscopic measurements of galaxy clustering. The distribution of galaxies traces the distribution of mass with high resolution (particularly in redshift, which is not possible with lensing), and the lensing data empirically calibrates the mass normalisation (bypassing the need for theoretical models). Two steps are needed to convert a galaxy survey into a density field. The first step is to create a smooth field from the galaxy positions, which is a point field. We investigate four possible methods for this: (i) Gaussian smoothing, (ii) convolution with truncated isothermal sphere, (iii) fifth nearest neighbour smoothing and (iv) a muliti-scale entropy method. The second step is to rescale this density field using a bias prescription. We calculate the optimal bias scaling for each method by comparing predictions from the smoothed density field with the measured weak lensing data, on a galaxy-by-galaxy basis. In general, we find scale-independent bias for all the smoothing schemes, to a precision of 10%. For the nearest neighbour smoothing case, we find the bias to be 2.51\pm 0.25. We also find evidence for a strongly evolving bias, increasing by a factor of ~3.5 between redshifts 0, Comment: Accepted by MNRAS. 12 pages with 6 Figures
Published: 2012
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37. Accreting supermassive black holes in the COSMOS Field and the connection to their host galaxies

Author: Bongiorno A., Merloni A., Magnelli B., Salvato M., Mignoli M., Zamorani G., Fiore F., Rosario D., Mainieri V., Comastri A., Balestra I., Bardelli S., Berta S., Civano F., Kampczyk P., Le Floc'h E., Lutz D., Pozzetti L., Riguccini L., Shankar F., Silverman J., BRUSA, MARCELLA, VIGNALI, CRISTIAN, LUSSO, ELISABETA, POZZI, FRANCESCA, Bongiorno A., Merloni A., Brusa M., Magnelli B., Salvato M., Mignoli M., Zamorani G., Fiore F., Rosario D., Mainieri V., Comastri A., Vignali C., Balestra I., Bardelli S., Berta S., Civano F., Kampczyk P., Le Floc'h E., Lusso E., Lutz D., Pozzetti L., Pozzi F., Riguccini L., Shankar F., and Silverman J.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, survey, galaxies: fundamental parameters, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract: Using the wide multiband photometry available in the Cosmic Evolution Survey (COSMOS) field, we explore the host galaxy properties of a large sample of active galactic nuclei (AGNs; ˜1700 objects) with Lbol ranging from 1043 to 1047 erg s-1, obtained by combining X-ray and optical spectroscopic selections. Based on a careful study of their spectral energy distributions, which have been parametrized using a two-component (AGN+galaxy) model fit, we have derived dust-corrected rest-frame magnitudes, colours and stellar masses of the obscured and unobscured AGN hosts up to high redshift (z≲3). Moreover, for the sample of obscured AGNs, we have also derived reliable star formation rates (SFRs). We find that AGN hosts span a large range of stellar masses and SFRs. No colour-bimodality is seen at any redshift in the AGN hosts, which are found to be mainly massive, red galaxies. Once we have accounted for the colour-mass degeneracy in well-defined mass-matched samples, we find a residual (marginal) enhancement of the incidence of AGNs in redder galaxies with lower specific SFRs. We argue that this result might emerge because of our ability to properly account for AGN light contamination and dust extinction, compared to surveys with a more limited multiwavelength coverage. However, because these colour shifts are relatively small, systematic effects could still be considered responsible for some of the observed trends. Interestingly, we find that the probability for a galaxy to host a black hole that is growing at any given 'specific accretion rate' (i.e. the ratio of X-ray luminosity to the host stellar mass) is almost independent of the host galaxy mass, while it decreases as a power law with LX/M*. By analysing the normalization of such a probability distribution, we show how the incidence of AGNs increases with redshift as rapidly as (1 + z)4, which closely resembles the overall evolution of the specific SFR of the entire galaxy population. We provide analytical fitting formulae that describe the probability of a galaxy of any mass (above the completeness limit of the COSMOS) to host an AGN of any given specific accretion rate as a function of redshift. These can be useful tools for theoretical studies of the growing population of black holes within galaxy evolution models. Although AGN activity and star formation in galaxies do appear to have a common triggering mechanism, at least in a statistical sense, within the COSMOS sample, we do not find any conclusive evidence to suggest that AGNs have a powerful influence on the star-forming properties of their host galaxies.
Published: 2012

38. On the nature of the absorber in IRAS 09104+4109: the X-ray and mid-infrared view

Author: Vignali, C., Piconcelli, E., Lanzuisi, G., Feltre, A., Feruglio, C., Maiolino, R., Fiore, F., Fritz, J., La Parola, V., Mignoli, M., Pozzi, F., Vignali C., Piconcelli E., Lanzuisi G., Feltre A., Feruglio C., Maiolino R., Fiore F., Fritz J., La Parola V., Mignoli M., and Pozzi F.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), quasars: general, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: nuclei, Astrophysics - High Energy Astrophysical Phenomena, quasars: individual: IRAS 09104+4109, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a long (~76 ks) Chandra observation of IRAS 09104+4109, a hyper-luminous galaxy, optically classified as a Type 2 AGN hosted in a cD galaxy in a cluster at z=0.442. We also report on the results obtained by fitting its broad-band spectral energy distribution. The Compton-thick nature of this source (which has been often referred to as an "archetype" of Compton-thick Type 2 quasars) was formerly claimed on the basis of its marginal detection in the PDS instrument onboard BeppoSAX, being then disputed using XMM-Newton data. Both Chandra analysis and optical/mid-IR spectral fitting are consistent with the presence of heavy (~1-5 10^{23} cm^{-2}) but not extreme (Compton-thick) obscuration. However, using the mid-IR and the [OIII] emission as proxies of the nuclear hard X-ray luminosity suggests the presence of heavier obscuration. The 54-month Swift BAT map shows excess hard X-ray emission likely related to a nearby (z=0.009) Type 2 AGN, close enough to IRAS 09104+4109 to significantly enhance and contaminate its emission in the early BeppoSAX PDS data., 10 pages, 4 figures, 2 tables, MNRAS. Some references added
Published: 2011

