HUBBLE SPACE TELESCOPE MORPHOLOGIES OF z ˜ 2 DUST-OBSCURED GALAXIES. II. BUMP SOURCES
Identifieur interne : 001D17 ( PascalFrancis/Corpus ); précédent : 001D16; suivant : 001D18HUBBLE SPACE TELESCOPE MORPHOLOGIES OF z ˜ 2 DUST-OBSCURED GALAXIES. II. BUMP SOURCES
Auteurs : R. S. Bussmann ; Arjun Dey ; J. Lotz ; L. Armus ; M. J. I. Brown ; V. Desai ; P. Eisenhardt ; J. Higdon ; S. Higdon ; B. T. Jannuzi ; E. Le Floc'H ; J. Melbourne ; B. T. Soifer ; D. WeedmanSource :
- The Astrophysical journal [ 0004-637X ] ; 2011.
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Abstract
We present Hubble Space Telescope imaging of 22 ultra-luminous infrared galaxies (ULIRGs) at z ≃ 2 with extremely red R - [24] colors (called dust-obscured galaxies, or DOGs) which have a local maximum in their spectral energy distribution (SED) at rest-frame 1.6 μm associated with stellar emission. These sources, which we call "bump DOGs," have star formation rates (SFRs) of 400-4000 Mo yr-1 and have redshifts derived from mid-IR spectra which show strong polycyclic aromatic hydrocarbon emission-a sign of vigorous ongoing star formation. Using a uniform morphological analysis, we look for quantifiable differences between bump DOGs, power-law DOGs (Spitzer-selected ULIRGs with mid-IR SEDs dominated by a power law and spectral features that are more typical of obscured active galactic nuclei than starbursts), submillimeter-selected galaxies, and other less-reddened ULIRGs from the Spitzer Extragalactic First Look Survey. Bump DOGs are larger than power-law DOGs (median Petrosian radius of 8.4 ± 2.7 kpc versus 5.5 ± 2.3 kpc) and exhibit more diffuse and irregular morphologies (median M20 of -1.08 ± 0.05 versus -1.48 ± 0.05). These trends are qualitatively consistent with expectations from simulations of major mergers in which merging systems during the peak SFR period evolve from M20 = -1.0 to M20 = -1.7. Less-obscured ULIRGs (i.e., non-DOGs) tend to have more regular, centrally peaked, single-object morphologies rather than diffuse and irregular morphologies. This distinction in morphologies may imply that less-obscured ULIRGs sample the merger near the end of the peak SFR period. Alternatively, it may indicate that the intense star formation in these less-obscured ULIRGs is not the result of a recent major merger.
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| NO : | PASCAL 11-0258025 INIST |
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| ET : | HUBBLE SPACE TELESCOPE MORPHOLOGIES OF z ˜ 2 DUST-OBSCURED GALAXIES. II. BUMP SOURCES |
| AU : | BUSSMANN (R. S.); DEY (Arjun); LOTZ (J.); ARMUS (L.); BROWN (M. J. I.); DESAI (V.); EISENHARDT (P.); HIGDON (J.); HIGDON (S.); JANNUZI (B. T.); LE FLOC'H (E.); MELBOURNE (J.); SOIFER (B. T.); WEEDMAN (D.) |
| AF : | Steward Observatory, Department of Astronomy, University of Arizona, 933 North Cherry Avenue/Tucson, AZ 85721/Etats-Unis (1 aut.); National Optical Astronomy Observatory, 950 North Cherry Avenue/Tucson, AZ 85719/Etats-Unis (2 aut., 3 aut., 10 aut.); Spitzer Science Center, California Institute of Technology, MS 220-6/Pasadena, CA 91125/Etats-Unis (4 aut., 6 aut., 13 aut.); School of Physics, Monash University/Clayton, Victoria 3800/Australie (5 aut.); Jet Propulsion Laboratory, California Institute of Technology, MC 169-327, 4800 Oak Grove Drive/Pasadena, CA 91109/Etats-Unis (7 aut., 8 aut.); Georgia Southern University. P.O. Box 8031/Statesboro, GA/Etats-Unis (9 aut.); Laboratoire AIM-Paris-Saclay, CEA-CNRS-Universite Paris Diderot, CEA Saclay/Gif-sur-Yvette, 91191/France (11 aut.); Caltech Optical Observatories, California Institute of Technology/Pasadena, CA 91125/Etats-Unis (12 aut., 13 aut.); Astronomy Department, Cornell University/Ithaca, NY 14853/Etats-Unis (14 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | The Astrophysical journal; ISSN 0004-637X; Coden ASJOAB; Royaume-Uni; Da. 2011; Vol. 733; No. 1 p. 1; 73321.1-73321.18; Bibl. 3/4 p. |
