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1. Diffusion of radial action in a galactic disc

Author: Herve Wozniak, Laboratoire Univers et Particules de Montpellier (LUPM), and 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)
Subjects: Angular momentum, Metallicity, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Galaxy formation and evolution, Disc, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Nonlinear Sciences - Chaotic Dynamics, Astrophysics - Astrophysics of Galaxies, Galaxy, Stars, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [NLIN.NLIN-CD]Nonlinear Sciences [physics]/Chaotic Dynamics [nlin.CD], Astrophysics::Earth and Planetary Astrophysics, Chaotic Dynamics (nlin.CD), Lindblad resonance
Abstract: Context. Stellar migration of the galactic disc stars has been invoked to explain the dispersion of stellar metallicity observed in the solar neighborhood. Aims. We seek to identify the dynamical mechanisms underlying stellar migration in an isolated galaxy disc under the influence of a bar. Our approach is to analyze the diffusion of dynamical quantities. Methods. We extend our previous work by exploring Chirikov's diffusion rate (and derived timescale) of the radial action $J_\mathrm{R}$ in an idealised N$-$body simulation of an isolated disc galaxy. We limit our study to the evolution of the disc region well after the formation of the bar, in a regime of adiabatic evolution. Results. The $J_\mathrm{R}$ diffusion timescales $T_\mathrm{D}(J_\mathrm{R})$ is less than 3 Gyr for roughly half the galaxy mass. It is always much shorter than the angular momentum diffusion timescale $T_\mathrm{D}(L_\mathrm{z})$ outside the stellar bar. In the disc, $\langle T_\mathrm{D}(J_\mathrm{R}) \rangle \sim 1$ Gyr. All non-axisymmetric morphological structures characteristic of resonances and waves in the disc are associated to particles with $T_\mathrm{D}(J_\mathrm{R}) < 3$ Gyr and $T_\mathrm{D}(L_\mathrm{z}) > 10$ Gyr. Short $T_\mathrm{D}(J_\mathrm{R})$ can be explained by the gradual decircularisation of initially circular orbits ($J_\mathrm{R}=0$) under the effect of intermittent ILR scattering by wave trains propagating in the disc, well beyond the bar OLR. This leads to a moderate secular heating of the disc beyond the bar OLR for 7 Gyr, comparable to solar neighbourhood observations. The complex multi-wave structure, mixing permanent and intermittent modes, allows for multiple resonance overlaps., 10 pages, 9 figures, accepted for A&A
Published: 2020
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2. Simulation Data Access Layer Version 1.0

Author: David Languignon, Marco Molinaro, Carlos Rodrigo, Gerard Lemson, Herve Wozniak, Franck Petit, ITA, USA, FRA, ESP, The IVOA Technical Coordination Group, and IVOA
Subjects: business.industry, Computer science, business, Data access layer, Computer network
Abstract: The Simulation Data Access Layer protocol (SimDAL) defines a set of resources and associated actions to discover and retrieve simulations and numerical models in the Virtual Observatory. SimDAL and the Simulation Data Model are dedicated to cover the needs for the publication and retrieval of any kind of simulations: N-body or MHD simulations, numerical models of astrophysical objects and processes, theoretical synthetic spectra, etc... SimDAL is divided in three parts. First, SimDAL Repositories store the descriptions of theoretical projects and numerical codes. They can be used by clients to discover theoretical services associated with projects of interest. Second, SimDAL Search services are dedicated to the discovery of precise datasets. Finally, SimDAL Data Access services are dedicated to retrieve the original simulation output data, as plain raw data or formatted datasets cut-outs. To manage any kind of data, eventually large or at high-dimensionality, the SimDAL standard lets publishers choose any underlying implementation technology.
Published: 2019
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3. Simulation Data Model Version 1.0

Author: Mireille Louys, Claudio Gheller, Norman Gray, Gerard Lemson, Benjamin Ooghe, Herve Wozniak, Laurent Bourges, Franck LePetit, Miguel Cervino, and Rick Wagner
Subjects: Data model, Computer science, Data mining, computer.software_genre, computer
Published: 2019
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4. Stellar migration in galaxy discs using the Chirikov diffusion rate

Author: Herve Wozniak, Laboratoire Univers et Particules de Montpellier (LUPM), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Angular momentum, Diffusion, FOS: Physical sciences, Astrophysics, Barred spiral galaxies, 01 natural sciences, Dynamical evolution, [PHYS.PHYS.PHYS-COMP-PH]Physics [physics]/Physics [physics]/Computational Physics [physics.comp-ph], Extragalactic astronomy, Galactic Archaeology, Galaxy evolution, 0103 physical sciences, Galaxy formation and evolution, N-body simulations, 010306 general physics, Adiabatic process, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Galaxy stellar disks, Astrophysics::Galaxy Astrophysics, Physics, Astronomy and Astrophysics, Nonlinear Sciences - Chaotic Dynamics, Astrophysics - Astrophysics of Galaxies, Galaxy, Barred spiral galaxy, Distribution function, Galaxy dynamics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [NLIN.NLIN-CD]Nonlinear Sciences [physics]/Chaotic Dynamics [nlin.CD], [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics::Earth and Planetary Astrophysics, Chaotic Dynamics (nlin.CD), Lindblad resonance
Abstract: We are re-examining the problem of stellar migration in disc galaxies from a diffusion perspective. We use for the first time the formulation of the diffusion rates introduced by \citet{1979PhR....52..263C}, applied to both energy $E$ and angular momentum $L_\mathrm{z}$ in self-consistent N$-$body experiments. We limit our study to the evolution of stellar discs well after the formation of the bar, in a regime of adiabatic evolution. We show that distribution functions of Chirikov diffusion rates have similar shapes regardless the simulations, but different slopes for energy and angular momentum. Distribution functions of derived diffusion time scales $T_D$ have also the same form for all simulations, but are different for $T_D(E)$ and $T_D(L_\mathrm{z})$. Diffusion time scales are strongly dependent on $L_\mathrm{z}$. $T_D(E) \lesssim 1$~Gyr in a $L_\mathrm{z}$ range roughly delimited by the set of stellar bar resonances (between the Ultra Harmonic Resonance and the Outer Lindblad Resonance). Only particles with low $L_\mathrm{z}$ have $T_D(L_\mathrm{z}) \lesssim 10$ Gyr, i.e. the simulation length. In terms of mass fraction, 35 to 42% turn out to diffuse energy in a characteristic time scale shorter than 10 Gyr, i.e. simulations length, while 60 to 64% undergo the diffusion of the angular momentum on the same time scale. Both the diffusion of $L_\mathrm{z}$ and $E$ are important in order to grasp the full characterisation of the radial migration process, and we showed that depending on the spatial region considered, one or the other of the two diffusions dominates., Comment: 15 pages, 17 figures, Accepted for publication to ApJ
Published: 2019
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5. 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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6. On the origin of M81 group extended dust emission

Author: Bernhard Schulz, L. Spinoglio, Maud Galametz, Andreas Papageorgiou, Jason Glenn, Jonathan Ivor Davies, Marc Sauvage, N. Lu, Matthew Joseph Griffin, Eli Dwek, Robbie Richard Auld, D. Elbaz, Seb Oliver, M. J. Barlow, Herve Wozniak, Laure Ciesla, B. O'Halloran, L. R. Levenson, Ismael Perez-Fournon, Alessandro Boselli, A. Rykala, M. Bradford, M. Trichas, Christine D. Wilson, Frédéric Galliano, Walter Kieran Gear, Naseem Rangwala, George J. Bendo, Maximilien R. P. Schirm, Maarten Baes, Mat Page, A. Cooray, Jamie Stevens, Mattia Vaccari, Koryo Okumura, N. Sacchi, Sundar Srinivasan, T. J. Parkin, Diane Cormier, Suzanne C. Madden, Pasquale Panuzzo, N. Castro-Rodriguez, V. Buat, E. E. Rigby, Michael Pohlen, Kate Gudrun Isaak, M. Symeonidis, Matthew Smith, Helene Roussel, David L. Clements, Luca Cortese, L. Vigroux, James J. Bock, Stephane Charlot, Sacha Hony, Gillian S. Wright, Haley Louise Gomez, Pierre Chanial, Stephen Anthony Eales, and Werner W. Zeilinger
Subjects: Physics, Infrared, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Minute of arc, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Wavelength, Space and Planetary Science, Group (periodic table), Cirrus, Optical emission spectroscopy, Astrophysics::Galaxy Astrophysics, Dust emission
Abstract: Galactic cirrus emission at far-infrared wavelengths affects many extragalactic observations. Separating this emission from that associated with extragalactic objects is both important and difficult. In this paper we discuss a particular case, the M81 group, and the identification of diffuse structures prominent in the infrared, but also detected at optical wavelengths. The origin of these structures has previously been controversial, ranging from them being the result of a past interaction between M81 and M82 or due to more local Galactic emission. We show that over of order a few arcminute scales the far-infrared (Herschel 250 &\mu&m) emission correlates spatially very well with a particular narrow velocity (2-3 km/s) component of the Galactic HI. We find no evidence that any of the far-infrared emission associated with these features actually originates in the M81 group. Thus we infer that the associated diffuse optical emission must be due to galactic light back scattered off dust in our galaxy. Ultra-violet observations pick out young stellar associations around M81, but no detectable far-infrared emission. We consider in detail one of the Galactic cirrus features, finding that the far-infrared HI relation breaks down below arc minute scales and that at smaller scales there can be quite large dust temperature variations.
Published: 2010
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7. The Herschel Reference Survey

Author: Jason Glenn, E. Dwek, George J. Bendo, Jamie Stevens, Alessandro Boselli, N. Sacchi, Mat Page, Walter Kieran Gear, L. Vigroux, Ismael Perez-Fournon, Maximilien R. P. Schirm, K. Okumura, P. Chanial, K. G. Isaak, A. Rykala, Diane Cormier, James J. Bock, Jonathan Ivor Davies, E. E. Rigby, Marc Sauvage, Stephane Charlot, Matthew Smith, Michael Pohlen, N. Castro-Rodriguez, G. Wright, L. Spinoglio, N. Rangwala, Louis Levenson, Robbie Richard Auld, D. Elbaz, Matthew Joseph Griffin, Helene Roussel, David L. Clements, Christine D. Wilson, B. O'Halloran, Benjamin L. Schulz, Luca Cortese, V. Buat, Werner W. Zeilinger, Frédéric Galliano, Haley Louise Gomez, Stephen Anthony Eales, Maarten Baes, M. Bradford, P. Panuzzo, Nanyao Y. Lu, M. J. Barlow, M. Symeonidis, Suzanne C. Madden, S. J. Oliver, Sacha Hony, T. J. Parkin, Herve Wozniak, Andreas Papageorgiou, Maud Galametz, and Mattia Vaccari
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, media_common.quotation_subject, FOS: Physical sciences, Astronomy and Astrophysics, Sample (statistics), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Virgo Cluster, Galaxy, Universe, Interstellar medium, Stars, Space and Planetary Science, Range (statistics), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, media_common
Abstract: The Herschel Reference Survey is a guaranteed time Herschel key project and will be a benchmark study of dust in the nearby universe. The survey will complement a number of other Herschel key projects including large cosmological surveys that trace dust in the distant universe. We will use Herschel to produce images of a statistically-complete sample of 323 galaxies at 250, 350 and 500 micron. The sample is volume-limited, containing sources with distances between 15 and 25 Mpc and flux limits in the K-band to minimize the selection effects associated with dust and with young high-mass stars and to introduce a selection in stellar mass. The sample spans the whole range of morphological types (ellipticals to late-type spirals) and environments (from the field to the centre of the Virgo Cluster) and as such will be useful for other purposes than our own. We plan to use the survey to investigate (i) the dust content of galaxies as a function of Hubble type, stellar mass and environment, (ii) the connection between the dust content and composition and the other phases of the interstellar medium and (iii) the origin and evolution of dust in galaxies. In this paper, we describe the goals of the survey, the details of the sample and some of the auxiliary observing programs that we have started to collect complementary data. We also use the available multi-frequency data to carry out an analysis of the statistical properties of the sample., Comment: Accepted for publication on PASP
Published: 2010
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8. Formation of young boxy/peanut bulges in ringed barred galaxies

