Discovery of hard X-ray emission from supernova 1987A

Sunyaev, R.; Kaniovsky, A. S.; Efremov, V. V.; Gilfanov, M.; Churazov, E.; Гребенев, С. А.; Кузнецов, А. В.; Melioranskiy, A. S.; Yamburenko, N.; Yunin, S.; Stepanov, D.; Chulkov, I.; Pappe, N. Yu.; Boyarskiy, M.; Gavrilova, E. A.; Loznikov, V. M.; Prudkoglyad, AF; Rodin, V. G.; Reppin, C.; Pietsch, W.; Engelhauser, J.; Trümper, J.; Voges, W.; Kendziorra, E.; Bezler, M.; Staubert, R.; Brinkman, A. C.; Heise, J.; Mels, W. A.; Jäger, R.; Skinner, G. K.; Al-Emam, O.; Patterson, T. G.; Willmore, A. P.

doi:10.1038/330227a0

Cited by 167 publications

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“…Indeed, the Ginga satellite (10-30 keV) and the Kvant-Roentgen experiment (15-103 keV) on the Mir mission detected X-rays already in the middle of August 1987. The shape of the X-spectrum corres ponds well to the theoretical predictions [7], The early arrival of X-rays was inter preted [3,4] as the result of the mixing of radioactive Ni and Co during the ex plosion. The explosion might have been non radial or might have had "fingers", alternatively a Rayleigh-Taylor instability due to the radiation of Ni and Co might have occurred and produced the neces sary mixing during the explosion -to quote some of the proposed explana tions.…”

Section: Photometric and Spectroscopic Obser Vationssupporting

confidence: 64%

Supernova 1987 A

Maeder¹

1989

Europhys. News

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Section: Photometric and Spectroscopic Obser Vationssupporting

confidence: 64%

Supernova 1987 A

Maeder¹

1989

Europhys. News

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“…The data taken with ART-P, on board the same satellite, but working in a lower energy band (3-15 keV), revealed LMC X-1 and the young rotation powered pulsar PSR B0540-69, without any significant detection above 10 keV (Grebenev et al 1991). The TTM telescope (2-27 keV) detected only LMC X-4 and supernova SN 1987A above 15 keV (Sunyaev et al 1990(Sunyaev et al , 1987.…”

Section: Introductionmentioning

confidence: 99%

An INTEGRAL hard X-ray survey of the Large Magellanic Cloud

Götz¹,

Mereghetti²,

Merlini

et al. 2006

A&A

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Two observation campaigns in 2003 and 2004 with the INTEGRAL satellite have provided the first sensitive survey of the Large Magellanic Cloud with an imaging instrument in the hard X-ray range (15 keV-10 MeV). The high energy flux and long-term variability of the black hole candidate LMC X-1 was measured for the first time without contamination by the nearby (∼25 ) young pulsar PSR B0540-69. We studied the accreting pulsar LMC X-4 by constraining the size of the hard X-ray emitting region (≤3 × 10 10 cm) from analysis of its eclipses and by measuring its spin period (13.497 ± 0.005 s) in the 20-40 keV band. As it was in a soft state during the first observation and possibly in an extremely low state in the second one, LMC X-3 was not detected. Thanks to the large field of view of the IBIS instrument, we could also study other sources falling serendipitously in the observed sky region around the LMC: the Galactic low mass X-ray binary EXO 0748-676, the accreting pulsar SMC X-1 in the Small Magellanic Cloud, and the Active Galactic Nucleus IRAS 04575-7537. In addition we discovered five new hard X-ray sources, two of which most likely belong to the LMC.

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“…Most studies have been conducted in the soft X-ray band by ROSAT and more recently by Chandra and XMM-Newton (Fox et al 2000;Kulkarni & Fox 2003;Schlegel 2002;Zimmermann & Aschenbach 2003). Information at harder energies is much more limited: only SNe 1987A, 1993J and 1998bw have been investigated at energies higher than 13 keV, and only the first two have been detected (Sunyaev et al 1987;Inoue et al 1991;Leising et al 1994). SN 2002ap in M 74 (NGC 628) is one of only four type Ic SNe detected in the X-rays, the others being the low-mass, normally energetic SN 1994I (Immler et al 1998;, the massive and energetic "hypernova" SN 1998bw…”

Section: Introductionmentioning

confidence: 99%

A second glance at SN 2002ap and the M 74 field withXMM-Newton

Soria¹,

Pian²,

Mazzali³

2003

A&A

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Abstract.We have re-observed the field of M 74 in January 2003 with XMM-Newton, 11 months after the X-ray detection of SN 2002ap. From a comparison of the two XMM-Newton observations we obtain more accurate values for the X-ray luminosity and colours of the source five days after the event, and a limit on its decline rate. We compare its X-ray behaviour (prompt soft Xray emission, relatively low luminosity) with that of other type Ic SNe, and speculate that SN 2002ap may share some physical properties (low mass-loss rate and high-velocity stellar wind from the progenitor star) with the candidate hypernova/gammaray-burst progenitor SN 1998bw, but with a lower (non-relativistic) speed of the ejecta. We suggest that the X-ray emission observed in 2002 is likely to come from the radiatively-cooling reverse shock, at a temperature kT ≈ 0.8 keV, and that this soft component was already detected 5 d after the event because the absorbing column density of the cool shell between the forward and reverse shocks was only ∼10 20 cm −2 , i.e., the shell was optically thin in the soft X-ray band. The new XMM-Newton data also allowed us to continue monitoring two bright variable sources in M 74 that had reached peak luminosities >10 39 erg s −1 in previous XMM-Newton and Chandra observations. Finally, we used two Chandra observations from 2001 to investigate the luminosity and colour distribution of the X-ray source population of M 74, typical of moderately-active late-type spirals.

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Discovery of hard X-ray emission from supernova 1987A

Cited by 167 publications

References 0 publications

Supernova 1987 A

Supernova 1987 A

An INTEGRAL hard X-ray survey of the Large Magellanic Cloud

A second glance at SN 2002ap and the M 74 field withXMM-Newton

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