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Title: CHANDRA DETECTION OF SN 2010da FOUR MONTHS AFTER OUTBURST: EVIDENCE FOR A HIGH-MASS X-RAY BINARY IN NGC 300

Abstract

We present the results of a 63 ks Chandra observation of the 'supernova impostor' SN 2010da four months after it was first observed on 2010 May 24. We detect an X-ray source at {approx}7{sigma} confidence coincident with the optical location of the outburst. Our imaging analysis has revealed a hard central point source, surrounded by soft diffuse emission extending {approx}8'' north of the central source. The diffuse emission has a hardness ratio ({approx}-0.4), 0.35-2 keV luminosity ({approx}6 x 10{sup 35} erg s{sup -1}), and size ({approx}70 pc) consistent with that of a supernova remnant, although the low number of counts prohibits detailed spectral modeling. The 0.5-6 keV spectrum of the central point source is well described by both a power law with {Gamma} {approx}0 and a blackbody with kT {approx} 1.8 keV, with no evidence for intrinsic absorption beyond the Galactic column. We estimate the 0.3-10 keV luminosity to be {approx}2 x 10{sup 37} erg s{sup -1}, a factor of {approx}25 decrease since the initial outburst. The high X-ray luminosity and slow fading rate is not consistent with this object being a single massive star undergoing an outburst. When combined with the optical and infrared properties of the outburst andmore » progenitor systems, our X-ray observations suggest the SN 2010da system may be a Be X-ray binary system which experienced an extremely bright optical outburst near simultaneously with a bright, Type II X-ray outburst.« less

Authors:
; ; ;  [1];  [2]; ;  [3]
  1. Department of Astronomy, University of Washington, Seattle, WA 98195 (United States)
  2. Institute of Astronomy and Department of Physics, National Tsing Hua University, Hsinchu 30013, Taiwan (China)
  3. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138 (United States)
Publication Date:
OSTI Identifier:
21565427
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal Letters
Additional Journal Information:
Journal Volume: 739; Journal Issue: 2; Other Information: DOI: 10.1088/2041-8205/739/2/L51; Journal ID: ISSN 2041-8205
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; EMISSION; LUMINOSITY; POINT SOURCES; SUPERNOVA REMNANTS; SUPERNOVAE; X RADIATION; X-RAY SOURCES; BINARY STARS; COSMIC RADIO SOURCES; ELECTROMAGNETIC RADIATION; ERUPTIVE VARIABLE STARS; IONIZING RADIATIONS; OPTICAL PROPERTIES; PHYSICAL PROPERTIES; RADIATION SOURCES; RADIATIONS; STARS; VARIABLE STARS

Citation Formats

Binder, B., Williams, B. F., Dalcanton, J. J., Weisz, D. R., Kong, A. K. H., Gaetz, T. J., and Plucinsky, P. P. CHANDRA DETECTION OF SN 2010da FOUR MONTHS AFTER OUTBURST: EVIDENCE FOR A HIGH-MASS X-RAY BINARY IN NGC 300. United States: N. p., 2011. Web. doi:10.1088/2041-8205/739/2/L51.
Binder, B., Williams, B. F., Dalcanton, J. J., Weisz, D. R., Kong, A. K. H., Gaetz, T. J., & Plucinsky, P. P. CHANDRA DETECTION OF SN 2010da FOUR MONTHS AFTER OUTBURST: EVIDENCE FOR A HIGH-MASS X-RAY BINARY IN NGC 300. United States. doi:10.1088/2041-8205/739/2/L51.
Binder, B., Williams, B. F., Dalcanton, J. J., Weisz, D. R., Kong, A. K. H., Gaetz, T. J., and Plucinsky, P. P. Sat . "CHANDRA DETECTION OF SN 2010da FOUR MONTHS AFTER OUTBURST: EVIDENCE FOR A HIGH-MASS X-RAY BINARY IN NGC 300". United States. doi:10.1088/2041-8205/739/2/L51.
@article{osti_21565427,
title = {CHANDRA DETECTION OF SN 2010da FOUR MONTHS AFTER OUTBURST: EVIDENCE FOR A HIGH-MASS X-RAY BINARY IN NGC 300},
author = {Binder, B. and Williams, B. F. and Dalcanton, J. J. and Weisz, D. R. and Kong, A. K. H. and Gaetz, T. J. and Plucinsky, P. P.},
abstractNote = {We present the results of a 63 ks Chandra observation of the 'supernova impostor' SN 2010da four months after it was first observed on 2010 May 24. We detect an X-ray source at {approx}7{sigma} confidence coincident with the optical location of the outburst. Our imaging analysis has revealed a hard central point source, surrounded by soft diffuse emission extending {approx}8'' north of the central source. The diffuse emission has a hardness ratio ({approx}-0.4), 0.35-2 keV luminosity ({approx}6 x 10{sup 35} erg s{sup -1}), and size ({approx}70 pc) consistent with that of a supernova remnant, although the low number of counts prohibits detailed spectral modeling. The 0.5-6 keV spectrum of the central point source is well described by both a power law with {Gamma} {approx}0 and a blackbody with kT {approx} 1.8 keV, with no evidence for intrinsic absorption beyond the Galactic column. We estimate the 0.3-10 keV luminosity to be {approx}2 x 10{sup 37} erg s{sup -1}, a factor of {approx}25 decrease since the initial outburst. The high X-ray luminosity and slow fading rate is not consistent with this object being a single massive star undergoing an outburst. When combined with the optical and infrared properties of the outburst and progenitor systems, our X-ray observations suggest the SN 2010da system may be a Be X-ray binary system which experienced an extremely bright optical outburst near simultaneously with a bright, Type II X-ray outburst.},
doi = {10.1088/2041-8205/739/2/L51},
journal = {Astrophysical Journal Letters},
issn = {2041-8205},
number = 2,
volume = 739,
place = {United States},
year = {2011},
month = {10}
}