The Afterglows of Swift-era Gamma-Ray Bursts. I. Comparing pre-Swift and Swift era Long/Soft (Type II) GRB Optical Afterglows
We have gathered optical photometry data from the literature on a large sample of Swift-era gamma-ray burst (GRB) afterglows including GRBs up to September 2009, for a total of 76 GRBs, and present an additional three pre-Swift GRBs not included in an earlier sample. Furthermore, we publish 840 addi...
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| creator | Kann, D A Klose, S Zhang, B Malesani, D Nakar, E Pozanenko, A Wilson, A C Butler, N R Jakobsson, P Schulze, S Andreev, M Antonelli, L A Bikmaev, I F Biryukov, V Böttcher, M Burenin, R A Castro Cerón, J M Castro-Tirado, A J Chincarini, G Cobb, B E Covino, S D'Avanzo, P D'Elia, V M Della Valle A de Ugarte Postigo Efimov, Yu Ferrero, P Fugazza, D Fynbo, J P U Gålfalk, M Grundahl, F Gorosabel, J Gupta, S Guziy, S Hafizov, B Hjorth, J Holhjem, K Ibrahimov, M M Im Israel, G L Jeĺinek, M Jensen, B L Karimov, R Khamitov, I M Kızıloǧlu, Ü Klunko, E Kubánek, P Kutyrev, A S Laursen, P Levan, A J Mannucci, F Martin, C M Mescheryakov, A Mirabal, N Norris, J P J -E Ovaldsen Paraficz, D Pavlenko, E Piranomonte, S Rossi, A Rumyantsev, V Salinas, R Sergeev, A Sharapov, D Sollerman, J Stecklum, B Stella, L Tagliaferri, G Tanvir, N R Telting, J Testa, V Updike, A C Volnova, A Watson, D Wiersema, K D Xu |
| description | We have gathered optical photometry data from the literature on a large sample of Swift-era gamma-ray burst (GRB) afterglows including GRBs up to September 2009, for a total of 76 GRBs, and present an additional three pre-Swift GRBs not included in an earlier sample. Furthermore, we publish 840 additional new photometry data points on a total of 42 GRB afterglows, including large data sets for GRBs 050319, 050408, 050802, 050820A, 050922C, 060418, 080413A and 080810. We analyzed the light curves of all GRBs in the sample and derived spectral energy distributions for the sample with the best data quality, allowing us to estimate the host galaxy extinction. We transformed the afterglow light curves into an extinction-corrected z=1 system and compared their luminosities with a sample of pre-Swift afterglows. The results of a former study, which showed that GRB afterglows clustered and exhibited a bimodal distribution in luminosity space, is weakened by the larger sample. We found that the luminosity distribution of the two afterglow samples (Swift-era and pre-Swift) are very similar, and that a subsample for which we were not able to estimate the extinction, which is fainter than the main sample, can be explained by assuming a moderate amount of line-of-sight host extinction. We derived bolometric isotropic energies for all GRBs in our sample, and found only a tentative correlation between the prompt energy release and the optical afterglow luminosity at one day after the GRB in the z=1 system. A comparative study of the optical luminosities of GRB afterglows with echelle spectra (which show a high number of foreground absorbing systems) and those without reveals no indication that the former are statistically significantly more luminous. (abridged) |
| doi_str_mv | 10.48550/arxiv.0712.2186 |
| format | Article |
