A late jet rebrightening revealed from multiwavelength monitoring of the black hole candidate XTE J1752-223
Identifieur interne : 001679 ( PascalFrancis/Corpus ); précédent : 001678; suivant : 001680A late jet rebrightening revealed from multiwavelength monitoring of the black hole candidate XTE J1752-223
Auteurs : D. M. Russell ; P. A. Curran ; T. Munoz-Darias ; F. Lewis ; S. Motta ; H. Stiele ; T. Belloni ; J. C. A. Miller-Jones ; P. G. Jonker ; K. O'Brien ; J. Homan ; P. Casella ; P. Gandhi ; P. Soleri ; S. Markoff ; D. Maitra ; E. Gallo ; M. Cadolle BelSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2012.
Descripteurs français
- Pascal (Inist)
- Jet, Trou noir, Quiescence, Courbe lumière, Emission optique, Sursaut optique, Densité spectrale énergie, Morphologie, Photométrie IR, Polarimétrie, Borne supérieure, Polarisation rectiligne, Indice spectral, Déplacement fréquence, Accrétion, Disque accrétion, Binaire RX, Source RX binaire, Cosmologie, Source RX cosmique.
English descriptors
- KwdEn :
- Accretion, Accretion disks, Binary X ray source, Black holes, Cosmic x-ray sources, Cosmology, Frequency shift, Infrared photometry, Jets, Light curves, Light emission, Linear polarization, Morphology, Optical burst, Polarimetry, Quiescence, Spectral energy distribution, Spectral index, Upper bound, X-ray binary stars.
Abstract
We present optical monitoring of the black hole candidate XTE J1752-223 during its 2009-10 outburst and decay to quiescence. The optical light curve can be described by an exponential decay followed by a plateau, then a more rapid fade towards quiescence. The plateau appears to be due to an extra component of optical emission that brightens and then fades over ∼40 days. We show evidence for the origin of this optical 'flare' to be the synchrotron jet during the decaying hard state, and we identify and isolate both disc and jet components in the spectral energy distributions. The optical flare has the same morphology and amplitude as a contemporaneous X-ray rebrightening. This suggests a common origin, but no firm conclusions can be made favouring or disfavouring the jet producing the X-ray flare. The quiescent optical magnitudes are B ≥ 20.6, V ≥ 21.1, R ≥ 19.5, i' ≥ 19.2. From the optical outburst amplitude we estimate a likely orbital period of <22 h. We also present near-infrared (NIR) photometry and polarimetry and rare mid-IR imaging (8-12 μm) when the source is nearing quiescence. The fading jet component, and possibly the companion star, may contribute to the NIR flux. We derive deep mid-IR flux upper limits and NIR linear polarization upper limits. With the inclusion of radio data, we measure an almost flat jet spectral index between radio and optical; Fν ν∼+0.05. The data favour the jet break to optically thin emission to reside in the IR, but may shift to frequencies as high as the optical or UV during the peak of the flare.
Notice en format standard (ISO 2709)
Pour connaître la documentation sur le format Inist Standard.
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Format Inist (serveur)
NO : | PASCAL 12-0042281 INIST |
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ET : | A late jet rebrightening revealed from multiwavelength monitoring of the black hole candidate XTE J1752-223 |
AU : | RUSSELL (D. M.); CURRAN (P. A.); MUNOZ-DARIAS (T.); LEWIS (F.); MOTTA (S.); STIELE (H.); BELLONI (T.); MILLER-JONES (J. C. A.); JONKER (P. G.); O'BRIEN (K.); HOMAN (J.); CASELLA (P.); GANDHI (P.); SOLERI (P.); MARKOFF (S.); MAITRA (D.); GALLO (E.); CADOLLE BEL (M.) |
