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Ultraluminous X-ray Source 1E 0953.8+6918 (M81 X-9): An Intermediate Mass Black Hole Candidate and its Environs | | Q. Daniel Wang
; | | Date: |
15 Dec 2001 | | Journal: | Mon.Not.Roy.Astron.Soc. 332 (2002) 764 | | Subject: | astro-ph | | Abstract: | We present a ROSAT and ASCA study of the Einstein source X-9 and its relation to a shock-heated shell-like optical nebula in a tidal arm of the M81 group of interacting galaxies. Our ASCA observation of the source shows a flat and featureless X-ray spectrum well described by a multi-color disk blackbody model. The source most likely represents an optically thick accretion disk around an intermediate mass black hole in its high/soft state, similar to other variable ultraluminous X-ray sources observed in nearby disk galaxies. Using constraints derived from both the innermost stable orbit around a black hole and the Eddington luminosity, we find that the black hole is fast-rotating and that its mass is between $sim 20/({
m cos} i) {
m M}_{odot} - 110/({
m cos} i)^{1/2} {
m M}_{odot}$, where $i$ is the inclination angle of the disk. The inferred bolometric luminosity of the accretion disk is $sim (8 imes 10^{39} {
m ergs s^{-1}})/({
m cos} i)^{1/2}$. Furthermore, we find that the optical nebula is very energetic and may contain large amounts of hot gas, accounting for a soft X-ray component as indicated by archival ROSAT PSPC data. The nebula is apparently associated with X-9; the latter may be powering the former and/or they could be formed in the same event (e.g., a hypernova). Such a connection, if confirmed, could have strong implications for understanding both the birth of intermediate mass black holes and the formation of energetic interstellar structures. | | Source: | arXiv, astro-ph/0201230 | | Services: | Forum | Review | PDF | Favorites | |
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