AstroSat view of GRS 1915+105 during the Soft State: Detection of HFQPOs and estimation of Mass and Spin
We report the results of AstroSat observations of GRS 1915\(+\)105 obtained using 100 ks guaranteed-time (GT) during the soft state. The Color-Color Diagram (CCD) indicates a variability class of \(\delta\) with the detection of High Frequency QPO (HFQPO) in the power density spectra (PDS). The HFQP...
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| description | We report the results of AstroSat observations of GRS 1915\(+\)105 obtained using 100 ks guaranteed-time (GT) during the soft state. The Color-Color Diagram (CCD) indicates a variability class of \(\delta\) with the detection of High Frequency QPO (HFQPO) in the power density spectra (PDS). The HFQPO is seen to vary in the frequency range of \(67.96 - 70.62\) Hz with percentage rms \(\sim 0.83 - 1.90\) % and significance varying from \(1.63 - 7.75\). The energy dependent power spectra show that the HFQPO features are dominant only in \(6 - 25\) keV energy band. The broadband energy spectra (\(0.7 - 50\) keV) of SXT (Soft X-ray Telescope) and LAXPC (Large Area X-ray Proportional Counter) modelled with nthComp and powerlaw imply that the source has an extended corona in addition to a compact 'Comptonizing corona' that produces high energy emission and exhibits HFQPOs. The broadband spectral modelling indicates that the source spectra are well described by thermal Comptonization with electron temperature (kT\(_{\rm e}\)) of \(2.07 - 2.43\) keV and photon-index (\(\Gamma_{\rm nth}\)) between \(1.73-2.45\) with an additional powerlaw component of photon-index (\(\Gamma_{\rm PL}\)) between \(2.94 - 3.28\). The norm of nthComp component is high (\(\sim 8\)) during the presence of strong HFQPO and low (\(\sim 3\)) during the absence of HFQPO. Further, we model the energy spectra with the kerrbb model to estimate the accretion rate, mass and spin of the source. Our findings indicate that the source accretes at super-Eddington rate of \(1.17-1.31~ \dot{M}_{\rm Edd}\). Moreover, we find the mass and spin of the source as \(12.44 - 13.09~M_{\odot}\) and \(0.990-0.997\) with \(90\%\) confidence suggesting that GRS 1915\(+\)105 is a maximally rotating stellar mass X-ray binary black hole source. |
| doi_str_mv | 10.48550/arxiv.2010.03782 |
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The Color-Color Diagram (CCD) indicates a variability class of \(\delta\) with the detection of High Frequency QPO (HFQPO) in the power density spectra (PDS). The HFQPO is seen to vary in the frequency range of \(67.96 - 70.62\) Hz with percentage rms \(\sim 0.83 - 1.90\) % and significance varying from \(1.63 - 7.75\). The energy dependent power spectra show that the HFQPO features are dominant only in \(6 - 25\) keV energy band. The broadband energy spectra (\(0.7 - 50\) keV) of SXT (Soft X-ray Telescope) and LAXPC (Large Area X-ray Proportional Counter) modelled with nthComp and powerlaw imply that the source has an extended corona in addition to a compact 'Comptonizing corona' that produces high energy emission and exhibits HFQPOs. The broadband spectral modelling indicates that the source spectra are well described by thermal Comptonization with electron temperature (kT\(_{\rm e}\)) of \(2.07 - 2.43\) keV and photon-index (\(\Gamma_{\rm nth}\)) between \(1.73-2.45\) with an additional powerlaw component of photon-index (\(\Gamma_{\rm PL}\)) between \(2.94 - 3.28\). The norm of nthComp component is high (\(\sim 8\)) during the presence of strong HFQPO and low (\(\sim 3\)) during the absence of HFQPO. Further, we model the energy spectra with the kerrbb model to estimate the accretion rate, mass and spin of the source. Our findings indicate that the source accretes at super-Eddington rate of \(1.17-1.31~ \dot{M}_{\rm Edd}\). Moreover, we find the mass and spin of the source as \(12.44 - 13.09~M_{\odot}\) and \(0.990-0.997\) with \(90\%\) confidence suggesting that GRS 1915\(+\)105 is a maximally rotating stellar mass X-ray binary black hole source.