Sub-MeV spectroscopy with AstroSat-CZT imager for gamma ray bursts
Abstract Cadmium–Zinc–Telluride Imager (CZTI) onboard AstroSat has been a prolific Gamma-Ray Burst (GRB) monitor. While the 2-pixel Compton scattered events (100–300 keV) are used to extract sensitive spectroscopic information, the inclusion of the low-gain pixels (%$\sim %$20%$\%%$ of the detector...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Chattopadhyay, Tanmoy [verfasserIn] Gupta, Soumya [verfasserIn] Sharma, Vidushi [verfasserIn] Iyyani, Shabnam [verfasserIn] Ratheesh, Ajay [verfasserIn] Mithun, N. P. S. [verfasserIn] Aarthy, E. [verfasserIn] Palit, Sourav [verfasserIn] Kumar, Abhay [verfasserIn] Vadawale, Santosh V. [verfasserIn] Rao, A. R. [verfasserIn] Bhalerao, Varun [verfasserIn] Bhattacharya, Dipankar [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2021 |
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| Schlagwörter: |
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| Anmerkung: |
© Indian Academy of Sciences 2021 |
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| Übergeordnetes Werk: |
Enthalten in: Journal of astrophysics and astronomy - Bangalore : Springer India, 1980, 42(2021), 2 vom: 21. Juli |
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| Übergeordnetes Werk: |
volume:42 ; year:2021 ; number:2 ; day:21 ; month:07 |
| Links: |
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| DOI / URN: |
10.1007/s12036-021-09718-2 |
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| Katalog-ID: |
SPR04461456X |
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| 520 | |a Abstract Cadmium–Zinc–Telluride Imager (CZTI) onboard AstroSat has been a prolific Gamma-Ray Burst (GRB) monitor. While the 2-pixel Compton scattered events (100–300 keV) are used to extract sensitive spectroscopic information, the inclusion of the low-gain pixels (%$\sim %$20%$\%%$ of the detector plane) after careful calibration extends the energy range of Compton energy spectra to 600 keV. The new feature also allows single-pixel spectroscopy of the GRBs to the sub-MeV range which is otherwise limited to 150 keV. We also introduced a new noise rejection algorithm in the analysis (‘Compton noise’). These new additions not only enhances the spectroscopic sensitivity of CZTI, but the sub-MeV spectroscopy will also allow proper characterization of the GRBs not detected by Fermi. This article describes the methodology of single, Compton event and veto spectroscopy in 100–900 keV combined for the GRBs detected in the first year of operation. CZTI in last five years has detected %$\sim %$20 bright GRBs. The new methodologies, when applied on the spectral analysis for this large sample of GRBs, has the potential to improve the results significantly and help in better understanding the prompt emission mechanism. | ||
| 650 | 4 | |a AstroSat |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a CZT imager |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a sub-MeV spectroscopy |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a gamma ray burst |7 (dpeaa)DE-He213 | |
| 700 | 1 | |a Gupta, Soumya |e verfasserin |4 aut | |
| 700 | 1 | |a Sharma, Vidushi |e verfasserin |4 aut | |
| 700 | 1 | |a Iyyani, Shabnam |e verfasserin |4 aut | |
| 700 | 1 | |a Ratheesh, Ajay |e verfasserin |4 aut | |
| 700 | 1 | |a Mithun, N. P. S. |e verfasserin |4 aut | |
| 700 | 1 | |a Aarthy, E. |e verfasserin |4 aut | |
| 700 | 1 | |a Palit, Sourav |e verfasserin |4 aut | |
| 700 | 1 | |a Kumar, Abhay |e verfasserin |4 aut | |
| 700 | 1 | |a Vadawale, Santosh V. |e verfasserin |4 aut | |
| 700 | 1 | |a Rao, A. R. |e verfasserin |4 aut | |
| 700 | 1 | |a Bhalerao, Varun |e verfasserin |4 aut | |
| 700 | 1 | |a Bhattacharya, Dipankar |e verfasserin |4 aut | |
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10.1007/s12036-021-09718-2 doi (DE-627)SPR04461456X (SPR)s12036-021-09718-2-e DE-627 ger DE-627 rakwb eng 520 ASE 39.22 bkl Chattopadhyay, Tanmoy verfasserin aut Sub-MeV spectroscopy with AstroSat-CZT imager for gamma ray bursts 2021 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Indian Academy of Sciences 2021 Abstract Cadmium–Zinc–Telluride Imager (CZTI) onboard AstroSat has been a prolific Gamma-Ray Burst (GRB) monitor. While the 2-pixel Compton scattered events (100–300 keV) are used to extract sensitive spectroscopic information, the inclusion of the low-gain pixels (%$\sim %$20%$\%%$ of the detector plane) after careful calibration