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Your search keyword '"ARNABOLDI M."' showing total 41 results
Start Over Author "ARNABOLDI M." Topic astronomy and astrophysics
41 results on '"ARNABOLDI M."'

1. The extended Planetary Nebula Spectrograph (ePN.S) early-type galaxy survey: The specific angular momentum of ETGs

Author

Pulsoni, C., Gerhard, O., Fall, S. M., Arnaboldi, M., Ennis, A. I., Hartke, J., Coccato, L., and Napolitano, N. R.

Subjects
Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

Mass and angular momentum are key parameters of galaxies. Their co-evolution establishes an empirical relation between the specific stellar angular momentum j* and the stellar mass M* that depends on morphology. In this work, we measure j* in a sample of 32 early type galaxies (ETGs) from the ePN.S survey, using full 2D kinematic information out to a mean 6Re. We present lambda and j* profiles. We derive the distribution of these galaxies on the total j*-M* plane and determine the ratio between the stellar j* and the specific angular momentum of the host dark matter halo. The radially extended, 2D kinematic data show that the stellar halos of ETGs do not contain large stellar mass fractions of high j*. The j*-profiles of fast-rotator ETGs are largely converged within the range of the data. For slow rotators, j* is still rising and is estimated to increase beyond 6Re by up to 40%. More than 60% of their halo angular momentum is in misaligned rotation. We find that the ePN.S ETG sample displays the well-known correlation between j*, M*, and morphology: elliptical galaxies have systematically lower j* than similar mass S0 galaxies. However, fast and slow rotators lie on the same relation within errors with the slow rotators falling at the high M* end. A power-law fit to the j*-M* relation gives a slope of 0.55+-0.17 for the S0s and 0.76+-0.23 for the ellipticals, with normalisation about 4 and 9 times lower than spirals, respectively. The estimated retained fraction of angular momentum at 10^10-10^10.5 Msun is 25% for S0s and >10% for ellipticals, and decreases by 1.5 orders of magnitude at M*~10^12 Msun. Our results show that ETGs have substantially lower j* than spiral galaxies with similar M*. Their j* must be lost during their evolution, and/or retained in the hot gas component and the satellite galaxies that have not yet merged with the central galaxy. [abridged], 26 pages, 14 figures, accepted for publication in A&A

Published
2023

2. The Fornax Cluster VLT Spectroscopic Survey:IV. cold kinematical substructures in the Fornax core from COSTA

Author

Napolitano, N. R., Gatto, M., Spiniello, C., Cantiello, M., Hilker, M., Arnaboldi, M., Tortora, C., Chaturvedi, A., D'Abrusco, R., Li, R., Paolillo, M., Peletier, R., Saifollahi, T., Spavone, M., Venhola, A., Pota, V., Capaccioli, M., Longo, G., Napolitano, N. R., Gatto, M., Spiniello, C., Cantiello, M., Hilker, M., Arnaboldi, M., Tortora, C., Chaturvedi, A., D'Abrusco, R., Li, R., Paolillo, M., Peletier, R., Saifollahi, T., Spavone, M., Venhola, A., Capaccioli, M., Longo, G., and Astronomy

Subjects
Physics, formation [galaxies], interactions [galaxies], FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Core (optical fiber), intergalactic medium, galaxies: interactions, galaxies: formation, galaxies: kinematics and dynamics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), kinematics and dynamics [galaxies], galaxies: interactions, galaxies: formation, Astrophysics::Solar and Stellar Astrophysics, intergalactic medium, Fornax Cluster, galaxies: kinematics and dynamics, Astrophysics::Galaxy Astrophysics
Abstract

The COld STream finder Algorithm (COSTA) is a novel algorithm to find streams in the phase space of planetary nebulae (PNe) and globular cluster (GCs) populations. COSTA isolates groups of particles with small velocity dispersion, using an iterative sigma-clipping over a defined number of neighbor particles. We have applied COSTA to a catalog of about 2000 PNe and GCs from the Fornax Cluster VLT Spectroscopic Survey (FVSS), within 200 kpc from the cluster core, to detect cold substructures and characterize their kinematics. We have found 13 cold substructures, with velocity dispersion ranging from 20 to 100 kms^{-1}, which are likely associated either to large galaxies or to ultra-compact dwarf (UCD) galaxies in the Fornax core. These streams show a clear correlation of their luminosity with the internal velocity dispersion, and their surface brightness with size and distance from the cluster center that are compatible with dissipative processes producing them. However, we cannot exclude that some of these substructures have formed by violent relaxation of massive satellites finally merged into the central galaxy. Among these substructures we have: a stream connecting NGC1387 to the central galaxy, NGC1399, previously reported in literature; a new giant stream produced by the interaction of NGC1382 with NGC1380 and possibly NGC1381; a series of streams kinematically connected to nearby ultra compact dwarf galaxies; clumps of tracers with no clear kinematical association to close cluster members. We show evidence for a variety of cold substructure predicted in simulations. Most of the streams are kinematically connected to UCDs, supporting the scenario that they can be remnants of disrupted dwarf systems. [abridged], 27 Pages, 15 Figures. Accepted for publication in Astronomy and Astrophysics

Published
2022

3. Resolving the Disc–Halo Degeneracy – II: NGC 6946

Author

Aniyan, S, Ponomareva, A A, Freeman, K C, Arnaboldi, M, Gerhard, O E, Coccato, L, Kuijken, K, and Merrifield, M

Subjects
Space and Planetary Science, Astronomy and Astrophysics
Abstract

The mass-to-light ratio (M/L) is a key parameter in decomposing galactic rotation curves into contributions from the baryonic components and the dark halo of a galaxy. One direct observational method to determine the disc M/L is by calculating the surface mass density of the disc from the stellar vertical velocity dispersion and the scale height of the disc. Usually, the scale height is obtained from near-IR studies of edge-on galaxies and pertains to the older, kinematically hotter stars in the disc, while the vertical velocity dispersion of stars is measured in the optical band and refers to stars of all ages (up to ∼10 Gyr) and velocity dispersions. This mismatch between the scale height and the velocity dispersion can lead to underestimates of the disc surface density and a misleading conclusion of the submaximality of galaxy discs. In this paper, we present the study of the stellar velocity dispersion of the disc galaxy NGC 6946 using integrated star light and individual planetary nebulae as dynamical tracers. We demonstrate the presence of two kinematically distinct populations of tracers that contribute to the total stellar velocity dispersion. Thus, we are able to use the dispersion and the scale height of the same dynamical population to derive the surface mass density of the disc over a radial extent. We find the disc of NGC 6946 to be closer to maximal with the baryonic component contributing most of the radial gravitational field in the inner parts of the galaxy (Vmax(bar) = 0.76(±0.14)Vmax).

Published
2021

4. Globular clusters in M31, Local Group, and external galaxies

Author

Larsen, S.S., Bragaglia, A., Arnaboldi, M., Rejkuba, M., and Romano, D.

Subjects
Physics, 010504 meteorology & atmospheric sciences, Astronomy, Local Group, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Galaxy groups and clusters, Space and Planetary Science, Galaxy group, Globular cluster, 0103 physical sciences, Elliptical galaxy, 010303 astronomy & astrophysics, Galaxy cluster, 0105 earth and related environmental sciences, Open cluster
Abstract

Throughout most of the Local Group, globular clusters (GCs) remain recognisable as extended objects in ground-based images taken in good seeing conditions. However, studying the full extent of the GC systems is challenging because of the large sky area that needs to be surveyed and recent years have seen dramatic progress in our knowledge of GC populations in nearby galaxies, thanks to large imaging surveys. At the same time, techniques for deriving detailed abundances from integrated-light spectra of GCs are maturing so that detailed comparisons of the chemical composition for GCs in different galaxies can now be made. Such comparisons may shed important light on the properties of proto-galactic fragments that were accreted onto galaxy halos. Nevertheless, our census of Local Group GCs probably remains far from complete, in particular at low luminosities and for very extended clusters.

Published
2016

5. Chemical Abundances of Metal-poor stars in Dwarf Galaxies

Author

Venn, Kim A., Jablonka, Pascale, Hill, Vanessa, Starkenburg, Else, Lemasle, Bertrand, Shetrone, Matthew, Irwin, Mike, Norris, John, Yong, David, Gilmore, Gerry, Salvadori, Stephania, Skuladottir, Asa, Tolstoy, Eline, Bragaglia, A., Arnaboldi, M., Rejkuba, M., Romano, D., and Astronomy

Subjects
Physics, Spiral galaxy, stars: abundances, K-type main-sequence star, Dwarf galaxy problem, Astronomy, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: dwarf, stellar content, Dwarf spheroidal galaxy, Space and Planetary Science, Globular cluster, evolution, Elliptical galaxy, Local Group, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Dwarf galaxy, Luminosity function (astronomy)
Abstract

Stars in low-mass dwarf galaxies show a larger range in their chemical properties than those in the Milky Way halo. The slower star formation efficiency make dwarf galaxies ideal systems for testing nucleosynthetic yields. Not only are alpha-poor stars found at lower metallicities, and a higher fraction of carbon-enhanced stars, but we are also finding stars in dwarf galaxies that appear to be iron-rich. These are compared with yields from a variety of supernova predictions.

Published
2016

6. Direct imaging of haloes and truncations in face-on nearby galaxies

Author

Knapen, J. H., Peters, S. P. C., van der Kruit, P. C., Trujillo, I., Fliri, J., Cisternas, M., Kelvin, L. S., Bragaglia, A., Arnaboldi, M., Rejkuba, M., Romano, D., and Astronomy

Subjects
Luminous infrared galaxy, Physics, Spiral galaxy, Astronomy, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Peculiar galaxy, Space and Planetary Science, Galaxies: structure, Galaxy group, Galaxy formation and evolution, Elliptical galaxy, Astrophysics::Solar and Stellar Astrophysics, Disc, Galaxies: haloes, Galaxies: spiral, Astrophysics::Galaxy Astrophysics
Abstract

We use ultra-deep imaging from the IAC Stripe 82 Legacy Project to study the surface photometry of 22 nearby, face-on to moderately inclined spiral galaxies. The reprocessed and co-added SDSS/Stripe 82 imaging allows us to probe down to 29–30 r′-mag/arcsec2 and thus reach into the very faint outskirts of the galaxies. We find extended stellar haloes in over half of our sample galaxies, and truncations in three of them. The presence of stellar haloes and truncations is mutually exclusive, and we argue that the presence of a stellar halo can hide a truncation. We find that the onset of the halo and the truncation scales tightly with galaxy size. We highlight the importance of a proper analysis of the extended wings of the point spread function (PSF), finding that around half the light at the faintest levels is from the inner regions of a galaxy, though not the nucleus, re-distributed to the outskirts by the PSF. We discuss implications of this effect for future deep imaging surveys, such as with the LSST.

Published
2016

7. Mapping the inner regions of the polar disk galaxy NGC 4650A with MUSE

Author

Iodice, E., Coccato, L., Combes, F., De Zeeuw, T., Arnaboldi, M., Weilbacher, P., Bacon, R., Kuntschner, H., Spavone, M., Gerin, Maryvonne, Falgarone, Edith, Godard, Benjamin, Lis, Darek, RTM - Alpes de Haute Provence - Digne les Bains, ONF - RTM - Alpes de Haute Provence - Digne les Bains, Chaire Galaxies et cosmologie, Collège de France (CdF (institution)), INAF - Osservatorio Astronomico di Capodimonte (OAC), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), ITA, FRA, DEU, NLD, INAF-Astronomical Observatory of Capodimonte, via Moiariello 16, 80131, Naples, Italy, European Southern Observatory (ESO), École normale supérieure - Paris (ENS-PSL), Collège de France - Chaire Galaxies et cosmologie, Astrophysikalisches Institut Potsdam (AIP), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Polar, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS
Abstract

[abridged] The polar disk galaxy NGC4650A was observed during the commissioning of the MUSE at the ESO VLT to obtain the first 2D map of the velocity and velocity dispersion for both stars and gas. The new MUSE data allow the analysis of the structure and kinematics towards the central regions of NGC4650A, where the two components co-exist. These regions were unexplored by the previous long-slit literature data available for this galaxy. The extended view of NGC~4650A given by the MUSE data is a galaxy made of two perpendicular disks that remain distinct and drive the kinematics right into the very centre of this object. In order to match this observed structure for NGC4650A, we constructed a multicomponent mass model made by the combined projection of two disks. By comparing the observations with the 2D kinematics derived from the model, we found that the modelled mass distribution in these two disks can, on average, account for the complex kinematics revealed by the MUSE data, also in the central regions of the galaxy where the two components coexist. This result is a strong constraint on the dynamics and formation history of this galaxy; it further supports the idea that polar disk galaxies like NGC~4650A were formed through the accretion of material that has different angular momentum., 14 pages, 10 figures; accepted for publication in Astronomy & Astrophysics

Published
2015

8. Building blocks of the Milky Way's stellar halo

Author

Oirschot, P. van, Starkenburg, E., Helmi, A., Nelemans, G.A., Bragaglia, A., Arnaboldi, M., Rejkuba, M., Romano, D., and Kapteyn Astronomical Institute

Subjects
Physics, Stellar kinematics, Stellar population, Astronomy, Milky Way, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Dark matter halo, Galactic halo, Space and Planetary Science, Galaxy group, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Dwarf galaxy
Abstract

We study the assembly history of the stellar halo of Milky Way-like galaxies using the six high-resolution Aquarius dark matter simulations combined with the Munich-Groningen semi-analytic galaxy formation model. Our goal is to understand the stellar population contents of the building blocks of the Milky Way halo, including their star formation histories and chemical evolution, as well as their internal dynamical properties. We are also interested in how they relate or are different from the surviving satellite population. Finally, we will use our models to compare to observations of halo stars in an attempt to reconstruct the assembly history of the Milky Way's stellar halo itself.

