AustralieFrV1, Main, Exploration, bibRecordById, Pascal:12-0121112

A YOUNG MASSIVE STELLAR POPULATION AROUND THE INTERMEDIATE-MASS BLACK HOLE ESO 243-49 HLX-1

Identifieur interne : 005F24 ( Main/Exploration ); précédent : 005F23; suivant : 005F25

A YOUNG MASSIVE STELLAR POPULATION AROUND THE INTERMEDIATE-MASS BLACK HOLE ESO 243-49 HLX-1

Auteurs : S. A. Farrell [Australie, Royaume-Uni] ; M. Servillat [États-Unis] ; J. Pforr [Royaume-Uni] ; T. J. Maccarone [Royaume-Uni] ; C. Knigge [Royaume-Uni] ; O. Godet [France] ; C. Maraston [Royaume-Uni] ; N. A. Webb [France] ; D. Barret [France] ; A. J. Gosling [Royaume-Uni] ; R. Belmont [France] ; K. Wiersema [Royaume-Uni]

Source :

The Astrophysical journal [ 0004-637X ] ; 2012.

RBID : Pascal:12-0121112

Descripteurs français

Pascal (Inist)
- Population stellaire, Trou noir, Observation RX, Densité spectrale énergie, Modèle, Disque accrétion, Age, Couloir poussière, Galaxies, Accrétion, Amas galaxies, Amas stellaire, Amas globulaire, Binaire RX, Source RX binaire, Cosmologie, Source RX cosmique.
Wicri :
- topic : Cosmologie.

English descriptors

KwdEn :
- Accretion, Accretion disks, Age, Binary X ray source, Black holes, Cosmic x-ray sources, Cosmology, Dust lane, Galaxies, Galaxy clusters, Globular clusters, Models, Spectral energy distribution, Star clusters, Stellar population, X ray observation, X-ray binary stars.

Abstract

We present Hubble Space Telescope and simultaneous Swift X-ray Telescope observations of the strongest candidate intermediate-mass black hole (IMBH) ESO 243-49 HLX-1. Fitting the spectral energy distribution from X-ray to near-infrared wavelengths showed that the broadband spectrum is not consistent with simple and irradiated disk models, but is well described by a model comprised of an irradiated accretion disk plus a ˜10⁶ M_◦. stellar population. The age of the population cannot be uniquely constrained, with both young and old stellar populations allowed. However, the old solution requires excessive disk reprocessing and an extremely small disk, so we favor the young solution (˜13 Myr). In addition, the presence of dust lanes and the lack of any nuclear activity from X-ray observations of the host galaxy suggest that a gas-rich minor merger may have taken place less than ˜200 Myr ago. Such a merger event would explain the presence of the IMBH and the young stellar population.

Affiliations:

