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Article: Limits from the Hubble space telescope on a point source in SN 1987A

TitleLimits from the Hubble space telescope on a point source in SN 1987A
Authors
KeywordsAccretion, Accretion Disks
Stars: Neutron
Supernovae: Individual (Sn 1987A)
Issue Date2005
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2005, v. 629 n. 2 I, p. 944-959 How to Cite?
AbstractWe observed supernova 1987A (SN 1987A) with the Space Telescope Imaging Spectrograph (STIS) on the Hubble Space Telescope (HST) in 1999 September and again with the Advanced Camera for Surveys (ACS) on the HST in 2003 November. Our spectral observations cover ultraviolet (UV) and optical wavelengths from 1140 to 10266 Å, and our imaging observations cover UV and optical wavelengths from 2900 to 9650 Å. No point source is observed in the remnant. We obtain a limiting flux of F opt ≤ 1.6 × 10 -14 ergs s -1 cm -2 in the wavelength range 2900-9650 Å for any continuum emitter at the center of the supernova remnant (SNR). This corresponds to an intrinsic luminosity of L opt ≤ 5 × 10 33 ergs s -1. It is likely that the SNR contains opaque dust that absorbs UV and optical emission, resulting in an attenuation of ∼35% due to dust absorption in the SNR. Correcting for this level of dust absorption would increase our upper limit on the luminosity of a continuum source by a factor of 1.54. Taking into account dust absorption in the remnant, we find a limit of L opt ≤ 8 × 10 33 ergs s -1. We compare this upper bound with empirical evidence from point sources in other supernova remnants and with theoretical models for possible compact sources. We show that any survivor of a possible binary system must be no more luminous than an F6 main-sequence star. Bright young pulsars such as Kes 75 or the Crab pulsar are excluded by optical and X-ray limits on SN 1987A. Other nonplerionic X-ray point sources have luminosities similar to the limits on a point source in SN 1987 A; RCW 103 and Cas A are slightly brighter than the limits on SN 1987A, while Pup A is slightly fainter. Of the young pulsars known to be associated with SNRs, those with ages ≤5000 yr are all too bright in X-rays to be compatible with the limits on SN 1987A. Examining theoretical models for accretion onto a compact object, we find that spherical accretion onto a neutron star is firmly ruled out and that spherical accretion onto a black hole is possible only if there is a larger amount of dust absorption in the remnant than predicted. In the case of thin-disk accretion, our flux limit requires a small disk, no larger than 10 10 cm, with an accretion rate no more than 0.3 times the Eddington accretion rate. Possible ways to hide a surviving compact object include the removal of all surrounding material at early times by a photon-driven wind, a small accretion disk, or very high levels of dust absorption in the remnant. It will not be easy to improve substantially on our optical-UV limit for a point source in SN 1987A, although we can hope that a better understanding of the thermal infrared emission will provide a more complete picture of the possible energy sources at the center of SN 1987 A. © 2005. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/174965
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorGraves, GJMen_US
dc.contributor.authorChallis, PMen_US
dc.contributor.authorChevalier, RAen_US
dc.contributor.authorCrotts, Aen_US
dc.contributor.authorFilippenko, AVen_US
dc.contributor.authorFransson, Cen_US
dc.contributor.authorGarnavich, Pen_US
dc.contributor.authorKirshner, RPen_US
dc.contributor.authorLi, Wen_US
dc.contributor.authorLundqvist, Pen_US
dc.contributor.authorMccray, Ren_US
dc.contributor.authorPanagia, Nen_US
dc.contributor.authorPhillips, MMen_US
dc.contributor.authorPun, CJSen_US
dc.contributor.authorSchmidt, BPen_US
dc.contributor.authorSonneborn, Gen_US
dc.contributor.authorSuntzeff, NBen_US
dc.contributor.authorWang, Len_US
dc.contributor.authorWheeler, JCen_US
dc.date.accessioned2012-11-26T08:48:24Z-
dc.date.available2012-11-26T08:48:24Z-
dc.date.issued2005en_US
dc.identifier.citationAstrophysical Journal Letters, 2005, v. 629 n. 2 I, p. 944-959en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/174965-