Published
2015

9. The VIMOS VLT Deep Survey - The evolution of galaxy clustering to z=2 from first epoch observations

Author

Le Fèvre O., Guzzo L., Meneux B., Pollo A., Cappi A., Colombi S., Iovino A., Marinoni C., McCracken H. J., Scaramella R., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J. P., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Arnouts S., Bardelli S., Blaizot J., Bolzonella M., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Gavignaud I., Ilbert O., Mathez G., Mazure A., Merighi R., Paltani S., Pellò R., Pozzetti L., Radovich M., Zamorani G., Zucca E., Bondi M., Busarello G., Lamareille F., Mellier Y., Merluzzi P., Ripepi V., Rizzo D. ns Astronomy, Astrophysics Volume 439 Issue 3 September I. 2005 p.p. 877 885, MARANO, BRUNO, BONGIORNO, ANGELA, 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), 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), Le Fèvre O., Guzzo L., Meneux B., Pollo A., Cappi A., Colombi S., Iovino A., Marinoni C., McCracken H. J., Scaramella R., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J. P., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Arnouts S., Bardelli S., Blaizot J., Bolzonella M., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Gavignaud I., Ilbert O., Marano B., Mathez G., Mazure A., Merighi R., Paltani S., Pellò R., Pozzetti L., Radovich M., Zamorani G., Zucca E., Bondi M., Bongiorno A., Busarello G., Lamareille F., Mellier Y., Merluzzi P., Ripepi V., and Rizzo D. ns Astronomy and Astrophysics Volume 439 Issue 3 September I 2005 pp.877-885

Subjects
GALAXIES: EVOLUTION, molecular data, Dark matter, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, infrared: ISM, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), COSMOLOGY:: LARGE SCALE STRUCTURE OF UNIVERSE, Astronomy and Astrophysics, Billion years, Galaxy, Redshift, ISM: molecules, Correlation function (statistical mechanics), Space and Planetary Science, ISM: individual objects: W49, Magnitude (astronomy), SURVEYS, ISM: individual objects: Sagittarius B2
Abstract

This paper presents the evolution of the clustering of the main population of galaxies from z=2.1 to z=0.2, from the first epoch VIMOS VLT Deep Survey (VVDS), a magnitude limited sample with 17.5, 11 pages, accepted 11-Apr-05 in A&A

Published
2005

10. The VIMOS-VLT deep survey. Evolution of the galaxy luminosity function up to z = 2 in first epoch data

Author

Ilbert O., Tresse L., Zucca E., Bardelli S., Arnouts S., Zamorani G., Pozzetti L., Bottini D., Garilli B., Le Brun V., Le Fèvre O., Maccagni D., Picat J. P., Scaramella R., Scodeggio M., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Bolzonella M., Cappi A., Charlot S., Contini T., Foucaud S., Franzetti P., Gavignaud I., Guzzo L., Iovino A., McCracken H. J., Marinoni C., Mathez G., Mazure A., Meneux B., Merighi R., Paltani S., Pello R., Pollo A., Radovich M., Bondi M., Busarello G., Ciliegi P., Lamareille F., Mellier Y., Merluzzi P., Ripepi V., Rizzo D. Astronomy, Astrophysics Volume 439 Issue 3 September I. 2005 p.p. 863 876, MARANO, BRUNO, BONGIORNO, ANGELA, Ilbert O., Tresse L., Zucca E., Bardelli S., Arnouts S., Zamorani G., Pozzetti L., Bottini D., Garilli B., Le Brun V., Le Fèvre O., Maccagni D., Picat J.-P., Scaramella R., Scodeggio M., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Bolzonella M., Cappi A., Charlot S., Contini T., Foucaud S., Franzetti P., Gavignaud I., Guzzo L., Iovino A., McCracken H. J., Marano B., Marinoni C., Mathez G., Mazure A., Meneux B., Merighi R., Paltani S., Pello R., Pollo A., Radovich M., Bondi M., Bongiorno A., Busarello G., Ciliegi P., Lamareille F., Mellier Y., Merluzzi P., Ripepi V., Rizzo D. Astronomy and Astrophysics Volume 439 Issue 3 September I 2005 pp.863-876, 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
GALAXIES: EVOLUTION, Epoch (astronomy), GALAXIES: STATISTICS, FOS: Physical sciences, Astrophysics, 01 natural sciences, Spectral line, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, GALAXIES:MASS FUNCTION, GALAXIES: LUMINOSITY FUNCTION, 010303 astronomy & astrophysics, Luminosity function (astronomy), Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Galaxy, Redshift, Wavelength, Space and Planetary Science, mass function, Magnitude (astronomy), SURVEYS
Abstract

We investigate the evolution of the galaxy luminosity function from the VIMOS-VLT Deep Survey (VVDS) from the present to z=2 in five (U, B, V, R and I) rest-frame band-passes. We use the first epoch VVDS deep sample of 11,034 spectra selected at 17.5, 17 pages, accepted for publication in Astronomy & Astrophysics

Published
2005

11. The Capodimonte Deep Field I - Presentation of the survey and first follow-up studies

Author

Alcalà, J. M., Pannella, M, Puddu, E, Radovich, M, Silvotti, R, Arnaboldi, M, Capaccioli, M, Covone, G, Dall'Ora, M, Grado, A, DE LUCIA, G, Longo, G, Mercurio, A, Musella, I, Napolitano, N, Pavlov, M, Rifatto, A, Ripepi, V, 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), Alcalá, J. M., Pannella, M., Puddu, E., Radovich, M., Silvotti, R., Arnaboldi, M., Capaccioli, M., Covone, Giovanni, Dall'Ora, M., De Lucia, G., Grado, A., Longo, Giuseppe, Mercurio, A., Musella, I., Napolitano, N., Pavlov, M., Rifatto, A., Ripepi, V., Scaramella, R., 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), Kapteyn Astronomical Institute, Beaussier, Catherine, ALCAL J., M, Pannella, M, Puddu, E, Radovich, M, Silvotti, R, Arnaboldi, A, Capaccioli, Massimo, Covone, G, Dall'Ora, M, Grado, A, DE LUCIA, G, Mercurio, A, Musella, I, Napolitano, N, Pavlov, M, Rifatto, A, and Ripepi, V

Subjects
QSOS, evoluzione delle galassie, Hubble Deep Field, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, STELLAR POPULATIONS, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], surveys, survey astronomiche, 0103 physical sciences, Galaxy formation and evolution, 010306 general physics, NUMBER COUNTS, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, FRANCE REDSHIFT SURVEY, HIERARCHICAL GALAXY FORMATION, Astrophysics (astro-ph), CLUSTER SURVEY, White dwarf, Astronomy and Astrophysics, AB magnitude, Galaxy, Redshift, OPTICAL-DATA, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, LUMINOSITY FUNCTION, IMAGING SURVEY, Halo, galaxies : clusters : general, PLANETARY-NEBULAE, SKY SURVEY, catalogs
Abstract

We present the Capodimonte Deep Field (OACDF), a deep field covering an area of 0.5 square degrees in the B, V, R optical bands plus six medium-band filters in the wavelength range 773--913 nm. The field reaches the following limiting AB magnitudes: B~25.3, V~24.8 and R~25.1 and contains about 50000 extended sources in the AB magnitude range 18 < R < 25 . Hence, it is intermediate between deep pencil beam surveys and very wide but shallow surveys. The main scientific goal of the OACDF is the identification and characterization of early-type field galaxies at different look-back times in order to study different scenarios of galaxy formation. Parallel goals include the search for groups and clusters of galaxies and the search for rare and peculiar objects (gravitational lenses, QSOs, halo White Dwarfs). In this paper we describe the OACDF data reduction, the methods adopted for the extraction of the photometric catalogs, the photometric calibration and the quality assessment of the catalogs by means of galaxy number counts, spectroscopic and photometric redshifts and star colors. We also present the first results of the search for galaxy overdensities. The depth of the OACDF and its relatively large spatial coverage with respect to pencil beam surveys make it a good tool for further studies of galaxy formation and evolution in the redshift range 0--1, as well as for stellar studies., 24 pages, accepted for pubblication on A&A

Published
2004

12. The Diffuse Light in Simulations of Galaxy Clusters

Author

Klaus Dolag, Magda Arnaboldi, Ortwin Gerhard, Giuseppe Murante, Giuseppe Tormen, Paolo Tozzi, Lauro Moscardini, Stefano Borgani, Luca Tornatore, Antonaldo Diaferio, L.-M. Cheng, MURANTE G., ARNABOLDI M., GERHARD O., BORGANI S., CHENG L.M., DIAFERIO A., DOLAG K., MOSCARDINI L., TORMEN G., TORNATORE L., TOZZI P., Murante, G, Arnaboldi, M, Gerhard, O, Borgani, Stefano, Chen, L. M, Diaferio, A, Dolag, K, Moscardini, L, Tormen, G, Tornatore, Luca, and Tozzi, P.

Subjects
Physics, Galaxy Cluster, Stellar population, Star formation, Galaxy Clusters, cD Galaxies, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Stars, Galaxy evolution, Space and Planetary Science, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, Surface brightness, Halo, Galaxy cluster, Astrophysics::Galaxy Astrophysics
Abstract

We study the properties of the diffuse light in galaxy clusters forming in a large hydrodynamical cosmological simulation of the Lambda-CDM cosmology. The simulation includes a model for radiative cooling, star formation in dense cold gas, and feedback by SN-II explosions. We select clusters having mass M>10^(14) h^(-1) Msun and study the spatial distribution of their star particles. While most stellar light is concentrated in gravitationally bound galaxies orbiting in the cluster potential, we find evidence for a substantial diffuse component, which may account for the extended halos of light observed around central cD galaxies. We find that more massive simulated clusters have a larger fraction of stars in the diffuse light than the less massive ones. The intracluster light is more centrally concentrated than the galaxy light, and the stars in the diffuse component are on average older than the stars in cluster galaxies, supporting the view that the diffuse light is not a random sampling of the stellar population in the cluster galaxies. We thus expect that at least ~10% of the stars in a cluster may be distributed as intracluster light, largely hidden thus far due to its very low surface brightness., 4 pages, 3 figures

Published
2004
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13. The first detection of ultra-diffuse galaxies in the Hydra I cluster from VEGAS survey

Author

Steffen Mieske, Marina Rejkuba, Laura Greggio, Chiara Spiniello, A. La Marca, Pietro Schipani, Duncan A. Forbes, Enrichetta Iodice, Marilena Spavone, Roberto Rampazzo, Massimo Capaccioli, Michele Cantiello, Giuseppe D'Ago, Magda Arnaboldi, Michael Hilker, Maurizio Paolillo, Iodice, E., Cantiello, M., Hilker, M., Rejkuba, M., Arnaboldi, M., Spavone, M., Greggio, L., Forbes, D. A., D'Ago, G., Mieske, S., Spiniello, C., La Marca, A., Rampazzo, R., Paolillo, M., Capaccioli, M., and Schipani, P.

