Characterizing a new class of variability in GRS 1915+105 with simultaneous INTEGRAL/RXTE observations
Identifieur interne : 001777 ( PascalFrancis/Curation ); précédent : 001776; suivant : 001778Characterizing a new class of variability in GRS 1915+105 with simultaneous INTEGRAL/RXTE observations
Auteurs : D. C. Hannikainen [Finlande] ; J. Rodriguez [France, Suisse] ; O. Vilhu [Finlande] ; L. Hjalmarsdotter [Finlande] ; A. A. Zdziarski [Pologne] ; T. Belloni [Italie] ; J. Poutanen [Finlande] ; K. Wu [Royaume-Uni] ; S. E. Shaw [Suisse, Royaume-Uni] ; V. Beckmann [États-Unis] ; R. W. Hunstead [Australie] ; G. G. Pooley [Royaume-Uni] ; N. J. Westergaard [Danemark] ; I. F. Mirabel [Chili] ; P. Hakala [Finlande] ; A. Castro-Tirado [Espagne] ; Ph. Durouchoux [France]Source :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2005.
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- Pascal (Inist)
- Wicri :
- topic : Cosmologie.
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Abstract
We report on the analysis of 100 ks INTEGRAL observations of the Galactic microquasar GRS 1915+105. We focus on INTEGRAL Revolution number 48 when the source was found to exhibit a new type of variability as preliminarily reported in Hannikainen (2003, A&A, 411, L415). The variability pattern, which we name ξ, is characterized by a pulsing behaviour, consisting of a main pulse and a shorter, softer, and smaller amplitude precursor pulse, on a timescale of 5 min in the JEM-X 3-35 keV lightcurve. We also present simultaneous RXTE data. From a study of the individual RXTE/PCA pulse profiles we find that the rising phase is shorter and harder than the declining phase, which is opposite to what has been observed in other otherwise similar variability classes in this source. The position in the colour-colour diagram throughout the revolution corresponds to Stale A (Belloni et al. 2000, A&A, 355, 271) but not to any previously known variability class. We separated the INTEGRAL data into two subsets covering the maxima and minima of the pulses and fitted the resulting two broadband spectra with a hybrid thermal-non-thermal Comptonization model. The fits show the source to be in a soft state characterized by a strong disc component below ∼6 keV and Comptonization by both thermal and non-thermal electrons at higher energies.
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<record><TEI><teiHeader><fileDesc><titleStmt><title xml:lang="en" level="a">Characterizing a new class of variability in GRS 1915+105 with simultaneous INTEGRAL/RXTE observations</title><author><name sortKey="Hannikainen, D C" sort="Hannikainen, D C" uniqKey="Hannikainen D" first="D. C." last="Hannikainen">D. C. Hannikainen</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Observatory, PO Box 14, 00014 University of Helsinki</s1><s3>FIN</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Finlande</country></affiliation></author><author><name sortKey="Rodriguez, J" sort="Rodriguez, J" uniqKey="Rodriguez J" first="J." last="Rodriguez">J. Rodriguez</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Centre d'Études de Saclay. 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Beckmann</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>NASA Goddard Space Flight Center, Code 661</s1><s2>Greenhelt, MD 20771</s2><s3>USA</s3><sZ>10 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>Joint Center for Astrophysics, Department of Physics, University of Maryland, Baltimore County</s1><s2>Baltimore, MD 21250</s2><s3>USA</s3><sZ>10 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Hunstead, R W" sort="Hunstead, R W" uniqKey="Hunstead R" first="R. W." last="Hunstead">R. W. Hunstead</name><affiliation wicri:level="1"><inist:fA14 i1="11"><s1>School of Physics, University of Sydney</s1><s2>Sydney NSW 2006</s2><s3>AUS</s3><sZ>11 