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.
Descripteurs français
- Pascal (Inist)
English descriptors
- KwdEn :
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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Pascal:11-0258025Le document en format XML
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<sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">HUBBLE SPACE TELESCOPE MORPHOLOGIES OF z ˜ 2 DUST-OBSCURED GALAXIES. II. BUMP SOURCES</title>
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<series><title level="j" type="main">The Astrophysical journal</title>
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<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>
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<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>
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</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>
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