extends the energy range of Compton energy spectra to 600 keV. The new feature also allows single-pixel spectroscopy of the GRBs to the sub-MeV range which is otherwise limited to 150 keV. We also introduced a new noise rejection algorithm in the analysis (‘Compton noise’). These new additions not only enhances the spectroscopic sensitivity of CZTI, but the sub-MeV spectroscopy will also allow proper characterization of the GRBs not detected by Fermi. This article describes the methodology of single, Compton event and veto spectroscopy in 100–900 keV combined for the GRBs detected in the first year of operation. CZTI in last five years has detected %$\sim %$20 bright GRBs. The new methodologies, when applied on the spectral analysis for this large sample of GRBs, has the potential to improve the results significantly and help in better understanding the prompt emission mechanism. AstroSat (dpeaa)DE-He213 CZT imager (dpeaa)DE-He213 sub-MeV spectroscopy (dpeaa)DE-He213 gamma ray burst (dpeaa)DE-He213 Gupta, Soumya verfasserin aut Sharma, Vidushi verfasserin aut Iyyani, Shabnam verfasserin aut Ratheesh, Ajay verfasserin aut Mithun, N. P. S. verfasserin aut Aarthy, E. verfasserin aut Palit, Sourav verfasserin aut Kumar, Abhay verfasserin aut Vadawale, Santosh V. verfasserin aut Rao, A. R. verfasserin aut Bhalerao, Varun verfasserin aut Bhattacharya, Dipankar verfasserin aut Enthalten in Journal of astrophysics and astronomy Bangalore : Springer India, 1980 42(2021), 2 vom: 21. Juli (DE-627)358454131 (DE-600)2096381-6 0973-7758 nnns volume:42 year:2021 number:2 day:21 month:07 https://dx.doi.org/10.1007/s12036-021-09718-2 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_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_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_4328 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 42 2021 2 21 07 |
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10.1007/s12036-021-09718-2 doi (DE-627)SPR04461456X (SPR)s12036-021-09718-2-e DE-627 ger DE-627 rakwb eng 520 ASE 39.22 bkl Chattopadhyay, Tanmoy verfasserin aut Sub-MeV spectroscopy with AstroSat-CZT imager for gamma ray bursts 2021 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Indian Academy of Sciences 2021 Abstract Cadmium–Zinc–Telluride Imager (CZTI) onboard AstroSat has been a prolific Gamma-Ray Burst (GRB) monitor. While the 2-pixel Compton scattered events (100–300 keV) are used to extract sensitive spectroscopic information, the inclusion of the low-gain pixels (%$\sim %$20%$\%%$ of the detector plane) after careful calibration extends the energy range of Compton energy spectra to 600 keV. The new feature also allows single-pixel spectroscopy of the GRBs to the sub-MeV range which is otherwise limited to 150 keV. We also introduced a new noise rejection algorithm in the analysis (‘Compton noise’). These new additions not only enhances the spectroscopic sensitivity of CZTI, but the sub-MeV spectroscopy will also allow proper characterization of the GRBs not detected by Fermi. This article describes the methodology of single, Compton event and veto spectroscopy in 100–900 keV combined for the GRBs detected in the first year of operation. CZTI in last five years has detected %$\sim %$20 bright GRBs. The new methodologies, when applied on the spectral analysis for this large sample of GRBs, has the potential to improve the results significantly and help in better understanding the prompt emission mechanism. AstroSat (dpeaa)DE-He213 CZT imager (dpeaa)DE-He213 sub-MeV spectroscopy (dpeaa)DE-He213 gamma ray burst (dpeaa)DE-He213 Gupta, Soumya verfasserin aut Sharma, Vidushi verfasserin aut Iyyani, Shabnam verfasserin aut Ratheesh, Ajay verfasserin aut Mithun, N. P. S. verfasserin aut Aarthy, E. verfasserin aut Palit, Sourav verfasserin aut Kumar, Abhay verfasserin aut Vadawale, Santosh V. verfasserin aut Rao, A. R. verfasserin aut Bhalerao, Varun verfasserin aut Bhattacharya, Dipankar verfasserin aut Enthalten in Journal of astrophysics and astronomy Bangalore : Springer India, 1980 42(2021), 2 vom: 21. Juli (DE-627)358454131 (DE-600)2096381-6 0973-7758 nnns volume:42 year:2021 number:2 day:21 month:07 https://dx.doi.org/10.1007/s12036-021-09718-2 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_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_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_4328 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 42 2021 2 21 07 |
