Author: "Galametz, A." / Publisher: hal ccsd - Searchworks@Jio Institute Digital Library Search Results

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43 results on '"Galametz, A."'

1. A nearby galaxy perspective on dust evolution

Author: A. Nersesian, Jacopo Fritz, Anthony P. Jones, Sambit Roychowdhury, Nathalie Ysard, Wouter Dobbels, Letizia, Ilse De Looze, Maarten Baes, P. Cassará, Emmanuel M. Xilouris, Maud Galametz, Aleksandr V. Mosenkov, Suzanne C. Madden, Viviana Casasola, Frédéric Galliano, Simone Bianchi, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université de Haute Bretagne ( Rennes 2 ) (UR 2), University College of London [London] (UCL), Indian Institute of Technology Bombay (IIT Bombay), Sterrenkundig Observatorium, Universiteit Gent, Centre Pluridisciplinaire Textes et Cultures [Dijon] (CPTC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université de Bourgogne (UB), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Universiteit Gent = Ghent University (UGENT), and Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES)
Subjects: 010504 meteorology & atmospheric sciences, Metallicity, statistical [methods], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, STAR-FORMATION RATES, 01 natural sciences, ISM: abundances, POLYCYCLIC AROMATIC-HYDROCARBONS, 0103 physical sciences, evolution, Astrophysics::Solar and Stellar Astrophysics, TO-GAS RATIO, SMALL-MAGELLANIC-CLOUD, LOW-TEMPERATURE MIR, Ejecta, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, abundances [ISM], Physics, methods: statistical, Star formation, extinction, Astronomy and Astrophysics, Mass ratio, Astrophysics - Astrophysics of Galaxies, ACTIVE GALACTIC NUCLEUS, MASS ABSORPTION-COEFFICIENT, Galaxy, Grain growth, Supernova, SPECTRAL ENERGY-DISTRIBUTION, Physics and Astronomy, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), MULTIBAND IMAGING PHOTOMETER, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, dust, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], LOW-METALLICITY ENVIRONMENTS
Abstract: Methods. We have modelled a sample of ~800 nearby galaxies, spanning a wide range of metallicity, gas fraction, specific star formation rate and Hubble stage. We have derived the dust properties of each object from its spectral energy distribution. Through an additional level of analysis, we have inferred the timescales of dust condensation in core-collapse supernova ejecta, grain growth in cold clouds and dust destruction by shock waves. Throughout this paper, we have adopted a hierarchical Bayesian approach, resulting in a single large probability distribution of all the parameters of all the galaxies, to ensure the most rigorous interpretation of our data. Results. We confirm the drastic evolution with metallicity of the dust-to-metal mass ratio (by two orders of magnitude), found by previous studies. We show that dust production by core-collapse supernovae is efficient only at very low-metallicity, a single supernova producing on average less than ~0.03 Msun/SN of dust. Our data indicate that grain growth is the dominant formation mechanism at metallicity above ~1/5 solar, with a grain growth timescale shorter than ~50 Myr at solar metallicity. Shock destruction is relatively efficient, a single supernova clearing dust on average in at least ~1200 Msun/SN of gas. These results are robust when assuming different stellar initial mass functions. In addition, we show that early-type galaxies are outliers in several scaling relations. This feature could result from grain thermal sputtering in hot X-ray emitting gas, an hypothesis supported by a negative correlation between the dust-to-stellar mass ratio and the X-ray photon rate per grain. Finally, we confirm the well-known evolution of the aromatic-feature-emitting grain mass fraction as a function of metallicity and interstellar radiation field intensity. Our data indicate the relation with metallicity is significantly stronger., Comment: 64 pages, 36 figures, accepted for publication in Astronomy & Astrophysics
Published: 2021
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2. An observational correlation between magnetic field, angular momentum and fragmentation in the envelopes of Class 0 protostars?

Author: Eric Keto, Qizhou Zhang, Shih-Ping Lai, Valeska Valdivia, Josep M. Girart, Anaëlle Maury, Victoria Cabedo-Soto, Patrick Hennebelle, M. Gaudel, Ramprasad Rao, Maud Galametz, Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), Harvard-Smithsonian Center for Astrophysics (CfA), Smithsonian Institution-Harvard University [Cambridge], Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), National Tsing Hua University [Hsinchu] (NTHU), European Project: 679937,H2020,ERC-2015-STG,MagneticYSOs(2016), 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), Harvard University-Smithsonian Institution, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), European Commission, Ministerio de Ciencia e Innovación (España), Agencia Estatal de Investigación (España), and Ministerio de Ciencia, Innovación y Universidades (España)
Subjects: Angular momentum, FOS: Physical sciences, Astrophysics, Kinetic energy, 7. Clean energy, 01 natural sciences, Submillimeter Array, protostars [Stars], 0103 physical sciences, Protostar, Astrophysics::Solar and Stellar Astrophysics, instrumentation: interferometers, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), formation [Stars], Astrophysics::Galaxy Astrophysics, Physics, ISM: kinematics and dynamics, [PHYS]Physics [physics], stars: formation, Magnetic energy, stars: protostars, 010308 nuclear & particles physics, Velocity gradient, magnetic fields [ISM], ISM [Submillimeter], Astronomy and Astrophysics, interferometers [Instrumentation], Astrophysics - Astrophysics of Galaxies, Magnetic field, kinematics and dynamics [ISM], Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), submillimeter: ISM, Outflow, Astrophysics::Earth and Planetary Astrophysics, ISM: magnetic fields, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Aims. The main goal of the following analysis is to assess the potential role of magnetic fields in regulating the envelope rotation, the formation of disks and the fragmentation of Class 0 protostars in multiple systems. Methods. We use the Submillimeter Array to carry out observations of the dust polarized emission at 0.87 mm, in the envelopes of a large sample of 20 Class 0 protostars. We estimate the mean magnetic field orientation over the central 1000 au envelope scales to characterize the orientation of the main component of the organized magnetic field at the envelope scales in these embedded protostars. This direction is compared to that of the protostellar outflow in order to study the relation between their misalignment and the kinematics of the circumstellar gas. The latter is traced via velocity gradient observed in the molecular line emission (mainly N2H+) of the gas at intermediate envelope scales. Results. We discover a strong relationship between the misalignment of the magnetic field orientation with the outflow and the amount of angular momentum observed at similar scales in the protostellar envelope, revealing a potential link between the kinetic and the magnetic energy at envelope scales. The relation could be driven by favored B-misalignments in more dynamical envelopes or a dependence of the envelope dynamics with the large-scale B initial configuration. Comparing the trend with the presence of fragmentation, we observe that single sources are mostly associated with conditions of low angular momentum in the inner envelope and good alignment of the magnetic field with protostellar outflows, at intermediate scales. Our results suggest that the properties of the magnetic field in protostellar envelopes bear a tight relationship with the rotating-infalling gas directly involved in the star and disk formation: we find that it may not only influence the fragmentation of protostellar cores into multiple stellar systems, but also set the conditions establishing the pristine properties of planet-forming disks., This project has received funding from the European Research Council (ERC) under the European Union Horizon 2020 research and innovation programme (MagneticYSOs project, grant agreement No. 679937, PI: Maury). J.M.G. is supported by the grant AYA2017-84390- C2-R (AEI/FEDER, UE).
Published: 2020
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3. Euclid preparation

Author: Collaboration, Euclid, Desprez, G., Almosallam, I., Alvarez-Ayllon, A., Amaro, V., Brodwin, M., De Vicente-Albendea, J., Fotopoulou, S., Hatfield, P. W., Hartley, W. G., Ilbert, O., Jarvis, M. J., Longo, G., Saha, R., Speagle, J. S., Tramacere, A., Dubath, F., Galametz, A., Kuemmel, M., Laigle, C., Merlin, E., Mohr, J. J., Pilo, S., Salvato, M., Rau, M. M., Bonino, D., Brinchmann, J., Castander, F. J., Cimatti, A., Cuby, J. -G., Degaudenzi, H., Douspis, M., Ealet, A., Fabricius, M., Fosalba, P., Fourmanoit, N., Fumana, M., Gillard, W., Gillis, B., Hailey, M., Haugan, S. V. H., Humphrey, A., Kilbinger, M., Kitching, T. D., Kohley, R., Maiorano, E., Maturi, M., Mei, S., Metcalf, R. Benton, Popa, L., Pozzetti, L., Rossetti, E., Stern, D., Tavagnacco, D., Zamorani, G., Zoubian, J., Benton Metcalf, R., Tallada Crespí, P., Knabenhans, M., Stadel, J., Potter, D., Dakin, J., Hannestad, S., Tram, T., Marelli, S., Schneider, A., Teyssier, R., Andreon, S., Auricchio, N., Baccigalupi, C., Balaguera-Antolínez, A., Baldi, M., Bardelli, S., Battaglia, P., Bender, R., Biviano, A., Bodendorf, C., Bozzo, E., Branchini, E., Brescia, M., Burigana, C., Cabanac, R., Camera, S., Capobianco, V., Cappi, A., Carbone, C., Carretero, J., Carvalho, C. S., Casas, R., Casas, S., Castellano, M., Castignani, G., Cavuoti, S., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Coupon, J., Courtois, H. M., Da Silva, A., de la Torre, S., Di Ferdinando, D., Duncan, C. A. J., Dupac, X., Fabbian, G., Farrens, S., Ferreira, P. G., Finelli, F., Frailis, M., Franceschi, E., Galeotta, S., Garilli, B., Giocoli, C., Gozaliasl, G., Graciá-Carpio, J., Grupp, F., Guzzo, L., Holmes, W., Hormuth, F., Israel, H., Jahnke, K., Keihanen, E., Kermiche, S., Kirkpatrick, C. C., Kubik, B., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maino, D., Marggraf, O., Markovic, K., Martinet, N., Marulli, F., Massey, R., Mauri, N., Maurogordato, S., Medinaceli, E., Meneghetti, M., Metcalf, B., Meylan, G., Moresco, M., Morin, B., Moscardini, L., Munari, E., Neissner, C., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Patrizii, L., Pettorino, V., Pires, S., Polenta, G., Poncet, M., Raison, F., Renzi, A., Rhodes, J., Riccio, G., Romelli, E., Roncarelli, M., Saglia, R., Sánchez, A. G., Sapone, D., Schneider, P., Scottez, V., Secroun, A., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Sureau, F., Crespí, P. Tallada, Taylor, A. N., Tenti, M., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Valenziano, L., Valiviita, J., Vassallo, T., Viel, M., Wang, Y., Welikala, N., Whittaker, L., Zacchei, A., Zucca, E., Joseph Louis LAGRANGE (LAGRANGE), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), and COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)
Subjects: [SDU]Sciences of the Universe [physics], Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract: Accepted in A&A, 25 pages, 13 figures, 7 tables; Forthcoming large photometric surveys for cosmology require precise and accurate photometric redshift (photo-z) measurements for the success of their main science objectives. However, to date, no method has been able to produce photo-$z$s at the required accuracy using only the broad-band photometry that those surveys will provide. An assessment of the strengths and weaknesses of current methods is a crucial step in the eventual development of an approach to meet this challenge. We report on the performance of 13 photometric redshift code single value redshift estimates and redshift probability distributions (PDZs) on a common set of data, focusing particularly on the 0.2--2.6 redshift range that the Euclid mission will probe. We design a challenge using emulated Euclid data drawn from three photometric surveys of the COSMOS field. The data are divided into two samples: one calibration sample for which photometry and redshifts are provided to the participants; and the validation sample, containing only the photometry, to ensure a blinded test of the methods. Participants were invited to provide a redshift single value estimate and a PDZ for each source in the validation sample, along with a rejection flag that indicates sources they consider unfit for use in cosmological analyses. The performance of each method is assessed through a set of informative metrics, using cross-matched spectroscopic and highly-accurate photometric redshifts as the ground truth. We show that the rejection criteria set by participants are efficient in removing strong outliers, sources for which the photo-z deviates by more than 0.15(1+z) from the spectroscopic-redshift (spec-z). We also show that, while all methods are able to provide reliable single value estimates, several machine-learning methods do not manage to produce useful PDZs. [abridged]
Published: 2020

4. I. An APEX survey of HCO + and HCN(2−1) toward the LMC and SMC

Author: Galametz, M., Schruba, A., De Breuck, C., Immer, K., Chevance, M., Galliano, F., Gusdorf, A., Lebouteiller, V., Lee, M. Y., Madden, S. C., Polles, F. L., van Kempen, T. A., 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), Max-Planck-Institut für Extraterrestrische Physik (MPE), European Southern Observatory (ESO), Joint Institute for VLBI in Europe (JIVE ERIC), Zentrum für Astronomie der Universität Heidelberg (ZAH), Universität Heidelberg [Heidelberg], Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Korea Astronomy and Space Science Institute (KASI), Okayama University, SRON Netherlands Institute for Space Research (SRON), This work was partly supported by the Programme National 'Physique et Chimie du Milieu Interstellaire' (PCMI) of CNRS/INSU with INC/INP co-funded by CEA and CNES., Funding from the ANR Grant LYRICS (ANR-16-CE31-0011)., APEX collaboration, SEPIA collaboration, European Project: 679937,H2020,ERC-2015-STG,MagneticYSOs(2016), 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), Universität Heidelberg [Heidelberg] = Heidelberg University, École normale supérieure - Paris (ENS-PSL), and ANR-16-CE31-0011,LYRICS,Le cycle du gaz autour des galaxies : origine et conditions physiques des flots de gaz froid(2016)
Subjects: molecular processes, stars: formation, Magellanic Clouds, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ISM: clouds, ISM: molecules, galaxies: ISM
Abstract: International audience; Context. Understanding the star-forming processes is key to understanding the evolution of galaxies. Investigating star formation requires precise knowledge of the properties of the dense molecular gas complexes where stars form and a quantification of how they are affected by the physical conditions to which they are exposed. The proximity, low metallicity, and wide range of star formation activity of the Large and Small Magellanic Clouds (LMC and SMC) make them prime laboratories to study how local physical conditions impact the dense gas reservoirs and their star formation efficiency.Aims. The aim of the Dense Gas Survey for the Magellanic Clouds (DeGaS-MC) project is to expand our knowledge of the relation between dense gas properties and star formation activity by targeting the LMC and SMC observed in the HCO+(2−1) and HCN(2−1) transitions.Methods. We carried out a pointing survey targeting two lines toward ∼30 LMC and SMC molecular clouds using the SEPIA180 instrument installed on the Atacama Pathfinder EXperiment (APEX) telescope. We performed a follow-up mapping campaign of the emission in the same transition in 13 star-forming regions. This first paper provides line characteristic catalogs and integrated line-intensity maps of the sources.Results. HCO+(2−1) is detected in 20 and HCN(2−1) in 8 of the 29 pointings observed. The dense gas velocity pattern follows the line-of-sight velocity field derived from the stellar population. The three SMC sources targeted during the mapping campaign were unfortunately not detected in our mapping campaign but both lines are detected toward the LMC 30Dor, N44, N105, N113, N159W, N159E, and N214 regions. The HCN emission is less extended than the HCO+ emission and is restricted to the densest regions. The HCO+(2−1)/HCN(2−1) brightness temperature ratios range from 1 to 7, which is consistent with the large ratios commonly observed in low-metallicity environments. A larger number of young stellar objects are found at high HCO+ intensities and lower HCO+/HCN flux ratios, and thus toward denser lines of sight. The dense gas luminosities correlate with the star formation rate traced by the total infrared luminosity over the two orders of magnitude covered by our observations, although substantial region-to-region variations are observed.
Published: 2020
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5. Angular momentum profiles of Class 0 protostellar envelopes