| LA : | Anglais |
| EA : | We present Hubble Space Telescope imaging of 22 ultra-luminous infrared galaxies (ULIRGs) at z ≃ 2 with extremely red R - [24] colors (called dust-obscured galaxies, or DOGs) which have a local maximum in their spectral energy distribution (SED) at rest-frame 1.6 μm associated with stellar emission. These sources, which we call "bump DOGs," have star formation rates (SFRs) of 400-4000 Mo yr-1 and have redshifts derived from mid-IR spectra which show strong polycyclic aromatic hydrocarbon emission-a sign of vigorous ongoing star formation. Using a uniform morphological analysis, we look for quantifiable differences between bump DOGs, power-law DOGs (Spitzer-selected ULIRGs with mid-IR SEDs dominated by a power law and spectral features that are more typical of obscured active galactic nuclei than starbursts), submillimeter-selected galaxies, and other less-reddened ULIRGs from the Spitzer Extragalactic First Look Survey. Bump DOGs are larger than power-law DOGs (median Petrosian radius of 8.4 ± 2.7 kpc versus 5.5 ± 2.3 kpc) and exhibit more diffuse and irregular morphologies (median M20 of -1.08 ± 0.05 versus -1.48 ± 0.05). These trends are qualitatively consistent with expectations from simulations of major mergers in which merging systems during the peak SFR period evolve from M20 = -1.0 to M20 = -1.7. Less-obscured ULIRGs (i.e., non-DOGs) tend to have more regular, centrally peaked, single-object morphologies rather than diffuse and irregular morphologies. This distinction in morphologies may imply that less-obscured ULIRGs sample the merger near the end of the peak SFR period. Alternatively, it may indicate that the intense star formation in these less-obscured ULIRGs is not the result of a recent major merger. |
| CC : | 001E03 |
| FD : | Morphologie; Galaxies infrarouges; Couleur; Densité spectrale énergie; Formation stellaire; Taux formation; Déplacement vers le rouge; Spectre IR; Hydrocarbure aromatique polycyclique; Loi puissance; Noyau galactique actif; Galaxies à flambée; Evolution galaxies; Galaxies actives; Noyau galaxies |
| ED : | Morphology; Infrared galaxies; Color; Spectral energy distribution; Star formation; Formation rate; Red shift; Infrared spectra; Polycyclic aromatic hydrocarbons; Power law; Active galaxy nuclei; Starburst galaxies; Galaxy evolution; Active galaxies; Galaxy nuclei |
| SD : | Galaxias infrarrojas; Densidad espectral energía; Grado formación; Ley poder; Galaxias llamarada estelar; Evolución galaxias |
| LO : | INIST-512.354000191605310210 |
| ID : | 11-0258025 |
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Desai</name><affiliation><inist:fA14 i1="03"><s1>Spitzer Science Center, California Institute of Technology, MS 220-6</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>4 aut.