Author: Herve Wozniak, L. Michel-Dansac, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Instituto de Astronomía Teórica y Experimental (IATE), Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET)-Universidad Nacional de Córdoba [Argentina], École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Universidad Nacional de Córdoba [Argentina]-Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET)
Subjects: galaxies: spiral, Stellar population, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies: active, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Bulge, 0103 physical sciences, Galaxy formation and evolution, 010306 general physics, education, 010303 astronomy & astrophysics, galaxies: kinematics and dynamics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, Spiral galaxy, Star formation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, galaxies: Seyfert, Galaxy, Barred spiral galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, galaxies: nuclei, galaxies: evolution
Abstract: We investigate whether the formation mechanism of boxy and peanut-shaped (B/PS) bulges could depend on the gas content of the galaxy. We have performed N-body simulations with and without a gaseous component. In the second case star formation/feedback recipes have also been implemented to create new stellar populations. As in many previous studies, in our N-body collisionless simulation, the B/PS is due to the classical break in the z mirror symmetry lasting roughly 200 Myr. When a gaseous component and star formation recipes are added to the simulation, the bulge-growing mechanism is quite different. The young stellar population that is born in the thin gaseous disc rapidly populates vertical resonant orbits triggered by the combined effects of the linear horizontal and vertical ILRs. This leads to a B/PS bulge mainly made of stellar material younger than the surrounding population. The non-linear analysis of the orbital structure shows that the main orbit family responsible for the B/PS is not the same in the two cases. The 2:2:1 orbits prevail in the collisionless simulation whereas additional asymmetrical families contribute to the B/PS if a dissipative component is present and can form new stars. We found that 2:3:1 and 2:5:1 orbits trap a significant fraction of the mass. A flat ringed discy stellar component also appears simultaneously with the thickening of the young population. It is due to the star formation in a nuclear gaseous disc located in the central kpc, inside the ILR, and accumulated there by the torques exerted by the large-scale bar. Remarkably, it remains flat throughout the simulation although it develops a nuclear bar, leading to a double-barred galaxy. We predict that two populations of B/PS bulges could exist and even coexist in the same galaxy., 10 pages, 11 Postscript figures, published in A&A
Published: 2008
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9. IMAGES IV: strong evolution of the oxygen abundance in gaseous phases of intermediate mass galaxies fromz ~ 0.8

Author: B. Guiderdoni, Göran Östlin, Ajit K. Kembhavi, Nicole P. H. Nesvadba, Isaura Fuentes-Carrera, F. Hammer, C. J. Cesarsky, Herve Wozniak, C. Balkowski, Lucia Pozzetti, Benoit Neichel, Hector Flores, Joel Vernet, Miguel Rodrigues, P. Amram, Daniela Vergani, S. di Serego Alighieri, R. Delgado, C. D. Ravikumar, Yun-Feng Liang, Helmut Dannerbauer, M. D. Lehnert, Mathieu Puech, A. Rawat, Y. Yang, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: galaxies: spiral, Stellar mass, Metallicity, Extinction (astronomy), Population, FOS: Physical sciences, galaxies: starburst, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Tully–Fisher relation, 01 natural sciences, infrared: galaxies, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Spectral resolution, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Astrophysics (astro-ph), Astronomy and Astrophysics, Galaxy, Space and Planetary Science, galaxies: evolution, galaxies: ISM
Abstract: Intermediate mass galaxies (logM(Msun)>10) at z~0.6 are the likeliest progenitors of the present-day numerous population of spirals. There is growing evidence that they have evolved rapidly since the last 6 to 8 Gyr ago, and likely have formed a significant fraction of their stellar mass, often showing perturbed morphologies and kinematics. We have gathered a representative sample of 88 such galaxies and have provided robust estimates of their gas phase metallicity. For doing so, we have used moderate spectral resolution spectroscopy at VLT/FORS2 with unprecedented high S/N allowing to remove biases coming from interstellar absorption lines and extinction to establish robust values of R23=([OII]3727 + [OIII]4959,5007)/Hbeta. We definitively confirm that the predominant population of z~0.6 starbursts and luminous IR galaxies (LIRGs) are on average, two times less metal rich than the local galaxies at a given stellar mass. We do find that the metal abundance of the gaseous phase of galaxies is evolving linearly with time, from z=1 to z=0 and after comparing with other studies, from z=3 to z=0. Combining our results with the reported evolution of the Tully Fisher relation, we do find that such an evolution requires that ~30% of the stellar mass of local galaxies have been formed through an external supply of gas, thus excluding the close box model. Distant starbursts & LIRGs have properties (metal abundance, star formation efficiency & morphologies) similar to those of local LIRGs. Their underlying physics is likely dominated by gas infall probably through merging or interactions. Our study further supports the rapid evolution of z~0.4-1 galaxies. Gas exchanges between galaxies is likely the main cause of this evolution., 21 pages, 12 figures, A&A, In press
Published: 2008
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10. IMAGES. I. Strong evolution of galaxy kinematics since z = 1

Author: Joel Vernet, Nicole P. H. Nesvadba, C. J. Cesarsky, Herve Wozniak, Hector Flores, S. diSeregoAlighieri, I. Fuentes-Carrera, D. Vergani, M. D. Lehnert, B. Guiderdoni, Lucia Pozzetti, Ajit K. Kembhavi, Benoit Neichel, Mathieu Puech, F. Hammer, Yun-Feng Liang, Helmut Dannerbauer, Göran Östlin, P. Amram, Chantal Balkowski, C. D. Ravikumar, Y. Yang, A. Rawat, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Paris (OP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), 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), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Beaussier, Catherine, Physique des Galaxies et Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Pôle Astronomie du LESIA, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, European Southern Observatory (ESO), Inter-University Centre for Astronomy and Astrophysics (IUCAA), INAF-Osservatorio Astronomico di Bologna (OABO), Max-Planck-Institut für Astronomie (MPIA), INAF-Osservatorio Astrofisico di Arcetri (INAF-OAA), National Astronomical Observatoires-CAS, Stockholm Observatory, AlbaNova University Center, Department of Physics, University of Calicut, and Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano)
Subjects: Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Kinematics, 01 natural sciences, Measure (mathematics), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Emission spectrum, education, Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Cosmic variance, Redshift, Galaxy, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: (abbreviated) We present the first results of the ESO large program, ``IMAGES'' which aims at obtaining robust measurements of the kinematics of distant galaxies using the multi-IFU mode of GIRAFFE on the VLT. 3D spectroscopy is essential to robustly measure the often distorted kinematics of distant galaxies (e.g., Flores et al. 2006). We derive the velocity fields and $\sigma$-maps of 36 galaxies at 0.4 15 A) at z=0.4-0.75, which are a representative subsample of the population of M_stellar>1.5x10^{10} M_sun emission line galaxies in this redshift range, and are largely unaffected by cosmic variance. Taking into account all galaxies -with or without emission lines- in that redshift range, we find that at least 41+/-7% of them have anomalous kinematics, i.e., they are not dynamically relaxed. This includes 26+/-7% of distant galaxies with complex kinematics, i.e., they are not simply pressure or rotationally supported. Our result implies that galaxy kinematics are among the most rapidly evolving properties, because locally, only a few percent of the galaxies in this mass range have complex kinematics., Comment: 17 pages, 6 figures, Accepted by A&A
Published: 2007
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11. How can double-barred galaxies be long-lived?

Author: Herve Wozniak, Observatoire astronomique de Strasbourg (ObAS), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: 010504 meteorology & atmospheric sciences, Stellar population, Bar (music), FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Rotation, 01 natural sciences, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Star formation, High Energy Physics::Phenomenology, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Mode coupling, High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, Lindblad resonance
Abstract: Double-barred galaxies account for almost one third of all barred galaxies, suggesting that secondary stellar bars, which are embedded in large-scale primary bars, are long-lived structures. However, up to now it has been hard to self-consistently simulate a disc galaxy that sustains two nested stellar bars for longer than a few rotation periods. N-body/hydrodynamical simulations including star formation recipes have been performed. Their properties have been compared with the most recent observational data in order to prove that they are representative of double-barred galaxies, even SB0. Overlaps in dynamical resonances and bar modes have been looked for using Fourier spectrograms. Double-barred galaxies have been successfully simulated with lifetimes as long as 7 Gyr. The stellar population of the secondary bar is younger on average than for the primary large-scale bar. An important feature of these simulations is the absence of any resonance overlap for several Gyr. In particular, there is no overlap between the primary bar ILR and the secondary bar corotation. Therefore, mode coupling cannot sustain the secondary bar mode. Star formation is identified here as possibly being responsible for bringing energy to the nuclear mode. Star formation is also responsible for limiting the amount of gas in the central region which prevents the orbits sustaining the secondary bar from being destroyed. Therefore, the secondary bar can dissolve but reappear after approx. 1 Gyr. When star formation is switched off the dynamical perturbation associated with the secondary bar needs several Gyr to fully vanish. Double-bars can be long-lived in numerical simulations with a gaseous component, even in the absence of overlap of resonances or mode coupling, provided that star formation remains active in the central region where the nuclear bar lies., Comment: 14 pages, 14 low resolution figures ; high resolution paper available at http://herve.wozniak.fr/DB.pdf (27 Mb)
Published: 2015

12. Lifetime of nuclear velocity dispersion drops in barred galaxies

Author: Nicolas Champavert and Herve Wozniak
Subjects: Physics, Star formation, Drop (liquid), Sigma, Velocity dispersion, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Central region, Galaxy, Space and Planetary Science, Bulge, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We have made hydro/N-body simulations with and without star formation to shed some light on the conditions under which a central kinematically cold stellar component (characterized by a velocity dispersion drop or \sigma-drop) could be created in a hot medium (e.g. a bulge) and survive enough time to be observed. We found that the timescale for a \sigma-drop formation could be short (less than 500 Myr) whereas its lifetime could be long (more than 1 Gyr) provided that the central region is continuously or regularly fed by fresh gas which leads to a continuous star formation activity. Star formation in the central region, even at a low rate as 1M_{sol} yr^{-1}, is mandatory to sustain a permanent \sigma-drop by replacing heated particles by new low-\sigma ones. We moreover show that as soon as star formation is switched off, the \sigma-drop begins to disappear.
Published: 2006
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13. Gas and stellar dynamics in NGC 1068

Author: Kambiz Fathi, Eva Schinnerer, Carole Mundell, Herve Wozniak, Pierre Ferruit, Eric Emsellem, and Kapteyn Astronomical Institute
Subjects: Stellar kinematics, galaxies : evolution, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies : kinematics and dynamics, GALAXY NGC 1068, TREMAINE-WEINBERG-METHOD, VELOCITY DISPERSION DROPS, SEYFERT-GALAXIES, Gravitational potential, IONIZED-GAS, galaxies : Seyfert, Stellar dynamics, galaxies : nuclei, Astrophysics::Galaxy Astrophysics, Physics, Spiral galaxy, Star formation, Astrophysics (astro-ph), Astronomy and Astrophysics, N-BODY SIMULATIONS, SAURON PROJECT, Galaxy, Accretion (astrophysics), Stars, NARROW-LINE REGION, Space and Planetary Science, galaxies : individual : NGC 1068, SPIRAL GALAXIES, BARRED GALAXIES
Abstract: We present Sauron 2D spectrography of the central 1.5 kpc of the nearby Sey2 galaxy NGC1068, encompassing the well-known NIR inner bar. We have successively disentangled the respective contributions of the ionized gas and stars, thus deriving their 2D distribution and kinematics. The [OIII] and Hbeta emission lines exhibit very different spatial distribution and kinematics, the latter following inner spiral arms with clumps associated with star formation. Strong inwards streaming motions are observed in both the Hbeta and [OIII] kinematics. The stellar kinematics also exhibit clear signatures of a non-axisymmetric tumbling potential, with a twist in both the velocity and h3 fields. We re-examined the long-slit data of Shapiro et al (2003) using pPXF: a strong decoupling of h3 is revealed, and the central decrease in h4 hinted in the Sauron data is confirmed. These data also suggest that NGC1068 is a good candidate for a so-called sigma-drop. We confirm the possible presence of two pattern speeds. We also examine the stellar kinematics of bars formed in N-body+SPH simulations built from axisymmetric initial conditions. These successfully reproduce a number of properties observed in the 2D kinematics of NGC1068, and the long-slit data, showing that the kinematic signature of the NIR bar is imprinted in the stellar kinematics. The remaining differences between the models and the observed properties are mostly due to the exclusion of star formation and the lack of the primary large-scale oval/bar in the simulations. These models suggest that the inner bar could drive a significant amount of gas down to a scale of ~300 pc. This is consistent with the interpretation of the sigma-drop in NGC1068 being the result of central gas accretion followed by an episode of star formation., Comment: accepted for publication in MNRAS, 20 pages, 17 figures (high res version available at www-obs.univ-lyon1.fr/eric.emsellem/preprints/NGC1068_Emsellemetal_final.pdf)
Published: 2006

