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Start Over Author "Boissier, S" Topic galaxies: evolution
31 results on '"Boissier, S"'

1. A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Author

Boselli, A., Fossati, M., Longobardi, A., Kianfar, K., Dametto, N.Z., Amram, P., Anderson, J. P., Andreani, P., Boissier, S., Boquien, Médéric, Buat, Véronique, Consolandi, G., Cortese, L., Côté, P., Cuillandre, J.C., Ferrarese, L., Galbany, Lluís, Gavazzi, G., Gwyn, Stephen, Hensler, G., Hutchings, J., Peng, E. W., Postma, J. F., Roediger, J., Roehlly, Y., Serra, P., Trinchieri, G., Centre National D'Etudes Spatiales (France), National Aeronautics and Space Administration (US), Indian Institue of Astrophysics, Canadian Space Agency, Korea Astronomy and Space Science Institute, National Institutes of Natural Sciences (Japan), Ministerio de Ciencia e Innovación (España), Australian Research Council, and European Commission

Subjects
Galaxies: elliptical and lenticular, clusters: individual: Virgo [Galaxies], Galaxies: evolution, interactions [Galaxies], clusters: general [Galaxies], Galaxies: clusters: individual: Virgo, evolution [Galaxies], Galaxies: interactions, cD, elliptical and lenticular [Galaxies], Galaxies: ISM, ISM [Galaxies], Galaxies: clusters: general
Abstract

As part of the Virgo Cluster Survey Tracing Ionised Gas Emission, a blind narrow-band H+[NII] imaging survey of the Virgo cluster carried out with MegaCam at the CFHT, we discovered eight massive (1010 . Mstar . 1011 M) lenticular galaxies with prominent ionised gas emission features in their inner (a few kiloparsec) regions. These features are either ionised gas filaments similar to those observed in cooling flows (two galaxies), or they are thin discs with sizes 0:7 . R(H) . 2:0 kpc (six galaxies), thus significantly smaller than those of the stellar disc (R(H) ' 7 22%Riso(r)). The morphological properties of these discs are similar to those of the dust seen in absorption in high-resolution HST images. Using a unique set of multifrequency data, including new or archival ASTROSAT/UVIT, GALEX, HST, CFHT, Spitzer, and Herschel imaging data, combined with IFU (MUSE, ALMA) and long-slit (SOAR) spectroscopy, we show that while the gas that is located within these inner discs is photoionised by young stars, which signals ongoing star formation, the gas in the filamentary structures is shock ionised. The star formation surface brightness of these discs is similar to that observed in late-type galaxies. Because of their reduced size, however, these lenticular galaxies are located below the main sequence of unperturbed or cluster star-forming systems. By comparing the dust masses measured from absorption maps in optical images, from the Balmer decrement, or estimated by fitting the UV-to-far-IR spectral energy distribution of the target galaxies, we confirm that the dust masses derived from optical attenuation maps are heavily underestimated because of geometrical eects due to the relative distribution of the absorbing dust and the emitting stars. We also show that these galaxies have gas-to-dust ratios of G=D ' 80320 30 , and that the star formation within these discs follows the Schmidt relation, but with an eciency that is reduced by a factor of 2.5. Using our unique set of multifrequency data, we discuss the possible origin of the ionised gas in these objects, which suggests multiple and complex formation scenarios for massive lenticular galaxies in clusters., We acknowledge financial support from “Programme National de Cosmologie and Galaxies” (PNCG) funded by CNRS/INSU-IN2P3-INP, CEA and CNES, France, and from “Projet International de Coopération Scientifique” (PICS) with Canada funded by the CNRS, France. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration and of the GOLDMine database (http://goldmine.mib.infn.it/) (Gavazzi et al. 2003). The UVIT project is collaboration between the following institutes from India: Indian Institute of Astrophysics (IIA), Bengaluru, Inter University Centre for Astronomy and Astrophysics (IUCAA), Pune, and National Centre for Radioastrophysics (NCRA) (TIFR), Pune, and the Canadian Space Agency (CSA). This paper makes use of the following ALMA data: ADS/JAO.ALMA 2013.1.00493.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. M.F. has received funding from the European Research Council (ERC) (grant agreement No 757535). N.Z.D. acknowledges partial support from FONDECYT through project 3190769. L.G. acknowledges financial support from the Spanish Ministry of Science and Innovation (MCIN) under the 2019 Ramón y Cajal program RYC2019-027683 and from the Spanish MCIN project HOSTFLOWS PID2020-115253GA-I00. M.B. gratefully acknowledges support by the ANID BASAL project FB210003 and the FONDECYT regular grant 1211000. L.C. acknowledges support from the Australian Research Council Discovery Project and Future Fellowship funding schemes (DP210100337, FT180100066). Parts of this research were conducted by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013.

Published
2022

2. A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Author

Longobardi, A., Boselli, A., Fossati, M., Villa-Vélez, J. A., Bianchi, S., Casasola, V., Sarpa, E., Combes, F., Hensler, G., Burgarella, D., Schimd, C., Nanni, A., Côté, P., Buat, V., Amram, P., Ferrarese, L., Braine, J., Trinchieri, G., Boissier, S., Boquien, M., Andreani, P., Gwyn, S., and Cuillandre, J. C.

Subjects
galaxies: clusters: individual: Virgo cluster, galaxies: clusters: intracluster medium, galaxies: clusters: general, galaxies: interactions, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, Astrophysics::Galaxy Astrophysics, galaxies: ISM
Abstract

Aims: We measure far-infrared (FIR) emission from tails of stripped dust following the ionised and atomic gas components in galaxies undergoing ram pressure stripping. We study the dust-to-gas relative distribution and mass ratio in the stripped interstellar medium and relate them to those of the intra-cluster medium (ICM), thus linking the cluster-ICM-galaxy evolution at small-scales. The galaxy sample consists of three Scd Virgo galaxies with stellar masses in the range of 10⁹ ≲ M* ≲ 10¹⁰ M⊙ and within 1 Mpc from the cluster centre, namely NGC 4330, NGC 4522, and NGC 4654. Methods: Through the analysis of Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE) Hα, Herschel SPIRE FIR, and VLA Imaging of Virgo in Atomic gas HI data, we trace the spatial distribution of the tails and infer the dust and gas masses from the measured FIR 250 μm and HI flux densities. Dust-to-gas mass ratios in the tails are analysed as a function of the galaxy mass, metallicity, and dust temperature. Results: Along the stripped component, the dust distribution closely follows the HI and Hα emitting gas, which extend beyond the optical disc (defined by the B-band 25th magnitude isophote). In these regions, the dust-to-gas mass ratios are 2.0 ± 0.6 × 10⁻³, 0.7 ± 0.1 × 10⁻³, and 0.4 ± 0.03 × 10⁻³ for NGC 4330, NGC 4522, and NGC 4654, respectively. Thus, dust is widespread in the stripped material with a lower dust-to-gas mass ratio (up to a factor of 15) than the one measured in the main body of nearby galaxies. We also find a negative trend in the dust-to-gas mass ratio as a function of the metallicity that can be explained in terms of a dust component more centrally concentrated in more metal-rich systems. Together with the finding that the stripped dust is cold, Td ≲ 25 K, our results can be interpreted as a consequence of an outside-in stripping of the galaxy interstellar medium. Conclusions: Gas and dust in galaxies are perturbed in a similar fashion by the cluster environment, although their relative contribution differs from the one measured in the main body of the galaxies. When this value is considered, ram pressure stripping is consistent with being one of the key mechanisms in building up the Virgo intra-cluster component, injecting dust grains into the ICM, thus contributing to its metal enrichment.

Published
2020

3. A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE): III. Star formation in the stripped gas of NGC 4254

Author

Boselli, A., Fossati, M., Cuillandre, J. C., Boissier, S., Boquien, M., Buat, V., Burgarella, D., Consolandi, G., Cortese, L., Côté, P., Côté, S., Durrell, P., Ferrarese, L., Fumagalli, M., Gavazzi, G., Gwyn, S., Hensler, G., Koribalski, B., Roediger, J., Roehlly, Y., Russeil, D., Sun, M., Toloba, E., Vollmer, B., Zavagno, Annie, 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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB), Bordeaux population health (BPH), Université de Bordeaux (UB)-Institut de Santé Publique, d'Épidémiologie et de Développement (ISPED)-Institut National de la Santé et de la Recherche Médicale (INSERM), Shanghai Maritime University, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Sciences, EDP

Subjects
galaxies: clusters: general, galaxies: individual: NGC 4254, galaxies: clusters: individual: Virgo, galaxies: interactions, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, galaxies: ISM
Abstract

International audience; During pilot observations of the Virgo Environmental Survey Tracing Galaxy Evolution (VESTIGE), a blind narrow-band Hα + [NII] imaging survey of the Virgo cluster carried out with MegaCam at the CFHT, we have observed the spiral galaxy NGC 4254 (M99). Deep Hα + [NII] narrow-band and GALEX UV images reveal the presence of 60 compact (70–500 pc radius) star-forming regions up to ≃20 kpc outside the optical disc of the galaxy. These regions are located along a tail of HI gas stripped from the disc of the galaxy after a rapid gravitational encounter with another Virgo cluster member that simulations indicate occurred 280–750 Myr ago. We have combined the VESTIGE data with multifrequency data from the UV to the far-infrared to characterise the stellar populations of these regions and study the star formation process in an extreme environment such as the tails of stripped gas embedded in the hot intracluster medium. The colour, spectral energy distribution (SED), and linear size consistently indicate that these regions are coeval and have been formed after a single burst of star formation that occurred ≲100 Myr ago. These regions might become free floating objects within the cluster potential well, and be the local analogues of compact sources produced after the interaction of gas-rich systems that occurred during the early formation of clusters.

Published
2018
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4. An Hα kinematic survey of the Herschel Reference Survey: I. Fabry–Perot observations with the 1.93 m telescope at OHP,.

Author

Gómez-López, J. A., Amram, P., Epinat, B., Boselli, A., Rosado, M., Marcelin, M., Boissier, S., Gach, J.-L., Sánchez-Cruces, M., and Sardaneta, M. M.

