Early In-orbit Performance of Scanning Sky Monitor Onboard AstroSat
Abstract We report the in-orbit performance of Scanning Sky Monitor (SSM) onboard AstroSat. The SSM operates in the energy range 2.5 to 10 keV and scans the sky to detect and locate transient X-ray sources. This information of any interesting phenomenon in the X-ray sky as observed by SSM is provide...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Ramadevi, M. C. [verfasserIn] Ravishankar, B. T. [verfasserIn] Sitaramamurthy, N. [verfasserIn] Meena, G. [verfasserIn] Singh, Brajpal [verfasserIn] Jain, Anand [verfasserIn] Yadav, Reena [verfasserIn] Agarwal, Anil [verfasserIn] Babu, V. Chandra [verfasserIn] Kushwaha, Ankur [verfasserIn] Vaishali, S. [verfasserIn] Iyer, Nirmal Kumar [verfasserIn] Nandi, Anuj [verfasserIn] V., Girish [verfasserIn] Agarwal, Vivek Kumar [verfasserIn] Seetha, S. [verfasserIn] Bhattacharya, Dipankar [verfasserIn] Balaji, K. [verfasserIn] Kumar, Manoj [verfasserIn] Kulshresta, Prashanth [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2017 |
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| Übergeordnetes Werk: |
Enthalten in: Journal of astrophysics and astronomy - Bangalore : Springer India, 1980, 38(2017), 2 vom: 19. Juni |
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| Übergeordnetes Werk: |
volume:38 ; year:2017 ; number:2 ; day:19 ; month:06 |
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| DOI / URN: |
10.1007/s12036-017-9454-9 |
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| Katalog-ID: |
SPR023997036 |
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| 100 | 1 | |a Ramadevi, M. C. |e verfasserin |4 aut | |
| 245 | 1 | 0 | |a Early In-orbit Performance of Scanning Sky Monitor Onboard AstroSat |
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| 520 | |a Abstract We report the in-orbit performance of Scanning Sky Monitor (SSM) onboard AstroSat. The SSM operates in the energy range 2.5 to 10 keV and scans the sky to detect and locate transient X-ray sources. This information of any interesting phenomenon in the X-ray sky as observed by SSM is provided to the astronomical community for follow-up observations. Following the launch of AstroSat on 28th September, 2015, SSM was commissioned on October 12th, 2015. The first power ON of the instrument was with the standard X-ray source, Crab in the field-of-view. The first orbit data revealed the basic expected performance of one of the detectors of SSM, SSM1. Following this in the subsequent orbits, the other detectors were also powered ON to find them perform in good health. Quick checks of the data from the first few orbits revealed that the instrument performed with the expected angular resolution of 12’ %$\times %$ 2.5%$^\circ %$ and effective area in the energy range of interest. This paper discusses the instrument aspects along with few on-board results immediately after power ON. | ||
| 650 | 4 | |a X-ray sky monitor |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a 1D position sensitive proportional counter |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a coded mask |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a AstroSat |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a X-ray transients |7 (dpeaa)DE-He213 | |
| 700 | 1 | |a Ravishankar, B. T. |e verfasserin |4 aut | |
| 700 | 1 | |a Sitaramamurthy, N. |e verfasserin |4 aut | |
| 700 | 1 | |a Meena, G. |e verfasserin |4 aut | |
| 700 | 1 | |a Singh, Brajpal |e verfasserin |4 aut | |
| 700 | 1 | |a Jain, Anand |e verfasserin |4 aut | |
| 700 | 1 | |a Yadav, Reena |e verfasserin |4 aut | |
| 700 | 1 | |a Agarwal, Anil |e verfasserin |4 aut | |
| 700 | 1 | |a Babu, V. Chandra |e verfasserin |4 aut | |
| 700 | 1 | |a Kushwaha, Ankur |e verfasserin |4 aut | |
| 700 | 1 | |a Vaishali, S. |e verfasserin |4 aut | |
| 700 | 1 | |a Iyer, Nirmal Kumar |e verfasserin |4 aut | |
| 700 | 1 | |a Nandi, Anuj |e verfasserin |4 aut | |
| 700 | 1 | |a V., Girish |e verfasserin |4 aut | |
