Discovery of X-ray QPOs from an Ultra-luminous X-ray Source in M82: Evidence Against Beaming

Details Discovery of X-ray QPOs from an Ultra-luminous X-ray Source in M82: Evidence Against Beaming Discovery of X-ray QPOs from an Ultra-luminous X-ray Source in M82: Evidence Against Beaming

2003-03-31

arxiv.org/abs/astro-ph/0303665v1

Astronomy and Astrophysics

Astrophysics

20 pages, 4 figures, AASTeX. A shortened version has been published in the Astrophysical Journal Letters (2003, 586, L61)

Scientific paper

10.1086/374732

We report the discovery with the EPIC CCD cameras onboard XMM-Newton of a 54 mHz quasiperiodic oscillation (QPO) in the > 2 keV X-ray flux from an ultraluminous X-ray source (ULX) in the starburst galaxy M82. This is the first detection of a QPO in the X-ray flux from an extra-Galactic ULX, and confirms that the source is a compact object. Based on the QPO strength and previous Chandra observations it appears likely that the QPO is associated with the most luminous object in the central region of M82, CXOM82 J095550.2+694047, however, XMM imaging alone is not sufficient to unambiguously confirm this. The other plausible candidate is CXOM82 J095551.1+694045, however, the QPO luminosity is comparable to the peak luminosity of this object in Chandra observations, which argues against it being the source of the QPO. The QPO had a centroid frequency of 54.3 +- 0.9 mHz, a coherence of 5, and an amplitude (rms) in the 2 - 10 keV band of 8.5%. Below 0.2 Hz the power spectrum can be described by a power-law with index ~1, and amplitude (rms) of 13.5%. The X-ray spectrum requires a curving continuum, with a disk-blackbody (diskbb) at T = 3.1 keV providing an acceptable fit. A broad Fe line centered at 6.55 keV is required in all fits, but the equivalent width (EW) is sensitive to the continuum model. There is no evidence of a reflection component. The implied bolometric luminosity is 4 - 5 x 10^{40} ergs/sec. Archival Rossi X-ray Timing Explorer (RXTE) pointings at M82 also show evidence for QPOs in the 50 - 100 mHz frequency range. We discuss the implications of our findings for models of ULXs.

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