Hubble Space Telescope imaging of the CFRS and LDSS redshift surveys – IV. Influence of mergers in the evolution of faint field galaxies from z∼1
Identifieur interne : 001E09 ( Istex/Curation ); précédent : 001E08; suivant : 001E10Hubble Space Telescope imaging of the CFRS and LDSS redshift surveys – IV. Influence of mergers in the evolution of faint field galaxies from z∼1
Auteurs : O. Le Fèvre [France] ; R. Abraham [Royaume-Uni] ; S. J. Lilly [Canada] ; R. S. Ellis [Royaume-Uni] ; J. Brinchmann [Royaume-Uni] ; D. Schade [Canada] ; L. Tresse [France, Italie] ; M. Colless [Australie] ; D. Crampton [Canada] ; K. Glazebrook [Australie] ; F. Hammer [France] ; T. Broadhurst [États-Unis]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2000-01-21.
Descripteurs français
- Wicri :
- topic : Fusion d'entreprises.
English descriptors
- KwdEn :
- Bright galaxies, Cent level, Cfrs, Cfrs1ldss, Companion galaxy, Complete sample, Considerable uncertainties, Data points, Double nuclei, Dwarf galaxies, Elli, Enhancement, Equivalent width, Excellent agreement, Fevre, Galaxy, Galaxy formation, Galaxy images, Galaxy pairs, Galaxy population, Glazebrook, Hernquist, High redshifts, Higher redshifts, Imaging, Imaging data, Important role, Individual image, Ldss, Ldss redshift surveys, Local universe, Luminosity, Luminosity density, Luminosity enhancement, Luminosity evolution, Luminosity function, Magnitude difference, Major mergers, Manual classification, Merger, Merger class, Merger events, Merger fraction, Merger rate, Mihos, Mihos hernquist, Minor mergers, Mnras, Number density, Number evolution, Ongoing, Ongoing mergers, Pair counts, Pair fraction, Patton, Physical pair fraction, Physical pairs, Present paper, Primary galaxy, Projection effects, Redshift, Redshift survey, Simple coaddition, Star formation, Star formation activity, Star formation rate, Star formation rate increase, Survey galaxies, Total number, Upcoming, Upcoming mergers, Upper right corner, Visual approach, Visual classification, Visual classification scheme, Visual identification, Whole sample.
- Teeft :
- Bright galaxies, Cent level, Cfrs, Cfrs1ldss, Companion galaxy, Complete sample, Considerable uncertainties, Data points, Double nuclei, Dwarf galaxies, Elli, Enhancement, Equivalent width, Excellent agreement, Fevre, Galaxy, Galaxy formation, Galaxy images, Galaxy pairs, Galaxy population, Glazebrook, Hernquist, High redshifts, Higher redshifts, Imaging, Imaging data, Important role, Individual image, Ldss, Ldss redshift surveys, Local universe, Luminosity, Luminosity density, Luminosity enhancement, Luminosity evolution, Luminosity function, Magnitude difference, Major mergers, Manual classification, Merger, Merger class, Merger events, Merger fraction, Merger rate, Mihos, Mihos hernquist, Minor mergers, Mnras, Number density, Number evolution, Ongoing, Ongoing mergers, Pair counts, Pair fraction, Patton, Physical pair fraction, Physical pairs, Present paper, Primary galaxy, Projection effects, Redshift, Redshift survey, Simple coaddition, Star formation, Star formation activity, Star formation rate, Star formation rate increase, Survey galaxies, Total number, Upcoming, Upcoming mergers, Upper right corner, Visual approach, Visual classification, Visual classification scheme, Visual identification, Whole sample.
Abstract
Hubble Space Telescope images of a sample of 285 galaxies with measured redshifts from the Canada–France Redshift Survey (CFRS) and Autofib–Low Dispersion Spectrograph Survey (LDSS) redshift surveys are analysed to derive the evolution of the merger fraction out to redshifts z∼1. We have performed visual and machine‐based merger identifications, as well as counts of bright pairs of galaxies with magnitude differences δm≤1.5 mag. We find that the pair fraction increases with redshift, with up to ∼20 per cent of the galaxies being in physical pairs at z∼0.75–1. We derive a merger fraction varying with redshift as ∝(1+z)3.2±0.6, after correction for line‐of‐sight contamination, in excellent agreement with the merger fraction derived from the visual classification of mergers for which m=3.4±0.6. After correcting for seeing effects on the ground‐based selection of survey galaxies, we conclude that the pair fraction evolves as ∝(1+z)2.7±0.6. This implies that an average L* galaxy will have undergone 0.8–1.8 merger events from z=1 to z=0, with 0.5 to 1.2 merger events occuring in a 2‐Gyr time‐span at around z∼0.9. This result is consistent with predictions from semi‐analytical models of galaxy formation. From the simple coaddition of the observed luminosities of the galaxies in pairs, physical mergers are computed to lead to a brightening of 0.5 mag for each pair on average, and a boost in star formation rate of a factor of 2, as derived from the average [O ii] equivalent widths. Mergers of galaxies are therefore contributing significantly to the evolution of both the luminosity function and luminosity density of the Universe out to z∼1.