AF : | Astronomical Institute 'Anton Pannekoek', University of Amsterdam, PO Box 94249/1090 GE Amsterdam/Pays-Bas (1 aut., 15 aut.); Laboratoire AIM, CEA/IRFU-Université Paris Diderot-CNRS/INSU, CEA DSM/IRFU/SAp, Centre de Saclay/91191 Gif-sur-Yvette/France (2 aut.); INAF-Osservatorio Astronomico di Brera, Via E. Bianchi 46/23807 Merate (LC/Italie (3 aut., 5 aut., 6 aut., 7 aut.); Faulkes Telescope Project, University of Glamorgan/Pontypridd CF37 1DL/Royaume-Uni (4 aut.); Department of Physics and Astronomy, The Open Universiy, Walton Hall/Milton Keynes MK7 6AA/Royaume-Uni (4 aut.); International Centre for Radio Astronomy Research, Curtin University, GPO Box U1987/Perth, WA 6845/Australie (8 aut.); SRON, Netherlands Institute for Space Research, Sorbonnelaan 2/3584 CA, Utrecht/Pays-Bas (9 aut.); Harvard-Smithsonian Center for Astrophysics, 60 Garden Street/Cambridge, MA 02138/Etats-Unis (9 aut.); Department of Astraphysics, IMAPP, Radboud University Nijmegen, PO Box 9010/6500 GL Nijmegen/Pays-Bas (9 aut.); Department of Physics, University of California/Santa Barbara, CA 93106-9530/Etats-Unis (10 aut.); MIT Kavli Institute for Astrophysics and Space Research, 70 Vassar Street/Cambridge, MA 02139/Etats-Unis (11 aut.); School of Physics and Astronomy, University of Southampton/Southampton, Hampshire SO17 IBJ/Royaume-Uni (12 aut.); ISAS, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, chuo-ku/Sngamihara, Kanagawa 229-8510/Japon (13 aut.); Kapteyn Astronomical Institute, University of Groningen, PO Box 800/9700 AV Groningen/Pays-Bas (14 aut.); Department of Astronomy, University of Michigan, 500 Church Street/Ann Arbor, MI 48109/Etats-Unis (16 aut., 17 aut.); ESAC, ISOC, Villanueva de la Canada, Madrid P. O. Box 78/28691/Espagne (18 aut.) |
DT : | Publication en série; Niveau analytique |
SO : | Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Etats-Unis; Da. 2012; Vol. 419; No. 2; Pp. 1740-1751; Bibl. 1 p.1/4 |
LA : | Anglais |
EA : | We present optical monitoring of the black hole candidate XTE J1752-223 during its 2009-10 outburst and decay to quiescence. The optical light curve can be described by an exponential decay followed by a plateau, then a more rapid fade towards quiescence. The plateau appears to be due to an extra component of optical emission that brightens and then fades over ∼40 days. We show evidence for the origin of this optical 'flare' to be the synchrotron jet during the decaying hard state, and we identify and isolate both disc and jet components in the spectral energy distributions. The optical flare has the same morphology and amplitude as a contemporaneous X-ray rebrightening. This suggests a common origin, but no firm conclusions can be made favouring or disfavouring the jet producing the X-ray flare. The quiescent optical magnitudes are B ≥ 20.6, V ≥ 21.1, R ≥ 19.5, i' ≥ 19.2. From the optical outburst amplitude we estimate a likely orbital period of <22 h. We also present near-infrared (NIR) photometry and polarimetry and rare mid-IR imaging (8-12 μm) when the source is nearing quiescence. The fading jet component, and possibly the companion star, may contribute to the NIR flux. We derive deep mid-IR flux upper limits and NIR linear polarization upper limits. With the inclusion of radio data, we measure an almost flat jet spectral index between radio and optical; Fν <is proportional to> ν∼+0.05. The data favour the jet break to optically thin emission to reside in the IR, but may shift to frequencies as high as the optical or UV during the peak of the flare. |
CC : | 001E03 |
FD : | Jet; Trou noir; Quiescence; Courbe lumière; Emission optique; Sursaut optique; Densité spectrale énergie; Morphologie; Photométrie IR; Polarimétrie; Borne supérieure; Polarisation rectiligne; Indice spectral; Déplacement fréquence; Accrétion; Disque accrétion; Binaire RX; Source RX binaire; Cosmologie; Source RX cosmique |
ED : | Jets; Black holes; Quiescence; Light curves; Light emission; Optical burst; Spectral energy distribution; Morphology; Infrared photometry; Polarimetry; Upper bound; Linear polarization; Spectral index; Frequency shift; Accretion; Accretion disks; X-ray binary stars; Binary X ray source; Cosmology; Cosmic x-ray sources |