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Comparing pre-Swift and Swift era Long/Soft (Type II) GRB Optical Afterglows</title><source>arXiv.org</source><source>Free E- Journals</source><creator>Kann, D A ; Klose, S ; Zhang, B ; Malesani, D ; Nakar, E ; Pozanenko, A ; Wilson, A C ; Butler, N R ; Jakobsson, P ; Schulze, S ; Andreev, M ; Antonelli, L A ; Bikmaev, I F ; Biryukov, V ; Böttcher, M ; Burenin, R A ; Castro Cerón, J M ; Castro-Tirado, A J ; Chincarini, G ; Cobb, B E ; Covino, S ; D'Avanzo, P ; D'Elia, V ; M Della Valle ; A de Ugarte Postigo ; Efimov, Yu ; Ferrero, P ; Fugazza, D ; Fynbo, J P U ; Gålfalk, M ; Grundahl, F ; Gorosabel, J ; Gupta, S ; Guziy, S ; Hafizov, B ; Hjorth, J ; Holhjem, K ; Ibrahimov, M ; M Im ; Israel, G L ; Jeĺinek, M ; Jensen, B L ; Karimov, R ; Khamitov, I M ; Kızıloǧlu, Ü ; Klunko, E ; Kubánek, P ; Kutyrev, A S ; Laursen, P ; Levan, A J ; Mannucci, F ; Martin, C M ; Mescheryakov, A ; Mirabal, N ; Norris, J P ; J -E Ovaldsen ; Paraficz, D ; Pavlenko, E ; Piranomonte, S ; Rossi, A ; Rumyantsev, V ; Salinas, R ; Sergeev, A ; Sharapov, D ; Sollerman, J ; Stecklum, B ; Stella, L ; Tagliaferri, G ; Tanvir, N R ; Telting, J ; Testa, V ; Updike, A C ; Volnova, A ; Watson, D ; Wiersema, K ; D Xu</creator><creatorcontrib>Kann, D A ; Klose, S ; Zhang, B ; Malesani, D ; Nakar, E ; Pozanenko, A ; Wilson, A C ; Butler, N R ; Jakobsson, P ; Schulze, S ; Andreev, M ; Antonelli, L A ; Bikmaev, I F ; Biryukov, V ; Böttcher, M ; Burenin, R A ; Castro Cerón, J M ; Castro-Tirado, A J ; Chincarini, G ; Cobb, B E ; Covino, S ; D'Avanzo, P ; D'Elia, V ; M Della Valle ; A de Ugarte Postigo ; Efimov, Yu ; Ferrero, P ; Fugazza, D ; Fynbo, J P U ; Gålfalk, M ; Grundahl, F ; Gorosabel, J ; Gupta, S ; Guziy, S ; Hafizov, B ; Hjorth, J ; Holhjem, K ; Ibrahimov, M ; M Im ; Israel, G L ; Jeĺinek, M ; Jensen, B L ; Karimov, R ; Khamitov, I M ; Kızıloǧlu, Ü ; Klunko, E ; Kubánek, P ; Kutyrev, A S ; Laursen, P ; Levan, A J ; Mannucci, F ; Martin, C M ; Mescheryakov, A ; Mirabal, N ; Norris, J P ; J -E Ovaldsen ; Paraficz, D ; Pavlenko, E ; Piranomonte, S ; Rossi, A ; Rumyantsev, V ; Salinas, R ; Sergeev, A ; Sharapov, D ; Sollerman, J ; Stecklum, B ; Stella, L ; Tagliaferri, G ; Tanvir, N R ; Telting, J ; Testa, V ; Updike, A C ; Volnova, A ; Watson, D ; Wiersema, K ; D Xu</creatorcontrib><description>We have gathered optical photometry data from the literature on a large sample of Swift-era gamma-ray burst (GRB) afterglows including GRBs up to September 2009, for a total of 76 GRBs, and present an additional three pre-Swift GRBs not included in an earlier sample. Furthermore, we publish 840 additional new photometry data points on a total of 42 GRB afterglows, including large data sets for GRBs 050319, 050408, 050802, 050820A, 050922C, 060418, 080413A and 080810. We analyzed the light curves of all GRBs in the sample and derived spectral energy distributions for the sample with the best data quality, allowing us to estimate the host galaxy extinction. We transformed the afterglow light curves into an extinction-corrected z=1 system and compared their luminosities with a sample of pre-Swift afterglows. The results of a former study, which showed that GRB afterglows clustered and exhibited a bimodal distribution in luminosity space, is weakened by the larger sample. We found that the luminosity distribution of the two afterglow samples (Swift-era and pre-Swift) are very similar, and that a subsample for which we were not able to estimate the extinction, which is fainter than the main sample, can be explained by assuming a