dc.description.abstractWe observed supernova 1987A (SN 1987A) with the Space Telescope Imaging Spectrograph (STIS) on the Hubble Space Telescope (HST) in 1999 September and again with the Advanced Camera for Surveys (ACS) on the HST in 2003 November. Our spectral observations cover ultraviolet (UV) and optical wavelengths from 1140 to 10266 Å, and our imaging observations cover UV and optical wavelengths from 2900 to 9650 Å. No point source is observed in the remnant. We obtain a limiting flux of F opt ≤ 1.6 × 10 -14 ergs s -1 cm -2 in the wavelength range 2900-9650 Å for any continuum emitter at the center of the supernova remnant (SNR). This corresponds to an intrinsic luminosity of L opt ≤ 5 × 10 33 ergs s -1. It is likely that the SNR contains opaque dust that absorbs UV and optical emission, resulting in an attenuation of ∼35% due to dust absorption in the SNR. Correcting for this level of dust absorption would increase our upper limit on the luminosity of a continuum source by a factor of 1.54. Taking into account dust absorption in the remnant, we find a limit of L opt ≤ 8 × 10 33 ergs s -1. We compare this upper bound with empirical evidence from point sources in other supernova remnants and with theoretical models for possible compact sources. We show that any survivor of a possible binary system must be no more luminous than an F6 main-sequence star. Bright young pulsars such as Kes 75 or the Crab pulsar are excluded by optical and X-ray limits on SN 1987A. Other nonplerionic X-ray point sources have luminosities similar to the limits on a point source in SN 1987 A; RCW 103 and Cas A are slightly brighter than the limits on SN 1987A, while Pup A is slightly fainter. Of the young pulsars known to be associated with SNRs, those with ages ≤5000 yr are all too bright in X-rays to be compatible with the limits on SN 1987A. Examining theoretical models for accretion onto a compact object, we find that spherical accretion onto a neutron star is firmly ruled out and that spherical accretion onto a black hole is possible only if there is a larger amount of dust absorption in the remnant than predicted. In the case of thin-disk accretion, our flux limit requires a small disk, no larger than 10 10 cm, with an accretion rate no more than 0.3 times the Eddington accretion rate. Possible ways to hide a surviving compact object include the removal of all surrounding material at early times by a photon-driven wind, a small accretion disk, or very high levels of dust absorption in the remnant. It will not be easy to improve substantially on our optical-UV limit for a point source in SN 1987A, although we can hope that a better understanding of the thermal infrared emission will provide a more complete picture of the possible energy sources at the center of SN 1987 A. © 2005. The American Astronomical Society. All rights reserved.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_US
dc.relation.ispartofAstrophysical Journal Lettersen_US
dc.subjectAccretion, Accretion Disksen_US
dc.subjectStars: Neutronen_US
dc.subjectSupernovae: Individual (Sn 1987A)en_US
dc.titleLimits from the Hubble space telescope on a point source in SN 1987Aen_US
dc.typeArticleen_US
dc.identifier.emailPun, CJS: jcspun@hkucc.hku.hken_US
dc.identifier.authorityPun, CJS=rp00772en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1086/431422en_US
dc.identifier.scopuseid_2-s2.0-25444498035en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-25444498035&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume629en_US
dc.identifier.issue2 Ien_US
dc.identifier.spage944en_US
dc.identifier.epage959en_US
dc.identifier.isiWOS:000231159500032-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridGraves, GJM=23967732800en_US
dc.identifier.scopusauthoridChallis, PM=7004555495en_US
dc.identifier.scopusauthoridChevalier, RA=7101871369en_US
dc.identifier.scopusauthoridCrotts, A=7003353108en_US
dc.identifier.scopusauthoridFilippenko, AV=34568722000en_US
dc.identifier.scopusauthoridFransson, C=7004051800en_US
dc.identifier.scopusauthoridGarnavich, P=7006524172en_US
dc.identifier.scopusauthoridKirshner, RP=35277140000en_US
dc.identifier.scopusauthoridLi, W=23993021700en_US
dc.identifier.scopusauthoridLundqvist, P=7004499555en_US
dc.identifier.scopusauthoridMcCray, R=35954431900en_US
dc.identifier.scopusauthoridPanagia, N=35400629400en_US
dc.identifier.scopusauthoridPhillips, MM=7402770160en_US
dc.identifier.scopusauthoridPun, CJS=7003931846en_US
dc.identifier.scopusauthoridSchmidt, BP=7402828523en_US
dc.identifier.scopusauthoridSonneborn, G=7006137500en_US
dc.identifier.scopusauthoridSuntzeff, NB=7006255654en_US
dc.identifier.scopusauthoridWang, L=7409176960en_US
dc.identifier.scopusauthoridWheeler, JC=7403110438en_US

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