</sZ><sZ>6 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Eisenhardt, P" sort="Eisenhardt, P" uniqKey="Eisenhardt P" first="P." last="Eisenhardt">P. Eisenhardt</name><affiliation><inist:fA14 i1="05"><s1>Jet Propulsion Laboratory, California Institute of Technology, MC 169-327, 4800 Oak Grove Drive</s1><s2>Pasadena, CA 91109</s2><s3>USA</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Higdon, J" sort="Higdon, J" uniqKey="Higdon J" first="J." last="Higdon">J. Higdon</name><affiliation><inist:fA14 i1="05"><s1>Jet Propulsion Laboratory, California Institute of Technology, MC 169-327, 4800 Oak Grove Drive</s1><s2>Pasadena, CA 91109</s2><s3>USA</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Higdon, S" sort="Higdon, S" uniqKey="Higdon S" first="S." last="Higdon">S. Higdon</name><affiliation><inist:fA14 i1="06"><s1>Georgia Southern University. P.O. Box 8031</s1><s2>Statesboro, GA</s2><s3>USA</s3><sZ>9 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Jannuzi, B T" sort="Jannuzi, B T" uniqKey="Jannuzi B" first="B. T." last="Jannuzi">B. T. Jannuzi</name><affiliation><inist:fA14 i1="02"><s1>National Optical Astronomy Observatory, 950 North Cherry Avenue</s1><s2>Tucson, AZ 85719</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Le Floc H, E" sort="Le Floc H, E" uniqKey="Le Floc H E" first="E." last="Le Floc'H">E. Le Floc'H</name><affiliation><inist:fA14 i1="07"><s1>Laboratoire AIM-Paris-Saclay, CEA-CNRS-Universite Paris Diderot, CEA Saclay</s1><s2>Gif-sur-Yvette, 91191</s2><s3>FRA</s3><sZ>11 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Melbourne, J" sort="Melbourne, J" uniqKey="Melbourne J" first="J." last="Melbourne">J. Melbourne</name><affiliation><inist:fA14 i1="08"><s1>Caltech Optical Observatories, California Institute of Technology</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>12 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Soifer, B T" sort="Soifer, B T" uniqKey="Soifer B" first="B. T." last="Soifer">B. T. Soifer</name><affiliation><inist:fA14 i1="03"><s1>Spitzer Science Center, California Institute of Technology, MS 220-6</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>4 aut.</sZ><sZ>6 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="08"><s1>Caltech Optical Observatories, California Institute of Technology</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>12 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Weedman, D" sort="Weedman, D" uniqKey="Weedman D" first="D." last="Weedman">D. Weedman</name><affiliation><inist:fA14 i1="09"><s1>Astronomy Department, Cornell University</s1><s2>Ithaca, NY 14853</s2><s3>USA</s3><sZ>14 aut.</sZ></inist:fA14></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">11-0258025</idno><date when="2011">2011</date><idno type="stanalyst">PASCAL 11-0258025 INIST</idno><idno type="RBID">Pascal:11-0258025</idno><idno type="wicri:Area/PascalFrancis/Corpus">001D17</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">HUBBLE SPACE TELESCOPE MORPHOLOGIES OF z ˜ 2 DUST-OBSCURED GALAXIES. II. BUMP SOURCES</title><author><name sortKey="Bussmann, R S" sort="Bussmann, R S" uniqKey="Bussmann R" first="R. S." last="Bussmann">R. S. Bussmann</name><affiliation><inist:fA14 i1="01"><s1>Steward Observatory, Department of Astronomy, University of Arizona, 933 North Cherry Avenue</s1><s2>Tucson, AZ 85721</s2><s3>USA</s3><sZ>1 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Dey, Arjun" sort="Dey, Arjun" uniqKey="Dey A" first="Arjun" last="Dey">Arjun Dey</name><affiliation><inist:fA14 i1="02"><s1>National Optical Astronomy Observatory, 950 North Cherry Avenue</s1><s2>Tucson, AZ 85719</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Lotz, J" sort="Lotz, J" uniqKey="Lotz J" first="J." last="Lotz">J. Lotz</name><affiliation><inist:fA14 i1="02"><s1>National Optical Astronomy Observatory, 950 North Cherry Avenue</s1><s2>Tucson, AZ 85719</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Armus, L" sort="Armus, L" uniqKey="Armus L" first="L." last="Armus">L. Armus</name><affiliation><inist:fA14 i1="03"><s1>Spitzer Science Center, California Institute of Technology, MS 220-6</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>4 aut.