moderate amount of line-of-sight host extinction. We derived bolometric isotropic energies for all GRBs in our sample, and found only a tentative correlation between the prompt energy release and the optical afterglow luminosity at one day after the GRB in the z=1 system. A comparative study of the optical luminosities of GRB afterglows with echelle spectra (which show a high number of foreground absorbing systems) and those without reveals no indication that the former are statistically significantly more luminous. (abridged)</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.0712.2186</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Afterglows ; Bolometers ; Comparative studies ; Data points ; Extinction ; Galaxies ; Gamma ray astronomy ; Gamma ray bursts ; Gamma rays ; Light curve ; Luminosity ; Photometry ; Physics - Astrophysics of Galaxies ; Physics - Cosmology and Nongalactic Astrophysics ; Physics - Earth and Planetary Astrophysics ; Physics - High Energy Astrophysical Phenomena ; Physics - Instrumentation and Methods for Astrophysics ; Physics - Solar and Stellar Astrophysics ; Statistical methods</subject><ispartof>arXiv.org, 2010-07</ispartof><rights>2010. 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>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,780,784,885,27924</link.rule.ids><backlink>$$Uhttps://doi.org/10.48550/arXiv.0712.2186$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.1088/0004-637X/720/2/1513$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink></links><search><creatorcontrib>Kann, D A</creatorcontrib><creatorcontrib>Klose, S</creatorcontrib><creatorcontrib>Zhang, B</creatorcontrib><creatorcontrib>Malesani, D</creatorcontrib><creatorcontrib>Nakar, E</creatorcontrib><creatorcontrib>Pozanenko, A</creatorcontrib><creatorcontrib>Wilson, A C</creatorcontrib><creatorcontrib>Butler, N R</creatorcontrib><creatorcontrib>Jakobsson, P</creatorcontrib><creatorcontrib>Schulze, S</creatorcontrib><creatorcontrib>Andreev, M</creatorcontrib><creatorcontrib>Antonelli, L A</creatorcontrib><creatorcontrib>Bikmaev, I F</creatorcontrib><creatorcontrib>Biryukov, V</creatorcontrib><creatorcontrib>Böttcher, M</creatorcontrib><creatorcontrib>Burenin, R A</creatorcontrib><creatorcontrib>Castro Cerón, J M</creatorcontrib><creatorcontrib>Castro-Tirado, A J</creatorcontrib><creatorcontrib>Chincarini, G</creatorcontrib><creatorcontrib>Cobb, B E</creatorcontrib><creatorcontrib>Covino, S</creatorcontrib><creatorcontrib>D'Avanzo, P</creatorcontrib><creatorcontrib>D'Elia, V</creatorcontrib><creatorcontrib>M Della Valle</creatorcontrib><creatorcontrib>A de Ugarte Postigo</creatorcontrib><creatorcontrib>Efimov, Yu</creatorcontrib><creatorcontrib>Ferrero, P</creatorcontrib><creatorcontrib>Fugazza, D</creatorcontrib><creatorcontrib>Fynbo, J P U</creatorcontrib><creatorcontrib>Gålfalk, M</creatorcontrib><creatorcontrib>Grundahl, F</creatorcontrib><creatorcontrib>Gorosabel, J</creatorcontrib><creatorcontrib>Gupta, S</creatorcontrib><creatorcontrib>Guziy, S</creatorcontrib><creatorcontrib>Hafizov, B</creatorcontrib><creatorcontrib>Hjorth, J</creatorcontrib><creatorcontrib>Holhjem, K</creatorcontrib><creatorcontrib>Ibrahimov, M</creatorcontrib><creatorcontrib>M Im</creatorcontrib><creatorcontrib>Israel, G L</creatorcontrib><creatorcontrib>Jeĺinek, M</creatorcontrib><creatorcontrib>Jensen, B L</creatorcontrib><creatorcontrib>Karimov, R</creatorcontrib><creatorcontrib>Khamitov, I