39. The Nonlinear Biasing of the zCOSMOS Galaxies up to z ~ 1 from the 10k Sample

Author: Kova, #269, Porciani C., Lilly S. J., Marinoni C., Guzzo L., Zamorani G., Iovino A., Oesch P., Bolzonella M., Peng Y., Meneux B., Zucca E., Bardelli S., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Mainieri V., Renzini A., Scodeggio M., Bongiorno A., Caputi K., Coppa G., de la Torre S., de Ravel L., Finoguenov A., Franzetti P., Garilli B., Kampczyk P., Knobel C., Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Mignoli M., Pello R., Perez Montero E., Pozzetti L., Ricciardelli E., Silverman J. D., Tanaka M., Tasca L. A. M., Tresse L., Vergani D., Abbas U., Bottini D., Cappi A., Cassata P., Fumana M., Koekemoer A. M., Leauthaud A., Maccagni D., McCracken H. J., Memeo P., Scaramella R., Scoville N. Z., CUCCIATI, OLGA, CIMATTI, ANDREA, Kova&#269, K., Porciani C., Lilly S. J., Marinoni C., Guzzo L., Cucciati O., Zamorani G., Iovino A., Oesch P., Bolzonella M., Peng Y., Meneux B., Zucca E., Bardelli S., Carollo C. M., Contini T., Kneib J.-P., Le Fèvre O., Mainieri V., Renzini A., Scodeggio M., Bongiorno A., Caputi K., Coppa G., de la Torre S., de Ravel L., Finoguenov A., Franzetti P., Garilli B., Kampczyk P., Knobel C., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Mignoli M., Pello R., Perez-Montero E., Pozzetti L., Ricciardelli E., Silverman J. D., Tanaka M., Tasca L. A. M., Tresse L., Vergani D., Abbas U., Bottini D., Cappi A., Cassata P., Cimatti A., Fumana M., Koekemoer A. M., Leauthaud A., Maccagni D., McCracken H. J., Memeo P., Scaramella R., and Scoville N. Z.
Subjects: Physics, cosmology: observation, Field (physics), 010308 nuclear & particles physics, Dark matter, Astronomy and Astrophysics, Biasing, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Redshift, Galaxy, Luminosity, Space and Planetary Science, cosmology: observations, 0103 physical sciences, Halo effect, galaxies: evolution, galaxies: statistics, 010303 astronomy & astrophysics, Smoothing, Astrophysics::Galaxy Astrophysics
Abstract: We use the zCOSMOS galaxy overdensity field to study the biasing of galaxies in the COSMOS field. By comparing the probability distribution function of the galaxy density contrast δ g to the lognormal approximation of the mass density contrast δ, we obtain the mean biasing function b(δ, z, R) between the galaxy and matter overdensity fields and its second moments \hat{b} and \tilde{b}. Over the redshift interval 0.4 < z < 1 the conditional mean function langδ g |δrang = b(δ, z, R)δ is of a characteristic shape, requiring nonlinear biasing in the most overdense and underdense regions. Taking into account the uncertainties due to cosmic variance, we do not detect any significant evolution in the langδ g |δrang function, but we do detect a significant redshift evolution in the linear biasing parameter \hat{b} from 1.23 ± 0.11 at z ~ 0.55 to 1.62 ± 0.14 at z ~ 0.75, for a luminosity-complete sample of MB < -20 - z galaxies. The \hat{b} parameter does not change significantly with smoothing scale between 8 and 12 h -1 Mpc, but increases systematically with luminosity (at 2σ-3σ significance between the MB < -20.5 - z and MB < -20 - z samples). The nonlinearity parameter \tilde{b}/ \hat{b} is offset from unity by at most 2%, with an uncertainty of the same order. The \tilde{b}/\hat{b} parameter does not show any significant redshift evolution, dependence on the smoothing scale or on the luminosity. By matching the linear bias of galaxies to the halo bias, we infer that the MB < -20 - z galaxies reside in dark matter halos with a characteristic mass of about (2.6 - 5.6) × 1012 M sun with a small dependence on the adopted bias-mass relation. Our detailed error analysis and comparison with previous studies lead us to conclude that cosmic variance is the main contributor to the differences in the linear bias measured from different surveys. While our results support the general picture of biased galaxy formation up to z ~ 1, the fine-tuning of the galaxy formation models is still limited by the restrictions of the current spectroscopic surveys at these redshifts.
Published: 2011

