|Launch date||28 September 2015|
|Launch site||Satish Dhawan Space Centre First Launch Pad, Sriharikota|
|Mission length||5 years|
|Mass||1,650 kg (3,640 lb)|
|Type of orbit||Near-equatorial|
|Orbit height||650 km (400 mi)|
|UVIT||UltraViolet imaging telescope|
|SXT||Soft X-ray telescope|
|LAXPC||X-ray timing and low-resolution spectral studies|
|CZTI||Hard X-ray imager|
After the success of the satellite-borne Indian X-ray Astronomy Experiment (IXAE), which was launched in 1996, the Indian Space Research Organization (ISRO) approved further development for a full-fledged astronomy satellite, Astrosat, in 2004.
A number of astronomy research institutions in India, and abroad have jointly built instruments for the satellite. Important areas requiring coverage include studies of astrophysical objects ranging from nearby solar system objects to distant stars and objects at cosmological distances; timing studies of variables ranging from pulsations of hot white dwarfs to those of active galactic nuclei can be conducted with Astrosat as well, with time scales ranging from milliseconds to days.
Astrosat is a multi-wavelength astronomy mission on an IRS-class satellite into a near-Earth, equatorial orbit. The five instruments on board cover the visible (320–530 nm), near UV (180–300 nm), far UV (130–180 nm), soft X-ray (0.3–8 keV and 2–10 keV) and hard X-ray (3–80 keV and 10–150 keV) regions of the electromagnetic spectrum.
Astrosat is a proposal-driven general purpose observatory, with main scientific focus on:
- Simultaneous multi-wavelength monitoring of intensity variations in a broad range of cosmic sources
- Monitoring the X-ray sky for new transients
- Sky surveys in the hard X-ray and UV bands
- Broadband spectroscopic studies of X-ray binaries, AGN, SNRs, clusters of galaxies, and stellar coronae
- Studies of periodic and non-periodic variability of X-ray sources
Astrosat performs multi-wavelength observations covering spectral bands from radio, optical, IR, UV, and X-ray wavelengths. Both individual studies of specific sources of interest and surveys are undertaken. While radio, optical, and IR observations would be coordinated through ground-based telescopes, the high energy regions, i.e., UV, X-ray and visible wavelength, would be covered by the dedicated satellite-borne instrumentation of Astrosat.
The mission would also study near simultaneous multi-wavelength data from different variable sources. In a binary system, for example, regions near the compact object emit predominantly in the X-ray, with the accretion disc emitting most of its light in the UV/optical waveband, whereas the mass of the donating star is brightest in the optical band.
The observatory will also carry out:
- Low- to moderate-resolution spectroscopy over a wide energy band with the primary emphasis on studies of X-ray-emitting objects
- Timing studies of periodic and aperiodic phenomena in X-ray binaries
- Studies of pulsations in X-ray pulsars
- Quasi-periodic oscillations, flickering, flaring, and other variations in X-ray binaries
- Short- and long-term intensity variations in active galactic nuclei
- Time-lag studies in low/hard X-rays and UV/optical radiation
- Detection and study of X-ray transients.
In particular, the mission will train its instruments at active galactic nuclei (such as that of the core of the Milky Way), which are believed to contain super-massive black holes.
The scientific payload has a mass of 1513 kg and contains six instruments.
- The Ultra Violet Imaging Telescope (UVIT) performs imaging simultaneously in three channels: 130–180 nm, 180–300 nm, and 320–530 nm. The field of view is a circle of ~28′ diameter and the angular resolution is 1.8" for the ultraviolet channels and 2.5″ for the visible channel. In each of the three channels a spectral band can be selected through a set of filters mounted on a wheel; in addition, for the two ultraviolet channels a grating can be selected in the wheel to do slitless spectroscopy with a resolution of ~100. The primary mirror diameter of the telescope is 40 cm.
- The Soft X-ray imaging Telescope (SXT) employs focusing optics and a deep depletion CCD camera at the focal plane to perform X-ray imaging in the 0.3–8.0 keV band. The optics will consist of 41 concentric shells of gold-coated conical foil mirrors in an approximate Wolter-I configuration (the effective area of 120 cm2). The focal plane CCD camera will be very similar to that flown on SWIFT XRT. The CCD will be operated at a temperature of about −80 °C by thermoelectric cooling.