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10.1007/s12036-021-09718-2 doi (DE-627)SPR04461456X (SPR)s12036-021-09718-2-e DE-627 ger DE-627 rakwb eng 520 ASE 39.22 bkl Chattopadhyay, Tanmoy verfasserin aut Sub-MeV spectroscopy with AstroSat-CZT imager for gamma ray bursts 2021 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Indian Academy of Sciences 2021 Abstract Cadmium–Zinc–Telluride Imager (CZTI) onboard AstroSat has been a prolific Gamma-Ray Burst (GRB) monitor. While the 2-pixel Compton scattered events (100–300 keV) are used to extract sensitive spectroscopic information, the inclusion of the low-gain pixels (%$\sim %$20%$\%%$ of the detector plane) after careful calibration extends the energy range of Compton energy spectra to 600 keV. The new feature also allows single-pixel spectroscopy of the GRBs to the sub-MeV range which is otherwise limited to 150 keV. We also introduced a new noise rejection algorithm in the analysis (‘Compton noise’). These new additions not only enhances the spectroscopic sensitivity of CZTI, but the sub-MeV spectroscopy will also allow proper characterization of the GRBs not detected by Fermi. This article describes the methodology of single, Compton event and veto spectroscopy in 100–900 keV combined for the GRBs detected in the first year of operation. CZTI in last five years has detected %$\sim %$20 bright GRBs. The new methodologies, when applied on the spectral analysis for this large sample of GRBs, has the potential to improve the results significantly and help in better understanding the prompt emission mechanism. AstroSat (dpeaa)DE-He213 CZT imager (dpeaa)DE-He213 sub-MeV spectroscopy (dpeaa)DE-He213 gamma ray burst (dpeaa)DE-He213 Gupta, Soumya verfasserin aut Sharma, Vidushi verfasserin aut Iyyani, Shabnam verfasserin aut Ratheesh, Ajay verfasserin aut Mithun, N. P. S. verfasserin aut Aarthy, E. verfasserin aut Palit, Sourav verfasserin aut Kumar, Abhay verfasserin aut Vadawale, Santosh V. verfasserin aut Rao, A. R. verfasserin aut Bhalerao, Varun verfasserin aut Bhattacharya, Dipankar verfasserin aut Enthalten in Journal of astrophysics and astronomy Bangalore : Springer India, 1980 42(2021), 2 vom: 21. Juli (DE-627)358454131 (DE-600)2096381-6 0973-7758 nnns volume:42 year:2021 number:2 day:21 month:07 https://dx.doi.org/10.1007/s12036-021-09718-2 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_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_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_4328 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 42 2021 2 21 07 |
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10.1007/s12036-021-09718-2 doi (DE-627)SPR04461456X (SPR)s12036-021-09718-2-e DE-627 ger DE-627 rakwb eng 520 ASE 39.22 bkl Chattopadhyay, Tanmoy verfasserin aut Sub-MeV spectroscopy with AstroSat-CZT imager for gamma ray bursts 2021 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Indian Academy of Sciences 2021 Abstract Cadmium–Zinc–Telluride Imager (CZTI) onboard AstroSat has been a prolific Gamma-Ray Burst (GRB) monitor. While the 2-pixel Compton scattered events (100–300 keV) are used to extract sensitive spectroscopic information, the inclusion of the low-gain pixels (%$\sim %$20%$\%%$ of the detector plane) after careful calibration extends the energy range of Compton energy spectra to 600 keV. The new feature also allows single-pixel spectroscopy of the GRBs to the sub-MeV range which is otherwise limited to 150 keV. We also introduced a new noise rejection algorithm in the analysis (‘Compton noise’). These new additions not only enhances the spectroscopic sensitivity of CZTI, but the sub-MeV spectroscopy will also allow proper characterization of the GRBs not detected by Fermi. This article describes the methodology of single, Compton event and veto spectroscopy in 100–900 keV combined for the GRBs detected in the first year of operation. CZTI in last five years has detected %$\sim %$20 bright GRBs. The new methodologies, when applied on the spectral analysis for this large sample of GRBs, has the potential to improve the results significantly and help in better understanding the prompt emission mechanism. AstroSat (dpeaa)DE-He213 CZT imager (dpeaa)DE-He213 sub-MeV spectroscopy (dpeaa)DE-He213 gamma ray burst (dpeaa)DE-He213 Gupta, Soumya verfasserin aut Sharma, Vidushi verfasserin aut Iyyani, Shabnam verfasserin aut Ratheesh, Ajay verfasserin aut Mithun, N. P. S. verfasserin aut Aarthy, E. verfasserin aut Palit, Sourav verfasserin aut Kumar, Abhay verfasserin aut Vadawale, Santosh V. verfasserin aut Rao, A. R. verfasserin aut Bhalerao, Varun verfasserin aut Bhattacharya, Dipankar verfasserin aut Enthalten in Journal of astrophysics and astronomy Bangalore : Springer India, 1980 42(2021), 2 vom: 21. Juli (DE-627)358454131 (DE-600)2096381-6 0973-7758 nnns volume:42 year:2021 number:2 day:21 month:07 https://dx.doi.org/10.1007/s12036-021-09718-2 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_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_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_4328 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 42 2021 2 21 07 |