| 700 | 1 | |a Agarwal, Vivek Kumar |e verfasserin |4 aut | |
| 700 | 1 | |a Seetha, S. |e verfasserin |4 aut | |
| 700 | 1 | |a Bhattacharya, Dipankar |e verfasserin |4 aut | |
| 700 | 1 | |a Balaji, K. |e verfasserin |4 aut | |
| 700 | 1 | |a Kumar, Manoj |e verfasserin |4 aut | |
| 700 | 1 | |a Kulshresta, Prashanth |e verfasserin |4 aut | |
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10.1007/s12036-017-9454-9 doi (DE-627)SPR023997036 (SPR)s12036-017-9454-9-e DE-627 ger DE-627 rakwb eng 520 ASE 39.22 bkl Ramadevi, M. C. verfasserin aut Early In-orbit Performance of Scanning Sky Monitor Onboard AstroSat 2017 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We report the in-orbit performance of Scanning Sky Monitor (SSM) onboard AstroSat. The SSM operates in the energy range 2.5 to 10 keV and scans the sky to detect and locate transient X-ray sources. This information of any interesting phenomenon in the X-ray sky as observed by SSM is provided to the astronomical community for follow-up observations. Following the launch of AstroSat on 28th September, 2015, SSM was commissioned on October 12th, 2015. The first power ON of the instrument was with the standard X-ray source, Crab in the field-of-view. The first orbit data revealed the basic expected performance of one of the detectors of SSM, SSM1. Following this in the subsequent orbits, the other detectors were also powered ON to find them perform in good health. Quick checks of the data from the first few orbits revealed that the instrument performed with the expected angular resolution of 12’ %$\times %$ 2.5%$^\circ %$ and effective area in the energy range of interest. This paper discusses the instrument aspects along with few on-board results immediately after power ON. X-ray sky monitor (dpeaa)DE-He213 1D position sensitive proportional counter (dpeaa)DE-He213 coded mask (dpeaa)DE-He213 AstroSat (dpeaa)DE-He213 X-ray transients (dpeaa)DE-He213 Ravishankar, B. T. verfasserin aut Sitaramamurthy, N. verfasserin aut Meena, G. verfasserin aut Singh, Brajpal verfasserin aut Jain, Anand verfasserin aut Yadav, Reena verfasserin aut Agarwal, Anil verfasserin aut Babu, V. Chandra verfasserin aut Kushwaha, Ankur verfasserin aut Vaishali, S. verfasserin aut Iyer, Nirmal Kumar verfasserin aut Nandi, Anuj verfasserin aut V., Girish verfasserin aut Agarwal, Vivek Kumar verfasserin aut Seetha, S. verfasserin aut Bhattacharya, Dipankar verfasserin aut Balaji, K. verfasserin aut Kumar, Manoj verfasserin aut Kulshresta, Prashanth verfasserin aut Enthalten in Journal of astrophysics and astronomy Bangalore : Springer India, 1980 38(2017), 2 vom: 19. Juni (DE-627)358454131 (DE-600)2096381-6 0973-7758 nnns volume:38 year:2017 number:2 day:19 month:06 https://dx.doi.org/10.1007/s12036-017-9454-9 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4393 GBV_ILN_4700 39.22 ASE AR 38 2017 2 19 06 |
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10.1007/s12036-017-9454-9 doi (DE-627)SPR023997036 (SPR)s12036-017-9454-9-e DE-627 ger DE-627 rakwb eng 520 ASE 39.22 bkl Ramadevi, M. C. verfasserin aut Early In-orbit Performance of Scanning Sky Monitor Onboard AstroSat 2017 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We report the in-orbit performance of Scanning Sky Monitor (SSM) onboard AstroSat. The SSM operates in the energy range 2.5 to 10 keV and scans the sky to detect and locate transient X-ray sources. This information of any interesting phenomenon in the X-ray sky as observed by SSM is provided to the astronomical community for follow-up observations. Following the launch of AstroSat on 28th September, 2015, SSM was commissioned on October 12th, 2015. The first power ON of the instrument was with the standard X-ray source, Crab in the field-of-view. The first orbit data revealed the basic expected performance of one of the detectors of SSM, SSM1. Following this in the subsequent orbits, the other detectors were also powered ON to find them perform in good health. Quick checks of the