Enriched haloes at redshift z = 2 with no star formation: implications for accretion and wind scenarios
Identifieur interne : 005C90 ( Main/Exploration ); précédent : 005C89; suivant : 005C91Enriched haloes at redshift z = 2 with no star formation: implications for accretion and wind scenarios
Auteurs : N. Bouche [États-Unis, France] ; M. T. Murphy [Australie] ; C. Peroux [France] ; T. Contini [France] ; C. L. Martin [États-Unis] ; N. M. Forster Schreiber [Allemagne] ; R. Genzel [Allemagne] ; D. Lutz [Allemagne] ; S. Gillessen [Allemagne] ; L. Tacconi [Allemagne] ; R. Davies [Allemagne] ; F. Eisenhauer [Allemagne]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2012.
Descripteurs français
- Pascal (Inist)
- Déplacement vers le rouge, Formation stellaire, Accrétion, Vent galactique, Galaxies raies émission, Quasar, Raie H alpha, Largeur équivalente, Taux formation, Fonction masse initiale, Continuum, Critère sélection, Paramètre impact, Ionisation, Vent stellaire, Masse stellaire, Evolution galaxies, Formation galaxies, Halo galaxies, Matière intergalactique, Raie absorption.
English descriptors
- KwdEn :
- Absorption line, Accretion, Continuum, Emission line galaxies, Equivalent width, Formation rate, Galactic wind, Galaxy evolution, Galaxy formation, Galaxy halo, H-alpha lines, Impact parameter, Initial mass function, Intergalactic matter, Ionization, Quasars, Red shift, Selection criterion, Star formation, Stellar mass, Stellar winds.
Abstract
In order to understand which process (e.g. galactic winds, cold accretion) is responsible for the cool (T ˜ 104 K) halo gas around galaxies, we embarked on a programme to study the star formation properties of galaxies selected by their Mg II absorption signature in quasar spectra. Specifically, we searched for the Hα line emission from galaxies near very strong z ≃ 2 Mg II absorbers (with rest-frame equivalent width Wλ2796r ? 2 Å) because these could be the signposts of outflows or inflows. Surprisingly, we detect Hα from only four hosts out of 20 sightlines (and two out of the 19 HI-selected sightlines), despite reaching a star formation rate (SFR) sensitivity limit of 2.9 M◦. yr-1 (5σ) for a Chabrier initial mass function. This low success rate (4/20) is in contrast with our z≃1 survey where we detected 66 per cent (14/21) of the Mg II hosts (down to 0.6 M◦. yr-1; 5σ). Taking into account the difference in sensitivity between the two surveys, we should have been able to detect ≥11.4 (≥7.6) of the 20 z ≃ 2 hosts - assuming that SFR evolves as (1 + z)γ with γ = 2.5 (or γ = 0) respectively -whereas we found only four galaxies. Interestingly, all the z = 2 detected hosts have observed SFRs ? 9 M◦. yr-1, well above our sensitivity limit, while at z = 1 they all have SFR < 9 M◦. yr-1, an evolution that is in good agreement with the evolution of the SFR main sequence, i.e. with γ = 2.5. Moreover, we show that the z = 2 undetected hosts are not hidden under the quasar continuum after stacking our data. They also cannot be outside our surveyed area as this latter option runs against our sample selection criteria (Wλ2796r > 2 Å) and the known Wλ2796r-impact parameter relation for low-ionization ions. Hence, strong Mg II absorbers could trace star-formation-driven winds in low-mass haloes (Mh ≤ 1010.6 M◦.), provided that the winds do not extend beyond 20 kpc in order not to violate the evolution of the absorber number density dN/dz (Mg II). Alternatively, our results imply that z = 2 galaxies traced by strong Mg II absorbers do not form stars at a rate expected (3-10 M◦.) yr-1) for their (halo or stellar) masses, supporting the existence of a transition in accretion efficiency at Mh ≃ 1011 M◦.. This scenario can explain both the detections and the non-detections.
Affiliations:
- Allemagne, Australie, France, États-Unis
- Midi-Pyrénées, Occitanie (région administrative), Provence-Alpes-Côte d'Azur
- Marseille, Toulouse
Links toward previous steps (curation, corpus...)