40. The zCOSMOS-Bright survey: the clustering of early and late galaxy morphological types since z≃ 1

Author: de la Torre S., Le Fèvre O., Porciani C., Guzzo L., Meneux B., Abbas U., Tasca L., Carollo C. M., Contini T., Kneib J. P., Lilly S. J., Mainieri V., Renzini A., Scodeggio M., Zamorani G., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Coppa G., de Ravel L., Franzetti P., Garilli B., Halliday C., Iovino A., Kampczyk P., Knobel C., Koekemoer A. M., Kova, #269, Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Mignoli M., Pelló R., Peng Y., Perez Montero E., Ricciardelli E., Silverman J., Tanaka M., Tresse L., Vergani D., Zucca E., Bottini D., Cappi A., Cassata P., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Oesch P., Pozzetti L., Scaramella R., CUCCIATI, OLGA, CIMATTI, ANDREA, de la Torre S., Le Fèvre O., Porciani C., Guzzo L., Meneux B., Abbas U., Tasca L., Carollo C. M., Contini T., Kneib J.-P., Lilly S. J., Mainieri V., Renzini A., Scodeggio M., Zamorani G., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Coppa G., Cucciati O., de Ravel L., Franzetti P., Garilli B., Halliday C., Iovino A., Kampczyk P., Knobel C., Koekemoer A. M., Kova&#269, K., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Mignoli M., Pelló R., Peng Y., Perez-Montero E., Ricciardelli E., Silverman J., Tanaka M., Tresse L., Vergani D., Zucca E., Bottini D., Cappi A., Cassata P., Cimatti A., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Oesch P., Pozzetti L., and Scaramella R.
Subjects: cosmology: observation, galaxies: high-redshift, galaxies: statistic, Astrophysics::Cosmology and Extragalactic Astrophysics, large-scale structure of Universe, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract: We measure the spatial clustering of galaxies as a function of their morphological type at z≃ 0.8, for the first time in a deep redshift survey with full morphological information. This is obtained by combining high-resolution Hubble Space Telescope imaging and Very Large Telescope spectroscopy for about 8500 galaxies to ? with accurate spectroscopic redshifts from the zCOSMOS-Bright redshift survey. At this epoch, early-type galaxies already show a significantly stronger clustering than late-type galaxies on all probed scales. A comparison to the Sloan Digital Sky Survey Data at z≃ 0.1 shows that the relative clustering strength between early and late morphological classes tends to increase with cosmic time at small separations, while on large scales it shows no significant evolution since z≃ 0.8. This suggests that most early-type galaxies had already formed in intermediate and dense environments at this epoch. Our results are consistent with a picture in which the relative clustering of different morphological types between z≃ 1 and 0 reflects the evolving role of environment in the morphological transformation of galaxies, on top of a global evolution driven by mass.
Published: 2011

41. The evolution of quiescent galaxies at high redshifts (z≥ 1.4)

Author: Domínguez Sánchez H., Gruppioni C., Ilbert O., Pozzetti L., McCracken H., Capak P., Le Floch E., Salvato M., Zamorani G., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Lilly S. J., Mainieri V., Renzini A., Scodeggio M., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Coppa G., de la Torre S., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., Kova, #269, Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Mignoli M., Pelló R., Peng Y., Perez Montero E., Ricciardelli E., Silverman J. D., Tanaka M., Tasca L. A. M., Tresse L., Vergani D., Zucca E., POZZI, FRANCESCA, CIMATTI, ANDREA, CUCCIATI, OLGA, Domínguez Sánchez H., Pozzi F., Gruppioni C., Cimatti A., Ilbert O., Pozzetti L., McCracken H., Capak P., Le Floch E., Salvato M., Zamorani G., Carollo C. M., Contini T., Kneib J.-P., Le Fèvre O., Lilly S. J., Mainieri V., Renzini A., Scodeggio M., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Coppa G., Cucciati O., de la Torre S., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., Kova&#269, K., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Mignoli M., Pelló R., Peng Y., Perez-Montero E., Ricciardelli E., Silverman J. D., Tanaka M., Tasca L. A. M., Tresse L., Vergani D., and Zucca E.
Subjects: galaxies: high-redshift, galaxies: star formation, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract: The goal of this work is to study the evolution of high-redshift (z≥ 1.4) quiescent galaxies over an effective area of ˜1.7 deg2 in the COSMOS field. Galaxies have been divided according to their star formation activity and the evolution of the different populations, in particular of the quiescent galaxies, has been investigated in detail. We have studied an IRAC (mag 3.6 μm < 22.0) selected sample of ˜18 000 galaxies at z≥ 1.4 in the COSMOS field with multiwavelength coverage extending from the U band to the Spitzer 24 μm one. We have derived accurate photometric redshifts (?) through a SED-fitting procedure. Other important physical parameters [masses, ages and star formation rates (SFR)] of the galaxies have been obtained using Maraston models. We have divided our sample into actively star-forming, intermediate and quiescent galaxies depending on their specific star formation rate (SSFR = SFR/M). We have computed the galaxy stellar mass function (GSMF) of the total sample and the different populations at z= 1.4-3.0. We have studied the properties of high-redshift quiescent galaxies finding that they are old (1-4 Gyr), massive (˜ 1010.65 M⊙), weakly star-forming stellar populations with low dust extinction [E(B-V) ≤ 0.15] and small e-folding time-scales (τ˜ 0.1-0.3 Gyr). We observe a significant evolution of the quiescent stellar mass function from 2.5 < z < 3.0 to 1.4 < z < 1.6, increasing by ˜1 dex in this redshift interval. We find that z˜ 1.5 is an epoch of transition of the GSMF: while the GSMF at z≳ 1.5 is dominated by the star-forming galaxies at all stellar masses, at z≲ 1.5 the contribution to the total GSMF of the quiescent galaxies is significant and becomes higher than that of the star-forming population for M≥ 1010.75 M⊙. The fraction of star-forming galaxies decreases from 60-20 per cent from z˜ 2.5-3.0 to 1.4-1.6 for M˜ 1011.0 M⊙, while the quiescent population increases from 10-50 per cent at the same redshift and mass intervals. We compare the fraction of quiescent galaxies derived with that predicted by theoretical models and find that the Kitzbichler & White model, implemented on the Millennium Simulation, is the one that better reproduces the shape of the data. Finally, we calculate the stellar mass density of the star-forming and quiescent populations as a function of redshift and find that there is already a significant number of quiescent galaxies at z > 2.5 (logρ[M⊙ Mpc-3]˜ 6), meaning that efficient star formation had to take place before that time.
Published: 2011