data from the first few orbits revealed that the instrument performed with the expected angular resolution of 12’ %$\times %$ 2.5%$^\circ %$ and effective area in the energy range of interest. This paper discusses the instrument aspects along with few on-board results immediately after power ON. X-ray sky monitor (dpeaa)DE-He213 1D position sensitive proportional counter (dpeaa)DE-He213 coded mask (dpeaa)DE-He213 AstroSat (dpeaa)DE-He213 X-ray transients (dpeaa)DE-He213 Ravishankar, B. T. verfasserin aut Sitaramamurthy, N. verfasserin aut Meena, G. verfasserin aut Singh, Brajpal verfasserin aut Jain, Anand verfasserin aut Yadav, Reena verfasserin aut Agarwal, Anil verfasserin aut Babu, V. Chandra verfasserin aut Kushwaha, Ankur verfasserin aut Vaishali, S. verfasserin aut Iyer, Nirmal Kumar verfasserin aut Nandi, Anuj verfasserin aut V., Girish verfasserin aut Agarwal, Vivek Kumar verfasserin aut Seetha, S. verfasserin aut Bhattacharya, Dipankar verfasserin aut Balaji, K. verfasserin aut Kumar, Manoj verfasserin aut Kulshresta, Prashanth verfasserin aut Enthalten in Journal of astrophysics and astronomy Bangalore : Springer India, 1980 38(2017), 2 vom: 19. Juni (DE-627)358454131 (DE-600)2096381-6 0973-7758 nnns volume:38 year:2017 number:2 day:19 month:06 https://dx.doi.org/10.1007/s12036-017-9454-9 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4393 GBV_ILN_4700 39.22 ASE AR 38 2017 2 19 06 |
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10.1007/s12036-017-9454-9 doi (DE-627)SPR023997036 (SPR)s12036-017-9454-9-e DE-627 ger DE-627 rakwb eng 520 ASE 39.22 bkl Ramadevi, M. C. verfasserin aut Early In-orbit Performance of Scanning Sky Monitor Onboard AstroSat 2017 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We report the in-orbit performance of Scanning Sky Monitor (SSM) onboard AstroSat. The SSM operates in the energy range 2.5 to 10 keV and scans the sky to detect and locate transient X-ray sources. This information of any interesting phenomenon in the X-ray sky as observed by SSM is provided to the astronomical community for follow-up observations. Following the launch of AstroSat on 28th September, 2015, SSM was commissioned on October 12th, 2015. The first power ON of the instrument was with the standard X-ray source, Crab in the field-of-view. The first orbit data revealed the basic expected performance of one of the detectors of SSM, SSM1. Following this in the subsequent orbits, the other detectors were also powered ON to find them perform in good health. Quick checks of the data from the first few orbits revealed that the instrument performed with the expected angular resolution of 12’ %$\times %$ 2.5%$^\circ %$ and effective area in the energy range of interest. This paper discusses the instrument aspects along with few on-board results immediately after power ON. X-ray sky monitor (dpeaa)DE-He213 1D position sensitive proportional counter (dpeaa)DE-He213 coded mask (dpeaa)DE-He213 AstroSat (dpeaa)DE-He213 X-ray transients (dpeaa)DE-He213 Ravishankar, B. T. verfasserin aut Sitaramamurthy, N. verfasserin aut Meena, G. verfasserin aut Singh, Brajpal verfasserin aut Jain, Anand verfasserin aut Yadav, Reena verfasserin aut Agarwal, Anil verfasserin aut Babu, V. Chandra verfasserin aut Kushwaha, Ankur verfasserin aut Vaishali, S. verfasserin aut Iyer, Nirmal Kumar verfasserin aut Nandi, Anuj verfasserin aut V., Girish verfasserin aut Agarwal, Vivek Kumar verfasserin aut Seetha, S. verfasserin aut Bhattacharya, Dipankar verfasserin aut Balaji, K. verfasserin aut Kumar, Manoj verfasserin aut Kulshresta, Prashanth verfasserin aut Enthalten in Journal of astrophysics and astronomy Bangalore : Springer India, 1980 38(2017), 2 vom: 19. Juni (DE-627)358454131 (DE-600)2096381-6 0973-7758 nnns volume:38 year:2017 number:2 day:19 month:06 https://dx.doi.org/10.1007/s12036-017-9454-9 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4393 GBV_ILN_4700 39.22 ASE AR 38 2017 2 19 06 |
