On the nature of the hard X-ray source IGR J2018+4043
We found a very likely counterpart to the recently discovered hard X-ray source IGR J2018+4043 in the multiwavelength observations of the source field. The source, originally discovered in the 20-40 keV band, is now confidently detected also in the 40-80 keV band, with a flux of (1.4 ± 0.4) × 10-11...
Guardado en:
| Autores principales: | , , , , , , , , , , , , , , , |
|---|---|
| Formato: | JOUR |
| Materias: | |
| Acceso en línea: | http://hdl.handle.net/20.500.12110/paper_0004637X_v649_n1II_pL21_Bykov |
| Aporte de: |
| id |
todo:paper_0004637X_v649_n1II_pL21_Bykov |
|---|---|
| record_format |
dspace |
| spelling |
todo:paper_0004637X_v649_n1II_pL21_Bykov2023-10-03T14:02:03Z On the nature of the hard X-ray source IGR J2018+4043 Bykov, A.M. Krassilchtchikov, A.M. Uvarov, Yu.A. Kennea, J.A. Pavlov, G.G. Dubner, G.M. Giacani, E.B. Bloemen, H. Hermsen, W. Kaastra, J. Lebrun, F. Renaud, M. Terrier, R. Debecker, M. Rauw, G. Swings, J.-P. ISM: Individual (γ Cygni) Supernova remnants X-rays: ISM We found a very likely counterpart to the recently discovered hard X-ray source IGR J2018+4043 in the multiwavelength observations of the source field. The source, originally discovered in the 20-40 keV band, is now confidently detected also in the 40-80 keV band, with a flux of (1.4 ± 0.4) × 10-11 ergs cm-2 s-1. A 5 ks Swift observation of the IGR J2018+4043 field revealed a hard pointlike source with an observed 0.5-10 keV flux of 3.4-0.8+0.7 × 10-12 ergs cm-2 s-1 (90% confidence level) at α = 20 h18m38.s55, δ = +40°41′00. ″4 (with a 4.″2 uncertainty). The combined Swift-INTEGRAL spectrum can be described by an absorbed power-law model with photon index Γ = 1.3 ± 0.2 and NH = 6.1-2.2+3.2 × 1022 cm-2. In archival optical and infrared data we found a slightly extended and highly absorbed object at the Swift source position. There is also an extended VLA 1.4 GHz source peaked at a beamwidth distance from the optical and X-ray positions. The observed morphology and multiwavelength spectra of IGR J2018+4043 are consistent with those expected for an obscured accreting object, i.e., an AGN or a Galactic X-ray binary. The identification suggests possible connection of IGR J2018+4043 to the bright γ-ray source GEV J2020+4023 detected by COS B and CGRO EGRET. © 2006. The American Astronomical Society. All rights reserved. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_0004637X_v649_n1II_pL21_Bykov |
| institution |
Universidad de Buenos Aires |
| institution_str |
I-28 |
| repository_str |
R-134 |
| collection |
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) |
| topic |
ISM: Individual (γ Cygni) Supernova remnants X-rays: ISM |
| spellingShingle |
ISM: Individual (γ Cygni) Supernova remnants X-rays: ISM Bykov, A.M. Krassilchtchikov, A.M. Uvarov, Yu.A. Kennea, J.A. Pavlov, G.G. Dubner, G.M. Giacani, E.B. Bloemen, H. Hermsen, W. Kaastra, J. Lebrun, F. Renaud, M. Terrier, R. Debecker, M. Rauw, G. Swings, J.-P. On the nature of the hard X-ray source IGR J2018+4043 |
| topic_facet |
ISM: Individual (γ Cygni) Supernova remnants X-rays: ISM |
| description |
We found a very likely counterpart to the recently discovered hard X-ray source IGR J2018+4043 in the multiwavelength observations of the source field. The source, originally discovered in the 20-40 keV band, is now confidently detected also in the 40-80 keV band, with a flux of (1.4 ± 0.4) × 10-11 ergs cm-2 s-1. A 5 ks Swift observation of the IGR J2018+4043 field revealed a hard pointlike source with an observed 0.5-10 keV flux of 3.4-0.8+0.7 × 10-12 ergs cm-2 s-1 (90% confidence level) at α = 20 h18m38.s55, δ = +40°41′00. ″4 (with a 4.″2 uncertainty). The combined Swift-INTEGRAL spectrum can be described by an absorbed power-law model with photon index Γ = 1.3 ± 0.2 and NH = 6.1-2.2+3.2 × 1022 cm-2. In archival optical and infrared data we found a slightly extended and highly absorbed object at the Swift source position. There is also an extended VLA 1.4 GHz source peaked at a beamwidth distance from the optical and X-ray positions. The observed morphology and multiwavelength spectra of IGR J2018+4043 are consistent with those expected for an obscured accreting object, i.e., an AGN or a Galactic X-ray binary. The identification suggests possible connection of IGR J2018+4043 to the bright γ-ray source GEV J2020+4023 detected by COS B and CGRO EGRET. © 2006. The American Astronomical Society. All rights reserved. |
| format |
JOUR |
| author |
Bykov, A.M. Krassilchtchikov, A.M. Uvarov, Yu.A. Kennea, J.A. Pavlov, G.G. Dubner, G.M. Giacani, E.B. Bloemen, H. Hermsen, W. Kaastra, J. Lebrun, F. Renaud, M. Terrier, R. Debecker, M. Rauw, G. Swings, J.-P. |
| author_facet |
Bykov, A.M. Krassilchtchikov, A.M. Uvarov, Yu.A. Kennea, J.A. Pavlov, G.G. Dubner, G.M. Giacani, E.B. Bloemen, H. Hermsen, W. Kaastra, J. Lebrun, F. Renaud, M. Terrier, R. Debecker, M. Rauw, G. Swings, J.-P. |
| author_sort |
Bykov, A.M. |
| title |
On the nature of the hard X-ray source IGR J2018+4043 |
| title_short |
On the nature of the hard X-ray source IGR J2018+4043 |
| title_full |
On the nature of the hard X-ray source IGR J2018+4043 |
| title_fullStr |
On the nature of the hard X-ray source IGR J2018+4043 |
| title_full_unstemmed |
On the nature of the hard X-ray source IGR J2018+4043 |
| title_sort |
on the nature of the hard x-ray source igr j2018+4043 |
| url |
http://hdl.handle.net/20.500.12110/paper_0004637X_v649_n1II_pL21_Bykov |
| work_keys_str_mv |
AT bykovam onthenatureofthehardxraysourceigrj20184043 AT krassilchtchikovam onthenatureofthehardxraysourceigrj20184043 AT uvarovyua onthenatureofthehardxraysourceigrj20184043 AT kenneaja onthenatureofthehardxraysourceigrj20184043 AT pavlovgg onthenatureofthehardxraysourceigrj20184043 AT dubnergm onthenatureofthehardxraysourceigrj20184043 AT giacanieb onthenatureofthehardxraysourceigrj20184043 AT bloemenh onthenatureofthehardxraysourceigrj20184043 AT hermsenw onthenatureofthehardxraysourceigrj20184043 AT kaastraj onthenatureofthehardxraysourceigrj20184043 AT lebrunf onthenatureofthehardxraysourceigrj20184043 AT renaudm onthenatureofthehardxraysourceigrj20184043 AT terrierr onthenatureofthehardxraysourceigrj20184043 AT debeckerm onthenatureofthehardxraysourceigrj20184043 AT rauwg onthenatureofthehardxraysourceigrj20184043 AT swingsjp onthenatureofthehardxraysourceigrj20184043 |
| _version_ |
1782029875948814336 |