Subjects
TELESCOPES, STELLAR mass, POWER spectra, DATA reduction, SPIRAL galaxies
Abstract

Aims. We present new 2D high resolution Fabry–Perot spectroscopic observations of 152 star-forming galaxies that are part of the Herschel Reference Survey (HRS), which is a complete K-band selected, volume-limited sample of nearby galaxies that spans a wide range of stellar mass and morphological types. Methods. By using improved data reduction techniques, that provide adaptive binning based on Voronoi tessellation, and using large field-of-view observations, we derived high spectral resolution (R >  10 000) Hα datacubes from which we computed Hα maps and radial 2D velocity fields that are based on several of thousand independent measurements. A robust method based on such fields allowed us to accurately compute rotation curves and kinematical parameters, for which uncertainties are calculated using a method based on the power spectrum of the residual velocity fields. Results. We checked the consistency of the rotation curves by comparing our maximum rotational velocities to those derived from H I data, and by computing the i-band, NIR, stellar, and baryonic Tully-Fisher relations. We used this set of kinematical data combined with those available at other frequencies to study, for the first time, the relation between the dynamical and the total baryonic mass (stars, atomic and molecular gas, metals, and dust) and to derive the baryonic and dynamical main sequence on a representative sample of the local universe. [ABSTRACT FROM AUTHOR]

Published
2019
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5. Mass assembly in quiescent and star-forming galaxies since z similar or equal to 4 from UltraVISTA

Author

Ilbert, O., McCracken, H. J., Le Fevre, O., Capak, P., Dunlop, J., Karim, A., Renzini, M. A., Caputi, K., Boissier, S., Arnouts, S., Aussel, H., Comparat, J., Guo, Q., Hudelot, P., Kartaltepe, J., Kneib, J. P., Krogager, J. K., Le Floc'h, E., Lilly, S., Mellier, Y., Milvang-Jensen, B., Moutard, T., Onodera, M., Richard, J., Salvato, M., Sanders, D. B., Scoville, N., Silverman, J. D., Taniguchi, Y., Tasca, L., Thomas, Rajat, Toft, S., Tresse, L., Vergani, D., Wolk, M., Zirm, A., and Astronomy

Subjects
ACTIVE GALACTIC NUCLEI, FORMATION HISTORY, Astrophysics::Cosmology and Extragalactic Astrophysics, VLT DEEP SURVEY, SPECTRAL ENERGY-DISTRIBUTIONS, COSMOS FIELD, STELLAR POPULATION SYNTHESIS, LUMINOSITY FUNCTION, galaxies: star formation, KECK SPECTROSCOPY, galaxies: stellar content, Astrophysics::Solar and Stellar Astrophysics, galaxies: formation, galaxies: distances and redshifts, galaxies: evolution, RED SEQUENCE, PHOTOMETRIC REDSHIFTS, Astrophysics::Galaxy Astrophysics
Abstract

We estimate the galaxy stellar mass function and stellar mass density for star-forming and quiescent galaxies with 0.2 1.5 consistent with the expected uncertainties. We also develop a new method to infer the specific star formation rate from the mass function of star-forming galaxies. We find that the specific star formation rate of 10(10-10.5) M-circle dot galaxies increases continuously in the redshift range 1

Published
2013

6. Quenching of the star formation activity in cluster galaxies.

Author

Boselli, A., Roehlly, Y., Fossati, M., Buat, V., Boissier, S., Burgarella, D., Boquien, M., Ciesla, L., Gavazzi, G., and Serra, P.

Subjects
GALAXY clusters, STAR formation, VIRGO (Constellation), SPECTRAL energy distribution, INTERSTELLAR hydrogen, GALACTIC evolution
Abstract

We study the star formation quenching mechanism in cluster galaxies by fitting the spectral energy distribution (SED) of the Herschel Reference Survey, a complete volume-limited K-band-selected sample of nearby galaxies including objects in different density regions, from the core of the Virgo cluster to the general field. The SEDs of the target galaxies were fitted using the CIGALE SED modelling code. The truncated activity of cluster galaxies was parametrised using a specific star formation history with two free parameters, the quenching age QA and the quenching factor QF. These two parameters are crucial for the identification of the quenching mechanism, which acts on long timescales when starvation processes are at work, but is rapid and efficient when ram pressure occurs. To be sensitive to an abrupt and recent variation of the star formation activity, we combined twenty photometric bands in the UV to far-infrared in a new way with three age-sensitive Balmer line absorption indices extracted from available medium-resolution (R ~ 1000) integrated spectroscopy and with Hα narrow-band imaging data. The use of a truncated star formation history significantly increases the quality of the fit in HI-deficient galaxies of the sample, that is to say, in those objects whose atomic gas content has been removed during the interaction with the hostile cluster environment. The typical quenching age of the perturbed late-type galaxies is QA ≲ 300 Myr whenever the activity of star formation is reduced by 50% < QF ≤ 80% and QA ≲ 500 Myr for QF > 80%, while that of the quiescent early-type objects is QA ≃ 1−3 Gyr. The fraction of late-type galaxies with a star formation activity reduced by QF > 80% and with an HI-deficiency parameter HI−def > 0.4 drops by a factor of ~5 from the inner half virial radius of the Virgo cluster (R/Rvir < 0.5), where the hot diffuse X-ray emitting gas of the cluster is located, to the outer regions (R/Rvir > 4). The efficient quenching of the star formation activity observed in Virgo suggests that the dominant stripping process is ram pressure. We discuss the implication of this result in the cosmological context of galaxy evolution. [ABSTRACT FROM AUTHOR]

Published
2016
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7. The properties of the Malin 1 galaxy giant disk A panchromatic view from the NGVS and GUViCS surveys.

Author

Boissier, S., Boselli, A., Ferrarese, L., Côté, P., Roehlly, Y., Gwyn, S. D. J., Cuillandre, J.-C., Roediger, J., Koda, J., Muños Mateos, J. C., Gil de Paz, A., and Madore, B. F.

Abstract

Context. Low surface brightness galaxies (LSBGs) represent a significant percentage of local galaxies but their formation and evolution remain elusive. They may hold crucial information for our understanding of many key issues (i.e., census of baryonic and dark matter, star formation in the low density regime, mass function). The most massive examples – the so called giant LSBGs – can be as massive as the Milky Way, but with this mass being distributed in a much larger disk. Aims. Malin 1 is an iconic giant LSBG – perhaps the largest disk galaxy known. We attempt to bring new insights on its structure and evolution on the basis of new images covering a wide range in wavelength. Methods. We have computed surface brightness profiles (and average surface brightnesses in 16 regions of interest), in six photometric bands (FUV, NUV, u, g, i, z). We compared these data to various models, testing a variety of assumptions concerning the formation and evolution of Malin 1. Results. We find that the surface brightness and color profiles can be reproduced by a long and quiet star-formation history due to the low surface density; no significant event, such as a collision, is necessary. Such quiet star formation across the giant disk is obtained in a disk model calibrated for the Milky Way, but with an angular momentum approximately 20 times larger. Signs of small variations of the star-formation history are indicated by the diversity of ages found when different regions within the galaxy are intercompared. Conclusions. For the first time, panchromatic images of Malin 1 are used to constrain the stellar populations and the history of this iconic example among giant LSBGs. Based on our model, the extreme disk of Malin 1 is found to have a long history of relatively low star formation (about 2 M⊙ yr-1). Our model allows us to make predictions on its stellar mass and metallicity. [ABSTRACT FROM AUTHOR]

Published
2016
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8. Metal enrichment in a semi-analytical model, fundamental scaling relations, and the case of Milky Way galaxies.

Author

Cousin, M., Buat, V., Boissier, S., Bethermin, M., Roehlly, Y., and Génois, M.

Abstract

Context. Gas flows play a fundamental role in galaxy formation and evolution, providing the fuel for the star formation process. These mechanisms leave an imprint in the amount of heavy elements that enrich the interstellar medium. Thus, the analysis of this metallicity signature provides additional constraint on the galaxy formation scenario. Aims. We aim to discriminate between four different galaxy formation models based on two accretion scenarios and two different star formation recipes. We address the impact of a bimodal accretion scenario and a strongly regulated star formation recipe on the metal enrichment process of galaxies. Methods. We present a new extension of the eGalICS model, which allows us to track the metal enrichment process in both stellar populations and in the gas phase. Based on stellar metallicity bins from 0 to 2.5 Z⊙, our new chemodynamical model is applicable for situations ranging from metal-free primordial accretion to very enriched interstellar gas contents. We use this new tool to predict the metallicity evolution of both the stellar populations and gas phase. We compare these predictions with recent observational measurements. We also address the evolution of the gas metallicity with the star formation rate (SFR). We then focus on a sub-sample of Milky Way-like galaxies. We compare both the cosmic stellar mass assembly and the metal enrichment process of such galaxies with observations and detailed chemical evolution models. Results. Our models, based on a strong star formation regulation, allow us to reproduce well the stellar mass to gas-phase metallicity relation observed in the local Universe. The shape of our average stellar mass to stellar metallicity relations is in good agreement with observations. However, we observe a systematic shift towards high masses. Our M⋆ − Zg −SFR relation is in good agreement with recent measurements: our best model predicts a clear dependence with the SFR. Both SFR and metal enrichment histories of our Milky Way-like galaxies are consistent with observational measurements and detailed chemical evolution models. We finally show that Milky Way progenitors start their evolution below the observed main sequence and progressively reach this observed relation at z ≃ 0. [ABSTRACT FROM AUTHOR]

Published
2016
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9. The GALEX Ultraviolet Virgo Cluster Survey (GUViCS).

Author

Boselli, A., Boissier, S., Voyer, E., Ferrarese, L., Consolandi, G., Cortese, L., Côté, P., Cuillandre, J. C., Gavazzi, G., Gwyn, S., Heinis, S., Ilbert, O., MacArthur, L., and Roehlly, Y.