Author: P. Palmeirim, Maud Galametz, Sébastien Maret, Ph. André, Linda Podio, Patrick Hennebelle, M. Gaudel, Claudio Codella, S. Cabrit, Leonardo Testi, Anaëlle Maury, Bilal Ladjelate, Arnaud Belloche, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), 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), Max-Planck-Institut für Radioastronomie (MPIFR), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), European Southern Observatory (ESO), Instituto de Astrofísica e Ciências do Espaço (IASTRO), Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), 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, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Harvard-Smithsonian Center for Astrophysics (CfA), Smithsonian Institution-Harvard University [Cambridge], European Project: 291294,EC:FP7:ERC,ERC-2011-ADG_20110209,ORISTARS(2012), European Project: 679937,H2020,ERC-2015-STG,MagneticYSOs(2016), École normale supérieure - Paris (ENS-PSL), 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 national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, 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), 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), and Harvard University-Smithsonian Institution
Subjects: Angular momentum, FOS: Physical sciences, Context (language use), Kinematics, Astrophysics, 01 natural sciences, Specific relative angular momentum, 0103 physical sciences, Differential rotation, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, ISM: kinematics and dynamics, [PHYS]Physics [physics], radio lines: ISM, stars: formation, stars: protostars, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Velocity gradient, Star formation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Accretion (astrophysics), Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: [abridged] Understanding how the infalling gas redistribute most of its initial angular momentum inherited from prestellar cores before reaching the stellar embryo is a key question. Disk formation has been naturally considered as a possible solution to this "angular momentum problem". However, how the initial angular momentum of protostellar cores is distributed and evolves during the main accretion phase and the beginning of disk formation has largely remained unconstrained up to now. In the framework of the IRAM CALYPSO survey, we used high dynamic range C$^{18}$O (2-1) and N$_2$H$^+$ (1-0) observations to quantify the distribution of specific angular momentum along the equatorial axis in a sample of 12 Class 0 protostellar envelopes from scales ~50 to 10000 au. The radial distributions of specific angular momentum in the CALYPSO sample suggest two distinct regimes within protostellar envelopes: the specific angular momentum decreases as $j \propto r^{1.6 \pm 0.2}$ down to ~1600 au and then tends to become relatively constant around 6 $\times$ 10$^{-4}$ km s$^{-1}$ pc down to ~50 au. The values of specific angular momentum measured in the inner Class 0 envelopes, namely that of the material directly involved in the star formation process ($$1600 au, suggesting that they may not be related to rotational motions of the envelopes. We conclude that the specific angular momentum observed at these scales could find its origin in core-forming motions (infall, turbulence) or trace an imprint of the initial conditions for the formation of protostellar cores., Comment: 62 pages, 66 figures
Published: 2020
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6. The ISM scaling relations in DustPedia late-type galaxies: A benchmark study for the Local Universe

Author: I. De Looze, Jonathan Ivor Davies, A. Nersesian, Letizia P. Cassarà, Maud Galametz, Maarten Baes, Viviana Casasola, Edvige Corbelli, S. Viaene, S. C. Madden, P. De Vis, Anthony P. Jones, Laura Magrini, Christopher J. R. Clark, Emmanuel M. Xilouris, Jacopo Fritz, Ana Trčka, Frédéric Galliano, Aleksandr V. Mosenkov, Simone Bianchi, W. Dobbels, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astrofisico di Arcetri (OAA), Cardiff University, Space Telescope Science Institute (STSci), Instituto de Radioastronomía y Astrofísica (IRyA), Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), National Observatory of Athens (NOA), National Technical University of Athens [Athens] (NTUA), Sterrenkundig Observatorium, Universiteit Gent = Ghent University (UGENT), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), University College of London [London] (UCL), 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), The Central Astronomical Observatory of the Russian Academy of Sciences [Pulkovo], Russian Academy of Sciences [Moscow] (RAS), St Petersburg State University (SPbU), European Project: 606847,EC:FP7:SPA,FP7-SPACE-2013-1,DUSTPEDIA(2014), Universidad Nacional Autónoma de México (UNAM), Universiteit Gent, 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 Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Stellar mass, Metallicity, MASS-METALLICITY RELATION, Extinction (astronomy), IRAM LEGACY SURVEY, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, ISM: atoms, CO OBSERVATIONS, 01 natural sciences, ISM: abundances, CO-TO-H-2 CONVERSION FACTOR, 0103 physical sciences, galaxies, evolution, Galaxy formation and evolution, STAR-FORMING GALAXIES, molecules, 010303 astronomy & astrophysics, ISM, Astrophysics::Galaxy Astrophysics, Physics, atoms, 010308 nuclear & particles physics, Star formation, abundances, extinction, GAS CONTENT, Astronomy and Astrophysics, Mass ratio, Astrophysics - Astrophysics of Galaxies, Galaxy, ATOMIC GAS, ISM: molecules, Interstellar medium, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), dust, STELLAR MASS, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], TO-MOLECULAR TRANSITION, NEARBY SPIRAL GALAXIES, galaxies: ISM
Abstract: The purpose of this work is the characterization of the main scaling relations between all the ISM components (dust, atomic/molecular/total gas), gas-phase metallicity, and other galaxy properties, such as Mstar and galaxy morphology, for late-type galaxies in the Local Universe. This study is performed by extracting late-type galaxies from the entire DustPedia sample and by exploiting the large and homogeneous dataset available thanks to the DustPedia project. The sample consists of 436 galaxies with morphological stage from T = 1 to 10, Mstar from 6 x 10^7 to 3 x 10^11 Msun, SFR from 6 x 10^(-4) to 60 Msun/yr, and 12 + log(O/H) from 8 to 9.5. The scaling relations involving the molecular gas are studied by assuming both a constant and a metallicity-dependent XCO. The analysis has been performed by means of the survival analysis technique. We confirm that the dust mass correlates very well with the total gas mass, and find -- for the first time -- that the dust mass correlates better with the atomic gas mass than the molecular one. We characterize important mass ratios such as gas fraction, molecular-to-atomic gas mass ratio, dust-to-total gas mass ratio (DGR), and dust-to-stellar mass ratio. Only the assumption of a metallicity-dependent XCO reproduces the expected decrease of the DGR with increasing morphological stage and decreasing gas-phase metallicity, with a slope of about 1. DGR, gas-phase metallicity, and the dust-to-stellar mass ratio are, for our galaxy sample, directly linked to the galaxy morphology. The molecular-to-atomic gas mass ratio and the DGR show a positive correlation for low molecular gas fractions, but for molecular gas rich galaxies this trend breaks down. This trend has never been found previously, to our knowledge. It provides new constraints for theoretical models of galaxy evolution and a reference for high-redshift studies., Comment: Accepted for publication in A&A, 21 pages, 14 Figures, 7 Tables, 2 Appendices (with 3 Tables). Published version, unchanged results with respect to the previously posted version
Published: 2020
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7. Physical conditions in the gas phases of the giant H II region LMC-N 11

Author: Lebouteiller, V., Cormier, D., Madden, S., Galametz, M., Hony, S., Galliano, F., Chevance, M., Lee, M.-Y., Braine, J., Polles, F., Requeña-Torres, M., Indebetouw, R., Hughes, A., Abel, N., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), University of North Carolina [Charlotte] (UNC), University of North Carolina System (UNC), 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), 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Université 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), This work was supported by the Programme National 'Physique et Chimie du Milieu Interstellaire' (PCMI) of CNRS/INSU with INC/INP co-funded by CEAand CNES., ANR-16-CE31-0011,LYRICS,Le cycle du gaz autour des galaxies : origine et conditions physiques des flots de gaz froid(2016), and European Project: 702622,H2020,H2020-MSCA-IF-2015,eGALISM(2017)
Subjects: [PHYS]Physics [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ISM: general, photon-dominated region, Magellanic Clouds, submillimeter: ISM, infrared: ISM, galaxies: star formation, ComputingMilieux_MISCELLANEOUS
Abstract: International audience; Context. The ambiguous origin of the [C II] 158μm line in the interstellar medium complicates its use for diagnostics concerning the star-formation rate and physical conditions in photodissociation regions.Aims. We investigate the origin of [C II] in order to measure the total molecular gas content, the fraction of CO-dark H2 gas, and how these parameters are impacted by environmental effects such as stellar feedback.Methods. We observed the giant H II region N 11 in the Large Magellanic Cloud with SOFIA/GREAT. The [C II] line is resolved in velocity and compared to H I and CO, using a Bayesian approach to decompose the line profiles. A simple model accounting for collisions in the neutral atomic and molecular gas was used in order to derive the H2 column density traced by C+.Results. The profile of [C II] most closely resembles that of CO, but the integrated [C II] line width lies between that of CO and that of H I. Using various methods, we find that [C II] mostly originates from the neutral gas. We show that [C II] mostly traces the CO-dark H2 gas but there is evidence of a weak contribution from neutral atomic gas preferentially in the faintest components (as opposed to components with low [C II]/CO or low CO column density). Most of the molecular gas is CO-dark. The CO-dark H2 gas, whose density is typically a few 100s cm−3 and thermal pressure in the range 103.5−5 K cm−3, is not always in pressure equilibrium with the neutral atomic gas. The fraction of CO-dark H2 gas decreases with increasing CO column density, with a slope that seems to depend on the impinging radiation field from nearby massive stars. Finally we extend previous measurements of the photoelectric-effect heating efficiency, which we find is constant across regions probed with Herschel, with [C II] and [O I] being the main coolants in faint and diffuse, and bright and compact regions, respectively, and with polycyclic aromatic hydrocarbon emission tracing the CO-dark H2 gas heating where [C II] and [O I] emit.Conclusions. We present an innovative spectral decomposition method that allows statistical trends to be derived for the molecular gas content using CO, [C II], and H I profiles. Our study highlights the importance of velocity-resolved photodissociation region (PDR) diagnostics and higher spatial resolution for H I observations as future steps.
Published: 2019
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8. An ALMA view of molecular filaments in the Large Magellanic Cloud II: An early stage of high-mass star formation embedded at colliding clouds in N159W-South

Author: Toshikazu Onishi, Maud Galametz, Yasuo Fukui, Omnarayani Nayak, Remy Indebetouw, Kazufumi Torii, Tsuyoshi Inoue, Atsushi Nishimura, Vianney Lebouteiller, Akiko Kawamura, Ryohei Harada, Norikazu Mizuno, Kazuki Tokuda, Marta Sewilo, Kazuya Saigo, Margaret Meixner, Sarolta Zahorecz, Kengo Tachihara, C.-H. Rosie Chen, Tetsuhiro Minamidani, Suzanne C. Madden, Kisetsu Tsuge, Kyoto University [Kyoto], 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), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Kyoto University, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Length scale, [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], 010504 meteorology & atmospheric sciences, Continuum (design consultancy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Protein filament, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Protostar, Astrophysics::Solar and Stellar Astrophysics, Large Magellanic Cloud, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Star formation, Molecular cloud, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, [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)
Abstract: We have conducted ALMA CO isotopes and 1.3 mm continuum observations toward filamentary molecular clouds of the N159W-South region in the Large Magellanic Cloud with an angular resolution of $\sim$0"25 ($\sim$0.07 pc). Although the previous lower-resolution ($\sim$1") ALMA observations revealed that there is a high-mass protostellar object at an intersection of two line-shaped filaments in $^{13}$CO with the length scale of $\sim$10 pc, the spatially resolved observations, in particular, toward the highest column density part traced by the 1.3 mm continuum emission, the N159W-South clump, show complicated hub-filamentary structures. We also discovered that there are multiple protostellar sources with bipolar outflows along the massive filament. The redshifted/blueshifted components of the $^{13}$CO emission around the massive filaments/protostars have complementary distributions, which is considered to be a possible piece of evidence for a cloud-cloud collision. We propose a new scenario in which the supersonically colliding gas flow triggers the formation of both the massive filament and protostars. This is a modification of the earlier scenario of cloud-cloud collision, by Fukui et al., that postulated the two filamentary clouds occur prior to the high-mass star formation. A recent theoretical study of the shock compression in colliding molecular flows by Inoue et al. demonstrates that the formation of filaments with hub structure is a usual outcome of the collision, lending support for the present scenario. The theory argues that the filaments are formed as dense parts in a shock compressed sheet-like layer, which resembles $"$an umbrella with pokes.$"$, Comments: 15 pages, 6 figures; Accepted for publication in ApJ
Published: 2019
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9. The First Maps of κd – the Dust Mass Absorption Coefficient – in Nearby Galaxies, with DustPedia