Subjects
Stellar mass, Population, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: formation, Computer Science::Computational Geometry, 01 natural sciences, 0103 physical sciences, Cluster (physics), Galaxies: clusters: individual: Hydra I, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Galaxies: dwarf, Astronomy and Astrophysics, Galaxies: photometry, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Globular cluster, Astrophysics of Galaxies (astro-ph.GA), Lernaean Hydra, Halo
Abstract

In this paper we report on the discovery of 27 low-surface brightness galaxies, of which 12 are candidate ultra-diffuse galaxy (UDG) in the Hydra I cluster, based on deep observations taken as part of the VST Early-type Galaxy Survey (VEGAS). This first sample of UDG candidates in the Hydra I cluster represents an important step in our project that aims to enlarge the number of confirmed UDGs and, through study of statistically relevant samples, constrain the nature and formation of UDGs. This study presents the main properties of this class of galaxies in the Hydra I cluster. For all UDGs, we analyse the light and colour distribution, and provide a census of the globular cluster (GC) systems around them. Given the limitations of a reliable GC selection based on two relatively close optical bands only, we find that half of the UDG candidates have a total GC population consistent with zero. Of the other half, two galaxies have a total population larger than zero at 2$\sigma$ level. We estimate the stellar mass, the total number of GCs and the GC specific frequency ($S_N$). Most of the candidates span a range of stellar masses of $10^7-10^8$~M$_{\odot}$. Based on the GC population of these newly discovered UDGs, we conclude that most of these galaxies have a standard or low dark matter content, with a halo mass of $\leq 10^{10}$~M$_{\odot}$., Comment: Accepted for publication in A&A

Published
2020

14. The Fornax Cluster VLT Spectroscopic Survey II - Planetary Nebulae kinematics within 200 kpc of the cluster core

Author

E. Iodice, Chiara Spiniello, M. Capaccioli, Nicola R. Napolitano, Magda Arnaboldi, P. Schipani, M. Spavone, C. Tortora, Lodovico Coccato, Ortwin Gerhard, Maurizio Paolillo, Reynier Peletier, Michele Cantiello, Spiniello, C., Napolitano, N. R., Arnaboldi, M., Tortora, C., Coccato, L., Capaccioli, M., Gerhard, O., Iodice, E., Spavone, M., Cantiello, M., Peletier, R., Paolillo, M., Schipani, P., and Astronomy

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), COMA CLUSTER, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Catalogue, dark matter, VIRGO-CLUSTER, Astronomical data base, ELLIPTIC GALAXIES, GLOBULAR-CLUSTERS, 0103 physical sciences, LARGE-SCALE STRUCTURE, Coma Cluster, Astrophysics::Solar and Stellar Astrophysics, galaxies: formation, EARLY-TYPE GALAXIES, INTRACLUSTER LIGHT, Fornax Cluster, 10. No inequality, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, catalogues, galaxies: kinematics and dynamics, Physics, Very Large Telescope, 010308 nuclear & particles physics, Velocity dispersion, Astronomy and Astrophysics, DIFFUSE LIGHT, Astronomy and Astrophysic, Virgo Cluster, Planetary nebula, Astrophysics - Astrophysics of Galaxies, Galaxy, COLD DARK-MATTER, COSMOLOGICAL SIMULATIONS, Space and Planetary Science, Astronomical data bases, Globular cluster, Astrophysics of Galaxies (astro-ph.GA), Galaxies: Kinematics and dynamic, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the largest and most spatially extended planetary nebulae (PNe) catalog ever obtained for the Fornax cluster. We measured velocities of 1452 PNe out to 200 kpc in the cluster core using a counter-dispersed slitless spectroscopic technique with data from FORS2 on the VLT. With such extended spatial coverage, we can study separately the stellar halos of some of the cluster main galaxies and the intracluster light. In this second paper of the Fornax Cluster VLT Spectroscopic Survey (FVSS), we identify and classify the emission-line sources, describe the method to select PNe and calculate their coordinates and velocities from the dispersed slitless images. From the PN 2D velocity map we identify stellar streams that are possibly tracing the gravitational interaction of NGC1399 with NGC1404 and NGC1387. We also present the velocity dispersion profile out to $\sim 200$ kpc radii, which shows signatures of a superposition of the bright central galaxy and the cluster potential, with the latter clearly dominating the regions outside R $\sim 1000$" ($\sim 100$ kpc)., 13 pages, 8 figures, Accepted for publication in MNRAS, companion paper FVSS-I (Pota et al, 2018, submitted)

Published
2018

15. The Very Large Telescope Visible Multi‐Object Spectrograph Mask Preparation Software

Author

G. Mathez, G. Vettolani, Magda Arnaboldi, A. Pollo, C. Adami, Alain Mazure, S. Paltani, Roberto Scaramella, D. Maccagni, A. Cappi, B. Garilli, V. Le Brun, O. Ilbert, R. Merighi, T. Contini, E. Zucca, S. Bardelli, M. Bolzonella, Stephane Charlot, H. J. McCracken, A. Iovino, J. P. Picat, L. Tresse, D. Bottini, B. Meneux, Stephane Arnouts, Bruno Marano, Sylvie Foucaud, Lucia Pozzetti, Christian Marinoni, P. Franzetti, O. Le Fevre, Paolo Ciliegi, Mario Radovich, A. Zanichelli, Marco Scodeggio, Luigi Guzzo, G. Zamorani, 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 Astronomico di Capodimonte (OAC), Istituto Nazionale di Astrofisica (INAF), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), 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 Astrophysik (MPA), Max-Planck-Gesellschaft, Services communs OMP (UMS 831), 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), 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), Università di Bologna, Dipartimento di Astronomia, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), Bottini D., Garilli B., Maccagni D., Tresse L., Le Brun V., Le Fèvre O., Picat J. P., Scaramella R., Scodeggio M., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Arnouts S., Bardelli S., Bolzonella M., Cappi A., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Guzzo L., Ilbert O., Iovino A., McCracken H. J., Marano B., Marinoni C., Mathez G., Mazure A., Meneux B., Merighi R., Paltani S., Pollo A., Pozzetti L., Radovich M., Zamorani G., and Zucca E.

Subjects
Physics, Very Large Telescope, Single exposure, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, business.industry, Software tool, Instrumentation: Spectrographs, Techniques: Spectroscopic, Astronomy and Astrophysics, Object (computer science), 01 natural sciences, Multiplexing, Software, Optics, Space and Planetary Science, Observatory, Methods: Numerical, 0103 physical sciences, business, 010303 astronomy & astrophysics, Spectrograph, Remote sensing
Abstract

VIMOS (Visible Multi-Object Spectrograph) is a multiobject imaging spectrograph installed at the VLT (Very large Telescope) at the ESO (European Southern Observatory) Paranal Observatory that is especially suited for survey work. VIMOS is characterized by its very high multiplexing factor: it is possible to take up to 800 spectra with 10" long slits in a single exposure. To fully exploit its multiplexing potential, we designed and implemented a dedicated software tool: the VIMOS Mask Preparation Software (VMMPS), which allows the astronomer to select the objects to be spectroscopically observed, and provides for automatic slit positioning and slit number maximization within the instrumental constraints. The output of VMMPS is used to manufacture the slit masks to be mounted in the instrument for spectroscopic observations.

Published
2005

16. Narrow band survey for intragroup light in the Leo HI cloud

Author

N. Castro-Rodriguez, Nicola R. Napolitano, J. Alfonso L. Aguerri, Massimo Capaccioli, Magda Arnaboldi, Ortwin Gerhard, Kenneth C. Freeman, Kapteyn Astronomical Institute, Astronomy, Castrorodriguez, N., Aguerri, J. A. L., Arnaboldi, M., Gerhard, O., Freeman, K. C., Napolitano, N. R., and Capaccioli, Massimo

Subjects
Stellar population, DEEP FIELD, FOS: Physical sciences, Astrophysics, LY-ALPHA EMITTERS, CANDLES, planetary nebulae : general, SOUTHERN SPECTROPHOTOMETRIC STANDARDS, Surface brightness, O-III, Luminosity function (astronomy), Physics, Astrophysics (astro-ph), galaxies : intergalactic medium, M96 GROUP, Astronomy and Astrophysics, VIRGO CLUSTER, Planetary nebula, Virgo Cluster, galaxies : clusters : individual : M 96, FE-II, Galaxy, Redshift, EVOLUTION, Space and Planetary Science, Elliptical galaxy, STARS, galaxies : ISM
Abstract

We have observed emission line objects located in a 0.26 deg^2 field in the M96 (Leo) group, coincident with the intergalactic HI cloud. The emission line objects were selected using the same procedure as used for the search for intracluster planetary nebulae in the Virgo cluster, and their m_5007 luminosity function has a bright cut-off ~1.2 magnitude fainter than for the PNLF associated with the elliptical galaxies in the M96 group.Therefore the vast majority of these emission line objects are compatible with not being intragroup planetary nebulae at the Leo group distance of 10 Mpc. Spectroscopic follow-up of two emission line objects in this Leo field showed that indeed these do not have the [OIII] doublet expected for a real PN. The brighter source is identified as a starburst object at redshift z = 3.128, because of a second emission in the near infrared, identified as FeII (\lambda 2220 AA). From these data we derive three main results: (i) from the absence of PN we can determine a more stringent upper limit to the surface brightness in any old stellar population associated with the Leo HI cloud. (ii) This translates to an upper limit of 1.6% for the fraction of luminosity in a diffuse intragroup component in the densest 3 x 2 deg area of the Leo group,relative to the light in galaxies. (iii) Using this Leo field as a blank field, we derive an average fraction of 13.6% background emission line objects that enter in surveys of Virgo intracluster PN. The small fraction confirms the validity of the selection criteria for intracluster PN candidates in Virgo., Comment: 11 pages, in press on Astronomy & Astrophysics

Published
2003

17. Intracluster Planetary Nebulae in Virgo: Photometric Selection, Spectroscopic Validation, and Cluster Depth

Author

Kenneth C. Freeman, Roberto H. Méndez, Nicola R. Napolitano, J. A. L. Aguerri, Magda Arnaboldi, R. P. Kudritzki, Massimo Capaccioli, John J. Feldmeier, Ortwin Gerhard, Arnaboldi, M, Aguerri, J. A. L., Napolitano, N. R., Gerhard, O, Freeman, K. C., Feldmeier, J, Capaccioli, Massimo, Kudritzki, R. P., and Mndez, R. H.

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Virgo Cluster, Planetary nebula, Planetary nebula luminosity function, Galaxy, Luminosity, Distance modulus, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Surface brightness, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy)
Abstract

We have imaged an empty area of 34'x34' one and a half degree north of the Virgo cluster core to survey for intracluster planetary nebula candidates. We have implemented and tested a fully automatic procedure for the selection of emission line objects in wide-field images, based on the on-off technique from Ciardullo and Jacoby. Freeman et al. have spectroscopically confirmed a sample of intracluster planetary nebulae in one Virgo field. We use the photometric and morphological properties of this sample to test our selection procedure. In our newly surveyed Virgo field, 75 objects were identified as best candidates for intracluster PNe. The luminosity function of the spectroscopically confirmed PNe shows a brighter cut-off than the planetary nebula luminosity function for the inner regions of M87. Such a brighter cut-off is also observed in the newly surveyed field and indicates a smaller distance modulus, implying that the front end of the Virgo cluster is closer to us by a significant amount: 14% closer (2.1 Mpc) than M87 for the spectroscopic field, using the PN luminosity function distance of 14.9 Mpc to M87, and 19% closer (2.8 Mpc) than M87 for the newly surveyed field. Independent distance indicators (Tully-Fisher relation for Virgo spirals and surface brightness fluctuations for Virgo ellipticals) agree with these findings. From these two Virgo cluster fields there is no evidence that the surface luminosity density for the diffuse stellar component in the cluster decreases with radius. The luminosity surface density of the diffuse stellar population is comparable to that of the galaxies., 30 pages, 8 figures, accepted for pubblication in AJ

Published
2002

18. Kinematic properties of early type galaxy halos using planetary nebulae

Author

Massimo Capaccioli, E. Noordermeer, Lodovico Coccato, Michael R. Merrifield, Ortwin Gerhard, Magda Arnaboldi, Konrad Kuijken, F. De Lorenzi, Nicola R. Napolitano, Nigel G. Douglas, Aaron J. Romanowsky, Payel Das, Arianna Cortesi, Coccato, L., Gerhard, O., Arnaboldi, M., Das, P., Douglas, N. G., Kuijken, K., Merrifield, M. R., Napolitano, N. R., Noordermeer, E., Romanowsky, A. J., Capaccioli, Massimo, Cortesi, A., Lorenzi, F. De, and Astronomy

Subjects
Physics, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Kinematics, Planetary nebula, Galaxy, Early type, Computer Science::Robotics, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Halo, Astrophysics::Galaxy Astrophysics
Abstract

We studied the kinematics of the halo of a sample of 16 early type galaxies out to 5-10 effective radii using Planetary Nebulae (PNe) as kinematic tracers (Coccato et al. 2009).