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10.1007/s12036-021-09718-2 doi (DE-627)SPR04461456X (SPR)s12036-021-09718-2-e DE-627 ger DE-627 rakwb eng 520 ASE 39.22 bkl Chattopadhyay, Tanmoy verfasserin aut Sub-MeV spectroscopy with AstroSat-CZT imager for gamma ray bursts 2021 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Indian Academy of Sciences 2021 Abstract Cadmium–Zinc–Telluride Imager (CZTI) onboard AstroSat has been a prolific Gamma-Ray Burst (GRB) monitor. While the 2-pixel Compton scattered events (100–300 keV) are used to extract sensitive spectroscopic information, the inclusion of the low-gain pixels (%$\sim %$20%$\%%$ of the detector plane) after careful calibration extends the energy range of Compton energy spectra to 600 keV. The new feature also allows single-pixel spectroscopy of the GRBs to the sub-MeV range which is otherwise limited to 150 keV. We also introduced a new noise rejection algorithm in the analysis (‘Compton noise’). These new additions not only enhances the spectroscopic sensitivity of CZTI, but the sub-MeV spectroscopy will also allow proper characterization of the GRBs not detected by Fermi. This article describes the methodology of single, Compton event and veto spectroscopy in 100–900 keV combined for the GRBs detected in the first year of operation. CZTI in last five years has detected %$\sim %$20 bright GRBs. The new methodologies, when applied on the spectral analysis for this large sample of GRBs, has the potential to improve the results significantly and help in better understanding the prompt emission mechanism. AstroSat (dpeaa)DE-He213 CZT imager (dpeaa)DE-He213 sub-MeV spectroscopy (dpeaa)DE-He213 gamma ray burst (dpeaa)DE-He213 Gupta, Soumya verfasserin aut Sharma, Vidushi verfasserin aut Iyyani, Shabnam verfasserin aut Ratheesh, Ajay verfasserin aut Mithun, N. P. S. verfasserin aut Aarthy, E. verfasserin aut Palit, Sourav verfasserin aut Kumar, Abhay verfasserin aut Vadawale, Santosh V. verfasserin aut Rao, A. R. verfasserin aut Bhalerao, Varun verfasserin aut Bhattacharya, Dipankar verfasserin aut Enthalten in Journal of astrophysics and astronomy Bangalore : Springer India, 1980 42(2021), 2 vom: 21. Juli (DE-627)358454131 (DE-600)2096381-6 0973-7758 nnns volume:42 year:2021 number:2 day:21 month:07 https://dx.doi.org/10.1007/s12036-021-09718-2 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_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_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_4328 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 42 2021 2 21 07 |
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Enthalten in Journal of astrophysics and astronomy 42(2021), 2 vom: 21. Juli volume:42 year:2021 number:2 day:21 month:07 |
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Chattopadhyay, Tanmoy @@aut@@ Gupta, Soumya @@aut@@ Sharma, Vidushi @@aut@@ Iyyani, Shabnam @@aut@@ Ratheesh, Ajay @@aut@@ Mithun, N. P. S. @@aut@@ Aarthy, E. @@aut@@ Palit, Sourav @@aut@@ Kumar, Abhay @@aut@@ Vadawale, Santosh V. @@aut@@ Rao, A. R. @@aut@@ Bhalerao, Varun @@aut@@ Bhattacharya, Dipankar @@aut@@ |
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<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">SPR04461456X</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20220111110916.