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AstroSat/LAXPC view of GX 17+2: spectral evolution along the Z-track

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Abstract

In this paper, we present the first results obtained using \(\sim 50\) ks observations of the bright low-mass X-ray binary (LMXB) GX 17+2 with Large Area X-ray Proportional Counter (LAXPC) onboard AstroSat. The source traced out a complete Z-track in the hardness intensity diagram (HID). The spectra at different sections of the Z-diagram are well described by either a combination of a thermal Comptonization component, a power-law and a relativistic iron line or a model consisting of a thermal disk component, a single temperature blackbody, a power-law and a relativistic iron line. Fitting the spectra with both phenomenological models suggests that the power-law component is strong in the horizontal branch (HB), becomes weaker as the source moves down the normal branch (NB) and then again becomes stronger as the sources moves up the flaring branch (FB). However, we find that the strength of the power-law component is model dependent, although the trend in the variation of the power-law strength along the Z-track is similar. A simple model composed by a Comptonized emission and power-law component, convolved with the ionized reflection, also describes the spectra very well.

A normal branch oscillation (NBO) with a centroid frequency \(7.42 \pm 0.23\) Hz, quality factor \(\text{(Q)} \sim 4.88\), rms \(1.41 \pm 0.29\)% and significance 5.1\(\sigma \) is detected at the middle of the NB. The parameters of the Comptonized emission show a systematic evolution along the Z-diagram. The optical depth of the corona increases as the source moves up along the FB, suggesting possible trigger of an outflow or dumping of the disc material in to the corona by radiation pressure.

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Change history

  • 19 March 2020

    In the <Emphasis Type="Bold">Discussion</Emphasis> section of the initial online publication an incorrect percentage was specified for the observed contribution of the hard X-ray tail in the middle and upper flaring branch to the total flux of 3.0–80.0 keV. The original article has been corrected.

  • 19 March 2020

    In the Discussion section of the initial online publication an incorrect percentage was specified for the observed contribution of the hard X-ray tail in the middle and upper flaring branch to the total flux of 3.0���80.0��keV. The original article has been corrected.

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Acknowledgements

We thank anonymous reviewer for providing useful suggestions which improved the quality of the paper. This research has made use of the data obtained through GT phase of AstroSat observation. Authors thank GD, SAG; DD, PDMSA and Director, URSC for encouragement and continuous support to carry out this research. This work has used the data from the LAXPC Instruments developed at TIFR, Mumbai and the LAXPC POC at TIFR is thanked for verifying and releasing the data via the ISSDC data archive. We thank the AstroSat Science Support Cell hosted by IUCAA and TIFR for providing the LaxpcSoft software which we used for LAXPC data analysis.

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  1. Space Astronomy Group, ISITE Campus, U R Rao Satellite Center, Bangalore, 560037, India

    V. K. Agrawal, Anuj Nandi & M. C. Ramadevi

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  1. V. K. Agrawal
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The original version of this article was revised: An incorrect percentage specified in the Discussion section was corrected.

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Agrawal, V.K., Nandi, A. & Ramadevi, M.C. AstroSat/LAXPC view of GX 17+2: spectral evolution along the Z-track. Astrophys Space Sci 365, 41 (2020). https://doi.org/10.1007/s10509-020-3748-0

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