Subjects
*STELLAR luminosity function, *ULTRAVIOLET radiation, *GALAXIES, *REDSHIFT, *LUMINOSITY, VIRGO Cluster
Abstract

We use the GALEX data of the GUViCS survey to construct the near-ultraviolet (NUV) luminosity function of the Virgo cluster over ∼300 deg2, an area covering the cluster and its surrounding regions up to ∼1.8 virial radii. The NUV luminosity function is also determined for galaxies of different morphological types and NUV - i colours, and for the different substructures within the cluster. These luminosity functions are robust vs. statistical corrections since based on a sample of 833 galaxies mainly identified as cluster members with spectroscopic redshift (808) or high-quality optical scaling relations (10). We fit these luminosity functions with a Schechter function, and compare the fitted parameters with those determined for other nearby clusters and for the field. The faint end slope of the Virgo NUV luminosity function (α = -1.19), here sampled down to ∼NUV = -11.5 mag, is significantly flatter than the value measured in other nearby clusters and similar to the field value. Similarly, M* = -17.56 is one to two magnitudes fainter than measured in Coma, A1367, the Shapley supercluster, and the field. These differences seem to be due to the quite uncertain statistical corrections and the small range in absolute magnitude sampled in these clusters. We do not observe strong systematic differences in the overall NUV luminosity function of the core of the cluster with respect to that of its periphery. We note, however, that the relative contribution of red and blue galaxies at the faint end is inverted, with red quiescent objects dominating the core of the cluster and star forming galaxies dominating beyond one virial radius. This observational evidence is discussed in the framework of galaxy evolution in dense environments. [ABSTRACT FROM AUTHOR]

Published
2016
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10. The GALEX Ultraviolet Virgo Cluster Survey (GUViCS).

Author

Boselli, A., Voyer, E., Boissier, S., Cucciati, O., Consolandi, G., Cortese, L., Fumagalli, M., Gavazzi, G., Heinis, S., Roehlly, Y., and Toloba, E.

Subjects
VIRGO Cluster, ASTRONOMICAL surveys, GALACTIC evolution, STAR formation, INTERSTELLAR medium, LOW mass stars
Abstract

We study the role of the environment on galaxy evolution using a sample of 868 galaxies in the Virgo cluster and in its surrounding regions that are selected from the GALEX Ultraviolet Virgo Cluster Survey (GUViCS) with the purpose of understanding the origin of the red sequence in dense environments. The sample spans a wide range in morphological types (from dwarf ellipticals to Im and BCD) and stellar masses (107 ≲ Mstar ≲ 1011.5 M☉). We collected multifrequency data covering the whole electromagnetic spectrum for most of the galaxies, including UV, optical, mid- and far-infrared imaging data, as well as optical and HI spectroscopic data. We first identify the different dynamical substructures that compose the Virgo cluster, and we calculate the local density of galaxies using different methods. We then study the distribution of galaxies belonging to the red sequence, the green valley, and the blue cloud within the different cluster substructures or as a function of galaxy density. Our analysis indicates that all the most massive galaxies (Mstar ☉ 1011 M☉) are slow rotators and are the dominant galaxies of the different cluster substructures, which are generally associated with a diffuse X-ray emission. They are probably the result of major merging events that occurred at early epochs, as also indicated by their very old stellar populations. Slow rotators of lower stellar mass (108.5 ≲ Mstar ≲ 1011 M☉) are also preferentially located within the different high-density substructures of the cluster. Their position in the velocity space indicates that they are virialised within the cluster; thus, they are Virgo members since its formation. They have been shaped by gravitational perturbations occurring within the infalling groups that later form the cluster (pre-processing). On the contrary, low-mass star-forming systems are extremely rare in the inner regions of the Virgo cluster A, where the density of the intergalactic medium is at its maximum. Our ram pressure stripping models consistently indicate that these star-forming systems can be rapidly deprived of their interstellar medium during their interaction with the intergalactic medium. The lack of gas quenches their star-formation activity transforming them into quiescent dwarf ellipticals. This mild transformation does not perturb the kinematic properties of these galaxies, which still have rotation curves typical of star-forming systems. [ABSTRACT FROM AUTHOR]

Published
2014
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11. Ultraviolet to infrared emission of z > 1 galaxies: Can we derive reliable star formation rates and stellar masses?

Author

Buat, V., Heinis, S., Boquien, M., Burgarella, D., Charmandaris, V., Boissier, S., Boselli, A., Le Borgne, D., and Morrison, G.

Subjects
STAR formation, STELLAR mass, REDSHIFT, GALAXY formation, MASS measurement
Abstract

Aims. Our knowledge of the cosmic mass assembly relies on measurements of star formation rates (SFRs) and stellar masses (Mstar), of galaxies as a function of redshift. These parameters must be estimated in a consistent way with a good knowledge of systematics before studying their correlation and the variation of the specific SFR. Constraining these fundamental properties of galaxies across the Universe is of utmost importance if we want to understand galaxy formation and evolution. Methods. We seek to derive SFRs and stellar masses in distant galaxies and to quantify the main uncertainties affecting their measurement. We explore the impact of the assumptions made in their derivation with standard calibrations or through a fitting process, as well as the impact of the available data, focusing on the role of infrared emission originating from dust. Results. We build a sample of galaxies with z > 1, all observed from the ultraviolet to the infrared in their rest frame. The data are fitted with the code CIGALE, which is also used to build and analyse a catalogue of mock galaxies. Models with different star formation histories are introduced: an exponentially decreasing or increasing SFR and a more complex one coupling a decreasing SFR with a younger burst of constant star formation. We define different sets of data, with or without a good sampling of the ultraviolet range, near-infrared, and thermal infrared data. Variations of the metallicity are also investigated. The impact of these different cases on the determination of stellar mass and SFR are analysed. Conclusions. Exponentially decreasing models with a redshift formation of the stellar population zf ≃ 8 cannot fit the data correctly. All the other models fit the data correctly at the price of unrealistically young ages when the age of the single stellar population is taken to be a free parameter, especially for the exponentially decreasing models. The best fits are obtained with two stellar populations. As long as one measurement of the dust emission continuum is available, SFR are robustly estimated whatever the chosen model is, including standard recipes. The stellar mass measurement is more subject to uncertainty, depending on the chosen model and the presence of near-infrared data, with an impact on the SFR-Mstar scatter plot. Conversely, when thermal infrared data from dust emission are missing, the uncertainty on SFR measurements largely exceeds that of stellar mass. Among all physical properties investigated here, the stellar ages are found to be the most diffcult to constrain and this uncertainty acts as a second parameter in SFR measurements and as the most important parameter for stellar mass measurements. [ABSTRACT FROM AUTHOR]

Published
2014
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12. A method for quantifying the gamma-ray burst bias Application in the redshift range of 0-1.1.

Author

Boissier, S., Salvaterra, R., Le Floc'h, E., Basa, S., Buat, V., Prantzos, N., Vergani, S. D., and Savaglio, S.

Subjects
*GAMMA ray bursts, *STAR formation, *ASTRONOMICAL observations, *REDSHIFT, *STELLAR mass
Abstract

Context. Long gamma-ray bursts (LGRBs) are related to the final stages of evolution of very massive stars. As such, they should follow the star formation rate (SFR) of galaxies. We can use them to probe for star-forming galaxies in the distant universe following this assumption. The relation between the rate of LGRBs in a given galaxy and its SFR (which we call the LGRB bias) may however be complex, as we have good indications that the LGRB hosts are not perfect analogues to the general population of star-forming galaxies. Aims. In this work, we try to quantify how the LGRB bias depends on physical parameters of their host galaxy, such as SFR or stellar mass. These trends may reveal more fundamental properties such as the role of the metallicity of LGRBs and of their progenitors . Methods. We propose an empirical method based on the comparison of stellar mass functions (and SFR distributions) of LGRB hosts and of star-forming galaxies to find how the bias depends on the stellar mass or the SFR. Results. By applying this method to a sample of LGRB hosts at redshifts lower than 1.1, where the properties of star-forming galaxies are fairly well established and where the properties of LGRB host galaxies can be deduced from observations (limiting ourselves to stellar masses higher than 109.25 M☉ and SFR higher than ~1.8 M☉ yr-1), we find that the LGRB bias depends on both the stellar mass and SFR. We find that the bias decreases with the SFR; that is, we see no preference for highly star-forming galaxies, once we account for the higher number of massive stars in galaxies with larger SFR. We do not find any trend with the specific star formation rate (SSFR), but the dynamical range in SSFR in our study is narrow. Through an indirect method, we relate these trends to a possible decrease in the LGRBs rate / SFR ratio with the metallicity. Conclusions. The method we propose suggests trends that may be useful to constrain models of LGRB progenitors, showing a clear decrease in the LGRB bias with the metallicity. This is promising for the future as the number of LGRB hosts studied will increase. [ABSTRACT FROM AUTHOR]

Published
2013
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13. Mass assembly in quiescent and star-forming galaxies since z ≃ 4 from UltraVISTA.

Author

Ilbert, O., McCracken, H. J., Le Fèvre, O., Capak, P., Dunlop, J., Karim, A., Renzini, M. A., Caputi, K., Boissier, S., Arnouts, S., Aussel, H., Comparat, J., Guo, Q., Hudelot, P., Kartaltepe, J., Kneib, J. P., Krogager, J. K., Le Floc'h, E., Lilly, S., and Mellier, Y.

Subjects
STAR formation, GALAXIES, STELLAR mass, MASS density gradients, REDSHIFT
Abstract

We estimate the galaxy stellar mass function and stellar mass density for star-forming and quiescent galaxies with 0.2 < z < 4. We construct a large, deep (Ks < 24) sample of 220 000 galaxies selected using the new UltraVISTA DR1 data release. Our analysis is based on precise 30-band photometric redshifts. By comparing these photometric redshifts with 10,800 spectroscopic redshifts from the zCOSMOS bright and faint surveys, we find a precision of σΔz/(1+z) = 0.008 at i+ < 22.5 and σΔ/(1+z) = 0.03 at 1.5 < z < 4. We derive the stellar mass function and correct for the Eddington bias. We find a mass-dependent evolution of the global and starforming populations, with the low-mass end of the mass functions evolving more rapidly than the high-mass end. This mass-dependent evolution is a direct consequence of the star formation being "quenched" in galaxies more massive than M ≳ 1010.7-10.9M⊚. For the mass function of the quiescent galaxies, we do not find any significant evolution of the high-mass end at z < 1; however we observe a clear flattening of the faint-end slope. From z ∼ 3 to z ∼ 1, the density of quiescent galaxies increases over the entire mass range. Their comoving stellar mass density increases by 1.6 dex between z ∼ 3 and z ∼ 1 and by less than 0.2 dex at z < 1. We infer the star formation history from the mass density evolution. This inferred star formation history is in excellent agreement with instantaneous star formation rate measurements at z < 1.5, while we find differences of 0.2 dex at z > 1.5 consistent with the expected uncertainties. We also develop a new method to infer the specific star formation rate from the mass function of star-forming galaxies. We find that the specific star formation rate of 1010-10.5M∼ galaxies increases continuously in the redshift range 1 < z < 4. Finally, we compare our results with a semi-analytical model and find that these models overestimate the density of low mass quiescent galaxies by an order of magnitude, while the density of low-mass star-forming galaxies is successfully reproduced. [ABSTRACT FROM AUTHOR]

Published
2013
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14. The GALEX view of the Herschel Reference Survey.