14. An Overview of the Dwarf Galaxy Survey (PASP, 125, 600, [2013])—Corrigendum

Author: Asantha Cooray, Marc Sauvage, I. De Looze, N. Y. Lu, Judith A. Irwin, Diane Cormier, Maarten Baes, Frédéric Galliano, Michael Pohlen, Maud Galametz, J. A. MacHattie, Ronin Wu, Eckhard Sturm, Kate Gudrun Isaak, N. Rangwala, Maximilien R. P. Schirm, S. Hony, M. J. Barlow, Christine D. Wilson, Mattia Vaccari, V. Lebouteiller, J. Kamenetzky, G. J. Bendo, Luigi Spinoglio, A. Contursi, A. Boselli, L. Ciesla, Benjamin L. Schulz, B. O'Halloran, Aurélie Rémy-Ruyer, L. R. Carlson, Herve Wozniak, M. W. L. Smith, O. Ł. Karczewski, M. Boquien, T. J. Parkin, H. Roussel, V. Doublier, Luca Cortese, Albrecht Poglitsch, S. C. Madden, Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), 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), University of Cambridge [UK] (CAM), 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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, University of Manchester [Manchester], School of Physics and Astronomy [Cardiff], Cardiff University, Laboratoire des matériaux et du génie physique (LMGP ), Institut National Polytechnique de Grenoble (INPG)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Max-Planck-Institut für Extraterrestrische Physik (MPE), Sterrenkundig Observatorium, Universiteit Gent, 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), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, California Institute of Technology (CALTECH), Center for Astrophysics and Space Astronomy [Boulder] (CASA), University of Colorado [Boulder], Infrared Processing and Analysis Center (IPAC), Antarctic Research a European Network for Astrophysics (ARENA), Dipartimento di Astronomia [Padova], Universita degli Studi di Padova, Department of Physics and Astronomy [South Africa], University of the Western Cape, Norwegian Water Resources and Energy Directorate (NVE), 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), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), 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 polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National Polytechnique de Grenoble (INPG)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Universiteit Gent = Ghent University (UGENT), 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), NASA-California Institute of Technology (CALTECH), Università degli Studi di Padova = University of Padua (Unipd), University of the Western Cape (UWC), Laboratoire des matériaux et du génie physique (LMGP), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique de Grenoble (INPG), Institut für Geologie und Mineralogie, and Dipartimento di Astronomia
Subjects: Physics, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Sample (graphics), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Dwarf galaxy
Abstract: After finding an error in the procedure for computing the stellar masses of the Dwarf Galaxy Survey sample, we present here the correct values for the stellar masses.
Published: 2014
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15. Dynamics of embedded bars and the connection with AGN

Author: Eric Emsellem, Herve Wozniak, Francoise Combes, D. Friedli, Stephane Leon, Emmanuel Pecontal, and D. Greusard
Subjects: Physics, Stellar kinematics, Active galactic nucleus, Astrophysics (astro-ph), FOS: Physical sciences, Velocity dispersion, Astronomy and Astrophysics, Angular velocity, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Kinematics, Galaxy, Stars, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Surface brightness, Astrophysics::Galaxy Astrophysics
Abstract: We present new stellar kinematical profiles of four galaxy hosts of active galactic nuclei, using the CO bandhead around 2.3 micron with the ISAAC/VLT spectrograph. We find that the nuclear bars or discs, embedded in large-scale primary bars, have all a decoupled kinematics, in the sense that the maximum of the rotational velocity occurs in the nuclear region. In three cases (NGC 1097, NGC 1808 and NGC 5728), the velocity dispersion displays a significant drop at the nucleus, a rarely observed phenomenon. We also detect kinematical asymmetries (m=1 mode) along the nuclear bar major-axis of NGC 1808 and NGC 5728, dynamical counterparts of corresponding asymmetries in the surface brightness. We have derived simple dynamical models in an attempt to fit the kinematics of each galaxy and reconstruct the full velocity field. For all four targets, the fits are good, and confirm the presence of the decoupled nuclear components. These models cannot however reproduce the observed central drop in the dispersion. We suggest that this drop is due to a transient cold nuclear disc, fuelled by gas inflow along the bar, that has recently formed new stars., Accepted for pub. in A&A, 12 pages, 12 figures
Published: 2001
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16. Near–infrared probing of embedded structures in starburst and Seyfert galaxies

Author: P. Martin, Herve Wozniak, L. Martinet, D. Friedli, and D. Greusard
Subjects: Physics, Photometry (astronomy), Bar (music), Primary (astronomy), Astrophysics (astro-ph), Magnitude (astronomy), Near-infrared spectroscopy, FOS: Physical sciences, General Physics and Astronomy, Astrophysics, Galaxy
Abstract: Surface photometry in the J and K' bands of 15 southern Seyfert or starburst galaxies is presented. The detailed central morphology and structural properties of these objects were analyzed by fitting ellipses to isophotes. New central peculiar structures have been identified like, for instance, three double-barred systems (ESO 215-G031; ESO 320-G030; ESO 443-G017), one object with a nested nuclear spiral structure at the center of a primary bar (NGC 5135), one object with a nuclear bar without evidence of a large-scale bar (NGC 4941), and one galaxy with a likely dissolved secondary bar within a primary one (ESO 508-G005). The J-K' radial profile proved to be reasonably well linked with the presence of a starburst, but not with the Seyfert activity. For significant starbursts, the central J-K' value is 0.3-1.5 magnitude larger than the disc one., 19 pages, 10 figures, accepted for publication in A&AS
Published: 2000
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17. Explaining two circumnuclear star forming rings in NGC 5248

Author: Sharon E. Meidt, Carole Mundell, T. P. R. van der Laan, L. Hunt, E. Emsellem, S. Haan, Eva Schinnerer, Herve Wozniak, G. Dumas, Torsten Boeker, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: ACTIVE GALACTIC NUCLEI, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Star (graph theory), Ring (chemistry), 01 natural sciences, Parsec, Gravitational potential, LINE KINEMATICS, individual: NGC 5248 [galaxies], 0103 physical sciences, Emission spectrum, Disc, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, INNER LINDBLAD RESONANCE, LENTICULAR GALAXIES, DOUBLE-BARRED, Physics, ISM [galaxies], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, DISK GALAXIES, stellar content [galaxies], SAURON PROJECT, MOLECULAR GAS, Galaxy, GALAXIES, HOST GALAXIES, Physics and Astronomy, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, SPIRAL GALAXIES, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The distribution of gas in the central kiloparsec of a galaxy has a dynamically rapid evolution. Nonaxisymmetries in the gravitational potential of the galactic disk, such as a large scale stellar bar or spiral, can lead to significant radial motion of gaseous material from larger radii to the central region. The large influx of gas and the subsequent star formation keep the central region constantly changing. However, the ability of gas to reach the nucleus proper to fuel an AGN phase is not guaranteed. Gas inflow can be halted at a circumnuclear star forming ring several hundred parsec away. The nearby galaxy NGC5248 is especially interesting in this sense since it is said to host 2 circumnuclear star forming rings at 100pc and 370pc from its quiescent nucleus. Here we present new subarcsecond PdBI+30m CO(2-1) emission line observations of the central region. For the first time the molecular gas distribution at the smallest stellar ring is resolved into a gas ring, consistent with the presence of a quiescent nucleus. However, the molecular gas shows no ring structure at the larger ring. We combine analyses of the gaseous and stellar content in the central kiloparsec of this galaxy to understand the gas distribution and dynamics of this star forming central region. We discuss the probability of two scenarios leading to the current observations, given our full understanding of this system, and discuss whether there are really two circumnuclear star forming rings in this galaxy., Accepted for publication in A&A, 14pages + long table
Published: 2013

18. An Overview of the Dwarf Galaxy Survey

Author: Julia Kamenetzky, George J. Bendo, Marc Sauvage, I. De Looze, Suzanne C. Madden, N. Y. Lu, Diane Cormier, Albrecht Poglitsch, Matthew Smith, H. Roussel, Laure Ciesla, M. Pohlen, A. Contursi, B. O Halloran, Asantha Cooray, M. J. Barlow, Eckhard Sturm, Frédéric Galliano, Maximilien R. P. Schirm, K. G. Isaak, T. J. Parkin, Vanessa Doublier, O. L. Karczewski, N. Rangwala, L. R. Carlson, Maud Galametz, Ronin Wu, Sacha Hony, Alessandro Boselli, Luca Cortese, Herve Wozniak, A. Remy Ruyer, Judith A. Irwin, J. A. MacHattie, Luigi Spinoglio, Vianney Lebouteiller, Christine D. Wilson, Maarten Baes, Médéric Boquien, Mattia Vaccari, Benjamin L. Schulz, 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), 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), 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: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Metallicity, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, ASTROPHYSICAL DUST EMISSION, 01 natural sciences, AROMATIC-HYDROCARBON EMISSION, H-II REGIONS, 158 MU-M, 0103 physical sciences, STAR-FORMING GALAXIES, 010303 astronomy & astrophysics, QB, media_common, Dwarf galaxy, Physics, NEUTRAL HYDROGEN OBSERVATIONS, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, HUBBLE-SPACE-TELESCOPE, Astrophysics - Astrophysics of Galaxies, Universe, Galaxy, Interstellar medium, Spire, Stars, SPECTRAL ENERGY-DISTRIBUTION, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), BLUE COMPACT GALAXIES, LOW-METALLICITY ENVIRONMENTS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Dwarf Galaxy Survey (DGS) program is studying low-metallicity galaxies using 230h of far-infrared (FIR) and submillimetre (submm) photometric and spectroscopic observations of the Herschel Space Observatory and draws to this a rich database of a wide range of wavelengths tracing the dust, gas and stars. This sample of 50 galaxies includes the largest metallicity range achievable in the local Universe including the lowest metallicity (Z) galaxies, 1/50 Zsun, and spans 4 orders of magnitude in star formation rates. The survey is designed to get a handle on the physics of the interstellar medium (ISM) of low metallicity dwarf galaxies, especially on their dust and gas properties and the ISM heating and cooling processes. The DGS produces PACS and SPIRE maps of low-metallicity galaxies observed at 70, 100, 160, 250, 350, and 500 mic with the highest sensitivity achievable to date in the FIR and submm. The FIR fine-structure lines, [CII] 158 mic, [OI] 63 mic, [OI] 145 mic, [OIII] 88 mic, [NIII] 57 mic and [NII] 122 and 205 mic have also been observed with the aim of studying the gas cooling in the neutral and ionized phases. The SPIRE FTS observations include many CO lines (J=4-3 to J=13-12), [NII] 205 mic and [CI] lines at 370 and 609 mic. This paper describes the sample selection and global properties of the galaxies, the observing strategy as well as the vast ancillary database available to complement the Herschel observations. The scientific potential of the full DGS survey is described with some example results included., Article accepted for PASP (april 25 2013)
Published: 2013
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19. The Wavy-Pattern of Stellar Rotation Curves in SBO Galaxies

Author: Daniel Pfenniger and Herve Wozniak
Subjects: Physics, Classical mechanics, Stellar rotation, Astrophysics, Galaxy
Abstract: We discuss the “rotation” curves of SB0 galaxies with self-consistent models constructed with Schwarzschild’s method. Their distribution functions are compared with that of N-body simulations.
Published: 1996
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20. FIR colours and SEDs of nearby galaxies observed with Herschel