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Le document en format XML

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<sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">A YOUNG MASSIVE STELLAR POPULATION AROUND THE INTERMEDIATE-MASS BLACK HOLE ESO 243-49 HLX-1</title>
<author><name sortKey="Farrell, S A" sort="Farrell, S A" uniqKey="Farrell S" first="S. A." last="Farrell">S. A. Farrell</name>
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<author><name sortKey="Gosling, A J" sort="Gosling, A J" uniqKey="Gosling A" first="A. J." last="Gosling">A. J. Gosling</name>
<affiliation wicri:level="4"><inist:fA14 i1="08"><s1>University of Oxford, Department of Physics, Keble Road</s1>
<s2>Oxford OX1 3RH</s2>
<s3>GBR</s3>
<sZ>10 aut.</sZ>
</inist:fA14>
<country>Royaume-Uni</country>
<wicri:noRegion>Oxford OX1 3RH</wicri:noRegion>
<orgName type="university">Université d'Oxford</orgName>
<placeName><settlement type="city">Oxford</settlement>
<region type="nation">Angleterre</region>
<region type="région" nuts="1">Oxfordshire</region>
</placeName>
</affiliation>
</author>
<author><name sortKey="Belmont, R" sort="Belmont, R" uniqKey="Belmont R" first="R." last="Belmont">R. Belmont</name>
<affiliation wicri:level="3"><inist:fA14 i1="06"><s1>Université de Toulouse, UPS-OMP, Institut de Recherche en Astrophysique et Planétologie (IRAP)</s1>
<s2>Toulouse</s2>
<s3>FRA</s3>
<sZ>6 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>9 aut.</sZ>
<sZ>11 aut.</sZ>
</inist:fA14>
<country>France</country>
<placeName><region type="region">Occitanie (région administrative)</region>
<region type="old region">Midi-Pyrénées</region>
<settlement type="city">Toulouse</settlement>
</placeName>
</affiliation>
<affiliation wicri:level="1"><inist:fA14 i1="07"><s1>CNRS, IRAP, 9 Avenue du Colonel Roche, BP 44346</s1>
<s2>31028 Toulouse</s2>
<s3>FRA</s3>
<sZ>6 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>9 aut.</sZ>
<sZ>11 aut.</sZ>
</inist:fA14>
<country>France</country>
<wicri:noRegion>31028 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="Wiersema, K" sort="Wiersema, K" uniqKey="Wiersema K" first="K." last="Wiersema">K. Wiersema</name>
<affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Department of Physics and Astronomy, University of Leicester, University Road</s1>
<s2>LEI 7RH Leicester</s2>
<s3>GBR</s3>
<sZ>1 aut.</sZ>
<sZ>12 aut.</sZ>
</inist:fA14>
<country>Royaume-Uni</country>
<wicri:noRegion>LEI 7RH Leicester</wicri:noRegion>
</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="2012">2012</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>Accretion</term>
<term>Accretion disks</term>
<term>Age</term>
<term>Binary X ray source</term>
<term>Black holes</term>
<term>Cosmic x-ray sources</term>
<term>Cosmology</term>
<term>Dust lane</term>
<term>Galaxies</term>
<term>Galaxy clusters</term>
<term>Globular clusters</term>
<term>Models</term>
<term>Spectral energy distribution</term>
<term>Star clusters</term>
<term>Stellar population</term>
<term>X ray observation</term>
<term>X-ray binary stars</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Population stellaire</term>
<term>Trou noir</term>
<term>Observation RX</term>
<term>Densité spectrale énergie</term>
<term>Modèle</term>
<term>Disque accrétion</term>
<term>Age</term>
<term>Couloir poussière</term>
<term>Galaxies</term>
<term>Accrétion</term>
<term>Amas galaxies</term>
<term>Amas stellaire</term>
<term>Amas globulaire</term>
<term>Binaire RX</term>
<term>Source RX binaire</term>
<term>Cosmologie</term>
<term>Source RX cosmique</term>
</keywords>
<keywords scheme="Wicri" type="topic" xml:lang="fr"><term>Cosmologie</term>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<front><div type="abstract" xml:lang="en">We present Hubble Space Telescope and simultaneous Swift X-ray Telescope observations of the strongest candidate intermediate-mass black hole (IMBH) ESO 243-49 HLX-1. Fitting the spectral energy distribution from X-ray to near-infrared wavelengths showed that the broadband spectrum is not consistent with simple and irradiated disk models, but is well described by a model comprised of an irradiated accretion disk plus a ˜10<sup>6</sup>
 M<sub>◦.</sub>
 stellar population. The age of the population cannot be uniquely constrained, with both young and old stellar populations allowed. However, the old solution requires excessive disk reprocessing and an extremely small disk, so we favor the young solution (˜13 Myr). In addition, the presence of dust lanes and the lack of any nuclear activity from X-ray observations of the host galaxy suggest that a gas-rich minor merger may have taken place less than ˜200 Myr ago. Such a merger event would explain the presence of the IMBH and the young stellar population.</div>
</front>
</TEI>
<affiliations><list><country><li>Australie</li>
<li>France</li>
<li>Royaume-Uni</li>
<li>États-Unis</li>
</country>
<region><li>Angleterre</li>
<li>Midi-Pyrénées</li>
<li>Nouvelle-Galles du Sud</li>
<li>Occitanie (région administrative)</li>
<li>Oxfordshire</li>
</region>
<settlement><li>Oxford</li>
<li>Sydney</li>
<li>Toulouse</li>
</settlement>
<orgName><li>Université d'Oxford</li>
<li>Université de Sydney</li>
</orgName>
</list>
<tree><country name="Australie"><region name="Nouvelle-Galles du Sud"><name sortKey="Farrell, S A" sort="Farrell, S A" uniqKey="Farrell S" first="S. A." last="Farrell">S. A. Farrell</name>
</region>
</country>
<country name="Royaume-Uni"><noRegion><name sortKey="Farrell, S A" sort="Farrell, S A" uniqKey="Farrell S" first="S. A." last="Farrell">S. A. Farrell</name>
</noRegion>
<name sortKey="Gosling, A J" sort="Gosling, A J" uniqKey="Gosling A" first="A. J." last="Gosling">A. J. Gosling</name>
<name sortKey="Knigge, C" sort="Knigge, C" uniqKey="Knigge C" first="C." last="Knigge">C. Knigge</name>
<name sortKey="Maccarone, T J" sort="Maccarone, T J" uniqKey="Maccarone T" first="T. J." last="Maccarone">T. J. Maccarone</name>
<name sortKey="Maraston, C" sort="Maraston, C" uniqKey="Maraston C" first="C." last="Maraston">C. Maraston</name>
<name sortKey="Pforr, J" sort="Pforr, J" uniqKey="Pforr J" first="J." last="Pforr">J. Pforr</name>
<name sortKey="Wiersema, K" sort="Wiersema, K" uniqKey="Wiersema K" first="K." last="Wiersema">K. Wiersema</name>
</country>
<country name="États-Unis"><noRegion><name sortKey="Servillat, M" sort="Servillat, M" uniqKey="Servillat M" first="M." last="Servillat">M. Servillat</name>
</noRegion>
</country>
<country name="France"><region name="Occitanie (région administrative)"><name sortKey="Godet, O" sort="Godet, O" uniqKey="Godet O" first="O." last="Godet">O. Godet</name>
</region>
<name sortKey="Barret, D" sort="Barret, D" uniqKey="Barret D" first="D." last="Barret">D. Barret</name>
<name sortKey="Barret, D" sort="Barret, D" uniqKey="Barret D" first="D." last="Barret">D. Barret</name>
<name sortKey="Belmont, R" sort="Belmont, R" uniqKey="Belmont R" first="R." last="Belmont">R. Belmont</name>
<name sortKey="Belmont, R" sort="Belmont, R" uniqKey="Belmont R" first="R." last="Belmont">R. Belmont</name>
<name sortKey="Godet, O" sort="Godet, O" uniqKey="Godet O" first="O." last="Godet">O. Godet</name>
<name sortKey="Webb, N A" sort="Webb, N A" uniqKey="Webb N" first="N. A." last="Webb">N. A. Webb</name>
<name sortKey="Webb, N A" sort="Webb, N A" uniqKey="Webb N" first="N. A." last="Webb">N. A. Webb</name>
</country>
</tree>
</affiliations>
</record>

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A YOUNG MASSIVE STELLAR POPULATION AROUND THE INTERMEDIATE-MASS BLACK HOLE ESO 243-49 HLX-1

A YOUNG MASSIVE STELLAR POPULATION AROUND THE INTERMEDIATE-MASS BLACK HOLE ESO 243-49 HLX-1

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