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153 results on '"Buat, Veronique"'

151. EVIDENCE FOR A WIDE RANGE OF ULTRAVIOLET OBSCURATION IN z ∼ 2 DUSTY GALAXIES FROM THE GOODS-HERSCHEL SURVEY.

Author

Penner, Kyle, Dickinson, Mark, Pope, Alexandra, Dey, Arjun, Magnelli, Benjamin, Pannella, Maurilio, Altieri, Bruno, Aussel, Herve, Buat, Veronique, Bussmann, Shane, Charmandaris, Vassilis, Coia, Daniela, Daddi, Emanuele, Dannerbauer, Helmut, Elbaz, David, Hwang, Ho Seong, Kartaltepe, Jeyhan, Lin, Lihwai, Magdis, Georgios, and Morrison, Glenn

Subjects
GALAXIES, INTERPLANETARY dust, INTERSTELLAR medium, ULTRAVIOLET radiation, POLYCYCLIC aromatic hydrocarbons
Abstract

Dusty galaxies at z ∼ 2 span a wide range of relative brightness between rest-frame mid-infrared (8 μm) and ultraviolet wavelengths. We attempt to determine the physical mechanism responsible for this diversity. Dust-obscured galaxies (DOGs), which have rest-frame mid-IR to UV flux density ratios ≳ 1000, might be abnormally bright in the mid-IR, perhaps due to prominent emission from active galactic nuclei and/or polycyclic aromatic hydrocarbons, or abnormally faint in the UV. We use far-infrared data from the GOODS-Herschel survey to show that most DOGs with 1012L☼ ≲ LIR ≲ 1013L☼ are not abnormally bright in the mid-IR when compared to other dusty galaxies with similar IR (8-1000 μm) luminosities. We observe a relation between the median IR to UV luminosity ratios and the median UV continuum power-law indices for these galaxies, and we find that only 24% have specific star formation rates that indicate the dominance of compact star-forming regions. This circumstantial evidence supports the idea that the UV- and IR-emitting regions in these galaxies are spatially coincident, which implies a connection between the abnormal UV faintness of DOGs and dust obscuration. We conclude that the range in rest-frame mid-IR to UV flux density ratios spanned by dusty galaxies at z ∼ 2 is due to differing amounts of UV obscuration. Of galaxies with these IR luminosities, DOGs are the most obscured. We attribute differences in UV obscuration to either (1) differences in the degree of alignment between the spatial distributions of dust and massive stars or (2) differences in the total dust content. [ABSTRACT FROM AUTHOR]

Published
2012
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152. Close-up view of a luminous star-forming galaxy at z = 2.95

Author

A. Carnero Rosell, I. Perez-Fournon, C. N. Herrera, Steve Serjeant, Andrew I. Harris, R. Neri, C. Yang, Axel Weiß, Lucia Marchetti, A. J. Young, Catherine Vlahakis, Hugo Messias, M. Krips, T. Bakx, Mattia Negrello, David H. Hughes, Asantha Cooray, Guilaine Lagache, Alexandre Beelen, Rob Ivison, Helmut Dannerbauer, Matthew D. Lehnert, Pierre Cox, S. Urquhart, Andrew J. Baker, P. van der Werf, Simon Dye, B. M. Jones, Alain Omont, V. Buat, Dominik Riechers, Shuowen Jin, Isabella Cortzen, Raphael Gavazzi, Loretta Dunne, F. Stanley, S. Berta, Steve Eales, Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Rutgers, The State University of New Jersey [New Brunswick] (RU), Rutgers University System (Rutgers), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Astronomia [Padova], Università degli Studi di Padova = University of Padua (Unipd), Tongji University, Department of Astronomy [Ithaca], Cornell University [New York], Institut für Astronomie [Wien], Universität Wien, Instituto de Astrofisica de Canarias (IAC), 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), 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), Department of Physics and Astronomy [Irvine], University of California [Irvine] (UC Irvine), University of California (UC)-University of California (UC), School of Physics and Astronomy [Cardiff], Cardiff University, Max-Planck-Institut für Extraterrestrische Physik (MPE), Max-Planck-Institut für Radioastronomie (MPIFR), AUTRES, CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Universita degli Studi di Padova, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of California [Irvine] (UCI), University of California-University of California, and BUAT, Veronique

Subjects
submillimeter: galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Absorption spectroscopy, Einstein ring, Infrared, Astrophysics - cosmology and nongalactic astrophysics, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, Spectral line, [SDU] Sciences of the Universe [physics], symbols.namesake, galaxies: high-redshift, 0103 physical sciences, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, [PHYS]Physics [physics], radio lines: ISM, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, gravitational lensing: strong, Astronomy and Astrophysics, Galaxy, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], galaxies: star formation, symbols, Millimeter, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM
Abstract