</sZ><sZ>6 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Brown, M J I" sort="Brown, M J I" uniqKey="Brown M" first="M. J. I." last="Brown">M. J. I. Brown</name><affiliation><inist:fA14 i1="04"><s1>School of Physics, Monash University</s1><s2>Clayton, Victoria 3800</s2><s3>AUS</s3><sZ>5 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Desai, V" sort="Desai, V" uniqKey="Desai V" first="V." last="Desai">V. Desai</name><affiliation><inist:fA14 i1="03"><s1>Spitzer Science Center, California Institute of Technology, MS 220-6</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>4 aut.</sZ><sZ>6 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Eisenhardt, P" sort="Eisenhardt, P" uniqKey="Eisenhardt P" first="P." last="Eisenhardt">P. Eisenhardt</name><affiliation><inist:fA14 i1="05"><s1>Jet Propulsion Laboratory, California Institute of Technology, MC 169-327, 4800 Oak Grove Drive</s1><s2>Pasadena, CA 91109</s2><s3>USA</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Higdon, J" sort="Higdon, J" uniqKey="Higdon J" first="J." last="Higdon">J. Higdon</name><affiliation><inist:fA14 i1="05"><s1>Jet Propulsion Laboratory, California Institute of Technology, MC 169-327, 4800 Oak Grove Drive</s1><s2>Pasadena, CA 91109</s2><s3>USA</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Higdon, S" sort="Higdon, S" uniqKey="Higdon S" first="S." last="Higdon">S. Higdon</name><affiliation><inist:fA14 i1="06"><s1>Georgia Southern University. P.O. Box 8031</s1><s2>Statesboro, GA</s2><s3>USA</s3><sZ>9 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Jannuzi, B T" sort="Jannuzi, B T" uniqKey="Jannuzi B" first="B. T." last="Jannuzi">B. T. Jannuzi</name><affiliation><inist:fA14 i1="02"><s1>National Optical Astronomy Observatory, 950 North Cherry Avenue</s1><s2>Tucson, AZ 85719</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Le Floc H, E" sort="Le Floc H, E" uniqKey="Le Floc H E" first="E." last="Le Floc'H">E. Le Floc'H</name><affiliation><inist:fA14 i1="07"><s1>Laboratoire AIM-Paris-Saclay, CEA-CNRS-Universite Paris Diderot, CEA Saclay</s1><s2>Gif-sur-Yvette, 91191</s2><s3>FRA</s3><sZ>11 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Melbourne, J" sort="Melbourne, J" uniqKey="Melbourne J" first="J." last="Melbourne">J. Melbourne</name><affiliation><inist:fA14 i1="08"><s1>Caltech Optical Observatories, California Institute of Technology</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>12 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Soifer, B T" sort="Soifer, B T" uniqKey="Soifer B" first="B. T." last="Soifer">B. T. Soifer</name><affiliation><inist:fA14 i1="03"><s1>Spitzer Science Center, California Institute of Technology, MS 220-6</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>4 aut.</sZ><sZ>6 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="08"><s1>Caltech Optical Observatories, California Institute of Technology</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>12 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Weedman, D" sort="Weedman, D" uniqKey="Weedman D" first="D." last="Weedman">D. Weedman</name><affiliation><inist:fA14 i1="09"><s1>Astronomy Department, Cornell University</s1><s2>Ithaca, NY 14853</s2><s3>USA</s3><sZ>14 aut.</sZ></inist:fA14></affiliation></author></analytic><series><title level="j" type="main">The Astrophysical journal</title><title level="j" type="abbreviated">Astrophys. j.</title><idno type="ISSN">0004-637X</idno><imprint><date when="2011">2011</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">The Astrophysical journal</title><title level="j" type="abbreviated">Astrophys. j.