Author

Cortese, L., Boissier, S., Boselli, A., Bendo, G. J., Buat, V., Davies, J. I., Eales, S., Heinis, S., Isaak, K. G., and Madden, S. C.

Subjects
*FAR ultraviolet radiation, *STAR formation, *GALAXIES, *ELECTROMAGNETIC measurements, *RADIAL bone
Abstract

We present GALEX far-ultraviolet (FUV) and near-ultraviolet (NUV) as well as SDSS g, r, i photometry and structural parameters for the Herschel Reference Survey, a magnitude-, volume-limited sample of nearby galaxies in different environments. We use this unique dataset to investigate the ultraviolet (UV) structural scaling relations of nearby galaxies and to determine how the properties of the UV disk vary with atomic hydrogen content and environment. We find a clear change of slope in the stellar mass vs. effective surface brightness relation when moving from the optical to the UV, with more massive galaxies having brighter optical but fainter UV surface brightnesses than smaller systems. A similar change of slope is also seen in the radius vs. surface brightness relation. By comparing our observations with the predictions of a simple multi-zone chemical model of galaxy evolution, we show that these findings are a natural consequence of a much more efficient inside-out growth of the stellar disk in massive galaxies. We confirm that isophotal radii are always a better proxy for the size of the stellar/star-forming disk than effective quantities and we show that the extent of the UV disk (normalized to the optical size) is strongly correlated to the integrated Hi gas fraction. This relation still holds even when cluster spirals are considered, with Hi-deficient systems having less extended star-forming disks than Hi-normal galaxies. Interestingly, the star formation in the inner part of Hi-deficient galaxies is significantly less affected by the removal of the atomic hydrogen, as expected in a simple ram-pressure stripping scenario. These results suggest that it is the amount of Hi that regulates the growth of the star-forming disk in the outskirts of galaxies. [ABSTRACT FROM AUTHOR]

Published
2012
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15. Stripped gas as fuel for newly formed H II regions in the encounter between VCC 1249 and M 49: a unified picture from NGVS and GUViCS.

Author

Battaia, F. Arrigoni, Gavazzi, G., Fumagalli, M., Boselli, A., Boissier, S., Cortese, L., Heinis, S., Ferrarese, L., Côté, P., Mihos, J. C., Cuillandre, J. C., Duc, P.-A., Durrell, P., Gwyn, S., Jordán, A., Liu, C., Peng, E., and Mei, S.

Subjects
GAS as fuel, INTERSTELLAR gases, ASTRONOMICAL observations, VIRGO Cluster, MILKY Way
Abstract

Context. We study the peculiar interacting galaxy system of VCC 1249/M 49 located in the core of the Virgo B subcluster. Owing to a recent interaction between the dwarf galaxy VCC 1249 and the halo gas of the elliptical galaxy M 49, neutral hydrogen has been displaced from the interstellar medium of this dwarf into the Virgo intracluster medium. Observations also reveal multiple compact star-forming regions (aka H ii regions) that are embedded in this H i cloud, with a projected separation up to 13 kpc from VCC 1249 in the northwest direction. Aims. Motivated by recent near-ultraviolet imaging from the GALEX Ultraviolet Virgo Cluster Survey (GUViCS) of the VCC 1249/M 49 system that shows significant ongoing/recent star formation in the compact regions, we aim to constrain the origin of these outlying H II regions with a multi-wavelength approach. Methods. Using deep optical (u,g,i,z) imaging from the Next Generation Virgo Cluster Survey (NGVS) and new Hα imaging obtained at the San Pedro Martir observatory together with Keck long-slit spectroscopy, we characterize the star formation rates, ages, and metallicity of VCC 1249 and its outlying compact regions. Moreover, we analyze the color and luminosity profile of the galaxy to investigate its recent interaction with M 49. Results. Our new observations indicate that VCC 1249 underwent a recent interaction with M 49 in which both ram-pressure stripping and tidal interaction occured. The joint action of the two mechanisms led to the removal of the H I gas from the interstellar medium of VCC 1249, while the gravitational tides triggered the stellar tail and counter-tail of VCC 1249. Our stellar population synthesis analysis reveals that the star formation in this galaxy was truncated around 200 Myr ago and that the outlying H II regions were born in situ ≈10 Myr ago out of pre-enriched gas removed from the dwarf galaxy. These observations also reveal that interactions between central and satellite galaxies similar to those between VCC 1249/M 49 may be an effective way of dispersing metals into the halos of massive galaxies. [ABSTRACT FROM AUTHOR]

Published
2012
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16. Stripped gas as fuel for newly formed Hii regions in the encounter between VCC1249 and M49: a unified picture from NGVS and GUViCS.

Author

Arrigoni Battaia, F., Gavazzi, G., Fumagalli, M., Boselli, A., Boissier, S., Cortese, L., Heinis, S., Ferrarese, L., Côté, P., Mihos, J. C., Cuillandre, J. C., Duc, P.-A., Durrell, P., Gwyn, S., Jordán, A., C. Liu, E. Peng, and Mei, S.

Subjects
STAR clusters, DWARF galaxies, HYDROGEN, ULTRAVIOLET radiation, WAVELENGTHS
Abstract

Context. We study the peculiar interacting galaxy system of VCC 1249/M 49 located in the core of the Virgo B subcluster. Owing to a recent interaction between the dwarf galaxy VCC 1249 and the halo gas of the elliptical galaxy M 49, neutral hydrogen has been displaced from the interstellar medium of this dwarf into the Virgo intracluster medium. Observations also reveal multiple compact star-forming regions (aka HII regions) that are embedded in this HI cloud, with a projected separation up to 13 kpc from VCC 1249 in the northwest direction. Aims. Motivated by recent near-ultraviolet imaging from the GALEX Ultraviolet Virgo Cluster Survey (GUViCS) of the VCC 1249/M 49 system that shows significant ongoing/recent star formation in the compact regions, we aim to constrain the origin of these outlying Hii regions with a multi-wavelength approach. Methods. Using deep optical (u, g, i, z) imaging from the Next Generation Virgo Cluster Survey (NGVS) and new Hα imaging obtained at the San Pedro Martir observatory together with Keck long-slit spectroscopy, we characterize the star formation rates, ages, and metallicity of VCC 1249 and its outlying compact regions. Moreover, we analyze the color and luminosity profile of the galaxy to investigate its recent interaction with M 49. Results. Our new observations indicate that VCC 1249 underwent a recent interaction withM49 in which both ram-pressure stripping and tidal interaction occured. The joint action of the two mechanisms led to the removal of the HI gas from the interstellar medium of VCC 1249, while the gravitational tides triggered the stellar tail and counter-tail of VCC 1249. Our stellar population synthesis analysis reveals that the star formation in this galaxy was truncated around 200 Myr ago and that the outlying Hii regions were born in situ ≈10 Myr ago out of pre-enriched gas removed from the dwarf galaxy. These observations also reveal that interactions between central and satellite galaxies similar to those between VCC 1249/M 49 may be an effective way of dispersing metals into the halos of massive galaxies. [ABSTRACT FROM AUTHOR]

Published
2012
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17. Ultraviolet dust attenuation in star-forming galaxies – II. Calibrating the A(UV) versus L TIR/ L UV relation.

Author

Cortese, L., Boselli, A., Franzetti, P., Decarli, R., Gavazzi, G., Boissier, S., and Buat, V.

Subjects
DUST, STELLAR populations, SPECTRAL energy distribution, GALAXIES, STAR formation, ULTRAVIOLET astronomy
Abstract

We investigate the dependence of the total-IR (TIR) to ultraviolet (UV) luminosity ratio method for calculating the UV dust attenuation from the age of the underlying stellar populations by using a library of spectral energy distributions for galaxies with different star formation histories. Our analysis confirms that the TIR/UV versus relation varies significantly with the age of the underlying stellar population: that is, for the same TIR/UV ratio, systems with low specific star formation rate (SSFR) suffer a lower UV attenuation than starbursts. Using a sample of nearby field and cluster spiral galaxies, we show that the use of a standard (i.e. age-independent) TIR/UV versus relation leads to a systematic overestimate up to 2 mag of the amount of UV dust attenuation suffered by objects with low SSFR and in particular H i-deficient star-forming cluster galaxies. This result points out that the age-independent TIR/UV versus relation cannot be used to study the UV properties of large samples of galaxies including low star-forming systems and passive spirals. Therefore, we give some simple empirical relations from which the UV attenuation can be estimated taking into account its dependence on the age of the stellar populations, providing a less biased view of UV properties of galaxies. [ABSTRACT FROM AUTHOR]

Published
2008
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18. Chemical and spectrophotometric evolution of low surface brightness galaxies.

Author

Boissier, S., Monnier Ragaigne, D., Prantzos, N., van Driel, W., Balkowski, C., and O'Neil, K.

Subjects
*SURFACE brightness (Astronomy), *GALAXIES, *SPECTROPHOTOMETRY
Abstract

ABSTRACT Based on the results of recent surveys, we have constructed a relatively homogeneous set of observational data concerning the chemical and photometric properties of low surface brightness galaxies (LSBs). We have compared the properties of this data set with the predictions of models of the chemical and spectrophotometric evolution of LSBs. The basic idea behind the models, i.e. that LSBs are similar to ‘classical’ high surface brightness spirals except for a larger angular momentum, is found to be consistent with the results of their comparison with these data. However, some observed properties of the LSBs (e.g. their colours, and specifically the existence of red LSBs), as well as the large scatter in these properties, cannot be reproduced by the simplest models with smoothly evolving star formation rates over time. We argue that the addition of bursts and/or truncations in the star formation rate histories can alleviate this discrepancy. [ABSTRACT FROM AUTHOR]

Published
2003
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19. Chemo-spectrophotometric evolution of spiral galaxies – V. Properties of galactic discs at high redshift.

Author

Boissier, S. and Prantzos, N.

