Early In-orbit Performance of Scanning Sky Monitor Onboard AstroSat

Ramadevi, M. C.; Ravishankar, B. T.; Sitaramamurthy, N.; Meena, G. S.; Singh, Brajpal; Jain, Abhay; Yadav, Reena; Agarwal, Anchal; Babu, V. C.; Kumar, Dilip; Kushwaha, Ankur; Vaishali, S.; Iyer, Nirmal; Nandi, Anuj; Girish, V.; Agarwal, Vivek; Seetha, S.; Bhattacharya, Dipankar; Balaji, K.; Kumar, Manoj; Kulshresta, Prashanth

doi:10.1007/s12036-017-9454-9

Cited by 17 publications

(7 citation statements)

References 8 publications

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“…For more details about SSM please see [33] and [34]. Results from the onboard calibration of SSM are described in [37].…”

Section: Scanning Sky Monitor (Ssm)mentioning

confidence: 99%

The AstroSat Observatory

Singh¹

2022

Preprint

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AstroSat is India's first Ultra-violet (UV) and X-ray astronomy observatory in space. The satellite was launched by the Indian Space Research Organisation on a Polar Satellite Launch Vehicle on 28 September 2015 from Sriharikota Range north of Chennai on the eastern coast of India. AstroSat carries five scientific instruments and one auxiliary instrument. Four of these consist of co-aligned telescopes and detectors mounted on a common deck of the satellite to observe stars and galaxies simultaneously in the near-and far-UV wavelengths and a broad range of X-ray energies (0.3 -80 keV). The fifth instrument consists of three X-ray detectors and is mounted on a rotating platform on a side that is oriented 90 degrees with respect to the other instruments to scan the sky for X-ray transients. An auxiliary instrument monitors the charged particle environment in the path of the satellite.

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“…For more details about SSM please see [33] and [34]. Results from the onboard calibration of SSM are described in [37].…”

Section: Scanning Sky Monitor (Ssm)mentioning

confidence: 99%

The AstroSat Observatory

Singh¹

2022

Preprint

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“…AstroSat is a multi-wavelength space observatory equipped with four co-aligned instruments to carry out broadband temporal and spectral studies of cosmic sources, namely, Soft X-ray Telescope (SXT ) (Singh et al 2014(Singh et al , 2017, Large Area X-ray Proportional Counter (LAXPC ) (Yadav et al 2016;Antia et al 2017), Cadmium Zinc Telluride Imager (CZTI ) (Vadawale et al 2016) and the Ultra Violet Imaging Telescope (UVIT ) (Tandon et al 2017). Apart from these, the Scanning Sky Monitor (SSM ) (Seetha et al 2006;Ramadevi et al 2017) scans the sky for X-ray events at all times. In this work, we extensively used broadband observational data from SXT and LAXPC instruments.…”

Section: Astrosatmentioning

confidence: 99%

AstroSat and MAXI view of the Black Hole binary 4U 1630-472 during 2016 and 2018 Outbursts

Baby,

Agrawal,

et al. 2020

Preprint

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We present an in-depth spectral and timing analysis of the Black Hole binary 4U 1630-472 during 2016 and 2018 outbursts as observed by AstroSat and MAXI. The extensive coverage of the outbursts with MAXI is used to obtain the Hardness Intensity Diagram (HID). The source follows a 'c'-shaped profile in agreement with earlier findings. Based on the HIDs of previous outbursts, we attempt to track the evolution of the source during a 'super'-outburst and 'mini'-outbursts. We model the broadband energy spectra (0.7 − 20.0 keV) of AstroSat observations of both outbursts using phenomenological and physical models. No Keplerian disc signature is observed at the beginning of 2016 outburst. However, the disc appears within a few hours after which it remains prominent with temperature (T in ) ∼ 1.3 keV and increase in photon index (Γ) from 1.8 to 2.0, whereas the source was at a disc dominant state throughout the AstroSat campaign of 2018 outburst. Based on the HIDs and spectral properties, we classify the outbursts into three different states -the 'canonical' hard and soft states along with an intermediate state. Evolution of rms along different states is seen although no Quasi-periodic Oscillations (QPOs) are detected. We fit the observed spectra using a dynamical accretion model and estimate the accretion parameters. Mass of the black hole is estimated using inner disc radius, bolometric luminosity and two component flow model to be 3 − 9 M ⊙ . Finally, we discuss the possible implications of our findings.

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“…There is also provision to stop the rotation and obtain long exposures on a desired target. The SSM is described in detail by Ramadevi et al (2017).…”

Section: Astrosat Science Instrumentsmentioning

confidence: 99%

Observing Compact Stars with AstroSat

Bhattacharya¹

2017

J Astrophys Astron

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Abstract. This article presents a brief description of India's AstroSat mission which is a powerful space based observatory for compact star research. An account is given of observational constraints and spectral and timing capabilities as realised post-launch. Some preliminary results of observations of the Crab pulsar and an X-ray binary system GX 301-2 are presented to illustrate some of the capabilities of the mission.

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Early In-orbit Performance of Scanning Sky Monitor Onboard AstroSat

Cited by 17 publications

References 8 publications

The AstroSat Observatory

The AstroSat Observatory

AstroSat and MAXI view of the Black Hole binary 4U 1630-472 during 2016 and 2018 Outbursts

Observing Compact Stars with AstroSat

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