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Pooley, G G" sort="Pooley, G G" uniqKey="Pooley G" first="G. G." last="Pooley">G. G. Pooley</name><affiliation wicri:level="1"><inist:fA14 i1="12"><s1>Astrophysics Group, Cavendish Laboratory, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 0HE</s2><s3>GBR</s3><sZ>12 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Westergaard, N J" sort="Westergaard, N J" uniqKey="Westergaard N" first="N. J." last="Westergaard">N. J. Westergaard</name><affiliation wicri:level="1"><inist:fA14 i1="13"><s1>Danish Space Research Institute, Juliane Maries Vej 30</s1><s2>2100 Copenhagen</s2><s3>DNK</s3><sZ>13 aut.</sZ></inist:fA14><country>Danemark</country></affiliation></author><author><name sortKey="Mirabel, I F" sort="Mirabel, I F" uniqKey="Mirabel I" first="I. F." last="Mirabel">I. F. Mirabel</name><affiliation wicri:level="1"><inist:fA14 i1="14"><s1>European Southern Observatory</s1><s2>Santiago</s2><s3>CHL</s3><sZ>14 aut.</sZ></inist:fA14><country>Chili</country></affiliation></author><author><name sortKey="Hakala, P" sort="Hakala, P" uniqKey="Hakala P" first="P." last="Hakala">P. Hakala</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Observatory, PO Box 14, 00014 University of Helsinki</s1><s3>FIN</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Finlande</country></affiliation></author><author><name sortKey="Castro Tirado, A" sort="Castro Tirado, A" uniqKey="Castro Tirado A" first="A." last="Castro-Tirado">A. Castro-Tirado</name><affiliation wicri:level="1"><inist:fA14 i1="15"><s1>Instituto de Astrofisica de Andalucía (IAA-CSIC), PO Box 03004</s1><s2>18080 Granada</s2><s3>ESP</s3><sZ>16 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Durouchoux, Ph" sort="Durouchoux, Ph" uniqKey="Durouchoux P" first="Ph." last="Durouchoux">Ph. Durouchoux</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Centre d'Études de Saclay. DAPNIA/Service d'Astrophysique (CNRS FRE 2591), Bât. 709, Orme des Merisiers</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>2 aut.</sZ><sZ>17 aut.</sZ></inist:fA14><country>France</country></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">05-0272474</idno><date when="2005">2005</date><idno type="stanalyst">PASCAL 05-0272474 INIST</idno><idno type="RBID">Pascal:05-0272474</idno><idno type="wicri:Area/PascalFrancis/Corpus">004926</idno><idno type="wicri:Area/PascalFrancis/Curation">001777</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Characterizing a new class of variability in GRS 1915+105 with simultaneous INTEGRAL/RXTE observations</title><author><name sortKey="Hannikainen, D C" sort="Hannikainen, D C" uniqKey="Hannikainen D" first="D. C." last="Hannikainen">D. C. Hannikainen</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Observatory, PO Box 14, 00014 University of Helsinki</s1><s3>FIN</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Finlande</country></affiliation></author><author><name sortKey="Rodriguez, J" sort="Rodriguez, J" uniqKey="Rodriguez J" first="J." last="Rodriguez">J. Rodriguez</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Centre d'Études de Saclay. DAPNIA/Service d'Astrophysique (CNRS FRE 2591), Bât. 709, Orme des Merisiers</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>2 aut.</sZ><sZ>17 aut.</sZ></inist:fA14><country>France</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>INTEGRAL Science Data Center, Chemin d'Écogia 16</s1><s2>1290 Versoix</s2><s3>CHE</s3><sZ>2 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Suisse</country></affiliation></author><author><name sortKey="Vilhu, O" sort="Vilhu, O" uniqKey="Vilhu O" first="O." last="Vilhu">O. Vilhu</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Observatory, PO Box 14, 00014 University of Helsinki</s1><s3>FIN</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Finlande</country></affiliation></author><author><name