42. The bimodality of the 10k zCOSMOS-bright galaxies up to z ~ 1: a new statistical and portable classification based on the optical galaxy properties

Author: Coppa G., Mignoli M., Zamorani G., Bardelli S., Lilly S. J., Bolzonella M., Scodeggio M., Vergani D., Nair P., Pozzetti L., Zucca E., Carollo C. M., Contini T., Le Fèvre O., Renzini A., Mainieri V., Bongiorno A., Caputi K. I., de la Torre S., de Ravel L., Franzetti P., Garilli B., Memeo P., Iovino A., Kampczyk P., Kneib J. P., Knobel C., Koekemoer A. M., Kova, #269, Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Pellò R., Peng Y., Perez Montero E., Ricciardelli E., Scarlata C., Silverman J. D., Tanaka M., Tasca L., Tresse L., Abbas U., Bottini D., Capak P., Cappi A., Cassata P., Fumana M., Guzzo L., Leauthaud A., Maccagni D., Marinoni C., Meneux B., Oesch P., Porciani C., Scaramella R., Scoville N., CIMATTI, ANDREA, CUCCIATI, OLGA, Coppa G., Mignoli M., Zamorani G., Bardelli S., Lilly S. J., Bolzonella M., Scodeggio M., Vergani D., Nair P., Pozzetti L., Cimatti A., Zucca E., Carollo C. M., Contini T., Le Fèvre O., Renzini A., Mainieri V., Bongiorno A., Caputi K. I., Cucciati O., de la Torre S., de Ravel L., Franzetti P., Garilli B., Memeo P., Iovino A., Kampczyk P., Kneib J.-P., Knobel C., Koekemoer A. M., Kova&#269, K., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Pellò R., Peng Y., Perez-Montero E., Ricciardelli E., Scarlata C., Silverman J. D., Tanaka M., Tasca L., Tresse L., Abbas U., Bottini D., Capak P., Cappi A., Cassata P., Fumana M., Guzzo L., Leauthaud A., Maccagni D., Marinoni C., Meneux B., Oesch P., Porciani C., Scaramella R., Scoville N., Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Bologna (OABO), University of Chicago, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), European Southern Observatory (ESO), College of Computing (GATECH), Georgia Institute of Technology [Atlanta], AUTRES, Dipartimento di Fisica, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), Ecole Polytechnique Fédérale de Lausanne (EPFL), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Département Informatique pour les Systèmes Coopératifs Ouverts et Décentralisés (ISCOD-ENSMSE), École des Mines de Saint-Étienne (Mines Saint-Étienne MSE), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Institut Henri Fayol, Laboratoire Léon Brillouin (LLB - UMR 12), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay, Hunan Normal University, Spitzer Science Center, California Institute of Technology (CALTECH), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique Théorique - UMR 6207 (CPT), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, Astronomy, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Hunan Normal University (HNU), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), and Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, STAR-FORMATION, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], MORPHOLOGICAL CLASSIFICATION, 0103 physical sciences, Range (statistics), PHOTOMETRIC REDSHIFTS, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Galaxies: evolution, Galaxies: fundamental parameters, Galaxies: general, Astronomy and Astrophysics, Space and Planetary Science, DIGITAL-SKY-SURVEY, 010308 nuclear & particles physics, FORMATION HISTORIES, HUBBLE DEEP FIELD, Order (ring theory), galaxies: fundamental parameters, ENVIRONMENTAL DEPENDENCE, Redshift survey, galaxies: general, Redshift, Galaxy, Bimodality, LUMINOSITY FUNCTION, SPECTROSCOPIC SAMPLE, STELLAR MASS FUNCTION, Cube, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Our goal is to develop a new and reliable statistical method to classify galaxies from large surveys. We probe the reliability of the method by comparing it with a three-dimensional classification cube, using the same set of spectral, photometric and morphological parameters.We applied two different methods of classification to a sample of galaxies extracted from the zCOSMOS redshift survey, in the redshift range 0.5 < z < 1.3. The first method is the combination of three independent classification schemes, while the second method exploits an entirely new approach based on statistical analyses like Principal Component Analysis (PCA) and Unsupervised Fuzzy Partition (UFP) clustering method. The PCA+UFP method has been applied also to a lower redshift sample (z < 0.5), exploiting the same set of data but the spectral ones, replaced by the equivalent width of H$��$. The comparison between the two methods shows fairly good agreement on the definition on the two main clusters, the early-type and the late-type galaxies ones. Our PCA-UFP method of classification is robust, flexible and capable of identifying the two main populations of galaxies as well as the intermediate population. The intermediate galaxy population shows many of the properties of the green valley galaxies, and constitutes a more coherent and homogeneous population. The fairly large redshift range of the studied sample allows us to behold the downsizing effect: galaxies with masses of the order of $3\cdot 10^{10}$ Msun mainly are found in transition from the late type to the early type group at $z>0.5$, while galaxies with lower masses - of the order of $10^{10}$ Msun - are in transition at later epochs; galaxies with $M 5\cdot 10^{10}$ Msun) mostly completed their transition before $z\sim 1$., 16 pages, 14 figures, accepted for publication in A&A
Published: 2010
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43. The XMM-Newton Wide-Field Survey in the COSMOS field (XMM-COSMOS): demography and multiwavelength properties of obscured and unobscured luminous AGN

