AustralieFrV1, PascalFrancis, Corpus, bibRecord, 001551

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

Identifieur interne : 001551 ( PascalFrancis/Corpus ); précédent : 001550; suivant : 001552

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

Auteurs : S. A. Farrell ; M. Servillat ; J. Pforr ; T. J. Maccarone ; C. Knigge ; O. Godet ; C. Maraston ; N. A. Webb ; D. Barret ; A. J. Gosling ; R. Belmont ; K. Wiersema

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.

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.

Notice en format standard (ISO 2709)

Pour connaître la documentation sur le format Inist Standard.

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A11	`01`	`1`		`@1 FARRELL (S. A.)`
A11	`02`	`1`		`@1 SERVILLAT (M.)`
A11	`03`	`1`		`@1 PFORR (J.)`
A11	`04`	`1`		`@1 MACCARONE (T. J.)`
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A11	`11`	`1`		`@1 BELMONT (R.)`
A11	`12`	`1`		`@1 WIERSEMA (K.)`
A14	`01`			`@1 Sydney Institute for Astronomy (SIfA), School of Physics, The University of Sydney @2 NSW 2006 @3 AUS @Z 1 aut.`
A14	`02`			`@1 Department of Physics and Astronomy, University of Leicester, University Road @2 LEI 7RH Leicester @3 GBR @Z 1 aut. @Z 12 aut.`
A14	`03`			`@1 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS-67 @2 Cambridge, MA 02138 @3 USA @Z 2 aut.`
A14	`04`			`@1 Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Burnaby Road @2 Portsmouth PO1 3FX @3 GBR @Z 3 aut. @Z 7 aut.`
A14	`05`			`@1 School of Physics and Astronomy, University of Southampton @2 Hampshire SO17 1BJ @3 GBR @Z 4 aut. @Z 5 aut.`
A14	`06`			`@1 Université de Toulouse, UPS-OMP, Institut de Recherche en Astrophysique et Planétologie (IRAP) @2 Toulouse @3 FRA @Z 6 aut. @Z 8 aut. @Z 9 aut. @Z 11 aut.`
A14	`07`			`@1 CNRS, IRAP, 9 Avenue du Colonel Roche, BP 44346 @2 31028 Toulouse @3 FRA @Z 6 aut. @Z 8 aut. @Z 9 aut. @Z 11 aut.`
A14	`08`			`@1 University of Oxford, Department of Physics, Keble Road @2 Oxford OX1 3RH @3 GBR @Z 10 aut.`
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A44				`@0 0000 @1 © 2012 INIST-CNRS. All rights reserved.`
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A60				`@1 P`
A61				`@0 A`
A64	`01`	`1`		`@0 The Astrophysical journal`
A66	`01`			`@0 GBR`
C01	`01`		`ENG`	@0 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.
C02	`01`	`3`		`@0 001E03`
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C03	`01`	`X`	`ENG`	`@0 Stellar population @5 26`
C03	`01`	`X`	`SPA`	`@0 Población estelar @5 26`
C03	`02`	`3`	`FRE`	`@0 Trou noir @5 27`
C03	`02`	`3`	`ENG`	`@0 Black holes @5 27`
C03	`03`	`X`	`FRE`	`@0 Observation RX @5 28`
C03	`03`	`X`	`ENG`	`@0 X ray observation @5 28`
C03	`03`	`X`	`SPA`	`@0 Observación RX @5 28`
C03	`04`	`X`	`FRE`	`@0 Densité spectrale énergie @5 29`
C03	`04`	`X`	`ENG`	`@0 Spectral energy distribution @5 29`
C03	`04`	`X`	`SPA`	`@0 Densidad espectral energía @5 29`
C03	`05`	`X`	`FRE`	`@0 Modèle @5 30`
C03	`05`	`X`	`ENG`	`@0 Models @5 30`
C03	`05`	`X`	`SPA`	`@0 Modelo @5 30`
C03	`06`	`3`	`FRE`	`@0 Disque accrétion @5 31`
C03	`06`	`3`	`ENG`	`@0 Accretion disks @5 31`
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C03	`07`	`X`	`ENG`	`@0 Age @5 32`
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C03	`08`	`X`	`ENG`	`@0 Dust lane @5 33`
C03	`08`	`X`	`SPA`	`@0 Pasillo polvo @5 33`
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C03	`11`	`3`	`ENG`	`@0 Galaxy clusters @5 36`
C03	`12`	`3`	`FRE`	`@0 Amas stellaire @5 37`
C03	`12`	`3`	`ENG`	`@0 Star clusters @5 37`
C03	`13`	`3`	`FRE`	`@0 Amas globulaire @5 38`
C03	`13`	`3`	`ENG`	`@0 Globular clusters @5 38`
C03	`14`	`3`	`FRE`	`@0 Binaire RX @5 39`
C03	`14`	`3`	`ENG`	`@0 X-ray binary stars @5 39`
C03	`15`	`X`	`FRE`	`@0 Source RX binaire @5 40`
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C03	`17`	`3`	`ENG`	`@0 Cosmic x-ray sources @5 42`
N21				`@1 093`
N44	`01`			`@1 OTO`
N82				`@1 OTO`