SD : | Quietud; Emisión óptica; Arrebato óptico; Densidad espectral energía; Fotometría IR; Cota superior; Desplazamiento frecuencia; Fuente RX binaria |
LO : | INIST-2067.354000506050220740 |
ID : | 12-0042281 |
Links to Exploration step
Pascal:12-0042281Le document en format XML
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<sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">A late jet rebrightening revealed from multiwavelength monitoring of the black hole candidate XTE J1752-223</title>
<author><name sortKey="Russell, D M" sort="Russell, D M" uniqKey="Russell D" first="D. M." last="Russell">D. M. Russell</name>
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<author><name sortKey="Curran, P A" sort="Curran, P A" uniqKey="Curran P" first="P. A." last="Curran">P. A. Curran</name>
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<author><name sortKey="Munoz Darias, T" sort="Munoz Darias, T" uniqKey="Munoz Darias T" first="T." last="Munoz-Darias">T. Munoz-Darias</name>
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<author><name sortKey="Lewis, F" sort="Lewis, F" uniqKey="Lewis F" first="F." last="Lewis">F. Lewis</name>
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<author><name sortKey="Stiele, H" sort="Stiele, H" uniqKey="Stiele H" first="H." last="Stiele">H. Stiele</name>
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<author><name sortKey="Belloni, T" sort="Belloni, T" uniqKey="Belloni T" first="T." last="Belloni">T. Belloni</name>
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<author><name sortKey="Miller Jones, J C A" sort="Miller Jones, J C A" uniqKey="Miller Jones J" first="J. C. A." last="Miller-Jones">J. C. A. Miller-Jones</name>
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<author><name sortKey="Jonker, P G" sort="Jonker, P G" uniqKey="Jonker P" first="P. G." last="Jonker">P. G. Jonker</name>
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<affiliation><inist:fA14 i1="08"><s1>Harvard-Smithsonian Center for Astrophysics, 60 Garden Street</s1>
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<affiliation><inist:fA14 i1="09"><s1>Department of Astraphysics, IMAPP, Radboud University Nijmegen, PO Box 9010</s1>
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<affiliation><inist:fA14 i1="10"><s1>Department of Physics, University of California</s1>
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<author><name sortKey="Homan, J" sort="Homan, J" uniqKey="Homan J" first="J." last="Homan">J. Homan</name>
<affiliation><inist:fA14 i1="11"><s1>MIT Kavli Institute for Astrophysics and Space Research, 70 Vassar Street</s1>
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<author><name sortKey="Casella, P" sort="Casella, P" uniqKey="Casella P" first="P." last="Casella">P. Casella</name>
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<author><name sortKey="Gandhi, P" sort="Gandhi, P" uniqKey="Gandhi P" first="P." last="Gandhi">P. Gandhi</name>
<affiliation><inist:fA14 i1="13"><s1>ISAS, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, chuo-ku</s1>
<s2>Sngamihara, Kanagawa 229-8510</s2>
<s3>JPN</s3>
<sZ>13 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Soleri, P" sort="Soleri, P" uniqKey="Soleri P" first="P." last="Soleri">P. Soleri</name>
<affiliation><inist:fA14 i1="14"><s1>Kapteyn Astronomical Institute, University of Groningen, PO Box 800</s1>
<s2>9700 AV Groningen</s2>
<s3>NLD</s3>
<sZ>14 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Markoff, S" sort="Markoff, S" uniqKey="Markoff S" first="S." last="Markoff">S. Markoff</name>
<affiliation><inist:fA14 i1="01"><s1>Astronomical Institute 'Anton Pannekoek', University of Amsterdam, PO Box 94249</s1>
<s2>1090 GE Amsterdam</s2>
<s3>NLD</s3>
<sZ>1 aut.</sZ>
<sZ>15 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Maitra, D" sort="Maitra, D" uniqKey="Maitra D" first="D." last="Maitra">D. Maitra</name>
<affiliation><inist:fA14 i1="15"><s1>Department of Astronomy, University of Michigan, 500 Church Street</s1>