Author: BRUSA, MARCELLA, LUSSO, ELISABETA, VIGNALI, CRISTIAN, Civano F., Comastri A., Miyaji T., Salvato M., Zamorani G., Cappelluti N., Fiore F., Hasinger G., Mainieri V., Merloni A., Bongiorno A., Capak P., Elvis M., Gilli R., Hao H., Jahnke K., Koekemoer A. M., Ilbert O., Le Floc'h E., Mignoli M., Schinnerer E., Silverman J. D., Treister E., Trump J. D., Zamojski M., Aldcroft T., Aussel H., Bardelli S., Bolzonella M., Cappi A., Caputi K., Contini T., Finoguenov A., Fruscione A., Garilli B., Impey C. D., Iovino A., Iwasawa K., Kampczyk P., Kartaltepe J., Kneib J. P., Knobel C., Kovac K., Lamareille F., Leborgne J. F., Le Brun V., Le Fevre O., Lilly S. J., Maier C., McCracken H. J., Pello R., Peng Y. J, Perez Montero E., de Ravel L., Sanders D., Scodeggio M., Scoville N. Z., Tanaka M., Taniguchi Y., Tasca L., de la Torre S., Tresse L., Vergani D., Zucca E., Brusa M., Civano F., Comastri A., Miyaji T., Salvato M., Zamorani G., Cappelluti N., Fiore F., Hasinger G., Mainieri V., Merloni A., Bongiorno A., Capak P., Elvis M., Gilli R., Hao H., Jahnke K., Koekemoer A. M., Ilbert O., Le Floc'h E., Lusso E., Mignoli M., Schinnerer E., Silverman J. D., Treister E., Trump J. D., Vignali C., Zamojski M., Aldcroft T., Aussel H., Bardelli S., Bolzonella M., Cappi A., Caputi K., Contini T., Finoguenov A., Fruscione A., Garilli B., Impey C. D., Iovino A., Iwasawa K., Kampczyk P., Kartaltepe J., Kneib J. P., Knobel C., Kovac K., Lamareille F., Leborgne J.-F., Le Brun V., Le Fevre O., Lilly S. J., Maier C., McCracken H. J., Pello R., Peng Y-J, Perez-Montero E., de Ravel L., Sanders D., Scodeggio M., Scoville N. Z., Tanaka M., Taniguchi Y., Tasca L., de la Torre S., Tresse L., Vergani D., and Zucca E.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, galaxies: active – surveys – X-rays: diffuse background – X-rays: galaxies – X-rays: general, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report the final optical identifications of the medium-depth (~60 ksec), contiguous (2 deg^2) XMM-Newton survey of the COSMOS field. XMM-Newton has detected ~800 X-ray sources down to limiting fluxes of ~5x10^{-16}, ~3x10^{-15}, and ~7x10^{-15} erg/cm2/s in the 0.5-2 keV, 2-10 keV and 5-10 keV bands, respectively. The work is complemented by an extensive collection of multi-wavelength data from 24 micron to UV, available from the COSMOS survey, for each of the X-ray sources, including spectroscopic redshifts for ~50% of the sample, and high-quality photometric redshifts for the rest. The XMM and multiwavelength flux limits are well matched: 1760 (98%) of the X-ray sources have optical counterparts, 1711 (~95%) have IRAC counterparts, and 1394 (~78%) have MIPS 24micron detections. Thanks to the redshift completeness (almost 100%) we were able to constrain the high-luminosity tail of the X-ray luminosity function confirming that the peak of the number density of logL_X>44.5 AGN is at z~2. Spectroscopically-identified obscured and unobscured AGN, as well as normal and starforming galaxies, present well-defined optical and infrared properties. We devised a robust method to identify a sample of ~150 high redshift (z>1), obscured AGN candidates for which optical spectroscopy is not available. We were able to determine that the fraction of the obscured AGN population at the highest (L_X>10^{44} erg s^{-1}) X-ray luminosity is ~15-30% when selection effects are taken into account, providing an important observational constraint for X-ray background synthesis. We studied in detail the optical spectrum and the overall spectral energy distribution of a prototypical Type 2 QSO, caught in a stage transitioning from being starburst dominated to AGN dominated, which was possible to isolate only thanks to the combination of X-ray and infrared observations., ApJ, in press. 59 pages, 14 figures, 2 Tables. A few typos corrected and a reference added. Table 2 is also available at http://www.mpe.mpg.de/XMMCosmos/xmm53_release ; a version of the paper in ApJ format (27 pages) is available at http://www.mpe.mpg.de/XMMCosmos/xmm53_release/brusa_xmmcosmos_optid.pdf
Published: 2010
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44. Understanding the shape of the galaxy two-point correlation function at z ~= 1 in the COSMOS field

Author: de la Torre S., Guzzo L., Kova, #269, Porciani C., Abbas U., Meneux B., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Lilly S. J., Mainieri V., Renzini A., Sanders D., Scodeggio M., Scoville N., Zamorani G., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Coppa G., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., Koekemoer A. M., Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Mignoli M., Pelló R., Peng Y., Perez Montero E., Ricciardelli E., Silverman J., Tanaka M., Tasca L., Tresse L., Vergani D., Welikala N., Zucca E., Bottini D., Cappi A., Cassata P., Fumana M., Ilbert O., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Nair P., Oesch P., Pozzetti L., Presotto V., Scaramella R., CUCCIATI, OLGA, CIMATTI, ANDREA, de la Torre S., Guzzo L., Kova&#269, K., Porciani C., Abbas U., Meneux B., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Lilly S. J., Mainieri V., Renzini A., Sanders D., Scodeggio M., Scoville N., Zamorani G., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Coppa G., Cucciati O., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., Koekemoer A. M., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Mignoli M., Pelló R., Peng Y., Perez-Montero E., Ricciardelli E., Silverman J., Tanaka M., Tasca L., Tresse L., Vergani D., Welikala N., Zucca E., Bottini D., Cappi A., Cassata P., Cimatti A., Fumana M., Ilbert O., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Nair P., Oesch P., Pozzetti L., Presotto V., and Scaramella R.
Published: 2010