Published
2010

19. The Planetary Nebula Spectrograph elliptical galaxy survey: the dark matter in NGC 4494

Author

Aaron J. Romanowsky, Ortwin Gerhard, Ewan O'Sullivan, M. Capaccioli, Nigel G. Douglas, Arianna Cortesi, Michael R. Merrifield, Lodovico Coccato, Nicola R. Napolitano, Payel Das, Konrad Kuijken, E. Noordermeer, Kenneth C. Freeman, M. Arnaboldi, F. De Lorenzi, Napolitano, N. R., Romanowsky, A. J., Coccato, L., Capaccioli, Massimo, Douglas, N. G., Noordermeer, E., Gerhard, O., Arnaboldi, M., de Lorenzi, F., Kuijken, K., Merrifield, M. R., O. Sullivan, E., Cortesi, A., Das, P., and Freeman, K. C.

Subjects
ABSORPTION-LINE SPECTRA, Stellar kinematics, galaxies: individual: NGC 4494, Dark matter, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, dark matter, cD, Galactic halo, SURFACE BRIGHTNESS GALAXIES, 0103 physical sciences, Galaxy formation and evolution, TO-LIGHT RATIO, Astrophysics::Solar and Stellar Astrophysics, planetary nebulae: general, galaxies: elliptical and lenticular, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, galaxies: kinematics and dynamics, Physics, 010308 nuclear & particles physics, EXTENDED ROTATION CURVES, Velocity dispersion, Astronomy and Astrophysics, HUBBLE-SPACE-TELESCOPE, Planetary nebula, Galaxy, KINEMATICALLY DISTINCT CORES, MODIFIED NEWTONIAN DYNAMICS, Space and Planetary Science, SPHERICAL STELLAR-SYSTEMS, GLOBULAR-CLUSTER SYSTEMS, Elliptical galaxy, galaxies: structure, Astrophysics::Earth and Planetary Astrophysics, SIGHT VELOCITY DISTRIBUTIONS
Abstract

We present new Planetary Nebula Spectrograph observations of the ordinary elliptical galaxy NGC 4494, resulting in positions and velocities of 255 PNe out to 7 effective radii (25 kpc). We also present new wide-field surface photometry from MMT/Megacam, and long-slit stellar kinematics from VLT/FORS2. The spatial and kinematical distributions of the PNe agree with the field stars in the region of overlap. The mean rotation is relatively low, with a possible kinematic axis twist outside 1 Re. The velocity dispersion profile declines with radius, though not very steeply, down to ~70 km/s at the last data point. We have constructed spherical dynamical models of the system, including Jeans analyses with multi-component LCDM-motivated galaxies as well as logarithmic potentials. These models include special attention to orbital anisotropy, which we constrain using fourth-order velocity moments. Given several different sets of modelling methods and assumptions, we find consistent results for the mass profile within the radial range constrained by the data. Some dark matter (DM) is required by the data; our best-fit solution has a radially anisotropic stellar halo, a plausible stellar mass-to-light ratio, and a DM halo with an unexpectedly low central density. We find that this result does not substantially change with a flattened axisymmetric model. Taken together with other results for galaxy halo masses, we find suggestions for a puzzling pattern wherein most intermediate-luminosity galaxies have very low concentration halos, while some high-mass ellipticals have very high concentrations. We discuss some possible implications of these results for DM and galaxy formation.

Published
2009

20. Kinematic properties of early-type galaxy haloes using planetary nebulae

Author

Aaron J. Romanowsky, Nicola R. Napolitano, Michael R. Merrifield, Magda Arnaboldi, Konrad Kuijken, Kenneth C. Freeman, Payel Das, Arianna Cortesi, Nigel G. Douglas, Lodovico Coccato, F. De Lorenzi, Massimo Capaccioli, E. Noordermeer, Ortwin Gerhard, Coccato, L., Gerhard, O., Arnaboldi, M., Das, P., Douglas, N. G., Kuijken, K., Merrifield, M. R., Napolitano, N. R., Noordermeer, E., Romanowsky, A. J., Capaccioli, Massimo, Cortesi, A., de Lorenzi, F., and Freeman, K. C.

Subjects
Stellar kinematics, Stellar mass, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, cD, STELLAR POPULATIONS, ELLIPTIC GALAXIES, MERGER REMNANTS, 0103 physical sciences, TO-LIGHT RATIO, DARK-MATTER, Astrophysics::Solar and Stellar Astrophysics, Surface brightness, galaxies: elliptical and lenticular, 010303 astronomy & astrophysics, galaxies: kinematics and dynamics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, CCD SURFACE PHOTOMETRY, Astrophysics (astro-ph), Velocity dispersion, Astronomy and Astrophysics, HUBBLE-SPACE-TELESCOPE, GALACTIC NUCLEUS FEEDBACK, Planetary nebula, galaxies: general, SAURON PROJECT, Galaxy, Radial velocity, galaxies: haloes, Space and Planetary Science, Halo, Astrophysics::Earth and Planetary Astrophysics, SIGHT VELOCITY DISTRIBUTIONS
Abstract

We present new planetary nebulae (PNe) positions, radial velocities, and magnitudes for 6 early-type galaxies obtained with the Planetary Nebulae Spectrograph, their two-dimensional velocity and velocity dispersion fields. We extend this study to include an additional 10 early-type galaxies with PNe radial velocity measurements available from the literature, to obtain a broader description of the outer-halo kinematics in early-type galaxies. These data extend the information derived from stellar kinematics to typically up to ~8 Re. The combination of photometry, stellar and PNe kinematics shows: i) good agreement between the PNe number density and the stellar surface brightness in the region where the two data sets overlap; ii) good agreement between PNe and stellar kinematics; iii) that the mean rms velocity profiles fall into two groups: with of the galaxies characterized by slowly decreasing profiles and the remainder having steeply falling profiles; iv) a larger variety of velocity dispersion profiles; v) that twists and misalignments in the velocity fields are more frequent at large radii, including some fast rotators; vi) that outer haloes are characterised by more complex radial profiles of the specific angular momentum-related lambda_R parameter than observed within 1Re; vii) that many objects are more rotationally dominated at large radii than in their central parts; and viii) that the halo kinematics are correlated with other galaxy properties, such as total luminosity, isophotal shape, total stellar mass, V/sigma, and alpha parameter, with a clear separation between fast and slow rotators., Comment: 36 pages, 21 figures, revised version for MNRAS

Published
2009

21. Eddington ratios of faint AGN at intermediate redshift: evidence for a population of half-starved black holes

Author

Roberto Scaramella, A. Mazure, Christian Marinoni, Vincenzo Ripepi, R. Merighi, Yannick Mellier, M. Radovich, Stéphane Arnouts, Laurence Tresse, G. Zamorani, B. Husemann, Angela Bongiorno, V. Le Brun, Paolo Ciliegi, P. Franzetti, E. Zucca, D. Rizzo, Thierry Contini, Paola Merluzzi, A. Cappi, A. Zanichelli, Daniela Vergani, B. Meneux, Sylvie Foucaud, I. Gavignaud, Lucia Pozzetti, Bruno Marano, M. Scodeggio, Lutz Wisotzki, Magda Arnaboldi, Giampaolo Vettolani, Luigi Guzzo, Bianca Garilli, A. Pollo, Palle Møller, M. Bolzonella, R. Pello, M. Bondi, M. Schramm, Stephane Charlot, D. Bottini, F. Lamareille, A. Iovino, S. Bardelli, O. Cucciati, O. Ilbert, G. Busarello, S. de la Torre, D. Maccagni, Stéphane Paltani, O. Le Fevre, H. J. McCracken, L. Gregorini, C. Adami, European Southern Observatory (ESO), 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), Laboratoire Astrophysique de Toulouse-Tarbes (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), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, 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), 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), INAF- Milano, Istituto Nazionale di Astrofisica (INAF), 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 Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-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), Gavignaud I., Wisotzki L., Bongiorno A., Paltani S., Zamorani G., Møller P., Le Brun V., Husemann B., Lamareille F., Schramm M., Le Fèvre O., Bottini D., Garilli B., Maccagni D., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Arnouts S., Bardelli S., Bolzonella M., Cappi A., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Guzzo L., Ilbert O., Iovino A., McCracken H. J., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Pellò R., Pollo A., Pozzetti L., Radovich M., Zucca E., Bondi M., Busarello G., Cucciati O., de La Torre S., Gregorini L., Mellier Y., Merluzzi P., Ripepi V., Rizzo D., and Vergani D.

Subjects
ACTIVE GALACTIC NUCLEI, Active galactic nucleus, Astrophysique (Planète et Univers), Astrophysics::High Energy Astrophysical Phenomena, Population, galaxies: active, enquête, EXTRAGALACTIC SURVEYS, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Virial theorem, symbols.namesake, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, BLACK HOLES, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation), Physics, Electronic appendix, education.field_of_study, 010308 nuclear & particles physics, galaxie, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Redshift, galaxies: Seyfert, Space and Planetary Science, COSMOLOGY, Eddington luminosity, symbols, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], catalogue, galaxies: nuclei, VIMOS-VLT Deep Survey, catalogs, surveys, quasars:general
Abstract

We use one of the deepest spectroscopic samples of broad line active galactic nuclei (AGN) currently available, extracted from the VIMOS VLT Deep Survey (VVDS), to compute MgII and CIV virial masses estimate of 120 super-massive black holes in the redshift range 1.0, Comment: accepted for publication in Astronomy & Astrophysics

Published
2008

22. Dearth of dark matter or massive dark halo? Mass-shape-anisotropy degeneracies revealed by NMAGIC dynamical models of the elliptical galaxy NGC 3379

Author

Aaron J. Romanowsky, Nicola R. Napolitano, Nigel G. Douglas, Massimo Capaccioli, E. Noordermeer, F. De Lorenzi, Michael R. Merrifield, Lodovico Coccato, Ortwin Gerhard, Magda Arnaboldi, Konrad Kuijken, Victor P. Debattista, Kenneth C. Freeman, de Lorenzi, F., Gerhard, O., Coccato, L., Arnaboldi, M., Capaccioli, Massimo, Douglas, N. G., Freeman, K. C., Kuijken, K., Merrifield, M. R., Napolitano, N. R., Noordermeer, E., Romanowsky, A. J., Debattista, V. P., and Kapteyn Astronomical Institute

Subjects
NGC-3379, 010504 meteorology & atmospheric sciences, Stellar mass, VELOCITY PROFILES, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, methods: numerical, SPHERICAL GALAXIES, 0103 physical sciences, TO-LIGHT RATIO, Astrophysics::Solar and Stellar Astrophysics, 3-INTEGRAL MODELS, KINEMATICS, galaxies: elliptical and lenticular, 010303 astronomy & astrophysics, galaxies: kinematics and dynamics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Astrophysics (astro-ph), LENS ACS SURVEY, Velocity dispersion, Astronomy and Astrophysics, EVOLUTION, Galaxy, Dark matter halo, STELLAR-SYSTEMS, galaxies: individual: NGC 3379, Space and Planetary Science, BLACK-HOLE, Elliptical galaxy, Halo, Astrophysics::Earth and Planetary Astrophysics
Abstract

Recent results from the Planetary Nebula Spectrograph (PN.S) survey have revealed a rapidly falling velocity dispersion profile in the nearby elliptical galaxy NGC 3379, casting doubts on whether this intermediate-luminosity galaxy has the kind of dark matter halo expected in LambdaCDM cosmology. We present a detailed dynamical study of this galaxy, combining long-slit spectroscopy, SAURON integral-field data, and PN.S velocities, reaching to more than seven effective radii (R_e). We construct spherical and axisymmetric dynamical models for these data with the flexible made-to-measure NMAGIC code, in a sequence of gravitational potentials with varying dark halo mass. We find that the data are consistent both with near-isotropic spherical systems dominated by the stellar mass, and with models in massive halos with strongly radially anisotropic outer parts (beta >~ 0.8 at 7R_e). Formal likelihood limits would exclude (at 1 sigma) the model with stars only, as well as halo models with v_circ(7R_e) >~ 250 km/s. A sequence of more realistic axisymmetric models of different inclinations and a small number of triaxial tests confirm the spherical results. All valid models fitting all the data are dynamically stable over Gyrs, including the most anisotropic ones. NGC 3379 may well have a dark matter halo as predicted by recent merger models within LambdaCDM cosmology, provided its outer envelope is strongly radially anisotropic. (abridged), 22 pages, 25 figures, revised version for MNRAS

Published
2008

23. The PN.S Elliptical Galaxy Survey: Data Reduction, Planetary Nebula Catalog, and Basic Dynamics for NGC 3379

Author

Massimo Capaccioli, H. R. Merrett, Aaron J. Romanowsky, Magda Arnaboldi, Michael R. Merrifield, L. Coccato, Konrad Kuijken, Nigel G. Douglas, Ortwin Gerhard, Kenneth C. Freeman, Nicola R. Napolitano, E. Noordermeer, Douglas, N. G., Napolitano, N. R., Romanowsky, A. J., Coccato, L, Kuijken, K, Merrifield, M. R., Arnaboldi, M, Gerhard, O, Freeman, K. C., Merrett, H. R., Noordermeer, E, Capaccioli, Massimo, and Kapteyn Astronomical Institute