<s2>Ann Arbor, MI 48109</s2>
<s3>USA</s3>
<sZ>16 aut.</sZ>
<sZ>17 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Gallo, E" sort="Gallo, E" uniqKey="Gallo E" first="E." last="Gallo">E. Gallo</name>
<affiliation><inist:fA14 i1="15"><s1>Department of Astronomy, University of Michigan, 500 Church Street</s1>
<s2>Ann Arbor, MI 48109</s2>
<s3>USA</s3>
<sZ>16 aut.</sZ>
<sZ>17 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Cadolle Bel, M" sort="Cadolle Bel, M" uniqKey="Cadolle Bel M" first="M." last="Cadolle Bel">M. Cadolle Bel</name>
<affiliation><inist:fA14 i1="16"><s1>ESAC, ISOC, Villanueva de la Canada, Madrid P. O. Box 78</s1>
<s2>28691</s2>
<s3>ESP</s3>
<sZ>18 aut.</sZ>
</inist:fA14>
</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>Accretion</term>
<term>Accretion disks</term>
<term>Binary X ray source</term>
<term>Black holes</term>
<term>Cosmic x-ray sources</term>
<term>Cosmology</term>
<term>Frequency shift</term>
<term>Infrared photometry</term>
<term>Jets</term>
<term>Light curves</term>
<term>Light emission</term>
<term>Linear polarization</term>
<term>Morphology</term>
<term>Optical burst</term>
<term>Polarimetry</term>
<term>Quiescence</term>
<term>Spectral energy distribution</term>
<term>Spectral index</term>
<term>Upper bound</term>
<term>X-ray binary stars</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Jet</term>
<term>Trou noir</term>
<term>Quiescence</term>
<term>Courbe lumière</term>
<term>Emission optique</term>
<term>Sursaut optique</term>
<term>Densité spectrale énergie</term>
<term>Morphologie</term>
<term>Photométrie IR</term>
<term>Polarimétrie</term>
<term>Borne supérieure</term>
<term>Polarisation rectiligne</term>
<term>Indice spectral</term>
<term>Déplacement fréquence</term>
<term>Accrétion</term>
<term>Disque accrétion</term>
<term>Binaire RX</term>
<term>Source RX binaire</term>
<term>Cosmologie</term>
<term>Source RX cosmique</term>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<front><div type="abstract" xml:lang="en">We present optical monitoring of the black hole candidate XTE J1752-223 during its 2009-10 outburst and decay to quiescence. The optical light curve can be described by an exponential decay followed by a plateau, then a more rapid fade towards quiescence. The plateau appears to be due to an extra component of optical emission that brightens and then fades over ∼40 days. We show evidence for the origin of this optical 'flare' to be the synchrotron jet during the decaying hard state, and we identify and isolate both disc and jet components in the spectral energy distributions. The optical flare has the same morphology and amplitude as a contemporaneous X-ray rebrightening. This suggests a common origin, but no firm conclusions can be made favouring or disfavouring the jet producing the X-ray flare. The quiescent optical magnitudes are B ≥ 20.6, V ≥ 21.1, R ≥ 19.5, i' ≥ 19.2. From the optical outburst amplitude we estimate a likely orbital period of <22 h. We also present near-infrared (NIR) photometry and polarimetry and rare mid-IR imaging (8-12 μm) when the source is nearing quiescence. The fading jet component, and possibly the companion star, may contribute to the NIR flux. We derive deep mid-IR flux upper limits and NIR linear polarization upper limits. With the inclusion of radio data, we measure an almost flat jet spectral index between radio and optical; F<sub>ν</sub>
ν<sup>∼+0.05</sup>
. The data favour the jet break to optically thin emission to reside in the IR, but may shift to frequencies as high as the optical or UV during the peak of the flare.</div>
</front>
</TEI>
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<fA05><s2>419</s2>
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<fA06><s2>2</s2>
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<fA08 i1="01" i2="1" l="ENG"><s1>A late jet rebrightening revealed from multiwavelength monitoring of the black hole candidate XTE J1752-223</s1>