45. The [O iii] emission line luminosity function of optically selected type-2 AGN from zCOSMOS

Author: Bongiorno A., Mignoli M., Zamorani G., Lamareille F., LANZUISI, GIORGIO, Miyaji T., Bolzonella M., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Lilly S. J., Mainieri V., Renzini A., Scodeggio M., Bardelli S., Caputi K., Civano F., Coppa G., de La Torre S., de Ravel L., Franzetti P., Garilli B., Halliday C., Hasinger G., Koekemoer A. M., Iovino A., Kampczyk P., Knobel C., Kova, #269, Le Borgne J. F., Le Brun V., Maier C., Merloni A., Nair P., Pello R., Peng Y., Perez Montero E., Ricciardelli E., Salvato M., Silverman J., Tanaka M., Tasca L., Tresse L., Vergani D., Zucca E., Abbas U., Bottini D., Cappi A., Cassata P., Guzzo L., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Oesch P., Porciani C., Pozzetti L., Scaramella R., BRUSA, MARCELLA, CUCCIATI, OLGA, CIMATTI, ANDREA, Bongiorno A., Mignoli M., Zamorani G., Lamareille F., Lanzuisi G., Miyaji T., Bolzonella M., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Lilly S. J., Mainieri V., Renzini A., Scodeggio M., Bardelli S., Brusa M., Caputi K., Civano F., Coppa G., Cucciati O., de La Torre S., de Ravel L., Franzetti P., Garilli B., Halliday C., Hasinger G., Koekemoer A. M., Iovino A., Kampczyk P., Knobel C., Kova&#269, K., Le Borgne J.-F., Le Brun V., Maier C., Merloni A., Nair P., Pello R., Peng Y., Perez Montero E., Ricciardelli E., Salvato M., Silverman J., Tanaka M., Tasca L., Tresse L., Vergani D., Zucca E., Abbas U., Bottini D., Cappi A., Cassata P., Cimatti A., Guzzo L., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Oesch P., Porciani C., Pozzetti L., Scaramella R., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Astronomy
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Type (model theory), Surveys, 01 natural sciences, Luminosity, 0103 physical sciences, Galaxies: active, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Density evolution, 0105 earth and related environmental sciences, Line (formation), Luminosity function (astronomy), Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Redshift, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a catalog of 213 type-2 AGN selected from the zCOSMOS survey. The selected sample covers a wide redshift range (0.15, Comment: 20 pages, 11 figures, accepted for publication in Astronomy and Astrophysics
Published: 2010
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46. Tracking the impact of environment on the galaxy stellar mass function up to z â¼ 1 in the 10 k zCOSMOS sample

Author: Bolzonella M., Kova, #269, Pozzetti L., Zucca E., Lilly S. J., Peng Y., Iovino A., Zamorani G., Vergani D., Tasca L. A. M., Lamareille F., Oesch P., Caputi K., Kampczyk P., Bardelli S., Maier C., Abbas U., Knobel C., Scodeggio M., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Mainieri V., Renzini A., Bongiorno A., Coppa G., de la Torre S., de Ravel L., Franzetti P., Garilli B., Le Borgne J. F., Le Brun V., Mignoli M., Pelló R., Perez Montero E., Ricciardelli E., Silverman J. D., Tanaka M., Tresse L., Bottini D., Cappi A., Cassata P., Guzzo L., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Porciani C., Scaramella R., Aussel H., Capak P., Halliday C., Ilbert O., Kartaltepe J., Salvato M., Sanders D., Scarlata C., Scoville N., Taniguchi Y., Thompson D., CUCCIATI, OLGA, CIMATTI, ANDREA, Bolzonella M., Kova&#269, K., Pozzetti L., Zucca E., Cucciati O., Lilly S. J., Peng Y., Iovino A., Zamorani G., Vergani D., Tasca L. A. M., Lamareille F., Oesch P., Caputi K., Kampczyk P., Bardelli S., Maier C., Abbas U., Knobel C., Scodeggio M., Carollo C. M., Contini T., Kneib J.-P., Le Fèvre O., Mainieri V., Renzini A., Bongiorno A., Coppa G., de la Torre S., de Ravel L., Franzetti P., Garilli B., Le Borgne J.-F., Le Brun V., Mignoli M., Pelló R., Perez-Montero E., Ricciardelli E., Silverman J. D., Tanaka M., Tresse L., Bottini D., Cappi A., Cassata P., Cimatti A., Guzzo L., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Porciani C., Scaramella R., Aussel H., Capak P., Halliday C., Ilbert O., Kartaltepe J., Salvato M., Sanders D., Scarlata C., Scoville N., Taniguchi Y., Thompson D., INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), AUTRES, INAF- Milano, Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), INAF - Osservatorio Astronomico di Brera (OAB), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), University of Chicago, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Human Genetics Center, The University of Texas Health Science Center at Houston (UTHealth), School of Biotechnology and Biomolecular Sciences, University of New South Wales [Sydney] (UNSW), Space Telescope Science Institute (STSci), Centre de Physique Théorique - UMR 6207 (CPT), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), California Institute of Technology (CALTECH), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Materials & Process technology, Boeing Company [Chicago], Sea Mammal Research Unit, St Andrews, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Photometry (optics), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Galaxy formation and evolution, Density contrast, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Star formation, galaxies: fundamental parameters, Astronomy and Astrophysics, Redshift, Galaxy, Bimodality, galaxies: luminosity function, mass function, Space and Planetary Science, cosmology: observations, galaxies: evolution, galaxies: luminosity function, mass function, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We study the impact of the environment on the evolution of galaxies in the zCOSMOS 10k sample in the redshift range 0.1, Comment: 17 pages, 11 figures. Version accepted for publication in Astronomy and Astrophysics, including referee's suggestions, a new section with comparison with literature data, and updated references
Published: 2010
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47. The Density Field of the 10k zCOSMOS Galaxies