Subjects
STANDARD CANDLES, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Kinematics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, cD, STELLAR POPULATIONS, SPHERICAL GALAXIES, planetary nebulae : general, 0103 physical sciences, galaxies : elliptical and lenticular, TO-LIGHT RATIO, DARK-MATTER, Astrophysics::Solar and Stellar Astrophysics, galaxies : structure, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, RADIAL-VELOCITIES, LEO-I GROUP, 010308 nuclear & particles physics, CCD SURFACE PHOTOMETRY, Astrophysics (astro-ph), Astronomy and Astrophysics, Radius, Planetary nebula, Galaxy, galaxies : individual (NGC 3379) galaxies : kinematics and dynamics, Dark matter halo, Space and Planetary Science, FUNDAMENTAL PLANE, Elliptical galaxy, MASSIVE BLACK-HOLE, Astrophysics::Earth and Planetary Astrophysics, Data reduction
Abstract

We present results from Planetary Nebula Spectrograph (PN.S) observations of the elliptical galaxy NGC 3379 and a description of the data reduction pipeline. We detected 214 planetary nebulae of which 191 are ascribed to NGC 3379, and 23 to the companion galaxy NGC 3384. Comparison with data from the literature show that the PN.S velocities have an internal error of, 21 pages, 15 figures, using emulateapj.cls. Accepted for publication in the Astrophysical Journal

Published
2007

24. The VIMOS-VLT Deep Survey. Galaxy luminosity function per morphological type up to z = 1.2

Author

Paolo Ciliegi, Angela Bongiorno, Paola Merluzzi, C. Adami, Marco Scodeggio, G. Mathez, Denis Burgarella, G. Busarello, Luigi Guzzo, Stéphane Charlot, D. Rizzo, S. Paltani, Roberto Scaramella, A. Zanichelli, H. J. McCracken, D. Maccagni, Lucia Pozzetti, M. Bolzonella, R. Merighi, O. Le Fevre, V. Le Brun, O. Ilbert, T. Contini, M. Bondi, D. Bottini, A. Cappi, Christian Marinoni, E. Zucca, S. Lauger, S. Arnout, R. Pello, G. Zamorani, L. Tresse, J. P. Picat, A. Pollo, Bruno Marano, P. Franzetti, I. Gavignaud, Mario Radovich, Sylvie Foucaud, A. Iovino, V. Ripepi, S. Bardelli, Yannick Mellier, G. Vettolani, V. Buat, B. Garilli, B. Meneux, M. Arnaboldi, Alain Mazure, 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), Laboratoire Astrophysique de Toulouse-Tarbes (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), 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), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, 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), 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 Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-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), Ilbert O., Lauger S., Tresse L., Buat V., Arnouts S., Le Fèvre O., Burgarella D., Zucca E., Bardelli S., Zamorani G., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J.-P., Scaramella R., Scodeggio M., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Bolzonella M., Cappi A., Charlot S., Contini T., Foucaud S., Franzetti P., Gavignaud I., Guzzo L., Iovino A., McCracken H. J., Marano B., Marinoni C., Mathez G., Mazure A., Meneux B., Merighi R., Paltani S., Pello R., Pollo A., Pozzetti L., Radovich M., Bondi M., Bongiorno A., Busarello G., Ciliegi P., Mellier Y., Merluzzi P., Ripepi V., and Rizzo D.

Subjects
GALAXIES: MASS FUNCTION, Population, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], surveys, Bulge, 0103 physical sciences, GALAXIES: EVOLUTION PARAMETERS, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), Physics, Galaxy: evolution, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Morphological type, Astronomy and Astrophysics, galaxies: fundamental parameters, Galaxy, Redshift, galaxies: luminosity function, Space and Planetary Science, mass function, Magnitude (astronomy), Elliptical galaxy
Abstract

Aims.We have computed the evolution of the rest-frame B-band luminosity function (LF) for bulge and disk-dominated galaxies since z=1.2. Methods: .We use a sample of 605 spectroscopic redshifts with IAB&leq; 24 in the Chandra Deep Field South from the VIMOS-VLT Deep Survey, 3555 galaxies with photometric redshifts from the COMBO-17 multi-color data, coupled with multi-color HST/ACS images from the Great Observatories Origin Deep Survey. We split the sample in bulge- and disk-dominated populations on the basis of asymmetry and concentration parameters measured in the rest-frame B-band. Results: .We find that at z=0.4-0.8, the LF slope is significantly steeper for the disk-dominated population (α=-1.19 ± 0.07) compared to the bulge-dominated population (α=-0.53 ± 0.13). The LF of the bulge-dominated population is composed of two distinct populations separated in rest-frame color: 68% of red (B-I)AB>0.9 and bright galaxies showing a strongly decreasing LF slope α=+0.55 ± 0.21, and 32% of blue (B-I)AB

Published
2006

25. Stellar kinematics for the central spheroid in the Polar Disk Galaxy NGC4650A

Author

J. S. Gallagher, Roberto P. Saglia, Francoise Combes, M. Capaccioli, Kenneth C. Freeman, M. Arnaboldi, Ortwin Gerhard, F. Bournaud, Enrica Iodice, Linda S. Sparke, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), INAF-Osservatorio Astrofisico di Torino (INAF-OATo), Max-Planck-Institut für Extraterrestriche Physik (MPE), University of Wisconsin-Madison, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Galaxies et cosmologie, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), University of Naples Federico II = Università degli studi di Napoli Federico II, Mount Stromlo Observatory, Australian National University, Henry, Florence, Iodice, E, Arnaboldi, M, Saglia, R. P., Sparke, L. S., Gerhard, O, Gallagher, J. S., Combes, F, Bournaud, F, Capaccioli, Massimo, and Freeman, K. C.

Subjects
Physics, Stellar kinematics, Astrophysics (astro-ph), Spheroid, Velocity dispersion, FOS: Physical sciences, Astronomy and Astrophysics, Kinematics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Spectral line, Galaxy, Accretion (astrophysics), Space and Planetary Science, Polar, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract

We have obtained high angular resolution, high signal-to-noise spectra of the Calcium triplet absorption lines on the photometric axes of the stellar spheroid in the polar disk galaxy NGC4650A. Along the major axis, the observed rotation and velocity dispersion measurements show the presence of a kinematically decoupled nucleus, and a flat velocity dispersion profile. The minor axis kinematics is determined for the first time: along this direction some rotation is measured, and the velocity dispersion is nearly constant and slightly increases at larger distances from the center. The new high resolution kinematic data suggest that the stellar component in NGC4650A resembles a nearly-exponential oblate spheroid supported by rotation. The main implications of these results on the previous mass models for NGC4650A are discussed. Moreover, the new kinematic data set constraints on current models for the formation scenarios of Polar Ring Galaxies (PRGs), supporting a slow accretion rather then a secondary strong dissipative event., Comment: 25 pages, 8 figures, accepted for publication in the Astrophysical Journal

Published
2006
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26. The VIMOS-VLT Deep Survey. The evolution of galaxy clustering per spectral type to z ~= 1.5

Author

Christian Marinoni, T. Contini, Luigi Guzzo, Paolo Ciliegi, G. Zamorani, A. Cappi, O. Cucciati, Angela Bongiorno, L. Tresse, Stephane Arnouts, Lucia Pozzetti, Yannick Mellier, V. Ripepi, E. Zucca, D. Rizzo, V. LeBrun, S. Paltani, Roberto Scaramella, Stéphane Charlot, G. Mathez, O. LeFevre, R. Merighi, I. Gavignaud, A. Zanichelli, M. Bondi, B. Meneux, D. Bottini, Alain Mazure, G. Vettolani, J. P. Picat, M. Bolzonella, A. Iovino, R. Pello, M. Arnaboldi, G. Busarello, B. Garilli, Marco Scodeggio, C. Adami, L. Gregorini, Mario Radovich, F. Lamareille, P. Franzetti, Paola Merluzzi, O. Ilbert, Bruno Marano, D. Maccagni, H. J. McCracken, Sylvie Foucaud, A. Pollo, S. Bardelli, 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 Astronomico di Brera (INAF-OAB), INAF-Osservatorio Astronomico di Bologna (OABO), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), INAF-Osservatorio Astronomico di Brera, 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), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), 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-Osservatorio Astronomico di Roma (INAF-OAR), IRA-INAF, Bologna, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Max-Planck-Institut für Astrophysik (MPA), School of Physics and Astronomy, University of Nottingham, European Southern Observatory (ESO), INTEGRAL Science Data Centre, 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), Meneux B., Le Fèvre O., Guzzo L., Pollo A., Cappi A., Ilbert O., Iovino A., Marinoni C., McCracken H. J., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J.P., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnouts S., Arnaboldi M., Bardelli S., Bolzonella M., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Gavignaud I., Marano B., Mazure A., Merighi R., Paltani S., Pello' R., Pozzetti L., Radovich M., Zamorani G., Zucca E., Bondi M., Bongiorno A., Busarello G., Cucciati O., Gregorini L., Lamareille F., Mathez G., Mellier Y., Merluzzi P., Ripepi V., and Rizzo D.

Subjects
Population, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Type (model theory), Stellar classification, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, 10. No inequality, education, Cluster analysis, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Star formation, Astrophysics (astro-ph), Astronomy and Astrophysics, Galaxy, Space and Planetary Science, Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We measure the evolution of clustering for galaxies with different spectral types from 6495 galaxies with 17.51.2, due to the growth in clustering of the star-forming population. We find similar results when splitting the sample into `red' and `blue' galaxies using the observed color bi-modality. When compared to the expected linear growth of mass fluctuations, a natural interpretation of these observations is that: (a) the assembly of massive early type galaxies is already mostly complete in the densest dark matter halos at z~=1; (b) luminous late-type galaxies are located in higher-density, more clustered regions of the Universe at z~=1.5 than at present, indicating that star formation activity is progressively increasing, going back in time, in the higher-density peaks that today are mostly dominated by old galaxies., 12 pages, Accepted on 11-Feb-06 for publication in Astronomy and Astrophysics

Published
2006

27. The VIMOS VLT Deep Survey - Evolution of the luminosity functions by galaxy type up to z=1.5 from first epoch data

Author

G. Zamorani, Stéphane Charlot, J. P. Picat, O. Le Fevre, A. Cappi, S. Paltani, E. Zucca, D. Rizzo, O. Cucciati, D. Bottini, A. Pollo, Roberto Scaramella, R. Merighi, Stephane Arnouts, G. Busarello, Yannick Mellier, L. Gregorini, Lucia Pozzetti, Sylvie Foucaud, D. Maccagni, Paolo Ciliegi, M. Bolzonella, S. Bardelli, B. Garilli, V. Ripepi, Bruno Marano, M. Bondi, G. Vettolani, C. Adami, Magda Arnaboldi, T. Contini, H. J. McCracken, B. Meneux, F. Lamareille, R. Pello, Paola Merluzzi, Christian Marinoni, Mario Radovich, A. Iovino, G. Mathez, I. Gavignaud, Angela Bongiorno, Marco Scodeggio, P. Franzetti, L. Tresse, A. Zanichelli, Alain Mazure, V. Le Brun, O. Ilbert, Luigi Guzzo, 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 Astronomico di Bologna (OABO), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), 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), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), 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), Istituto di Radioastronomia, Bologna, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Max-Planck-Institut für Astrophysik (MPA), European Southern Observatory (ESO), INAF-Osservatorio Astronomico di Brera, 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), Zucca E., Ilbert O., Bardelli S., Tresse L., Zamorani G., Arnouts S., Pozzetti L., Bolzonella M., McCracken H. J., Bottini D., Garilli B., Le Brun V., Le Fevre O., Maccagni D., Picat J.P., Scaramella R., Scodeggio M., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Cappi A., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Gavignaud I., Guzzo L., Iovino A., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Paltani S., Pello' R., Pollo A., Radovich M., Bondi M., Bongiorno A., Busarello G., Cucciati O., Gregorini L., Lamareille F., Mathez G., Mellier Y., Merluzzi P., Ripepi V., and Rizzo D.

