Chemical and Photometric Evolution of Extended Ultraviolet Disks: Optical Spectroscopy of M83 (NGC5236) and NGC4625

A. Gil de Paz; Barry F. Madore; S. Boissier; D. Thilker; Luciana Bianchi; C. Sánchez Contreras; Tom A. Barlow; T. Conrow; Karl Forster; Peter G. Friedman; Christopher Martin; Patrick Morrissey; S. G. Neff; R. M. Rich; D. Schiminovich; M. Seibert; T. Small; J. Donas; Timothy M. Heckman; Young-Wook Lee; Bruno Milliard; A. S. Szalay; T. K. Wyder; S. Yi

hal-00131501, version 1

Chemical and Photometric Evolution of Extended Ultraviolet Disks: Optical Spectroscopy of M83 (NGC5236) and NGC4625

A. Gil de Paz ¹, Barry F. Madore ^1, 2, 3, S. Boissier ^1, 2, D. Thilker, Luciana Bianchi ⁴, C. Sánchez Contreras ⁵, Tom A. Barlow ⁶, T. Conrow, Karl Forster ⁶, Peter G. Friedman ⁶, Christopher Martin ^{7, 8, 9, 10}, Patrick Morrissey ⁶, S. G. Neff, R. M. Rich, D. Schiminovich, M. Seibert, T. Small, J. Donas ², Timothy M. Heckman ^11, 12, 13, Young-Wook Lee ^14, 15, Bruno Milliard ², A. S. Szalay, T. K. Wyder, S. Yi

(2007)

Abstract: We present the results from the analysis of optical spectra of 31 Halpha-selected regions in the extended UV (XUV) disks of M83 (NGC5236) and NGC4625 recently discovered by GALEX. The spectra were obtained using IMACS at Las Campanas Observatory 6.5m Magellan I telescope and COSMIC at the Palomar 200-inch telescope, respectively for M83 and NGC4625. The line ratios measured indicate nebular oxygen abundances (derived from the R23 parameter) of the order of Zsun/5-Zsun/10. For most emission-line regions analyzed the line fluxes and ratios measured are best reproduced by models of photoionization by single stars with masses in the range 20-40 Msun and oxygen abundances comparable to those derived from the R23 parameter. We find indications for a relatively high N/O abundance ratio in the XUV disk of M83. Although the metallicities derived imply that these are not the first stars formed in the XUV disks, such a level of enrichment could be reached in young spiral disks only 1 Gyr after these first stars would have formed. The amount of gas in the XUV disks allow maintaining the current level of star formation for at least a few Gyr.

1: Institut d'Astrophysique de Paris (IAP)
CNRS : UMR7095 – INSU – Université Pierre et Marie Curie [UPMC] - Paris VI
2: Laboratoire d'Astrophysique de Marseille (LAM)
CNRS : UMR6110 – INSU – Université de Provence - Aix-Marseille I
3: Observatories of the Carnegie Institution of Washington (OCIW)
Carnegie Institution of Washington
4: Deptartment of Physics and Astronomy
Johns Hopkins University
5: JACQUARD (INRIA Futurs)
INRIA – CNRS : UMR8022 – Université Lille I - Sciences et technologies
6: California Institute of Technology (CALTECH)
California Institute of Technology
7: Centre de Recherche en Economie et Management (CREM)
CNRS : UMR6211 – Université de Rennes 1 – Université de Caen Basse-Normandie
8: Institut de Biologie du Développement de Marseille Luminy (IBDML)
CNRS : UMR6216 – Université de la Méditerranée - Aix-Marseille II
9: Centre de biophysique moléculaire (CBM)
CNRS : UPR4301
10: Institut de biologie du développement de Marseille (IBDM)
CNRS : IFR138 – INSERM : IFR138 – Université de la Méditerranée - Aix-Marseille II
11: Department of Physics and Astronomy
University of California at Los Angeles
12: Department of Physics and Astronomy
University of California, Los Angeles
13: Department of Physics and Astronomy
Johns Hopkins University
14: POSTECH-UZH Cooperative Laboratory
Pohang University of Science and Technology
15: Meteorological Research Institute
Korea Meteorological Administration

hal-00131501, version 1
http://hal.archives-ouvertes.fr/hal-00131501
oai:hal.archives-ouvertes.fr:hal-00131501
From: Catherine Beaussier <>
Submitted on: Friday, 16 February 2007 15:34:32
Updated on: Thursday, 18 March 2010 14:00:25

