Abstract
We present extensive optical photometry of the afterglow of GRB 221009A. Our data cover 0.9-59.9 days from the time of Swift and Fermi gamma-ray burst (GRB) detections. Photometry in rizy-band filters was collected primarily with Pan-STARRS and supplemented by multiple 1-4 m imaging facilities. We analyzed the Swift X-ray data of the afterglow and found a single decline rate power law f(t) ∝ t −1.556±0.002 best describes the light curve. In addition to the high foreground Milky Way dust extinction along this line of sight, the data favor additional extinction to consistently model the optical to X-ray flux with optically thin synchrotron emission. We fit the X-ray-derived power law to the optical light curve and find good agreement with the measured data up to 5−6 days. Thereafter we find a flux excess in the riy bands that peaks in the observer frame at ∼20 days. This excess shares similar light-curve profiles to the Type Ic broad-lined supernovae SN 2016jca and SN 2017iuk once corrected for the GRB redshift of z = 0.151 and arbitrarily scaled. This may be representative of an SN emerging from the declining afterglow. We measure rest-frame absolute peak AB magnitudes of M g = −19.8 ± 0.6 and M r = − 19.4 ± 0.3 and M z = −20.1 ± 0.3. If this is an SN component, then Bayesian modeling of the excess flux would imply explosion parameters of M ej = 7.1 − 1.7 + 2.4 M ⊙, M Ni = 1.0 − 0.4 + 0.6 M ⊙, and v ej = 33,900 − 5700 + 5900 km s−1, for the ejecta mass, nickel mass, and ejecta velocity respectively, inferring an explosion energy of E kin ≃ 2.6-9.0 × 1052 erg.
Original language | English (US) |
---|---|
Article number | L22 |
Journal | Astrophysical Journal Letters |
Volume | 946 |
Issue number | 1 |
DOIs | |
State | Published - Mar 1 2023 |
Funding
Pan-STARRS is a project of the Institute for Astronomy of the University of Hawaii, and is supported by the NASA SSO Near Earth Observation Program under grants 80NSSC18K0971, NNX14AM74G, NNX12AR65G, NNX13AQ47G, NNX08AR22G, 80NSSC21K1572 and by the State of Hawaii. The Pan-STARRS1 Sky Survey data were facilitated by the University of Hawaii, the Pan-STARRS Project Office, the Max Planck Society (MPIA, MPE), Johns Hopkins University, Durham University, University of Edinburgh, Queen’s University Belfast, the Harvard–Smithsonian CfA the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, NASA grant No. NNX08AR22G, NSF grant No. AST-1238877, the University of Maryland, Eotvos Lorand University, and the Los Alamos National Laboratory. The Young Supernova Experiment (YSE) and its research infrastructure is supported by the European Research Council under the European Union’s Horizon 2020 research and innovation program (ERC Grant Agreement 101002652, PI K. Mandel), the Heising-Simons Foundation (2018-0913, PI R. Foley; 2018-0911, PI R. Margutti), NASA (NNG17PX03C, PI R. Foley), NSF (AST-1720756, AST-1815935, PI R. Foley; AST-1909796, AST-1944985, PI R. Margutti), the David & Lucille Packard Foundation (PI R. Foley), VILLUM FONDEN (project 16599, PI J. Hjorth), and the Center for AstroPhysical Surveys (CAPS) at the National Center for Supercomputing Applications (NCSA) and the University of Illinois Urbana-Champaign. S.J.S., K.W.S., and D.Y. acknowledge STFC grants ST/P000312/1. L.I. and J.H. were supported by a VILLUM FONDEN Investigator grant awarded to J.H. (project number 16599). C.D.K. was supported in part by a CIERA Postdoctoral Fellowship. M.N. is supported by the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 948381) and by a Fellowship from the Alan Turing Institute. S.Y. has been supported by the research project grant “Understanding the Dynamic Universe” funded by the Knut and Alice Wallenberg Foundation under Dnr KAW 2018.0067, and the G.R.E.A.T research environment, funded by Vetenskapsrå det, the Swedish Research Council, project number 2016-06012. D.A.C. acknowledges support from the National Science Foundation Graduate Research Fellowship under Grant DGE1339067. The UCSC team is supported in part by NASA grant 80NSSC20K0953, NSF grant AST–1815935, the Gordon & Betty Moore Foundation, the Heising-Simons Foundation, and by a fellowship from the David and Lucile Packard Foundation to R. J. Foley. This work includes data obtained with the Swope Telescope at Las Campanas Observatory, Chile, as part of the Swope Time Domain Key Project (PI: Piro, Co-Is: Drout, Phillips, Holoien, French, Cowperthwaite, Burns, Madore, Foley, Kilpatrick, Rojas-Bravo, Dimitriadis, Hsiao). We thank Abdo Campillay and Yilin Kong Riveros for performing the Swope observations. Data from NOIR DECam supported by proposals 2021A-0275 and 2021B-0325. We thank Lulin staff H.