Subjects
*SPIRAL galaxies, *DARK matter, *GALACTIC evolution, *SPECTROPHOTOMETRY, *REDSHIFT
Abstract

We explore the implications for the high-redshift universe of ‘state-of-the-art’ models for the chemical and spectrophotometric evolution of spiral galaxies. The models are based on simple ‘scaling relations’ for discs, obtained in the framework of cold dark matter models for galaxy formation, and were ‘calibrated’ so as to reproduce the properties of the Milky Way and of nearby discs (at redshift z∼0). In this paper, we compare the predictions of our ‘hybrid’ approach to galaxy evolution to observations at moderate and high redshift. We find that the models are in fairly good agreement with observations up to z∼1, while some problems appear at higher redshift (provided there is no selection bias in the data); these discrepancies may suggest that galaxy mergers (not considered in this work) played a non-negligible role at z>1. We also predict the existence of a ‘universal’ correlation between abundance gradients and disc scalelengths, independent of redshift. [ABSTRACT FROM AUTHOR]

Published
2001
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20. Mass assembly in quiescent and star-forming galaxies since z ≃ 4 from UltraVISTA DR1 in the COSMOS field

Author

Ilbert, O., McCracken, H. J., Le Fèvre, O., Capak, P., Dunlop, J., Karim, A., Renzini, M. A., Caputi, K., Boissier, S., Cambresy, L., Martins, F., Nuss, E, Palacios, A., Astronomy, and Kapteyn Astronomical Institute

Subjects
Galaxies: distances and redshifts, Galaxies: star formation, Astrophysics::Solar and Stellar Astrophysics, Galaxies: evolution, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: formation, Galaxies: stellar content, Astrophysics::Galaxy Astrophysics
Abstract

We estimate the galaxy stellar mass function and stellar mass density for star-forming and quiescent galaxies out to z=4. We construct a sample of 220000 galaxies selected at K_{s}1.5 consistent with the expected uncertainties. Finally, we present a new method to infer the specific star formation rate from the mass function of star-forming galaxies and we find a continous increase of the sSFR with redshift out to z˜ 4. The photometric catalogues and associated photometric redshifts are available at http://terapix.iap.fr/article.php?id_article=844.

21. A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Author

A. Boselli, M. Fossati, A. Longobardi, K. Kianfar, N. Z. Dametto, P. Amram, J. P. Anderson, P. Andreani, S. Boissier, M. Boquien, V. Buat, G. Consolandi, L. Cortese, P. Côté, J. C. Cuillandre, L. Ferrarese, L. Galbany, G. Gavazzi, S. Gwyn, G. Hensler, J. Hutchings, E. W. Peng, J. Postma, J. Roediger, Y. Roehlly, P. Serra, G. Trinchieri, Boselli, A, Fossati, M, Longobardi, A, Kianfar, K, Dametto, N, Amram, P, Anderson, J, Andreani, P, Boissier, S, Boquien, M, Buat, V, Consolandi, G, Cortese, L, Cote, P, Cuillandre, J, Ferrarese, L, Galbany, L, Gavazzi, G, Gwyn, S, Hensler, G, Hutchings, J, Peng, E, Postma, J, Roediger, J, Roehlly, Y, Serra, P, Trinchieri, G, 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), Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB), Dipartimento di Fisica e Astronomia 'Galileo Galilei', Università degli Studi di Padova = University of Padua (Unipd), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), National Research Council of Canada (NRC), University of Vienna [Vienna], Forschungszentrum Jülich GmbH | Centre de recherche de Juliers, Helmholtz-Gemeinschaft = Helmholtz Association, NRC Herzberg Astronomy and Astrophysics, Conseil National de Recherches Canada (CNRC), INAF - Osservatorio Astronomico di Cagliari (OAC), Istituto Nazionale di Astrofisica (INAF), and INAF - Osservatorio Astronomico di Brera (OAB)

Subjects
Physics, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies: elliptical and lenticular CD, FOS: Physical sciences, Galaxies: evolution, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Tracing, Galaxies: clusters: individual: Virgo, Astrophysics - Astrophysics of Galaxies, Galaxies: elliptical and lenticular, cD, Galaxies: ISM, Space and Planetary Science, Galaxies: interaction, Astrophysics of Galaxies (astro-ph.GA), galaxies: interactions, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Galaxies: clusters: general, Lenticular galaxy, Astrophysics::Galaxy Astrophysics
Abstract

As part of the VESTIGE survey, a blind narrow-band Ha+[NII] imaging survey of the Virgo cluster carried out with MegaCam at the CFHT, we discovered 8 massive lenticular galaxies with prominent ionised gas emission features in their inner (few kpc) regions. These features are either ionised gas filaments similar to those observed in cooling flows (2 gal), or thin discs with sizes 0.7, Comment: Accepted for publication on A&A

Published
2022
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22. A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Author

null Junais, S. Boissier, A. Boselli, L. Ferrarese, P. Côté, S. Gwyn, J. Roediger, S. Lim, E. W. Peng, J.-C. Cuillandre, A. Longobardi, M. Fossati, G. Hensler, J. Koda, J. Bautista, M. Boquien, K. Małek, P. Amram, Y. Roehlly, Junais, Boissier, S, Boselli, A, Ferrarese, L, Cote, P, Gwyn, S, Roediger, J, Lim, S, Peng, E, Cuillandre, J, Longobardi, A, Fossati, M, Hensler, G, Koda, J, Bautista, J, Boquien, M, Maaek, K, Amram, P, Roehlly, Y, 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: star formation, [SDU]Sciences of the Universe [physics], Galaxies: interaction, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Galaxies: evolution, Astronomy and Astrophysics, Galaxies: clusters: general, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxies: clusters: individual: Virgo, Astrophysics - Astrophysics of Galaxies
Abstract

Low-surface-brightness galaxies (LSBs) contribute to a significant fraction of all the galaxies in the Universe. Ultra-diffuse galaxies (UDGs) form a subclass of LSBs that has attracted a lot of attention in recent years (although its definition may vary between studies). Although UDGs are found in large numbers in galaxy clusters, groups, and in the field, their formation and evolution are still very much debated. Using a comprehensive set of multiwavelength data from the NGVS (optical), VESTIGE (H$\alpha$ narrowband), and GUViCS (UV) surveys, we studied a sample of 64 diffuse galaxies and UDGs in the Virgo cluster to investigate their formation history. We analyzed the photometric colors and surface-brightness profiles of these galaxies and then compared them to models of galaxy evolution, including ram-pressure stripping (RPS) events to infer any possible strong interactions with the hot cluster gas in the past. While our sample consists mainly of red LSBs, which is typical in cluster environments, we found evidence of a color variation with the cluster-centric distance. Blue, HI-bearing, star-forming diffuse galaxies are found at larger distances from the cluster center than the rest of the sample. The comparison of our models with multifrequency observations suggests that most of the galaxies of the sample might have undergone a strong RPS event in their lifetime, on average 1.6 Gyr ago (with a large dispersion, and RPS still ongoing for some of them). This process resulted in the transformation of initially gas-rich diffuse blue galaxies into gas-poor and red ones that form the dominant population now, the more extreme UDGs having undergone the process in a more distant past on average. The RPS in dense environments could be one of the major mechanisms for the formation of the large number of quiescent UDGs we observe in galaxy clusters., Comment: 57 pages, 14 Figures, accepted for publication in A&A

Published
2022
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23. A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE): VIII. Modeling ram pressure stripping of diffuse gas in the Virgo cluster spiral galaxy NGC 4330

Author

Stephen Gwyn, Médéric Boquien, Marian Soida, P. Amram, Jean-Charles Cuillandre, Gerhard Hensler, Alessandro Boselli, Samuel Boissier, Bernd Vollmer, Matteo Fossati, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), 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), National Research Council of Canada (NRC), Observatoire de Paris, Université Paris sciences et lettres (PSL), 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), University of Vienna [Vienna], Vollmer, B, Fossati, M, Boselli, A, Soida, M, Gwyn, S, Cuillandre, J, Amram, P, Boissier, S, Boquien, M, Hensler, G, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)

Subjects
Stellar population, galaxies: individual: NGC 4330, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, individual: NGC 4330 [galaxies], Galaxies: kinematics and dynamic, Intracluster medium, kinematics and dynamics [galaxies], 0103 physical sciences, galaxies: interactions, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, galaxies: kinematics and dynamics, Physics, Spiral galaxy, ISM [galaxies], interactions [galaxies], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Virgo Cluster, Astrophysics - Astrophysics of Galaxies, Galaxy, Ram pressure, Interstellar medium, 13. Climate action, Space and Planetary Science, Galaxies: interaction, Astrophysics of Galaxies (astro-ph.GA), galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM
Abstract

NGC 4330 is one of the Virgo galaxies whose UV distribution shows a tail structure. An associated tail structure is also observed in the HI and H$\alpha$ emission distributions. Previous dynamical modeling showed that the galaxy is approaching the cluster center and is therefore undergoing increasing ram pressure stripping. Recent stellar population fitting of deep optical spectra together with multiband photometry lead to the determination of the time when star formation was quenched in the galactic disk. We introduce a new version of the dynamical model that includes the diffuse ionized gas and aim to reproduce the HI, H$\alpha$, UV distributions together with the star formation histories of the outer gas-free parts of the galactic disk. The results of 50 simulations with five different Lorentzian temporal ram-pressure profiles and five different delays between the simulation onset and peak ram pressure are presented. The inclusion of diffuse gas stripping changes significantly the HI, UV, and H$\alpha$ emission distributions. The simulations with diffuse gas stripping naturally lead to vertical low surface density filaments in the downwind region of the galactic disk. These filaments occur less frequently in the simulations without diffuse gas stripping. The simulations with diffuse gas stripping lead to better joint fits to the SEDs and optical spectra. The HI, NUV, and H$\alpha$ morphologies of the model snapshots which best reproduce the SEDs and optical spectra are sufficiently different to permit a selection of best-fit models. We conclude that the inclusion of diffuse gas stripping significantly improves the resemblance between the model and observations. Our preferred model yields a time to peak ram pressure of 140 Myr in the future. The spatial coincidence of the radio continuum and diffuse H$\alpha$ tails suggests that both gas phases are stripped together., Comment: accepted for publication in A&A

Published
2021
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24. A Virgo Environmental Survey Tracing Ionised Gas Emission. VESTIGE VIII. Bridging the cluster-ICM-galaxy evolution at small scales