Author: Viviana Casasola, Sébastien Viaene, R. Evans, Simone Bianchi, Jonathan Ivor Davies, Emmanuel M. Xilouris, P. De Vis, S. C. Madden, S. Verstocken, Frédéric Galliano, Sophia Lianou, I. De Looze, Wouter Dobbels, Christopher J. R. Clark, Maud Galametz, Anthony P. Jones, Nathalie Ysard, Letizia P. Cassarà, Maarten Baes, A. V. Mosenkov, Sterrenkundig Observatorium, Universiteit Gent, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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 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), Universiteit Gent = Ghent University (UGENT), École normale supérieure - Paris (ENS-PSL), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université 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), 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, and PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP)
Subjects: INFRARED-EMISSION, Metallicity, Milky Way, observational [methods], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, CHEMICAL-COMPOSITION, 01 natural sciences, STAR-FORMATION, NUCLEAR STARBURST, 0103 physical sciences, ISM [submillimetre], Mass attenuation coefficient, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Cosmic dust, abundances [ISM], Physics, Spiral galaxy, ISM [galaxies], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, ELEMENTAL ABUNDANCES, HERSCHEL-ATLAS, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, MOLECULAR GAS, Galaxy, Interstellar medium, Physics and Astronomy, Space and Planetary Science, MILKY-WAY, MAGELLANIC-CLOUD, INTERSTELLAR DUST, general [galaxies]
Abstract: The dust mass absorption coefficient, $\kappa_{d}$, is the conversion function used to infer physical dust masses from observations of dust emission. However, it is notoriously poorly constrained, and it is highly uncertain how it varies, either between or within galaxies. Here we present the results of a proof-of concept study, using the DustPedia data for two nearby face-on spiral galaxies M74 (NGC 628) and M83 (NGC 5236), to create the first ever maps of $\kappa_{d}$ in galaxies. We determine $\kappa_{d}$ using an empirical method that exploits the fact that the dust-to-metals ratio of the interstellar medium is constrained by direct measurements of the depletion of gas-phase metals. We apply this method pixel-by-pixel within M74 and M83, to create maps of $\kappa_{d}$. We also demonstrate a novel method of producing metallicity maps for galaxies with irregularly-sampled measurements, using the machine learning technique of Gaussian process regression. We find strong evidence for significant variation in $\kappa_{d}$. We find values of $\kappa_{d}$ at 500 $\mu$m spanning the range 0.11-0.25 ${\rm m^{2}\,kg^{-1}}$ in M74, and 0.15-0.80 ${\rm m^{2}\,kg^{-1}}$ in M83. Surprisingly, we find that $\kappa_{d}$ shows a distinct inverse correlation with the local density of the interstellar medium. This inverse correlation is the opposite of what is predicted by standard dust models. However, we find this relationship to be robust against a large range of changes to our method - only the adoption of unphysical or highly unusual assumptions would be able to suppress it., Comment: Corrected typographical error in Equation A1, as per erratum accepted by MNRAS on 20th April 2022. No results or conclusions effected by the error, or by this correction
Published: 2019
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10. The Herschel Dwarf Galaxy Survey

Author: F. L. Polles, I. De Looze, Diane Cormier, Sacha Hony, A. Lambert-Huyghe, N. P. Abel, Frédéric Galliano, S. C. Madden, Vianney Lebouteiller, Maud Galametz, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), 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), Sterrenkundig Observatorium, Universiteit Gent, University of Cambridge [UK] (CAM), Lebouteiller, Vianney, 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 Cincinnati (UC), Zentrum für Astronomie der Universität Heidelberg (ZAH), Universität Heidelberg [Heidelberg] = Heidelberg University, 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), Universiteit Gent = Ghent University (UGENT), University College of London [London] (UCL), Programme National 'Physique et Chimie du Milieu Interstellaire' (PCMI) of CNRS/INSU with INC/INP co-funded by CEA and CNES.NASA and SOFIA through grant program SOF 05-0084.DFG program HO 5475/2-1.Research Foundation – Flanders(FWO). DAAD/PROCOPE projects 57210883/35265PE., European Project: 702622,H2020,H2020-MSCA-IF-2015,eGALISM(2017), Universität Heidelberg [Heidelberg], 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), and PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP)
Subjects: dwarf [galaxies], Infrared, Astrophysics, 01 natural sciences, FAR-INFRARED LINE, photon-dominated region, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Line (formation), infrared: ISM, Physics, [PHYS.ASTR.GA] Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], ISM [infrared], galaxies: dwarf, radiative transfer, Astrophysics::Earth and Planetary Astrophysics, galaxies: ISM, HII regions, [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], Metallicity, MU-M, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, PHOTODISSOCIATION REGIONS, Photodissociation region, CHEMICAL-COMPOSITION, STAR-FORMATION, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Astrophysics::Galaxy Astrophysics, Dwarf galaxy, ISM [galaxies], INTERSTELLAR-MEDIUM, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Interstellar medium, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Physics and Astronomy, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), IONIZING-RADIATION, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR.IM] Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], ELECTRON-DENSITY, MASSIVE STARS, [PHYS.ASTR.HE] Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], FINE-STRUCTURE LINES
Abstract: The sensitive infrared telescopes, Spitzer and Herschel, have been used to target low-metallicity star-forming galaxies, allowing us to investigate the properties of their interstellar medium (ISM) in unprecedented detail. Interpretation of the observations in physical terms relies on careful modeling of those properties. We have employed a multiphase approach to model the ISM phases (HII region and photodissociation region) with the spectral synthesis code Cloudy. Our goal is to characterize the physical conditions (gas densities, radiation fields, etc.) in the ISM of the galaxies from the Herschel Dwarf Galaxy Survey. We are particularly interested in correlations between those physical conditions and metallicity or star-formation rate. Other key issues we have addressed are the contribution of different ISM phases to the total line emission, especially of the [CII]157um line, and the characterization of the porosity of the ISM. We find that the lower-metallicity galaxies of our sample tend to have higher ionization parameters and galaxies with higher specific star-formation rates have higher gas densities. The [CII] emission arises mainly from PDRs and the contribution from the ionized gas phases is small, typically less than 30% of the observed emission. We also find correlation - though with scatter - between metallicity and both the PDR covering factor and the fraction of [CII] from the ionized gas. Overall, the low metal abundances appear to be driving most of the changes in the ISM structure and conditions of these galaxies, and not the high specific star-formation rates. These results demonstrate in a quantitative way the increase of ISM porosity at low metallicity. Such porosity may be typical of galaxies in the young Universe., Accepted in A&A. 20 pages, 12 figures, 5 tables plus appendices
Published: 2019
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11. Comprehensive comparison of models for spectral energy distributions from 0.1 μ m to 1 mm of nearby star-forming galaxies

Author: I. De Looze, Stefano Zibetti, Laura Silva, L. K. Hunt, Andrea Rossi, Karl D. Gordon, Bruce T. Draine, Jin Koda, D. Calzetti, K. V. Croxall, Bernhard R. Brandl, Karin Sandstrom, Robert C. Kennicutt, M. Galametz, Jd Smith, George Helou, Samir Salim, M. Boquien, Daniel A. Dale, Monica Relaño, Christine D. Wilson, Stefano Bianchi, Gian Luigi Granato, L. Ciesla, J. L. Hinz, Rodrigo Herrera-Camus, R. Nikutta, S. Viaene, Brent Groves, 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 ITA
Subjects: Stellar mass, Extinction (astronomy), FOS: Physical sciences, PHYSICAL-PROPERTIES, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies [infrared], 01 natural sciences, 0103 physical sciences, Galaxy formation and evolution, fundamental parameters [galaxies], Astrophysics::Solar and Stellar Astrophysics, TOTAL INFRARED LUMINOSITY, 010303 astronomy & astrophysics, Scaling, Astrophysics::Galaxy Astrophysics, Physics, DUST ATTENUATION, ISM [galaxies], 010308 nuclear & particles physics, Attenuation, Spectral density, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, FORMATION RATES, MOLECULAR GAS, Galaxy, spiral [galaxies], Physics and Astronomy, STELLAR POPULATION SYNTHESIS, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), COLOR-MAGNITUDE DIAGRAM, Principal component analysis, MULTIPLE-SCATTERING, Astrophysics::Earth and Planetary Astrophysics, star formation [galaxies], galaxies [ultraviolet], INTERSTELLAR DUST, SPITZER OBSERVATIONS
Abstract: We have fit the far-ultraviolet (FUV) to sub-millimeter (850 micron) spectral energy distributions (SEDs) of the 61 galaxies from the "Key Insights on Nearby Galaxies: A Far-Infrared Survey with Herschel" (KINGFISH). The fitting has been performed using three models: the Code for Investigating GALaxy Evolution (CIGALE), the GRAphite-SILicate approach (GRASIL), and the Multi-wavelength Analysis of Galaxy PHYSical properties (MAGPHYS). We have analyzed the results of the three codes in terms of the SED shapes, and by comparing the derived quantities with simple "recipes" for stellar mass (Mstar), star-formation rate (SFR), dust mass (Mdust), and monochromatic luminosities. Although the algorithms rely on different assumptions for star-formation history, dust attenuation and dust reprocessing, they all well approximate the observed SEDs and are in generally good agreement for the associated quantities. However, the three codes show very different behavior in the mid-infrared regime, in particular between 25 and 70 micron where there are no observational constraints for the KINGFISH sample. We find that different algorithms give discordant SFR estimates for galaxies with low specific SFR, and that the standard "recipes" for calculating FUV absorption overestimate the extinction compared to the SED-fitting results. Results also suggest that assuming a "standard" constant stellar mass-to-light ratio overestimates Mstar relative to the SED fitting, and we provide new SED-based formulations for estimating Mstar from WISE W1 (3.4 micron) luminosities and colors. From a Principal Component Analysis of Mstar, SFR, Mdust, and O/H, we reproduce previous scaling relations among Mstar, SFR, and O/H, and find that Mdust can be predicted to within roughly 0.3 dex using only Mstar and SFR., 42 pages, 23 figures, 8 tables, 2 appendices: updated to v2, A&A, accepted
Published: 2019
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12. Modeling ionized gas in low-metallicity environments: the Local Group dwarf galaxy IC 10

Author: F. L. Polles, O. Ł. Karczewski, Sophia Lianou, S. Hony, S. C. Madden, Min-Young Lee, Diane Cormier, N. P. Abel, Frédéric Galliano, Mélanie Chevance, Maud Galametz, V. Lebouteiller, 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'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University of Cincinnati (UC), Zentrum für Astronomie der Universität Heidelberg (ZAH), Universität Heidelberg [Heidelberg], Max-Planck-Institut für Radioastronomie (MPIFR), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Universität Heidelberg [Heidelberg] = Heidelberg University, 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, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)
Subjects: HII regions, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Metallicity, galaxies: individual: IC 10, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Dwarf galaxy, Physics, 010308 nuclear & particles physics, Local Group, Astronomy and Astrophysics, Plasma, Astrophysics - Astrophysics of Galaxies, ISM: lines and bands, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, galaxies: ISM, techniques: spectroscopic
Abstract: Our objective is to investigate the physical properties of the ionised gas of the low-metallicity dwarf galaxy, IC 10, at various spatial scales: from individual HII regions to the entire galaxy scale and examine whether diagnostics for integrated measurements introduce bias in the results. We modeled the ionised gas combining the mid- and far-infrared fine-structure cooling lines observed with Spitzer/IRS and Herschel/PACS, with the photoionisation code Cloudy. The free parameters of the models are the age of the stellar cluster, the density and the ionisation parameter of the ionised gas as well as the depth of the cloud. The latter is used to investigate the leakage of the ionising photons from the analysed regions of IC 10. We investigate HII regions in the main star-forming body, on scales of ~25 pc, three in the main star-forming region in the center of the galaxy and two on the first arc. We then consider larger sizes on the scale of ~200 pc. We find that most clumps have nearly identical properties, density ~10$^{2.} $ - 10$^{2.6}$ cm$^{-3}$, ionisation parameter between 10$^{-2.2}$ and 10$^{-1.6}$ and age of the stellar cluster ~5.5 Myr. All of them are matter-bounded regions, allowing ionising photons to leak. The relatively uniform physical properties of the clumps suggest a common origin for their star formation activity, which could be related to the feedback from stellar winds or supernovae of a previous generation of stars. The properties derived for ~200 pc size "zones" have similar properties as the HII regions they encompass, but with the larger regions tending to be more radiation-bounded. Finally, we investigate the fraction of [CII] 157.7 {\mu}m, [SiII] 34.8 {\mu}m, and [FeII] 25.9 {\mu}m, emission arising from the ionised gas phase and we find that most of the emission originates from the neutral gas, not from the ionised gas., Comment: accepted for publication in A&A
Published: 2019
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13. Indirect evidence of significant grain growth in young protostellar envelopes from polarized dust emission

Author: Stefan Reissl, Valeska Valdivia, Anaëlle Maury, Robert Brauer, Patrick Hennebelle, Vincent Guillet, Maud Galametz, 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), 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), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), and 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)
Subjects: Planetesimal, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, magnetic fields, 01 natural sciences, methods: numerical, Planet, 0103 physical sciences, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], polarization, stars: protostars, Star formation, Astronomy and Astrophysics, Polarization (waves), Astrophysics - Astrophysics of Galaxies, Grain size, Grain growth, Wavelength, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics
Abstract: How and when in the star formation sequence do dust grains start to grow into pebbles is a cornerstone question to both star and planet formation. We compute the polarized radiative transfer from a model solar-type protostellar core, using the POLARIS code, aligning the dust grains with the local magnetic field, following the radiative torques (RATs) theory. We test the dependency of the resulting dust polarized emission with the maximum grain size of the dust size distribution at the envelope scale, from amax = 1 micron to 50 micron. Our work shows that, in the framework of RAT alignment, large dust grains are required to produce polarized dust emission at levels similar to those currently observed in solar-type protostellar envelopes at millimeter wavelengths. Considering the current theoretical dificulties to align a large fraction of small ISM-like grains in the conditions typical of protostellar envelopes, our results suggest that grain growth (typically > 10 micron) might have already significantly progressed at scales 100-1000 au in the youngest objects, observed less than 10^5 years after the onset of collapse. Observations of dust polarized emission might open a new avenue to explore dust pristine properties and describe, for example, the initial conditions for the formation of planetesimals., Accepted for publication in MNRAS. Accepted 2019 July 23. Received 2019 July 23; in original form 2019 April 05
Published: 2019
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14. Probing the cold magnetized Universe with SPICA-POL (B-BOP)

