A 4.1 keV spectral feature in a type 1 X-ray burst from EXO 1747 - 214

Magnier, E. A.; Lewin, W. H. G.; Paradijs, J. van; Tan, J.; Penninx, W.; Damen, E.

doi:10.1093/mnras/237.3.729

Cited by 30 publications

(41 citation statements)

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“…We used the spectral fitting package XSPEC version 11.3.1t to perform least-squares fits to the ME spectrum, and our results do not confirm those of Magnier et al (1989). A power law with (interstellar) absorption gives a very poor fit to the spectrum with 2 / ¼ 498/28.…”

Section: à2mentioning

confidence: 76%

“…This system was discovered during the EXOSAT Galactic plane scans in 1984 June ( Warwick et al 1988;Parmar et al 1985) and was detected again by EXOSAT in 1985 April at about the same flux level (Magnier et al 1989;Parmar et al 1985). These are the only two known detections of the source, so it has apparently been in quiescence for 20 yr. An X-ray burst was detected in 1985, demonstrating that the system definitely harbors a neutron star (Magnier et al 1989). Although EXOSAT provided a relatively good 15 00 position for the source, and the extinction along the line of sight to the source (l ¼ 7N00; b ¼ þ2N95) is fairly low, the source has not been optically identified.…”

Section: Introductionmentioning

confidence: 89%

“…The observation lasted for more than 6 hr, and, as reported in Magnier et al (1989), included one type I X-ray burst. The original analysis by Magnier et al (1989) a The three filters cover the 0.05-2.5 keV energy range with the different effective area curves described in the text.…”

Section: Column Density and Distance Upper Limit From Exosatmentioning

confidence: 95%

“…To derive the peak flux, we use the X-ray burst spectral results from Magnier et al (1989) and the peak 1-8 keV count rate of 2343 counts s À1 , which we obtain from our reanalysis of the EXOSAT data. Fitting spectra around the peak of the burst with 0.5 s time resolution with a blackbody model, Magnier et al (1989) find that the peak burst temperature is $2 keV. After fixing the temperature to 2 keV and assuming N H ¼ 4 ; 10 21 cm À2 , we adjusted the blackbody normalization to give the peak 1-8 keV count rate.…”

Section: à2mentioning

confidence: 99%

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The Low Quiescent X‐Ray Luminosity of the Transient X‐Ray Burster EXO 1747−214

Tomsick¹,

Gelino²,

Kaaret³

2005

ApJ

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We report on X-ray and optical observations of the X-ray burster EXO 1747À214. This source is an X-ray transient, and its only known outburst was observed in 1984-1985 by the EXOSAT satellite. We reanalyzed the EXOSAT data to derive the source position, column density, and a distance upper limit using its peak X-ray burst flux. We observed the EXO 1747À214 field in 2003 July with the Chandra X-Ray Observatory to search for the quiescent counterpart. We found one possible candidate just outside the EXOSAT error circle, but we cannot rule out the possibility that the source is unrelated to EXO 1747À214. Our conclusion is that the upper limit on the unabsorbed 0.3-8 keV luminosity is L < 7 ; 10 31 ergs s À1, making EXO 1747À214 one of the faintest neutron star transients in quiescence. We compare this luminosity upper limit to the quiescent luminosities of 19 neutron star and 14 black hole systems and discuss the results in the context of the differences between neutron stars and black holes. Based on the theory of deep crustal heating suggested by Brown and coworkers, the luminosity implies an outburst recurrence time of >1300 yr unless some form of enhanced cooling occurs within the neutron star. The position of the possible X-ray counterpart is consistent with three blended optical / IR sources with R magnitudes between 19.4 and 19.8 and J magnitudes between 17.2 and 17.6. One of these sources could be the quiescent optical / IR counterpart of EXO 1747À214.

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Section: à2mentioning

confidence: 76%

Section: Introductionmentioning

confidence: 89%

Section: Column Density and Distance Upper Limit From Exosatmentioning

confidence: 95%

Section: à2mentioning

confidence: 99%

See 2 more Smart Citations

The Low Quiescent X‐Ray Luminosity of the Transient X‐Ray Burster EXO 1747−214

Tomsick¹,

Gelino²,

Kaaret³

2005

ApJ

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“…One possible way is to measure spectral lines in X-ray burst spectra (Lewin 1994). Absorption features at 4.1 keV (Waki et al 1984;Nakamura et al 1988;Magnier et al 1989) and 5.7 keV (Waki et al 1984) were reported in X-ray burst spectra with Tenma and EXOSAT. However, they were never confirmed with more sensitive instruments.…”

Section: Introductionmentioning

confidence: 94%

Nondetection of Gravitationally Redshifted Absorption Lines in the X-Ray Burst Spectra of GS 1826-24

Kong

Miller

Méndez

et al. 2007

ApJ

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During a 200 ks observation with the XMM-Newton Reflection Grating Spectrometer, we detected 16 type I X-ray bursts from GS 1826Ϫ24. We combined the burst spectra in an attempt to measure the gravitational redshifts from the surface of the neutron star. We divided the composite GS 1826Ϫ24 burst spectrum into three groups based on the blackbody temperature during the bursts. The spectra do not show any obvious discrete absorption lines. We compare our observations with those of EXO 0748Ϫ676.

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5.6.4 X-ray bursters

Trümper¹,

Fink²

Stars and Star Clusters

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A 4.1 keV spectral feature in a type 1 X-ray burst from EXO 1747 - 214

Cited by 30 publications

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The Low Quiescent X‐Ray Luminosity of the Transient X‐Ray Burster EXO 1747−214

The Low Quiescent X‐Ray Luminosity of the Transient X‐Ray Burster EXO 1747−214

Nondetection of Gravitationally Redshifted Absorption Lines in the X-Ray Burst Spectra of GS 1826-24

5.6.4 X-ray bursters

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