Author

Liu, Chengze, Côté, Patrick, Peng, Eric W., Roediger, Joel, Zhang, Hongxin, Ferrarese, Laura, Sánchez-Janssen, Rubén, Guhathakurta, Puragra, Yang, Xiaohu, Jing, Yipeng, Alamo-Martinez, Karla, Blakeslee, John P., Boselli, Alessandro, Cuilandre, Jean-Charles, Duc, Pierre-Alain, Durrell, Patrick, Gwyn, Stephen, Jordán, Andres, Ko, Youkyung, Lançon, Ariane, Lim, Sungsoon, Longobardi, Alessia, Mei, Simona, Mihos, J. Christopher, Munoz, Roberto, Powalka, Mathieu, Puzia, Thomas, Spengler, Chelsea, Toloba, Elisa, Boselli, Alessandro, Max-Planck-Institut für Extraterrestrische Physik (MPE), 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), Chaire Galaxies et cosmologie, Collège de France (CdF (institution)), University of Vienna [Vienna], NRC Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), FORMATION STELLAIRE 2019, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-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), Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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), Collège de France - Chaire 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), École normale supérieure - Paris (ENS-PSL), 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), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Longobardi, A, Boselli, A, Fossati, M, Villa-Velez, J, Bianchi, S, Casasola, V, Sarpa, E, Combes, F, Hensler, G, Burgarella, D, Schimd, C, Nanni, A, Cote, P, Buat, V, Amram, P, Ferrarese, L, Braine, J, Trinchieri, G, Boissier, S, Boquien, M, Andreani, P, Gwyn, S, and Cuillandre, J

Subjects
galaxies: clusters: intracluster medium, Metallicity, Astrophysics::High Energy Astrophysical Phenomena, Isophote, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Spatial distribution, 01 natural sciences, galaxies: clusters: individual: Virgo cluster, [SDU] Sciences of the Universe [physics], 0103 physical sciences, Galaxy formation and evolution, galaxies: interactions, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, Mass ratio, Astrophysics - Astrophysics of Galaxies, Galaxy, Ram pressure, Interstellar medium, Galaxies: interaction, Space and Planetary Science, [SDU]Sciences of the Universe [physics], galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM
Abstract

We measure FIR emission from tails of stripped dust following the ionised and atomic gas components in galaxies undergoing ram pressure stripping. We study the dust-to-gas relative distribution and mass ratio in the stripped interstellar medium and relate them to those of the intra-cluster medium, thus linking the cluster-ICM-galaxy evolution at small-scales. The galaxy sample consists of three Scd Virgo galaxies with stellar masses in the range $10^9\lesssim \mathrm{M_{*}} \lesssim 10^{10}\, \mathrm{M_{\odot}}$, and within 1 Mpc from the cluster centre, namely NGC 4330, NGC 4522, and NGC 4654. Through the analysis of VESTIGE H$\alpha$, $Herschel$ SPIRE far-infrared, and VIVA HI data, we trace the spatial distribution of the tails and infer the dust and gas masses from the measured far-infrared 250 $\mu$m and HI flux densities. Dust-to-gas mass ratios (DGRs) in the tails are analysed as a function of the galaxy mass, metallicity, and dust temperature. Along the stripped component, the dust distribution closely follows the HI and H$\alpha$ emitting gas, all extending beyond the optical disc. In these regions, the DGRs are $2.0\pm0.6\times10^{-3}$, $0.7\pm0.1\times10^{-3}$, and $0.4\pm0.03\times10^{-3}$, for NGC 4330, NGC 4522, and NGC 4654, respectively, i.e. up to a factor of 15 less than the values measured in the main body of nearby galaxies. We also find a negative trend in the DGR as a function of the metallicity that can be explained in terms of a dust component more centrally concentrated in more metal-rich systems. Together with the finding that the stripped dust is cold, $T_{d} \lesssim 25\, K$, our results support an outside-in stripping scenario of the galaxy interstellar medium. This study shows that ram pressure stripping is a key mechanism in the building up of the Virgo intra-cluster component injecting dust grains into the ICM, thus contributing to its metal enrichment., Comment: 15 pages, 7 images, 4 tables. Accepted on A\&A

Published
2020
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25. A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE).IV. A tail of Ionised Gas in the Merger Remnant NGC 4424

Author

P. Cote, Laura Ferrarese, Hanindyo Kuncarayakti, P. Amram, Jean-Charles Cuillandre, V. Buat, Gerhard Hensler, Benoît Epinat, Médéric Boquien, J. Roediger, Elisa Toloba, G. Consolandi, Patrick R. Durrell, Rubén Sánchez-Janssen, Matteo Fossati, Luca Cortese, Ginevra Trinchieri, Lluís Galbany, Sebastián F. Sánchez, Samuel Boissier, Joseph P. Anderson, M. Marcelin, J. A. Gómez-López, S. D. J. Gwyn, Denis Burgarella, Michele Fumagalli, Chong Ge, B. Vollmer, Y. Roehlly, Giuseppe Gavazzi, Alessandro Boselli, C. Mendes de Oliveira, Ming Sun, Bruno Quint, 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), Università degli Studi di Milano-Bicocca [Milano] (UNIMIB), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Ingénierie des Matériaux Polymères (IMP), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet [Saint-Étienne] (UJM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Uppsala University, European Synchrotron Radiation Facility (ESRF), Centre de Recherche en Paléontologie - Paris (CR2P), Muséum national d'Histoire naturelle (MNHN)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Service d'Oncologie Médicale [CHRU Besançon], Centre Hospitalier Régional Universitaire de Besançon (CHRU Besançon)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB), Youngstown State University (YSU), NRC Herzberg Astronomy and Astrophysics, Conseil National de Recherches Canada (CNRC), University of Vienna [Vienna], UCO/Lick Observatory, University of California [Santa Cruz] (UC Santa Cruz), University of California (UC)-University of California (UC), CDS, Centre de Données astronomiques de Strasbourg, Observatoire astronomique de Strasbourg, France + ESO, European Southern Observatory, Garching bei Muenchen, Allemagne, Université de Strasbourg (UNISTRA)-Université Louis Pasteur - Strasbourg I, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet - Saint-Étienne (UJM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), University of California [Santa Cruz] (UCSC), University of California-University of California, Boselli, A, Fossati, M, Consolandi, G, Amram, P, Ge, C, Sun, M, Anderson, J, Boissier, S, Boquien, M, Buat, V, Burgarella, D, Cortese, L, Cote, P, Cuillandre, J, Durrell, P, Epinat, B, Ferrarese, L, Fumagalli, M, Galbany, L, Gavazzi, G, Gomez-Lopez, J, Gwyn, S, Hensler, G, Kuncarayakti, H, Marcelin, M, Mendes De Oliveira, C, Quint, B, Roediger, J, Roehlly, Y, Sanchez, S, Sanchez-Janssen, R, Toloba, E, Trinchieri, G, Vollmer, B, ITA, USA, GBR, FRA, DEU, AUS, CAN, and CHL

Subjects
Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Peculiar galaxy, Intracluster medium, 0103 physical sciences, Galaxy formation and evolution, galaxies: interactions, Astrophysics::Solar and Stellar Astrophysics, Surface brightness, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, GALÁXIAS, Virgo Cluster, Astrophysics - Astrophysics of Galaxies, Galaxy, Ram pressure, Galaxies: interaction, 13. Climate action, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), galaxies: clusters: individual: Virgo, galaxies: individual: NGC 4424, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM
Abstract

We have observed the late-type peculiar galaxy NGC 4424 during VESTIGE, a blind narrow-band Halpha[NII] imaging survey of the Virgo cluster carried out with MegaCam at the CFHT. The presence of a 110 kpc long HI tail in the S direction indicates that this galaxy is undergoing a ram pressure stripping event. The deep narrow-band image revealed the presence of a low surface brightness ionised gas tail ~10 kpc long extending from the centre of the galaxy to the NW direction, in the direction opposite to the HI tail. Chandra and XMM X-rays data do not show any compact source in the nucleus nor the presence of an extended tail of hot gas, while MUSE spectroscopy indicates that the gas is photo-ionised in the inner regions and shock-ionised in the outer parts. IFU spectroscopy confirms that the ionised gas is kinematically decoupled from the stellar component and indicates the presence of two kinematically distinct structures in the stellar disc. The analysis of the SED of the galaxy indicates that the activity of star formation has been totally quenched in the outer disc ~ 250-280 Myr ago, while only reduced by ~80% in the central regions. All this observational evidence suggests that NGC 4424 is the remnant of an unequal-mass merger occurred, Accepted for publication on Astronomy & Astrophysics

Published
2018
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26. A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE). II. Constraining the quenching time in the stripped galaxy NGC 4330

Author

Jean-Charles Cuillandre, Patrick R. Durrell, P. Côté, E. Toloba, Ming Sun, A. Longobardi, Gerhard Hensler, Joel Roediger, Matteo Fossati, J. A. Gómez-López, G. Consolandi, Stephen Gwyn, Médéric Boquien, Eric W. Peng, P. Amram, V. Buat, Luca Cortese, Baerbel Koribalski, J. T. Mendel, Michele Fumagalli, Alessandro Boselli, Denis Burgarella, Giuseppe Gavazzi, Laura Ferrarese, Stephanie Cote, Bernd Vollmer, Samuel Boissier, Max-Planck-Institut für Extraterrestrische Physik (MPE), 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), Università degli Studi di Milano-Bicocca [Milano] (UNIMIB), NRC Herzberg Astronomy and Astrophysics, Conseil National de Recherches Canada (CNRC), NRC Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Youngstown State University (YSU), University of Vienna [Vienna], Australia Telescope National Facility, Australian National University (ANU), UCO/Lick Observatory, University of California [Santa Cruz] (UCSC), University of California-University of California, 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), Universitá degli Studi di Milano-Bicocca, Universitá degli Studi di Milan-Bocca, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), University of California [Santa Cruz] (UC Santa Cruz), University of California (UC)-University of California (UC), Fossati, M, Mendel, J, Boselli, A, Cuillandre, J, Vollmer, B, Boissier, S, Consolandi, G, Ferrarese, L, Gwyn, S, Amram, P, Boquien, M, Buat, V, Burgarella, D, Cortese, L, Cote, P, Cote, S, Durrell, P, Fumagalli, M, Gavazzi, G, Gomez-Lopez, J, Hensler, G, Koribalski, B, Longobardi, A, Peng, E, Roediger, J, Sun, M, and Toloba, E