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10.1007/s12036-017-9454-9 doi (DE-627)SPR023997036 (SPR)s12036-017-9454-9-e DE-627 ger DE-627 rakwb eng 520 ASE 39.22 bkl Ramadevi, M. C. verfasserin aut Early In-orbit Performance of Scanning Sky Monitor Onboard AstroSat 2017 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We report the in-orbit performance of Scanning Sky Monitor (SSM) onboard AstroSat. The SSM operates in the energy range 2.5 to 10 keV and scans the sky to detect and locate transient X-ray sources. This information of any interesting phenomenon in the X-ray sky as observed by SSM is provided to the astronomical community for follow-up observations. Following the launch of AstroSat on 28th September, 2015, SSM was commissioned on October 12th, 2015. The first power ON of the instrument was with the standard X-ray source, Crab in the field-of-view. The first orbit data revealed the basic expected performance of one of the detectors of SSM, SSM1. Following this in the subsequent orbits, the other detectors were also powered ON to find them perform in good health. Quick checks of the data from the first few orbits revealed that the instrument performed with the expected angular resolution of 12’ %$\times %$ 2.5%$^\circ %$ and effective area in the energy range of interest. This paper discusses the instrument aspects along with few on-board results immediately after power ON. X-ray sky monitor (dpeaa)DE-He213 1D position sensitive proportional counter (dpeaa)DE-He213 coded mask (dpeaa)DE-He213 AstroSat (dpeaa)DE-He213 X-ray transients (dpeaa)DE-He213 Ravishankar, B. T. verfasserin aut Sitaramamurthy, N. verfasserin aut Meena, G. verfasserin aut Singh, Brajpal verfasserin aut Jain, Anand verfasserin aut Yadav, Reena verfasserin aut Agarwal, Anil verfasserin aut Babu, V. Chandra verfasserin aut Kushwaha, Ankur verfasserin aut Vaishali, S. verfasserin aut Iyer, Nirmal Kumar verfasserin aut Nandi, Anuj verfasserin aut V., Girish verfasserin aut Agarwal, Vivek Kumar verfasserin aut Seetha, S. verfasserin aut Bhattacharya, Dipankar verfasserin aut Balaji, K. verfasserin aut Kumar, Manoj verfasserin aut Kulshresta, Prashanth verfasserin aut Enthalten in Journal of astrophysics and astronomy Bangalore : Springer India, 1980 38(2017), 2 vom: 19. Juni (DE-627)358454131 (DE-600)2096381-6 0973-7758 nnns volume:38 year:2017 number:2 day:19 month:06 https://dx.doi.org/10.1007/s12036-017-9454-9 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4393 GBV_ILN_4700 39.22 ASE AR 38 2017 2 19 06 |
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10.1007/s12036-017-9454-9 doi (DE-627)SPR023997036 (SPR)s12036-017-9454-9-e DE-627 ger DE-627 rakwb eng 520 ASE 39.22 bkl Ramadevi, M. C. verfasserin aut Early In-orbit Performance of Scanning Sky Monitor Onboard AstroSat 2017 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We report the in-orbit performance of Scanning Sky Monitor (SSM) onboard AstroSat. The SSM operates in the energy range 2.5 to 10 keV and scans the sky to detect and locate transient X-ray sources. This information of any interesting phenomenon in the X-ray sky as observed by SSM is provided to the astronomical community for follow-up observations. Following the launch of AstroSat on 28th September, 2015, SSM was commissioned on October 12th, 2015. The first power ON of the instrument was with the standard X-ray source, Crab in the field-of-view. The first orbit data revealed the basic expected performance of one of the detectors of SSM, SSM1. Following this in the subsequent orbits, the other detectors were also powered ON to find them perform in good health. Quick checks of the data from the first few orbits revealed that the instrument performed with the expected angular resolution of 12’ %$\times %$ 2.5%$^\circ %$ and effective area in the energy range of interest. This paper discusses the instrument aspects along with few on-board results immediately after power ON. X-ray sky monitor (dpeaa)DE-He213 1D position sensitive proportional counter (dpeaa)DE-He213 