Soft X-Ray Emission from the Spiral Galaxy NGC 1313

Colbert, E. J. M.; Petre, Robert; Schlegel, Eric M.; Ryder, S. D.

doi:10.1086/175777

Cited by 41 publications

(49 citation statements)

References 25 publications

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“…These objects have X-ray luminosities L X ∼ 10 39−42 erg s −1 which seems too bright for normal (stellar-mass) black hole X-ray binaries (BHXRBs), but far dimmer than normal active galactic nuclei (AGN). The first hints of these intermediate-luminosity X-ray point sources were found in the 1980s (Fabbiano 1989;Colbert et al 1995). Observations with ROSAT, and subsequent high resolution X-ray satellites, confirmed these findings and showed that these intriguing sources are often not in the centers of the galaxies (Colbert & Mushotzky 1999;Roberts & Warwick 2000).…”

Section: Introductionmentioning

confidence: 92%

A radio monitoring survey of ultra-luminous X-ray sources

Körding¹,

Colbert

Falcke

2005

A&A

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Abstract. We present the results of a radio monitoring campaign to search for radio emission from nearby ultra-luminous X-ray sources (ULXs). These sources are bright off-nuclear X-ray point sources with luminosities exceeding L X > 10 39 erg s −1 . A well-defined sample of the 9 nearest ULXs has been monitored eight times over 5 months with the Very Large Array in A and B configuration. Our limiting sensitivity is ≈0.15 mJy (4σ) for radio flares and ≈60 µJy for continuous emission. In M 82 two ULXs seem to have coincident compact radio sources, which are probably supernova remnants. No continuous or flaring radio emission has been detected from any other ULX. Thus, ULXs do not generally emit steady-state radio emission above radio powers of 1.5 × 10 17 W/Hz. The non-detections of the continuous emission are consistent with beamed or unbeamed radio emission from accreting black holes of ≤10 3 M based on the radio/X-ray correlation. Other published radio detections (M 82, NGC 5408) are also discussed in this context. Both detections are significantly above our detection limit. If ULXs have flaring radio emission above 4 × 10 17 W/Hz we can give an upper limit on the duty cycle of the flares of 6%. This upper limit is in agreement with the observed number of flares in Galactic radio transients. Additionally we present a yet unreported radio double structure in the nearby low-luminosity AGN NGC 4736.

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Section: Introductionmentioning

confidence: 92%

A radio monitoring survey of ultra-luminous X-ray sources

Körding¹,

Colbert

Falcke

2005

A&A

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“…It hosts 3 ULXs (Colbert et al 1995), one of whom is a known supernova remnant. Observations by Pagel, Edmunds & Smith (1980), and by Hadfield & Crowther (2007) where r is the elliptical radius, and r 25 4.…”

Section: The Environment Of Ngc1313 X-2mentioning

confidence: 99%

The metallicity of the nebula surrounding the ultra‐luminous X‐ray source NGC 1313 X‐2

Ripamonti¹,

Mapelli²,

Zampieri³

et al. 2011

Astron Nachr

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Recent models of the formation of ultra-luminous X-ray sources (ULXs) predict that they preferentially form in lowmetallicity environments. We look at the metallicity of the nebula surrounding NGC 1313 X-2, one of the best-studied ULXs. Simple estimates, based on the extrapolation of the metallicity gradient within NGC 1313, or on empirical calibrations (relating metallicity to strong oxygen lines) suggest a quite low metal content (Z ∼ 0.1Z ). But such estimates do not account for the remarkably strong X-ray flux irradiating the nebula. Then, we build photoionization models of the nebula using CLOUDY; using such models, the constraints on the metallicity weaken substantially, as we find 0.15Z ≤ Z ≤ 0.5Z .

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“…Several ROSAT HRI observations of these two sources show variability on the order of a factor $2 (Colbert & Ptak 2002). X-1 has a radio counterpart with a luminosity of $10 35 ergs s À1 (Colbert et al 1995). An optical counterpart to X-2 with an R magnitude of 21.6 has been reported by Zampieri et al (2003).…”

Section: Introductionmentioning

confidence: 99%

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

Wang

Yao

Fukui

et al. 2004

ApJ

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We present a systematic spectral analysis of six ultraluminous X-ray sources (NGC 1313 X-1 and X-2, IC 342 X-1, Ho IX X-1, NGC 5408 X-1, and NGC 3628 X-1) observed with the XMM-Newton observatory. These extranuclear X-ray sources in nearby late-type galaxies have been considered as intermediate-mass black hole candidates. We have performed Monte Carlo simulations of Comptonized multicolor blackbody accretion disks. This unified and self-consistent spectral model assumes a spherically symmetric, thermal corona around each disk and accounts for the radiation transfer in the Comptonization. We find that the model provides satisfactory fits to the XMM-Newton spectra of the sources. The characteristic temperatures of the accretion disks (T in ), for example, are in the range of $0.05-0.3 keV, consistent with the intermediate-mass black hole interpretation. We find that the black hole mass is typically about a few times 10 3 M and has an accretion rate of $10 À6 to 10 À5 M yr À1 . For the spectra considered here, we find that the commonly used multicolor blackbody accretion disk model with an additive power-law component, although not physical, provides a good mathematical approximation to the Monte Carlo simulated model. However, the latter model provides additional constraints on the properties of the accretion systems, such as the disk inclination angles and corona optical depths.

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Soft X-Ray Emission from the Spiral Galaxy NGC 1313

Cited by 41 publications

References 25 publications

A radio monitoring survey of ultra-luminous X-ray sources

A radio monitoring survey of ultra-luminous X-ray sources

The metallicity of the nebula surrounding the ultra‐luminous X‐ray source NGC 1313 X‐2

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

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