<i>XMM‐Newton</i>Spectra of Intermediate‐Mass Black Hole Candidates: Application of a Monte Carlo Simulated Model

Wang, Q. Daniel; Yao, Yangsen; Fukui, Wakako; Zhang, Shuang‐Nan; Williams, R. M.

doi:10.1086/420970

Cited by 29 publications

(32 citation statements)

References 41 publications

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“…(2003) found their photon indices to be in the range 0:6 < À PSR < 2:1 (while their associated pulsar wind nebulae had 1:3 < À PSR < 2:3). It should be noted that several ULXs have power-law spectral components consistent with this range of values (Wang et al 2004). Pulsations might be detected with high time resolution, high-throughput X-ray light curves of ULXs.…”

Section: Observv Ational Diagg Nostics Of the Younggpulsar Populationsupporting

confidence: 70%

Young Crab‐like Pulsars and Luminous X‐Ray Sources in Starbursts and Optically Dull Galaxies

Perna

Stella

2004

ApJ

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Recent Chandra observations of nearby galaxies have revealed a number of ultraluminous X-ray sources (ULXs) with super-Eddington luminosities, away from the central regions of nonactive galaxies. The nature of these sources is still debated. We argue that a fraction of them could be young, Crab-like pulsars, the X-ray luminosity of which is powered by rotation. We use the pulsar birth parameters estimated from radio pulsar data to compute the steady state pulsar X-ray luminosity distribution as a function of the star formation rate (SFR) in the galaxy. We find that $10% of optically dull galaxies are expected to have a source with L X k 10 39 ergs s À1 , while starburst galaxies should each have several of these sources. We estimate that the X-ray luminosity of a few percent of galaxies is dominated by a single bright pulsar with L X k 10 39 ergs s À1 , roughly independently of its SFR. We discuss observational diagnostics that can help distinguish the young pulsar population in ULXs.

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Section: Observv Ational Diagg Nostics Of the Younggpulsar Populationsupporting

confidence: 70%

Young Crab‐like Pulsars and Luminous X‐Ray Sources in Starbursts and Optically Dull Galaxies

Perna

Stella

2004

ApJ

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“…This effect vanishes at higher energies and above 1.0 keV a central point source appears. Actually, the X-ray emitter close to the nucleus is the strongest source throughout all energy bands and is most likely a variable high mass X-ray binary (Dahlem et al 1995a;Wang et al 2004).…”

Section: Ngc 3628mentioning

confidence: 99%

The multi-phase gaseous halos of star forming late-type galaxies

Tüllmann

Pietsch²,

Rossa³

et al. 2006

A&A

150

175

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This study presents first results from an X-ray mini-survey carried out with XMM-Newton to investigate the diffuse Hot Ionized Medium in the halos of nine nearby star-forming edge-on spiral galaxies. Diffuse gaseous X-ray halos are detected in eight of our targets, covering a wide range of star formation rates from quiescent to starburst cases. For four edge-on spiral galaxies, namely NGC 3044, NGC 3221, NGC 4634, and NGC 5775, we present the first published high resolution/sensitivity detections of extended soft X-ray halos. EPIC X-ray contour maps overlaid onto Hα imaging data reveals that in all cases the presence of X-ray halos is correlated with extraplanar Diffuse Ionized Gas. Moreover, these halos are also associated with non-thermal cosmic ray halos, as evidenced by radio continuum observations. Supplemental UV-data obtained with the OM-telescope at 210 nm show Diffuse Ionized Gas to be well associated with UV emission originating in the underlying disk. Beside NGC 891, NGC 4634 is the second non-starburst galaxy with a diffuse soft X-ray halo (|z| ≤ 4 kpc). In case of NGC 3877, for which we also present the first high resolution X-ray imaging data, no halo emission is detectable. EPIC pn spectra (0.3-12 keV) of the diffuse X-ray emission are extracted at different offset positions from the disk, giving evidence to a significant decrease of gas temperatures, electron densities, and gas masses with increasing distance to the plane. A comparison between dynamical and radiative cooling time scales implies that the outflow in all targets is likely to be sustained. We find very strong indications that spatially correlated multi-phase gaseous halos are created by star forming activity in the disk plane. In a forthcoming paper, we will present multi-frequency luminosity relations and evaluate key parameters which might trigger the formation of multi-phase galaxy halos.

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“…These compact ULXs may be binary systems containing black holes with masses of 10 2 -10 4 M (Colbert & Mushotzky 1999;Wang et al 2004). The existence of such intermediate-mass black holes (IMBHs) is intriguing, as they cannot be produced by current stellar evolutionary models.…”

Section: Introductionmentioning

confidence: 99%

An Optical Study of Stellar and Interstellar Environments of Seven Luminous and Ultraluminous X‐Ray Sources

Ramsey

Williams

Gruendl

et al. 2006

ApJ

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We have studied the stellar and interstellar environments of two luminous X-ray sources and five ultraluminous X-ray sources (ULXs) in order to gain insight into their nature. Archival Hubble Space Telescope images were used to identify the optical counterparts of the ULXs Ho IX X-1 and NGC 1313 X-2, and to make photometric measurements of the local stellar populations of these and the luminous source IC 10 X-1. We obtained high-dispersion spectroscopic observations of the nebulae around these seven sources to search for He ii k4686 emission and to estimate the expansion velocities and kinetic energies of these nebulae. Our observations did not detect nebular He ii emission from any source, with the exception of LMC X-1; this is either because we missed the He iii regions or because the nebulae are too diffuse to produce He ii surface brightnesses that lie within our detection limit. We compare the observed ionization and kinematics of the supershells around the ULXs Ho IX X-1 and NGC 1313 X-2 with the energy feedback expected from the underlying stellar population to assess whether additional energy contributions from the ULXs are needed. In both cases, we find insufficient UV fluxes or mechanical energies from the stellar population; thus these ULXs may be partially responsible for the ionization and energetics of their supershells. All seven sources that we studied are in young stellar environments, and six of them have optical counterparts with masses k7 M ; thus, these sources are most likely high-mass X-ray binaries.

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XMM‐NewtonSpectra of Intermediate‐Mass Black Hole Candidates: Application of a Monte Carlo Simulated Model

Cited by 29 publications

References 41 publications

Young Crab‐like Pulsars and Luminous X‐Ray Sources in Starbursts and Optically Dull Galaxies

Young Crab‐like Pulsars and Luminous X‐Ray Sources in Starbursts and Optically Dull Galaxies

The multi-phase gaseous halos of star forming late-type galaxies

An Optical Study of Stellar and Interstellar Environments of Seven Luminous and Ultraluminous X‐Ray Sources

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