(Abridged) Exploiting the sensitivity and broad band width of NOEMA, we have studied the molecular gas and dust in the galaxy HerBS-89a, at z=2.95. High angular resolution images reveal a partial 1.0" diameter Einstein ring in the dust continuum emission and the molecular emission lines of 12CO(9-8) and H2O(2_02-1_11). We report the detection of the three fundamental transitions of the molecular ion OH+, seen in absorption; the molecular ion CH+(1-0) seen in absorption (and tentatively in emission); two transitions of amidogen (NH2), seen in emission; and HCN(11-10) and/or NH(1_2-0_1) seen in absorption. The NOEMA data are complemented with VLA data tracing the 12CO(1-0) emission line, which provides a measurement of the total mass of molecular gas and an anchor for a CO excitation analysis. In addition, we present HST imaging that reveals the foreground lensing galaxy in the near-infrared. Together with data from the GTC, we derive a photometric redshift of z(phot)~0.9 for the foreground lensing galaxy. Modelling the lensing of HerBS-89a, we reconstruct the dust continuum and molecular emission lines (magnified by a factor ~4-5) in the source plane. The 12CO(9-8) and H2O emission lines have comparable spatial and kinematic distributions; the source-plane reconstructions do not clearly distinguish between a one-component and a two-component scenario, but the latter accounts for the observed broad line widths. HerBS-89a is a powerful star forming galaxy with a dust-to-gas ratio delta(GDR)~80, a SFR = 614 +/- 59 Msun/yr and a depletion timescale tau(depl) = (3.4 +/- 1.0) 1e8 years. The OH+ and CH+ absorption lines, all have their main velocity component red-shifted by \Delta(V)~100 km/s relative to the global CO reservoir. We argue that these absorption lines trace a rare example of gas inflow towards the center of the galaxy., Comment: 33 pages, Accepted for publication on A&A

Published
2021

153. X-ray flux in the SED modelling: An application of X-CIGALE in the XMM-XXL field

Author

G. Mountrichas, Laure Ciesla, Denis Burgarella, Guang Yang, Médéric Boquien, V. Buat, BUAT, Veronique, Instituto de Física de Cantabria (IFCA), Universidad de Cantabria [Santander]-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 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 Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Fondo Nacional de Desarrollo Científico y Tecnológico (Chile), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), active [Galaxies], Infrared, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, X-rays: general, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, Luminosity, Photometry (optics), [SDU] Sciences of the Universe [physics], Flux (metallurgy), Methods: data analysis, general [X-rays], 0103 physical sciences, data analysis [Methods], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Galaxies: active, Redshift, galaxies [X-rays], X-rays: galaxies, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Spectral energy distribution, Polar, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

arXiv:2011.09220v1, X-CIGALE is built on the spectral energy distribution (SED) code of CIGALE and implements important new features: the code accounts for obscuring material in the poles of AGNs and has the ability to fit X-ray fluxes. In this work, we used ∼2500 spectroscopic X-ray AGNs from the XMM-XXL-north field and examined the improvements the new features bring to the SED modelling analysis. Based on our results, X-CIGALE successfully connects the X-ray with the UV luminosity in the whole range spanned by our sample (log LX(2−10 keV) = (42−46) erg s−1). The addition of the new features generally improves the efficiency of X-CIGALE in the estimation and characterisation of the AGN component. Classification as type 1 or type 2 based on their inclination angle is improved, especially at redshifts lower than 1. The statistical significance of AGN fraction, fracAGN, measurements is increased, in particular for luminous X-ray sources (LX > 1045 erg s−1). These conclusions hold under the condition that (mid-) IR photometry is available in the SED fitting process. The addition of polar dust increases the AGN fraction and the efficiency of the SED decomposition to detect AGNs among X-ray selected sources. X-CIGALE estimates a strong AGN (fracAGN > 0.3) in more than 90% of the IR-selected AGNs and 75% of X-ray-detected AGNs not selected by IR colour criteria. The latter drops to ∼50% when polar dust is not included. The ability of X-CIGALE to include X-ray information in the SED fitting process can be instrumental in the optimal exploitation of the wealth of data that current (eROSITA) and future (ATHENA) missions will provide us., GM acknowledges support by the Agencia Estatal de Investigación, Unidad de Excelencia María de Maeztu, ref. MDM-2017-0765. MB acknowledges FONDECYT regular grant 1170618.

Published
2020

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