- to stream PascalFrancis, to step Corpus: 001692
- to stream PascalFrancis, to step Curation: 004817
- to stream PascalFrancis, to step Checkpoint: 001166
- to stream Main, to step Merge: 006001
- to stream Main, to step Curation: 005C90
Le document en format XML
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Bouche</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics, University of California</s1><s2>Santa Barbara, CA 93106</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ></inist:fA14><country>États-Unis</country><wicri:noRegion>Santa Barbara, CA 93106</wicri:noRegion></affiliation><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>CNRS, Institut de Recherche en Astrophysique et Planétologie [IRAP] de Toulouse, 14 Avenue E. Belin</s1><s2>31400 Toulouse</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>4 aut.</sZ></inist:fA14><country>France</country><wicri:noRegion>31400 Toulouse</wicri:noRegion><placeName><settlement type="city">Toulouse</settlement><region type="region" nuts="2">Occitanie (région administrative)</region><region type="old region" nuts="2">Midi-Pyrénées</region></placeName></affiliation><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Université Paul Sabatier de Toulouse, UPS-OMP, IRAP</s1><s2>31400 Toulouse</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>4 aut.</sZ></inist:fA14><country>France</country><wicri:noRegion>31400 Toulouse</wicri:noRegion><placeName><settlement type="city">Toulouse</settlement><region type="region" nuts="2">Occitanie (région administrative)</region><region type="old region" nuts="2">Midi-Pyrénées</region></placeName></affiliation></author><author><name sortKey="Murphy, M T" sort="Murphy, M T" uniqKey="Murphy M" first="M. T." last="Murphy">M. T. Murphy</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Swinburne University of Technology, Mail H30, PO Box 218</s1><s2>Hawthorn, VIC 3122</s2><s3>AUS</s3><sZ>2 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Hawthorn, VIC 3122</wicri:noRegion></affiliation></author><author><name sortKey="Peroux, C" sort="Peroux, C" uniqKey="Peroux C" first="C." last="Peroux">C. Peroux</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Observatoire d'Astrophysique de Marseille-Provence, 38 rue Frédéric Joliot-Curie</s1><s2>13388 Marseille</s2><s3>FRA</s3><sZ>3 aut.</sZ></inist:fA14><country>France</country><wicri:noRegion>13388 Marseille</wicri:noRegion><placeName><settlement type="city">Marseille</settlement><region type="région" nuts="2">Provence-Alpes-Côte d'Azur</region></placeName></affiliation></author><author><name sortKey="Contini, T" sort="Contini, T" uniqKey="Contini T" first="T." last="Contini">T. Contini</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>CNRS, Institut de Recherche en Astrophysique et Planétologie [IRAP] de Toulouse, 14 Avenue E. Belin</s1><s2>31400 Toulouse</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>4 aut.</sZ></inist:fA14><country>France</country><wicri:noRegion>31400 Toulouse</wicri:noRegion><placeName><settlement type="city">Toulouse</settlement><region type="region" nuts="2">Occitanie (région administrative)</region><region type="old region" nuts="2">Midi-Pyrénées</region></placeName></affiliation><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Université Paul Sabatier de Toulouse, UPS-OMP, IRAP</s1><s2>31400 Toulouse</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>4 aut.</sZ></inist:fA14><country>France</country><wicri:noRegion>31400 Toulouse</wicri:noRegion><placeName><settlement type="city">Toulouse</settlement><region type="region" nuts="2">Occitanie (région administrative)</region><region type="old region" nuts="2">Midi-Pyrénées</region></placeName></affiliation></author><author><name sortKey="Martin, C L" sort="Martin, C L" uniqKey="Martin C" first="C. L." last="Martin">C. L. Martin</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics, University of California</s1><s2>Santa Barbara, CA 93106</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ></inist:fA14><country>États-Unis</country><wicri:noRegion>Santa Barbara, CA 93106</wicri:noRegion></affiliation></author><author><name sortKey="Forster Schreiber, N M" sort="Forster Schreiber, N M" uniqKey="Forster Schreiber N" first="N. M." last="Forster Schreiber">N. M. Forster Schreiber</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Max Planck Institut für extraterrestrische Physik, Giessenbachstrasse</s1><s2>85748 Garching</s2><s3>DEU</s3><sZ>6 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>12 aut.