</title><idno type="ISSN">0004-637X</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Active galaxies</term><term>Active galaxy nuclei</term><term>Color</term><term>Formation rate</term><term>Galaxy evolution</term><term>Galaxy nuclei</term><term>Infrared galaxies</term><term>Infrared spectra</term><term>Morphology</term><term>Polycyclic aromatic hydrocarbons</term><term>Power law</term><term>Red shift</term><term>Spectral energy distribution</term><term>Star formation</term><term>Starburst galaxies</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Morphologie</term><term>Galaxies infrarouges</term><term>Couleur</term><term>Densité spectrale énergie</term><term>Formation stellaire</term><term>Taux formation</term><term>Déplacement vers le rouge</term><term>Spectre IR</term><term>Hydrocarbure aromatique polycyclique</term><term>Loi puissance</term><term>Noyau galactique actif</term><term>Galaxies à flambée</term><term>Evolution galaxies</term><term>Galaxies actives</term><term>Noyau galaxies</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present Hubble Space Telescope imaging of 22 ultra-luminous infrared galaxies (ULIRGs) at z ≃ 2 with extremely red R - [24] colors (called dust-obscured galaxies, or DOGs) which have a local maximum in their spectral energy distribution (SED) at rest-frame 1.6 μm associated with stellar emission. These sources, which we call "bump DOGs," have star formation rates (SFRs) of 400-4000 M<sub>o</sub> yr<sup>-1</sup> and have redshifts derived from mid-IR spectra which show strong polycyclic aromatic hydrocarbon emission-a sign of vigorous ongoing star formation. Using a uniform morphological analysis, we look for quantifiable differences between bump DOGs, power-law DOGs (Spitzer-selected ULIRGs with mid-IR SEDs dominated by a power law and spectral features that are more typical of obscured active galactic nuclei than starbursts), submillimeter-selected galaxies, and other less-reddened ULIRGs from the Spitzer Extragalactic First Look Survey. Bump DOGs are larger than power-law DOGs (median Petrosian radius of 8.4 ± 2.7 kpc versus 5.5 ± 2.3 kpc) and exhibit more diffuse and irregular morphologies (median M<sub>20</sub> of -1.08 ± 0.05 versus -1.48 ± 0.05). These trends are qualitatively consistent with expectations from simulations of major mergers in which merging systems during the peak SFR period evolve from M<sub>20</sub> = -1.0 to M<sub>20</sub> = -1.7. Less-obscured ULIRGs (i.e., non-DOGs) tend to have more regular, centrally peaked, single-object morphologies rather than diffuse and irregular morphologies. This distinction in morphologies may imply that less-obscured ULIRGs sample the merger near the end of the peak SFR period. Alternatively, it may indicate that the intense star formation in these less-obscured ULIRGs is not the result of a recent major merger.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0004-637X</s0></fA01><fA02 i1="01"><s0>ASJOAB</s0></fA02><fA03 i2="1"><s0>Astrophys. j.</s0></fA03><fA05><s2>733</s2></fA05><fA06><s2>1</s2><s3>p. 1</s3></fA06><fA08 i1="01" i2="1" l="ENG"><s1>HUBBLE SPACE TELESCOPE MORPHOLOGIES OF z ˜ 2 DUST-OBSCURED GALAXIES. II. BUMP SOURCES</s1></fA08><fA11 i1="01" i2="1"><s1>BUSSMANN (R. S.)</s1></fA11><fA11 i1="02" i2="1"><s1>DEY (Arjun)</s1></fA11><fA11 i1="03" i2="1"><s1>LOTZ (J.)</s1></fA11><fA11 i1="04" i2="1"><s1>ARMUS (L.)</s1></fA11><fA11 i1="05" i2="1"><s1>BROWN (M. J. I.)</s1></fA11><fA11 i1="06" i2="1"><s1>DESAI (V.)</s1></fA11><fA11 i1="07" i2="1"><s1>EISENHARDT (P.)</s1></fA11><fA11 i1="08" i2="1"><s1>HIGDON (J.)</s1></fA11><fA11 i1="09" i2="1"><s1>HIGDON (S.)</s1></fA11><fA11 i1="10" i2="1"><s1>JANNUZI (B. T.)