Author: André, Ph., Hughes, A., Guillet, Vincent, Boulanger, F., Bracco, A., Ntormousi, E., Arzoumanian, D., Maury, A. J., Bernard, J.-Ph., Bontemps, Sylvain, Ristorcelli, I., Girart, J. M., Motte, F., Tassis, K., Pantin, E., Montmerle, T., Johnstone, D., Gabici, S., Efstathiou, A., Basu, S., Béthermin, M., Beuther, H., Braine, J., Di Francesco, J., Falgarone, E., Ferrière, K., Fletcher, A., Galametz, M., Giard, M., Hennebelle, P., Jones, A., Kepley, A. A., Kwon, J., Lagache, Guilaine, Lesaffre, Pierre, Levrier, F., Li, D., Li, Z.-Y., Mao, S. A., Nakagawa, T., Onaka, T., Paladino, R., Peretto, N., Poglitsch, A., Reveret, V., Rodriguez, L., Sauvage, M., Soler, J. D., Spinoglio, L., Tabatabaei, F., Tritsis, A., van Der Tak, F., Ward-Thompson, D., Wiesemeyer, H., Ysard, N., Zhang, H., 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 recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), 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), Laboratoire Univers et Particules de Montpellier (LUPM), 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), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Istituto Nazionale di Fisica Nucleare (INFN), FORMATION STELLAIRE 2019, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7 Canada, Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Groupement de Recherche et d'Etudes en Gestion à HEC (GREGH), Ecole des Hautes Etudes Commerciales (HEC Paris)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), 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), University of Cambridge [UK] (CAM), 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), Yangzhou University, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Max Planck Institute for Extraterrestrial Physics (MPE), Telespazio, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Institut für Physik (Institut für Physik), Universität Potsdam, Jeremiah Horrocks Institute for Mathematics, Physics and Astronomy [Preston], University of Central Lancashire [Preston] (UCLAN), Max-Planck-Institut für Radioastronomie (MPIFR), 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), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Laboratoire Pluridisciplinaire de Recherche en Ingénierie des Systèmes, Mécanique et Energétique (PRISME), Université d'Orléans (UO)-Ecole Nationale Supérieure d'Ingénieurs de Bourges (ENSI Bourges), Istituto Nazionale di Fisica Nucleare [Milano] (INFN), APC - Astrophysique des Hautes Energies (APC - AHE), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), 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, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Università di Bologna [Bologna] (UNIBO), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), 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)-Université Fédérale Toulouse Midi-Pyrénées-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), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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), 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), and University of Potsdam = Universität Potsdam
Subjects: Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: SPICA, the cryogenic infrared space telescope recently pre-selected for a `Phase A' concept study as one of the three remaining candidates for ESA's fifth medium class (M5) mission, is foreseen to include a far-infrared polarimetric imager (SPICA-POL, now called B-BOP), which would offer a unique opportunity to resolve major issues in our understanding of the nearby, cold magnetized Universe. This paper presents an overview of the main science drivers for B-BOP, including high dynamic range polarimetric imaging of the cold interstellar medium (ISM) in both our Milky Way and nearby galaxies. Thanks to a cooled telescope, B-BOP will deliver wide-field 100-350 micron images of linearly polarized dust emission in Stokes Q and U with a resolution, signal-to-noise ratio, and both intensity and spatial dynamic ranges comparable to those achieved by Herschel images of the cold ISM in total intensity (Stokes I). The B-BOP 200 micron images will also have a factor ~30 higher resolution than Planck polarization data. This will make B-BOP a unique tool for characterizing the statistical properties of the magnetized interstellar medium and probing the role of magnetic fields in the formation and evolution of the interstellar web of dusty molecular filaments giving birth to most stars in our Galaxy. B-BOP will also be a powerful instrument for studying the magnetism of nearby galaxies and testing galactic dynamo models, constraining the physics of dust grain alignment, informing the problem of the interaction of cosmic rays with molecular clouds, tracing magnetic fields in the inner layers of protoplanetary disks, and monitoring accretion bursts in embedded protostars., Comment: Accepted for publication in PASA; 37 pages, 16 figures
Published: 2019
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15. DustPedia: A Definitive Study of Cosmic Dust in the Local Universe

Author: Anthony P. Jones, Christopher J. R. Clark, Jonathan Ivor Davies, Sébastien Viaene, M. Xilouris, Nathalie Ysard, Suzanne C. Madden, G. Wagle, M. Vika, Aleksandr V. Mosenkov, Sophia Lianou, Maud Galametz, Matthew Smith, Viviana Casasola, M. Bocchio, S. Verstocken, Letizia P. Cassarà, I. De Looze, Frédéric Galliano, Maarten Baes, Simone Bianchi, Jacopo Fritz, Richard Evans, Universiteit Gent = Ghent University (UGENT), Met Office Hadley Centre for Climate Change (MOHC), United Kingdom Met Office [Exeter], 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), Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing [Penteli] (IAASARS), National Observatory of Athens (NOA), Istituto Nazionale di Astrofisica (INAF), 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), Sterrenkundig Observatorium, Laboratoire de Biophotonique et Pharmacologie - UMR 7213 (LBP), Centre National de la Recherche Scientifique (CNRS)-Réseau nanophotonique et optique, Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS), University of Cambridge [UK] (CAM), 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), Universiteit Gent [Ghent], Met Office Hadley Centre (MOHC), 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), 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), Universiteit Gent, Réseau nanophotonique et optique, Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (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), 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 ), Laboratoire AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, Universiteit Gent = Ghent University [Belgium] (UGENT), and Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))
Subjects: (ISM:)dust, galaxies: spiral, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, astronomical databases: miscellaneous, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, cD, symbols.namesake, galaxies:luminosity function, 0103 physical sciences, Planck, galaxies: elliptical and lenticular, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, media_common, Cosmic dust, ISM: general, QB, Physics, COSMIC cancer database, 010308 nuclear & particles physics, Star formation, extinction, Astronomy, Astronomy and Astrophysics, galaxies: dwarf, Astrophysics - Astrophysics of Galaxies, galaxies: general, cD, galaxies: elliptical and lenticular, galaxies: dwarf, extinction, (ISM:)dust, ISM: general, astronomical databases: miscellaneous, galaxies: evolution, galaxies: general, galaxies: ISM, galaxies:luminosity function, mass function, galaxies: spiral, Galaxy, Universe, Interstellar medium, 13. Climate action, Space and Planetary Science, mass function, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), symbols, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The European Space Agency has invested heavily in two cornerstones missions; Herschel and Planck. The legacy data from these missions provides us with an unprecedented opportunity to study cosmic dust in galaxies so that we can answer fundamental questions about, for example: the origin of the chemical elements, physical processes in the interstellar medium (ISM), its effect on stellar radiation, its relation to star formation and how this relates to the cosmic far infrared background. In this paper we describe the DustPedia project, which is enabling us to develop tools and computer models that will help us relate observed cosmic dust emission to its physical properties (chemical composition, size distribution, temperature), to its origins (evolved stars, super novae, growth in the ISM) and the processes that destroy it (high energy collisions and shock heated gas). To carry out this research we will combine the Herschel/Planck data with that from other sources of data, providing observations at numerous wavelengths (< 41) across the spectral energy distribution, thus creating the DustPedia database. To maximise our spatial resolution and sensitivity to cosmic dust we limit our analysis to 4231 local galaxies (v < 3000 km/s) selected via their near infrared luminosity (stellar mass). To help us interpret the data we have developed a new physical model for dust (THEMIS), a new Bayesian method of fitting and interpreting spectral energy distributions (HerBIE) and a state-of-the-art Monte Carlo photon tracing radiative transfer model (SKIRT). In this the first of the DustPedia papers we describe the project objectives, data sets used and provide an insight into the new scientific methods we plan to implement., 66 pages, accepted for publication in PASP
Published: 2017
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16. Erratum: 'Dust and Gas in the Magellanic Clouds from the HERITAGE Herschel Key Project. I. Dust Properties and Insights into the Origin of the Submm Excess Emission' (2014, ApJ, 797, 85)

Author: Karl D. Gordon, Annie Hughes, C. Bot, Monica Rubio, Remy Indebetouw, Frank P. Israel, Maud Galametz, Julia Roman-Duval, Suzanne C. Madden, E. Montiel, Katie Jameson, Marc Sauvage, Akiko Kawamura, Martha L. Boyer, D. Paradis, Karin Sandstrom, Aigen Li, Frédéric Galliano, Mikako Matsuura, Brian Babler, J. Seale, Ramin A. Skibba, Pasquale Panuzzo, Marta Sewilo, Vianney Lebouteiller, Toshikazu Onishi, Yasuo Fukui, Jean-Philippe Bernard, Kirill Tchernyshyov, Karl Misselt, Sacha Hony, Margaret Meixner, K. Okumura, Alberto D. Bolatto, Geoffrey C. Clayton, Charles W. Engelbracht, 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), Centre d'étude spatiale des rayonnements (CESR), 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), Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Department of Physics & Astronomy [Louisiana State University] (LSU), Louisiana State University (LSU), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, 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 Manchester [Manchester], Department of Physics and Astronomy [BatonRouge] (LSU), 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)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, 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 Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), and Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)
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], 010504 meteorology & atmospheric sciences, Astronomy, Astronomy and Astrophysics, 01 natural sciences, Astrobiology, [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, 0103 physical sciences, Key (cryptography), 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract: International audience; Not Available
Published: 2017
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17. KINEMATIC STRUCTURE OF MOLECULAR GAS AROUND HIGH-MASS YSO, PAPILLON NEBULA, IN N159 EAST IN THE LARGE MAGELLANIC CLOUD: A NEW PERSPECTIVE WITH ALMA

Author: Vianney Lebouteiller, C.-H. Rosie Chen, Tetsuhiro Minamidani, Norikazu Mizuno, Yusuke Hattori, Maud Galametz, Suzanne C. Madden, Yuuki Morioka, Tsuyoshi Inoue, Margaret Meixner, Ryohei Harada, Remy Indebetouw, Kengo Tachihara, Akiko Kawamura, Kazuya Saigo, Kazufumi Torii, Marta Sewilo, Akio Ohama, Hiroaki Yamamoto, Toshikazu Onishi, Kazuki Tokuda, Omnarayani Nayak, Yasuo Fukui, Department of Information Engineering, Shinshu University (DIE-SU), Kyoto University, 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), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Kyoto University [Kyoto], Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), and 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)
Subjects: Physics, ISM: kinematics and dynamics, H II region, Nebula, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], stars: formation, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010308 nuclear & particles physics, Star formation, Molecular cloud, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, ISM: clouds, Galaxy, ISM: molecules, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Stars, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], 13. Climate action, Space and Planetary Science, 0103 physical sciences, Large Magellanic Cloud, 010303 astronomy & astrophysics, Line (formation)
Abstract: International audience; We present the ALMA Band 3 and Band 6 results of 12CO(2-1), 13CO(2-1), H30α recombination line, free-free emission around 98 GHz, and the dust thermal emission around 230 GHz toward the N159 East Giant Molecular Cloud (N159E) in the Large Magellanic Cloud (LMC). LMC is the nearest active high-mass star-forming face-on galaxy at a distance of 50 kpc and is the best target for studing high-mass star formation. ALMA observations show that N159E is the complex of filamentary clouds with the width and length of ˜1 pc and several parsecs. The total molecular mass is 0.92 × 105 M⊙ from the 13CO(2-1) intensity. N159E harbors the well-known Papillon Nebula, a compact high-excitation H II region. We found that a YSO associated with the Papillon Nebula has the mass of 35 M⊙ and is located at the intersection of three filamentary clouds. It indicates that the formation of the high-mass YSO was induced by the collision of filamentary clouds. Fukui et al. reported a similar kinematic structure toward two YSOs in the N159 West region, which are the other YSOs that have the mass of ≳35 M⊙. This suggests that the collision of filamentary clouds is a primary mechanism of high-mass star formation. We found a small molecular hole around the YSO in Papillon Nebula with a sub-parsec scale. It is filled by free-free and H30α emission. The temperature of the molecular gas around the hole reaches ˜80 K. It indicates that this YSO has just started the distruction of parental molecular cloud.
Published: 2017
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18. Radiative and mechanical feedback into the molecular gas in the Large Magellanic Cloud

Author: Lee, M.-Y., Madden, S. C., Lebouteiller, Vianney, Gusdorf, A., Godard, B., Wu, R., Galametz, M., Cormier, D., Le Petit, F., Roueff, E., Bron, E., Carlson, L., Chevance, M., Fukui, Y., Galliano, F., Hony, S., Hughes, A., Indebetouw, R., Israel, F. P., Kawamura, A., Le Bourlot, J., Lesaffre, Pierre, Meixner, M., Muller, E., Nayak, O., Onishi, T., Roman-Duval, J., Sewiło, M., 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), 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'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), University of Cambridge [UK] (CAM), Department of Astrophysics [Nagoya], Nagoya University, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institute of Environmental Systems (SUIKO), Kyushu University, 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), 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, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Kyushu University [Fukuoka], and École normale supérieure - Paris (ENS Paris)
Subjects: infrared: ISM, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Magellanic Clouds, ISM: molecules, galaxies: ISM
Abstract: International audience; We present Herschel SPIRE Fourier Transform Spectrometer (FTS) observations of N159W, an active star-forming region in the Large Magellanic Cloud (LMC). In our observations, a number of far-infrared cooling lines, including carbon monoxide (CO) J = 4 → 3 to J = 12 → 11, [CI] 609 μm and 370 μm, and [NII] 205 μm, are clearly detected. With an aim of investigating the physical conditions and excitation processes of molecular gas, we first construct CO spectral line energy distributions (SLEDs) on 10 pc scales by combining the FTS CO transitions with ground-based low-J CO data and analyze the observed CO SLEDs using non-LTE (local thermodynamic equilibrium) radiative transfer models. We find that the CO-traced molecular gas in N159W is warm (kinetic temperature of 153-754 K) and moderately dense (H2 number density of (1.1-4.5) × 103 cm-3). To assess the impact of the energetic processes in the interstellar medium on the physical conditions of the CO-emitting gas, we then compare the observed CO line intensities with the models of photodissociation regions (PDRs) and shocks. We first constrain the properties of PDRs by modeling Herschel observations of [OI] 145 μm, [CII] 158 μm, and [CI] 370 μm fine-structure lines and find that the constrained PDR components emit very weak CO emission. X-rays and cosmic-rays are also found to provide a negligible contribution to theCO emission, essentially ruling out ionizing sources (ultraviolet photons, X-rays, and cosmic-rays) as the dominant heating source for CO in N159W. On the other hand, mechanical heating by low-velocity C-type shocks with 10 km s-1 appears sufficient enough to reproduce the observed warm CO. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.The final reduced Herschel data (FITS files) are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/596/A85
Published: 2016
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19. VizieR Online Data Catalog: Dust properties in galaxies (Remy-Ruyer+, 2015)

Author: Remy-Ruyer, A., Madden, S.~c., Galliano, F., Lebouteiller, V., Baes, M., Bendo, G.~j., Boselli, A., Ciesla, L., Cormier, D., Cooray, A., Cortese, L., Looze, I., Doublier-Pritchard, V., Galametz, M., Jones, A.~p., Karczewski, O.~l., Lu, N., Spinoglio, L., 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: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Interstellar medium, Galaxies: IR, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], Photometry: infrared
Abstract: International audience; For this study, we combine two samples of local galaxies observed with Herschel: the Dwarf Galaxy Survey (DGS, Madden et al., 2013PASP..125..600M) and the Key Insights on Nearby Galaxies: a Far-Infrared Survey with Herschel (KINGFISH, Kennicutt et al., 2011PASP..123.1347K). (7 data files).
Published: 2016