</fA08>
<fA11 i1="01" i2="1"><s1>RUSSELL (D. M.)</s1>
</fA11>
<fA11 i1="02" i2="1"><s1>CURRAN (P. A.)</s1>
</fA11>
<fA11 i1="03" i2="1"><s1>MUNOZ-DARIAS (T.)</s1>
</fA11>
<fA11 i1="04" i2="1"><s1>LEWIS (F.)</s1>
</fA11>
<fA11 i1="05" i2="1"><s1>MOTTA (S.)</s1>
</fA11>
<fA11 i1="06" i2="1"><s1>STIELE (H.)</s1>
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<fA11 i1="07" i2="1"><s1>BELLONI (T.)</s1>
</fA11>
<fA11 i1="08" i2="1"><s1>MILLER-JONES (J. C. A.)</s1>
</fA11>
<fA11 i1="09" i2="1"><s1>JONKER (P. G.)</s1>
</fA11>
<fA11 i1="10" i2="1"><s1>O'BRIEN (K.)</s1>
</fA11>
<fA11 i1="11" i2="1"><s1>HOMAN (J.)</s1>
</fA11>
<fA11 i1="12" i2="1"><s1>CASELLA (P.)</s1>
</fA11>
<fA11 i1="13" i2="1"><s1>GANDHI (P.)</s1>
</fA11>
<fA11 i1="14" i2="1"><s1>SOLERI (P.)</s1>
</fA11>
<fA11 i1="15" i2="1"><s1>MARKOFF (S.)</s1>
</fA11>
<fA11 i1="16" i2="1"><s1>MAITRA (D.)</s1>
</fA11>
<fA11 i1="17" i2="1"><s1>GALLO (E.)</s1>
</fA11>
<fA11 i1="18" i2="1"><s1>CADOLLE BEL (M.)</s1>
</fA11>
<fA14 i1="01"><s1>Astronomical Institute 'Anton Pannekoek', University of Amsterdam, PO Box 94249</s1>
<s2>1090 GE Amsterdam</s2>
<s3>NLD</s3>
<sZ>1 aut.</sZ>
<sZ>15 aut.</sZ>
</fA14>
<fA14 i1="02"><s1>Laboratoire AIM, CEA/IRFU-Université Paris Diderot-CNRS/INSU, CEA DSM/IRFU/SAp, Centre de Saclay</s1>
<s2>91191 Gif-sur-Yvette</s2>
<s3>FRA</s3>
<sZ>2 aut.</sZ>
</fA14>
<fA14 i1="03"><s1>INAF-Osservatorio Astronomico di Brera, Via E. Bianchi 46</s1>
<s2>23807 Merate (LC</s2>
<s3>ITA</s3>
<sZ>3 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>7 aut.</sZ>
</fA14>
<fA14 i1="04"><s1>Faulkes Telescope Project, University of Glamorgan</s1>
<s2>Pontypridd CF37 1DL</s2>
<s3>GBR</s3>
<sZ>4 aut.</sZ>
</fA14>
<fA14 i1="05"><s1>Department of Physics and Astronomy, The Open Universiy, Walton Hall</s1>
<s2>Milton Keynes MK7 6AA</s2>
<s3>GBR</s3>
<sZ>4 aut.</sZ>
</fA14>
<fA14 i1="06"><s1>International Centre for Radio Astronomy Research, Curtin University, GPO Box U1987</s1>
<s2>Perth, WA 6845</s2>
<s3>AUS</s3>
<sZ>8 aut.</sZ>
</fA14>
<fA14 i1="07"><s1>SRON, Netherlands Institute for Space Research, Sorbonnelaan 2</s1>
<s2>3584 CA, Utrecht</s2>
<s3>NLD</s3>
<sZ>9 aut.</sZ>
</fA14>
<fA14 i1="08"><s1>Harvard-Smithsonian Center for Astrophysics, 60 Garden Street</s1>
<s2>Cambridge, MA 02138</s2>
<s3>USA</s3>
<sZ>9 aut.</sZ>
</fA14>
<fA14 i1="09"><s1>Department of Astraphysics, IMAPP, Radboud University Nijmegen, PO Box 9010</s1>
<s2>6500 GL Nijmegen</s2>
<s3>NLD</s3>
<sZ>9 aut.</sZ>
</fA14>
<fA14 i1="10"><s1>Department of Physics, University of California</s1>
<s2>Santa Barbara, CA 93106-9530</s2>
<s3>USA</s3>
<sZ>10 aut.</sZ>
</fA14>
<fA14 i1="11"><s1>MIT Kavli Institute for Astrophysics and Space Research, 70 Vassar Street</s1>
<s2>Cambridge, MA 02139</s2>
<s3>USA</s3>
<sZ>11 aut.</sZ>
</fA14>
<fA14 i1="12"><s1>School of Physics and Astronomy, University of Southampton</s1>
<s2>Southampton, Hampshire SO17 IBJ</s2>
<s3>GBR</s3>
<sZ>12 aut.</sZ>
</fA14>
<fA14 i1="13"><s1>ISAS, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, chuo-ku</s1>
<s2>Sngamihara, Kanagawa 229-8510</s2>
<s3>JPN</s3>
<sZ>13 aut.</sZ>
</fA14>
<fA14 i1="14"><s1>Kapteyn Astronomical Institute, University of Groningen, PO Box 800</s1>
<s2>9700 AV Groningen</s2>
<s3>NLD</s3>
<sZ>14 aut.</sZ>
</fA14>
<fA14 i1="15"><s1>Department of Astronomy, University of Michigan, 500 Church Street</s1>
<s2>Ann Arbor, MI 48109</s2>
<s3>USA</s3>
<sZ>16 aut.</sZ>
<sZ>17 aut.</sZ>
</fA14>
<fA14 i1="16"><s1>ESAC, ISOC, Villanueva de la Canada, Madrid P. O. Box 78</s1>
<s2>28691</s2>
<s3>ESP</s3>
<sZ>18 aut.</sZ>
</fA14>
<fA20><s1>1740-1751</s1>
</fA20>
<fA21><s1>2012</s1>
</fA21>
<fA23 i1="01"><s0>ENG</s0>
</fA23>
<fA43 i1="01"><s1>INIST</s1>
<s2>2067</s2>
<s5>354000506050220740</s5>
</fA43>
<fA44><s0>0000</s0>
<s1>© 2012 INIST-CNRS. All rights reserved.</s1>
</fA44>
<fA45><s0>1 p.1/4</s0>
</fA45>
<fA47 i1="01" i2="1"><s0>12-0042281</s0>