sortKey="Hjalmarsdotter, L" sort="Hjalmarsdotter, L" uniqKey="Hjalmarsdotter L" first="L." last="Hjalmarsdotter">L. Hjalmarsdotter</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Observatory, PO Box 14, 00014 University of Helsinki</s1><s3>FIN</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Finlande</country></affiliation></author><author><name sortKey="Zdziarski, A A" sort="Zdziarski, A A" uniqKey="Zdziarski A" first="A. A." last="Zdziarski">A. A. Zdziarski</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Nicolaus Copernicus Astronomical Center, Bartycka 18</s1><s2>00-716 Warszawa</s2><s3>POL</s3><sZ>5 aut.</sZ></inist:fA14><country>Pologne</country></affiliation></author><author><name sortKey="Belloni, T" sort="Belloni, T" uniqKey="Belloni T" first="T." last="Belloni">T. Belloni</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>INAF - Osservatorio Astronomico di Brera, via E. Bianchi 46</s1><s2>23807 Merate (LC)</s2><s3>ITA</s3><sZ>6 aut.</sZ></inist:fA14><country>Italie</country></affiliation></author><author><name sortKey="Poutanen, J" sort="Poutanen, J" uniqKey="Poutanen J" first="J." last="Poutanen">J. Poutanen</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Astronomy Division, University of Oulu, PO Box 3000</s1><s2>Oulu 90014</s2><s3>FIN</s3><sZ>7 aut.</sZ></inist:fA14><country>Finlande</country></affiliation></author><author><name sortKey="Wu, K" sort="Wu, K" uniqKey="Wu K" first="K." last="Wu">K. Wu</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>MSSL, University College London, Holmbury St. Mary</s1><s2>Surrey, RH5 6NT</s2><s3>GBR</s3><sZ>8 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Shaw, S E" sort="Shaw, S E" uniqKey="Shaw S" first="S. E." last="Shaw">S. E. Shaw</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>INTEGRAL Science Data Center, Chemin d'Écogia 16</s1><s2>1290 Versoix</s2><s3>CHE</s3><sZ>2 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Suisse</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Dept. of Physics and Astronomy, University of Southampton</s1><s2>Southampton SO 17 1 BJ</s2><s3>GBR</s3><sZ>9 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Beckmann, V" sort="Beckmann, V" uniqKey="Beckmann V" first="V." last="Beckmann">V. Beckmann</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>NASA Goddard Space Flight Center, Code 661</s1><s2>Greenhelt, MD 20771</s2><s3>USA</s3><sZ>10 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>Joint Center for Astrophysics, Department of Physics, University of Maryland, Baltimore County</s1><s2>Baltimore, MD 21250</s2><s3>USA</s3><sZ>10 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Hunstead, R W" sort="Hunstead, R W" uniqKey="Hunstead R" first="R. W." last="Hunstead">R. W. Hunstead</name><affiliation wicri:level="1"><inist:fA14 i1="11"><s1>School of Physics, University of Sydney</s1><s2>Sydney NSW 2006</s2><s3>AUS</s3><sZ>11 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Pooley, G G" sort="Pooley, G G" uniqKey="Pooley G" first="G. G." last="Pooley">G. G. Pooley</name><affiliation wicri:level="1"><inist:fA14 i1="12"><s1>Astrophysics Group, Cavendish Laboratory, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 0HE</s2><s3>GBR</s3><sZ>12 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Westergaard, N J" sort="Westergaard, N J" uniqKey="Westergaard N" first="N. J." last="Westergaard">N. J. Westergaard</name><affiliation wicri:level="1"><inist:fA14 i1="13"><s1>Danish Space Research Institute, Juliane Maries Vej 30</s1><s2>2100 Copenhagen</s2><s3>DNK</s3><sZ>13 aut.</sZ></inist:fA14><country>Danemark</country></affiliation></author><author><name sortKey="Mirabel, I F" sort="Mirabel, I F" uniqKey="Mirabel I" first="I. F." last="Mirabel">I. F. Mirabel</name><affiliation wicri:level="1"><inist:fA14 i1="14"><s1>European Southern Observatory</s1><s2>Santiago</s2><s3>CHL</s3><sZ>14 aut.