coded mask (dpeaa)DE-He213 AstroSat (dpeaa)DE-He213 X-ray transients (dpeaa)DE-He213 Ravishankar, B. T. verfasserin aut Sitaramamurthy, N. verfasserin aut Meena, G. verfasserin aut Singh, Brajpal verfasserin aut Jain, Anand verfasserin aut Yadav, Reena verfasserin aut Agarwal, Anil verfasserin aut Babu, V. Chandra verfasserin aut Kushwaha, Ankur verfasserin aut Vaishali, S. verfasserin aut Iyer, Nirmal Kumar verfasserin aut Nandi, Anuj verfasserin aut V., Girish verfasserin aut Agarwal, Vivek Kumar verfasserin aut Seetha, S. verfasserin aut Bhattacharya, Dipankar verfasserin aut Balaji, K. verfasserin aut Kumar, Manoj verfasserin aut Kulshresta, Prashanth verfasserin aut Enthalten in Journal of astrophysics and astronomy Bangalore : Springer India, 1980 38(2017), 2 vom: 19. Juni (DE-627)358454131 (DE-600)2096381-6 0973-7758 nnns volume:38 year:2017 number:2 day:19 month:06 https://dx.doi.org/10.1007/s12036-017-9454-9 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4393 GBV_ILN_4700 39.22 ASE AR 38 2017 2 19 06 |
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Enthalten in Journal of astrophysics and astronomy 38(2017), 2 vom: 19. Juni volume:38 year:2017 number:2 day:19 month:06 |
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Ramadevi, M. C. @@aut@@ Ravishankar, B. T. @@aut@@ Sitaramamurthy, N. @@aut@@ Meena, G. @@aut@@ Singh, Brajpal @@aut@@ Jain, Anand @@aut@@ Yadav, Reena @@aut@@ Agarwal, Anil @@aut@@ Babu, V. Chandra @@aut@@ Kushwaha, Ankur @@aut@@ Vaishali, S. @@aut@@ Iyer, Nirmal Kumar @@aut@@ Nandi, Anuj @@aut@@ V., Girish @@aut@@ Agarwal, Vivek Kumar @@aut@@ Seetha, S. @@aut@@ Bhattacharya, Dipankar @@aut@@ Balaji, K. @@aut@@ Kumar, Manoj @@aut@@ Kulshresta, Prashanth @@aut@@ |
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Ramadevi, M. C. |
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Ramadevi, M. C. ddc 520 bkl 39.22 misc X-ray sky monitor misc 1D position sensitive proportional counter misc coded mask misc AstroSat misc X-ray transients Early In-orbit Performance of Scanning Sky Monitor Onboard AstroSat |
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520 ASE 39.22 bkl Early In-orbit Performance of Scanning Sky Monitor Onboard AstroSat X-ray sky monitor (dpeaa)DE-He213 1D position sensitive proportional counter (dpeaa)DE-He213 coded mask (dpeaa)DE-He213 AstroSat (dpeaa)DE-He213 X-ray transients (dpeaa)DE-He213 |
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ddc 520 bkl 39.22 misc X-ray sky monitor misc 1D position sensitive proportional counter misc coded mask misc AstroSat misc X-ray transients |
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ddc 520 bkl 39.22 misc X-ray sky monitor misc 1D position sensitive proportional counter misc coded mask misc AstroSat misc X-ray transients |
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ddc 520 bkl 39.22 misc X-ray sky monitor misc 1D position sensitive proportional counter misc coded mask misc AstroSat misc X-ray transients |
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Early In-orbit Performance of Scanning Sky Monitor Onboard AstroSat |
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Early In-orbit Performance of Scanning Sky Monitor Onboard AstroSat |
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Ramadevi, M. C. |
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Journal of astrophysics and astronomy |
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Ramadevi, M. C. Ravishankar, B. T. Sitaramamurthy, N. Meena, G. Singh, Brajpal Jain, Anand Yadav, Reena Agarwal, Anil Babu, V. Chandra Kushwaha, Ankur Vaishali, S. Iyer, Nirmal Kumar Nandi, Anuj V., Girish Agarwal, Vivek Kumar Seetha, S. Bhattacharya, Dipankar Balaji, K. Kumar, Manoj Kulshresta, Prashanth |
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10.1007/s12036-017-9454-9 |
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verfasserin |
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early in-orbit performance of scanning sky monitor onboard astrosat |
