Black Hole Mass of the Ultraluminous X-Ray Source M82 X-1

Dewangan, G. C.; Titarchuk, Lev; Griffiths, R. E.

doi:10.1086/499235

Cited by 95 publications

(115 citation statements)

References 27 publications

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“…Dewangan et al (2006a) used this proportionality for ULX X-1 in M82 and found the mass of the BH to be in the range of (25−520)M ⊙ . We used the same scaling argument to approximate the mass of the BH in X-2 of NGC 4736.…”

Section: Discussion and Summarymentioning

confidence: 99%

A search for periodicities from a ULX in the LINER galaxy NGC 4736

Avdan

Akyüz

et al. 2014

Astrophys Space Sci

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We report our findings on a new quasi-periodic oscillation (QPO) and a long period from the ultraluminous X-ray source (ULX) X-2 in nearby galaxy NGC 4736 based on the Chandra and XMM-Newton archival data. To examine the timing properties, power density spectra of the source have been obtained using Fast Fourier Transform. Also the spectral parameters of the source have been calculated by obtaining and fitting the energy spectra. Power density spectrum of this source reveals a QPO peak at 0.73 +0.16 −0.14 mHz with an fractional rms variability of 16% using the Chandra data (in the year 2000-lower state of the source). The XMM-Newton data analysis indicates a peak at 0.53 +0.09 −0.35 mHz with a fractional rms variation of 5% (in the year 2006-higher state of the source). These recovered QPOs overlap within errors and may be the same oscillation. In addition, we detect a long periodicity or a QPO in the Chandra data of about (5.2 ± 2.0) × 10 −5 Hz (∼ 5.4 hrs) over 3 σ confidence level. If this is a QPO, it is the lowest QPO detected from a ULX. The mass of the compact object in ULX X-2 is estimated using the Eddington luminosity and a disk blackbody model in the range (10−80) M ⊙ .

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Section: Discussion and Summarymentioning

confidence: 99%

A search for periodicities from a ULX in the LINER galaxy NGC 4736

Avdan

Akyüz

et al. 2014

Astrophys Space Sci

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“…Their X-ray luminosities (Colbert & Mushotzky 1999;Kaaret et al 2001), thermal disk emissions (Kaaret et al 2003), variation timescales (Strohmayer & Mushotzky 2003;Dewangan et al 2006), and surrounding emission-line nebulae (Pakull & Mirioni 2003;Kaaret et al 2004b) suggest that they might have masses of 20-10 3 , falling into the class of intermediate-mass black M , holes (IMBHs). However, if the emission is beamed (King et al 2001;Körding et al 2002) or exceeds the Eddington limit (Begelman 2002;Ebisawa et al 2003), some or all ULXs may be stellar-mass black holes.…”

Section: Fabbiano and White 2006) Many Ulxs Show Strong Variabilitymentioning

confidence: 99%

Spectral State Transitions of the Ultraluminous X-Ray Sources X-1 and X-2 in NGC 1313

Feng

Kaaret

2006

ApJ

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X-ray spectral state transitions are a key signature of black hole X-ray binaries and follow a well-defined pattern. We examined 12 XMM-Newton observations of the nearby spiral galaxy NGC 1313, which harbors two compact ultraluminous X-ray sources (ULXs), X-1 and X-2, in order to determine if the state transitions in ULXs follow the same pattern. For both sources, the spectra were adequately fitted by an absorbed power law with the addition of a low-temperature ( keV) disk blackbody component required in six of the 12 obserkT p 0.1-0.3 vations. As the X-ray luminosity of X-1 increases to a maximum at ergs s Ϫ1 , the power-law photon 40 3 # 10 index softens to 2.5-3.0. This behavior is similar to the canonical spectral state transitions in Galactic black hole binaries, but the source never enters the high/soft or thermal-dominant state and instead enters the steep powerlaw state at high luminosities. X-2 has the opposite behavior and appears to be in the hard state, with a photon index of at high luminosity, but can soften to at the lower luminosities. G p 1.7-2.0 G p 2.5

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“…If PBHs can grow sufficiently by accretion (or if they are very large at birth), they may account for intermediate-mass black holes (IMBHs) in the mass range 10 2 M P M P10 4 M , which have been suggested as the engines behind ultraluminous X-ray sources (ULXs) recently discovered in nearby galactic disks (Dewangan et al 2006;Madhusudhan et al 2006;Miller 2005;Mushotzky 2004). On the basis of the observed ULX luminosities of $10 39 erg s À1 , stellar-mass black holes are ruled out unless the emission is highly beamed; there is at present no evidence for beaming (Mushotzky 2004;Freeland et al 2006;Poutanen et al 2007;Miniutti et al 2006).…”

Section: Introductionmentioning

confidence: 99%

Growth of Structure Seeded by Primordial Black Holes

Mack

Ostriker

Ricotti

2007

ApJ

157

187

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We discuss the possibilities for the growth of primordial black holes (PBHs) via the accretion of dark matter. In agreement with previous works, we find that accretion during the radiation-dominated era does not lead to a significant mass increase. However, during matter domination, PBHs may grow by up to 2 orders of magnitude in mass through the acquisition of large dark matter halos. We discuss the possibility of PBHs being an important component in dark matter halos of galaxies, as well as their potential to explain the ultraluminous X-ray sources (ULXs) observed in nearby galactic disks. We point out that although PBHs are ruled out as the dominant component of dark matter, there is still a great deal of parameter space that is open to their playing a role in the modern-day universe. For example, a primordial halo population of PBHs each at 10 2.5 M , making up 0.1% of the dark matter, grows to 10 4.5 M via the accumulation of dark matter halos and accounts for $10% of the dark matter mass by a redshift of z % 30. These intermediate-mass black holes may then ''light up'' when passing through molecular clouds, becoming visible as ULXs at the present day, or they may form the seeds for supermassive black holes at the centers of galaxies.

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Black Hole Mass of the Ultraluminous X-Ray Source M82 X-1

Cited by 95 publications

References 27 publications

A search for periodicities from a ULX in the LINER galaxy NGC 4736

A search for periodicities from a ULX in the LINER galaxy NGC 4736

Spectral State Transitions of the Ultraluminous X-Ray Sources X-1 and X-2 in NGC 1313

Growth of Structure Seeded by Primordial Black Holes

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