</s1></fA11><fA11 i1="11" i2="1"><s1>LE FLOC'H (E.)</s1></fA11><fA11 i1="12" i2="1"><s1>MELBOURNE (J.)</s1></fA11><fA11 i1="13" i2="1"><s1>SOIFER (B. T.)</s1></fA11><fA11 i1="14" i2="1"><s1>WEEDMAN (D.)</s1></fA11><fA14 i1="01"><s1>Steward Observatory, Department of Astronomy, University of Arizona, 933 North Cherry Avenue</s1><s2>Tucson, AZ 85721</s2><s3>USA</s3><sZ>1 aut.</sZ></fA14><fA14 i1="02"><s1>National Optical Astronomy Observatory, 950 North Cherry Avenue</s1><s2>Tucson, AZ 85719</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>10 aut.</sZ></fA14><fA14 i1="03"><s1>Spitzer Science Center, California Institute of Technology, MS 220-6</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>4 aut.</sZ><sZ>6 aut.</sZ><sZ>13 aut.</sZ></fA14><fA14 i1="04"><s1>School of Physics, Monash University</s1><s2>Clayton, Victoria 3800</s2><s3>AUS</s3><sZ>5 aut.</sZ></fA14><fA14 i1="05"><s1>Jet Propulsion Laboratory, California Institute of Technology, MC 169-327, 4800 Oak Grove Drive</s1><s2>Pasadena, CA 91109</s2><s3>USA</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ></fA14><fA14 i1="06"><s1>Georgia Southern University. P.O. Box 8031</s1><s2>Statesboro, GA</s2><s3>USA</s3><sZ>9 aut.</sZ></fA14><fA14 i1="07"><s1>Laboratoire AIM-Paris-Saclay, CEA-CNRS-Universite Paris Diderot, CEA Saclay</s1><s2>Gif-sur-Yvette, 91191</s2><s3>FRA</s3><sZ>11 aut.</sZ></fA14><fA14 i1="08"><s1>Caltech Optical Observatories, California Institute of Technology</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>12 aut.</sZ><sZ>13 aut.</sZ></fA14><fA14 i1="09"><s1>Astronomy Department, Cornell University</s1><s2>Ithaca, NY 14853</s2><s3>USA</s3><sZ>14 aut.</sZ></fA14><fA20><s2>73321.1-73321.18</s2></fA20><fA21><s1>2011</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>512</s2><s5>354000191605310210</s5></fA43><fA44><s0>0000</s0><s1>© 2011 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>3/4 p.</s0></fA45><fA47 i1="01" i2="1"><s0>11-0258025</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>The Astrophysical journal</s0></fA64><fA66 i1="01"><s0>GBR</s0></fA66><fC01 i1="01" l="ENG"><s0>We present Hubble Space Telescope imaging of 22 ultra-luminous infrared galaxies (ULIRGs) at z ≃ 2 with extremely red R - [24] colors (called dust-obscured galaxies, or DOGs) which have a local maximum in their spectral energy distribution (SED) at rest-frame 1.6 μm associated with stellar emission. These sources, which we call "bump DOGs," have star formation rates (SFRs) of 400-4000 M<sub>o</sub> yr<sup>-1</sup> and have redshifts derived from mid-IR spectra which show strong polycyclic aromatic hydrocarbon emission-a sign of vigorous ongoing star formation. Using a uniform morphological analysis, we look for quantifiable differences between bump DOGs, power-law DOGs (Spitzer-selected ULIRGs with mid-IR SEDs dominated by a power law and spectral features that are more typical of obscured active galactic nuclei than starbursts), submillimeter-selected galaxies, and other less-reddened ULIRGs from the Spitzer Extragalactic First Look Survey. Bump DOGs are larger than power-law DOGs (median Petrosian radius of 8.4 ± 2.7 kpc versus 5.5 ± 2.3 kpc) and exhibit more diffuse and irregular morphologies (median M<sub>20</sub> of -1.08 ± 0.05 versus -1.48 ± 0.05). These trends are qualitatively consistent with expectations from simulations of major mergers in which merging systems during the peak SFR period evolve from M<sub>20</sub> = -1.0 to M<sub>20</sub> = -1.7. Less-obscured ULIRGs (i.e., non-DOGs) tend to have more regular, centrally peaked, single-object morphologies rather than diffuse and irregular morphologies. This distinction in morphologies may imply that less-obscured ULIRGs sample the merger near the end of the peak SFR period. Alternatively, it may indicate that the intense star formation in these less-obscured ULIRGs is not the result of a recent major merger.