Author: Kova, #269, Lilly S. J., Porciani C., Iovino A., Zamorani G., Oesch P., Bolzonella M., Knobel C., Finoguenov A., Peng Y., Carollo C. M., Pozzetti L., Caputi K., Silverman J. D., Tasca L. A. M., Scodeggio M., Vergani D., Scoville N. Z., Capak P., Contini T., Kneib J. P., Le Fèvre O., Mainieri V., Renzini A., Bardelli S., Bongiorno A., Coppa G., de la Torre S., de Ravel L., Franzetti P., Garilli B., Guzzo L., Kampczyk P., Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Mignoli M., Pello R., Perez Montero E., Ricciardelli E., Tanaka M., Tresse L., Zucca E., Abbas U., Bottini D., Cappi A., Cassata P., Fumana M., Koekemoer A. M., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Scaramella R., CUCCIATI, OLGA, CIMATTI, ANDREA, Centre de Physique Théorique - UMR 6207 (CPT), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Kova&#269, K., Lilly S. J., Cucciati O., Porciani C., Iovino A., Zamorani G., Oesch P., Bolzonella M., Knobel C., Finoguenov A., Peng Y., Carollo C. M., Pozzetti L.,Caputi K., Silverman J. D., Tasca L. A. M., Scodeggio M., Vergani D., Scoville N. Z., Capak P., Contini T., Kneib J.-P., Le Fèvre O., Mainieri V., Renzini A., Bardelli S., Bongiorno A., Coppa G., de la Torre S., de Ravel L., Franzetti P., Garilli B., Guzzo L., Kampczyk P., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Mignoli M., Pello R., Perez Montero E., Ricciardelli E., Tanaka M., Tresse L., Zucca E., Abbas U., Bottini D., Cappi A., Cassata P., Cimatti A., Fumana M., Koekemoer A. M., Maccagni D., Marinoni C., McCracken H. J.,Memeo P., Meneux B., Scaramella R., Astronomy, and Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), FOS: Physical sciences, Scale (descriptive set theory), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], LY-ALPHA EMITTERS, surveys, galaxies: high-redshift, 0103 physical sciences, LARGE-SCALE STRUCTURE, 010303 astronomy & astrophysics, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, large-scale structure of universe, REDSHIFT SURVEY, 010308 nuclear & particles physics, Shot noise, Astronomy and Astrophysics, VLT DEEP SURVEY, ENVIRONMENTAL DEPENDENCE, Galaxy, Redshift, COSMOS FIELD, Space and Planetary Science, Galaxies: high-redshift, Large-scale structure of universe, Surveys, SMOOTHED PARTICLE HYDRODYNAMICS, LUMINOSITY DEPENDENCE, DIGITAL SKY SURVEY, STELLAR MASS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use the current sample of ~10,000 zCOSMOS spectra of sources selected with I(AB) < 22.5 to define the density field out to z~1, with much greater resolution in the radial dimension than has been possible with either photometric redshifts or weak lensing. We apply new algorithms that we have developed (ZADE) to incorporate objects not yet observed spectroscopically by modifying their photometric redshift probability distributions using the spectroscopic redshifts of nearby galaxies. This strategy allows us to probe a broader range of galaxy environments and reduce the Poisson noise in the density field. The reconstructed overdensity field of the 10k zCOSMOS galaxies consists of cluster-like patterns surrounded by void-like regions, extending up to z~1. Some of these structures are very large, spanning the ~50 Mpc/h transverse direction of the COSMOS field and extending up to Delta z~0.05 in redshift. We present the three dimensional overdensity maps and compare the reconstructed overdensity field to the independently identified virialised groups of galaxies and clusters detected in the visible and in X-rays. The distribution of the overdense structures is in general well traced by these virialised structures. A comparison of the large scale structures in the zCOSMOS data and in the mock catalogues reveals an excellent agreement between the fractions of the volume enclosed in structures of all sizes above a given overdensity between the data and the mocks in 0.2, Comment: 35 pages, 20 figures; submitted to ApJ; the high resolution pdf available at http://www.exp-astro.phys.ethz.ch/kovac/public/zCOSMOS
Published: 2010
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48. The star formation rate cookbook at 1 < z < 3: Extinction-corrected relations for UV & [OII]��3727 luminosities

Author: Talia, M., Cimatti, A., Pozzetti, L., Rodighiero, G., Gruppioni, C., Pozzi, F., Daddi, E., Maraston, C., Mignoli, M., and Kurk, J.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We use a spectroscopic sample of 286 star-forming galaxies (SFGs) at 1, Accepted for publication in A&A; 20 pages, 19 figures, 5 tables
Published: 2015
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49. On the cosmic evolution of the scaling relations between black holes and their host galaxies: Broad Line AGN in the zCOSMOS survey