Subjects
Physics, 010308 nuclear & particles physics, Epoch (astronomy), Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Rest frame, Stellar classification, 01 natural sciences, Redshift, Galaxy, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Magnitude (astronomy), 10. No inequality, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy)
Abstract

From the first epoch observations of the VVDS up to z=1.5 we have derived luminosity functions (LF) of different spectral type galaxies. The VVDS data, covering ~70% of the life of the Universe, allow for the first time to study from the same sample and with good statistical accuracy the evolution of the LFs by galaxy type in several rest frame bands from a purely magnitude selected sample. The magnitude limit of the VVDS allows the determination of the faint end slope of the LF with unprecedented accuracy. Galaxies have been classified in four spectral classes, using their colours and redshift, and LFs have been derived in the U, B, V, R and I rest frame bands from z=0.05 to z=1.5. We find a significant steepening of the LF going from early to late types. The M* parameter is significantly fainter for late type galaxies and this difference increases in the redder bands. Within each of the galaxy spectral types we find a brightening of M* with increasing redshift, ranging from =< 0.5 mag for early type galaxies to ~1 mag for the latest type galaxies, while the slope of the LF of each spectral type is consistent with being constant with redshift. The LF of early type galaxies is consistent with passive evolution up to z~1.1, while the number of bright early type galaxies has decreased by ~40% from z~0.3 to z~1.1. We also find a strong evolution in the normalization of the LF of latest type galaxies, with an increase of more than a factor 2 from z~0.3 to z~1.3: the density of bright late type galaxies in the same redshift range increases of a factor ~6.6. These results indicate a strong type-dependent evolution and identifies the latest spectral types as responsible for most of the evolution of the UV-optical luminosity function out to z=1.5., 18 pages with encapsulated figures, revised version after referee's comments, accepted for publication in A&A

Published
2006

28. The VIMOS Integral Field Unit: data reduction methods and quality assessment

Author

E. Zucca, D. Rizzo, V. Le Brun, Magda Arnaboldi, Laurence Tresse, Olivier Ilbert, R. Pello, Paolo Ciliegi, Stéphane Arnouts, A. Iovino, B. Meneux, D. Maccagni, Christian Marinoni, D. Bottini, C. Adami, P. Franzetti, Bianca Garilli, J. P. Picat, Stéphane Paltani, O. Le Fevre, A. Zanichelli, Bruno Marano, G. Mathez, M. Radovich, Roberto Scaramella, A. Mazure, Agnieszka Pollo, S. Bardelli, Giampaolo Vettolani, H. J. McCracken, Luigi Guzzo, R. Merighi, Sylvie Foucaud, Stephane Charlot, M. Scodeggio, Thierry Contini, I. Gavignaud, G. Zamorani, A. Cappi, Lucia Pozzetti, M. Bolzonella, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Services communs OMP (UMS 831), 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), 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), Università di Bologna, Dipartimento di Astronomia, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), 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), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, European Southern Observatory (ESO), IRA-INAF, Bologna, Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), 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-Osservatorio Astronomico di Bologna (OABO), 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 Astronomico di Capodimonte (INAF-OAC), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), INAF-Osservatorio Astronomico di Brera, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Zanichelli A., Garilli B., Scodeggio M., Franzetti P., Rizzo D., Maccagni D., Merighi R., Picat J. P., Le Fèvre O., Foucaud S., Bottini D., Le Brun V., Scaramella R., Tresse L., Vettolani G., Adami, C., Arnaboldi M., Arnouts S., Bardelli S., Bolzonella M., Cappi A., Charlot S., Ciliegi P., Contini T., Gavignaud I., Guzzo L., Ilbert O., Iovino A., McCracken H. J., Marano B., Marinoni C., Mathez G., Mazure A., Meneux B., Paltani S., Pellò R., Pollo A., Pozzetti L., Radovich M., Zamorani G., and Zucca E.

Subjects
Physics, TECHNIQUES: SPECTROSCOPIC, Data processing, 010308 nuclear & particles physics, Real-time computing, SIGNAL (programming language), Astrophysics (astro-ph), Process (computing), FOS: Physical sciences, Astronomy and Astrophysics, METHODS: DATA ANALYSIS, Astrophysics, 01 natural sciences, Sample (graphics), Field (computer science), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, 0103 physical sciences, Focus (optics), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Spectrograph, INSTRUMENTATION: SPECTROGRAPHS, Data reduction
Abstract

With new generation spectrographs integral field spectroscopy is becoming a widely used observational technique. The Integral Field Unit of the VIsible Multi-Object Spectrograph on the ESO-VLT allows to sample a field as large as 54" x 54" covered by 6400 fibers coupled with micro-lenses. We are presenting here the methods of the data processing software developed to extract the astrophysical signal of faint sources from the VIMOS IFU observations. We focus on the treatment of the fiber-to-fiber relative transmission and the sky subtraction, and the dedicated tasks we have built to address the peculiarities and unprecedented complexity of the dataset. We review the automated process we have developed under the VIPGI data organization and reduction environment (Scodeggio et al. 2005), along with the quality control performed to validate the process. The VIPGI-IFU data processing environment is available to the scientific community to process VIMOS-IFU data since November 2003., Comment: 19 pages, 10 figures and 1 table. Accepted for publication in PASP

Published
2005

29. The Vimos-VLT Deep Survey: Results from the First-Epoch Observations

Author

R. Pello, Mario Radovich, B. Meneux, Paolo Ciliegi, Vincenzo Ripepi, Stephane Charlot, H. J. McCracken, M. Bondi, Alain Mazure, C. Adami, G. Busarello, E. Zucca, Marco Scodeggio, D. Rizzo, D. Bottini, V. Le Brun, Bruno Marano, B. Garilli, I. Gavignaud, D. Maccagni, O. Ilbert, Yannick Mellier, C. Marinoni, S. Paltani, Roberto Scaramella, L. Tresse, R. Merighi, Sylvie Foucaud, A. Pollo, T. Contini, L. Gregorini, M. Bolzonella, Paola Merluzzi, Angela Bongiorno, G. Vettolani, Luigi Guzzo, P. Franzetti, G. Mathez, Magda Arnaboldi, A. Cappi, S. Bardelli, O. Le Fevre, J. P. Picat, A. Iovino, G. Zamorani, Stephane Arnouts, Lucia Pozzetti, A. Zanichelli, 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), Yannick Mellier, Georges Meylan, YANNICK MELLIER AND GEORGES MEYLAN, Paltani S., Ilbert O., Le Fèvre O., Marinoni C., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J.-P., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Arnouts S., Bardelli S., Bolzonella M., Cappi A., Charlot S., Contini T., Foucaud S., Franzetti P., Gavignaud I., Guzzo L., Iovino A., McCracken H. J., Marano B., Mazure A., Meneux B., Merighi R., Pellò R., Pollo A., Pozzetti L., Radovich M., Zamorani G., Zucca E., Bondi M., Bongiorno A., Busarello G., Ciliegi P., Gregorini L., Mathez G., Mellier Y., Merluzzi P., Ripepi V., Rizzo D, and 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)

Subjects
Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy, Astronomy and Astrophysics, Function (mathematics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Redshift survey, Galaxy, Redshift, Spectral line, Luminosity, Space and Planetary Science, Limiting magnitude, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy)
Abstract

ISBN 0521851963; The Vimos-VLT Deep Survey is a spectroscopic survey aiming at collecting more than 50000 spectra down to a limiting magnitude IAB=24, and 100000 down to IAB=22.5, on a total of about 16 deg2 without any color or morphology preselection. We present the N(z) distribution up to z~ 5, obtained from a purely magnitude-limited sample down to IAB=24, which is an important input to weak-lensing studies. We discuss the evolution of the galaxy luminosity function up to z~ 2, which exhibits a very strong increase in the typical galaxy luminosity Delta M*&simeq; -2.5 in the U band compared to the local value. Surveys like the VVDS also allow to study the galaxy bias as a function of redshift without assumption about its linearity, an assumption that we find to be violated in some cases. A low bias is found, and the linear bias is shown to increase with redshift.

Published
2005

30. The VIRMOS deep imaging survey IV: Near-infrared observations

Author

Thierry Contini, I. Gavignaud, G. Zamorani, M. Scodeggio, O. Le Fevre, M. Radovich, G. Mathez, Bianca Garilli, G. Busarello, H. J. McCracken, Stéphane Arnouts, Giampaolo Vettolani, D. Maccagni, Paola Merluzzi, Stéphane Paltani, Stephane Charlot, D. Bottini, L. Gregorini, Paolo Saracco, R. Pello, Bruno Marano, A. Zanichelli, Yannick Mellier, A. Cappi, Emmanuel Bertin, Olivier Ilbert, B. Meneux, A. Iovino, Paolo Ciliegi, Olga Cucciati, A. Pollo, Roberto Scaramella, A. Mazure, Lucia Pozzetti, R. Merighi, S. Bardelli, J. P. Picat, Magda Arnaboldi, Laurence Tresse, M. Bondi, E. Zucca, D. Rizzo, L. Paioro, V. Le Brun, P. Franzetti, Luigi Guzzo, Angela Bongiorno, Vincenzo Ripepi, Sylvie Foucaud, Christian Marinoni, M. Bolzonella, C. Adami, INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), 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), 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), Services communs OMP (UMS 831), 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 - Osservatorio Astronomico di Bologna (OABO), INAF - Osservatorio Astronomico di Capodimonte (OAC), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, European Southern Observatory (ESO), Dipartimento di Fisica, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Departement de Radioastronomie Millimétrique (DEMIRM), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), 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), Università di Bologna, Dipartimento di Astronomia, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), École normale supérieure - Paris (ENS Paris), Iovino A., McCracken H. J., Garilli B., Foucaud S., Le Fèvre O., Maccagni D., Saracco P., Bardelli S., Busarello G., Scodeggio M., Zanichelli A., Paioro L., Bottini D., Le Brun V., Picat J. P., Scaramella R., Tresse L., Vettolani G., Adami C., Arnaboldi M., Arnouts S., Bolzonella M., Cappi A., Charlot S., Ciliegi P., Contini T., Franzetti P., Gavignaud I., Guzzo L., Ilbert O., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Paltani S., Pellò R., Pollo A., Pozzetti L., Radovich M., Zamorani G., Zucca E., Bertin E., Bondi M., Bongiorno A., Cucciati O., Gregorini L., Mathez G., Mellier Y., Merluzzi P., Ripepi V., and Rizzo D.

Subjects
FOS: Physical sciences, Magnitude (mathematics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, GALAXIES: SURVEYS, infrared: galaxies, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], surveys, 0103 physical sciences, Cluster analysis, 010303 astronomy & astrophysics, Scaling, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Near-infrared spectroscopy, Astronomy and Astrophysics, galaxies: general, cosmology: large-scale structure of Universe, Galaxy, Wavelength, Amplitude, 13. Climate action, Space and Planetary Science, Limiting magnitude
Abstract

In this paper we present a new deep, wide-field near-infrared imaging survey. Our J- and K-band observations in four separate fields complement optical BVRI, ultraviolet and spectroscopic observations undertaken as part of the VIMOS-VLT deep survey (VVDS). In total, our survey spans ~400arcmis^2. Our catalogues are reliable in all fields to at least Kvega~20.75 and Jvega~21.50 (defined as the magnitude where object contamination is less than 10% and completeness greater than 90%). Taken together these four fields represents a unique combination of depth, wavelength coverage and area. We describe the complete data reduction process and outline a comprehensive series of tests carried out to characterise the reliability of the final catalogues. We compare the statistical properties of our catalogues with literature compilations. We find that our J- and K-selected galaxy counts are in good agreement with previously published works, as are our (J-K) versus K colour-magnitude diagrams. Stellar number counts extracted from our fields are consistent with a synthetic model of our galaxy. Using the location of the stellar locus in colour-magnitude space and the measured field-to-field variation in galaxy number counts we demonstrate that the absolute accuracy of our photometric calibration is at the 5% level or better. Finally, an investigation of the angular clustering of K- selected extended sources in our survey displays the expected scaling behaviour with limiting magnitude, with amplitudes in each magnitude bin in broad agreement with literature values., 15 pages, 19 figs, Accepted by A&A

Published
2005

31. The VIMOS VLT deep survey. Computing the two point correlation statistics and associated uncertainties

Author

A. Pollo, B. Meneux, L. Guzzo, O. Le Fèvre, J. Blaizot, A. Cappi, A. Iovino, C. Marinoni, H. J. McCracken, D. Bottini, B. Garilli, V. Le Brun, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, M. Arnaboldi, S. Arnouts, S. Bardelli, M. Bolzonella, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, I. Gavignaud, O. Ilbert, B. Marano, G. Mathez, A. Mazure, R. Merighi, S. Paltani, R. Pellò, L. Pozzetti, M. Radovich, G. Zamorani, E. Zucca, M. Bondi, A. Bongiorno, G. Busarello, L. Gregorini, F. Lamareille, Y. Mellier, P. Merluzzi, V. Ripepi, D. Rizzo, INAF-Osservatorio Astronomico di Brera (INAF-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), INAF-Osservatorio Astronomico di Bologna (OABO), INAF-Osservatorio Astronomico di Brera, 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), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), 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-Osservatorio Astronomico di Roma (INAF-OAR), Istituto di Radioastronomia, Bologna, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Max-Planck-Institut für Astrophysik (MPA), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Pollo A., Meneux B., Guzzo L., Le Fèvre O., Blaizot J., Cappi A., Iovino A., Marinoni C., McCracken H. J., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J.P., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Arnouts S., Bardelli S., Bolzonella M., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Gavignaud I., Ilbert O., Marano B., Mathez G., Mazure A., Merighi R., Paltani S., Pello R., Pozzetti L., Radovich M., Zamorani G., Zucca E., Bondi M., Bongiorno A., Busarello G., Gregorini L., Lamareille F., Mellier Y., Merluzzi P., Ripepi V., Rizzo D., and 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)