Author: Stefano Zibetti, Matthew Joseph Griffin, Diane Cormier, Werner W. Zeilinger, Maud Galametz, L. Spinoglio, E. E. Rigby, Thomas M. Hughes, Andreas Papageorgiou, Aliakbar Dariush, Simone Bianchi, Jonathan Ivor Davies, Dario Fadda, Michael Pohlen, Anthony P. Jones, Marc Sauvage, Leslie K. Hunt, N. Lu, N. Castro-Rodriguez, Daniele Pierini, Gillian S. Wright, Jamie Stevens, Sacha Hony, Laure Ciesla, Herve Wozniak, Eli Dwek, Pierre Chanial, Jacopo Fritz, Kate Gudrun Isaak, Asantha Cooray, Ismael Perez-Fournon, L. Vigroux, Maximilien R. P. Schirm, Jason Glenn, Matthew Smith, D. J. Bomans, George J. Bendo, Alessandro Boselli, Marco Grossi, D. A. Garcia-Appadoo, Mattia Vaccari, M. Bradford, A. Rykala, Suzanne C. Madden, V. Buat, Koryo Okumura, Catherine Vlahakis, S. Sabatini, Christine D. Wilson, B. O'Halloran, Edvige Corbelli, James J. Bock, Frédéric Galliano, L. R. Levenson, Giuseppe Gavazzi, Markos Trichas, Helene Roussel, David L. Clements, Luca Cortese, Marcel Clemens, Benjamin L. Schulz, Seb Oliver, Stephane Charlot, Carlo Giovanardi, Maarten Baes, Emmanuel M. Xilouris, Joris Verstappen, Naseem Rangwala, Stephen Anthony Eales, N. Sacchi, P. Panuzzo, Robbie Richard Auld, T. J. Parkin, S. Sundar, M. J. Page, David Elbaz, M. Symeonidis, S. di Serego Alighieri, Haley Louise Gomez, Walter Kieran Gear, I. De Looze, 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), Science and Technology Facilities Council (STFC), Boselli, A, Ciesla, L, Buat, V, Cortese, L, Auld, R, Baes, M, Bendo, G, Bianchi, S, Bock, J, Bomans, D, Bradford, M, Castro Rodriguez, N, Chanial, P, Charlot, S, Clemens, M, Clements, D, Corbelli, E, Cooray, A, Cormier, D, Dariush, A, Davies, J, De Looze, I, di Serego Alighieri, S, Dwek, E, Eales, S, Elbaz, D, Fadda, D, Fritz, J, Galametz, M, Galliano, F, Garcia Appadoo, D, Gavazzi, G, Gear, W, Giovanardi, C, Glenn, J, Gomez, H, Griffin, M, Grossi, M, Hony, S, Hughes, T, Hunt, L, Isaak, K, Jones, A, Levenson, L, Lu, N, Madden, S, O'Halloran, B, Okumura, K, Oliver, S, Page, M, Panuzzo, P, Papageorgiou, A, Parkin, T, Perez Fournon, I, Pierini, D, Pohlen, M, Rangwala, N, Rigby, E, Roussel, H, Rykala, A, Sabatini, S, Sacchi, N, Sauvage, M, Schulz, B, Schirm, M, Smith, M, Spinoglio, L, Stevens, J, Sundar, S, Symeonidis, M, Trichas, M, Vaccari, M, Verstappen, J, Vigroux, L, Vlahakis, C, Wilson, C, Wozniak, H, Wright, G, Xilouris, E, Zeilinger, W, and Zibetti, S
Subjects: Infrared, Radio galaxy, DUST, Astrophysics, 01 natural sciences, galaxies [infrared], Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, QB, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ATLAS, VIRGO CLUSTER, spiral [galaxies], Physical Sciences, astro-ph.CO, Astrophysics::Earth and Planetary Astrophysics, galaxies: ISM, Astrophysics - Cosmology and Nongalactic Astrophysics, galaxies: spiral, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Metallicity, INFRARED-EMISSION, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Color temperature, infrared: galaxies, cD, FIS/05 - ASTRONOMIA E ASTROFISICA, 0103 physical sciences, Emissivity, STAR-FORMING GALAXIES, DISTRIBUTIONS, Astrophysics::Galaxy Astrophysics, Science & Technology, ISM [galaxies], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Galaxy, UV, 0201 Astronomical And Space Sciences, SPITZER, SPECTRAL ENERGY-DISTRIBUTION, Physics and Astronomy, 13. Climate action, Space and Planetary Science, galaxies: elliptical and lenticular, cD, elliptical and lenticular [galaxies]
Abstract: We present infrared colours (in the 25-500 mic spectral range) and UV to radio continuum spectral energy distributions of a sample of 51 nearby galaxies observed with SPIRE on Herschel. The observed sample includes all morphological classes, from quiescent ellipticals to active starbursts. Active galaxies have warmer colour temperatures than normal spirals. In ellipticals hosting a radio galaxy, the far-infrared (FIR) emission is dominated bynthe synchrotron nuclear emission. The colour temperature of the cold dust is higher in quiescent E-S0a than in star-forming systems probably because of the different nature of their dust heating sources (evolved stellar populations, X-ray, fast electrons) and dust grain properties. In contrast to the colour temperature of the warm dust, the f350/f500 index sensitive to the cold dust decreases with star formation and increases with metallicity, suggesting an overabundance of cold dust or an emissivity parameter beta, Accepted for publication on A&A, Herschel special issue
Published: 2010
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21. The central region of spiral galaxies as seen by Herschel: M 81, M 99, and M 100

Author: George J. Bendo, Haley Louise Gomez, B. O'Halloran, Werner W. Zeilinger, S. J. Oliver, N. Castro-Rodriguez, Gillian S. Wright, Herve Wozniak, Michael Pohlen, Walter Kieran Gear, Diane Cormier, E. E. Rigby, Andreas Papageorgiou, H. Roussel, Matthew Joseph Griffin, Louis Levenson, David L. Clements, P. Chanial, A. Boselli, Luca Cortese, Steve Eales, M. Bradford, Laure Ciesla, Matthew Smith, Jason Glenn, Sacha Hony, Benjamin L. Schulz, Nanyao Y. Lu, Mattia Vaccari, M. Symeonidis, N. Sacchi, Stéphane Charlot, Christine D. Wilson, L. Vigroux, Asantha Cooray, K. Okumura, A. Rykala, Jamie Stevens, T. J. Parkin, Maarten Baes, Maud Galametz, I. Perez-Fournon, Sundar Srinivasan, Luigi Spinoglio, Maximilien R. P. Schirm, K. G. Isaak, E. Dwek, P. Panuzzo, M. J. Barlow, Jonathan Ivor Davies, Marc Sauvage, Frédéric Galliano, N. Rangwala, J. J. Bock, M. J. Page, Robbie Richard Auld, D. Elbaz, M. Trichas, V. Buat, and S. C. Madden
Subjects: Brightness, Cosmology and Nongalactic Astrophysics (astro-ph.CO), nuclei [galaxies], FOS: Physical sciences, galaxies [submillimeter], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies [infrared], 01 natural sciences, Central region, Bulge, 0103 physical sciences, fundamental parameters [galaxies], DUST EMISSION, 010303 astronomy & astrophysics, Image resolution, Astrophysics::Galaxy Astrophysics, Physics, Spiral galaxy, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Wavelength, spiral [galaxies], Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: With appropriate spatial resolution, images of spiral galaxies in thermal infrared (~10 micron and beyond) often reveal a bright central component, distinct from the stellar bulge, superimposed on a disk with prominent spiral arms. ISO and Spitzer studies have shown that much of the scatter in the mid-infrared colors of spiral galaxies is related to changes in the relative importance of these two components, rather than to other modifications, such as the morphological type or star formation rate, that affect the properties of the galaxy as a whole. With the Herschel imaging capability from 70 to 500 micron, we revisit this two-component approach at longer wavelengths, to see if it still provides a working description of the brightness distribution of galaxies, and to determine its implications on the interpretation of global far-infrared properties of galaxies., 5 pages, 2 figures, accepted for the A&A Herschel Special Issue
Published: 2010

22. SPIRE imaging of M 82: Cool dust in the wind and tidal streams

Author: Laure Ciesla, Asantha Cooray, Steve Eales, Luigi Spinoglio, Walter Kieran Gear, P. Chanial, Diane Cormier, E. E. Rigby, B. O'Halloran, Frédéric Galliano, Stéphane Charlot, D. L. Clements, I. Perez-Fournon, Robbie Richard Auld, A. Rykala, Maximilien R. P. Schirm, D. Elbaz, S. Hony, Luca Cortese, K. G. Isaak, E. Dwek, Benjamin L. Schulz, Jonathan Ivor Davies, J. J. Bock, Christine D. Wilson, T. J. Parkin, Louis Levenson, M. Pohlen, M. J. Page, Werner W. Zeilinger, V. Buat, Marc Sauvage, N. Rangwala, M. Trichas, Andreas Papageorgiou, Maarten Baes, N. Sacchi, Sundar Srinivasan, Nanyao Y. Lu, Matthew Joseph Griffin, P. Panuzzo, M. Symeonidis, Jamie Stevens, Mattia Vaccari, M. J. Barlow, G. J. Bendo, L. Vigroux, M. W. L. Smith, M. Bradford, N. Castro-Rodriguez, S. C. Madden, H. Roussel, Gillian S. Wright, Herve Wozniak, Jason Glenn, Seb Oliver, M. Galametz, K. Okumura, A. Boselli, Haley Louise Gomez, 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), 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), 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), Instituto de Astrofisica de Canarias (IAC), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Observational Cosmology Lab, NASA Goddard Space Flight Center (GSFC), School of Physics and Astronomy [Cardiff], Cardiff University, University of Patras [Patras], Center for Astrophysics and Space Astronomy [Boulder] (CASA), University of Colorado [Boulder], Astrophysics Group, Blackett Laboratory, Imperial College London-Imperial College London, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Department of Physics and Astronomy [UCL London], University College of London [London] (UCL), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), SPIRE, HERSCHEL, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-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), University of Patras, Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), 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'Etudes Spatiales ( CNES ), Instituto de Astrofisica de Canarias ( IAC ), Conservatoire National des Arts et Métiers - Haute Normandie ( CNAM Haute-Normandie ), Conservatoire National des Arts et Métiers [CNAM] ( CNAM ), European Southern Observatory ( ESO ), NASA Goddard Space Flight Center ( GSFC ), School of Physics & Astronomy [Cardiff], Center for Astrophysics and Space Astronomy [Boulder] ( CASA ), University of Colorado Boulder [Boulder], Institut de Physique de Rennes ( IPR ), Université de Rennes 1 ( UR1 ), Université de Rennes ( UNIV-RENNES ) -Université de Rennes ( UNIV-RENNES ) -Centre National de la Recherche Scientifique ( CNRS ), Centre de Recherche Astrophysique de Lyon ( CRAL ), École normale supérieure - Lyon ( ENS Lyon ) -Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), University College of London [London] ( UCL ), Jet Propulsion Laboratory ( JPL ), NASA-California Institute of Technology ( CALTECH ), School of Physics and Astronomy, Cardiff University, Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-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: SUPER STAR-CLUSTERS, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, galaxies: starburst, Astrophysics, STREAMS, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Coincident, 0103 physical sciences, evolution, galaxies: interactions, Astrophysics::Solar and Stellar Astrophysics, COLD DUST, 14. Life underwater, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, QB, Physics, infrared: ISM, [PHYS]Physics [physics], [ PHYS ] Physics [physics], Mass distribution, starburst [galaxies], interactions [galaxies], 010308 nuclear & particles physics, extinction, GALAXY M 82, ISM [infrared], Astronomy and Astrophysics, Galaxy, Interstellar medium, Spire, Physics and Astronomy, OUTFLOWS, GAS, 13. Climate action, Space and Planetary Science, STARBURST, Polar, Halo, dust, Astrophysics::Earth and Planetary Astrophysics, EMISSION, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: M82 is a unique representative of a whole class of galaxies, starbursts with superwinds, in the Very Nearby Galaxy Survey with Herschel. In addition, its interaction with the M81 group has stripped a significant portion of its interstellar medium from its disk. SPIRE maps now afford better characterization of the far-infrared emission from cool dust outside the disk, and sketch a far more complete picture of its mass distribution and energetics than previously possible. They show emission coincident in projection with the starburst wind and in a large halo, much more extended than the PAH band emission seen with Spitzer. Some complex substructures coincide with the brightest PAH filaments, and others with tidal streams seen in atomic hydrogen. We subtract the far-infrared emission of the starburst and underlying disk from the maps, and derive spatially-resolved far-infrared colors for the wind and halo. We interpret the results in terms of dust mass, dust temperature, and global physical conditions. In particular, we examine variations in the dust physical properties as a function of distance from the center and the wind polar axis, and conclude that more than two thirds of the extraplanar dust has been removed by tidal interaction, and not entrained by the starburst wind., accepted in A&A Herschel special issue
Published: 2010
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23. The dust morphology of the elliptical Galaxy M86 with SPIRE