Author: Merloni, A., Bongiorno, A., Bolzonella, M., Brusa, M., Civano, F., Comastri, A., Elvis, M., Fiore, F., Gilli, R., Hao, H., Jahnke, K., Koekemoer, A. M., Lusso, E., Mainieri, V., Mignoli, M., Miyaji, T., Renzini, A., Salvato, M., Silverman, J., Trump, J., Vignali, C., Zamorani, G., Capak, P., Lilly, S. J., Sanders, D., Taniguchi, Y., Bardelli, S., Carollo, C. M., Caputi, K., Contini, T., Coppa, G., Cucciati, O., de la Torre, S., de Ravel, L., Franzetti, P., Garilli, B., Hasinger, G., Impey, C., Iovino, A., Iwasawa, K., Kampczyk, P., Kneib, J. -P., Knobel, C., Kovac, K., Lamareille, F., Borgne, J. -F. Le, Brun, V. Le, Fevre, O. Le, Maier, C., Pello, R., Peng, Y., Montero, E. Perez, Ricciardelli, E., Scodeggio, M., Tanaka, M., Tasca, L. A. M., Tresse, L., Vergani, D., Zucca, E., Merloni A., Bongiorno A., Bolzonella M., Brusa M., Civano F., Comastri A., Elvis M., Fiore F., Gilli R., Hao H., Jahnke K., Koekemoer A.M., Lusso E., Mainieri V., Mignoli M., Miyaji T., Renzini A., Salvato M., Silverman J., Trump J., Vignali C., Zamorani G., Capak P., Lilly S.J., Sanders D., Taniguchi Y., Bardelli S., Carollo C.M., Caputi K., Contini T., Coppa G., Cucciati O., de la Torre S., de Ravel L., Franzetti P., Garilli B., Hasinger G., Impey C., Iovino A., Iwasawa K., Kampczyk P., Kneib J.-P., Knobel C., Kovac K., Lamareille F., Le Borgne J.-F., Le Brun V., Le Fevre O., Maier C., Pello R., Peng Y., Perez Montero E., Ricciardelli E., Scodeggio M., Tanaka M., Tasca L. A. M., Tresse L., Vergani D., and Zucca E.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), cosmology: observations – galaxies: active – galaxies: evolution – quasars: emission lines, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: (Abriged) We report on the measurement of the rest frame K-band luminosity and total stellar mass of the hosts of 89 broad line Active Galactic Nuclei detected in the zCOSMOS survey in the redshift range 1, Comment: 47 pages, 8 figures. Accepted for publication in ApJ
Published: 2009

50. The zCOSMOS Redshift Survey: How group environment alters global downsizing trends

Author: Iovino A., Scodeggio M., Knobel C., Kova, #269, Lilly S., Bolzonella M., Tasca L. A. M., Zamorani G., Zucca E., Caputi K., Pozzetti L., Oesch P., Lamareille F., Halliday C., Bardelli S., Finoguenov A., Guzzo L., Kampczyk P., Maier C., Tanaka M., Vergani D., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Mainieri V., Renzini A., Bongiorno A., Coppa G., de La Torre S., de Ravel L., Franzetti P., Garilli B., Le Borgne J. F., Le Brun V., Mignoli M., Pellò R., Peng Y., Perez Montero E., Ricciardelli E., Silverman J. D., Tresse L., Abbas U., Bottini D., Cappi A., Cassata P., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Porciani C., Scaramella R., Schiminovich D., Scoville N., CUCCIATI, OLGA, CIMATTI, ANDREA, AUTRES, Dipartimento di Fisica, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), INAF- Milano, Istituto Nazionale di Astrofisica (INAF), Università di Bologna, Dipartimento di Astronomia, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), INAF - Osservatorio Astronomico di Brera (OAB), INAF - Osservatorio Astronomico di Bologna (OABO), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Tokai University, INAF - Osservatorio Astrofisico di Arcetri (OAA), University of Chicago, Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Space Telescope Science Institute (STSci), Centre de Physique Théorique - UMR 6207 (CPT), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), California Institute of Technology (CALTECH), Iovino A., Cucciati O., Scodeggio M., Knobel C., Kova&#269, K., Lilly S., Bolzonella M., Tasca L. A. M., Zamorani G., Zucca E., Caputi K., Pozzetti L., Oesch P., Lamareille F., Halliday C., Bardelli S., Finoguenov A., Guzzo L., Kampczyk P., Maier C., Tanaka M., Vergani D., Carollo C. M., Contini T., Kneib J.-P., Le Fèvre O., Mainieri V., Renzini A., Bongiorno A., Coppa G., de La Torre S., de Ravel L., Franzetti P., Garilli B., Le Borgne J.-F., Le Brun V., Mignoli M., Pellò R., Peng Y., Perez-Montero E., Ricciardelli E., Silverman J. D., Tresse L., Abbas U., Bottini D., Cappi A., Cassata P., Cimatti A., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Porciani C., Scaramella R., Schiminovich D., Scoville N., Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), and Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Interactions, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, Clusters, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Galaxy formation and evolution, Mass segregation, Evolution - Galaxies, Galaxies, General - Galaxies, Astronomy and Astrophysics, Space and Planetary Science, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Redshift survey, Galaxy, Redshift, Low Mass, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We took advantage of the wealth of information provided by the first ~10000 galaxies of the zCOSMOS-bright survey and its group catalogue to study the complex interplay between group environment and galaxy properties. The classical indicator F_blue (fraction of blue galaxies) proved to be a simple but powerful diagnostic tool. We studied its variation for different luminosity and mass selected galaxy samples. Using rest-frame B-band selected samples, the groups galaxy population exhibits significant blueing as redshift increases, but maintains a lower F_blue with respect both to the global and the isolated galaxy population. However moving to mass selected samples it becomes apparent that such differences are largely due to the biased view imposed by the B-band luminosity selection, being driven by the population of lower mass, bright blue galaxies for which we miss the redder, equally low mass, counterparts. By focusing the analysis on narrow mass bins such that mass segregation becomes negligible we find that only for the lowest mass bin explored (logMass = 10.8 are already in place at z ~ 1 and do not exhibit any strong environmental dependence, possibly originating from so-called 'nature'/internal mechanisms. In contrast, for lower galaxy masses and redshifts lower than z ~ 1, we observe the emergence in groups of a population of 'nurture' red galaxies: slightly deviating from the trend of the downsizing scenario followed by the global galaxy population, and more so with cosmic time. These galaxies exhibit signatures of group-related secular physical mechanisms directly influencing galaxy evolution., Submitted to A&A, revised version after referee comments
Published: 2009
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