20. The dust properties and physical conditions of the interstellar medium in the LMC massive star-forming complex N11

Author: J.M. Oliviera, Sacha Hony, Annie Hughes, S. C. Madden, C. Bot, Alberto D. Bolatto, Vianney Lebouteiller, Maud Galametz, Julia Roman-Duval, Diane Cormier, D. Paradis, Min-Young Lee, Toshikazu Onishi, Monica Rubio, Frank P. Israel, Yasuo Fukui, Akiko Kawamura, Margaret Meixner, Frédéric Galliano, Marta Sewilo, M. Albrecht, Eric W. Pellegrini, University of Cambridge [UK] (CAM), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Leibniz-Institut für Kristallzüchtung, 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), 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), Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, 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), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Météo-France [Paris], Météo France, Institut Laue-Langevin (ILL), ILL, Department of Astrophysics [Nagoya], Nagoya University, Institute of Environmental Systems (SUIKO), Kyushu University [Fukuoka], 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), Universiteit Leiden, Météo-France, and Kyushu University
Subjects: [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], 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Magellanic Clouds, Astrophysics::Solar and Stellar Astrophysics, Large Magellanic Cloud, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Cosmic dust, Line (formation), ISM: general, Physics, infrared: ISM, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy, Spectral density, Astronomy and Astrophysics, galaxies: dwarf, Intergalactic dust, Mass ratio, Astrophysics - Astrophysics of Galaxies, Galaxy, Interstellar medium, submillimetre: ISM, [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), Astrophysics::Earth and Planetary Astrophysics, galaxies: ISM
Abstract: We combine Spitzer and Herschel data of the star-forming region N11 in the Large Magellanic Cloud to produce detailed maps of the dust properties in the complex and study their variations with the ISM conditions. We also compare APEX/LABOCA 870um observations with our model predictions in order to decompose the 870um emission into dust and non-dust (free-free emission and CO(3-2) line) contributions. We find that in N11, the 870um can be fully accounted for by these 3 components. The dust surface density map of N11 is combined with HI and CO observations to study local variations in the gas-to-dust mass ratios. Our analysis leads to values lower than those expected from the LMC low-metallicity as well as to a decrease of the gas-to-dust mass ratio with the dust surface density. We explore potential hypotheses that could explain the low observed gas-to-dust mass ratios (variations in the XCO factor, presence of CO-dark gas or of optically thick HI or variations in the dust abundance in the dense regions). We finally decompose the local SEDs using a Principal Component Analysis (i.e. with no a priori assumption on the dust composition in the complex). Our results lead to a promising decomposition of the local SEDs in various dust components (hot, warm, cold) coherent with that expected for the region. Further analysis on a larger sample of galaxies will follow in order to understand how unique this decomposition is or how it evolves from one environment to another., 24 pages, 16 figures, accepted for publication in MNRAS
Published: 2015
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21. Linking dust emission to fundamental properties in galaxies: the low-metallicity picture

Author: Laure Ciesla, V. Doublier-Pritchard, Anthony P. Jones, Nanyao Y. Lu, L. Spinoglio, George J. Bendo, Maarten Baes, I. De Looze, Luca Cortese, Alessandro Boselli, Frédéric Galliano, Diane Cormier, Maud Galametz, O. Ł. Karczewski, A. Cooray, A. Rémy-Ruyer, Vianney Lebouteiller, Suzanne C. Madden, 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), 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), Sterrenkundig Observatorium, Universiteit Gent = Ghent University (UGENT), 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), ANR-11-BS56-0023,SYMPATICO,SYnthetic MultiPhase Analysis of The Ism of Cosmic Objects(2011), European Project: 606847,EC:FP7:SPA,FP7-SPACE-2013-1,DUSTPEDIA(2014), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Universiteit Gent, 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: HERSCHEL REFERENCE SURVEY, ACTIVE GALACTIC NUCLEI, dwarf [galaxies], Infrared, Metallicity, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, galaxies [infrared], Luminosity, infrared: galaxies, POLYCYCLIC AROMATIC-HYDROCARBONS, 0103 physical sciences, COMPACT DWARF GALAXIES, evolution, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, Black-body radiation, TO-GAS RATIO, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Dwarf galaxy, Physics, infrared: ISM, 010308 nuclear & particles physics, extinction, Sigma, ISM [infrared], Astronomy and Astrophysics, HUBBLE-SPACE-TELESCOPE, galaxies: dwarf, Mass ratio, Astrophysics - Astrophysics of Galaxies, Galaxy, SPECTRAL ENERGY-DISTRIBUTION, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), MULTIBAND IMAGING PHOTOMETER, LARGE-MAGELLANIC-CLOUD, Astrophysics::Earth and Planetary Astrophysics, dust, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: In this work, we aim at providing a consistent analysis of the dust properties from metal-poor to metal-rich environments by linking them to fundamental galactic parameters. We consider two samples of galaxies: the Dwarf Galaxy Survey (DGS) and KINGFISH, totalling 109 galaxies, spanning almost 2 dex in metallicity. We collect infrared (IR) to submillimetre (submm) data for both samples and present the complete data set for the DGS sample. We model the observed spectral energy distributions (SED) with a physically-motivated dust model to access the dust properties. Using a different SED model (modified blackbody), dust composition (amorphous carbon), or wavelength coverage at submm wavelengths results in differences in the dust mass estimate of a factor two to three, showing that this parameter is subject to non-negligible systematic modelling uncertainties. For eight galaxies in our sample, we find a rather small excess at 500 microns (< 1.5 sigma). We find that the dust SED of low-metallicity galaxies is broader and peaks at shorter wavelengths compared to more metal-rich systems, a sign of a clumpier medium in dwarf galaxies. The PAH mass fraction and the dust temperature distribution are found to be driven mostly by the specific star-formation rate, SSFR, with secondary effects from metallicity. The correlations between metallicity and dust mass or total-IR luminosity are direct consequences of the stellar mass-metallicity relation. The dust-to-stellar mass ratios of metal-rich sources follow the well-studied trend of decreasing ratio for decreasing SSFR. The relation is more complex for highly star-forming low-metallicity galaxies and depends on the chemical evolutionary stage of the source (i.e., gas-to-dust mass ratio). Dust growth processes in the ISM play a key role in the dust mass build-up with respect to the stellar content at high SSFR and low metallicity. (abridged), 44 pages (20 pages main body plus 5 Appendices), 11 figures, 9 tables, accepted for publication in A&A
Published: 2015
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22. Star-forming Blue ETGs in Two Newly Discovered Galaxy Overdensities in the HUDF at z=1.84 and 1.9: Unveiling the Progenitors of Passive ETGs in Cluster Cores

Author: Simona Mei, Steven L. Finkelstein, Casey Papovich, Anton M. Koekemoer, Jeffrey A. Newman, Benjamin J. Weiner, Marc Rafelski, Matthew L. N. Ashby, Laura Pentericci, Harry I. Tepliz, Claudia Scarlata, Norman A. Grogin, Audrey Galametz, Ray A. Lucas, Caterina Lani, C. J. Conselice, Marc Huertas-Company, Marco Castellano, 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), AUTRES, INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Space Telescope Science Institute (STSci), Observatoire de Paris, and Université Paris sciences et lettres (PSL)
Subjects: Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star (game theory), Population, FOS: Physical sciences, Velocity dispersion, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Instability, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, galaxies: clusters: general, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Hubble space telescope, 0103 physical sciences, Cluster (physics), education, galaxies: evolution, 010303 astronomy & astrophysics
Abstract: We present the discovery of two galaxy overdensities in the Hubble Space Telescope UDF: a proto-cluster, HUDFJ0332.4-2746.6 at $z = 1.84 \pm 0.01$, and a group, HUDFJ0332.5-2747.3 at $z =1.90 \pm 0.01$. Assuming viralization, the velocity dispersion of HUDFJ0332.4-2746.6 implies a mass of $M_{200}= (2.2 \pm 1.8) \times 10^{14} M_{\odot}$, consistent with the lack of extended X-ray emission. Neither overdensity shows evidence of a red sequence. About $50\%$ of their members show interactions and/or disturbed morphologies, which are signatures of merger remnants or disk instability. Most of their ETGs have blue colors and show recent star-formation. These observations reveal for the first time large fractions of spectroscopically confirmed star-forming blue ETGs in proto-clusters at $z\approx 2$. These star-forming ETGs are most likely among the progenitors of the quiescent population in clusters at more recent epochs. Their mass-size relation is consistent with that of passive ETGs in clusters at $z\sim0.7-1.5$. If these galaxies are the progenitors of cluster ETGs at these lower redshifts, their size would evolve according to a similar mass-size relation. It is noteworthy that quiescent ETGs in clusters at $z=1.8-2$ also do not show any significant size evolution over this redshift range, contrary to field ETGs. The ETG fraction is $\lesssim 50\%$, compared to the typical quiescent ETG fraction of $\approx 80\%$ in cluster cores at $z< 1$. The fraction, masses, and colors of the newly discovered ETGs imply that other cluster ETGs will be formed/accreted at a later time., 33 pages, 13 figures. ApJ, in press
Published: 2015
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23. Erratum: 'The Herschel Inventory of the Agents of Galaxy Evolution (Heritage) in the Magellanic Clouds, a Herschel Open Time Key Program' (2013, AJ, 146, 62)

Author: Alberto D. Bolatto, Karl D. Gordon, Sundar Srinivasan, Linda J. Smith, Marc Sauvage, P. Chanial, Barbara A. Whitney, Remy Indebetouw, Frank P. Israel, K. Okumura, Martha L. Boyer, Tracy L. Beck, E. Montiel, Francisca Kemper, Mikako Matsuura, C. Bot, Pasquale Panuzzo, L. R. Carlson, Ramin A. Skibba, J. Seale, Brian Babler, Alexander G. G. M. Tielens, S. Hony, Yasuo Fukui, C.-H. R. Chen, Diane Cormier, Joseph L. Hora, Thomas P. Robitaille, Masaaki Otsuka, J.-P. Bernard, Sungeun Kim, Vianney Lebouteiller, Marta Sewilo, Annie Hughes, Chad Engelbracht, Karl Misselt, Toshikazu Onishi, Erik Muller, B. A. Sargent, Julia Roman-Duval, William T. Reach, Geoffrey C. Clayton, D. Paradis, Joana M. Oliveira, Maud Galametz, E. Kwon, Margaret Meixner, Monica Rubio, Frédéric Galliano, Aigen Li, Akiko Kawamura, Albrecht Poglitsch, S. C. Madden, Knox S. Long, J. Th. van Loon, 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), 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), Steward Observatory, University of Arizona, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, 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), Department of Astrophysics [Nagoya], Nagoya University, University of Cambridge [UK] (CAM), University of Virginia, Leiden Observatory [Leiden], Universiteit Leiden, Institute of Environmental Systems (SUIKO), Kyushu University, 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), Department of Physics and Astronomy [UCL London], University College of London [London] (UCL), Météo-France, Max-Planck-Institut für Extraterrestrische Physik (MPE), inconnu, Inconnu, 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), University of Virginia [Charlottesville], Universiteit Leiden [Leiden], Kyushu University [Fukuoka], Météo-France [Paris], Météo France, and PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, 010504 meteorology & atmospheric sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Milky Way, Subtraction, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Table (information), 01 natural sciences, Galaxy, Spire, Space and Planetary Science, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Galaxy formation and evolution, Calibration, Cirrus, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract: We provide a corrected Table 4 that lists the total galaxy fluxes for the HERTIAGE bands and corresponding Figure 19 which plots these fluxes in comparison to prior measurements These corrected fluxes differ by up to 41% to what we reported in the original paper. These revised fluxes utilize a more appropriate subtraction of the Milky Way Foreground Cirrus emission which contaminates especially the PACS 100 and 160 micron bands. The subtraction process uses the HI 21 cm emission to develop a model for the MW cirrus dust emission. In addition, the better subtraction process corrected for an over subtraction of the background in the SPIRE images of the SMC that occurred during the original data processing. The need for these better foreground subtractions was realized while working on an analysis of the dust masses and gas-to-dust ratios in the LMC and SMC reported by Gordon et al. (2014) and Roman-Duval et al. (2014). After the subtraction has been done, the fluxes were derived by simply summing up all the pixels in the image. The errors we quote for the fluxes reflect the absolute flux calibration errors for extended sources which are approx.10% for PACS and approx. 8% for SPIRE. In the revised Figure 19, we confirm that these corrected global fluxes remain within the range of prior global measurements for both the LMC and SMC. Indeed, the shape of the corrected spectral energy distributions appears better aligned with prior measurements.
Published: 2015
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24. 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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25. Cool dust heating and temperature mixing in nearby star-forming galaxies

Author: Jin Koda, R. C. Kennicutt, Marc Sauvage, Karin Sandstrom, Maud Galametz, Kevin V. Croxall, Karl D. Gordon, A. Gil de Paz, Médéric Boquien, Daniel A. Dale, Alberto D. Bolatto, Christine D. Wilson, George Helou, Simone Bianchi, Leslie K. Hunt, Juan-Carlos Muñoz-Mateos, G. Aniano, Daniela Calzetti, Bruce T. Draine, Stefano Zibetti, Joannah L. Hinz, Helene Roussel, L. Vigroux, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), 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), 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 Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), and ITA
Subjects: HERSCHEL REFERENCE SURVEY, Brightness, DWARF GALAXIES, INFRARED-EMISSION, FOS: Physical sciences, SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radiation, 60 MU-M, Emissivity, Astrophysics::Solar and Stellar Astrophysics, COLD DUST, SMALL-MAGELLANIC-CLOUD, Astrophysics::Galaxy Astrophysics, SUBMILLIMETER EXCESS EMISSION, Physics, Range (particle radiation), ISM [galaxies], extinction, Astronomy and Astrophysics, Radius, Astrophysics - Astrophysics of Galaxies, Galaxy, Interstellar medium, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, dust, star formation [galaxies], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], SPIRAL GALAXIES, INTERSTELLAR DUST, galaxies: ISM
Abstract: Physical conditions of the interstellar medium in galaxies are closely linked to the ambient radiation field and the heating of dust grains. In order to characterize dust properties in galaxies over a wide range of physical conditions, we present here the radial surface brightness profiles of the entire sample of 61 galaxies from Key Insights into Nearby Galaxies: Far-Infrared Survey with Herschel (KINGFISH). The main goal of our work is the characterization of the grain emissivities, dust temperatures, and interstellar radiation fields responsible for heating the dust. After fitting the dust and stellar radial profiles with exponential functions, we fit the far-infrared spectral energy distribution (SED) in each annular region with single-temperature modified black bodies using both variable (MBBV) and fixed (MBBF) emissivity indices beta, as well as with physically motivated dust models. Results show that while most SED parameters decrease with radius, the emissivity index beta also decreases with radius in some galaxies, but in others is increasing, or rising in the inner regions and falling in the outer ones. Despite the fixed grain emissivity (average beta~ 2.1) of the physically-motivated models, they are well able to accommodate flat spectral slopes with beta, 28 pages, 20 figures, accepted for publication in A&A
Published: 2015
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26. The Herschel Dwarf Galaxy Survey: I. Properties of the low-metallicity ISM from PACS spectroscopy