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<fA60><s1>P</s1>
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<fA61><s0>A</s0>
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<fA64 i1="01" i2="1"><s0>Monthly Notices of the Royal Astronomical Society</s0>
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<fA66 i1="01"><s0>USA</s0>
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<fC01 i1="01" l="ENG"><s0>We present optical monitoring of the black hole candidate XTE J1752-223 during its 2009-10 outburst and decay to quiescence. The optical light curve can be described by an exponential decay followed by a plateau, then a more rapid fade towards quiescence. The plateau appears to be due to an extra component of optical emission that brightens and then fades over ∼40 days. We show evidence for the origin of this optical 'flare' to be the synchrotron jet during the decaying hard state, and we identify and isolate both disc and jet components in the spectral energy distributions. The optical flare has the same morphology and amplitude as a contemporaneous X-ray rebrightening. This suggests a common origin, but no firm conclusions can be made favouring or disfavouring the jet producing the X-ray flare. The quiescent optical magnitudes are B ≥ 20.6, V ≥ 21.1, R ≥ 19.5, i' ≥ 19.2. From the optical outburst amplitude we estimate a likely orbital period of <22 h. We also present near-infrared (NIR) photometry and polarimetry and rare mid-IR imaging (8-12 μm) when the source is nearing quiescence. The fading jet component, and possibly the companion star, may contribute to the NIR flux. We derive deep mid-IR flux upper limits and NIR linear polarization upper limits. With the inclusion of radio data, we measure an almost flat jet spectral index between radio and optical; F<sub>ν</sub>
ν<sup>∼+0.05</sup>
. The data favour the jet break to optically thin emission to reside in the IR, but may shift to frequencies as high as the optical or UV during the peak of the flare.</s0>
</fC01>
<fC02 i1="01" i2="3"><s0>001E03</s0>
</fC02>
<fC03 i1="01" i2="3" l="FRE"><s0>Jet</s0>
<s5>26</s5>
</fC03>
<fC03 i1="01" i2="3" l="ENG"><s0>Jets</s0>
<s5>26</s5>
</fC03>
<fC03 i1="02" i2="3" l="FRE"><s0>Trou noir</s0>
<s5>27</s5>
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<fC03 i1="02" i2="3" l="ENG"><s0>Black holes</s0>
<s5>27</s5>
</fC03>
<fC03 i1="03" i2="X" l="FRE"><s0>Quiescence</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="X" l="ENG"><s0>Quiescence</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="X" l="SPA"><s0>Quietud</s0>
<s5>28</s5>
</fC03>
<fC03 i1="04" i2="3" l="FRE"><s0>Courbe lumière</s0>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="3" l="ENG"><s0>Light curves</s0>
<s5>29</s5>
</fC03>
<fC03 i1="05" i2="X" l="FRE"><s0>Emission optique</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="X" l="ENG"><s0>Light emission</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="X" l="SPA"><s0>Emisión óptica</s0>
<s5>30</s5>
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<fC03 i1="06" i2="X" l="FRE"><s0>Sursaut optique</s0>
<s5>31</s5>
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<fC03 i1="06" i2="X" l="ENG"><s0>Optical burst</s0>
<s5>31</s5>
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<fC03 i1="06" i2="X" l="SPA"><s0>Arrebato óptico</s0>
<s5>31</s5>
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<fC03 i1="07" i2="X" l="FRE"><s0>Densité spectrale énergie</s0>
<s5>32</s5>
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<fC03 i1="07" i2="X" l="ENG"><s0>Spectral energy distribution</s0>
<s5>32</s5>
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<fC03 i1="07" i2="X" l="SPA"><s0>Densidad espectral energía</s0>
<s5>32</s5>
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<fC03 i1="08" i2="3" l="FRE"><s0>Morphologie</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="3" l="ENG"><s0>Morphology</s0>