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2010.03782</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Binary stars ; Broadband ; Color-color diagram ; Deposition ; Electron energy ; Energy bands ; Energy spectra ; Frequency ranges ; Photons ; Physics - High Energy Astrophysical Phenomena ; Power spectra ; Proportional counters ; Soft x rays ; Stellar mass ; Stellar rotation ; X ray binaries ; X ray stars ; X ray telescopes</subject><ispartof>arXiv.org, 2020-10</ispartof><rights>2020. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,778,782,883,27912</link.rule.ids><backlink>$$Uhttps://doi.org/10.48550/arXiv.2010.03782$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.1093/mnras/staa3135$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink></links><search><creatorcontrib>Sreehari, H</creatorcontrib><creatorcontrib>Nandi, Anuj</creatorcontrib><creatorcontrib>Das, Santabrata</creatorcontrib><creatorcontrib>Agrawal, V K</creatorcontrib><creatorcontrib>Mandal, Samir</creatorcontrib><creatorcontrib>Ramadevi, M C</creatorcontrib><creatorcontrib>Katoch, Tilak</creatorcontrib><title>AstroSat view of GRS 1915+105 during the Soft State: Detection of HFQPOs and estimation of Mass and Spin</title><title>arXiv.org</title><description>We report the results of AstroSat observations of GRS 1915\(+\)105 obtained using 100 ks guaranteed-time (GT) during the soft state. The Color-Color Diagram (CCD) indicates a variability class of \(\delta\) with the detection of High Frequency QPO (HFQPO) in the power density spectra (PDS). The HFQPO is seen to vary in the frequency range of \(67.96 - 70.62\) Hz with percentage rms \(\sim 0.83 - 1.90\) % and significance varying from \(1.63 - 7.75\). The energy dependent power spectra show that the HFQPO features are dominant only in \(6 - 25\) keV energy band. The broadband energy spectra (\(0.7 - 50\) keV) of SXT (Soft X-ray Telescope) and LAXPC (Large Area X-ray Proportional Counter) modelled with nthComp and powerlaw imply that the source has an extended corona in addition to a compact 'Comptonizing corona' that produces high energy emission and exhibits HFQPOs. The broadband spectral modelling indicates that the source spectra are well described by thermal Comptonization with electron temperature (kT\(_{\rm e}\)) of \(2.07 - 2.43\) keV and photon-index (\(\Gamma_{\rm nth}\)) between \(1.73-2.45\) with an additional powerlaw component of photon-index (\(\Gamma_{\rm PL}\)) between \(2.94 - 3.28\). The norm of nthComp component is high (\(\sim 8\)) during the presence of strong HFQPO and low (\(\sim 3\)) during the absence of HFQPO. Further, we model the energy spectra with the kerrbb model to estimate the accretion rate, mass and spin of the source. Our findings indicate that the source accretes at super-Eddington rate of \(1.17-1.31~ \dot{M}_{\rm Edd}\). Moreover, we find the mass and spin of the source as \(12.44 - 13.09~M_{\odot}\) and \(0.990-0.997\) with \(90\%\) confidence suggesting that GRS 1915\(+\)105 is a maximally rotating stellar mass X-ray binary black hole source.</description><subject>Binary stars</subject><subject>Broadband</subject><subject>Color-color diagram</subject><subject>Deposition</subject><subject>Electron energy</subject><subject>Energy bands</subject><subject>Energy spectra</subject><subject>Frequency ranges</subject><subject>Photons</subject><subject>Physics - High Energy Astrophysical Phenomena</subject><subject>Power spectra</subject><subject>Proportional counters</subject><subject>Soft x rays</subject><subject>Stellar mass</subject><subject>Stellar rotation</subject><subject>X ray binaries</subject><subject>X ray stars</subject><subject>X ray telescopes</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2020</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNo1kE9PwkAUxDcmJhLkA3hyE4-muv9ed-uNoIAJBrXcm7d0KyXaYndB_fYuoKeXzPvNZDKEXHB2owwAu8Xuu97dCBYFJrURJ6QnpOSJUUKckYH3a8aYSLUAkD2yGvrQtTkGuqvdF20rOnnNKc84XHMGtNx2dfNGw8rRvK0CzQMGd0fvXXDLULfN3jAdvzzPPcWmpM6H-gP_H0_oj3K-qZtzclrhu3eDv9sni_HDYjRNZvPJ42g4SxAEJKYqESwipCZVRlueKVNqRKuZcpoLVXGjjckASiOXDtIIOmurlHGU1mayTy6PsYcZik0X-3Q_xX6O4jBHJK6OxKZrP7excbFut10TOxVCqZislQb5C2MEX8E</recordid><startdate>20201008</startdate><enddate>20201008</enddate><creator>Sreehari, H</creator><creator>Nandi, Anuj</creator><creator>Das, Santabrata</creator><creator>Agrawal, V K</creator><creator>Mandal, Samir</creator><creator>Ramadevi, M