The ultraluminous X-ray source in M82: an intermediate-mass black hole with a giant companion

Patruno, A.; Zwart, Simon F. Portegies; Dewi, Jasinta; Hopman, Clovis

doi:10.1111/j.1745-3933.2006.00176.x

Cited by 49 publications

(44 citation statements)

References 34 publications

(56 reference statements)

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“…Other authors have suggested that ULXs may be due to IMBHs accreting from captured stellar companions rather than molecular clouds ( Pooley & Rappaport 2005;Patruno et al 2006;Madhusudhan et al 2006). In this case, the ULXs would ''turn on'' when residing in dense star clusters.…”

Section: Pbhs As Ulxsmentioning

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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Section: Pbhs As Ulxsmentioning

confidence: 99%

Growth of Structure Seeded by Primordial Black Holes

Mack

Ostriker

Ricotti

2007

ApJ

157

187

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“…The HCN and HCO + data are in good agreement with previous measurements (e.g., Nguyen et al 1992). The gas disk in M82 is known to house two giant photodissociation regions (PDRs; e.g., García-Burillo et al 2002) and probably also a central massive black hole in formation (e.g., Matsushita et al 2000;Patruno et al 2006) and a superbubble emerging from a past SNE (e.g., Wei% et al 1999;Kronberg et al 1985). A different gas chemistry could hence be at play in the center than in the two PDRs.…”

Section: M82: Sb-dominated Galaxymentioning

confidence: 99%

A Multi‐Transition HCN and HCO⁺Study of 12 Nearby Active Galaxies: Active Galactic Nucleus versus Starburst Environments

Krips

Neri

García‐Burillo

et al. 2008

ApJ

250

377

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Recent studies have indicated that the HCN-to-CO(J ¼ 1Y0) and HCO + -to-HCN(J ¼ 1Y0) ratios are significantly different between galaxies with AGN (active galactic nucleus) and SB (starburst) signatures. In order to study the molecular gas properties in active galaxies and search for differences between AGN and SB environments, we observed the, and HCO + (J ¼ 3Y2) emission with the IRAM 30 m in the center of 12 nearby active galaxies which either exhibit nuclear SB and/or AGN signatures. Consistent with previous results, we find a significant difference of the HCN(, and HCO + -to-HCN intensity ratios between the sources dominated by an AGN and those with an additional or pure central SB: the HCN, HCO + , and HCO + -to-HCN intensity ratios tend to be higher in the galaxies of our sample with a central SB as opposed to the pure AGN cases, which show rather low intensity ratios. Based on an LVG analysis of these data, i.e., assuming purely collisional excitation, the (average) molecular gas densities in the SB-dominated sources of our sample seem to be systematically higher than in the AGN sources. The LVG analysis seems to further support systematically higher HCN and/or lower HCO + abundances as well as similar or higher gas temperatures in AGNs compared to the SB sources of our sample. In addition, we find that the HCN-to-CO ratios decrease with increasing rotational number J for the AGNs while they stay mostly constant for the SB sources.

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“…M82 X-1's previous mass estimates of a few hundred solar masses combined with the Type-C identification 2,4,9 of its mHz X-ray quasi-periodic oscillations suggest that 3:2 ratio, twin-peak, high-frequency oscillations analogous to those seen in stellar-mass black holes, if present, should be detectable in the frequency range of a few Hz 16 . We accordingly searched Rossi X-ray Timing Explorer's (RXTE's) proportional counter array archival data to look for 3:2 oscillation pairs in the frequency range of [1][2][3][4][5][6][7][8][9][10][11][12][13][14][15][16] Hz which corresponds to a black hole mass range of 50-2000 M ⊙ .…”

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confidence: 99%

A 400-solar-mass black hole in the galaxy M82

Pasham

Strohmayer

Mushotzky

2014

Nature

199

197

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The brightest X-ray source in M82 has been thought to be an intermediatemass black hole (10 2−4 solar masses, M ⊙ ) because of its extremely high luminosity and variability characteristics 1−6 , although some models suggest that its mass may be only ∼ 20 M ⊙ 3,7 . The previous mass estimates are based on scaling relations which use low-frequency characteristic timescales which have large intrinsic uncertainties 8,9 . In stellar-mass black holes we know that the high frequency quasi-periodic oscillations that occur in a 3:2 ratio (100-450 Hz) are stable and scale inversely with black hole mass with a reasonably small dispersion 10−15 . The discovery of such stable oscillations thus potentially offers an alternative and less ambiguous mass determination for intermediate-mass black holes, but has hitherto not been realized. Here, we report stable, twin-peak (3:2 frequency ratio) X-ray quasi-periodic oscillations from M82 X-1 at the frequencies of 3.32±0.06Hz and 5.07±0.06 Hz. Assuming that we can scale the stellar-mass relationship, we estimate its black hole mass to be 428±105 M ⊙ . In addition, we can estimate the mass using the relativistic precession model, from which we get a value ofOscillations arising from general relativistic effects should scale inversely with the black hole mass if they arise from orbital motion near the innermost stable circular orbit in the We detected two power spectral peaks at 3.32±0.06 Hz (coherence, Q = centroid frequency (ν)/width(∆ν) > 27) and 5.07±0.06 Hz (Q > 40) consistent with a 3:2 frequency ratio ( Fig. 1a, b). The combined statistical significance of the detection is greater than 4.7σ (see Methods for details).The proportional counter array's field of view (1 • ×1 • ) of M82 includes a number of accreting X-ray sources in addition to M82 X-1 18 . The remarkable stability of the two quasiperiodic oscillations on timescales of a few years (Movies 1 & 2), their 3:2 frequency ratio and their high oscillation luminosities strongly suggest they are not low-frequency quasi-periodic oscillations from a contaminating stellar-mass black hole (see Methods for details). Also a pulsar origin is very unlikely for several reasons. First, a pulsar signal would be much more coherent than that of the observed quasi-periodic oscillations, which clearly have a finite width. Second, based on the observed high quasi-periodic oscillation luminosities it is extremely implausible that they originate from a pulsar (see Methods for details). Finally, it would be highly coincidental to have two pulsars in the same field of view with spins in the 3:2 ratio. Also, based on the average power spectra of the background sky and a sample of accreting super-massive black holes monitored by the proportional counter array in the same epoch as M82, we rule out an instrumental origin for these oscillations 3 & 4). This leaves M82 X-1, persistently the brightest source in the field of view, as the most likely source associated with the 3:2 ratio quasi-periodic oscillation pair.We estimated M82 X-1's black hole ...

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The ultraluminous X-ray source in M82: an intermediate-mass black hole with a giant companion

Cited by 49 publications

References 34 publications

Growth of Structure Seeded by Primordial Black Holes

Growth of Structure Seeded by Primordial Black Holes

A Multi‐Transition HCN and HCO⁺Study of 12 Nearby Active Galaxies: Active Galactic Nucleus versus Starburst Environments

A 400-solar-mass black hole in the galaxy M82

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The ultraluminous X-ray source in M82: an intermediate-mass black hole with a giant companion

Cited by 49 publications

References 34 publications

Growth of Structure Seeded by Primordial Black Holes

Growth of Structure Seeded by Primordial Black Holes

A Multi‐Transition HCN and HCO+Study of 12 Nearby Active Galaxies: Active Galactic Nucleus versus Starburst Environments

A 400-solar-mass black hole in the galaxy M82

Contact Info

Product

Resources

About

A Multi‐Transition HCN and HCO⁺Study of 12 Nearby Active Galaxies: Active Galactic Nucleus versus Starburst Environments