<s5>33</s5>
</fC03>
<fC03 i1="09" i2="X" l="FRE"><s0>Photométrie IR</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="X" l="ENG"><s0>Infrared photometry</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="X" l="SPA"><s0>Fotometría IR</s0>
<s5>34</s5>
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<fC03 i1="10" i2="3" l="FRE"><s0>Polarimétrie</s0>
<s5>35</s5>
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<fC03 i1="10" i2="3" l="ENG"><s0>Polarimetry</s0>
<s5>35</s5>
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<fC03 i1="11" i2="X" l="FRE"><s0>Borne supérieure</s0>
<s5>36</s5>
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<fC03 i1="11" i2="X" l="ENG"><s0>Upper bound</s0>
<s5>36</s5>
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<fC03 i1="11" i2="X" l="SPA"><s0>Cota superior</s0>
<s5>36</s5>
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<fC03 i1="12" i2="3" l="FRE"><s0>Polarisation rectiligne</s0>
<s5>37</s5>
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<s5>37</s5>
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<fC03 i1="13" i2="3" l="FRE"><s0>Indice spectral</s0>
<s5>38</s5>
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<fC03 i1="13" i2="3" l="ENG"><s0>Spectral index</s0>
<s5>38</s5>
</fC03>
<fC03 i1="14" i2="X" l="FRE"><s0>Déplacement fréquence</s0>
<s5>39</s5>
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<fC03 i1="14" i2="X" l="ENG"><s0>Frequency shift</s0>
<s5>39</s5>
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<fC03 i1="14" i2="X" l="SPA"><s0>Desplazamiento frecuencia</s0>
<s5>39</s5>
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<fC03 i1="15" i2="3" l="FRE"><s0>Accrétion</s0>
<s5>40</s5>
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<s5>40</s5>
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<s5>41</s5>
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<s5>41</s5>
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<s5>42</s5>
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<fC03 i1="17" i2="3" l="ENG"><s0>X-ray binary stars</s0>
<s5>42</s5>
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<fC03 i1="18" i2="X" l="FRE"><s0>Source RX binaire</s0>
<s5>43</s5>
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<fC03 i1="18" i2="X" l="ENG"><s0>Binary X ray source</s0>
<s5>43</s5>
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<fC03 i1="18" i2="X" l="SPA"><s0>Fuente RX binaria</s0>
<s5>43</s5>
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<s5>44</s5>
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<s5>45</s5>
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<fC03 i1="20" i2="3" l="ENG"><s0>Cosmic x-ray sources</s0>
<s5>45</s5>
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<fN21><s1>023</s1>
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<fN44 i1="01"><s1>OTO</s1>
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<server><NO>PASCAL 12-0042281 INIST</NO>
<ET>A late jet rebrightening revealed from multiwavelength monitoring of the black hole candidate XTE J1752-223</ET>
<AU>RUSSELL (D. M.); CURRAN (P. A.); MUNOZ-DARIAS (T.); LEWIS (F.); MOTTA (S.); STIELE (H.); BELLONI (T.); MILLER-JONES (J. C. A.); JONKER (P. G.); O'BRIEN (K.); HOMAN (J.); CASELLA (P.); GANDHI (P.); SOLERI (P.); MARKOFF (S.); MAITRA (D.); GALLO (E.); CADOLLE BEL (M.)</AU>