C</creator><creator>Katoch, Tilak</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20201008</creationdate><title>AstroSat view of GRS 1915+105 during the Soft State: Detection of HFQPOs and estimation of Mass and Spin</title><author>Sreehari, H ; Nandi, Anuj ; Das, Santabrata ; Agrawal, V K ; Mandal, Samir ; Ramadevi, M C ; Katoch, Tilak</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a525-8fda5baa5686487b1948d7aab704e7124f18788955d83ce56568ebbf601a3bb93</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2020</creationdate><topic>Binary stars</topic><topic>Broadband</topic><topic>Color-color diagram</topic><topic>Deposition</topic><topic>Electron energy</topic><topic>Energy bands</topic><topic>Energy spectra</topic><topic>Frequency ranges</topic><topic>Photons</topic><topic>Physics - High Energy Astrophysical Phenomena</topic><topic>Power spectra</topic><topic>Proportional counters</topic><topic>Soft x rays</topic><topic>Stellar mass</topic><topic>Stellar rotation</topic><topic>X ray binaries</topic><topic>X ray stars</topic><topic>X ray telescopes</topic><toplevel>online_resources</toplevel><creatorcontrib>Sreehari, H</creatorcontrib><creatorcontrib>Nandi, Anuj</creatorcontrib><creatorcontrib>Das, Santabrata</creatorcontrib><creatorcontrib>Agrawal, V K</creatorcontrib><creatorcontrib>Mandal, Samir</creatorcontrib><creatorcontrib>Ramadevi, M C</creatorcontrib><creatorcontrib>Katoch, Tilak</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Sreehari, H</au><au>Nandi, Anuj</au><au>Das, Santabrata</au><au>Agrawal, V K</au><au>Mandal, Samir</au><au>Ramadevi, M C</au><au>Katoch, Tilak</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>AstroSat view of GRS 1915+105 during the Soft State: Detection of HFQPOs and estimation of Mass and Spin</atitle><jtitle>arXiv.org</jtitle><date>2020-10-08</date><risdate>2020</risdate><eissn>2331-8422</eissn><abstract>We report the results of AstroSat observations of GRS 1915\(+\)105 obtained using 100 ks guaranteed-time (GT) during the soft state. The Color-Color Diagram (CCD) indicates a variability class of \(\delta\) with the detection of High Frequency QPO (HFQPO) in the power density spectra (PDS). The HFQPO is seen to vary in the frequency range of \(67.96 - 70.62\) Hz with percentage rms \(\sim 0.83 - 1.90\) % and significance varying from \(1.63 - 7.75\). The energy dependent power spectra show that the HFQPO features are dominant only in \(6 - 25\) keV energy band. The broadband energy spectra (\(0.7 - 50\) keV) of SXT (Soft X-ray Telescope) and LAXPC (Large Area X-ray Proportional Counter) modelled with nthComp and powerlaw imply that the source has an extended corona in addition to a compact 'Comptonizing corona' that produces high energy emission and exhibits HFQPOs. The broadband spectral modelling indicates that the source spectra are well described by thermal Comptonization with electron temperature (kT\(_{\rm e}\)) of \(2.07 - 2.43\) keV and photon-index (\(\Gamma_{\rm nth}\)) between \(1.73-2.45\) with an additional powerlaw component of photon-index (\(\Gamma_{\rm PL}\)) between \(2.94 - 3.28\). The norm of nthComp component is high (\(\sim 8\)) during the presence of strong HFQPO and low (\(\sim 3\)) during the absence of HFQPO. Further, we model the energy spectra with the kerrbb model to estimate the accretion rate, mass and spin of the source. Our findings indicate that the source accretes at super-Eddington rate of \(1.17-1.31~ \dot{M}_{\rm Edd}\). Moreover, we find the mass and spin of the source as \(12.44 - 13.09~M_{\odot}\) and \(0.990-0.997\) with \(90\%\) confidence suggesting that GRS 1915\(+\)105 is a maximally rotating stellar mass X-ray binary black hole source.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2010.03782</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Binary stars Broadband Color-color diagram Deposition Electron energy Energy bands Energy spectra Frequency ranges Photons Physics - High Energy Astrophysical Phenomena Power spectra Proportional counters Soft x rays Stellar mass Stellar rotation X ray binaries X ray stars X ray telescopes |
| title | AstroSat view of GRS 1915+105 during the Soft State: Detection of HFQPOs and estimation of Mass and Spin |
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