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Early In-orbit Performance of Scanning Sky Monitor Onboard AstroSat |
| abstract |
Abstract We report the in-orbit performance of Scanning Sky Monitor (SSM) onboard AstroSat. The SSM operates in the energy range 2.5 to 10 keV and scans the sky to detect and locate transient X-ray sources. This information of any interesting phenomenon in the X-ray sky as observed by SSM is provided to the astronomical community for follow-up observations. Following the launch of AstroSat on 28th September, 2015, SSM was commissioned on October 12th, 2015. The first power ON of the instrument was with the standard X-ray source, Crab in the field-of-view. The first orbit data revealed the basic expected performance of one of the detectors of SSM, SSM1. Following this in the subsequent orbits, the other detectors were also powered ON to find them perform in good health. Quick checks of the data from the first few orbits revealed that the instrument performed with the expected angular resolution of 12’ %$\times %$ 2.5%$^\circ %$ and effective area in the energy range of interest. This paper discusses the instrument aspects along with few on-board results immediately after power ON. |
| abstractGer |
Abstract We report the in-orbit performance of Scanning Sky Monitor (SSM) onboard AstroSat. The SSM operates in the energy range 2.5 to 10 keV and scans the sky to detect and locate transient X-ray sources. This information of any interesting phenomenon in the X-ray sky as observed by SSM is provided to the astronomical community for follow-up observations. Following the launch of AstroSat on 28th September, 2015, SSM was commissioned on October 12th, 2015. The first power ON of the instrument was with the standard X-ray source, Crab in the field-of-view. The first orbit data revealed the basic expected performance of one of the detectors of SSM, SSM1. Following this in the subsequent orbits, the other detectors were also powered ON to find them perform in good health. Quick checks of the data from the first few orbits revealed that the instrument performed with the expected angular resolution of 12’ %$\times %$ 2.5%$^\circ %$ and effective area in the energy range of interest. This paper discusses the instrument aspects along with few on-board results immediately after power ON. |
| abstract_unstemmed |
Abstract We report the in-orbit performance of Scanning Sky Monitor (SSM) onboard AstroSat. The SSM operates in the energy range 2.5 to 10 keV and scans the sky to detect and locate transient X-ray sources. This information of any interesting phenomenon in the X-ray sky as observed by SSM is provided to the astronomical community for follow-up observations. Following the launch of AstroSat on 28th September, 2015, SSM was commissioned on October 12th, 2015. The first power ON of the instrument was with the standard X-ray source, Crab in the field-of-view. The first orbit data revealed the basic expected performance of one of the detectors of SSM, SSM1. Following this in the subsequent orbits, the other detectors were also powered ON to find them perform in good health. Quick checks of the data from the first few orbits revealed that the instrument performed with the expected angular resolution of 12’ %$\times %$ 2.5%$^\circ %$ and effective area in the energy range of interest. This paper discusses the instrument aspects along with few on-board results immediately after power ON. |
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Early In-orbit Performance of Scanning Sky Monitor Onboard AstroSat |
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Ravishankar, B. T. Sitaramamurthy, N. Meena, G. Singh, Brajpal Jain, Anand Yadav, Reena Agarwal, Anil Babu, V. Chandra Kushwaha, Ankur Vaishali, S. Iyer, Nirmal Kumar Nandi, Anuj V., Girish Agarwal, Vivek Kumar Seetha, S. Bhattacharya, Dipankar Balaji, K. Kumar, Manoj Kulshresta, Prashanth |
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