Author: Cormier, D., Madden, S. C., Lebouteiller, V., Abel, N., Hony, S., Galliano, F., Rémy-Ruyer, A., Bigiel, F., Baes, M., Boselli, A., Chevance, M., Cooray, A., de Looze, I., Doublier, V., Galametz, M., Hughes, T., Karczewski, O. Ł., Lee, M.-Y., Lu, N., Spinoglio, L., Universität Heidelberg [Heidelberg], 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), 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), ANR-11-BS56-0023,SYMPATICO,SYnthetic MultiPhase Analysis of The Ism of Cosmic Objects(2011), Universität Heidelberg [Heidelberg] = Heidelberg University, 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), 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: infrared: ISM, HII regions, radiative transfer, photon-dominated region (PDR), galaxies: dwarf, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], techniques: spectroscopic
Abstract: International audience; Context. The far-infrared (FIR) lines are important tracers of the cooling and physical conditions of the interstellar medium (ISM) and are rapidly becoming workhorse diagnostics for galaxies throughout the universe. There are clear indications of a different behavior of these lines at low metallicity that needs to be explored. Aims. Our goal is to explain the main differences and trends observed in the FIR line emission of dwarf galaxies compared to more metal-rich galaxies, and how this translates in ISM properties. Methods. We present Herschel/PACS spectroscopic observations of the [C ii] 157 μm, [O i] 63 and 145 μm, [O iii] 88 μm, [N ii] 122 and 205 μm, and [N iii] 57 μm fine-structure cooling lines in a sample of 48 low-metallicity star-forming galaxies of the guaranteed time key program Dwarf Galaxy Survey. We correlate PACS line ratios and line-to-LTIR ratios with LTIR, LTIR/LB, metallicity, and FIR color, and interpret the observed trends in terms of ISM conditions and phase filling factors with Cloudy radiative transfer models. Results. We find that the FIR lines together account for up to 3 percent of LTIR and that star-forming regions dominate the overall emission in dwarf galaxies. Compared to metal-rich galaxies, the ratios of [O iii]88/[N ii]122 and [N iii]57/[N ii]122 are high, indicative of hard radiation fields. In the photodissociation region (PDR), the [C ii]157/[O i]63 ratio is slightly higher than in metal-rich galaxies, with a small increase with metallicity, and the [O i]145/[O i]63 ratio is generally lower than 0.1, demonstrating that optical depth effects should be small on the scales probed. The [O iii]88/[O i]63 ratio can be used as an indicator of the ionized gas/PDR filling factor, and is found to be ~4 times higher in the dwarfs than in metal-rich galaxies. The high [C ii]/LTIR, [O i]/LTIR, and [O iii]/LTIR ratios, which decrease with increasing LTIR and LTIR/LB, are interpreted as a combination of moderate far-UV fields and a low PDR covering factor. Harboring compact phases of a low filling factor and a large volume filling factor of diffuse gas, the ISM of low-metallicity dwarf galaxies has a more porous structure than that of metal-rich galaxies.
Published: 2015
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27. 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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28. THE PHYSICAL CHARACTERISTICS OF THE GAS IN THE DISK OF CENTAURUS A USING THE HERSCHEL SPACE OBSERVATORY

Author: Christine D. Wilson, I. De Looze, Médéric Boquien, L. Spinoglio, Alessandro Boselli, M. R. P. Schirm, Matthew Smith, Helene Roussel, Maarten Baes, Vianney Lebouteiller, Suzanne C. Madden, D. Cormier, O. Ł. Karczewski, Maud Galametz, T. J. Parkin, McMaster University [Hamilton, Ontario], Sterrenkundig Observatorium, Universiteit Gent = Ghent University (UGENT), 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), Universität Heidelberg [Heidelberg] = Heidelberg University, University of Cambridge [UK] (CAM), 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), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), AUTRES, Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Universiteit Gent, 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), Universität Heidelberg [Heidelberg], 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: ULTRALUMINOUS INFRARED GALAXIES, C-II, Centaurus A, Doubly ionized oxygen, MU-M, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, PHOTODISSOCIATION REGIONS, 01 natural sciences, PHOTON-DOMINATED REGIONS, 0103 physical sciences, STAR-FORMING GALAXIES, EARLY-TYPE GALAXIES, Emission spectrum, Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB, Physics, individual (Centaurus A) [galaxies], Spiral galaxy, ISM [galaxies], INTERSTELLAR-MEDIUM, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, ISM [infrared], Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, MOLECULAR GAS, Interstellar medium, Physics and Astronomy, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), NGC 5128, Elliptical galaxy, lines and bands [ISM]
Abstract: We search for variations in the disk of Centaurus A of the emission from atomic fine structure lines using Herschel PACS and SPIRE spectroscopy. In particular we observe the [C II](158 $\mu$m), [N II](122 and 205 $\mu$m), [O I](63 and 145 $\mu$m) and [O III](88 $\mu$m) lines, which all play an important role in cooling the gas in photo-ionized and photodissociation regions. We determine that the ([C II]+[O I]$_{63}$)/$F_{TIR}$ line ratio, a proxy for the heating efficiency of the gas, shows no significant radial trend across the observed region, in contrast to observations of other nearby galaxies. We determine that 10 - 20% of the observed [C II] emission originates in ionized gas. Comparison between our observations and a PDR model shows that the strength of the far-ultraviolet radiation field, $G_0$, varies between $10^{1.75}$ and $10^{2.75}$ and the hydrogen nucleus density varies between $10^{2.75}$ and $10^{3.75}$ cm$^{-3}$, with no significant radial trend in either property. In the context of the emission line properties of the grand-design spiral galaxy M51 and the elliptical galaxy NGC 4125, the gas in Cen A appears more characteristic of that in typical disk galaxies rather than elliptical galaxies., Comment: Accepted for publication in the Astrophysical Journal. 22 pages, 10 figures, 5 tables
Published: 2014
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29. Dust spectral energy distributions of nearby galaxies: an insight from the Herschel Reference Survey

Author: Luca Cortese, Stephen Anthony Eales, S. C. Madden, Alessandro Boselli, George J. Bendo, Maarten Baes, Matthew Smith, Sébastien Viaene, Sebastien Heinis, Laure Ciesla, I. De Looze, S. di Serego Alighieri, V. Buat, Daniele Pierini, A. Rémy-Ruyer, Thomas M. Hughes, Simone Bianchi, Catherine Vlahakis, Médéric Boquien, Frédéric Galliano, L. Spinoglio, Maud Galametz, Mattia Vaccari, 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), Sterrenkundig Observatorium, Universiteit Gent, Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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 Universiteit Gent = Ghent University (UGENT)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar population, Infrared, Metallicity, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies [infrared], infrared: galaxies, POLYCYCLIC AROMATIC-HYDROCARBONS, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, Surface brightness, SMALL-MAGELLANIC-CLOUD, education, Astrophysics::Galaxy Astrophysics, QB, SPITZER-SPACE-TELESCOPE, Physics, education.field_of_study, ISM [galaxies], extinction, Astronomy and Astrophysics, MID-IR EMISSION, VIRGO CLUSTER, Astrophysics - Astrophysics of Galaxies, FAR-INFRARED PROPERTIES, Galaxy, Stars, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, dust, Low Mass, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], SPIRAL GALAXIES, LOW-METALLICITY ENVIRONMENTS, INTERSTELLAR DUST, galaxies: ISM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We gather infrared (IR) photometric data from 8 to 500 microns (Spitzer, WISE, IRAS and Herschel) for all of the HRS galaxies. Draine & Li (2007) models are fit to the data from which the stellar contribution has been carefully removed. We find that our photometric coverage is sufficient to constrain all of the models parameters and that a strong constraint on the 20-60 microns range is mandatory to estimate the relative contribution of the photo-dissociation regions to the IR SED. The SED models tend to systematically under-estimate the observed 500 microns flux densities, especially for low mass systems. We provide the output parameters for all of the galaxies: the minimum intensity of the interstellar radiation field (ISRF), the fraction of PAH, the relative contribution of PDR and evolved stellar population to the dust heating, the $M_{dust}$ and the $L_{IR}$. For a subsample of gas-rich galaxies, we analyze the relations between these parameters and the integrated properties of galaxies, such as $M_*$, SFR, metallicity, H$\alpha$ and H-band surface brightness, and the FUV attenuation. A good correlation between the fraction of PAH and the metallicity is found implying a weakening of the PAH emission in galaxies with low metallicities. The intensity of the IRSF and the H-band and H$\alpha$ surface brightnesses are correlated, suggesting that the diffuse dust component is heated by both the young stars in star forming regions and the diffuse evolved population. We use these results to provide a new set of IR templates calibrated with Herschel observations on nearby galaxies and a mean SED template to provide the z=0 reference for cosmological studies. For the same purpose, we put our sample on the SFR-$M_*$ diagram. The templates are compared to the most popular IR SED libraries, enlightening a large discrepancy between all of them in the 20-100 microns range., Comment: 37 pages, 17 figures, 11 tables, accepted for publication in A&A
Published: 2014
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30. A resolved analysis of cold dust and gas in the nearby edge-on spiral NGC 891

Author: Jonathan Ivor Davies, Alessandro Boselli, L. Spinoglio, F. Allaert, George J. Bendo, Jacopo Fritz, A. Rémy-Ruyer, Maud Galametz, Gianfranco Gentile, Sébastien Viaene, T. M. Hughes, Médéric Boquien, T. J. Parkin, Matthew Smith, I. De Looze, Suzanne C. Madden, David L. Clements, Christine D. Wilson, Maarten Baes, Joris Verstappen, Simone Bianchi, Sterrenkundig Observatorium, Universiteit Gent = Ghent University (UGENT), 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), Universiteit Gent, 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), 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), Astrophysics, and Astronomy and Astrophysics Research Group
Subjects: HERSCHEL REFERENCE SURVEY, submillimeter: galaxies, galaxies: spiral, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar population, FOS: Physical sciences, galaxies [submillimeter], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, LOCAL GALAXY ANDROMEDA, galaxies [infrared], 01 natural sciences, infrared: galaxies, POLYCYCLIC AROMATIC-HYDROCARBONS, CO-TO-H-2 CONVERSION FACTOR, VIRGO CLUSTER SURVEY, 0103 physical sciences, galaxies: individual: NGC 891, Emissivity, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, SPITZER-SPACE-TELESCOPE, Physics, Spectral index, NEUTRAL HYDROGEN OBSERVATIONS, Spiral galaxy, ISM [galaxies], Mass distribution, 010308 nuclear & particles physics, Star formation, CLERK-MAXWELL-TELESCOPE, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, spiral [galaxies], Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), individual: NGC 891 [galaxies], MULTIBAND IMAGING PHOTOMETER, Hydrogen line, Spectral energy distribution, LARGE-MAGELLANIC-CLOUD, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We investigate the connection between dust and gas in the nearby edge-on spiral galaxy NGC 891. High resolution Herschel PACS and SPIRE 70, 100, 160, 250, 350, and 500 $\mu$m images are combined with JCMT SCUBA 850 $\mu$m observations to trace the far-infrared/submillimetre spectral energy distribution (SED). Maps of the HI 21 cm line and CO(J=3-2) emission trace the atomic and molecular hydrogen gas, respectively. We fit one-component modified blackbody models to the integrated SED, finding a global dust mass of 8.5$\times$10$^{7}$ M$_{\odot}$ and an average temperature of 23$\pm$2 K. We also fit the pixel-by-pixel SEDs to produce maps of the dust mass and temperature. The dust mass distribution correlates with the total stellar population as traced by the 3.6 $\mu$m emission. The derived dust temperature, which ranges from approximately 17 to 24 K, is found to correlate with the 24 $\mu$m emission. Allowing the dust emissivity index to vary, we find an average value of $\beta$ = 1.9$\pm$0.3. We confirm an inverse relation between the dust emissivity spectral index and dust temperature, but do not observe any variation of this relationship with vertical height from the mid-plane of the disk. A comparison of the dust properties with the gaseous components of the ISM reveals strong spatial correlations between the surface mass densities of dust and the molecular hydrogen and total gas surface densities. Observed asymmetries in the dust temperature, and the H$_{2}$-to-dust and total gas-to-dust ratios hint that an enhancement in the star formation rate may be the result of larger quantities of molecular gas available to fuel star formation in the NE compared to the SW. Whilst the asymmetry likely arises from dust obscuration due to the geometry of the line-of-sight projection of the spiral arms, we cannot exclude an enhancement in the star formation rate in the NE side of the disk., Comment: Accepted for publication in A&A. 21 pages, including 13 figures and 4 tables
Published: 2014
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31. COLD DUST BUT WARM GAS IN THE UNUSUAL ELLIPTICAL GALAXY NGC 4125

Author: A. Cridland, A. Cooray, K. Foyle, Walter Kieran Gear, I. De Looze, Marc Sauvage, Médéric Boquien, Suzanne C. Madden, Christine D. Wilson, A. Rémy-Ruyer, Maarten Baes, Matthew Smith, Helene Roussel, David L. Clements, Miguel Pereira-Santaella, Laure Ciesla, E. Mentuch Cooper, T. J. Parkin, George J. Bendo, Alessandro Boselli, Vianney Lebouteiller, Maud Galametz, 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), 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 (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: HERSCHEL REFERENCE SURVEY, Cosmology and Nongalactic Astrophysics (astro-ph.CO), C-II, Stellar mass, Astrophysics::High Energy Astrophysical Phenomena, MU-M, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, SCALING RELATIONS, 01 natural sciences, galaxies [infrared], STAR-FORMATION, cD, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, NEARBY GALAXIES, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), individual (NGC 4125) [galaxies], Astrophysics::Galaxy Astrophysics, QB, Cosmic dust, Physics, Luminous infrared galaxy, INTERSTELLAR-MEDIUM, ISM [galaxies], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, MOLECULAR GAS, Interstellar medium, OBSCURED GALAXIES, Astrophysics - Solar and Stellar Astrophysics, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Elliptical galaxy, Astrophysics::Earth and Planetary Astrophysics, MAGELLANIC-CLOUD, elliptical and lenticular [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Data from the Herschel Space Observatory have revealed an unusual elliptical galaxy, NGC 4125, which has strong and extended submillimeter emission from cold dust but only very strict upper limits to its CO and HI emission. Depending on the dust emissivity, the total dust mass is 2-5x10^6 Msun. While the neutral gas-to-dust mass ratio is extremely low (< 12-30), including the ionized gas traced by [CII] emission raises this limit to < 39-100. The dust emission follows a similar r^{1/4} profile to the stellar light and the dust to stellar mass ratio is towards the high end of what is found in nearby elliptical galaxies. We suggest that NGC 4125 is currently in an unusual phase where evolved stars produced in a merger-triggered burst of star formation are pumping large amounts of gas and dust into the interstellar medium. In this scenario, the low neutral gas-to-dust mass ratio is explained by the gas being heated to temperatures >= 10^4 K faster than the dust is evaporated. If galaxies like NGC 4125, where the far-infrared emission does not trace neutral gas in the usual manner, are common at higher redshift, this could have significant implications for our understanding of high redshift galaxies and galaxy evolution., Accepted to ApJ Letters
Published: 2013
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32. THE HERSCHEL INVENTORY OF THE AGENTS OF GALAXY EVOLUTION IN THE MAGELLANIC CLOUDS, A HERSCHEL OPEN TIME KEY PROGRAM