Subjects
Active galactic nucleus, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Surface brightness, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Very Large Telescope, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Galaxies: evolution, Astronomy and Astrophysics, Galaxies: clusters: individual: Virgo, Astrophysics - Astrophysics of Galaxies, Virgo Cluster, Galaxy, Ram pressure, Galaxies: interactions, Galaxies: ISM, Photometry (astronomy), Galaxies: interaction, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Galaxies: clusters: general, Astrophysics::Earth and Planetary Astrophysics, Galaxies: ISM Visiting Astronomer at NRC Herzberg Astronomy and Astro- physics
Abstract

The Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE) is a blind narrow-band H$\alpha$+[NII] imaging survey carried out with MegaCam at the CFHT. During pilot observations we have observed NGC 4330, an intermediate mass, edge-on star forming spiral currently falling into the core of the Virgo cluster. New deep observations revealed a low surface brightness 10 kpc tail exhibiting a peculiar filamentary structure. The filaments are remarkably parallel one another and clearly indicate the direction of motion of the galaxy in the Virgo potential. Motivated by the detection of these features, indicating ongoing gas stripping, we collected literature photometry in 15 bands from the far-UV to the far-IR and deep optical long slit spectroscopy using the FORS2 instrument at the ESO Very Large Telescope. Using a newly developed Monte Carlo code that jointly fits spectroscopy and photometry, we reconstructed the star formation histories in apertures along the major axis of the galaxy. Our results have been validated against the output of CIGALE, a fitting code which has been previously used for similar studies. We found a clear outside-in gradient with radius of the time when the quenching event started: the outermost radii have been stripped 500 Myr ago, while the stripping has reached the inner 5 kpc from the center in the last 100 Myr. Regions at even smaller radii are currently still forming stars fueled by the presence of HI and H2 gas. When compared to statistical studies of the quenching timescales in the local Universe we find that ram pressure stripping of the cold gas is an effective mechanism to reduce the transformation times for galaxies falling into massive clusters. Future systematic studies of all the active galaxies observed by VESTIGE in the Virgo cluster will extend these results to a robust statistical framework., Comment: 17 pages, 10 figures, 2 tables, A&A in press

Published
2018
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27. A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE).I. Introduction to the Survey

Author

Marc-Antoine Miville-Deschênes, T. Burdullis, Bernd Vollmer, Kanoa Withington, Stephanie Cote, Joel Roediger, Carmelle Robert, Stephen Gwyn, Michael L. Balogh, Simon Prunet, William E. Harris, A. Longobardi, M. Marcelin, J. A. Gómez-López, P. Salome, D. Russeil, Francoise Combes, Jean-Charles Cuillandre, Patrick Côté, Médéric Boquien, Jamilah Taylor, Benoît Epinat, B. Mahoney, David R. Patton, Thierry Contini, Eric W. Peng, Matteo Fossati, Rubén Sánchez-Janssen, Ming Sun, N. Manset, Yannick Roehlly, F. Boulanger, Samuel Boissier, Laura Ferrarese, Alan W. McConnachie, Baerbel Koribalski, Daniel Devost, Kristine Spekkens, Julio F. Navarro, Paolo Serra, Michele Fumagalli, Andreea Petric, Nikos Prantzos, Pauline Barmby, P. Amram, Gerhard Hensler, Denis Burgarella, Henri Plana, V. Buat, Herve Wozniak, G. Consolandi, Laurent Drissen, Stephanie Tonnesen, Sarah Gallagher, Luca Cortese, Giuseppe Gavazzi, Jon Willis, Jonathan Braine, Alessandro Boselli, 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), Max-Planck-Institut für Extraterrestrische Physik (MPE), NRC Herzberg Astronomy and Astrophysics, Conseil National de Recherches Canada (CNRC), Observatories [Carnegie Institution], Carnegie Institution for Science, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB), Department of Civil Engineering, Università degli Studi di Salerno = University of Salerno (UNISA), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), FORMATION STELLAIRE 2018, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), 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 de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Collège de France - Chaire Galaxies et cosmologie, Collège de France (CdF (institution)), 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), European Southern Observatory (ESO), Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), D´epartement de Physique, de G´enie Physique et d'Optique and Observatoire du mont M´egantic, Université Laval [Québec] (ULaval), Department of Philosophy [University of Memphis], University of Memphis, CHU Grenoble, Université Joseph Fourier - Grenoble 1 (UJF)-CHU Grenoble, University of Vienna [Vienna], Australia Telescope National Facility, Australian National University (ANU), Department of Physics and Astronomy [Peterborough], Trent University, 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), Centre de recherche Université Laval Robert Giffard (CRULRG), 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), Ministry of Agriculture of the People's Republic of China (MOA), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Departments of Medicine, Pharmacology and Therapeutics, McGill University = Université McGill [Montréal, Canada], Programme National de Cosmologie and Galaxies' (PNCG) funded by CNRS/INSU-IN2P3-INP, CEA and CNES, France, Carnegie Institution for Science [Washington], Università degli Studi di Milano-Bicocca [Milano] (UNIMIB), Università degli Studi di Salerno (UNISA), Smithsonian Institution-Harvard University [Cambridge], Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Chaire Galaxies et cosmologie, Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), École normale supérieure - Paris (ENS Paris), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Boselli, A, Fossati, M, Ferrarese, L, Boissier, S, Consolandi, G, Longobardi, A, Amram, P, Balogh, M, Barmby, P, Boquien, M, Boulanger, F, Braine, J, Buat, V, Burgarella, D, Combes, F, Contini, T, Cortese, L, Cote, P, Cote, S, Cuillandre, J, Drissen, L, Epinat, B, Fumagalli, M, Gallagher, S, Gavazzi, G, Gomez-Lopez, J, Gwyn, S, Harris, W, Hensler, G, Koribalski, B, Marcelin, M, Mcconnachie, A, Miville-Deschenes, M, Navarro, J, Patton, D, Peng, E, Plana, H, Prantzos, N, Robert, C, Roediger, J, Roehlly, Y, Russeil, D, Salome, P, Sanchez-Janssen, R, Serra, P, Spekkens, K, Sun, M, Taylor, J, Tonnesen, S, Vollmer, B, Willis, J, Wozniak, H, Burdullis, T, Devost, D, Mahoney, B, Manset, N, Petric, A, Prunet, S, Withington, K, 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), University of Salerno (UNISA), Harvard University [Cambridge]-Smithsonian Institution, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Laval, Geography Department, University of Dundee, École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), McGill University, Telescope CFH (TCFH), and Telescope CFH

Subjects
Stellar mass, clusters: individual: Virgo [Galaxies], Milky Way, FOS: Physical sciences, interactions [Galaxies], Astrophysics, clusters: general [Galaxies], 01 natural sciences, ISM [Galaxies], 0103 physical sciences, Galaxy formation and evolution, Emission spectrum, 010303 astronomy & astrophysics, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Star formation, Galaxies: evolution, Astronomy and Astrophysics, evolution [Galaxies], Galaxies: clusters: individual: Virgo, Virgo Cluster, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Galaxies: interactions, Galaxies: ISM, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], 13. Climate action, Space and Planetary Science, Galaxies: interaction, Astrophysics of Galaxies (astro-ph.GA), Galaxies: clusters: general, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE) is a blind narrow-band Halpha+[NII] imaging survey carried out with MegaCam at the Canada-France-Hawaii Telescope. The survey covers the whole Virgo cluster region from its core to one virial radius (104 deg^2). The sensitivity of the survey is of f(Halpha) ~ 4 x 10^-17 erg sec-1 cm^-2 (5 sigma detection limit) for point sources and Sigma (Halpha) ~ 2 x 10^-18 erg sec^-1 cm^-2 arcsec^-2 (1 sigma detection limit at 3 arcsec resolution) for extended sources, making VESTIGE the deepest and largest blind narrow-band survey of a nearby cluster. This paper presents the survey in all its technical aspects, including the survey design, the observing strategy, the achieved sensitivity in both the narrow-band Halpha+[NII] and in the broad-band r filter used for the stellar continuum subtraction, the data reduction, calibration, and products, as well as its status after the first observing semester. We briefly describe the Halpha properties of galaxies located in a 4x1 deg^2 strip in the core of the cluster north of M87, where several extended tails of ionised gas are detected. This paper also lists the main scientific motivations of VESTIGE, which include the study of the effects of the environment on galaxy evolution, the fate of the stripped gas in cluster objects, the star formation process in nearby galaxies of different type and stellar mass, the determination of the Halpha luminosity function and of the Halpha scaling relations down to ~ 10^6 Mo stellar mass objects, and the reconstruction of the dynamical structure of the Virgo cluster. This unique set of data will also be used to study the HII luminosity function in hundreds of galaxies, the diffuse Halpha+[NII] emission of the Milky Way at high Galactic latitude, and the properties of emission line galaxies at high redshift., Accepted for publication on Astronomy & Astrophysics

Published
2018
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28. Quenching of the star formation activity in cluster galaxies

Author

Yannick Roehlly, Médéric Boquien, Giuseppe Gavazzi, Paolo Serra, Alessandro Boselli, Denis Burgarella, Samuel Boissier, V. Buat, Laure Ciesla, Matteo Fossati, 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), Boselli, A, Roehlly, Y, Fossati, M, Buat, V, Boissier, S, Boquien, M, Burgarella, D, Ciesla, L, Gavazzi, G, and Serra, P

Subjects
FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Virial theorem, symbols.namesake, 0103 physical sciences, Galaxy formation and evolution, galaxies: interactions, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Balmer series, Astronomy and Astrophysics, Astronomy and Astrophysic, Virgo Cluster, Astrophysics - Astrophysics of Galaxies, Galaxy, Ram pressure, Galaxies: interaction, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, symbols, galaxies: clusters: individual: Virgo, Spectral energy distribution, galaxies: evolution, galaxies: ISM
Abstract