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">210722s2021 xx |||||o 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1007/s12036-021-09718-2</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)SPR04461456X</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(SPR)s12036-021-09718-2-e</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">520</subfield><subfield code="q">ASE</subfield></datafield><datafield tag="084" ind1=" " ind2=" "><subfield code="a">39.22</subfield><subfield code="2">bkl</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Chattopadhyay, Tanmoy</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Sub-MeV spectroscopy with AstroSat-CZT imager for gamma ray bursts</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2021</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="500" ind1=" " ind2=" "><subfield code="a">© Indian Academy of Sciences 2021</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract Cadmium–Zinc–Telluride Imager (CZTI) onboard AstroSat has been a prolific Gamma-Ray Burst (GRB) monitor. While the 2-pixel Compton scattered events (100–300 keV) are used to extract sensitive spectroscopic information, the inclusion of the low-gain pixels (%$\sim %$20%$\%%$ of the detector plane) after careful calibration extends the energy range of Compton energy spectra to 600 keV. The new feature also allows single-pixel spectroscopy of the GRBs to the sub-MeV range which is otherwise limited to 150 keV. We also introduced a new noise rejection algorithm in the analysis (‘Compton noise’). These new additions not only enhances the spectroscopic sensitivity of CZTI, but the sub-MeV spectroscopy will also allow proper characterization of the GRBs not detected by Fermi. This article describes the methodology of single, Compton event and veto spectroscopy in 100–900 keV combined for the GRBs detected in the first year of operation. CZTI in last five years has detected %$\sim %$20 bright GRBs. 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|
| author |
Chattopadhyay, Tanmoy |
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Chattopadhyay, Tanmoy ddc 520 bkl 39.22 misc AstroSat misc CZT imager misc sub-MeV spectroscopy misc gamma ray burst Sub-MeV spectroscopy with AstroSat-CZT imager for gamma ray bursts |
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Chattopadhyay, Tanmoy |
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520 - Astronomy & allied sciences |
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0973-7758 |
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520 ASE 39.22 bkl Sub-MeV spectroscopy with AstroSat-CZT imager for gamma ray bursts AstroSat (dpeaa)DE-He213 CZT imager (dpeaa)DE-He213 sub-MeV spectroscopy (dpeaa)DE-He213 gamma ray burst (dpeaa)DE-He213 |
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ddc 520 bkl 39.22 misc AstroSat misc CZT imager misc sub-MeV spectroscopy misc gamma ray burst |
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ddc 520 bkl 39.22 misc AstroSat misc CZT imager misc sub-MeV spectroscopy misc gamma ray burst |
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ddc 520 bkl 39.22 misc AstroSat misc CZT imager misc sub-MeV spectroscopy misc gamma ray burst |
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Elektronische Aufsätze Aufsätze Elektronische Ressource |
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Journal of astrophysics and astronomy |
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Sub-MeV spectroscopy with AstroSat-CZT imager for gamma ray bursts |
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Sub-MeV spectroscopy with AstroSat-CZT imager for gamma ray bursts |
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Chattopadhyay, Tanmoy |
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Journal of astrophysics and astronomy |
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Journal of astrophysics and astronomy |
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eng |
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2021 |
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Chattopadhyay, Tanmoy Gupta, Soumya Sharma, Vidushi Iyyani, Shabnam Ratheesh, Ajay Mithun, N. P. S. Aarthy, E. Palit, Sourav Kumar, Abhay Vadawale, Santosh V. Rao, A. R. Bhalerao, Varun Bhattacharya, Dipankar |
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Elektronische Aufsätze |
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Chattopadhyay, Tanmoy |
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10.1007/s12036-021-09718-2 |
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520 |
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verfasserin |
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sub-mev spectroscopy with astrosat-czt imager for gamma ray bursts |
| title_auth |
Sub-MeV spectroscopy with AstroSat-CZT imager for gamma ray bursts |
| abstract |