<AF>Astronomical Institute 'Anton Pannekoek', University of Amsterdam, PO Box 94249/1090 GE Amsterdam/Pays-Bas (1 aut., 15 aut.); Laboratoire AIM, CEA/IRFU-Université Paris Diderot-CNRS/INSU, CEA DSM/IRFU/SAp, Centre de Saclay/91191 Gif-sur-Yvette/France (2 aut.); INAF-Osservatorio Astronomico di Brera, Via E. Bianchi 46/23807 Merate (LC/Italie (3 aut., 5 aut., 6 aut., 7 aut.); Faulkes Telescope Project, University of Glamorgan/Pontypridd CF37 1DL/Royaume-Uni (4 aut.); Department of Physics and Astronomy, The Open Universiy, Walton Hall/Milton Keynes MK7 6AA/Royaume-Uni (4 aut.); International Centre for Radio Astronomy Research, Curtin University, GPO Box U1987/Perth, WA 6845/Australie (8 aut.); SRON, Netherlands Institute for Space Research, Sorbonnelaan 2/3584 CA, Utrecht/Pays-Bas (9 aut.); Harvard-Smithsonian Center for Astrophysics, 60 Garden Street/Cambridge, MA 02138/Etats-Unis (9 aut.); Department of Astraphysics, IMAPP, Radboud University Nijmegen, PO Box 9010/6500 GL Nijmegen/Pays-Bas (9 aut.); Department of Physics, University of California/Santa Barbara, CA 93106-9530/Etats-Unis (10 aut.); MIT Kavli Institute for Astrophysics and Space Research, 70 Vassar Street/Cambridge, MA 02139/Etats-Unis (11 aut.); School of Physics and Astronomy, University of Southampton/Southampton, Hampshire SO17 IBJ/Royaume-Uni (12 aut.); ISAS, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, chuo-ku/Sngamihara, Kanagawa 229-8510/Japon (13 aut.); Kapteyn Astronomical Institute, University of Groningen, PO Box 800/9700 AV Groningen/Pays-Bas (14 aut.); Department of Astronomy, University of Michigan, 500 Church Street/Ann Arbor, MI 48109/Etats-Unis (16 aut., 17 aut.); ESAC, ISOC, Villanueva de la Canada, Madrid P. O. Box 78/28691/Espagne (18 aut.)</AF>
<DT>Publication en série; Niveau analytique</DT>
<SO>Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Etats-Unis; Da. 2012; Vol. 419; No. 2; Pp. 1740-1751; Bibl. 1 p.1/4</SO>
<LA>Anglais</LA>
<EA>We present optical monitoring of the black hole candidate XTE J1752-223 during its 2009-10 outburst and decay to quiescence. The optical light curve can be described by an exponential decay followed by a plateau, then a more rapid fade towards quiescence. The plateau appears to be due to an extra component of optical emission that brightens and then fades over ∼40 days. We show evidence for the origin of this optical 'flare' to be the synchrotron jet during the decaying hard state, and we identify and isolate both disc and jet components in the spectral energy distributions. The optical flare has the same morphology and amplitude as a contemporaneous X-ray rebrightening. This suggests a common origin, but no firm conclusions can be made favouring or disfavouring the jet producing the X-ray flare. The quiescent optical magnitudes are B ≥ 20.6, V ≥ 21.1, R ≥ 19.5, i' ≥ 19.2. From the optical outburst amplitude we estimate a likely orbital period of <22 h. We also present near-infrared (NIR) photometry and polarimetry and rare mid-IR imaging (8-12 μm) when the source is nearing quiescence. The fading jet component, and possibly the companion star, may contribute to the NIR flux. We derive deep mid-IR flux upper limits and NIR linear polarization upper limits. With the inclusion of radio data, we measure an almost flat jet spectral index between radio and optical; F<sub>ν</sub>
ν<sup>∼+0.05</sup>
. The data favour the jet break to optically thin emission to reside in the IR, but may shift to frequencies as high as the optical or UV during the peak of the flare.</EA>
<CC>001E03</CC>
<FD>Jet; Trou noir; Quiescence; Courbe lumière; Emission optique; Sursaut optique; Densité spectrale énergie; Morphologie; Photométrie IR; Polarimétrie; Borne supérieure; Polarisation rectiligne; Indice spectral; Déplacement fréquence; Accrétion; Disque accrétion; Binaire RX; Source RX binaire; Cosmologie; Source RX cosmique</FD>
<ED>Jets; Black holes; Quiescence; Light curves; Light emission; Optical burst; Spectral energy distribution; Morphology; Infrared photometry; Polarimetry; Upper bound; Linear polarization; Spectral index; Frequency shift; Accretion; Accretion disks; X-ray binary stars; Binary X ray source; Cosmology; Cosmic x-ray sources</ED>
<SD>Quietud; Emisión óptica; Arrebato óptico; Densidad espectral energía; Fotometría IR; Cota superior; Desplazamiento frecuencia; Fuente RX binaria</SD>
<LO>INIST-2067.354000506050220740</LO>
<ID>12-0042281</ID>
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