Author: Sungeun Kim, Pasquale Panuzzo, Martha L. Boyer, Barbara A. Whitney, William T. Reach, Geoffrey C. Clayton, Chad Engelbracht, E. Montiel, Francisca Kemper, Tracy L. Beck, Thomas P. Robitaille, Alberto D. Bolatto, Marc Sauvage, J.-P. Bernard, Sundar Srinivasan, Albrecht Poglitsch, C. Bot, D. Paradis, K. Okumura, Toshikazu Onishi, S. C. Madden, Joana M. Oliveira, B. A. Sargent, Karl Misselt, Frédéric Galliano, Maud Galametz, L. R. Carlson, Ramin A. Skibba, Monica Rubio, Marta Sewilo, Julia Roman-Duval, C.-H. R. Chen, Margaret Meixner, Aigen Li, Alexander G. G. M. Tielens, Erik Muller, Annie Hughes, Masaaki Otsuka, E. Kwon, Akiko Kawamura, Vianney Lebouteiller, J. Seale, Mikako Matsuura, Brian Babler, Yasuo Fukui, Diane Cormier, Joseph L. Hora, Knox S. Long, J. Th. van Loon, Sacha Hony, Karl D. Gordon, Linda J. Smith, P. Chanial, Remy Indebetouw, Frank P. Israel, 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), Steward Observatory, University of Arizona, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), Matrice extracellulaire et dynamique cellulaire - UMR 7369 (MEDyC), SFR CAP Santé (Champagne-Ardenne Picardie Santé), Université de Reims Champagne-Ardenne (URCA)-Université de Picardie Jules Verne (UPJV)-Université de Reims Champagne-Ardenne (URCA)-Université de Picardie Jules Verne (UPJV)-Université de Reims Champagne-Ardenne (URCA)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, 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), University of California [Los Angeles] (UCLA), University of California, Laboratoire de Génie Civil et Génie Mécanique (LGCGM), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA), Department of Astrophysics [Nagoya], Nagoya University, University of Cambridge [UK] (CAM), Institute of Environmental Systems (SUIKO), Kyushu University [Fukuoka], Institute of Oceanology [China], Earth Consultants International, Department of Physics and Astronomy [UCL London], University College of London [London] (UCL), CQ-VR, Universidade de Trás-os-Montes e Alto Douro, Météo-France [Paris], Météo France, Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Centre de recherche de l'hôpital Sainte Justine, CHU Sainte Justine [Montréal], inconnu, Inconnu, 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), 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), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), University of California (UC), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA), Kyushu University, Météo-France, Centre de recherche du CHU Sainte-Justine / Research Center of the Sainte-Justine University Hospital [Montreal, Canada], Université de Montréal (UdeM)-CHU Sainte Justine [Montréal], Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Luminous infrared galaxy, 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], 010308 nuclear & particles physics, Young stellar object, Extinction (astronomy), Astronomy, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Interstellar medium, [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], 13. Climate action, Space and Planetary Science, 0103 physical sciences, Small Magellanic Cloud, Large Magellanic Cloud, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Cosmic dust, QB
Abstract: We present an overview of the HERschel Inventory of The Agents of Galaxy Evolution (HERITAGE) in the Magellanic Clouds project, which is a Herschel Space Observatory open time key program. We mapped the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) at 100, 160, 250, 350, and 500 μm with the Spectral and Photometric Imaging Receiver (SPIRE) and Photodetector Array Camera and Spectrometer (PACS) instruments on board Herschel using the SPIRE/PACS parallel mode. The overriding science goal of HERITAGE is to study the life cycle of matter as traced by dust in the LMC and SMC. The far-infrared and submillimeter emission is an effective tracer of the interstellar medium (ISM) dust, the most deeply embedded young stellar objects (YSOs), and the dust ejected by the most massive stars. We describe in detail the data processing, particularly for the PACS data, which required some custom steps because of the large angular extent of a single observational unit and overall the large amount of data to be processed as an ensemble. We report total global fluxes for the LMC and SMC and demonstrate their agreement with measurements by prior missions. The HERITAGE maps of the LMC and SMC are dominated by the ISM dust emission and bear most resemblance to the tracers of ISM gas rather than the stellar content of the galaxies. We describe the point source extraction processing and the criteria used to establish a catalog for each waveband for the HERITAGE program. The 250 μm band is the most sensitive and the source catalogs for this band have ~25,000 objects for the LMC and ~5500 objects for the SMC. These data enable studies of ISM dust properties, submillimeter excess dust emission, dust-to-gas ratio, Class 0 YSO candidates, dusty massive evolved stars, supernova remnants (including SN1987A), H II regions, and dust evolution in the LMC and SMC. All images and catalogs are delivered to the Herschel Science Center as part of the community support aspects of the project. These HERITAGE images and catalogs provide an excellent basis for future research and follow up with other facilities.
Published: 2013
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33. A multiwavelength study of the Magellanic-type galaxy NGC 4449-I. Modelling the spectral energy distribution, the ionization structure and the star formation history

Author: Maud Galametz, Vianney Lebouteiller, O. Ł. Karczewski, Luigi Spinoglio, Maarten Baes, Frédéric Galliano, M. J. Barlow, Matthew Smith, I. De Looze, M. J. Page, N. P. M. Kuin, Ignacio Ferreras, Aurélie Rémy-Ruyer, Alessandro Boselli, Asantha Cooray, Diane Cormier, Michael Pohlen, Suzanne C. Madden, George J. Bendo, 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, Stellar mass, dwarf [galaxies], Astrophysics::High Energy Astrophysical Phenomena, INFRARED-EMISSION, Extinction (astronomy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, POLYCYCLIC AROMATIC-HYDROCARBONS, IRREGULAR GALAXIES, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Large Magellanic Cloud, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, QB, Physics, ISM [galaxies], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, individual: NGC 4449 [galaxies], extinction, Astronomy, Astronomy and Astrophysics, numerical [methods], stellar content [galaxies], ON-ORBIT PERFORMANCE, HERSCHEL PHOTOMETRIC-OBSERVATIONS, DIFFUSE INTERSTELLAR-MEDIUM, Galaxy, Physics and Astronomy, 13. Climate action, Space and Planetary Science, Spectral energy distribution, DIGITAL SKY SURVEY, dust, Astrophysics::Earth and Planetary Astrophysics, SWIFT ULTRAVIOLET/OPTICAL TELESCOPE, Irregular galaxy, Astrophysics - Instrumentation and Methods for Astrophysics, STELLAR POPULATION-MODELS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: [Abridged] We present an integrated photometric spectral energy distribution (SED) of the Magellanic-type galaxy NGC 4449 from the far-ultraviolet (UV) to the submillimetre, including new observations acquired by the Herschel Space Observatory. We include integrated UV photometry from the Swift Ultraviolet and Optical Telescope using a measurement technique which is appropriate for extended sources with coincidence loss. In this paper, we examine the available multiwavelength data to infer a range of ages, metallicities and star formation rates for the underlying stellar populations, as well as the composition and the total mass of dust in NGC 4449. We present an iterative scheme, which allows us to build an in-depth and multicomponent representation of NGC 4449 `bottom-up', taking advantage of the broad capabilities of the photoionization and radiative transfer code MOCASSIN (MOnte CArlo SimulationS of Ionized Nebulae). We fit the observed SED, the global ionization structure and the emission line intensities, and infer a recent SFR of 0.4 Msolar/yr and a total stellar mass of approximately 1e9 Msolar emitting with a bolometric luminosity of 5.7e9 Lsolar. Our fits yield a total dust mass of 2.9e6 Msolar including 2 per cent attributed to polycyclic aromatic hydrocarbons. We deduce a dust to gas mass ratio of 1/190 within the modelled region. While we do not consider possible additional contributions from even colder dust, we note that including the extended HI envelope and the molecular gas is likely to bring the ratio down to as low as ~ 1/800., 22 pages, 11 figures, 8 tables, published in MNRAS, 431, 2493 (2013)
Published: 2013
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34. The Herschel view of the environment of the radio galaxy 4C+41.17 at z = 3.8

Author: Jamie Stevens, Huub Röttgering, Dominika Wylezalek, Klaus Meisenheimer, Rob Ivison, M. Haas, D. Stern, M. Lehnert, Nina A. Hatch, George K. Miley, Thomas R. Greve, Joel Vernet, Nick Seymour, C. De Breuck, Matt J. Jarvis, Nicole P. H. Nesvadba, Guillaume Drouart, Pieter Barthel, Audrey Galametz, 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), INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Royal Observatory Edinburgh (ROE), University of Edinburgh, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Universiteit Leiden, and Astronomy
Subjects: ACTIVE GALACTIC NUCLEI, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: individual: 4C+41.17, Radio galaxy, ARRAY CAMERA, REDSHIFT, MU-M, FOS: Physical sciences, 02 engineering and technology, Astrophysics, SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, techniques: photometric, 4C 41.17, X-shaped radio galaxy, Spitzer Space Telescope, galaxies: high-redshift, 0103 physical sciences, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, NUMBER COUNTS, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, SPITZER-SPACE-TELESCOPE, Physics, [PHYS]Physics [physics], Astronomy, Astronomy and Astrophysics, 021001 nanoscience & nanotechnology, Redshift, Galaxy, 13. Climate action, Space and Planetary Science, galaxies: clusters: general, LUMINOSITY FUNCTION, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, 0210 nano-technology, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present Herschel observations at 70, 160, 250, 350 and 500 micron of the environment of the radio galaxy 4C+41.17 at z = 3.792. About 65% of the extracted sources are securely identified with mid-IR sources observed with the Spitzer Space Telescope at 3.6, 4.5, 5.8, 8 and 24 micron. We derive simple photometric redshifts, also including existing 850 micron and 1200 micron data, using templates of AGN, starburst-dominated systems and evolved stellar populations. We find that most of the Herschel sources are foreground to the radio galaxy and therefore do not belong to a structure associated with 4C+41.17. We do, however, find that the SED of the closest (~ 25" offset) source to the radio galaxy is fully consistent with being at the same redshift as 4C+41.17. We show that finding such a bright source that close to the radio galaxy at the same redshift is a very unlikely event, making the environment of 4C+41.17 a special case. We demonstrate that multi-wavelength data, in particular on the Rayleigh-Jeans side of the spectral energy distribution, allow us to confirm or rule out the presence of protocluster candidates that were previously selected by single wavelength data sets., 17 pages, accepted for publication in the Monthly Notices of the Royal Astronomical Society
Published: 2013
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35. Submillimetre photometry of 323 nearby galaxies from the Herschel Reference Survey (Corrigendum)

Author: I. De Looze, Maarten Baes, A. Boselli, S. di Serego Alighieri, M. Galametz, Ciro Pappalardo, Mattia Vaccari, Aurelie Remy, Luigi Spinoglio, D. L. Clements, Luca Cortese, V. Lebouteiller, M. Boquien, Asantha Cooray, M. Pohlen, S. C. Madden, Robbie Richard Auld, Simone Bianchi, George J. Bendo, V. Buat, Jonathan Ivor Davies, Stefano Zibetti, M. W. L. Smith, H. L. Gomez, L. Ciesla, Steve Eales, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), University of Manchester [Manchester], School of Physics and Astronomy [Cardiff], Cardiff University, Department of Pathology, Università degli Studi di Firenze = University of Florence (UniFI), 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), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Sterrenkundig Observatorium, Universiteit Gent = Ghent University (UGENT), California Institute of Technology (CALTECH), University of Cambridge [UK] (CAM), Infectious Diseases Unit, Hospital Universitari Mutua de Terrassa, University of Barcelona, 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), aucun, Macif, Antarctic Research a European Network for Astrophysics (ARENA), Dipartimento di Astronomia [Padova], Università degli Studi di Padova = University of Padua (Unipd), 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 Florence (UNIFI), 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), Universiteit Gent, Dipartimento di Astronomia, Universita degli Studi di Padova, and Università degli Studi di Firenze = University of Florence [Firenze] (UNIFI)
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 and Astrophysics, Astrophysics, 01 natural sciences, Galaxy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Photometry (astronomy), [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS
Abstract: International audience
Published: 2013
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36. CAN DUST EMISSION BE USED TO ESTIMATE THE MASS OF THE INTERS℡LAR MEDIUM IN GALAXIES-A PILOT PROJECT WITH THE HERSCHEL REFERENCE SURVEY

Author: Laure Ciesla, Michael Pohlen, Stephen Anthony Eales, Ilse De Looze, Asantha Cooray, George J. Bendo, Walter Kieran Gear, David L. Clements, Alessandro Boselli, Haley Louise Gomez, Luca Cortese, Thomas M. Hughes, Robbie Richard Auld, Simone Bianchi, Maud Galametz, Laura Magrini, Luigi Spinoglio, Christine D. Wilson, Joris Verstappen, Suzanne C. Madden, J. I. Davies, Maarten Baes, Gianfranco Gentile, Matthew Smith, Catherine Vlahakis, Jacapo Fritz, 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), Physics, and Astrophysics
Subjects: Physics, galaxies: spiral, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Radio galaxy, Milky Way, Astronomy and Astrophysics, Quasar, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Virgo Cluster, Galaxy, Interstellar medium, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Hydrogen line, dust, extinction, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, galaxies: ISM, Astrophysics::Galaxy Astrophysics, Cosmic dust
Abstract: International audience; The standard method for estimating the mass of the interstellar medium (ISM) in a galaxy is to use the 21 cm line to trace the atomic gas and the CO 1-0 line to trace the molecular gas. In this paper, we investigate the alternative technique of using the continuum dust emission to estimate the mass of gas in all phases of the ISM. Using Herschel observations of 10 galaxies from the Herschel Reference Survey and the Herschel Virgo Cluster Survey, we show that the emission detected by Herschel is mostly from dust that has a temperature and emissivity index similar to that of dust in the local ISM in our galaxy, with the temperature generally increasing toward the center of each galaxy. We calibrate the dust method using the CO and 21 cm observations to provide an independent estimate of the mass of hydrogen in each galaxy, solving the problem of the uncertain “X-factor” for the CO observations by minimizing the dispersion in the ratio of the masses estimated using the two methods. With the calibration for the dust method and the estimate of the X-factor produced in this way, the dispersion in the ratio of the two gas masses is 25%. The calibration we obtain for the dust method is similar to those obtained from Herschel observations of M31 and from Planck observations of the Milky Way. We discuss the practical problems in using this method.
Published: 2012
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37. SPATIALLY RESOLVED S℡LAR, DUST, AND GAS PROPERTIES OF THE POST-INTERACTING WHIRLPOOL GALAXY SYSTEM