M</creatorcontrib><creatorcontrib>Kızıloǧlu, Ü</creatorcontrib><creatorcontrib>Klunko, E</creatorcontrib><creatorcontrib>Kubánek, P</creatorcontrib><creatorcontrib>Kutyrev, A S</creatorcontrib><creatorcontrib>Laursen, P</creatorcontrib><creatorcontrib>Levan, A J</creatorcontrib><creatorcontrib>Mannucci, F</creatorcontrib><creatorcontrib>Martin, C M</creatorcontrib><creatorcontrib>Mescheryakov, A</creatorcontrib><creatorcontrib>Mirabal, N</creatorcontrib><creatorcontrib>Norris, J P</creatorcontrib><creatorcontrib>J -E Ovaldsen</creatorcontrib><creatorcontrib>Paraficz, D</creatorcontrib><creatorcontrib>Pavlenko, E</creatorcontrib><creatorcontrib>Piranomonte, S</creatorcontrib><creatorcontrib>Rossi, A</creatorcontrib><creatorcontrib>Rumyantsev, V</creatorcontrib><creatorcontrib>Salinas, R</creatorcontrib><creatorcontrib>Sergeev, A</creatorcontrib><creatorcontrib>Sharapov, D</creatorcontrib><creatorcontrib>Sollerman, J</creatorcontrib><creatorcontrib>Stecklum, B</creatorcontrib><creatorcontrib>Stella, L</creatorcontrib><creatorcontrib>Tagliaferri, G</creatorcontrib><creatorcontrib>Tanvir, N R</creatorcontrib><creatorcontrib>Telting, J</creatorcontrib><creatorcontrib>Testa, V</creatorcontrib><creatorcontrib>Updike, A C</creatorcontrib><creatorcontrib>Volnova, A</creatorcontrib><creatorcontrib>Watson, D</creatorcontrib><creatorcontrib>Wiersema, K</creatorcontrib><creatorcontrib>D Xu</creatorcontrib><title>The Afterglows of Swift-era Gamma-Ray Bursts. I. Comparing pre-Swift and Swift era Long/Soft (Type II) GRB Optical Afterglows</title><title>arXiv.org</title><description>We have gathered optical photometry data from the literature on a large sample of Swift-era gamma-ray burst (GRB) afterglows including GRBs up to September 2009, for a total of 76 GRBs, and present an additional three pre-Swift GRBs not included in an earlier sample. Furthermore, we publish 840 additional new photometry data points on a total of 42 GRB afterglows, including large data sets for GRBs 050319, 050408, 050802, 050820A, 050922C, 060418, 080413A and 080810. We analyzed the light curves of all GRBs in the sample and derived spectral energy distributions for the sample with the best data quality, allowing us to estimate the host galaxy extinction. We transformed the afterglow light curves into an extinction-corrected z=1 system and compared their luminosities with a sample of pre-Swift afterglows. The results of a former study, which showed that GRB afterglows clustered and exhibited a bimodal distribution in luminosity space, is weakened by the larger sample. We found that the luminosity distribution of the two afterglow samples (Swift-era and pre-Swift) are very similar, and that a subsample for which we were not able to estimate the extinction, which is fainter than the main sample, can be explained by assuming a moderate amount of line-of-sight host extinction. We derived bolometric isotropic energies for all GRBs in our sample, and found only a tentative correlation between the prompt energy release and the optical afterglow luminosity at one day after the GRB in the z=1 system. A comparative study of the optical luminosities of GRB afterglows with echelle spectra (which show a high number of foreground absorbing systems) and those without reveals no indication that the former are statistically significantly more