2019). Observed data consisted of 15 continuous segments corresponding to 15 individual orbits of the satellite. 2019 ). The AstroSat satellite is designed for multi-wavelength astronomy for observations covering a spectral range from soft and hard X-rays to the ultra-violet. Data reduction and analysis Typically all X-ray observations are made by X-ray detectors onboard different satellites. The meeting will include oral as well as poster presentations that will cover a wide spectrum of topics using AstroSat data. The space science missions planned for future includes ASTROSAT, a multi-wavelength astronomical observatory in space, aimed at studying the distant celestial sources and scheduled to be launched using PSLV-XL in 2015-16. 2. Particularly helpful is being able to see the results of the data-reduction steps as they are performed in near-real time. All astronomical data is distributed in a standard file format called FITS format. In the Raman Research Institute, work on the timing and spectral calibration of the ASTROSAT-LAXPC instrument and development of the data reduction software is in progress at the X-ray astronomy laboratory. SXT data were reduced using SXT pipeline AS1SXTLevel2 -1.4>a and the calibration files released with the pipeline. The first stage of processing is shown in Figure 1. DATA REDUCTION AND ANALYSIS 2.1. Data Reduction and Analysis 2.1. Data Reduction We have analyzed ∼93 ks simultaneous data from SXT and LAXPC on board AstroSat spanning over a period of 2 days starting from 2018 March 30. Observations. Low frequency Type-C QPOs (0.85–6.68 Hz) are detected. The Ultraviolet Imaging Telescope (UVIT) is the only non-X-ray telescope on AstroSat and it pro-vides the long lever arm to the multi-wavelength ob-servations. 2 OBSERVATIONS AND DATA REDUCTION AstroSat Target of Opportunity (ToO) observations of RX J0209.6-7427 were performed approximately three weeks after the source woke up from its deep slumber on 2019 November 20 detected by the MAXI mission (Negoro et al. AstroSat has observed a wide variety of targets such as normal galaxies, active galaxies, galaxy clusters, star clusters, various type of binary stars, planetary nebulae, compact objects etc. The input to CZTI level-2 data reduction pipeline is the data set produced at Level 1. Chandrayaan-2, a follow-on mission to Chandrayaan-1 with an Orbiter, Lander and Rover, is to be launched onboard GSLV.
A complementary charged particle monitor is also onboard to provide data on particle flux. The original data is received by telemetry at the Indian Space Science Data Centre (ISSDC), during each visible pass over Bengaluru, India.
For further details on this project please click here or contact Prof. Biswajit Paul. CCDLAB can perform all of the typical image data-reduction operations required for FITS image data, such as Understand high energy processes in binary systems Search for black hole sources in the Galaxy. Observations and data reduction 2.1. This data is transmitted to ground station, from where it is distributed to the scientists. The standard data reduction pipelines and tools, disbursed by AstroSat Science Support Center (ASSC)1, are utilized to perform the data analysis. The features of QPOs presented by Swift J1658.2–4242 are similar to many black hole transients. Using the observations of Insight-HXMT, NICER and AstroSat, we overview the whole outburst of Swift J1658.2–4242 in 2018.
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