Author: Maud Galametz, Jamie Stevens, Stéphane Charlot, D. L. Clements, Steve Eales, M. J. Page, B. O'Halloran, Laure Ciesla, Mattia Vaccari, Haley Louise Gomez, Maarten Baes, Walter Kieran Gear, Sundar Srinivasan, Jonathan Ivor Davies, Asantha Cooray, M. J. Barlow, Diane Cormier, Andreas Papageorgiou, P. Panuzzo, Marc Sauvage, Benjamin L. Schulz, P. Chanial, M. W. L. Smith, E. E. Rigby, I. Perez-Fournon, Werner W. Zeilinger, Louis Levenson, E. Dwek, Matthew Joseph Griffin, M. Pohlen, A. Boselli, Christine D. Wilson, Gillian S. Wright, S. di Serego Alighieri, M. Bradford, L. Vigroux, Herve Wozniak, Nanyao Y. Lu, Maximilien R. P. Schirm, S. Hony, M. Symeonidis, K. G. Isaak, A. Rykala, Jason Glenn, V. Buat, S. J. Oliver, J. J. Bock, K. Okumura, N. Castro-Rodriguez, N. Sacchi, H. Roussel, G. J. Bendo, Luigi Spinoglio, T. J. Parkin, Luca Cortese, S. C. Madden, N. Rangwala, Frédéric Galliano, M. Trichas, Robbie Richard Auld, D. Elbaz, 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), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, M86, FOS: Physical sciences, galaxies: ellipticals and lenticular, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: individual: M 86, Central region, cD, Coincident, Ionization, Astrophysics::Solar and Stellar Astrophysics, MULTIPHASE INTERSTELLAR-MEDIUM, COLD DUST, ISM [submillimeter], NGC-4406, Astrophysics::Galaxy Astrophysics, QB, Physics, Solar mass, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], extinction, individual: M 86 [galaxies], Spire (mollusc), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, ellipticals and lenticular [galaxies], VIRGO CLUSTER, Dust lane, M-86, Physics and Astronomy, GAS, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Elliptical galaxy, submillimeter: ISM, dust, Astrophysics::Earth and Planetary Astrophysics, EMISSION, Dust emission, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present Herschel-SPIRE observations at 250-500um of the giant elliptical galaxy M86 and examine the distribution of the resolved cold dust emission and its relation with other galactic tracers. The SPIRE images reveal three dust components: emission from the central region; a dust lane extending north-south; and a bright emission feature 10kpc to the south-east. We estimate that approximately 10^6 solar masses of dust is spatially coincident with atomic and ionized hydrogen, originating from stripped material from the nearby spiral NGC4438 due to recent tidal interactions with M86. The gas-to-dust ratio of the cold gas component ranges from ~20-80. We discuss the different heating mechanisms for the dust features., Comment: 5 pages and 3 figures, accepted for A & A Herschel special issue
Published: 2010
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24. Mapping the interstellar medium in galaxies with Herschel/SPIRE

Author: Werner W. Zeilinger, Jamie Stevens, L. Vigroux, Maud Galametz, Helene Roussel, David L. Clements, Jonathan Ivor Davies, Luca Cortese, Marc Sauvage, N. Lu, Walter Kieran Gear, B. O'Halloran, Matthew Joseph Griffin, Herve Wozniak, Eli Dwek, Diane Cormier, Ismael Perez-Fournon, M. J. Barlow, E. E. Rigby, Christine D. Wilson, Naseem Rangwala, Maximilien R. P. Schirm, Michael Pohlen, Andreas Papageorgiou, Alessandro Boselli, Mat Page, Sacha Hony, V. Buat, Jason Glenn, Pierre Chanial, Gillian S. Wright, Maarten Baes, L. R. Levenson, Haley Louise Gomez, N. Sacchi, George J. Bendo, Matthew Smith, Mattia Vaccari, Sundar Srinivasan, Benjamin L. Schulz, A. Cooray, M. Symeonidis, Kate Gudrun Isaak, James J. Bock, Pasquale Panuzzo, A. Rykala, Seb Oliver, Stephane Charlot, Robbie Richard Auld, T. J. Parkin, Stephen Anthony Eales, Laure Ciesla, Markos Trichas, Suzanne C. Madden, M. Bradford, Frédéric Galliano, Koryo Okumura, L. Spinoglio, N. Castro-Rodriguez, D. Elbaz, 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), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, galaxies: spiral, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], extinction, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, ISM: abundances, Interstellar medium, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics::Earth and Planetary Astrophysics, dust, Astrophysics::Galaxy Astrophysics, galaxies: ISM, QB, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The standard method of mapping the interstellar medium in a galaxy, by observing the molecular gas in the CO 1-0 line and the atomic gas in the 21-cm line, is largely limited with current telescopes to galaxies in the nearby universe. In this letter, we use SPIRE observations of the galaxies M99 and M100 to explore the alternative approach of mapping the interstellar medium using the continuum emission from the dust. We have compared the methods by measuring the relationship between the star-formation rate and the surface density of gas in the galaxies. We find the two methods give relationships with a similar dispersion, confirming that observing the continuum emission from the dust is a promising method of mapping the interstellar medium in galaxies., Astronomy and Astrophysics in press
Published: 2010
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25. Herschel photometric observations of the nearby low metallicity irregular galaxy NGC 6822

Author: N. Sacchi, George J. Bendo, Mat Page, Ismael Perez-Fournon, Michael Pohlen, Alessandro Boselli, L. R. Levenson, Eli Dwek, Benjamin L. Schulz, B. O'Halloran, A. Cooray, Laure Ciesla, Maud Galametz, Pierre Chanial, M. J. Barlow, A. Rykala, Pasquale Panuzzo, Maximilien R. P. Schirm, Walter Kieran Gear, Naseem Rangwala, Jason Glenn, V. Buat, Jamie Stevens, Jonathan Ivor Davies, Marc Sauvage, Christine D. Wilson, Diane Cormier, Markos Trichas, N. Lu, Herve Wozniak, E. E. Rigby, Maarten Baes, Frédéric Galliano, Werner W. Zeilinger, Andreas Papageorgiou, Seb Oliver, Robbie Richard Auld, D. Elbaz, Matthew Smith, Haley Louise Gomez, James J. Bock, L. Spinoglio, Stephane Charlot, Kate Gudrun Isaak, Sacha Hony, Gillian S. Wright, Mattia Vaccari, T. J. Parkin, Stephen Anthony Eales, Matthew Joseph Griffin, N. Castro-Rodriguez, M. Symeonidis, M. Bradford, Koryo Okumura, S. Sundar, Suzanne C. Madden, Helene Roussel, David L. Clements, Luca Cortese, L. Vigroux, 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), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: GRAPHITE, Cosmology and Nongalactic Astrophysics (astro-ph.CO), dwarf [galaxies], Metallicity, INFRARED-EMISSION, Carbon dust, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, AMORPHOUS-CARBON, Emissivity, Astrophysics::Solar and Stellar Astrophysics, Surface brightness, education, Astrophysics::Galaxy Astrophysics, QB, Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ISM [galaxies], Star formation, Astronomy and Astrophysics, galaxies: dwarf, STAR-FORMATION HISTORY, Galaxy, galaxies: photometry, Spire, Physics and Astronomy, [SDU]Sciences of the Universe [physics], Space and Planetary Science, photometry [galaxies], Astrophysics::Earth and Planetary Astrophysics, Irregular galaxy, galaxies: ISM, INTERSTELLAR DUST, Astrophysics - Cosmology and Nongalactic Astrophysics, LOCAL GROUP, SPITZE
Abstract: We present the first Herschel PACS and SPIRE images of the low-metallicity galaxy NGC6822 observed from 70 to 500 mu and clearly resolve the HII regions with PACS and SPIRE. We find that the ratio 250/500 is dependent on the 24 mu surface brightness in NGC6822, which would locally link the heating processes of the coldest phases of dust in the ISM to the star formation activity. We model the SEDs of some regions HII regions and less active regions across the galaxy and find that the SEDs of HII regions show warmer ranges of dust temperatures. We derive very high dust masses when graphite is used in our model to describe carbon dust. Using amorphous carbon, instead, requires less dust mass to account for submm emission due to its lower emissivity properties. This indicates that SED models including Herschel constraints may require different dust properties than commonly used., Comment: Accepted for publication in the A&A Herschel first results Special Issue
Published: 2010
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26. Herschel-SPIRE observations of the disturbed galaxy NGC 4438

Author: Laure Ciesla, Pierre Chanial, James J. Bock, Stephane Charlot, B. O'Halloran, Michael Pohlen, Jonathan Ivor Davies, Naseem Rangwala, M. Bradford, Andreas Papageorgiou, V. Buat, Markos Trichas, Koryo Okumura, Maud Galametz, George J. Bendo, Marc Sauvage, N. Lu, Robbie Richard Auld, David Elbaz, M. Griffin, Mattia Vaccari, Walter Kieran Gear, L. R. Levenson, S. C. Madden, C. D. Wilson, Herve Wozniak, Pasquale Panuzzo, Werner W. Zeilinger, Helene Roussel, David L. Clements, N. Sacchi, Stephen Anthony Eales, Sundar Srinivasan, Diane Cormier, Jamie Stevens, Luca Cortese, N. Castro-Rodriguez, Kate Gudrun Isaak, Frédéric Galliano, E. E. Rigby, M. Symeonidis, Sacha Hony, Ismael Perez-Fournon, Gillian S. Wright, Maximilien R. P. Schirm, Alessandro Boselli, T. J. Parkin, Jason Glenn, M. J. Page, L. Spinoglio, Seb Oliver, Haley Louise Gomez, L. Vigroux, A. Rykala, Eli Dwek, Bernhard Schulz, Maarten Baes, A. Cooray, Matthew Smith, 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), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: individual: NGC4438 [galaxies], Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, DUST, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies [infrared], infrared: galaxies, POLYCYCLIC AROMATIC-HYDROCARBONS, ABUNDANCES, VIEW, Cluster (physics), Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, galaxies: individual: NGC 4438, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], extinction, Hydrogen molecule, Astronomy and Astrophysics, VIRGO CLUSTER, Virgo Cluster, Galaxy, Spire, Physics and Astronomy, NGC 4438, GAS, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics::Earth and Planetary Astrophysics, dust, EMISSION, galaxies: evolution, SYSTEM, NGC-4438, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present Herschel-SPIRE observations of the perturbed galaxy NGC4438 in the Virgo cluster. These images reveal the presence of extra-planar dust up to ~4-5 kpc away from the galaxy's disk. The dust closely follows the distribution of the stripped atomic and molecular hydrogen, supporting the idea that gas and dust are perturbed in a similar fashion by the cluster environment. Interestingly, the extra-planar dust lacks a warm temperature component when compared to the material still present in the disk, explaining why it was missed by previous far-infrared investigations. Our study provides evidence for dust stripping in clusters of galaxies and illustrates the potential of Herschel data for our understanding of environmental effects on galaxy evolution., Comment: 5 pages, 2 figures. Accepted for publication on the A&A Herschel Special Issue
Published: 2010
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27. Herschel photometric observations of the low metallicity dwarf galaxy NGC 1705

Author: Asantha Cooray, M. J. Barlow, P. Chanial, George J. Bendo, Ismael Perez-Fournon, M. Trichas, E. Dwek, Gillian S. Wright, Herve Wozniak, Walter Kieran Gear, Robbie Richard Auld, J. J. Bock, L. Vigroux, Jason Glenn, D. Elbaz, Christine D. Wilson, Alessandro Boselli, Diane Cormier, Benjamin L. Schulz, Maarten Baes, Frédéric Galliano, Stephen Anthony Eales, Jonathan Ivor Davies, Laure Ciesla, N. Sacchi, E. E. Rigby, N. Castro-Rodriguez, Michael Pohlen, Jamie Stevens, Seb Oliver, Suzanne C. Madden, Marc Sauvage, Matthew Smith, P. Panuzzo, Matthew Joseph Griffin, L. Spinoglio, A. Rykala, M. Bradford, Haley Louise Gomez, N. Rangwala, Mat Page, K. Okumura, Helene Roussel, David L. Clements, Luca Cortese, Maximilien R. P. Schirm, V. Buat, K. G. Isaak, B. O'Halloran, Mattia Vaccari, Andreas Papageorgiou, Maud Galametz, Werner W. Zeilinger, Sacha Hony, Stéphane Charlot, S. Sundar, Louis Levenson, Nanyao Y. Lu, M. Symeonidis, T. J. Parkin, 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: Cosmology and Nongalactic Astrophysics (astro-ph.CO), dwarf [galaxies], Metallicity, FOS: Physical sciences, Astrophysics, HII-REGIONS, 01 natural sciences, Photometry (optics), POLYCYCLIC AROMATIC-HYDROCARBONS, AMORPHOUS-CARBON, 0103 physical sciences, evolution, Emissivity, 010303 astronomy & astrophysics, QB, Dwarf galaxy, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, extinction, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Wavelength, Star cluster, SPECTRAL ENERGY-DISTRIBUTION, Physics and Astronomy, SPINNING DUST GRAINS, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), STARBURST, Spectral energy distribution, MILKY-WAY, dust, NGC-1705, EMISSION, INTERSTELLAR DUST, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present Herschel SPIRE and PACS photometeric observations of the low metallicity (Z ~ 0.35 solar) nearby dwarf galaxy, NGC 1705, in six wavelength bands as part of the Dwarf Galaxy Survey guaranteed time Herschel Key Program. We confirm the presence of two dominant circumnuclear IR-bright regions surrounding the central super star cluster that had been previously noted at mid-IR wavelengths and in the sub-mm by LABOCA. On constructing a global spectral energy distribution using the SPIRE and PACS photometry, in conjunction with archival IR measurements, we note the presence of an excess at sub-mm wavelengths. This excess suggests the presence of a significant cold dust component within NGC 1705 and was modeled as an additional cold component in the SED. Although alternative explanations for the sub-mm excess beyond 350 microns, such as changes to the dust emissivity cannot be ruled out, the most likely explanation for the observed submillimetre excess is that of an additional cold dust component., 5 pages, 2 figures, accepted for publication in A&A (Herschel special issue)
Published: 2010
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28. New Science Opportunities Offered by MUSE