luminous. (abridged)</description><subject>Afterglows</subject><subject>Bolometers</subject><subject>Comparative studies</subject><subject>Data points</subject><subject>Extinction</subject><subject>Galaxies</subject><subject>Gamma ray astronomy</subject><subject>Gamma ray bursts</subject><subject>Gamma rays</subject><subject>Light curve</subject><subject>Luminosity</subject><subject>Photometry</subject><subject>Physics - Astrophysics of Galaxies</subject><subject>Physics - Cosmology and Nongalactic Astrophysics</subject><subject>Physics - Earth and Planetary Astrophysics</subject><subject>Physics - High Energy Astrophysical Phenomena</subject><subject>Physics - Instrumentation and Methods for Astrophysics</subject><subject>Physics - Solar and Stellar Astrophysics</subject><subject>Statistical methods</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2010</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>eNpNkM9rwjAYhsNgMHHedxqBXbZDapofbXJU2bqCIKj3kprEVWzTJXXOw_73Vd1hp5cPnvf7Ph4AHmIcMcE5Hiv_XX1FOI1JRGKR3IABoTRGghFyB0Yh7DDGJEkJ53QAftYfBk5sZ_x2744BOgtXx8p2yHgFM1XXCi3VCU4PPnQhgnkEZ65ula-aLWy9QRcYqkZfa_Bcm7tmO165fnpen1oD8_wFZsspXLRdtVH7f-fuwa1V-2BGfzkEq7fX9ewdzRdZPpvMkeIxRsJumJaamVhaRXSZlmVqueVES8axtpZiXdJSCkU2vBRxn2ViBJOGS0skHYLH69aLmaL1Va38qTgbKs6GeuDpCrTefR5M6IqdO_im_6ggOBUJkYxi-gstx2hk</recordid><startdate>20100716</startdate><enddate>20100716</enddate><creator>Kann, D A</creator><creator>Klose, S</creator><creator>Zhang, B</creator><creator>Malesani, D</creator><creator>Nakar, E</creator><creator>Pozanenko, A</creator><creator>Wilson, A C</creator><creator>Butler, N R</creator><creator>Jakobsson, P</creator><creator>Schulze, S</creator><creator>Andreev, M</creator><creator>Antonelli, L A</creator><creator>Bikmaev, I F</creator><creator>Biryukov, V</creator><creator>Böttcher, M</creator><creator>Burenin, R A</creator><creator>Castro Cerón, J M</creator><creator>Castro-Tirado, A J</creator><creator>Chincarini, G</creator><creator>Cobb, B E</creator><creator>Covino, S</creator><creator>D'Avanzo, P</creator><creator>D'Elia, V</creator><creator>M Della Valle</creator><creator>A de Ugarte Postigo</creator><creator>Efimov, Yu</creator><creator>Ferrero, P</creator><creator>Fugazza, D</creator><creator>Fynbo, J P U</creator><creator>Gålfalk, M</creator><creator>Grundahl, F</creator><creator>Gorosabel, J</creator><creator>Gupta, S</creator><creator>Guziy, S</creator><creator>Hafizov, B</creator><creator>Hjorth, J</creator><creator>Holhjem, K</creator><creator>Ibrahimov, M</creator><creator>M Im</creator><creator>Israel, G L</creator><creator>Jeĺinek, M</creator><creator>Jensen, B L</creator><creator>Karimov, R</creator><creator>Khamitov, I M</creator><creator>Kızıloǧlu, Ü</creator><creator>Klunko, E</creator><creator>Kubánek, P</creator><creator>Kutyrev, A S</creator><creator>Laursen, P</creator><creator>Levan, A J</creator><creator>Mannucci, F</creator><creator>Martin, C M</creator><creator>Mescheryakov, A</creator><creator>Mirabal, N</creator><creator>Norris, J P</creator><creator>J -E Ovaldsen</creator><creator>Paraficz, D</creator><creator>Pavlenko, E</creator><creator>Piranomonte, S</creator><creator>Rossi, A</creator><creator>Rumyantsev, V</creator><creator>Salinas, R</creator><creator>Sergeev, A</creator><creator>Sharapov, D</creator><creator>Sollerman, J</creator><creator>Stecklum, B</creator><creator>Stella, L</creator><creator>Tagliaferri, G</creator><creator>Tanvir, N