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arXiv: astro-ph/0702302

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%% hal-00131501, version 1
%% http://hal.archives-ouvertes.fr/hal-00131501
@unpublished{depaz:hal-00131501,
    hal_id = {hal-00131501},
    url = {http://hal.archives-ouvertes.fr/hal-00131501},
    title = {{Chemical and Photometric Evolution of Extended Ultraviolet Disks: Optical Spectroscopy of M83 (NGC5236) and NGC4625}},
    author = {de Paz, A. Gil and Madore, Barry F. and Boissier, S. and Thilker, D. and Bianchi, Luciana and Contreras, C. S{\'a}nchez and Barlow, Tom A. and Conrow, T. and Forster, Karl and Friedman, Peter G. and Martin, Christopher and Morrissey, Patrick and Neff, S. G. and Rich, R. M. and Schiminovich, D. and Seibert, M. and Small, T. and Donas, J. and Heckman, Timothy M. and Lee, Young-Wook and Milliard, Bruno and Szalay, A. S. and Wyder, T. K. and Yi, S.},
    abstract = {{We present the results from the analysis of optical spectra of 31 Halpha-selected regions in the extended UV (XUV) disks of M83 (NGC5236) and NGC4625 recently discovered by GALEX. The spectra were obtained using IMACS at Las Campanas Observatory 6.5m Magellan I telescope and COSMIC at the Palomar 200-inch telescope, respectively for M83 and NGC4625. The line ratios measured indicate nebular oxygen abundances (derived from the R23 parameter) of the order of Zsun/5-Zsun/10. For most emission-line regions analyzed the line fluxes and ratios measured are best reproduced by models of photoionization by single stars with masses in the range 20-40 Msun and oxygen abundances comparable to those derived from the R23 parameter. We find indications for a relatively high N/O abundance ratio in the XUV disk of M83. Although the metallicities derived imply that these are not the first stars formed in the XUV disks, such a level of enrichment could be reached in young spiral disks only 1 Gyr after these first stars would have formed. The amount of gas in the XUV disks allow maintaining the current level of star formation for at least a few Gyr.}},
    language = {English},
    affiliation = {Institut d'Astrophysique de Paris - IAP , Laboratoire d'Astrophysique de Marseille - LAM , Observatories of the Carnegie Institution of Washington - OCIW , Deptartment of Physics and Astronomy , JACQUARD - INRIA Futurs , California Institute of Technology - CALTECH , Centre de Recherche en Economie et Management - CREM , Institut de Biologie du D{\'e}veloppement de Marseille Luminy - IBDML , Centre de biophysique mol{\'e}culaire - CBM , Institut de biologie du d{\'e}veloppement de Marseille - IBDM , Department of Physics and Astronomy , POSTECH-UZH Cooperative Laboratory , Meteorological Research Institute},
    note = {52 pages, 8 tables, 7 figures, accepted for publication in ApJ LAM POPULATIONS STELLAIRES ET EVOLUTION DES GALAXIES LAM POPULATIONS STELLAIRES ET EVOLUTION DES GALAXIES },
    year = {2007},
}

%F hal-00131501, version 1
%0 Unpublished Work
%U http://hal.archives-ouvertes.fr/hal-00131501
%2 PHYS:ASTR:CO;SDU:ASTR
%T Chemical and Photometric Evolution of Extended Ultraviolet Disks: Optical Spectroscopy of M83 (NGC5236) and NGC4625
%A de Paz, A. Gil
%A Madore, Barry F.
%A Boissier, S.
%A Thilker, D.
%A Bianchi, Luciana
%A Contreras, C. Sánchez
%A Barlow, Tom A.
%A Conrow, T.
%A Forster, Karl
%A Friedman, Peter G.
%A Martin, Christopher
%A Morrissey, Patrick
%A Neff, S. G.
%A Rich, R. M.
%A Schiminovich, D.
%A Seibert, M.
%A Small, T.
%A Donas, J.
%A Heckman, Timothy M.
%A Lee, Young-Wook
%A Milliard, Bruno
%A Szalay, A. S.
%A Wyder, T. K.
%A Yi, S.
%+ Institut d'Astrophysique de Paris - IAP , Laboratoire d'Astrophysique de Marseille - LAM , Observatories of the Carnegie Institution of Washington - OCIW , Deptartment of Physics and Astronomy , JACQUARD - INRIA Futurs , California Institute of Technology - CALTECH , Centre de Recherche en Economie et Management - CREM , Institut de Biologie du Développement de Marseille Luminy - IBDML , Centre de biophysique moléculaire - CBM , Institut de biologie du développement de Marseille - IBDM , Department of Physics and Astronomy , POSTECH-UZH Cooperative Laboratory , Meteorological Research Institute
%X We present the results from the analysis of optical spectra of 31 Halpha-selected regions in the extended UV (XUV) disks of M83 (NGC5236) and NGC4625 recently discovered by GALEX. The spectra were obtained using IMACS at Las Campanas Observatory 6.5m Magellan I telescope and COSMIC at the Palomar 200-inch telescope, respectively for M83 and NGC4625. The line ratios measured indicate nebular oxygen abundances (derived from the R23 parameter) of the order of Zsun/5-Zsun/10. For most emission-line regions analyzed the line fluxes and ratios measured are best reproduced by models of photoionization by single stars with masses in the range 20-40 Msun and oxygen abundances comparable to those derived from the R23 parameter. We find indications for a relatively high N/O abundance ratio in the XUV disk of M83. Although the metallicities derived imply that these are not the first stars formed in the XUV disks, such a level of enrichment could be reached in young spiral disks only 1 Gyr after these first stars would have formed. The amount of gas in the XUV disks allow maintaining the current level of star formation for at least a few Gyr.
%G English
%2 2007
%Z 52 pages, 8 tables, 7 figures, accepted for publication in ApJ
%Z LAM POPULATIONS STELLAIRES ET EVOLUTION DES GALAXIES

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