A variable Quasi-Periodic Oscillation in M82 X-1. Timing and spectral analysis of XMM–Newton and RossiXTE observations |
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| Authors: | P Mucciarelli P Casella T Belloni L Zampieri P Ranalli |
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| Institution: | INAF –Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italy;Dipartimento di Astronomia, Universitàdi Padova, Vicolo dell'Osservatorio 2, I-35122 Padova, Italy;INAF –Osservatorio Astronomico di Brera, Via E. Bianchi 46, I-23807 Merate (LC), Italy;INAF –Osservatorio Astronomico di Bologna, Via Ranzani 1, I-40127 Bologna, Italy |
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| Abstract: | We report results from a spectral and timing analysis of M82 X-1, one of the brightest known ultraluminous X-ray sources. Data from a new 105-ks XMM–Newton observation of M82 X-1, performed in 2004 April, and of archival RossiXTE observations are presented. A very soft thermal component is present in the XMM spectrum. Although it is not possible to rule out a residual contamination from the host galaxy, modelling it with a standard accretion disc would imply a black hole (BH) mass of ≈103 M⊙ . An emission line was also detected at an energy typical for fluorescent Fe emission. The power density spectrum of the XMM observation shows a variable Quasi-Periodic Oscillation (QPO) at frequency of 113 mHz with properties similar to those discovered by Strohmayer and Mushotzky. The QPO was also found in seven archival RXTE observations, that include those analysed by Strohmayer and Mushotzky, and Fiorito and Titarchuk. A comparison of the properties of this QPO with those of the various types of QPOs observed in Galactic black hole candidates strongly suggests an association with the type-C, low-frequency QPOs. Scaling the frequency inversely to the BH mass, the observed QPO frequency range (from 50 to 166 mHz) would yield a BH mass anywhere in the interval few tens to 1000 M⊙ . |
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| Keywords: | stars: oscillations galaxies: individual: M82 X-rays: binaries X-rays: individual: M82 X-1 X-rays: stars |
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