R</creator><creator>Telting, J</creator><creator>Testa, V</creator><creator>Updike, A C</creator><creator>Volnova, A</creator><creator>Watson, D</creator><creator>Wiersema, K</creator><creator>D Xu</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>20100716</creationdate><title>The Afterglows of Swift-era Gamma-Ray Bursts. I. Comparing pre-Swift and Swift era Long/Soft (Type II) GRB Optical Afterglows</title><author>Kann, D A ; Klose, S ; Zhang, B ; Malesani, D ; Nakar, E ; Pozanenko, A ; Wilson, A C ; Butler, N R ; Jakobsson, P ; Schulze, S ; Andreev, M ; Antonelli, L A ; Bikmaev, I F ; Biryukov, V ; Böttcher, M ; Burenin, R A ; Castro Cerón, J M ; Castro-Tirado, A J ; Chincarini, G ; Cobb, B E ; Covino, S ; D'Avanzo, P ; D'Elia, V ; M Della Valle ; A de Ugarte Postigo ; Efimov, Yu ; Ferrero, P ; Fugazza, D ; Fynbo, J P U ; Gålfalk, M ; Grundahl, F ; Gorosabel, J ; Gupta, S ; Guziy, S ; Hafizov, B ; Hjorth, J ; Holhjem, K ; Ibrahimov, M ; M Im ; Israel, G L ; Jeĺinek, M ; Jensen, B L ; Karimov, R ; Khamitov, I M ; Kızıloǧlu, Ü ; Klunko, E ; Kubánek, P ; Kutyrev, A S ; Laursen, P ; Levan, A J ; Mannucci, F ; Martin, C M ; Mescheryakov, A ; Mirabal, N ; Norris, J P ; J -E Ovaldsen ; Paraficz, D ; Pavlenko, E ; Piranomonte, S ; Rossi, A ; Rumyantsev, V ; Salinas, R ; Sergeev, A ; Sharapov, D ; Sollerman, J ; Stecklum, B ; Stella, L ; Tagliaferri, G ; Tanvir, N R ; Telting, J ; Testa, V ; Updike, A C ; Volnova, A ; Watson, D ; Wiersema, K ; D Xu</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a510-8fc4d9d4e19fa2db7bb7f5f52d9450dff30db3b98a2c5b818a2b6e849e59f293</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2010</creationdate><topic>Afterglows</topic><topic>Bolometers</topic><topic>Comparative studies</topic><topic>Data points</topic><topic>Extinction</topic><topic>Galaxies</topic><topic>Gamma ray astronomy</topic><topic>Gamma ray bursts</topic><topic>Gamma rays</topic><topic>Light curve</topic><topic>Luminosity</topic><topic>Photometry</topic><topic>Physics - Astrophysics of Galaxies</topic><topic>Physics - Cosmology and Nongalactic Astrophysics</topic><topic>Physics - Earth and Planetary Astrophysics</topic><topic>Physics - High Energy Astrophysical Phenomena</topic><topic>Physics - Instrumentation and Methods for Astrophysics</topic><topic>Physics - Solar and Stellar Astrophysics</topic><topic>Statistical methods</topic><toplevel>online_resources</toplevel><creatorcontrib>Kann, D A</creatorcontrib><creatorcontrib>Klose, S</creatorcontrib><creatorcontrib>Zhang, B</creatorcontrib><creatorcontrib>Malesani, D</creatorcontrib><creatorcontrib>Nakar, E</creatorcontrib><creatorcontrib>Pozanenko, A</creatorcontrib><creatorcontrib>Wilson, A C</creatorcontrib><creatorcontrib>Butler, N R</creatorcontrib><creatorcontrib>Jakobsson, P</creatorcontrib><creatorcontrib>Schulze, S</creatorcontrib><creatorcontrib>Andreev, M</creatorcontrib><creatorcontrib>Antonelli, L A</creatorcontrib><creatorcontrib>Bikmaev, I F</creatorcontrib><creatorcontrib>Biryukov, V</creatorcontrib><creatorcontrib>Böttcher, M</creatorcontrib><creatorcontrib>Burenin, R A</creatorcontrib><creatorcontrib>Castro Cerón, J M</creatorcontrib><creatorcontrib>Castro-Tirado, A J</creatorcontrib><creatorcontrib>Chincarini, G</creatorcontrib><creatorcontrib>Cobb, B E</creatorcontrib><creatorcontrib>Covino, S</creatorcontrib><creatorcontrib>D'Avanzo, P</creatorcontrib><creatorcontrib>D'Elia, V</creatorcontrib><creatorcontrib>M Della