</sZ></inist:fA14><country>Allemagne</country><wicri:noRegion>85748 Garching</wicri:noRegion><wicri:noRegion>Giessenbachstrasse</wicri:noRegion><wicri:noRegion>85748 Garching</wicri:noRegion></affiliation></author><author><name sortKey="Genzel, R" sort="Genzel, R" uniqKey="Genzel R" first="R." last="Genzel">R. Genzel</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Max Planck Institut für extraterrestrische Physik, Giessenbachstrasse</s1><s2>85748 Garching</s2><s3>DEU</s3><sZ>6 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>12 aut.</sZ></inist:fA14><country>Allemagne</country><wicri:noRegion>85748 Garching</wicri:noRegion><wicri:noRegion>Giessenbachstrasse</wicri:noRegion><wicri:noRegion>85748 Garching</wicri:noRegion></affiliation></author><author><name sortKey="Lutz, D" sort="Lutz, D" uniqKey="Lutz D" first="D." last="Lutz">D. Lutz</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Max Planck Institut für extraterrestrische Physik, Giessenbachstrasse</s1><s2>85748 Garching</s2><s3>DEU</s3><sZ>6 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>12 aut.</sZ></inist:fA14><country>Allemagne</country><wicri:noRegion>85748 Garching</wicri:noRegion><wicri:noRegion>Giessenbachstrasse</wicri:noRegion><wicri:noRegion>85748 Garching</wicri:noRegion></affiliation></author><author><name sortKey="Gillessen, S" sort="Gillessen, S" uniqKey="Gillessen S" first="S." last="Gillessen">S. Gillessen</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Max Planck Institut für extraterrestrische Physik, Giessenbachstrasse</s1><s2>85748 Garching</s2><s3>DEU</s3><sZ>6 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>12 aut.</sZ></inist:fA14><country>Allemagne</country><wicri:noRegion>85748 Garching</wicri:noRegion><wicri:noRegion>Giessenbachstrasse</wicri:noRegion><wicri:noRegion>85748 Garching</wicri:noRegion></affiliation></author><author><name sortKey="Tacconi, L" sort="Tacconi, L" uniqKey="Tacconi L" first="L." last="Tacconi">L. Tacconi</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Max Planck Institut für extraterrestrische Physik, Giessenbachstrasse</s1><s2>85748 Garching</s2><s3>DEU</s3><sZ>6 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>12 aut.</sZ></inist:fA14><country>Allemagne</country><wicri:noRegion>85748 Garching</wicri:noRegion><wicri:noRegion>Giessenbachstrasse</wicri:noRegion><wicri:noRegion>85748 Garching</wicri:noRegion></affiliation></author><author><name sortKey="Davies, R" sort="Davies, R" uniqKey="Davies R" first="R." last="Davies">R. Davies</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Max Planck Institut für extraterrestrische Physik, Giessenbachstrasse</s1><s2>85748 Garching</s2><s3>DEU</s3><sZ>6 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>12 aut.</sZ></inist:fA14><country>Allemagne</country><wicri:noRegion>85748 Garching</wicri:noRegion><wicri:noRegion>Giessenbachstrasse</wicri:noRegion><wicri:noRegion>85748 Garching</wicri:noRegion></affiliation></author><author><name sortKey="Eisenhauer, F" sort="Eisenhauer, F" uniqKey="Eisenhauer F" first="F." last="Eisenhauer">F. Eisenhauer</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Max Planck Institut für extraterrestrische Physik, Giessenbachstrasse</s1><s2>85748 Garching</s2><s3>DEU</s3><sZ>6 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>12 aut.</sZ></inist:fA14><country>Allemagne</country><wicri:noRegion>85748 Garching</wicri:noRegion><wicri:noRegion>Giessenbachstrasse</wicri:noRegion><wicri:noRegion>85748 Garching</wicri:noRegion></affiliation></author></analytic><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno><imprint><date when="2012">2012</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Absorption line</term><term>Accretion</term><term>Continuum</term><term>Emission line galaxies</term><term>Equivalent width</term><term>Formation rate</term><term>Galactic wind</term><term>Galaxy evolution</term><term>Galaxy formation</term><term>Galaxy halo</term><term>H-alpha lines</term><term>Impact parameter</term><term>Initial mass function</term><term>Intergalactic matter</term><term>Ionization</term><term>Quasars</term><term>Red shift</term><term>Selection criterion</term><term>Star formation</term><term>Stellar mass</term><term>Stellar winds</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Déplacement vers le rouge</term><term>Formation stellaire</term><term>Accrétion</term><term>Vent galactique</term><term>Galaxies raies émission</term><term>Quasar</term><term>Raie H alpha</term><term>Largeur équivalente</term><term>Taux formation</term><term>Fonction masse initiale</term><term>Continuum</term><term>Critère sélection</term><term>Paramètre impact</term><term>Ionisation</term><term>Vent stellaire</term><term>Masse stellaire</term><term>Evolution galaxies</term><term>Formation galaxies</term><term>Halo galaxies</term><term>Matière intergalactique</term><term>Raie absorption</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">In order to understand which process (e.g. galactic winds, cold accretion) is responsible for the cool (T ˜ 10<sup>4</sup> K) halo gas around galaxies, we embarked on a programme to study the star formation properties of galaxies selected by their Mg II absorption signature in quasar spectra. Specifically, we searched for the Hα line emission from galaxies near very strong z ≃ 2 Mg II absorbers (with rest-frame equivalent width W<sup>λ2796</sup><sub>r </sub>? 