ISO observations of the environment of the soft gamma-ray repeater SGR 1806-20
Observations at near5 and mid-infrared wavelengths (1-18 μum) of SGR 1806-20 suggest that it is associated with a cluster of giant massive stars which are enshrouded in a dense cloud of dust. The centre of the best sky position of the gammaray source (Hurley et al. 1999) lies on top of the dust clou...
Guardado en:
| Autores principales: | , , , , , |
|---|---|
| Formato: | JOUR |
| Materias: | |
| Acceso en línea: | http://hdl.handle.net/20.500.12110/paper_00046361_v350_n3_p891_Fuchs |
| Aporte de: |
| id |
todo:paper_00046361_v350_n3_p891_Fuchs |
|---|---|
| record_format |
dspace |
| spelling |
todo:paper_00046361_v350_n3_p891_Fuchs2023-10-03T13:59:54Z ISO observations of the environment of the soft gamma-ray repeater SGR 1806-20 Fuchs, Y. Mirabel, F. Chaty, S. Claret, A. Cesarsky, C.J. Cesarsky, D.A. Gamma rays: bursts Infrared: stars Stars: individual: SGR 1806-20 Stars: peculiar-stars: pulsars: individual: SGR 1806-20 X-rays: stars Observations at near5 and mid-infrared wavelengths (1-18 μum) of SGR 1806-20 suggest that it is associated with a cluster of giant massive stars which are enshrouded in a dense cloud of dust. The centre of the best sky position of the gammaray source (Hurley et al. 1999) lies on top of the dust cloud at only 7 arcsec (∼ 0.5 pc at a distance of 14.5 kpc) from the star cluster, and 12 arcsec (∼ 0.85 pc) from a Luminous Blue Variable Star (LBV) which had been proposed to be associated with the SGR (Kulkarni et al. 1995). The bright cloud of interstellar gas and dust observed with ISO (Infrared Space Observatory) is probably the birth site of the cluster of massive stars, the LBV star, and the progenitor of the soft gamma-ray repeater pulsar. The presence of such a young star formation region is compatible with the current interpretation of soft gamma-ray repeaters as young neutron stars. The SGR 1806-20 compact source is unlikely to form a bound binary system with any of the infrared luminous massive stars, since no flux variations in the near-infrared were detected from the latter in an interval of 4 years. The ISO observations were made over two epochs, 11 days before and 2 hours after a soft gamma-ray burst detected with the Interplanetary Network, and they show no enhanced mid-infrared emission associated to the high energy activity of the SGR. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_00046361_v350_n3_p891_Fuchs |
| institution |
Universidad de Buenos Aires |
| institution_str |
I-28 |
| repository_str |
R-134 |
| collection |
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) |
| topic |
Gamma rays: bursts Infrared: stars Stars: individual: SGR 1806-20 Stars: peculiar-stars: pulsars: individual: SGR 1806-20 X-rays: stars |
| spellingShingle |
Gamma rays: bursts Infrared: stars Stars: individual: SGR 1806-20 Stars: peculiar-stars: pulsars: individual: SGR 1806-20 X-rays: stars Fuchs, Y. Mirabel, F. Chaty, S. Claret, A. Cesarsky, C.J. Cesarsky, D.A. ISO observations of the environment of the soft gamma-ray repeater SGR 1806-20 |
| topic_facet |
Gamma rays: bursts Infrared: stars Stars: individual: SGR 1806-20 Stars: peculiar-stars: pulsars: individual: SGR 1806-20 X-rays: stars |
| description |
Observations at near5 and mid-infrared wavelengths (1-18 μum) of SGR 1806-20 suggest that it is associated with a cluster of giant massive stars which are enshrouded in a dense cloud of dust. The centre of the best sky position of the gammaray source (Hurley et al. 1999) lies on top of the dust cloud at only 7 arcsec (∼ 0.5 pc at a distance of 14.5 kpc) from the star cluster, and 12 arcsec (∼ 0.85 pc) from a Luminous Blue Variable Star (LBV) which had been proposed to be associated with the SGR (Kulkarni et al. 1995). The bright cloud of interstellar gas and dust observed with ISO (Infrared Space Observatory) is probably the birth site of the cluster of massive stars, the LBV star, and the progenitor of the soft gamma-ray repeater pulsar. The presence of such a young star formation region is compatible with the current interpretation of soft gamma-ray repeaters as young neutron stars. The SGR 1806-20 compact source is unlikely to form a bound binary system with any of the infrared luminous massive stars, since no flux variations in the near-infrared were detected from the latter in an interval of 4 years. The ISO observations were made over two epochs, 11 days before and 2 hours after a soft gamma-ray burst detected with the Interplanetary Network, and they show no enhanced mid-infrared emission associated to the high energy activity of the SGR. |
| format |
JOUR |
| author |
Fuchs, Y. Mirabel, F. Chaty, S. Claret, A. Cesarsky, C.J. Cesarsky, D.A. |
| author_facet |
Fuchs, Y. Mirabel, F. Chaty, S. Claret, A. Cesarsky, C.J. Cesarsky, D.A. |
| author_sort |
Fuchs, Y. |
| title |
ISO observations of the environment of the soft gamma-ray repeater SGR 1806-20 |
| title_short |
ISO observations of the environment of the soft gamma-ray repeater SGR 1806-20 |
| title_full |
ISO observations of the environment of the soft gamma-ray repeater SGR 1806-20 |
| title_fullStr |
ISO observations of the environment of the soft gamma-ray repeater SGR 1806-20 |
| title_full_unstemmed |
ISO observations of the environment of the soft gamma-ray repeater SGR 1806-20 |
| title_sort |
iso observations of the environment of the soft gamma-ray repeater sgr 1806-20 |
| url |
http://hdl.handle.net/20.500.12110/paper_00046361_v350_n3_p891_Fuchs |
| work_keys_str_mv |
AT fuchsy isoobservationsoftheenvironmentofthesoftgammarayrepeatersgr180620 AT mirabelf isoobservationsoftheenvironmentofthesoftgammarayrepeatersgr180620 AT chatys isoobservationsoftheenvironmentofthesoftgammarayrepeatersgr180620 AT clareta isoobservationsoftheenvironmentofthesoftgammarayrepeatersgr180620 AT cesarskycj isoobservationsoftheenvironmentofthesoftgammarayrepeatersgr180620 AT cesarskyda isoobservationsoftheenvironmentofthesoftgammarayrepeatersgr180620 |
| _version_ |
1782028558583988224 |