Valle</creatorcontrib><creatorcontrib>A de Ugarte Postigo</creatorcontrib><creatorcontrib>Efimov, Yu</creatorcontrib><creatorcontrib>Ferrero, P</creatorcontrib><creatorcontrib>Fugazza, D</creatorcontrib><creatorcontrib>Fynbo, J P U</creatorcontrib><creatorcontrib>Gålfalk, M</creatorcontrib><creatorcontrib>Grundahl, F</creatorcontrib><creatorcontrib>Gorosabel, J</creatorcontrib><creatorcontrib>Gupta, S</creatorcontrib><creatorcontrib>Guziy, S</creatorcontrib><creatorcontrib>Hafizov, B</creatorcontrib><creatorcontrib>Hjorth, J</creatorcontrib><creatorcontrib>Holhjem, K</creatorcontrib><creatorcontrib>Ibrahimov, M</creatorcontrib><creatorcontrib>M Im</creatorcontrib><creatorcontrib>Israel, G L</creatorcontrib><creatorcontrib>Jeĺinek, M</creatorcontrib><creatorcontrib>Jensen, B L</creatorcontrib><creatorcontrib>Karimov, R</creatorcontrib><creatorcontrib>Khamitov, I M</creatorcontrib><creatorcontrib>Kızıloǧlu, Ü</creatorcontrib><creatorcontrib>Klunko, E</creatorcontrib><creatorcontrib>Kubánek, P</creatorcontrib><creatorcontrib>Kutyrev, A S</creatorcontrib><creatorcontrib>Laursen, P</creatorcontrib><creatorcontrib>Levan, A J</creatorcontrib><creatorcontrib>Mannucci, F</creatorcontrib><creatorcontrib>Martin, C M</creatorcontrib><creatorcontrib>Mescheryakov, A</creatorcontrib><creatorcontrib>Mirabal, N</creatorcontrib><creatorcontrib>Norris, J P</creatorcontrib><creatorcontrib>J -E Ovaldsen</creatorcontrib><creatorcontrib>Paraficz, D</creatorcontrib><creatorcontrib>Pavlenko, E</creatorcontrib><creatorcontrib>Piranomonte, S</creatorcontrib><creatorcontrib>Rossi, A</creatorcontrib><creatorcontrib>Rumyantsev, V</creatorcontrib><creatorcontrib>Salinas, R</creatorcontrib><creatorcontrib>Sergeev, A</creatorcontrib><creatorcontrib>Sharapov, D</creatorcontrib><creatorcontrib>Sollerman, J</creatorcontrib><creatorcontrib>Stecklum, B</creatorcontrib><creatorcontrib>Stella, L</creatorcontrib><creatorcontrib>Tagliaferri, G</creatorcontrib><creatorcontrib>Tanvir, N R</creatorcontrib><creatorcontrib>Telting, J</creatorcontrib><creatorcontrib>Testa, V</creatorcontrib><creatorcontrib>Updike, A C</creatorcontrib><creatorcontrib>Volnova, A</creatorcontrib><creatorcontrib>Watson, D</creatorcontrib><creatorcontrib>Wiersema, K</creatorcontrib><creatorcontrib>D Xu</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>Kann, D A</au><au>Klose, S</au><au>Zhang, B</au><au>Malesani, D</au><au>Nakar, E</au><au>Pozanenko, A</au><au>Wilson, A C</au><au>Butler, N R</au><au>Jakobsson, P</au><au>Schulze, S</au><au>Andreev, M</au><au>Antonelli, L A</au><au>Bikmaev, I F</au><au>Biryukov, V</au><au>Böttcher, M</au><au>Burenin, R A</au><au>Castro Cerón, J M</au><au>Castro-Tirado, A J</au><au>Chincarini, G</au><au>Cobb, B E</au><au>Covino, S</au><au>D'Avanzo, P</au><au>D'Elia, V</au><au>M Della Valle</au><au>A de Ugarte Postigo</au><au>Efimov, Yu</au><au>Ferrero, P</au><au>Fugazza, D</au><au>Fynbo, J P U</au><au>Gålfalk, M</au><au>Grundahl, F</au><au>Gorosabel, J</au><au>Gupta, S</au><au>Guziy, S</au><au>Hafizov, B</au><au>Hjorth, J</au><au>Holhjem, K</au><au>Ibrahimov, M</au><au>M Im</au><au>Israel, G L</au><au>Jeĺinek, M</au><au>Jensen, B L</au><au>Karimov, R</au><au>Khamitov, I M</au><au>Kızıloǧlu, Ü</au><au>Klunko, E</au><au>Kubánek, P</au><au>Kutyrev, A S</au><au>Laursen, P</au><au>Levan, A J</au><au>Mannucci, F</au><au>Martin, C M</au><au>Mescheryakov, A</au><au>Mirabal, N</au><au>Norris, J P</au><au>J -E Ovaldsen</au><au>Paraficz, D</au><au>Pavlenko, E</au><au>Piranomonte, S</au><au>Rossi, A</au><au>Rumyantsev, V</au><au>Salinas, R</au><au>Sergeev, A</au><au>Sharapov, D</au><au>Sollerman, J</au><au>Stecklum, B</au><au>Stella, L</au><au>Tagliaferri, G</au><au>Tanvir, N R</au><au>Telting, J</au><au>Testa, V</au><au>Updike, A C</au><au>Volnova, A</au><au>Watson, D</au><au>Wiersema, K</au><au>D Xu</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The Afterglows of Swift-era Gamma-Ray Bursts. I. Comparing pre-Swift and Swift era Long/Soft (Type II) GRB Optical Afterglows</atitle><jtitle>arXiv.org</jtitle><date>2010-07-16</date><risdate>2010</risdate><eissn>2331-8422</eissn><abstract>We have gathered optical photometry data from the literature on a large sample of Swift-era gamma-ray burst (GRB) afterglows including GRBs up to September 2009, for a total of 76 GRBs, and present an additional three pre-Swift GRBs not included in an earlier sample. Furthermore, we publish 840 additional new photometry data points on a total of 42 GRB afterglows, including large data sets for GRBs 050319, 050408, 050802, 050820A, 050922C, 060418, 080413A and 080810. We analyzed the light curves of all GRBs in the sample and derived spectral energy distributions for the sample with the best data quality, allowing us to estimate the host galaxy extinction. We transformed the afterglow light curves into an extinction-corrected z=1 system and compared their luminosities with a sample of pre-Swift afterglows. The results of a former study, which showed that GRB afterglows clustered and exhibited a bimodal distribution in luminosity space, is weakened by the larger sample. We found that the luminosity distribution of the two afterglow samples (Swift-era and pre-Swift) are very similar, and that a subsample for which we were not able to estimate the extinction, which is fainter than the main sample, can be explained by assuming a moderate amount of line-of-sight host extinction. We derived bolometric isotropic energies for all GRBs in our sample, and found only a tentative correlation between the prompt energy release and the optical afterglow luminosity at one day after the GRB in the z=1 system. A comparative study of the optical luminosities of GRB afterglows with echelle spectra (which show a high number of foreground absorbing systems) and those without reveals no indication that the former are statistically significantly more luminous. (abridged)</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.0712.2186</doi><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | EISSN: 2331-8422 |
| ispartof | arXiv.org, 2010-07 |
| issn | 2331-8422 |
| language | eng |
| recordid | cdi_arxiv_primary_0712_2186 |
| source | arXiv.org; Free E- Journals |
| subjects | Afterglows Bolometers Comparative studies Data points Extinction Galaxies Gamma ray astronomy Gamma ray bursts Gamma rays Light curve Luminosity Photometry Physics - Astrophysics of Galaxies Physics - Cosmology and Nongalactic Astrophysics Physics - Earth and Planetary Astrophysics Physics - High Energy Astrophysical Phenomena Physics - Instrumentation and Methods for Astrophysics Physics - Solar and Stellar Astrophysics Statistical methods |
| title | The Afterglows of Swift-era Gamma-Ray Bursts. I. Comparing pre-Swift and Swift era Long/Soft (Type II) GRB Optical Afterglows |
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