2 Å) because these could be the signposts of outflows or inflows. Surprisingly, we detect Hα from only four hosts out of 20 sightlines (and two out of the 19 HI-selected sightlines), despite reaching a star formation rate (SFR) sensitivity limit of 2.9 M<sub>◦.</sub> yr<sup>-1 </sup>(5σ) for a Chabrier initial mass function. This low success rate (4/20) is in contrast with our z≃1 survey where we detected 66 per cent (14/21) of the Mg II hosts (down to 0.6 M<sub>◦.</sub> yr<sup>-1</sup>; 5σ). Taking into account the difference in sensitivity between the two surveys, we should have been able to detect ≥11.4 (≥7.6) of the 20 z ≃ 2 hosts - assuming that SFR evolves as (1 + z)<sup>γ</sup> with γ = 2.5 (or γ = 0) respectively -whereas we found only four galaxies. Interestingly, all the z = 2 detected hosts have observed SFRs ? 9 M<sub>◦. </sub>yr<sup>-1</sup>, well above our sensitivity limit, while at z = 1 they all have SFR < 9 M<sub>◦.</sub> yr<sup>-1</sup>, an evolution that is in good agreement with the evolution of the SFR main sequence, i.e. with γ = 2.5. Moreover, we show that the z = 2 undetected hosts are not hidden under the quasar continuum after stacking our data. They also cannot be outside our surveyed area as this latter option runs against our sample selection criteria (W<sup>λ2796</sup><sub>r </sub>> 2 Å) and the known W<sup>λ2796</sup><sub>r</sub>-impact parameter relation for low-ionization ions. Hence, strong Mg II absorbers could trace star-formation-driven winds in low-mass haloes (M<sub>h</sub> ≤ 10<sup>10.6</sup> M<sub>◦.</sub>), provided that the winds do not extend beyond 20 kpc in order not to violate the evolution of the absorber number density dN/dz (Mg II). Alternatively, our results imply that z = 2 galaxies traced by strong Mg II absorbers do not form stars at a rate expected (3-10 M<sub>◦.</sub>) yr<sup>-1</sup>) for their (halo or stellar) masses, supporting the existence of a transition in accretion efficiency at M<sub>h</sub> ≃ 10<sup>11</sup> M<sub>◦.</sub>. This scenario can explain both the detections and the non-detections.</div> </front></TEI><affiliations><list><country><li>Allemagne</li><li>Australie</li><li>France</li><li>États-Unis</li></country><region><li>Midi-Pyrénées</li><li>Occitanie (région administrative)</li><li>Provence-Alpes-Côte d'Azur</li></region><settlement><li>Marseille</li><li>Toulouse</li></settlement></list><tree><country name="États-Unis"><noRegion><name sortKey="Bouche, N" sort="Bouche, N" uniqKey="Bouche N" first="N." last="Bouche">N. Bouche</name></noRegion><name sortKey="Martin, C L" sort="Martin, C L" uniqKey="Martin C" first="C. L." last="Martin">C. L. Martin</name></country><country name="France"><region name="Occitanie (région administrative)"><name sortKey="Bouche, N" sort="Bouche, N" uniqKey="Bouche N" first="N." last="Bouche">N. Bouche</name></region><name sortKey="Bouche, N" sort="Bouche, N" uniqKey="Bouche N" first="N." last="Bouche">N. Bouche</name><name sortKey="Contini, T" sort="Contini, T" uniqKey="Contini T" first="T." last="Contini">T. Contini</name><name sortKey="Contini, T" sort="Contini, T" uniqKey="Contini T" first="T." last="Contini">T. Contini</name><name sortKey="Peroux, C" sort="Peroux, C" uniqKey="Peroux C" first="C." last="Peroux">C. Peroux</name></country><country name="Australie"><noRegion><name sortKey="Murphy, M T" sort="Murphy, M T" uniqKey="Murphy M" first="M. T." last="Murphy">M. T. Murphy</name></noRegion></country><country name="Allemagne"><noRegion><name sortKey="Forster Schreiber, N M" sort="Forster Schreiber, N M" uniqKey="Forster Schreiber N" first="N. M." last="Forster Schreiber">N. M. Forster Schreiber</name></noRegion><name sortKey="Davies, R" sort="Davies, R" uniqKey="Davies R" first="R." last="Davies">R. Davies</name><name sortKey="Eisenhauer, F" sort="Eisenhauer, F" uniqKey="Eisenhauer F" first="F." last="Eisenhauer">F. Eisenhauer</name><name sortKey="Genzel, R" sort="Genzel, R" uniqKey="Genzel R" first="R." last="Genzel">R. Genzel</name><name sortKey="Gillessen, S" sort="Gillessen, S" uniqKey="Gillessen S" first="S." last="Gillessen">S. Gillessen</name><name sortKey="Lutz, D" sort="Lutz, D" uniqKey="Lutz D" first="D." last="Lutz">D. Lutz</name><name sortKey="Tacconi, L" sort="Tacconi, L" uniqKey="Tacconi L" first="L." last="Tacconi">L. Tacconi</name></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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