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DOI: 10.1046/j.1365-8711.2000.03083.x
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Influence of mergers in the evolution of faint field galaxies from <hi rend="italic">z</hi>∼1</title><author><name sortKey="Le Fevre, O" sort="Le Fevre, O" uniqKey="Le Fevre O" first="O." last="Le Fèvre">O. Le Fèvre</name><affiliation wicri:level="1"><mods:affiliation>Laboratoire d’Astronomie Spatiale ‐ CNRS, Traverse du Siphon, B.P.8, 13376 Marseille Cedex 12, France</mods:affiliation><country xml:lang="fr">France</country><wicri:regionArea>Laboratoire d’Astronomie Spatiale ‐ CNRS, Traverse du Siphon, B.P.8, 13376 Marseille Cedex 12</wicri:regionArea></affiliation><affiliation wicri:level="1"><mods:affiliation>E-mail: lefevre@astrsp‐mrs.fr</mods:affiliation><country wicri:rule="url">France</country></affiliation></author><author><name sortKey="Abraham, R" sort="Abraham, R" uniqKey="Abraham R" first="R." last="Abraham">R. Abraham</name><affiliation wicri:level="4"><mods:affiliation>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA</mods:affiliation><orgName type="university">Université de Cambridge</orgName><country>Royaume-Uni</country><placeName><settlement type="city">Cambridge</settlement><region type="country">Angleterre</region><region type="région" nuts="1">Angleterre de l'Est</region></placeName></affiliation></author><author><name sortKey="Lilly, S J" sort="Lilly, S J" uniqKey="Lilly S" first="S. J." last="Lilly">S. J. Lilly</name><affiliation wicri:level="1"><mods:affiliation>Department of Astronomy, University of Toronto, 60 St George Street, Toronto, Ontario, M5S 3H8, Canada</mods:affiliation><country xml:lang="fr">Canada</country><wicri:regionArea>Department of Astronomy, University of Toronto, 60 St George Street, Toronto, Ontario, M5S 3H8</wicri:regionArea></affiliation></author><author><name sortKey="Ellis, R S" sort="Ellis, R S" uniqKey="Ellis R" first="R. S." last="Ellis">R. S. Ellis</name><affiliation wicri:level="4"><mods:affiliation>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA</mods:affiliation><orgName type="university">Université de Cambridge</orgName><country>Royaume-Uni</country><placeName><settlement type="city">Cambridge</settlement><region type="country">Angleterre</region><region type="région" nuts="1">Angleterre de l'Est</region></placeName></affiliation></author><author><name sortKey="Brinchmann, J" sort="Brinchmann, J" uniqKey="Brinchmann J" first="J." last="Brinchmann">J. Brinchmann</name><affiliation wicri:level="4"><mods:affiliation>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA</mods:affiliation><orgName type="university">Université de Cambridge</orgName><country>Royaume-Uni</country><placeName><settlement type="city">Cambridge</settlement><region type="country">Angleterre</region><region type="région" nuts="1">Angleterre de l'Est</region></placeName></affiliation></author><author><name sortKey="Schade, D" sort="Schade, D" uniqKey="Schade D" first="D." last="Schade">D. Schade</name><affiliation wicri:level="1"><mods:affiliation>Dominion Astrophysical Observatory, 5071 West Saanich Road, Victoria, BC, V8X 4M6, Canada</mods:affiliation><country xml:lang="fr">Canada</country><wicri:regionArea>Dominion Astrophysical Observatory, 5071 West Saanich Road, Victoria, BC, V8X 4M6</wicri:regionArea></affiliation></author><author><name sortKey="Tresse, L" sort="Tresse, L" uniqKey="Tresse L" first="L." last="Tresse">L. Tresse</name><affiliation wicri:level="1"><mods:affiliation>Laboratoire d’Astronomie Spatiale ‐ CNRS, Traverse du Siphon, B.P.8, 13376 Marseille Cedex 12, France</mods:affiliation><country xml:lang="fr">France</country><wicri:regionArea>Laboratoire d’Astronomie Spatiale ‐ CNRS, Traverse du Siphon, B.P.8, 13376 Marseille Cedex 12</wicri:regionArea></affiliation><affiliation wicri:level="1"><mods:affiliation>Istituto di Radioastronomia – CNR, Via P. Gobetti, 101 40129 Bologna, Italy</mods:affiliation><country xml:lang="fr">Italie</country><wicri:regionArea>Istituto di Radioastronomia – CNR, Via P. Gobetti, 101 40129 Bologna</wicri:regionArea></affiliation></author><author><name sortKey="Colless, M" sort="Colless, M" uniqKey="Colless M" first="M." last="Colless">M. Colless</name><affiliation wicri:level="1"><mods:affiliation>Mount Stromlo & Siding Spring Observatories, Australian National University, Weston Creek, Canberra, ACT 