On the nature of the soft γ-ray emission in the hard state of the black hole transient GRS 1716−249
The black hole transient GRS 1716−249 was monitored from the radio to the γ -ray band during its 2016-2017 outburst. This paper focuses on the spectral energy distribution (SED) obtained in 2017 February-March, when GRS 1716−249 was in a bright hard spectral state. The soft γ -ray data collected wit...
| Main Authors: | , , , , , , , , , , , |
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| Format: | Journal Article |
| Language: | English |
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OXFORD UNIV PRESS
2020
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| Online Access: | http://purl.org/au-research/grants/arc/FT140101082 http://hdl.handle.net/20.500.11937/91531 |
| _version_ | 1848765539973857280 |
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| author | Bassi, T. Malzac, J. Del Santo, M. Jourdain, E. Roques, J.P. D'Aì, A. Miller-Jones, James Belmont, R. Motta, S.E. Segreto, A. Testa, V. Casella, P. |
| author_facet | Bassi, T. Malzac, J. Del Santo, M. Jourdain, E. Roques, J.P. D'Aì, A. Miller-Jones, James Belmont, R. Motta, S.E. Segreto, A. Testa, V. Casella, P. |
| author_sort | Bassi, T. |
| building | Curtin Institutional Repository |
| collection | Online Access |
| description | The black hole transient GRS 1716−249 was monitored from the radio to the γ -ray band during its 2016-2017 outburst. This paper focuses on the spectral energy distribution (SED) obtained in 2017 February-March, when GRS 1716−249 was in a bright hard spectral state. The soft γ -ray data collected with the INTEGRAL/SPI telescope show the presence of a spectral component that is in excess of the thermal Comptonization emission. This component is usually interpreted as inverse Compton emission from a tiny fraction of non-thermal electrons in the X-ray corona. We find that hybrid thermal/non-thermal Comptonization models provide a good fit to the X-/γ -ray spectrum of GRS 1716−249. The best-fitting parameters are typical of the bright hard state spectra observed in other black hole X-ray binaries. Moreover, the magnetized hybrid Comptonization model BELM provides an upper limit on the intensity of the coronal magnetic field of about 106 G. Alternatively, this soft γ -ray emission could originate from synchrotron emission in the radio jet. In order to test this hypothesis, we fit the SED with the irradiated disc plus Comptonization model combined with the jet internal shock emission model ISHEM. We found that a jet with an electron distribution of p = 2.1 can reproduce the soft γ -ray emission of GRS 1716−249. However, if we introduce the expected cooling break around 10 keV, the jet model can no longer explain the observed soft γ -ray emission, unless the index of the electron energy distribution is significantly harder (p < 2). |
| first_indexed | 2025-11-14T11:36:52Z |
| format | Journal Article |
| id | curtin-20.500.11937-91531 |
| institution | Curtin University Malaysia |
| institution_category | Local University |
| language | English |
| last_indexed | 2025-11-14T11:36:52Z |
| publishDate | 2020 |
| publisher | OXFORD UNIV PRESS |
| recordtype | eprints |
| repository_type | Digital Repository |
| spelling | curtin-20.500.11937-915312023-05-11T02:59:47Z On the nature of the soft γ-ray emission in the hard state of the black hole transient GRS 1716−249 Bassi, T. Malzac, J. Del Santo, M. Jourdain, E. Roques, J.P. D'Aì, A. Miller-Jones, James Belmont, R. Motta, S.E. Segreto, A. Testa, V. Casella, P. Science & Technology Physical Sciences Astronomy & Astrophysics accretion, accretion discs black hole physics ISM: jets and outflows gammarays: general X-rays: binaries SPECTRAL ENERGY-DISTRIBUTION X-RAY COMPACT JET INTERNAL SHOCKS CYGNUS X-1 ACCRETION RADIO VARIABILITY SYNCHROTRON RADIATION The black hole transient GRS 1716−249 was monitored from the radio to the γ -ray band during its 2016-2017 outburst. This paper focuses on the spectral energy distribution (SED) obtained in 2017 February-March, when GRS 1716−249 was in a bright hard spectral state. The soft γ -ray data collected with the INTEGRAL/SPI telescope show the presence of a spectral component that is in excess of the thermal Comptonization emission. This component is usually interpreted as inverse Compton emission from a tiny fraction of non-thermal electrons in the X-ray corona. We find that hybrid thermal/non-thermal Comptonization models provide a good fit to the X-/γ -ray spectrum of GRS 1716−249. The best-fitting parameters are typical of the bright hard state spectra observed in other black hole X-ray binaries. Moreover, the magnetized hybrid Comptonization model BELM provides an upper limit on the intensity of the coronal magnetic field of about 106 G. Alternatively, this soft γ -ray emission could originate from synchrotron emission in the radio jet. In order to test this hypothesis, we fit the SED with the irradiated disc plus Comptonization model combined with the jet internal shock emission model ISHEM. We found that a jet with an electron distribution of p = 2.1 can reproduce the soft γ -ray emission of GRS 1716−249. However, if we introduce the expected cooling break around 10 keV, the jet model can no longer explain the observed soft γ -ray emission, unless the index of the electron energy distribution is significantly harder (p < 2). 2020 Journal Article http://hdl.handle.net/20.500.11937/91531 10.1093/mnras/staa739 English http://purl.org/au-research/grants/arc/FT140101082 OXFORD UNIV PRESS fulltext |
| spellingShingle | Science & Technology Physical Sciences Astronomy & Astrophysics accretion, accretion discs black hole physics ISM: jets and outflows gammarays: general X-rays: binaries SPECTRAL ENERGY-DISTRIBUTION X-RAY COMPACT JET INTERNAL SHOCKS CYGNUS X-1 ACCRETION RADIO VARIABILITY SYNCHROTRON RADIATION Bassi, T. Malzac, J. Del Santo, M. Jourdain, E. Roques, J.P. D'Aì, A. Miller-Jones, James Belmont, R. Motta, S.E. Segreto, A. Testa, V. Casella, P. On the nature of the soft γ-ray emission in the hard state of the black hole transient GRS 1716−249 |
| title | On the nature of the soft γ-ray emission in the hard state of the black hole transient GRS 1716−249 |
| title_full | On the nature of the soft γ-ray emission in the hard state of the black hole transient GRS 1716−249 |
| title_fullStr | On the nature of the soft γ-ray emission in the hard state of the black hole transient GRS 1716−249 |
| title_full_unstemmed | On the nature of the soft γ-ray emission in the hard state of the black hole transient GRS 1716−249 |
| title_short | On the nature of the soft γ-ray emission in the hard state of the black hole transient GRS 1716−249 |
| title_sort | on the nature of the soft γ-ray emission in the hard state of the black hole transient grs 1716−249 |
| topic | Science & Technology Physical Sciences Astronomy & Astrophysics accretion, accretion discs black hole physics ISM: jets and outflows gammarays: general X-rays: binaries SPECTRAL ENERGY-DISTRIBUTION X-RAY COMPACT JET INTERNAL SHOCKS CYGNUS X-1 ACCRETION RADIO VARIABILITY SYNCHROTRON RADIATION |
| url | http://purl.org/au-research/grants/arc/FT140101082 http://hdl.handle.net/20.500.11937/91531 |