Author: Marcella Carollo, Luca Pasquini, J. Gerssen, Herve Wozniak, L. Parès, A. Pecontal, Jean-Pierre Dubois, Johan Kosmalski, Stefan Ströbele, L. Capoani, R. Pello, Antonio Manescau, Christian Monstein, G. Gallou, Cyril Petit, Aurélien Jarno, M. Dupieux, B. Guiderdoni, Joop Schaye, Peter M. Weilbacher, D. Hofmann, T. Contini, Pierre Ferruit, Stefan Dreizler, Marc François, J. L. Lizon, E. Emsellem, Lutz Wisotzki, Florence Laurent, Patrick Caillier, B. Delabre, J. Moultaka, Harald Nicklas, Roland Reiss, Andreas Kelz, A. Remillieux, C. Koehler, M. Loupias, Matthias Steinmetz, Martin Roth, S. Brau-Nogué, G. Hansali, J. P. Dupin, S. J. Lilly, Edgard Renault, E. Daguisé, Wolfram Kollatschny, M. Franx, Remko Stuik, Svend-Marian Bauer, and Roland Bacon
Subjects: Physics, Narrow-band imaging, Stellar population, Astronomy
Published: 2009
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29. IMAGES-III: The evolution of the Near-Infrared Tully-Fisher relation over the last 6 Gyr

Author: Joel Vernet, Nicole P. H. Nesvadba, L. Chemin, B. Guiderdoni, P. Amram, F. Hammer, S. di Serego Alighieri, Benoit Epinat, C. J. Cesarsky, Lucia Pozzetti, C. D. Ravikumar, Isaura Fuentes-Carrera, Yun-Feng Liang, C. Balkowski, M. D. Lehnert, A. Rawat, Helmut Dannerbauer, Goeran Oestlin, Ajit K. Kembhavi, Mathieu Puech, Herve Wozniak, Y. Yang, Hector Flores, Benoit Neichel, D. Vergani, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: galaxies: spiral, Field (physics), FOS: Physical sciences, Angular velocity, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Tully–Fisher relation, Rotation, 01 natural sciences, Luminosity, galaxies: high-redshift, 0103 physical sciences, Emission spectrum, 010303 astronomy & astrophysics, galaxies: kinematics and dynamics, Astrophysics::Galaxy Astrophysics, Physics, galaxies, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, interactions, galaxies: general, Galaxy, Stars, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution
Abstract: Using the multi-integral field spectrograph GIRAFFE at VLT, we have derived the K-band Tully-Fisher relation (TFR) at z~0.6 for a representative sample of 65 galaxies with emission lines. We confirm that the scatter in the z~0.6 TFR is caused by galaxies with anomalous kinematics, and find a positive and strong correlation between the complexity of the kinematics and the scatter that they contribute to the TFR. Considering only relaxed-rotating disks, the scatter, and possibly also the slope of the TFR, do not appear to evolve with z. We detect an evolution of the K-band TFR zero point between z~0.6 and z=0, which, if interpreted as an evolution of the K-band luminosity of rotating disks, would imply that a brightening of 0.66+/-0.14 mag occurs between z~0.6 and z=0. Any disagreement with the results of Flores et al. (2006) are attributed to both an improvement of the local TFR and the more detailed accurate measurement of the rotation velocities in the distant sample. Most of the uncertainty can be explained by the relatively coarse spatial-resolution of the kinematical data. Because most rotating disks at z~0.6 are unlikely to experience further merging events, one may assume that their rotational velocity does not evolve dramatically. If true, our result implies that rotating disks observed at z~0.6 are rapidly transforming their gas into stars, to be able to double their stellar masses and be observed on the TFR at z=0. The rotating disks observed are indeed emission-line galaxies that are either starbursts or LIRGs, which implies that they are forming stars at a high rate. Thus, a significant fraction of the rotating disks are forming the bulk of their stars within 6 to 8 Gyr, in good agreement with former studies of the evolution of the M-Z relation., 17 pages, 11 figures, accepted for publication in A&A. v2 taking into account comments from language editor
Published: 2008
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30. IMAGES II. A surprisingly low fraction of undisturbed rotating spiral disks at z~0.6: The morpho-kinematical relation 6 Gyrs ago

Author: Herve Wozniak, A. Rawat, Hector Flores, M. Lehnert, Yanchun Liang, I. Fuentes-Carrera, Nicole P. H. Nesvadba, Joel Vernet, Benoit Neichel, C. D. Ravikumar, Catherine Cesarsky, M. Puech, D. Vergani, B. Guiderdoni, Lucia Pozzetti, Göran Östlin, C. Balkowski, Helmut Dannerbauer, Francois Hammer, Yanbin Yang, S. di Serego Alighieri, R. Delgado, P. Amram, Ajit Kembhavi, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), 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), Observatoire de Paris - Site de Paris (OP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Inter-University Centre for Astronomy and Astrophysics [Pune] (IUCAA), National Astronomical Observatories, Chinese Academy of Sciences, Chinese Academy of Sciences [Beijing] (CAS), Stockholm Observatory Department of Astronomy, Stockholm University, INAF - Osservatorio Astronomico di Capodimonte (OAC), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Bologna (OABO), Space Telescope European Coordinating Facility (STECF), Space Telescope European Coordinating Facility, INAF - Osservatorio Astrofisico di Arcetri (OAA), Beaussier, Catherine, Physique des Galaxies et Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, European Southern Observatory (ESO), Inter-University Centre for Astronomy and Astrophysics (IUCAA), IFARHU-SENACYT, Technological University of Panama, National Astronomical Observatoires-CAS, Stockholm Observatory, AlbaNova University Center, INAF-Osservatorio Astronomico di Bologna (OABO), Department of Physics, University of Calicut, INAF-Osservatorio Astrofisico di Arcetri (INAF-OAA), Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), 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), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), 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: FOS: Physical sciences, Kinematics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Peculiar galaxy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Galaxy formation and evolution, 10. No inequality, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, biology, 010308 nuclear & particles physics, Gas supply, Astrophysics (astro-ph), Astronomy and Astrophysics, Morpho, biology.organism_classification, Galaxy, Accretion (astrophysics), Stars, Space and Planetary Science, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We present a first combined analysis of the morphological and dynamical properties for the Intermediate MAss Galaxy Evolution Sequence (IMAGES) sample. It is a representative sample of 52 z~0.6 galaxies with Mstell from 1.5 to 15 10^10Msun and possessing 3D resolved kinematics and HST deep imaging in at least two broad band filters. We aim at evaluate robustly the evolution of rotating spirals since z~0.6, as well as to test the different schemes for classifying galaxies morphologically. We used all the information provided by multi-band images, color maps and 2 dimensional light fitting to assign to each object a morphological class. We divided our sample between spiral disks, peculiar objects, compact objects and mergers. Using our morphological classification scheme, 4/5 of identified spirals are rotating disks and more than 4/5 of identified peculiar galaxies show complex kinematics, while automatic classification methods such as Concentration-Asymmetry and GINI-M20 severely overestimate the fraction of relaxed disk galaxies. Using this methodology, we find that the fraction of rotating spirals has increased by a factor ~ 2 during the last 6 Gyrs, a much higher fraction that found previously based on morphologies alone. These rotating spiral disks are forming stars very rapidly, doubling their stellar masses over the last 6 Gyrs, while most of their stars have been formed few Gyrs earlier, which reveals the presence of a large gas supply. Because they are likely the progenitors of local spirals, we can conjecture how their properties are evolving. Their disks show some evidence for an inside-out growth and the gas supply/accretion is not made randomly as the disk need to be stable in order to match the local disk properties., Typos corrected, reference added
Published: 2008
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31. The IVOA in 2007: Assessment, Future Roadmap Version 1.00

Author: François Ochsenbein, Herve Wozniak, Keith Noddle, Bob Hanisch, Rob Seaman, Mark Allen, Mark Taylor, Gerard Lemson, Aurélien Stébé, Matthew J. Graham, Dave deYoung, Yuji Shirasaki, Mireille Louys, Ray Plante, Markus Dolensky, Roy Williams, Françoise Genova, Sebastien Derriere, Petdro Osuna, Christophe Arviset, Anita M. S. Richards, and Andrea Preite Martinez
Published: 2007
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32. The distribution of stellar population age in galactic bars

Author: Herve Wozniak, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Wozniak, Hervé, École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: Stellar population, Bar (music), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Spatial distribution, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, Resonance (particle physics), 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, [SDU.ASTR.CO] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Astrophysics (astro-ph), Astronomy and Astrophysics, Galaxy, Population model, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], [SDU.ASTR.GA] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Lindblad resonance
Abstract: Recent analysis of stellar populations in barred galaxies have focused on the spatial distribution of stellar population ages and metallicities. However, barred galaxies are complex objects where dynamical instabilities play a leading role in shaping any spatial distribution. The age distribution of stellar populations should thus be analyzed from the two points of view of stellar population evolution and dynamical secular evolution. Chemodynamical simulations of single barred galaxies with simple but realistic star formation and feedback recipes are used to produce face-on mass-weighted maps of stellar population ages. Luminosity-weighted maps in V-band are also displayed after calibrating the simulation with mass-to-light ratios provided by a synthesis population model. It is shown that inside a stellar bar two persistent diametrically opposed regions display a mean age lower than the surrounding average. These two low-age regions are due to the accumulation of young stellar populations trapped on elliptical-like orbits along the bar, near the ultra-harmonic resonance. Age gradients along the bar major-axis are comparable to recent observations. Another low-age region is the outer ring located near the Outer Lindblad Resonance, but the presence and strength of this structure is very time-dependent., Comment: Accepted for publication in A&A Letters, 4 pages, 4 figures. Fig.3 is available at full resolution at: http://cral.univ-lyon1.fr/herve.wozniak/Articles/age_bar_6.eps.gz
Published: 2007

33. New spectroscopic redshifts from the CDFS and a test of the cosmological relevance of the GOODS-South field

Author: Yun-Feng Liang, Helmut Dannerbauer, A. Cimatti, Francoise Combes, P. Amram, B. Guiderdoni, M. D. Lehnert, Hector Flores, C. J. Cesarsky, D. Vergani, D. Proust, Mathieu Puech, E. Daddi, D. Elbaz, Ajit K. Kembhavi, S. di Serego Alighieri, C. D. Ravikumar, F. Hammer, Paolo Cassata, Lucia Pozzetti, Chantal Balkowski, Denis Burgarella, Herve Wozniak, A. Rawat, Joel Vernet, Xianzhong Zheng, Ravikumar C. D., Puech M., Flores H., Proust D., Hammer F., Lehnert M., Rawat A., Amram P., Balkowski C., Burgarella D., Cassata P., Cesarsky C., Cimatti A., Combes F., Daddi E., Dannerbauer H., di Serego Alighieri S., Elbaz D., Guiderdoni B., Kembhavi A., Liang Y. C., Pozzetti L., Vergani D., Vernet J., Wozniak H., Zheng X. Z., Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Physique des Galaxies et Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestriche Physik (MPE), Inter-University Centre for Astronomy and Astrophysics (IUCAA), 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 Padova = University of Padua (Unipd), European Southern Observatory (ESO), INAF-Osservatorio Astrofisico di Arcetri (INAF-OAA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Galaxies et cosmologie, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), National Optical Astronomy Observatory, Tucson (NOAO), 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), Max-Planck-Institut für Astronomie (MPIA), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), National Astronomical Observatoires-CAS, and INAF-Osservatorio Astronomico di Bologna (OABO)
Subjects: 010504 meteorology & atmospheric sciences, Stellar mass, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Surveys, 01 natural sciences, Luminosity, Galaxies: distances and redshifts, Cosmology: large scale structure of Universe, Cosmology: observations, Galaxies: evolution, Galaxies: high-redshift, Astronomy and Astrophysics, Space and Planetary Science, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Photometric redshift, Physics, Star formation, Cosmic variance, Galaxy, Chandra Deep Field South, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: (Abbrev.) This paper prepares a series of papers analysing the Intermediate MAss Galaxy Evolution Sequence (IMAGES) up to z=1. Intermediate mass galaxies (MJ
Published: 2007