2611, Australia</mods:affiliation><country xml:lang="fr">Australie</country><wicri:regionArea>Mount Stromlo & Siding Spring Observatories, Australian National University, Weston Creek, Canberra, ACT 2611</wicri:regionArea></affiliation></author><author><name sortKey="Crampton, D" sort="Crampton, D" uniqKey="Crampton D" first="D." last="Crampton">D. Crampton</name><affiliation wicri:level="1"><mods:affiliation>Dominion Astrophysical Observatory, 5071 West Saanich Road, Victoria, BC, V8X 4M6, Canada</mods:affiliation><country xml:lang="fr">Canada</country><wicri:regionArea>Dominion Astrophysical Observatory, 5071 West Saanich Road, Victoria, BC, V8X 4M6</wicri:regionArea></affiliation></author><author><name sortKey="Glazebrook, K" sort="Glazebrook, K" uniqKey="Glazebrook K" first="K." last="Glazebrook">K. Glazebrook</name><affiliation wicri:level="1"><mods:affiliation>Anglo‐Australian Observatory, P.O. Box 296, Epping, NSW 1710, Australia</mods:affiliation><country xml:lang="fr">Australie</country><wicri:regionArea>Anglo‐Australian Observatory, P.O. Box 296, Epping, NSW 1710</wicri:regionArea></affiliation></author><author><name sortKey="Hammer, F" sort="Hammer, F" uniqKey="Hammer F" first="F." last="Hammer">F. Hammer</name><affiliation wicri:level="1"><mods:affiliation>DAEC, Observatoire de Paris‐Meudon, 92195 Meudon Cedex, France</mods:affiliation><country xml:lang="fr">France</country><wicri:regionArea>DAEC, Observatoire de Paris‐Meudon, 92195 Meudon Cedex</wicri:regionArea></affiliation></author><author><name sortKey="Broadhurst, T" sort="Broadhurst, T" uniqKey="Broadhurst T" first="T." last="Broadhurst">T. Broadhurst</name><affiliation wicri:level="1"><mods:affiliation>Department of Astronomy, University of California, 601 Campbell Hall, University of California, Berkeley CA 94720‐3411, USA</mods:affiliation><country xml:lang="fr">États-Unis</country><wicri:regionArea>Department of Astronomy, University of California, 601 Campbell Hall, University of California, Berkeley CA 94720‐3411</wicri:regionArea></affiliation></author></analytic><monogr></monogr><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><biblScope unit="vol">311</biblScope><biblScope unit="issue">3</biblScope><biblScope unit="page" from="565">565</biblScope><biblScope unit="page" to="575">575</biblScope><biblScope unit="page-count">11</biblScope><publisher>Blackwell Science Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2000-01-21">2000-01-21</date></imprint><idno type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Bright galaxies</term><term>Cent level</term><term>Cfrs</term><term>Cfrs1ldss</term><term>Companion galaxy</term><term>Complete sample</term><term>Considerable uncertainties</term><term>Data points</term><term>Double nuclei</term><term>Dwarf galaxies</term><term>Elli</term><term>Enhancement</term><term>Equivalent width</term><term>Excellent agreement</term><term>Fevre</term><term>Galaxy</term><term>Galaxy formation</term><term>Galaxy images</term><term>Galaxy pairs</term><term>Galaxy population</term><term>Glazebrook</term><term>Hernquist</term><term>High redshifts</term><term>Higher redshifts</term><term>Imaging</term><term>Imaging data</term><term>Important role</term><term>Individual image</term><term>Ldss</term><term>Ldss redshift surveys</term><term>Local universe</term><term>Luminosity</term><term>Luminosity density</term><term>Luminosity enhancement</term><term>Luminosity evolution</term><term>Luminosity function</term><term>Magnitude difference</term><term>Major mergers</term><term>Manual classification</term><term>Merger</term><term>Merger class</term><term>Merger events</term><term>Merger fraction</term><term>Merger rate</term><term>Mihos</term><term>Mihos hernquist</term><term>Minor mergers</term><term>Mnras</term><term>Number density</term><term>Number evolution</term><term>Ongoing</term><term>Ongoing mergers</term><term>Pair counts</term><term>Pair fraction</term><term>Patton</term><term>Physical pair fraction</term><term>Physical pairs</term><term>Present paper</term><term>Primary galaxy</term><term>Projection effects</term><term>Redshift</term><term>Redshift survey</term><term>Simple coaddition</term><term>Star formation</term><term>Star formation activity</term><term>Star formation rate</term><term>Star formation rate increase</term><term>Survey galaxies</term><term>Total number</term><term>Upcoming</term><term>Upcoming mergers</term><term>Upper right