-Y. Hsiao, C.-S. Lin, W.-J. Hou, H.-C. Lin, and J.-K. Guo for observations and data management. T.-W.C. thanks D. B. Malesani for photometric measurement on the SLT GCN circular and Y.-C. Cheng for LOT time. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology. Pan-STARRS is a project of the Institute for Astronomy of the University of Hawaii, and is supported by the NASA SSO Near Earth Observation Program under grants 80NSSC18K0971, NNX14AM74G, NNX12AR65G, NNX13AQ47G, NNX08AR22G, 80NSSC21K1572 and by the State of Hawaii. The Pan-STARRS1 Sky Survey data were facilitated by the University of Hawaii, the Pan-STARRS Project Office, the Max Planck Society (MPIA, MPE), Johns Hopkins University, Durham University, University of Edinburgh, Queen’s University Belfast, the Harvard-Smithsonian CfA the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, NASA grant No. NNX08AR22G, NSF grant No. AST-1238877, the University of Maryland, Eotvos Lorand University, and the Los Alamos National Laboratory. The Young Supernova Experiment (YSE) and its research infrastructure is supported by the European Research Council under the European Union’s Horizon 2020 research and innovation program (ERC Grant Agreement 101002652, PI K. Mandel), the Heising-Simons Foundation (2018-0913, PI R. Foley; 2018-0911, PI R. Margutti), NASA (NNG17PX03C, PI R. Foley), NSF (AST-1720756, AST-1815935, PI R. Foley; AST-1909796, AST-1944985, PI R. Margutti), the David & Lucille Packard Foundation (PI R. Foley), VILLUM FONDEN (project 16599, PI J. Hjorth), and the Center for AstroPhysical Surveys (CAPS) at the National Center for Supercomputing Applications (NCSA) and the University of Illinois Urbana-Champaign. S.J.S., K.W.S., and D.Y. acknowledge STFC grants ST/P000312/1. L.I. and J.H. were supported by a VILLUM FONDEN Investigator grant awarded to J.H. (project number 16599). C.D.K. was supported in part by a CIERA Postdoctoral Fellowship. M.N. is supported by the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 948381) and by a Fellowship from the Alan Turing Institute. S.Y. has been supported by the research project grant “Understanding the Dynamic Universe” funded by the Knut and Alice Wallenberg Foundation under Dnr KAW 2018.0067, and the G.R.E.A.T research environment, funded by Vetenskapsrådet, the Swedish Research Council, project number 2016-06012. D.A.C. acknowledges support from the National Science Foundation Graduate Research Fellowship under Grant DGE1339067. The UCSC team is supported in part by NASA grant 80NSSC20K0953, NSF grant AST-1815935, the Gordon & Betty Moore Foundation, the Heising-Simons Foundation, and by a fellowship from the David and Lucile Packard Foundation to R. J. Foley. This work includes data obtained with the Swope Telescope at Las Campanas Observatory, Chile, as part of the Swope Time Domain Key Project (PI: Piro, Co-Is: Drout, Phillips, Holoien, French, Cowperthwaite, Burns, Madore, Foley, Kilpatrick, Rojas-Bravo, Dimitriadis, Hsiao). We thank Abdo Campillay and Yilin Kong Riveros for performing the Swope observations. Data from NOIR DECam supported by proposals 2021A-0275 and 2021B-0325. We thank Lulin staff H.-Y. Hsiao, C.-S. Lin, W.-J. Hou, H.-C. Lin, and J.-K. Guo for observations and data management. T.-W.C. thanks D. B. Malesani for photometric measurement on the SLT GCN circular and Y.-C. Cheng for LOT time. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology.
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science