</sZ></inist:fA14><country>Chili</country></affiliation></author><author><name sortKey="Hakala, P" sort="Hakala, P" uniqKey="Hakala P" first="P." last="Hakala">P. Hakala</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Observatory, PO Box 14, 00014 University of Helsinki</s1><s3>FIN</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Finlande</country></affiliation></author><author><name sortKey="Castro Tirado, A" sort="Castro Tirado, A" uniqKey="Castro Tirado A" first="A." last="Castro-Tirado">A. Castro-Tirado</name><affiliation wicri:level="1"><inist:fA14 i1="15"><s1>Instituto de Astrofisica de Andalucía (IAA-CSIC), PO Box 03004</s1><s2>18080 Granada</s2><s3>ESP</s3><sZ>16 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Durouchoux, Ph" sort="Durouchoux, Ph" uniqKey="Durouchoux P" first="Ph." last="Durouchoux">Ph. Durouchoux</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Centre d'Études de Saclay. DAPNIA/Service d'Astrophysique (CNRS FRE 2591), Bât. 709, Orme des Merisiers</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>2 aut.</sZ><sZ>17 aut.</sZ></inist:fA14><country>France</country></affiliation></author></analytic><series><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno><imprint><date when="2005">2005</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Binary X ray source</term><term>Black holes</term><term>Cosmic x-ray sources</term><term>Cosmology</term><term>Gamma radiation</term><term>Light curves</term><term>Models</term><term>Positions</term><term>Precursor</term><term>Pulse shape</term><term>Simultaneous observation</term><term>Thermal electron</term><term>Two color diagram</term><term>Variability</term><term>X-ray binary stars</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Variabilité</term><term>Observation simultanée</term><term>Précurseur</term><term>Courbe lumière</term><term>Forme impulsion</term><term>Position</term><term>Diagramme 2 couleurs</term><term>Modèle</term><term>Electron thermique</term><term>Binaire RX</term><term>Source RX binaire</term><term>Rayonnement gamma</term><term>Trou noir</term><term>Source RX cosmique</term><term>Cosmologie</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 report on the analysis of 100 ks INTEGRAL observations of the Galactic microquasar GRS 1915+105. We focus on INTEGRAL Revolution number 48 when the source was found to exhibit a new type of variability as preliminarily reported in Hannikainen (2003, A&A, 411, L415). The variability pattern, which we name ξ, is characterized by a pulsing behaviour, consisting of a main pulse and a shorter, softer, and smaller amplitude precursor pulse, on a timescale of 5 min in the JEM-X 3-35 keV lightcurve. We also present simultaneous RXTE data. From a study of the individual RXTE/PCA pulse profiles we find that the rising phase is shorter and harder than the declining phase, which is opposite to what has been observed in other otherwise similar variability classes in this source. The position in the colour-colour diagram throughout the revolution corresponds to Stale A (Belloni et al. 2000, A&A, 355, 271) but not to any previously known variability class. We separated the INTEGRAL data into two subsets covering the maxima and minima of the pulses and fitted the resulting two broadband spectra with a hybrid thermal-non-thermal Comptonization model. The fits show the source to be in a soft state characterized by a strong disc component below ∼6 keV and Comptonization by both thermal and non-thermal electrons at higher energies.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0004-6361</s0></fA01><fA02 i1="01"><s0>AAEJAF</s0></fA02><fA03 i2="1"><s0>Astron. astrophys. : (Berl., Print)</s0></fA03><fA05><s2>435</s2></fA05><fA06><s2>3</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Characterizing a new class of variability in GRS 1915+105 with simultaneous INTEGRAL/RXTE observations</s1></fA08><fA11 i1="01" i2="1"><s1>HANNIKAINEN (D. C.)