corner</term><term>Visual approach</term><term>Visual classification</term><term>Visual classification scheme</term><term>Visual identification</term><term>Whole sample</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Bright galaxies</term><term>Cent level</term><term>Cfrs</term><term>Cfrs1ldss</term><term>Companion galaxy</term><term>Complete sample</term><term>Considerable uncertainties</term><term>Data points</term><term>Double nuclei</term><term>Dwarf galaxies</term><term>Elli</term><term>Enhancement</term><term>Equivalent width</term><term>Excellent agreement</term><term>Fevre</term><term>Galaxy</term><term>Galaxy formation</term><term>Galaxy images</term><term>Galaxy pairs</term><term>Galaxy population</term><term>Glazebrook</term><term>Hernquist</term><term>High redshifts</term><term>Higher redshifts</term><term>Imaging</term><term>Imaging data</term><term>Important role</term><term>Individual image</term><term>Ldss</term><term>Ldss redshift surveys</term><term>Local universe</term><term>Luminosity</term><term>Luminosity density</term><term>Luminosity enhancement</term><term>Luminosity evolution</term><term>Luminosity function</term><term>Magnitude difference</term><term>Major mergers</term><term>Manual classification</term><term>Merger</term><term>Merger class</term><term>Merger events</term><term>Merger fraction</term><term>Merger rate</term><term>Mihos</term><term>Mihos hernquist</term><term>Minor mergers</term><term>Mnras</term><term>Number density</term><term>Number evolution</term><term>Ongoing</term><term>Ongoing mergers</term><term>Pair counts</term><term>Pair fraction</term><term>Patton</term><term>Physical pair fraction</term><term>Physical pairs</term><term>Present paper</term><term>Primary galaxy</term><term>Projection effects</term><term>Redshift</term><term>Redshift survey</term><term>Simple coaddition</term><term>Star formation</term><term>Star formation activity</term><term>Star formation rate</term><term>Star formation rate increase</term><term>Survey galaxies</term><term>Total number</term><term>Upcoming</term><term>Upcoming mergers</term><term>Upper right corner</term><term>Visual approach</term><term>Visual classification</term><term>Visual classification scheme</term><term>Visual identification</term><term>Whole sample</term></keywords><keywords scheme="Wicri" type="topic" xml:lang="fr"><term>Fusion d'entreprises</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Hubble Space Telescope images of a sample of 285 galaxies with measured redshifts from the Canada–France Redshift Survey (CFRS) and Autofib–Low Dispersion Spectrograph Survey (LDSS) redshift surveys are analysed to derive the evolution of the merger fraction out to redshifts z∼1. We have performed visual and machine‐based merger identifications, as well as counts of bright pairs of galaxies with magnitude differences δm≤1.5 mag. We find that the pair fraction increases with redshift, with up to ∼20 per cent of the galaxies being in physical pairs at z∼0.75–1. We derive a merger fraction varying with redshift as ∝(1+z)3.2±0.6, after correction for line‐of‐sight contamination, in excellent agreement with the merger fraction derived from the visual classification of mergers for which m=3.4±0.6. After correcting for seeing effects on the ground‐based selection of survey galaxies, we conclude that the pair fraction evolves as ∝(1+z)2.7±0.6. This implies that an average L* galaxy will have undergone 0.8–1.8 merger events from z=1 to z=0, with 0.5 to 1.2 merger events occuring in a 2‐Gyr time‐span at around z∼0.9. This result is consistent with predictions from semi‐analytical models of galaxy formation. From the simple coaddition of the observed luminosities of the galaxies in pairs, physical mergers are computed to lead to a brightening of 0.5 mag for each pair on average, and a boost in star formation rate of a factor of 2, as derived from the average [O ii] equivalent widths. Mergers of galaxies are therefore contributing significantly to the evolution of both the luminosity function and luminosity density of the Universe out to z∼1.</div></front></TEI></record>Pour manipuler ce document sous Unix (Dilib)
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|texte= Hubble Space Telescope imaging of the CFRS and LDSS redshift surveys – IV. Influence of mergers in the evolution of faint field galaxies from z∼1
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