34. A New Chemodynamical Tool to Study the Evolution of Galaxies in the Local Universe: a Quick and Accurate Numerical Technique to Compute the Gas Cooling Rate for any Chemical Composition

Author: Nicolas Champavert and Herve Wozniak
Subjects: Physics, media_common.quotation_subject, ComputerApplications_GENERAL, Numerical technique, Gas cooling, Astrophysics, Chemical composition, ComputingMilieux_MISCELLANEOUS, Universe, Galaxy, media_common
Abstract: We have developed a quick and accurate numerical tool to compute gas cooling whichever its chemical composition.
Published: 2007
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35. Probing unexplored territories with MUSE: a second generation instrument for the VLT

Author: E. Popow, Antonio Manescau, Martin M. Roth, Harald Nicklas, Thierry Contini, Roser Pello, L. Capoani, Patrick Caillier, Remko Stuik, Didier Boudon, Christian Monstein, Stefan Dreizler, Luca Pasquini, Marijn Franx, Julien Devriendt, J. Gerssen, Herve Wozniak, Matthias Steinmetz, L. Parès, Aurélien Jarno, P. Ferruit, Richard M. McDermid, Eric Emsellem, Roland Bacon, P. T. de Zeeuw, Andreas Quirrenbach, Roland Reiss, T. Hahn, G. Soucail, Stefan Stroebele, P. Boehm, Peter M. Weilbacher, C. Petit, Bernard Delabre, M. Dupieux, Simon J. Lilly, C. M. Carollo, Florence Laurent, Johan Kosmalski, B. Guiderdoni, Jean-Louis Lizon, Svend M. Bauer, Eric Daguisé, Emmanuel Pecontal, Andreas Kelz, J.-P. Picat, S. Lynn, Joop Schaye, C. Koehler, Arlette Pécontal-Rousset, Wolfram Kollatschny, Edgard Renault, J. P. Dupin, D. Dalle, D. Hofmann, Jean-Pierre Dubois, G. Gallou, S. Brau-Nogué, Magali Loupias, and N. Champavert
Subjects: Physics, Supermassive black hole, Young stellar object, Milky Way, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Multi Unit Spectroscopic Explorer, Galaxy, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Adaptive optics, Spectrograph, Astrophysics::Galaxy Astrophysics
Abstract: The Multi Unit Spectroscopic Explorer (MUSE) is a second-generation VLT panoramic integral-field spectrograph under preliminary design study. MUSE has a field of 1x1 arcmin**2 sampled at 0.2x0.2 arcsec**2 and is assisted by the VLT ground layer adaptive optics ESO facility using four laser guide stars. The simultaneous spectral range is 465-930 nm, at a resolution of R~3000. MUSE couples the discovery potential of a large imaging device to the measuring capabilities of a high-quality spectrograph, while taking advantage of the increased spatial resolution provided by adaptive optics. This makes MUSE a unique and tremendously powerful instrument for discovering and characterizing objects that lie beyond the reach of even the deepest imaging surveys. MUSE has also a high spatial resolution mode with 7.5x7.5 arcsec**2 field of view sampled at 25 milli-arcsec. In this mode MUSE should be able to obtain diffraction limited data-cubes in the 600-930 nm wavelength range. Although the MUSE design has been optimized for the study of galaxy formation and evolution, it has a wide range of possible applications; e.g. monitoring of outer planets atmosphere, environment of young stellar objects, super massive black holes and active nuclei in nearby galaxies or massive spectroscopic surveys of stellar fields in the Milky Way and nearby galaxies., Astronomical Telescopes and Instrumentation, SPIE 6265 Orlando 24-31May 2006 9 pages
Published: 2006

36. The length of stellar bars in SB galaxies and N-body simulations

Author: Leo Michel-Dansac and Herve Wozniak
Subjects: Physics, Bar (music), Star formation, Astrophysics (astro-ph), Phase (waves), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Stars, symbols.namesake, Fourier transform, Space and Planetary Science, symbols, Astrophysics::Solar and Stellar Astrophysics, Surface brightness, Fourier series, Astrophysics::Galaxy Astrophysics
Abstract: We have investigated the accuracy and reliability of six methods used to determine the length of stellar bars in galaxies or N-body simulations. All these methods use ellipse fitting and Fourier decomposition of the surface brightness. We have applied them to N-body simulations that include stars, gas, star formation, and feedback. Stellar particles were photometrically calibrated to make B and K-band mock images. Dust absorption is also included. We discuss the advantages and drawbacks of each method, the effects of projection and resolution, as well as the uncertainties introduced by the presence of dust. The use of N-body simulations allows us to compare the location of Ultra Harmonic Resonance (UHR or 4/1) and corotation (CR) with measured bar lengths. We show that the minimum of ellipticity located just outside the bulk of the bar is correlated with the corotation, whereas the location of the UHR can be approximated using the phase of the fitted ellipses or the phase of the m=2 Fourier development of the surface brightness. We give evidence that the classification of slow/fast bars, based on the ratio R = Rcr/Rbar could increase from 1 (fast bar) to 1.4 (slow bar) just by a change of method. We thus conclude that one has to select the right bar-length estimator depending on the application, since these various estimators do not define the same physical area., Major revision, A&A in press
Published: 2005

37. On the relevance of the Tremaine-Weinberg method applied to H-alpha velocity field.Pattern speeds determination in M100 (NGC 4321)

Author: Claude Carignan, Oscar F. Hernández, L. Chemin, Olivier Daigle, Herve Wozniak, P. Amram, Département de Physique [Montréal], Université de Montréal (UdeM), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), and Beaussier, Catherine
Subjects: Physics, 010504 meteorology & atmospheric sciences, Bar (music), Star formation, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Virgo Cluster, Galaxy, Dark matter halo, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, 0103 physical sciences, Vector field, H-alpha, 010303 astronomy & astrophysics, Spiral, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract: The relevance of the Tremaine-Weinberg (TW) method is tested to measure the bar, spiral and inner structure pattern speeds using a gaseous velocity field. The TW method is applied to various simulated barred galaxies in order to demonstrate its validity in seven different configurations, including star formation or/and dark matter halo. The reliability of the different physical processes involved and of the various observational parameters are also tested. The simulations show that the TW method could be applied to the gaseous velocity fields to get a good estimate of the bar pattern speed, under the condition that regions of shocks are avoided and measurements are confined to regions where the gaseous bar is well formed. We successfully apply the TW method to the \ha velocity field of the Virgo Cluster Galaxy M100 (NGC 4321) and derive pattern speeds of 55+/-5 km/s/kpc for the nuclear structure, 30+/-2 km/s/kpc for the bar and 20+/-1 km/s/kpc for the spiral pattern, in full agreement with published determinations using the same method or alternative ones., 29 pages, 8 figures, accepted for publication in ApJ. To obtain a higher resolution version, visit to http://www.astro.umontreal.ca/fantomm/bhabar/
Published: 2005

38. Photometric and dynamic evolution of an isolated disc galaxy simulation

Author: Herve Wozniak, Leo Michel-Dansac, 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 Beaussier, Catherine
Subjects: Physics, Star formation, Metallicity, Extinction (astronomy), Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Radius, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Stars, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Stellar evolution, Astrophysics::Galaxy Astrophysics
Abstract: We present a detailed analysis of the evolution of a simulated isolated disc galaxy. The simulation includes stars, gas, star formation and simple chemical yields. Stellar particles are split in two populations: the old one is present at the beginning of the simulation and is calibrated according to various ages and metallicities; the new population borns in the course of the simulation and inherits the metallicity of the gas particles. The results have been calibrated in four wavebands with the spectro-photometric evolutionary model GISSEL2000 (Bruzual & Charlot 1993). Dust extinction has also been taken into account. A rest-frame morphological and bidimensional photometric analysis has been performed on simulated images, with the same tools as for observations. The effects of the stellar bar formation and the linked star formation episode on the global properties of the galaxy (mass and luminosity distribution, colours, isophotal radii) have been analysed. In particular, we have disentangled the effects of stellar evolution from dynamic evolution to explain the cause of the isophotal radii variations. We show that the dynamic properties (e.g. mass) of the area enclosed by any isophotal radius depends on the waveband and on the level of star formation activity. It is also shown that the bar isophotes remain thinner than mass isodensities a long time (> 0.7 Gyr) after the maximum of star formation rate. We show that bar ellipticity is very wavelength dependent as suggested by real observations. Effects of dust extinction on photometric and morphological measurements are systematically quantified., 14 pages, 16 figures (13 in eps, 3 in jpg format). Accepted for publication in A&A
Published: 2004

39. MUSE: a second-generation integral-field spectrograph for the VLT

Author: Thierry Contini, C. M. Carollo, Florence Laurent, Antonio Manescau, Martin M. Roth, E. Popow, Andreas Kelz, L. Capoani, P. Caillier, Christian Monstein, Lutz Wisotzki, N. Champavert, C. Koehler, Stefan Dreizler, P. Boehm, Roland Bacon, Peter M. Weilbacher, Simon J. Lilly, Cyril Petit, P. T. de Zeeuw, Aurélien Jarno, Joop Schaye, Julien Devriendt, D. Hofmann, Stefan Stroebele, Jean-Pierre Dubois, Magali Loupias, Luca Pasquini, G. Soucail, Roland Reiss, R. Pello, Eric Emsellem, J. Gerssen, Herve Wozniak, G. Gallou, Matthias Steinmetz, L. Parès, Svend M. Bauer, S. Brau-Nogué, Harald Nicklas, Richard M. McDermid, Bernard Delabre, Didier Boudon, Emmanuel Pecontal, Eric Daguisé, M. Dupieux, Johan Kosmalski, Andreas Quirrenbach, Edgard Renault, J. P. Dupin, Wolfram Kollatschny, Marijn Franx, B. Guiderdoni, J.-P. Picat, T. Hahn, Arlette Pécontal-Rousset, J.-L. Lizon, Remko Stuik, and Pierre Ferruit
Subjects: Very Large Telescope, Pixel, Galactic astronomy, Computer science, business.industry, Astronomy, Multi Unit Spectroscopic Explorer, Data cube, Integral field spectrograph, Optics, Observatory, Guide star, business, Adaptive optics, Spectrograph
Abstract: The Multi Unit Spectroscopic Explorer (MUSE) is a second-generation instrument in development for the Very Large Telescope (VLT) of the European Southern Observatory (ESO), due to begin operation in 2011/12. MUSE will be an extremely powerful integral-field spectrograph fed by a new multiple-laser adaptive optics system on the VLT. In its usual operating mode, MUSE will, in a single observation, produce a 3-dimensional data cube consisting of 90,000 R 3000 spectra, each covering a full spectral octave (480-930 nm), and fully sampling a contiguous 1×1 arcmin2 field with 0.2×0.2 arcsec2 apertures. A high-resolution mode will increase the spatial sampling to 0.025 arcsec per pixel. MUSE is built around a novel arrangement of 24 identical spectrographs (each comparable to a 1st generation VLT instrument), which are fed by a set of 24 precision image slicers. MUSE is designed for stability, with only 2 modes, and virtually no moving parts, allowing very long exposures to be accumulated. Together with high throughput, this ensures that MUSE will have extreme sensitivity for observing faint objects. We overview the technical and scientific aspects of MUSE, highlighting the key challenges for dealing with the unprecedented quantity and complexity of the data, and the integration with the VLT adaptive optics facility (AOF) - a key development on the path to extremely large telescopes (ELTs). © 2008 Springer-Verlag Berlin Heidelberg.
Published: 2003
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40. Numerical simulations of central stellar velocity dispersion drops in disc galaxies