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Morphologie</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Morphology</s0><s5>26</s5></fC03><fC03 i1="02" i2="X" l="FRE"><s0>Galaxies infrarouges</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="ENG"><s0>Infrared galaxies</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="SPA"><s0>Galaxias infrarrojas</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Couleur</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Color</s0><s5>28</s5></fC03><fC03 i1="04" i2="X" l="FRE"><s0>Densité spectrale énergie</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="ENG"><s0>Spectral energy distribution</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="SPA"><s0>Densidad espectral energía</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Formation stellaire</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Star formation</s0><s5>30</s5></fC03><fC03 i1="06" i2="X" l="FRE"><s0>Taux formation</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="ENG"><s0>Formation rate</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="SPA"><s0>Grado formación</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Déplacement vers le rouge</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Red shift</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Spectre IR</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Infrared spectra</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Hydrocarbure aromatique polycyclique</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Polycyclic aromatic hydrocarbons</s0><s5>34</s5></fC03><fC03 i1="10" i2="X" l="FRE"><s0>Loi puissance</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="ENG"><s0>Power law</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="SPA"><s0>Ley poder</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Noyau galactique actif</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Active galaxy nuclei</s0><s5>36</s5></fC03><fC03 i1="12" i2="X" l="FRE"><s0>Galaxies à flambée</s0><s5>37</s5></fC03><fC03 i1="12" i2="X" l="ENG"><s0>Starburst galaxies</s0><s5>37</s5></fC03><fC03 i1="12" i2="X" l="SPA"><s0>Galaxias llamarada estelar</s0><s5>37</s5></fC03><fC03 i1="13" i2="X" l="FRE"><s0>Evolution galaxies</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="ENG"><s0>Galaxy evolution</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="SPA"><s0>Evolución galaxias</s0><s5>38</s5></fC03><fC03 i1="14" i2="3" l="FRE"><s0>Galaxies actives</s0><s5>39</s5></fC03><fC03 i1="14" i2="3" l="ENG"><s0>Active galaxies</s0><s5>39</s5></fC03><fC03 i1="15" i2="3" l="FRE"><s0>Noyau galaxies</s0><s5>40</s5></fC03><fC03 i1="15" i2="3" l="ENG"><s0>Galaxy nuclei</s0><s5>40</s5></fC03><fN21><s1>178</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 11-0258025 INIST</NO><ET>HUBBLE SPACE TELESCOPE MORPHOLOGIES OF z ˜ 2 DUST-OBSCURED GALAXIES. II. BUMP SOURCES</ET><AU>BUSSMANN (R. S.); DEY (Arjun); LOTZ (J.); ARMUS (L.); BROWN (M. J. I.); DESAI (V.); EISENHARDT (P.); HIGDON (J.); HIGDON (S.); JANNUZI (B. T.); LE FLOC'H (E.); MELBOURNE (J.); SOIFER (B. T.); WEEDMAN (D.)