</s1></fA11><fA11 i1="02" i2="1"><s1>RODRIGUEZ (J.)</s1></fA11><fA11 i1="03" i2="1"><s1>VILHU (O.)</s1></fA11><fA11 i1="04" i2="1"><s1>HJALMARSDOTTER (L.)</s1></fA11><fA11 i1="05" i2="1"><s1>ZDZIARSKI (A. A.)</s1></fA11><fA11 i1="06" i2="1"><s1>BELLONI (T.)</s1></fA11><fA11 i1="07" i2="1"><s1>POUTANEN (J.)</s1></fA11><fA11 i1="08" i2="1"><s1>WU (K.)</s1></fA11><fA11 i1="09" i2="1"><s1>SHAW (S. E.)</s1></fA11><fA11 i1="10" i2="1"><s1>BECKMANN (V.)</s1></fA11><fA11 i1="11" i2="1"><s1>HUNSTEAD (R. W.)</s1></fA11><fA11 i1="12" i2="1"><s1>POOLEY (G. G.)</s1></fA11><fA11 i1="13" i2="1"><s1>WESTERGAARD (N. J.)</s1></fA11><fA11 i1="14" i2="1"><s1>MIRABEL (I. F.)</s1></fA11><fA11 i1="15" i2="1"><s1>HAKALA (P.)</s1></fA11><fA11 i1="16" i2="1"><s1>CASTRO-TIRADO (A.)</s1></fA11><fA11 i1="17" i2="1"><s1>DUROUCHOUX (Ph.)</s1></fA11><fA14 i1="01"><s1>Observatory, PO Box 14, 00014 University of Helsinki</s1><s3>FIN</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>15 aut.</sZ></fA14><fA14 i1="02"><s1>Centre d'Études de Saclay. DAPNIA/Service d'Astrophysique (CNRS FRE 2591), Bât. 709, Orme des Merisiers</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>2 aut.</sZ><sZ>17 aut.</sZ></fA14><fA14 i1="03"><s1>INTEGRAL Science Data Center, Chemin d'Écogia 16</s1><s2>1290 Versoix</s2><s3>CHE</s3><sZ>2 aut.</sZ><sZ>9 aut.</sZ></fA14><fA14 i1="04"><s1>Nicolaus Copernicus Astronomical Center, Bartycka 18</s1><s2>00-716 Warszawa</s2><s3>POL</s3><sZ>5 aut.</sZ></fA14><fA14 i1="05"><s1>INAF - Osservatorio Astronomico di Brera, via E. Bianchi 46</s1><s2>23807 Merate (LC)</s2><s3>ITA</s3><sZ>6 aut.</sZ></fA14><fA14 i1="06"><s1>Astronomy Division, University of Oulu, PO Box 3000</s1><s2>Oulu 90014</s2><s3>FIN</s3><sZ>7 aut.</sZ></fA14><fA14 i1="07"><s1>MSSL, University College London, Holmbury St. Mary</s1><s2>Surrey, RH5 6NT</s2><s3>GBR</s3><sZ>8 aut.</sZ></fA14><fA14 i1="08"><s1>Dept. of Physics and Astronomy, University of Southampton</s1><s2>Southampton SO 17 1 BJ</s2><s3>GBR</s3><sZ>9 aut.</sZ></fA14><fA14 i1="09"><s1>NASA Goddard Space Flight Center, Code 661</s1><s2>Greenhelt, MD 20771</s2><s3>USA</s3><sZ>10 aut.</sZ></fA14><fA14 i1="10"><s1>Joint Center for Astrophysics, Department of Physics, University of Maryland, Baltimore County</s1><s2>Baltimore, MD 21250</s2><s3>USA</s3><sZ>10 aut.</sZ></fA14><fA14 i1="11"><s1>School of Physics, University of Sydney</s1><s2>Sydney NSW 2006</s2><s3>AUS</s3><sZ>11 aut.</sZ></fA14><fA14 i1="12"><s1>Astrophysics Group, Cavendish Laboratory, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 0HE</s2><s3>GBR</s3><sZ>12 aut.</sZ></fA14><fA14 i1="13"><s1>Danish Space Research Institute, Juliane Maries Vej 30</s1><s2>2100 Copenhagen</s2><s3>DNK</s3><sZ>13 aut.</sZ></fA14><fA14 i1="14"><s1>European Southern Observatory</s1><s2>Santiago</s2><s3>CHL</s3><sZ>14 aut.</sZ></fA14><fA14 i1="15"><s1>Instituto de Astrofisica de Andalucía (IAA-CSIC), PO Box 03004</s1><s2>18080 Granada</s2><s3>ESP</s3><sZ>16 aut.</sZ></fA14><fA20><s1>995-1004</s1></fA20><fA21><s1>2005</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>14176</s2><s5>354000129907100190</s5></fA43><fA44><s0>0000</s0><s1>© 2005 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>50 ref.