- The LAXPC Instrument covers X-ray timing and low-resolution spectral studies over a broad energy band (3–80 keV), Astrosat will use a cluster of 3 co-aligned identical Large Area X-ray Proportional Counters (LAXPCs), each with a multi-wire-multi-layer configuration and a Field of View of 1° × 1°. These detectors are designed to achieve (I) wide energy band of 3–80 keV, (II) high detection efficiency over the entire energy band, (III) narrow field of view to minimize source confusion, (IV) moderate energy resolution, (V) small internal background and (VI) long lifetime in space. The effective area of the telescope is 6000 cm2.
- The Cadmium Zinc Telluride Imager (CZTI) is a hard X-ray imager in the form of CZTI. It will consist of a Pixellated Cadmium-Zinc-Telluride detector array of 500 cm2 effective area and the energy range from 10 to 150 kev. The detectors have the detection efficiency close to 100% up to 100 keV, and have a superior energy resolution (~2% at 60 keV) compared to scintillation and proportional counters. Their small pixel size also facilitates medium resolution imaging in hard x-rays. The CZTI will be fitted with a two dimensional coded mask, for imaging purposes. The sky brightness distribution will be obtained by applying a deconvolution procedure to the shadow pattern of the coded mask recorded by the detector. Apart from spectroscopic studies, CZTI would be able to do sensitive polarization measurements for bright galactic X-ray sources in 100–300 keV.
- The Scanning Sky Monitor (SSM) consists of three position sensitive proportional counters, each with a one-dimensional coded mask, very similar in design to the All Sky Monitor on NASA's RXTE satellite. The gas-filled proportional counter will have resistive wires as anodes. The ratio of the output charge on either ends of the wire will provide the position of the x-ray interaction, providing an imaging plane at the detector. The coded mask, consisting of a series of slits, will cast a shadow on the detector, from which the sky brightness distribution will be derived.
- The Charged Particle Monitor (CPM) will be included as a part of Astrosat payloads to control the operation of the LAXPC, SXT and SSM. Even though the orbital inclination of the satellite will be 8 deg or less, in about 2/3 of the orbits, the satellite will spend a considerable time (15–20 minutes) in the South Atlantic Anomaly (SAA) region which has high fluxes of low energy protons and electrons. The high voltage will be lowered or put off using data from CPM when the satellite enters the SAA region to prevent damage to the detectors as well as to minimize ageing effect in the Proportional Counters.
|This section does not cite any references (sources). (September 2015)|
The Ground Command and Control Centre for Astrosat will be ISRO Telemetry, Tracking and Command Network (ISTRAC), Bangalore, India. Commanding and data download will be possible during every visible pass over Bangalore. Ten out of 14 orbits per day will be visible to the ground station. The satellite is capable of gathering 420 gigabits of data every day that can be down loaded in 10 to 11 orbits visible at Tracking and Data receiving center of ISRO in Bangalore. A third 11-meter antenna at the Indian Deep Space Network (IDSN) was operational in July 2009 to track Astrosat.
- 28 Sep 2015: ASTROSAT has been successfully launched into orbit.
- 10 Aug 2015: All tests passed. Pre-shipment review successfully completed.
- 24 July 2015: Thermovac completed. Solar panels attached. Start of final vibration tests.
- May 2015 : The integration of Astrosat is complete and final tests are under way. ISRO issued a press release stating that "The satellite is planned to be launched during the second half of 2015 by PSLV C-34 to a 650 km near equatorial orbit around the Earth." 
- April 2009 : Scientists from Tata Institute of Fundamental Research (TIFR) have completed the developmental phase of complex science payloads and have begun integrating them before delivery of the 1,650 kg satellite Astrosat. The challenges in the design of payloads and Attitude Control System have been overcome and in a recent review committee meeting, it was decided that the delivery of the payload to the ISRO Satellite Centre will begin from the middle of 2009 and continue until early 2010 to enable the launch of ASTROSAT in 2010 using ISRO workhorse PSLV-C34.
Two of the instruments were harder to complete than expected. "The satellite’s soft x-ray telescope proved to be a huge challenge that took 11 years..."
The Astrosat project is a collaborative effort of many different research institutions. The participants are:
- Indian Space Research Organization
- Tata Institute of Fundamental Research, Mumbai
- Indian Institute of Astrophysics, Bangalore
- Raman Research Institute, Bangalore
- Inter-University Centre for Astronomy and Astrophysics, Pune
- Bhabha Atomic Research Centre, Mumbai
- S.N. Bose National Centre for Basic Sciences, Kolkata
- Canadian Space Agency
- University of Leicester
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