</AU><AF>Steward Observatory, Department of Astronomy, University of Arizona, 933 North Cherry Avenue/Tucson, AZ 85721/Etats-Unis (1 aut.); National Optical Astronomy Observatory, 950 North Cherry Avenue/Tucson, AZ 85719/Etats-Unis (2 aut., 3 aut., 10 aut.); Spitzer Science Center, California Institute of Technology, MS 220-6/Pasadena, CA 91125/Etats-Unis (4 aut., 6 aut., 13 aut.); School of Physics, Monash University/Clayton, Victoria 3800/Australie (5 aut.); Jet Propulsion Laboratory, California Institute of Technology, MC 169-327, 4800 Oak Grove Drive/Pasadena, CA 91109/Etats-Unis (7 aut., 8 aut.); Georgia Southern University. P.O. Box 8031/Statesboro, GA/Etats-Unis (9 aut.); Laboratoire AIM-Paris-Saclay, CEA-CNRS-Universite Paris Diderot, CEA Saclay/Gif-sur-Yvette, 91191/France (11 aut.); Caltech Optical Observatories, California Institute of Technology/Pasadena, CA 91125/Etats-Unis (12 aut., 13 aut.); Astronomy Department, Cornell University/Ithaca, NY 14853/Etats-Unis (14 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>The Astrophysical journal; ISSN 0004-637X; Coden ASJOAB; Royaume-Uni; Da. 2011; Vol. 733; No. 1 p. 1; 73321.1-73321.18; Bibl. 3/4 p.</SO><LA>Anglais</LA><EA>We present Hubble Space Telescope imaging of 22 ultra-luminous infrared galaxies (ULIRGs) at z ≃ 2 with extremely red R - [24] colors (called dust-obscured galaxies, or DOGs) which have a local maximum in their spectral energy distribution (SED) at rest-frame 1.6 μm associated with stellar emission. These sources, which we call "bump DOGs," have star formation rates (SFRs) of 400-4000 M<sub>o</sub> yr<sup>-1</sup> and have redshifts derived from mid-IR spectra which show strong polycyclic aromatic hydrocarbon emission-a sign of vigorous ongoing star formation. Using a uniform morphological analysis, we look for quantifiable differences between bump DOGs, power-law DOGs (Spitzer-selected ULIRGs with mid-IR SEDs dominated by a power law and spectral features that are more typical of obscured active galactic nuclei than starbursts), submillimeter-selected galaxies, and other less-reddened ULIRGs from the Spitzer Extragalactic First Look Survey. Bump DOGs are larger than power-law DOGs (median Petrosian radius of 8.4 ± 2.7 kpc versus 5.5 ± 2.3 kpc) and exhibit more diffuse and irregular morphologies (median M<sub>20</sub> of -1.08 ± 0.05 versus -1.48 ± 0.05). These trends are qualitatively consistent with expectations from simulations of major mergers in which merging systems during the peak SFR period evolve from M<sub>20</sub> = -1.0 to M<sub>20</sub> = -1.7. Less-obscured ULIRGs (i.e., non-DOGs) tend to have more regular, centrally peaked, single-object morphologies rather than diffuse and irregular morphologies. This distinction in morphologies may imply that less-obscured ULIRGs sample the merger near the end of the peak SFR period. Alternatively, it may indicate that the intense star formation in these less-obscured ULIRGs is not the result of a recent major merger.</EA><CC>001E03</CC><FD>Morphologie; Galaxies infrarouges; Couleur; Densité spectrale énergie; Formation stellaire; Taux formation; Déplacement vers le rouge; Spectre IR; Hydrocarbure aromatique polycyclique; Loi puissance; Noyau galactique actif; Galaxies à flambée; Evolution galaxies; Galaxies actives; Noyau galaxies</FD><ED>Morphology; Infrared galaxies; Color; Spectral energy distribution; Star formation; Formation rate; Red shift; Infrared spectra; Polycyclic aromatic hydrocarbons; Power law; Active galaxy nuclei; Starburst galaxies; Galaxy evolution; Active galaxies; Galaxy nuclei</ED><SD>Galaxias infrarrojas; Densidad espectral energía; Grado formación; Ley poder; Galaxias llamarada estelar; Evolución galaxias</SD><LO>INIST-512.354000191605310210</LO><ID>11-0258025</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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