We study the star formation quenching mechanism in cluster galaxies by fitting the SED of the Herschel Reference Survey, a complete volume-limited K-band-selected sample of nearby galaxies including objects in different density regions, from the core of the Virgo cluster to the general field. The SED are fitted using the CIGALE SED modelling code. The truncated activity of cluster galaxies is parametrised using a specific SFH with 2 free parameters, the quenching age QA and the quenching factor QF. These 2 parameters are crucial for the identification of the quenching mechanism which acts on long timescales if starvation while rapid and efficient if ram pressure. To be sensitive to an abrupt and recent variation of the star formation activity, we combine in a new way 20 UV to FIR photometric bands with 3 age-sensitive Balmer line absorption indices extracted from available medium-resolution integrated spectroscopy and with Halpha narrow band imaging data. The use of a truncated SFH significantly increases the quality of the fit in those objects whose atomic gas content has been removed during the interaction with the hostile cluster environment. The typical QA of the perturbed late-type galaxies is QA < 300 Myr whenever the activity of star formation is reduced by 50% < QF 80%, while that of the quiescent early-types is QA ~ 1-3 Gyr. The fraction of late-types with a star formation activity reduced by QF > 80% and with an HI-deficiency parameter HI-def > 0.4 drops by a factor of ~ 5 from the inner half virial radius of the Virgo cluster, where the hot diffuse X-ray emitting gas of the cluster is located, to the outer regions. The efficient quenching of the star formation activity observed in Virgo suggests that the dominant stripping process is ram pressure. We discuss the implication of this result in the cosmological context of galaxy evolution., Accepted fro publication on Astronomy & Astrophysics

Published
2016
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29. The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Author

E. Voyer, Yannick Roehlly, Stephen Gwyn, Laura Ferrarese, Olivier Ilbert, Samuel Boissier, Lauren A. MacArthur, P. Côté, Sebastien Heinis, Alessandro Boselli, G. Consolandi, Giuseppe Gavazzi, Jean-Charles Cuillandre, Luca Cortese, 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), NRC Herzberg Astronomy and Astrophysics, Conseil National de Recherches Canada (CNRC), Università degli Studi di Milano-Bicocca [Milano] (UNIMIB), Centre for Astrophysics and Supercomputing (Centre for Astrophysics and Supercomputing), Swinburne University of Technology [Melbourne], Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Department of Astrophysical Sciences [Princeton], Princeton University, This research has been financed by the French ANR grant VIRAGE and the French national program PNCG., ANR-10-BLAN-0506,VIRAGE,VIRAGE: Virgo - Alterations des Galaxies dans les Environnements denses(2010), Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB), Boselli, A, Boissier, S, Voyer, E, Ferrarese, L, Consolandi, G, Cortese, L, Côté, P, Cuillandre, J, Gavazzi, G, Gwyn, S, Heinis, S, Ilbert, O, Macarthur, L, and Roehlly, Y

Subjects
Absolute magnitude, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, Supercluster, 0103 physical sciences, Galaxy formation and evolution, galaxies: interactions, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astronomy and Astrophysic, Virgo Cluster, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Galaxies: interaction, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, galaxies: clusters: individual: Virgo, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM
Abstract

We use the GALEX data of the GUViCS survey to construct the NUV luminosity function of the Virgo cluster over ~ 300 deg.2, an area covering the cluster and its surrounding regions up to ~ 1.8 virial radii. The NUV luminosity function is also determined for galaxies of different morphological type and NUV-i colour, and for the different substructures within the cluster. These luminosity functions are robust vs. statistical corrections since based on a sample of 833 galaxies mainly identified as cluster members with spectroscopic redshift (808) or high-quality optical scaling relations (10). We fit these luminosity functions with a Schechter function, and compare the fitted parameters with those determined for other nearby clusters and for the field. The faint end slope of the Virgo NUV luminosity function (alpha = -1.19), here sampled down to ~ NUV = -11.5 mag, is significantly flatter than the one measured in other nearby clusters and similar to the field one. Similarly M* = -17.56 is one-to-two magnitudes fainter than measured in Coma, A1367, the Shapley supercluster, and the field. These differences seem due to the quite uncertain statistical corrections and the small range in absolute magnitude sampled in these clusters. We do not observe strong systematic differences in the overall NUV luminosity function of the core of the cluster with respect to that of its periphery. We notice, however, that the relative contribution of red-to-blue galaxies at the faint end is inverted, with red quiescent objects dominating the core of the cluster and star forming galaxies dominating beyond one virial radius. These observational evidences are discussed in the framework of galaxy evolution in dense environments., Accepted for publication on Astronomy & Astrophsyics

Published
2015
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30. The GALEX ultraviolet virgo cluster survey (GUViCS): IV. the role of the cluster environment on galaxy evolution

Author

Luca Cortese, E. Voyer, Olga Cucciati, G. Consolandi, Sebastien Heinis, Michele Fumagalli, Alessandro Boselli, Yannick Roehlly, E. Toloba, Giuseppe Gavazzi, Samuel Boissier, Boselli, A, Voyer, E, Boissier, S, Cucciati, O, Consolandi, G, Cortese, L, Fumagalli, M, Gavazzi, G, Heinis, S, Roehlly, Y, Toloba, E, 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), 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
Stellar mass, clusters: individual: Virgo [Galaxies], FOS: Physical sciences, Astrophysics, interactions [Galaxies], Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], 01 natural sciences, 0103 physical sciences, ISM [Galaxies], Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Galaxy rotation curve, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Galaxies: star formation, 010308 nuclear & particles physics, Star formation, Galaxies: evolution, Astronomy and Astrophysics, Astronomy and Astrophysic, evolution [Galaxies], Galaxies: clusters: individual: Virgo, Virgo Cluster, Astrophysics - Astrophysics of Galaxies, Galaxy, Ram pressure, Interstellar medium, Galaxies: ISM, Galaxies: interaction, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Galaxies: clusters: general, star formation. [Galaxies]
Abstract

We study the role of the environment on galaxy evolution using a sample of 868 galaxies in the Virgo cluster and in its surrounding regions selected from the GUViCS Survey with the purpose of understanding the origin of the red sequence in dense environments. We collected multifrequency data covering the whole electromagnetic spectrum for most of the galaxies. We identify the different dynamical substructures composing the Virgo cluster and we calculate the local density of galaxies using different methods. We then study the distribution of galaxies belonging to the red sequence, the green valley, and the blue cloud within the different cluster substructures. Our analysis indicates that all the most massive galaxies are slow rotators and are the dominant galaxies of the different cluster substructures generally associated with a diffuse X-ray emission. They are probably the result of major merging events that occurred at early epochs. Slow rotators of lower stellar mass are also preferentially located within the different high-density substructures of the cluster. They are virialised within the cluster, thus Virgo members since its formation. They have been shaped by gravitational perturbations occurring within the infalling groups that later formed the cluster. On the contrary, low-mass star-forming systems are extremely rare in the inner regions of the Virgo cluster A, where the density of the intergalactic medium is at its maximum. Our ram pressure stripping models consistently indicate that these star-forming systems can be rapidly deprived of their interstellar medium during their interaction with the intergalactic medium. The lack of gas quenches their star formation activity transforming them into quiescent dwarf ellipticals. This mild transformation does not perturb the kinematic properties of these galaxies which still have rotation curves typical of star-forming systems., Comment: Submitted for publication on Astronomy & Astrophysics

Published
2014
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31. Spectacular tails of ionized gas in the Virgo cluster galaxy NGC 4569

Author

G. Anselmi, G. Consolandi, Laura Ferrarese, Dominik J. Bomans, S. D. J. Gwyn, Jean-Charles Cuillandre, P. Cote, E. Toloba, Matteo Fossati, A. Boselli, Gerhard Hensler, Michele Fumagalli, Luca Cortese, Mouyuan Sun, Giuseppe Gavazzi, S. Boissier, P. R. Durrell, 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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), Universitätssternwarte, Ruhr-Universität Bochum [Bochum], Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB), Coelum Astronomia, The University of Western Australia (UWA), NRC Herzberg Astronomy and Astrophysics, Conseil National de Recherches Canada (CNRC), Youngstown State University (YSU), NRC Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), Durham University, University of Vienna [Vienna], University of Alabama in Huntsville (UAH), UCO/Lick Observatory, University of California [Santa Cruz] (UC Santa Cruz), University of California (UC)-University of California (UC), Texas Tech University [Lubbock] (TTU), This research has been financed by the French ANR grant VIRAGE and the French national program PNCG, ANR-10-BLAN-0506,VIRAGE,VIRAGE: Virgo - Alterations des Galaxies dans les Environnements denses(2010), 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), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Università degli Studi di Milano-Bicocca [Milano] (UNIMIB), University of California [Santa Cruz] (UCSC), University of California-University of California, Boselli, A, Cuillandre, J, Fossati, M, Boissier, S, Bomans, D, Consolandi, G, Anselmi, G, Cortese, L, Côté, P, Durrell, P, Ferrarese, L, Fumagalli, M, Gavazzi, G, Gwyn, S, Hensler, G, Sun, M, and Toloba, E

Subjects
Stripping (chemistry), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, 0103 physical sciences, galaxies: interactions, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Surface brightness, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Virgo Cluster, Galaxy, Ram pressure, Galaxies: interaction, galaxies: clusters: general, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: clusters: individual: Virgo, Outflow, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: individual: NGC 4569, galaxies: ISM
Abstract

We obtained using MegaCam at the CFHT a deep narrow band Halpha+[NII] wide field image of NGC 4569, the brightest late-type galaxy in the Virgo cluster. The image reveals the presence of long tails of diffuse ionised gas without any associated stellar component extending from the disc of the galaxy up to ~ 80 kpc (projected distance) with a typical surface brightness of a few 10^-18 erg s-1 cm-2 arcsec-2. These features provide direct evidence that NGC 4569 is undergoing a ram presure stripping event. The image also shows a prominent 8 kpc spur of ionised gas associated to the nucleus that spectroscopic data identify as an outflow. With some assumptions on the 3D distribution of the gas, we use the Halpha surface brightness of these extended low surface brightness features to derive the density and the mass of the gas stripped during the interaction of the galaxy with the ICM. The comparison with ad-hoc chemo-spectrophotometric models of galaxy evolution indicates that the mass of the Halpha emitting gas in the tail is comparable to that of the cold phase stripped from the disc, suggesting that the gas is ionised within the tail during the stripping process. The lack of star forming regions suggests that mechanisms other than photoionisation are responsible for the excitation of the gas (shocks, heat conduction, magneto hydrodynamic waves). This analysis indicates that ram pressure stripping is efficient in massive (M_star ~ 10^10.5 Mo) galaxies located in intermediate mass (~ 10^14 Mo) clusters under formation. It also shows that the mass of gas expelled by the nuclear outflow is ~ 1 % than that removed during the ram pressure stripping event. All together these results indicate that ram pressure stripping, rather than starvation through nuclear feedback, can be the dominant mechanism responsible for the quenching of the star formation activity of galaxies in high density environments., Comment: Accepted for publication on Astronomy & Astrophysics

Published
2016
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