X-Rays from the Magellanic Clouds

Price, R. E.; Groves, D. J.; Rodrigues, Roberto M.; Seward, F. D.; Swift, C. D.; Toor, A.

doi:10.1086/180773

Cited by 47 publications

(22 citation statements)

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“…Orbital period of the system is ∼3.9 d (Schreier et al 1972). The system has been observed with several observatories since it was discovered during a rocket flight (Price et al 1971). It is the only discovered HMXB with a supergiant companion in SMC so far (Galache et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Analysis ofRXTE-PCA Observations of SMC X-1

İnam

Baykal

Beklen

2010

Monthly Notices of the Royal Astronomical Society

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We present timing and spectral analysis of Rossi X‐ray Timing Explorer‐Proportional Counter Array observations of SMC X‐1 between 1996 January and 2003 December. From observations around 1996 August 30 with a time‐span of ∼6 d, we obtain a precise timing solution for the source and resolve the eccentricity as 0.00089(6). We find an orbital decay rate of which is close to the previous results. Using our timing analysis and the previous studies, we construct a ∼30 yr long pulse period history of the source. We show that frequency derivative shows long‐ (i.e. more than a few years) and short‐term (i.e. order of days) fluctuations. From the spectral analysis, we found that all spectral parameters except Hydrogen column density showed no significant variation with time and X‐ray flux. Hydrogen column density is found to be higher as X‐ray flux gets lower. This may be due to the increase in soft absorption when the pulsar is partially obscured as in Her X‐1 or may just be an artefact of the tail of a soft excess in energy spectrum.

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Section: Introductionmentioning

confidence: 99%

Analysis ofRXTE-PCA Observations of SMC X-1

İnam

Baykal

Beklen

2010

Monthly Notices of the Royal Astronomical Society

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“…X-ray emission from the MCs was first observed in a rocket mission in 1970 (Price et al 1971). The first discovered single X-ray source in the Small Magellanic Cloud (SMC) was SMC X-1 detected in an Uhuru observation (Leong et al 1971).…”

Section: Introductionmentioning

confidence: 99%

ROSAT HRI catalogue of X-ray sources in the SMC region

Sasaki

Haberl

Pietsch

2000

Astron. Astrophys. Suppl. Ser.

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Abstract. During the operational phase of the ROSAT satellite between 1990 and 1998 the X-ray telescope pointed 71 times to the Small Magellanic Cloud (SMC) for observations with the High Resolution Imager (HRI), covering a field of 5• × 5• . From these data a catalogue of 121 discrete X-ray sources was derived. By cross-correlating the source catalogue with the SIMBAD data base and the TYCHO catalogue, the systematic positional error of the HRI source positions could be reduced. In total the X-ray position for 99 HRI sources was corrected yielding positional errors between 1 and 16 . The HRI catalogue was also cross-correlated with the catalogues derived from the ROSAT Position Sensitive Propotional Counter (PSPC) pointings (Kahabka et al. 1999;. For 75 HRI sources PSPC counterparts were found and thus hardness ratios are given. With the help of the information obtained from the cross-correlations 56 HRI sources were identified with objects of known or proposed nature. Four foreground stars, six supernova remnants, four supersoft sources, 12 X-ray binaries, and one AGN were detected by the HRI. Based on the existence of a likely optical counterpart or properties like hardness ratio and X-ray to optical flux ratio, further 15 HRI sources were classified into different source types.

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“…Magellanic Cloud observed by Price et al (1971) comes from SMC X-l, the photon spectrum between 5 and 20 KeV was found (Schreier et al) to The optical object corresponding to SMCX-1 was suggested to be SK 160 (Sanduleak, 1968) by Webster et al (1972) and Liller (1972c). 1.0 10 100 Energy (keV) Fig.…”

Section: Iii52 Optical Propertiesmentioning

confidence: 97%

“…SMC X-1 (2U0115-73) III.6.1. X-ray Observations X-ray observations of the Small Magellanic Cloud have been attempted by Lewin et al (1968) and Price et al (1971). An upper limit was obtained for its flux by Lewin et al (1968); while Price et al (1971) obtained a finite flux which has since been attributed to the whole cloud.…”

Section: Iii52 Optical Propertiesmentioning

confidence: 99%

“…X-ray Observations X-ray observations of the Small Magellanic Cloud have been attempted by Lewin et al (1968) and Price et al (1971). An upper limit was obtained for its flux by Lewin et al (1968); while Price et al (1971) obtained a finite flux which has since been attributed to the whole cloud. The UHURU observation of Leong et al (1971) resolved the source and it was found that most of the flux from Small Magellanic Cloud comes from this source which was designated SMC X-1.…”

Section: Iii52 Optical Propertiesmentioning

confidence: 99%

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