Author: D. Friedli, E. Emsellem, Herve Wozniak, Francoise Combes, Wozniak, Hervé, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-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), 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), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), 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), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), École normale supérieure - Paris (ENS Paris), and Université de Genève (UNIGE)
Subjects: Stellar population, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Disc galaxy, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Dispersion (optics), Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, 010308 nuclear & particles physics, Star formation, [PHYS.ASTR.GA] Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Velocity dispersion, Astronomy, Astronomy and Astrophysics, Barred spiral galaxy, Stars, Wavelength, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph]
Abstract: We present an interpretation of the stellar velocity dispersion drops discovered in the nuclear regions of three barred galaxy hosts of active/starburst galactic nuclei (NGC 1097, NGC 1808 and NGC 5728) by Emsellem et al. ([CITE]). Using self-consistent N -body simulations including stars, gas and star formation, we show that young stars born in the nuclear regions from dynamically cold gas have a lower velocity dispersion than the older stellar population. The young population (less than 0.9 Gyr old in our models), being more massive and brighter than the older one at near infrared wavelengths, fully dominates the observed line-of-sight kinematics of the circumnuclear regions.
Published: 2003

41. GHASP: A 3-D Survey of Spiral and Irregular Galaxies at Hα

Author: M. Marcelin, C. Adami, J. Boulesteix, Oscar F. Hernández, O. Garrido, Claude Carignan, C. Balkowski, S. Blais-Ouellette, Herve Wozniak, L. Michel-Dansac, A. Boselli, Henri Plana, D. Russeil, V. Cayatte, L. Chemin, Philippe Amram, Jean-Luc Gach, and B. Vollmer
Subjects: Luminous infrared galaxy, Physics, Spiral galaxy, Elliptical galaxy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Irregular galaxy, Astrophysics::Galaxy Astrophysics, Galaxy, Galaxy rotation curve, Spiral, Line (formation)
Abstract: The survey GHASP (Gassendi HAlpha survey of SPirals) will provide a 3-D sample of about 200 nearby spiral galaxies in the Hα line, using a Fabry-Perot system. The data cubes obtained for each galaxy allow to derive line maps, velocity fields and other moment analysis. This data base will allow the following four key ponts.
Published: 2002
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42. Sub-KPC Stellar Kinematics of AGN as Revealed by Isaac (VLT/ANTU) Spectroscopy

Author: Herve Wozniak, D. Friedli, D. Greusard, E. Emsellem, Daniel Pfenniger, and Francoise Combes
Subjects: Physics, Stellar kinematics, Accretion (meteorology), Bar (music), Astronomy, Kinematics, Astrophysics, Spectroscopy, Galaxy, Cosmology
Abstract: This study is part of the ‘Dynamics of Embedded Bars and Connections with AGN’ (DEBCA) project whose main goal is to provide new insights on the fueling processes of AGN. For that purpose the DEBCA team plans to observe and compare to numerical simulations a sample of 12 galaxies: Seyfert (1 or 2) or not, with or without double-bars. Fueling the central activity of AGN is a long-standing dilemma. Various ‘fueling engines’ have been proposed so far: e.g. nuclear bars nested in large-scale bars, or nuclear spirals. As the processes involved in these phenomena (bars, gas flows, accretion, ...) are dynamical with different time-scales, morphological studies have not brought definite answers yet. This issue clearly requires a kinematic study as well. Figure 1 shows the stellar kinematics of NGC 1097, as extracted from long slit observations of the CO bandheads (≈2.3 μm). The slit was aligned along the major and minor axis of the nuclear bar (which has an extent of ≈ 10″). Note the unusual central dip in the dispersion profiles. Papers presenting the whole data set analysis are in preparation.
Published: 2001
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43. Stellar kinematics of barred galaxies

Author: Herve Wozniak
Subjects: High Energy Physics::Phenomenology, Astrophysics (astro-ph), FOS: Physical sciences, High Energy Physics::Experiment, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: I show that the counter-rotating core of the barred galaxy NGC 5728 could be explained by the internal dynamics of the bar. This supports the idea that the nuclear bar is counter-rotating., Comment: To appear in "Galaxy dynamics: from the early universe to the present", ASP Conference Series, F. Combes, G.A. Mamon, V. Charmandaris (eds.). LaTeX, 2 pages, 1 postscript figure, newpasp.sty included
Published: 1999
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44. Preface

Author: Herve Wozniak
Subjects: Space and Planetary Science, General Engineering, Astronomy and Astrophysics
Published: 2007
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45. Préface

Author: Herve Wozniak
Subjects: Space and Planetary Science, General Engineering, Astronomy and Astrophysics
Published: 2007
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46. First Results from ISOCAM Images of Circumnuclear Starbursts in Barred Galaxies

Author: Herve Wozniak, Friedli, D., Martinet, L., and Pfenniger, D.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: For a sample of ten nearby barred galaxies, images at 6.75\um and 15\um of circumnuclear starbursts are being taken by ISOCAM on board of the ISO satellite. We first recall the main goals of our project, give its current status, and finally, as an example, preliminary results for NGC 4321 (M100) are presented., Comment: To appear in "Extragalactic Astronomy in the Infrared", eds. G.A. Mamon, Trinh Xuan Thuan, and J. Tran Thanh Van, Editions Frontieres, Gif-sur-Yvette. LaTeX, 6 pages, 3 postscript figures, moriond.sty included. See also at ftp://www-obs.cnrs-mrs.fr/wozniak/moriond97.ps-gz
Published: 1997
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47. Starbursts in Barred Spiral Galaxies. II. Molecular and Optical Study of Three Wolf-Rayet Galaxies

Author: Contini, T., Herve Wozniak, Considere, S., and Davoust, E.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We have searched for dense molecular gas in three barred spiral galaxies with young starbursts, NGC 3049, 5430 and 6764, which are known Wolf-Rayet galaxies. We detected HCN in the latter two, and CS was marginally detected in NGC 6764. The dense molecular gas contents of the three galaxies are compared to those of other galaxies and to other indicators of star formation. The HCN luminosities (relative to the CO and far infrared ones) in these galaxies with very young starbursts are consistent with those observed in galaxies with older starbursts and in normal galaxies, and so are our upper limits to the CS intensities (relative to CO). The starburst ages evaluated from our spectrophotometric observations are in the range 3.4 to 6.0 Myr. A circum-nuclear ring is apparent on our images of NGC 5430, the galaxy with the oldest central starburst; this galaxy also has the widest molecular lines. The central star formation rates derived from the Halpha luminosity are consistent with those expected from the global FIR luminosities, and are correlated with the HCN luminosities. Finally, an independent estimate of the H_2 column density is obtained by optical spectrophotometry; it leads to a H_2 column density to CO intensity ratio which is about 2 to 3 times lower than the standard value, because the CO intensities of the three galaxies are higher than average, relative to their far infrared fluxes., Comment: Accepted for publication in A&A. 11 pages, including 4 Postscript figures and 4 tables. LateX using l-aa and epsf macros
Published: 1997
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48. Disc galaxies with multiple triaxial structures. II. JHK surface photometry and numerical simulations

Author: P. Bratschi, Herve Wozniak, D. Friedli, Marcia J. Rieke, and L. Martinet
Subjects: Physics, Luminous infrared galaxy, Surface brightness fluctuation, Astrophysics (astro-ph), High Energy Physics::Phenomenology, FOS: Physical sciences, General Physics and Astronomy, Astronomy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Bulge, Galaxy group, Elliptical galaxy, Disc, Lenticular galaxy, Galaxy cluster, Astrophysics::Galaxy Astrophysics
Abstract: We present detailed JHK surface photometry with ellipse fits of 13 galaxies selected from previous optical observations as likely candidates for having a secondary bar or a triaxial bulge within the primary bar. We have found 7 double-barred galaxies, 3 double-barred galaxies with an additional intermediate structure with twisted isophotes, and 3 galaxies with a bar and central twisted isophotes. A global analysis of the structural parameter characteristics in the I- and K-bands is presented. Various numerical models of galaxies with bars within bars are also analysed using the ellipse fitting technique and compared to the observations. A thorough review of the possible hypotheses able to explain this phenomenon is given with emphasis on the most likely ones., 12 pages, AATEX. Accepted for publication in A&A. Large color postscript figures omitted (Figs. 1), figures 2-9 included; gzip'ed postscript files of the paper and Figs. 1 available via anonymous ftp at ftp://obsftp.unige.ch/pub/fri/aasjhk/ , files fri_aasjhk.ps.gz and ngc*.ps.gz
Published: 1996

49. Radial migration in galactic disks caused by resonance overlap of multiple patterns: Self-consistent simulations

Author: Benoit Famaey, P. Di Matteo, Ivan Minchev, Francoise Combes, M. Mouhcine, Herve Wozniak, Leibniz-Institut für Astrophysik Potsdam (AIP), 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), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Wozniak, Hervé, Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), École normale supérieure - Paris (ENS Paris), Astrophysikalisches Institut Potsdam (AIP), Observatoire astronomique de Strasbourg (OAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Rheinische Friedrich-Wilhelms-Universität Bonn, Galaxies et cosmologie, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Physique stellaire et galactique, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), and ARI, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead
Subjects: Angular momentum, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Milky Way, Metallicity, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, 0103 physical sciences, Galaxy formation and evolution, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Physics, Spiral galaxy, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Barred spiral galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics::Earth and Planetary Astrophysics, [SDU.ASTR.GA] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Lindblad resonance, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We have recently identified a new radial migration mechanism resulting from the overlap of spiral and bar resonances in galactic disks. Here we confirm the efficiency of this mechanism in fully self-consistent, Tree-SPH simulations, as well as high-resolution pure N-body simulations. In all barred cases we clearly identify the effect of spiral-bar resonance overlap by measuring a bimodality in the changes of angular momentum in the disk, dL, whose maxima are near the bar's corotation and outer Lindblad resonance. This contrasts with the smooth distribution of dL for a simulation with no stable bar present, where strong radial migration is induced by multiple spirals. The presence of a disk gaseous component appears to increase the rate of angular momentum exchange by about 20%. The efficiency of this mechanism is such that galactic stellar disks can extend to over 10 scale-lengths within 1-3 Gyr in both Milky Way size and low-mass galaxies (circular velocity ~100 km/s). We also show that metallicity gradients can flatten in less than 1 Gyr rendering mixing in barred galaxies an order of magnitude more efficient than previously thought., replaced with accepted version: 5 pages, 5 figures (one new figure added), minor changes
Published: 2011
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50. TheHerschelSpace Observatory view of dust in M81

Author: Marc Sauvage, N. Lu, Pierre Chanial, Walter Kieran Gear, L. Vigroux, Pasquale Panuzzo, M. Symeonidis, Herve Wozniak, Diane Cormier, George J. Bendo, B. O'Halloran, James J. Bock, M. J. Barlow, Werner W. Zeilinger, Jamie Stevens, Mattia Vaccari, E. E. Rigby, Stephane Charlot, Helene Roussel, David L. Clements, Luca Cortese, Naseem Rangwala, T. J. Parkin, Michael Pohlen, N. Castro-Rodriguez, Matthew Joseph Griffin, Matthew Smith, Sacha Hony, S. Sundar, Maud Galametz, Alessandro Boselli, A. Cooray, Gillian S. Wright, Christine D. Wilson, M. Bradford, Haley Louise Gomez, Stephen Anthony Eales, Koryo Okumura, Andreas Papageorgiou, Eli Dwek, Maximilien R. P. Schirm, Laure Ciesla, Kate Gudrun Isaak, Maarten Baes, N. Sacchi, Suzanne C. Madden, L. R. Levenson, Benjamin L. Schulz, Markos Trichas, Seb Oliver, V. Buat, Ismael Perez-Fournon, Mat Page, Jason Glenn, Robbie Richard Auld, D. Elbaz, Frédéric Galliano, L. Spinoglio, A. Rykala, Jonathan Ivor Davies, 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), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: galaxies: spiral, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, TELESCOPE, H-ALPHA, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, THINGS, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, STAR-FORMATION RATES, individual: M81 [galaxies], galaxies: individual: M81, Bulge, Astrophysics::Solar and Stellar Astrophysics, Surface brightness, FIELD, Astrophysics::Galaxy Astrophysics, QB, Physics, Spiral galaxy, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ISM [galaxies], Spectral density, Astronomy and Astrophysics, Radius, Space observatory, GALAXIES, SPITZER, Stars, spiral [galaxies], Physics and Astronomy, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, EMISSION, galaxies: ISM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use Herschel Space Observatory data to place observational constraints on the peak and Rayleigh-Jeans slope of dust emission observed at 70-500 microns in the nearby spiral galaxy M81. We find that the ratios of wave bands between 160 and 500 microns are primarily dependent on radius but that the ratio of 70 to 160 micron emission shows no clear dependence on surface brightness or radius. These results along with analyses of the spectral energy distributions imply that the 160-500 micron emission traces 15-30 K dust heated by evolved stars in the bulge and disc whereas the 70 micron emission includes dust heated by the active galactic nucleus and young stars in star forming regions., Accepted for A & A Herschel special issue
Published: 2010
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