Format Inist (serveur)

NO :	PASCAL 12-0121112 INIST
ET :	A YOUNG MASSIVE STELLAR POPULATION AROUND THE INTERMEDIATE-MASS BLACK HOLE ESO 243-49 HLX-1
AU :	FARRELL (S. A.); SERVILLAT (M.); PFORR (J.); MACCARONE (T. J.); KNIGGE (C.); GODET (O.); MARASTON (C.); WEBB (N. A.); BARRET (D.); GOSLING (A. J.); BELMONT (R.); WIERSEMA (K.)
AF :	Sydney Institute for Astronomy (SIfA), School of Physics, The University of Sydney/NSW 2006/Australie (1 aut.); Department of Physics and Astronomy, University of Leicester, University Road/LEI 7RH Leicester/Royaume-Uni (1 aut., 12 aut.); Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS-67/Cambridge, MA 02138/Etats-Unis (2 aut.); Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Burnaby Road/Portsmouth PO1 3FX/Royaume-Uni (3 aut., 7 aut.); School of Physics and Astronomy, University of Southampton/Hampshire SO17 1BJ/Royaume-Uni (4 aut., 5 aut.); Université de Toulouse, UPS-OMP, Institut de Recherche en Astrophysique et Planétologie (IRAP)/Toulouse/France (6 aut., 8 aut., 9 aut., 11 aut.); CNRS, IRAP, 9 Avenue du Colonel Roche, BP 44346/31028 Toulouse/France (6 aut., 8 aut., 9 aut., 11 aut.); University of Oxford, Department of Physics, Keble Road/Oxford OX1 3RH/Royaume-Uni (10 aut.)
DT :	Publication en série; Niveau analytique
SO :	The Astrophysical journal; ISSN 0004-637X; Coden ASJOAB; Royaume-Uni; Da. 2012; Vol. 747; No. 1 p. 2; L13.1-L13.6; Bibl. 1/4 p.
LA :	Anglais
EA :	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.
CC :	001E03
FD :	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
ED :	Stellar population; Black holes; X ray observation; Spectral energy distribution; Models; Accretion disks; Age; Dust lane; Galaxies; Accretion; Galaxy clusters; Star clusters; Globular clusters; X-ray binary stars; Binary X ray source; Cosmology; Cosmic x-ray sources
SD :	Población estelar; Observación RX; Densidad espectral energía; Modelo; Edad; Pasillo polvo; Fuente RX binaria
LO :	INIST-512.354000502835310130
ID :	12-0121112