Author: Maud Galametz, Jin Koda, Luigi Spinoglio, George J. Bendo, Alessandro Boselli, Vianney Lebouteiller, Marc Sauvage, Hélène Roussel, Matthew Smith, Laure Ciesla, Médéric Boquien, K. Foyle, T. J. Parkin, Christine D. Wilson, Maarten Baes, Steve Eales, Asantha Cooray, Erin Mentuch Cooper, 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: Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB, Physics, Spiral galaxy, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Mass ratio, Galaxy, Space and Planetary Science, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Using infrared imaging from the Herschel Space Observatory, observed as part of the VNGS, we investigate the spatially resolved dust properties of the interacting Whirlpool galaxy system (NGC 5194 and NGC 5195), on physical scales of 1 kpc. Spectral energy distribution modelling of the new infrared images in combination with archival optical, near- through mid-infrared images confirms that both galaxies underwent a burst of star formation ~370-480 Myr ago and provides spatially resolved maps of the stellar and dust mass surface densities. The resulting average dust-to-stellar mass ratios are comparable to other spiral and spheroidal galaxies studied with Herschel, with NGC 5194 at log M(dust)/M(star)= -2.5+/-0.2 and NGC 5195 at log M(dust)/M(star)= -3.5+/-0.3. The dust-to-stellar mass ratio is constant across NGC 5194 suggesting the stellar and dust components are coupled. In contrast, the mass ratio increases with radius in NGC 5195 with decreasing stellar mass density. Archival mass surface density maps of the neutral and molecular hydrogen gas are also folded into our analysis. The gas-to-dust mass ratio, 94+/-17, is relatively constant across NGC 5194. Somewhat surprisingly, we find the dust in NGC 5195 is heated by a strong interstellar radiation field, over 20 times that of the ISRF in the Milky Way, resulting in relatively high characteristic dust temperatures (~30 K). This post-starburst galaxy contains a substantial amount of low-density molecular gas and displays a gas-to-dust ratio (73+/-35) similar to spiral galaxies. It is unclear why the dust in NGC 5195 is heated to such high temperatures as there is no star formation in the galaxy and its active galactic nucleus is 5-10 times less luminous than the one in NGC 5194, which exhibits only a modest enhancement in the amplitude of its ISRF., Comment: 26 pages, 24 figures, Accepted for publication in ApJ
Published: 2012
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38. Herschel observations of Cen A: stellar heating of two extragalactic dust clouds

Author: Baes, M., Boselli, A., Cooray, A., Davies, J. I., Eales, S., Elbaz, D., Galametz, M., Isaak, K., Oosterloo, T., Page, M., Rigby, E., Spinoglio, L., Struve, C., Auld, R., Smith, M. W. L., Bendo, G., Pohlen, M., Wilson, C., Gomez, H., Cortese, L., Morganti, R., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and Astronomy
Subjects: EMISSION-LINE FILAMENTS, Cosmology and Nongalactic Astrophysics (astro-ph.CO), CENTAURUS-A EVIDENCE, INTERSTELLAR-MEDIUM, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], extinction, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, ENERGY PARTICLE-ACCELERATION, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: jets, 160 MU-M, submillimetre: ISM, INDUCED STAR-FORMATION, X-RAY-EMISSION, MULTIBAND IMAGING PHOTOMETER, NGC 5128, Astrophysics::Solar and Stellar Astrophysics, dust, FORMATION RATE INDICATORS, submillimetre: galaxies, galaxies: ISM, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the first results of a multi-wavelength survey, incoporating Herschel-SPIRE, Spitzer, GALEX and ATCA observations, of a 1 deg x 1 deg field centred on Centaurus A. As well as detecting the inner lobes of the active galactic nucleus (AGN) jet and counterjet, we have found two clouds, bright at sub-mm wavelengths, ~15 kpc from the centre of Cen A that are co-aligned with the jets. Flux measurements at Herschel wavelengths have proved vital in constraining fits to the Spectral Energy Distributions (SEDs). The clouds are well fit by a single-temperature, modified blackbody spectrum (beta=2) indicating that we are looking at two cold dust clouds on the outskirts of Cen A. The temperature and masses of the clouds are: T_{north} = 12.6^{+1.1}_{-1.2} K, T_{south} = 15.1^{+1.7}_{-1.6} K; log(M_{north} / M_o) = 5.8^{+0.2}_{-0.2}, log(M_{south} / M_o) = 5.6^{+0.2}_{-0.2} and the gas-dust ratio for both clouds is ~100. The measured values for the northern dust cloud are consistent with previous measurements from ISO while the southern cloud is a new sub-mm detection. The two dust clouds are located at the termini of the partial HI ring that surrounds Cen A which is also where the gas column density peaks... abridged, Comment: 16 pages, 9 figures, Accepted for publication in MNRAS, author email: robbie.auld@astro.cf.ac.uk
Published: 2012
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39. Toward the Comprehension of the Infrared to Submillimeter View of the Interstellar Medium of Nearby Galaxies

Author: Galametz, Maud, Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Université Paris-Diderot - Paris VII, and Suzanne Madden
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Densité Spectrale d'énergie, Galaxies à faible métallicité, Nearby galaxies, Low-metallicity Galaxies, Milieu Interstellaire, Spectral Energy Distribution, Galaxies Proches, Interstellar Medium
Abstract: This thesis aims to study the interstellar medium (ISM) of nearby galaxies to characterize the phys- ical properties of the gas and dust. We especially focused our study on low-metallicity galaxies of the Local Universe, ideal candidates to study the influence of metal enrichment on the ISM properties of galaxies. Previous studies have shown that the Spectral Energy Distributions (SEDs) of low metallicity galaxies differ significantly from those of massive galaxies and that the dust-to-gas mass ratio (D/G) of the galaxy could be dependent of the metallicity. Observations of low-metallicity galaxies also often led to the detection of an excess at submillimeter (submm) wavelengths not always accounted for in usual SED models. Further studies and observations had to be performed to better cover the far-IR to submm range and probe the coldest phase of dust. We adopt a multi-wavelength approach to model and analyse the SEDs of 4 low-metallicity galaxies observed with LABOCA at 870 μm. We estimated the fraction of cool dust to be significant compared to the total dust mass of the galaxies. Some D/Gs are incoherent compared to what is expected from the current chemical evolution model, revealing possible reservoirs of gas not detected by current HI or CO observations. I enlarged the first sample to a wider range of metallicities and showed that submm measure- ments significantly affect the dust mass estimates of galaxies. For dustier galaxies for which the SED usually peaks at longer wavelengths, submm fluxes are crucial to position the peak and the Rayleigh-Jeans slope of their SED. For low-metallicity galaxies, the submm wavelength domain harbours an excess that may imply a large amount of very cold dust. Our results confirm that low-metallicity galaxies can exhibit a submm excess when observed at longer wavelengths. Obtaining a more precise inventory of the cold dust and resolve the main actors of dust evolution in massive star forming regions and molecular clouds was the logical following step. We obtain LABOCA observations of a resolved star forming region of the Large Magellanic Cloud (LMC), the N158/N159/N160 complex, situated in the south of the 30 Doradus complex. The proximity of the LMC enables us to resolve structures of a few parsecs at the LABOCA resolution to model the SEDs of individual and isolated regions across the complex and get a handle on the temperature distribution of the dust (hot, warm, cold). I am also comparing the dust distribution with the Hi, CO and Hα observations to spatially quantify the variations of the D/G. I finally present the first Herschel observations of the galaxies NGC 6822 and NGC 1705, two low- metallicity galaxies observed as part of the Science Demonstration phase of the telescope launched in May 2009. In NGC 6822, we model the SEDs of some 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 the same submm emission due to its lower emissivity properties. This indicates that SED models including Herschel constraints may require different dust properties than commonly used.; Cette thèse s'attache à l'étude du milieu interstellaire (MIS) des galaxies proches afin de mieux comprendre les processus physiques de ses composantes de gaz et de poussière. Nous nous sommes principalement concentrés sur les galaxies de faible métallicité pour étudier l'influence de l'enrichissement en métaux sur les propriétés du MIS. Les études précédentes ont montré que les densités spectrales d'énergie (SED) des galaxies à faible métallicité présentaient des différences notables avec celles des galaxies plus massives. Le rapport en masse poussière sur gaz (D/G) semble d'ailleurs dépendre de la métallicité. L'observation de ces galaxies conduit souvent à la détection d'un excès submm qui n'est pas pris en compte dans la modélisation actuelle des SEDs. Des études complémentaires sont donc nécessaires pour comprendre les phénomènes physiques liés aux différentes populations de grains de poussière responsables de l'émission IR/submm et d'en sonder les composantes froides. Nous avons adopté une approche multi-longueur d'onde pour modéliser les SEDs de 4 galaxies à faible métallicité observées avec LABOCA (870 μm). La fraction de poussière froide de ces galaxies semble être importante au regard de leur masse totale. Certains D/Gs ne correspondent pas aux prédictions des modèles d'évolution chimique et suggérent la présence de réservoirs de gaz moléculaire non détecté par les observations actuelles en HI et CO. Nous avons élargi cet échantillon à un intervalle plus varié de métallicité et montré que les contraintes submm affectent significativement la masse de poussière totale. La modélisation des galaxies riches en poussière dont les SEDs piquent généralement à grande longueur d'onde nécessite des contraintes submm pour échantillonner à la fois le pic et la pente submm de leur SED. Les galaxies à faible métallicité, quant à elles, peuvent présenter un excès en submm. Cet excès a des conséquences importantes sur la quantification de la masse de poussière et sur la caractérisation de cette poussière froide. Il nous fallait maintenant faire l'inventaire complet de cette population froide de grains et résoudre les principaux acteurs de l'émission IR et submm dans les régions massives de formation d'étoiles et dans les nuages moléculaires. Nous avons obtenu des observations LABOCA du complexe N158/N159/N160, une région intense de formation d'étoiles dans le Grand Nuage de Magellan, située au sud de 30 Doradus. La proximité du nuage de Magellan nous permet de résoudre des structures de quelques parsecs à 870 μm avec LABOCA. Cela permet d'effectuer une étude spatiale de l'évolution des SEDs à travers le complexe afin d'étudier la distribution de température des grains. Je compare également la distribution IR et submm avec les observations déjà disponibles en HI, CO et Hα afin notamment de réaliser une étude spatiale du D/G. Je présente enfin les premières images Herschel des galaxies NGC 6822 et NGC 1705 observées lors de la phase SD du télescope lancé en mai 2009. Pour NGC 6822, nous avons modélisé les SEDs de régions HII ainsi que de régions moins actives. Les SEDs des régions HII présentent des intervalles de températures plus chauds. Nous obtenons des masses de poussières importantes lorsque les graphites sont utilisés pour décrire la poussière carbonnée. L'utilisation de grains de carbone amorphe diminue ces masses de poussière. Cela semble indiquer que les modèles de SED incluant des données Herschel nécessitent l'utilisation des propriétés différentes des poussière.
Published: 2010

40. The central region of spiral galaxies as seen by Herschel

Author: Sauvage, M., Sacchi, N., Bendo, G. J., Boselli, A., Pohlen, M., Wilson, C. D., Auld, R., Baes, M., Barlow, M. J., Bock, J. J., Bradford, M., Buat, V., Castro-Rodriguez, N., Chanial, P., Charlot, S., Ciesla, L., Clements, D. L., Cooray, A., Cormier, D., Cortese, L., Davies, J. I., Dwek, E., Eales, S. A., Elbaz, D., Galametz, M., Galliano, F., Gear, W. K., Glenn, J., Gomez, H. L., Griffin, M., Hony, S., Isaak, K. G., Levenson, L. R., Lu, N., Madden, S. C., O'Halloran, B., Okumura, K., Oliver, S., Page, M. J., Panuzzo, P., Papageorgiou, A., Parkin, T. J., Perez-Fournon, I., Rangwala, N., Rigby, E. E., Roussel, H., Rykala, A., Schulz, B., Schirm, M. R. P., Smith, M. W. L., Spinoglio, L., Stevens, J. A., Srinivasan, S., Symeonidis, M., Trichas, M., Vaccari, M., Vigroux, L., Wozniak, H., Wright, G. S., Zeilinger, W. W., 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: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: International audience; With appropriate spatial resolution, images of spiral galaxies in thermal infrared (similar to 10 mu m 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 mu m, 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. We quantify the luminosity of the central component by both a decomposition of the radial surface brightness profile and a direct extraction in 2D. We find the central component contribution is variable within the three galaxies in our sample, possibly connected more directly to the presence of a bar than to the morphological type. The central component's relative contribution is at its maximum in the mid-infrared range and drops around 160 mu m to reach a constant value beyond 200 mu m. The central component contains a greater fraction of hot dust than the disk component, and while the colors of the central components are scattered, colors of the disk components are more homogenous from one galaxy to the next.
Published: 2010
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41. On the origin of M81 group extended dust emission

Author: Davies, J. I., Wilson, C. D., Auld, R., Baes, M., Barlow, M. J., Bendo, G. J., Bock, J. J., Boselli, A., Bradford, M., Buat, V., Castro-Rodriguez, N., Chanial, P., Charlot, S., Ciesla, L., Clements, D. L., Cooray, A., Cormier, D., Cortese, L., Dwek, E., Eales, S. A., Elbaz, D., Galametz, M., Galliano, F., Gear, W. K., Glenn, J., Gomez, H. L., Griffin, M., Hony, S., Isaak, K. G., Levenson, L. R., Lu, N., Madden, S., O'Halloran, B., Okumura, K., Oliver, S., Page, M. J., Panuzzo, P., Papageorgiou, A., Parkin, T. J., Perez-Fournon, I., Pohlen, M., Rangwala, N., Rigby, E. E., Roussel, H., Rykala, A., Sacchi, N., Sauvage, M., Schulz, B., Schirm, M. R. P., Smith, M. W. L., Spinoglio, L., Stevens, J. A., Srinivasan, S., Symeonidis, M., Trichas, M., Vaccari, M., Vigroux, L., Wozniak, H., Wright, G. S., Zeilinger, W. W., 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: individual: M81, Cosmology and Nongalactic Astrophysics (astro-ph.CO), dust, extinction, galaxies: evolution, galaxies: individual: M81, extinction, [SDU]Sciences of the Universe [physics], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, dust, galaxies: evolution, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
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 &��&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., 6 pages, 4 figures, accepted for publication in MNRAS
Published: 2010
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42. 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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43. 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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