</s0></fA45><fA47 i1="01" i2="1"><s0>05-0272474</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Astronomy and astrophysics : (Berlin. Print)</s0></fA64><fA66 i1="01"><s0>FRA</s0></fA66><fC01 i1="01" l="ENG"><s0>We report on the analysis of 100 ks INTEGRAL observations of the Galactic microquasar GRS 1915+105. We focus on INTEGRAL Revolution number 48 when the source was found to exhibit a new type of variability as preliminarily reported in Hannikainen (2003, A&A, 411, L415). The variability pattern, which we name ξ, is characterized by a pulsing behaviour, consisting of a main pulse and a shorter, softer, and smaller amplitude precursor pulse, on a timescale of 5 min in the JEM-X 3-35 keV lightcurve. We also present simultaneous RXTE data. From a study of the individual RXTE/PCA pulse profiles we find that the rising phase is shorter and harder than the declining phase, which is opposite to what has been observed in other otherwise similar variability classes in this source. The position in the colour-colour diagram throughout the revolution corresponds to Stale A (Belloni et al. 2000, A&A, 355, 271) but not to any previously known variability class. We separated the INTEGRAL data into two subsets covering the maxima and minima of the pulses and fitted the resulting two broadband spectra with a hybrid thermal-non-thermal Comptonization model. The fits show the source to be in a soft state characterized by a strong disc component below ∼6 keV and Comptonization by both thermal and non-thermal electrons at higher energies.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="X" l="FRE"><s0>Variabilité</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="ENG"><s0>Variability</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="SPA"><s0>Variabilidad</s0><s5>26</s5></fC03><fC03 i1="02" i2="X" l="FRE"><s0>Observation simultanée</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="ENG"><s0>Simultaneous observation</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="SPA"><s0>Observación simultánea</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Précurseur</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Precursor</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>Forme impulsion</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="ENG"><s0>Pulse shape</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="SPA"><s0>Forma impulsión</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Position</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Positions</s0><s5>31</s5></fC03><fC03 i1="07" i2="X" l="FRE"><s0>Diagramme 2 couleurs</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="ENG"><s0>Two color diagram</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="SPA"><s0>Diagrama 2 colores</s0><s5>32</s5></fC03><fC03 i1="08" i2="X" l="FRE"><s0>Modèle</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="ENG"><s0>Models</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="SPA"><s0>Modelo</s0><s5>33</s5></fC03><fC03 i1="09" i2="X" l="FRE"><s0>Electron thermique</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="ENG"><s0>Thermal electron</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="SPA"><s0>Electrón térmico</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Binaire RX</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>X-ray binary stars</s0><s5>35</s5></fC03><fC03 i1="11" i2="X" l="FRE"><s0>Source RX binaire</s0><s5>36</s5></fC03><fC03 i1="11" i2="X" l="ENG"><s0>Binary X ray source</s0><s5>36</s5></fC03><fC03 i1="11" i2="X" l="SPA"><s0>Fuente RX binaria</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Rayonnement gamma</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Gamma radiation</s0><s5>37</s5></fC03><fC03 i1="13" i2="3" l="FRE"><s0>Trou noir</s0><s5>38</s5></fC03><fC03 i1="13" i2="3" l="ENG"><s0>Black holes</s0><s5>38</s5></fC03><fC03 i1="14" i2="3" l="FRE"><s0>Source RX cosmique</s0><s5>39</s5></fC03><fC03 i1="14" i2="3" l="ENG"><s0>Cosmic x-ray sources</s0><s5>39</s5></fC03><fC03 i1="15" i2="3" l="FRE"><s0>Cosmologie</s0><s5>40</s5></fC03><fC03 i1="15" i2="3" l="ENG"><s0>Cosmology</s0><s5>40</s5></fC03><fN21><s1>192</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard></inist></record>Pour manipuler ce document sous Unix (Dilib)
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