Subjects
Physics, COSMIC cancer database, 010308 nuclear & particles physics, Epoch (reference date), Astrophysics (astro-ph), FOS: Physical sciences, Sampling (statistics), Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Correlation function (statistical mechanics), Space and Planetary Science, 0103 physical sciences, Statistics, Galaxy formation and evolution, Cluster analysis, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, VIMOS-VLT Deep Survey
Abstract

We are presenting in this paper a detailed account of the methods used to compute the three-dimensional two-point galaxy correlation function in the VIMOS-VLT deep survey (VVDS). We investigate how instrumental selection effects and observational biases affect the measurements and identify the methods to correct them. We quantify the accuracy of our correction method using an ensemble of fifty mock galaxy surveys generated with the GalICS semi-analytic model of galaxy formation which incorporate the same selection biases and tiling strategy as the real data does. We demonstrate that we are able to recover the real-space two-point correlation function xi(s) to an accuracy better than 10% on scales larger than 1 h^{-1} Mpc, and of about 30% on scales below 1 h^{-1} Mpc, with the sampling strategy used for the first epoch VVDS data. The projected correlation function w_p(r_p) is recovered with an accuracy better than 10% on all scales 0.1, 16 pages, accepted 10-Mar-05 in A&A

Published
2005

32. The GALEX VIMOS-VLT Deep Survey Measurement of the Evolution of the 1500 Å Luminosity Function

Author

S. Arnouts, D. Schiminovich, O. Ilbert, L. Tresse, B. Milliard, M. Treyer, S. Bardelli, T. Budavari, T. K. Wyder, E. Zucca, O. Le Fèvre, D. C. Martin, G. Vettolani, C. Adami, M. Arnaboldi, T. Barlow, L. Bianchi, M. Bolzonella, D. Bottini, Y.-I. Byun, A. Cappi, S. Charlot, T. Contini, J. Donas, K. Forster, S. Foucaud, P. Franzetti, P. G. Friedman, B. Garilli, I. Gavignaud, L. Guzzo, T. M. Heckman, C. Hoopes, A. Iovino, P. Jelinsky, V. Le Brun, Y.-W. Lee, D. Maccagni, B. F. Madore, R. Malina, B. Marano, C. Marinoni, H. J. McCracken, A. Mazure, B. Meneux, R. Merighi, P. Morrissey, S. Neff, S. Paltani, R. Pellò, J. P. Picat, A. Pollo, L. Pozzetti, M. Radovich, R. M. Rich, R. Scaramella, M. Scodeggio, M. Seibert, O. Siegmund, T. Small, A. S. Szalay, B. Welsh, C. K. Xu, G. Zamorani, A. Zanichelli, 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), Schiminovich D., Ilbert O., Arnouts S., Milliard B., Tresse L., Le Fèvre O., Treyer M., Wyder T. K., Budavári T., Zucca E., Zamorani G., Martin D. C., Adami C., Arnaboldi M., Bardelli S., Barlow T., Bianchi L., Bolzonella M., Bottini D., Byun Y.I., Cappi A., Contini T., Charlot S., Donas J., Forster K., Foucaud S., Franzetti P., Friedman P. G., Garilli B., Gavignaud I., Guzzo L., Heckman T. M., Hoopes C., Iovino A., Jelinsky P., Le Brun V., Lee Y.W., Maccagni D., Madore B. F., Malina R., Marano B., Marinoni C., McCracken H. J., Mazure A., Meneux B., Morrissey P., Neff S., Paltani S., Pellò R., Picat J. P., Pollo A., Pozzetti L., Radovich M., Rich R. M., Scaramella R., Scodeggio M., Seibert M., Siegmund O., Small T., Szalay A. S., Vettolani G., Welsh B., Xu C. K., Zanichelli A., and 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)

Subjects
Physics, GALAXIES: MASS FUNCTION, Number density, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, media_common.quotation_subject, Galaxies: Luminosity Function, Astronomy and Astrophysics, Astrophysics, Ultraviolet: Galaxies, 01 natural sciences, Cosmology: Observations, Redshift, Universe, Galaxy, Luminosity, Mass Function, Space and Planetary Science, 0103 physical sciences, Galaxies: Evolution, 010303 astronomy & astrophysics, Luminosity function (astronomy), media_common
Abstract

We present the first measurement of the galaxy luminosity function (LF) at 1500 Å in the range 0.2=alpha>=-1.65, with a marginally significant hint of increase at higher z. (3) We split the sample in three rest-frame (B-I) intervals, providing an approximate spectral type classification: Sb-Sd, Sd-Irr, and unobscured starbursts. We find that the bluest class evolves less strongly in luminosity than the two other classes. On the other hand, their number density increases sharply with z (~15% in the local universe to ~55% at z~1), while that of the reddest classes decreases.

Published
2005

33. The GALEX-VVDS Measurement of the Evolution of the Far-Ultraviolet Luminosity Density and the Cosmic Star Formation Rate

Author

D. Schiminovich, O. Ilbert, S. Arnouts, B. Milliard, L. Tresse, O. Le Fèvre, M. Treyer, T. K. Wyder, T. Budavári, E. Zucca, G. Zamorani, D. C. Martin, C. Adami, M. Arnaboldi, S. Bardelli, T. Barlow, L. Bianchi, M. Bolzonella, D. Bottini, Y.-I. Byun, A. Cappi, T. Contini, S. Charlot, J. Donas, K. Forster, S. Foucaud, P. Franzetti, P. G. Friedman, B. Garilli, I. Gavignaud, L. Guzzo, T. M. Heckman, C. Hoopes, A. Iovino, P. Jelinsky, V. Le Brun, Y.-W. Lee, D. Maccagni, B. F. Madore, R. Malina, B. Marano, C. Marinoni, H. J. McCracken, A. Mazure, B. Meneux, P. Morrissey, S. Neff, S. Paltani, R. Pellò, J. P. Picat, A. Pollo, L. Pozzetti, M. Radovich, R. M. Rich, R. Scaramella, M. Scodeggio, M. Seibert, O. Siegmund, T. Small, A. S. Szalay, G. Vettolani, B. Welsh, C. K. Xu, A. Zanichelli, 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), Schiminovich D., Ilbert O., Arnouts S., Milliard B., Tresse L., Le Fèvre O., Treyer M., Wyder T. K., Budavári T., Zucca E., Zamorani G., Martin D. C., Adami C., Arnaboldi M., Bardelli S., Barlow T., Bianchi L., Bolzonella M., Bottini D., Byun Y.I., Cappi A., Contini T., Charlot S., Donas J., Forster K., Foucaud S., Franzetti P., Friedman P. G., Garilli B., Gavignaud I., Guzzo L., Heckman T. M., Hoopes C., Iovino A., Jelinsky P., Le Brun V., Lee Y.W., Maccagni D., Madore B. F., Malina R., Marano B., Marinoni C., McCracken H. J., Mazure A., Meneux B., Morrissey P., Neff S., Paltani S., Pellò R., Picat J. P., Pollo A., Pozzetti L., Radovich M., Rich R. M., Scaramella R., Scodeggio M., Seibert M., Siegmund O., Small T., Szalay A. S., Vettolani G., Welsh B., Xu C. K., Zanichelli A., and 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)

Subjects
GALAXIES: MASS FUNCTION, Galaxies: Luminosity Function, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Ultraviolet: Galaxies, medicine.disease_cause, 01 natural sciences, Cosmology: Observations, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Galaxies: Evolution, medicine, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), Physics, COSMIC cancer database, 010308 nuclear & particles physics, Star formation, Attenuation, Astrophysics (astro-ph), Astronomy and Astrophysics, Redshift, Galaxy, Mass Function, Space and Planetary Science, Ultraviolet
Abstract

In a companion paper (Arnouts et al. 2004) we presented new measurements of the galaxy luminosity function at 1500 Angstroms out to z~1 using GALEX-VVDS observations (1039 galaxies with NUV0.2) and at higher z using existing data sets. In this paper we use the same sample to study evolution of the FUV luminosity density. We detect evolution consistent with a (1+z)^{2.5+/-0.7} rise to z~1 and (1+z)^{0.5+/-0.4} for z>1. The luminosity density from the most UV-luminous galaxies (UVLG) is undergoing dramatic evolution (x30) between 025%) of the total FUV luminosity density at z, Comment: This paper will be published as part of the Galaxy Evolution Explorer (GALEX) Astrophysical Journal Letters Special Issue. Links to the full set of papers will be available at http://www.galex.caltech.edu/PUBLICATIONS/ after November 22, 2004

Published
2005

34. The VVDS data reduction pipeline: introducing VIPGI, the VIMOS Interactive Pipeline and Graphical Interface

Author

M. Scodeggio, P. Franzetti, B. Garilli, A. Zanichelli, S. Paltani, D. Maccagni, D. Bottini, V. Le Brun, T. Contini, R. Scaramella, C. Adami, S. Bardelli, E. Zucca, L. Tresse, O. Ilbert, S. Foucaud, A. Iovino, R. Merighi, G. Zamorani, I. Gavignaud, D. Rizzo, H. J. McCracken, O. Le Fèvre, J. P. Picat, G. Vettolani, M. Arnaboldi, S. Arnouts, M. Bolzonella, A. Cappi, S. Charlot, P. Ciliegi, L. Guzzo, B. Marano, C. Marinoni, G. Mathez, A. Mazure, B. Meneux, R. Pellò, A. Pollo, L. Pozzetti, M. Radovich, 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), Scodeggio M., Franzetti P., Garilli B., Zanichelli A., Paltani S., Maccagni D., Bottini D., Le Brun V., Contini T., Scaramella R., Adami C., Bardelli S., Zucca E., Tresse L., Ilbert O ., Foucaud S., Iovino A., Merighi R., Zamorani G., Gavignaud I., Rizzo D., McCracken H. J., Le Fèvre O., Picat J. P., Vettolani G., Arnaboldi M., Arnouts S., Bolzonella M., Cappi A., Charlot S., Ciliegi P., Guzzo L., Marano B., Marinoni C., Mathez G., Mazure A., Meneux B., Pellò R., Pollo A., Pozzetti L., Radovich M., 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
Real-time computing, FOS: Physical sciences, Instrumentation: Spectrographs, Techniques: Spectroscopic, Astrophysics, 01 natural sciences, Reduction (complexity), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Methods: Data Analysis, Observatory, 0103 physical sciences, 010303 astronomy & astrophysics, Spectrograph, Graphical user interface, Physics, Very Large Telescope, Measure (data warehouse), 010308 nuclear & particles physics, business.industry, Astrophysics (astro-ph), Astronomy and Astrophysics, Pipeline (software), Space and Planetary Science, business, Data reduction
Abstract

The VIMOS VLT Deep Survey (VVDS), designed to measure 150,000 galaxy redshifts, requires a dedicated data reduction and analysis pipeline to process in a timely fashion the large amount of spectroscopic data being produced. This requirement has lead to the development of the VIMOS Interactive Pipeline and Graphical Interface (VIPGI), a new software package designed to simplify to a very high degree the task of reducing astronomical data obtained with VIMOS, the imaging spectrograph built by the VIRMOS Consortium for the European Southern Observatory, and mounted on Unit 3 (Melipal) of the Very Large Telescope (VLT) at Paranal Observatory (Chile). VIPGI provides the astronomer with specially designed VIMOS data reduction functions, a VIMOS-centric data organizer, and dedicated data browsing and plotting tools, that can be used to verify the quality and accuracy of the various stages of the data reduction process. The quality and accuracy of the data reduction pipeline are comparable to those obtained using well known IRAF tasks, but the speed of the data reduction process is significantly increased, thanks to the large set of dedicated features. In this paper we discuss the details of the MOS data reduction pipeline implemented in VIPGI, as applied to the reduction of some 20,000 VVDS spectra, assessing quantitatively the accuracy of the various reduction steps. We also provide a more general overview of VIPGI capabilities, a tool that can be used for the reduction of any kind of VIMOS data., 10 pages, submitted to Astronomy and Astrophysics

Published
2005

35. The VVDS-VLA deep field. II. Optical and near infrared identifications of VLA S1.4 GHz > 80 mu Jy sources in the VIMOS VLT deep survey VVDS-02h field

Author

P. Ciliegi, G. Zamorani, M. Bondi, L. Pozzetti, M. Bolzonella, L. Gregorini, B. Garilli, A. Iovino, H. J. McCracken, Y. Mellier, M. Radovich, H. R. de Ruiter, P. Parma, D. Bottini, V. Le Brun, O. Le Fèvre, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, M. Arnaboldi, S. Arnouts, S. Bardelli, A. Cappi, S. Charlot, T. Contini, S. Foucaud, P. Franzetti, L. Guzzo, O. Ilbert, B. Marano, C. Marinoni, G. Mathez, A. Mazure, B. Meneux, R. Merighi, P. Merluzzi, S. Paltani, A. Pollo, E. Zucca, A. Bongiorno, G. Busarello, I. Gavignaud, R. Pellò, V. Ripepi, D. Rizzo, 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), 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), Ciliegi P., Zamorani G., Bondi M., Pozzetti L., Bolzonella M., Gregorini L., Garilli B., Iovino A., McCracken H. J., Mellier Y., Radovich M., de Ruiter H. R., Parma P., Bottini D., Le Brun V., Le Fèvre O., Maccagni D., Picat J. P., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Arnouts S., Bardelli S., Cappi A., Charlot S., Contini T., Foucaud S., Franzetti P., Guzzo L., Ilbert O., Marano B., Marinoni C., Mathez G., Mazure A., Meneux B., Merighi R., Merluzzi P., Paltani S., Pollo A., Zucca E., Bongiorno A., Busarello G., Gavignaud I., Pellò R., Ripepi V., and Rizzo D.