Abstract Cadmium–Zinc–Telluride Imager (CZTI) onboard AstroSat has been a prolific Gamma-Ray Burst (GRB) monitor. While the 2-pixel Compton scattered events (100–300 keV) are used to extract sensitive spectroscopic information, the inclusion of the low-gain pixels (%$\sim %$20%$\%%$ of the detector plane) after careful calibration extends the energy range of Compton energy spectra to 600 keV. The new feature also allows single-pixel spectroscopy of the GRBs to the sub-MeV range which is otherwise limited to 150 keV. We also introduced a new noise rejection algorithm in the analysis (‘Compton noise’). These new additions not only enhances the spectroscopic sensitivity of CZTI, but the sub-MeV spectroscopy will also allow proper characterization of the GRBs not detected by Fermi. This article describes the methodology of single, Compton event and veto spectroscopy in 100–900 keV combined for the GRBs detected in the first year of operation. CZTI in last five years has detected %$\sim %$20 bright GRBs. The new methodologies, when applied on the spectral analysis for this large sample of GRBs, has the potential to improve the results significantly and help in better understanding the prompt emission mechanism. © Indian Academy of Sciences 2021 |
| abstractGer |
Abstract Cadmium–Zinc–Telluride Imager (CZTI) onboard AstroSat has been a prolific Gamma-Ray Burst (GRB) monitor. While the 2-pixel Compton scattered events (100–300 keV) are used to extract sensitive spectroscopic information, the inclusion of the low-gain pixels (%$\sim %$20%$\%%$ of the detector plane) after careful calibration extends the energy range of Compton energy spectra to 600 keV. The new feature also allows single-pixel spectroscopy of the GRBs to the sub-MeV range which is otherwise limited to 150 keV. We also introduced a new noise rejection algorithm in the analysis (‘Compton noise’). These new additions not only enhances the spectroscopic sensitivity of CZTI, but the sub-MeV spectroscopy will also allow proper characterization of the GRBs not detected by Fermi. This article describes the methodology of single, Compton event and veto spectroscopy in 100–900 keV combined for the GRBs detected in the first year of operation. CZTI in last five years has detected %$\sim %$20 bright GRBs. The new methodologies, when applied on the spectral analysis for this large sample of GRBs, has the potential to improve the results significantly and help in better understanding the prompt emission mechanism. © Indian Academy of Sciences 2021 |
| abstract_unstemmed |
Abstract Cadmium–Zinc–Telluride Imager (CZTI) onboard AstroSat has been a prolific Gamma-Ray Burst (GRB) monitor. While the 2-pixel Compton scattered events (100–300 keV) are used to extract sensitive spectroscopic information, the inclusion of the low-gain pixels (%$\sim %$20%$\%%$ of the detector plane) after careful calibration extends the energy range of Compton energy spectra to 600 keV. The new feature also allows single-pixel spectroscopy of the GRBs to the sub-MeV range which is otherwise limited to 150 keV. We also introduced a new noise rejection algorithm in the analysis (‘Compton noise’). These new additions not only enhances the spectroscopic sensitivity of CZTI, but the sub-MeV spectroscopy will also allow proper characterization of the GRBs not detected by Fermi. This article describes the methodology of single, Compton event and veto spectroscopy in 100–900 keV combined for the GRBs detected in the first year of operation. CZTI in last five years has detected %$\sim %$20 bright GRBs. The new methodologies, when applied on the spectral analysis for this large sample of GRBs, has the potential to improve the results significantly and help in better understanding the prompt emission mechanism. © Indian Academy of Sciences 2021 |
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Sub-MeV spectroscopy with AstroSat-CZT imager for gamma ray bursts |
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https://dx.doi.org/10.1007/s12036-021-09718-2 |
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Gupta, Soumya Sharma, Vidushi Iyyani, Shabnam Ratheesh, Ajay Mithun, N. P. S. Aarthy, E. Palit, Sourav Kumar, Abhay Vadawale, Santosh V. Rao, A. R. Bhalerao, Varun Bhattacharya, Dipankar |
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Gupta, Soumya Sharma, Vidushi Iyyani, Shabnam Ratheesh, Ajay Mithun, N. P. S. Aarthy, E. Palit, Sourav Kumar, Abhay Vadawale, Santosh V. Rao, A. R. Bhalerao, Varun Bhattacharya, Dipankar |
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|
| score |
7.400978 |