Links to Exploration step

Pascal:12-0121112

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>
<affiliation><inist:fA14 i1="01"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, The University of Sydney</s1>
<s2>NSW 2006</s2>
<s3>AUS</s3>
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<affiliation><inist:fA14 i1="02"><s1>Department of Physics and Astronomy, University of Leicester, University Road</s1>
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<author><name sortKey="Servillat, M" sort="Servillat, M" uniqKey="Servillat M" first="M." last="Servillat">M. Servillat</name>
<affiliation><inist:fA14 i1="03"><s1>Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS-67</s1>
<s2>Cambridge, MA 02138</s2>
<s3>USA</s3>
<sZ>2 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Pforr, J" sort="Pforr, J" uniqKey="Pforr J" first="J." last="Pforr">J. Pforr</name>
<affiliation><inist:fA14 i1="04"><s1>Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Burnaby Road</s1>
<s2>Portsmouth PO1 3FX</s2>
<s3>GBR</s3>
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</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Maccarone, T J" sort="Maccarone, T J" uniqKey="Maccarone T" first="T. J." last="Maccarone">T. J. Maccarone</name>
<affiliation><inist:fA14 i1="05"><s1>School of Physics and Astronomy, University of Southampton</s1>
<s2>Hampshire SO17 1BJ</s2>
<s3>GBR</s3>
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</author>
<author><name sortKey="Knigge, C" sort="Knigge, C" uniqKey="Knigge C" first="C." last="Knigge">C. Knigge</name>
<affiliation><inist:fA14 i1="05"><s1>School of Physics and Astronomy, University of Southampton</s1>
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<author><name sortKey="Godet, O" sort="Godet, O" uniqKey="Godet O" first="O." last="Godet">O. Godet</name>
<affiliation><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>
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<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>
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 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.</s0>
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<ET>A YOUNG MASSIVE STELLAR POPULATION AROUND THE INTERMEDIATE-MASS BLACK HOLE ESO 243-49 HLX-1</ET>
<AU>FARRELL (S. A.); SERVILLAT (M.); PFORR (J.); MACCARONE (T. J.); KNIGGE (C.); GODET (O.); MARASTON (C.); WEBB (N. A.); BARRET (D.); GOSLING (A. J.); BELMONT (R.); WIERSEMA (K.)</AU>
<AF>Sydney Institute for Astronomy (SIfA), School of Physics, The University of Sydney/NSW 2006/Australie (1 aut.); Department of Physics and Astronomy, University of Leicester, University Road/LEI 7RH Leicester/Royaume-Uni (1 aut., 12 aut.); Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS-67/Cambridge, MA 02138/Etats-Unis (2 aut.); Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Burnaby Road/Portsmouth PO1 3FX/Royaume-Uni (3 aut., 7 aut.); School of Physics and Astronomy, University of Southampton/Hampshire SO17 1BJ/Royaume-Uni (4 aut., 5 aut.); Université de Toulouse, UPS-OMP, Institut de Recherche en Astrophysique et Planétologie (IRAP)/Toulouse/France (6 aut., 8 aut., 9 aut., 11 aut.); CNRS, IRAP, 9 Avenue du Colonel Roche, BP 44346/31028 Toulouse/France (6 aut., 8 aut., 9 aut., 11 aut.); University of Oxford, Department of Physics, Keble Road/Oxford OX1 3RH/Royaume-Uni (10 aut.)</AF>
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<SO>The Astrophysical journal; ISSN 0004-637X; Coden ASJOAB; Royaume-Uni; Da. 2012; Vol. 747; No. 1 p. 2; L13.1-L13.6; Bibl. 1/4 p.</SO>
<LA>Anglais</LA>
<EA>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.</EA>
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<ED>Stellar population; Black holes; X ray observation; Spectral energy distribution; Models; Accretion disks; Age; Dust lane; Galaxies; Accretion; Galaxy clusters; Star clusters; Globular clusters; X-ray binary stars; Binary X ray source; Cosmology; Cosmic x-ray sources</ED>
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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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