Subjects
Physics, radio continuum: galaxies, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Hubble Deep Field, Astrophysics::High Energy Astrophysical Phenomena, Near-infrared spectroscopy, Flux, Astronomy and Astrophysics, galaxies: starburst, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, galaxies: general, Galaxy, Redshift, Luminosity, Space and Planetary Science, cosmology: observations, 0103 physical sciences, Magnitude (astronomy), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Photometric redshift
Abstract

In this paper we present the optical and near-infrared identifications of the 1054 radio sources detected in the 20 cm deep radio survey down to a 5sigma flux limit of ~80 muJy obtained with the VLA in the VIMOS VLT Deep Survey VVDS-02h deep field. Using U,B,V,R,I and K data, with limiting magnitudes of UAB~25.4, BAB~26.5, VAB~26.2, RAB~25.9 IAB~25.0, JAB~24.2, KAB~23.9 (50% completeness) we identified 718 radio sources (~74% of the whole sample). The photometric redshift analysis shows that, in each magnitude bin, the radio sample has a higher median photometric redshift than the whole optical sample, while the median (V-I)AB color of the radio sources is redder than the median color of the whole optical sample. These results suggest that radio detection is preferentially selecting galaxies with higher intrinsic optical luminosity. From the analysis of the optical properties of the radio sources as function of the radio flux, we found that while about 35% of the radio sources are optically unidentified in the higher radio flux bin (S> 1.0 mJy), the percentage of unidentified sources decreases to about 25% in the faintest bins (S< 0.5 mJy). The median IAB magnitude for the total sample of radio sources, i.e. including also the unidentified ones, is brighter in the faintest radio bins than in the bin with higher radio flux. This suggests that most of the faintest radio sources are likely to be associated to relatively lower radio luminosity objects at relatively modest redshift, rather than radio-powerful, AGN type objects at high redshift. Using a classification in early-type and late-type galaxies based on the (B-I)AB color and the photometric redshift, we found that the majority of the radio sources below ~0.15 mJy are indeed late-type star forming galaxies. Finally, the radio sources without optical counterpart in our deep imaging have a median radio flux of 0.15 mJy, equal to that of identified sources. Given the very faint optical limits, these unidentified radio sources probably contain a significant fraction of obscured and/or high redshift galaxies.

Published
2005

36. Mass-to-light ratio gradients in early-type galaxy haloes

Author

Kenneth C. Freeman, Nigel G. Douglas, Michael R. Merrifield, Nicola R. Napolitano, Konrad Kuijken, Aaron J. Romanowsky, M. Capaccioli, Magda Arnaboldi, Ortwin Gerhard, N. R., Napolitano, A. J., Romanowsky, N. G., Dougla, M. R., Merrifield, K., Kuijken, M., Arnaboldi, O., Gerhard, K. C., Freeman, Capaccioli, Massimo, Napolitano, N. R, Romanowsky, A. J., Douglas, N. G., Merrifield, M. R., Kuijken, K, Arnaboldi, M, Gerhard, O, and Freeman, K. C.

Subjects
Radial gradient, galaxies : evolution, DWARF SPHEROIDAL GALAXIES, Population, FOS: Physical sciences, DARK-MATTER HALOS, Astrophysics, galaxies : kinematics and dynamics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, dark matter, Luminosity, galaxies : fundamental parameters, ELLIPTIC GALAXIES, 0103 physical sciences, galaxies : haloes, 010306 general physics, education, 010303 astronomy & astrophysics, Mass-to-light ratio, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, Star formation, Astrophysics (astro-ph), Astronomy and Astrophysics, Galaxy, Early type, GLOBULAR-CLUSTER SYSTEM, Space and Planetary Science, DIGITAL SKY SURVEY, Halo, INFRARED FUNDAMENTAL PLANE, VELOCITY DISPERSION, LAMBDA-CDM UNIVERSE, SPIRAL GALAXIES, STELLAR POPULATION
Abstract

Since the near future should see a rapidly expanding set of probes of the halo masses of individual early-type galaxies, we introduce a convenient parameter for characterising the halo masses from both observational and theoretical results: \dML, the logarithmic radial gradient of the mass-to-light ratio. Using halo density profiles from LCDM simulations, we derive predictions for this gradient for various galaxy luminosities and star formation efficiencies $\epsilon_{SF}$. As a pilot study, we assemble the available \dML\ data from kinematics in early-type galaxies - representing the first unbiassed study of halo masses in a wide range of early-type galaxy luminosities - and find a correlation between luminosity and \dML, such that the brightest galaxies appear the most dark-matter dominated. We find that the gradients in most of the brightest galaxies may fit in well with the LCDM predictions, but that there is also a population of fainter galaxies whose gradients are so low as to imply an unreasonably high star formation efficiency $\epsilon_{SF} > 1$. This difficulty is eased if dark haloes are not assumed to have the standard LCDM profiles, but lower central concentrations., Comment: 17 pages, 13 figures. Accepted for publication on MNRAS

Published
2004
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37. Polar Ring Galaxies and the Tully Fisher relation: implications for the dark halo shape

Author

Enrica Iodice, Linda S. Sparke, Wim van Driel, Francoise Combes, F. Bournaud, Massimo Capaccioli, Magda Arnaboldi, Arnaboldi, M., Iodice, E., Bournaud, F., Combes, F., Sparke, L. S., van Driel, W., Capaccioli, Massimo, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Galaxies et cosmologie, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), University of Wisconsin-Madison, 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), Physique des Galaxies et Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Spiral galaxy, Astrophysics (astro-ph), Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Tully–Fisher relation, Ring (chemistry), Disc galaxy, Galaxy, Luminosity, Galactic halo, Dark matter halo, Space and Planetary Science, Elliptical galaxy, Polar, Halo, Disc, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract

We have investigated the Tully-Fisher relation for Polar Ring Galaxies (PRGs), based on near infrared, optical and HI data available for a sample of these peculiar objects. The total K-band luminosity, which mainly comes from the central host galaxy, and the measured HI linewidth at 20% of the peak line flux density, which traces the potential in the polar plane, place most polar rings of the sample far from the Tully-Fisher relation defined for spiral galaxies, with many PRGs showing larger HI linewidths than expected for the observed K band luminosity. This result is confirmed by a larger sample of objects, based on B-band data. This observational evidence may be related to the dark halo shape and orientation in these systems, which we study by numerical modeling of PRG formation and dynamics: the larger rotation velocities observed in PRGs can be explained by a flattened polar halo, aligned with the polar ring., 22 pages, 8 postscript figures, accepted for publication in Astrophysical Journal

Published
2002

38. Detection, photometry and slitless radial velocities of 535 planetary nebulae in the flattened elliptical galaxy NGC 4697

Author

Kenneth C. Freeman, Arno Riffeser, Ortwin Gerhard, Rolf-Peter Kudritzki, Michael Matthias, Roberto H. Méndez, Magda Arnaboldi, Massimo Capaccioli, Mndez, R. H., A., RIFFESER A, Kudritzki, R. P., Matthias, M, Freeman, K. C., Arnaboldi, M, Capaccioli, Massimo, and Gerhard, O.

Subjects
Physics, Dark matter, Astrophysics (astro-ph), Velocity dispersion, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Planetary nebula, Planetary nebula luminosity function, Galaxy, Photometry (astronomy), Space and Planetary Science, Elliptical galaxy, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Galaxy rotation curve, Astrophysics::Galaxy Astrophysics
Abstract

We have detected 535 planetary nebulae (PNs) in NGC 4697, using the classic on-band, off-band filter technique with the Focal Reducer and Spectrograph (FORS) at the Cassegrain focus of the first 8-meter telescope unit of the ESO Very Large Telescope. From our photometry we have built the [O III] 5007 planetary nebula luminosity function (PNLF) of NGC 4697. It indicates a distance of 10.5 Mpc, substantially smaller than a previous estimate of 24 Mpc used in earlier dynamical studies. The PNLF also provides an estimate of the specific PN formation rate. Combining the information from on-band images with PN positions on dispersed, slitless grism images, we have obtained radial velocities for 531 of the 535 PNs. They provide kinematic information up to a distance of almost three effective radii from the nucleus. Some rotation is detected in the outer regions, but the rotation curve of this galaxy appears to drop beyond one effective radius. Assuming an isotropic velocity distribution, the velocity dispersion profile is consistent with no dark matter within three effective radii of the nucleus (however, some dark matter can be present if the velocity distribution is anisotropic). We obtain a blue mass-to-light ratio of 11. Earlier M/L ratios for NGC 4697 were too small, because of the too large distance used for their derivation., Comment: 52 pages, 24 Postscript figures, ApJ 2001, in press

Published
2001
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39. The stellar dynamics and mass of NGC 1316 using the radial velocities of planetary nebulae

Author

Roberto H. Méndez, Magda Arnaboldi, Massimo Capaccioli, Rolf-Peter Kudritzki, M. Matthias, Holland C. Ford, Kenneth C. Freeman, Ortwin Gerhard, Arnaboldi, M, Freeman, K. C., Gerhard, O, Matthias, M, Kudritzki, R. P., Mndez, R. H., Capaccioli, Massimo, and Ford, H.

Subjects
Physics, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radius, Astrophysics::Cosmology and Extragalactic Astrophysics, Rotation, 01 natural sciences, Planetary nebula, Galaxy, Dust lane, Spectral line, Radial velocity, Space and Planetary Science, Stellar dynamics, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract

We present a study of the kinematics of the outer regions of the early-type galaxy NGC 1316, based on radial velocity measurements of 43 planetary nebulae as well as deep integrated-light absorption line spectra. The smoothed velocity field of NGC 1316 indicates fast rotation at a distance of 16 kpc, possibly associated with an elongated feature orthogonal to the inner dust lanes. The mean square stellar velocity is approximately independent of radius, and the estimated total mass of the system is 2.6 x 10^11 M_sun within a radius of 16 kpc, implying an integrated mass-to-light ratio of M/L_B = 8., 39 pages, 14 figures, in press on The Astrophysical Journal n. 507

Published
1998

40. Kinematics of the Ionized Gas in NGC 253

Author

Enrico Cappellaro, Baerbel Koribalski, Magda Arnaboldi, M. Capaccioli, Enrico V. Held, Arnaboldi, M., Capaccioli, Massimo, Cappellaro, E., Held, E. V., and Koribalski, B.

Subjects
Physics, Space and Planetary Science, Astronomy, Astronomy and Astrophysics, Astrophysics, Plasma, Kinematics, Galaxy
Published
1995

41. NGC 1399: A complex dynamical case

Author

Magda Arnaboldi, Massimo Capaccioli, Nicola R. Napolitano, Napolitano, N. R, Arnaboldi, M, and Capaccioli, Massimo

Subjects
Physics, Mass distribution, Dark matter, Astrophysics (astro-ph), Velocity dispersion, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Impulse (physics), Planetary nebula, Galaxy, Space and Planetary Science, Globular cluster, Halo, Astrophysics::Galaxy Astrophysics
Abstract

Evidence for a disturbed velocity structure in the outer regions of the galaxy NGC1399 comes from a re-analysis of the planetary nebulae data from Arnaboldi et al. (1994). We find a strong rotation along a P.A.=140 degrees for R, 10 pages, 15 figures, accepted for pubblication in A&A

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