The Optical Light Curve of GRB 221009A: The Afterglow and the Emerging Supernova

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...

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Published inAstrophysical journal. Letters Vol. 946; no. 1; p. L22
Main Authors Fulton, M. D., Smartt, S. J., Rhodes, L., Huber, M. E., Villar, V. A., Moore, T., Srivastav, S., Schultz, A. S. B., Chambers, K. C., Izzo, L., Hjorth, J., Chen, T.-W., Nicholl, M., Foley, R. J., Rest, A., Smith, K. W., Young, D. R., Sim, S. A., Bright, J., Zenati, Y., de Boer, T., Bulger, J., Fairlamb, J., Gao, H., Lin, C.-C., Lowe, T., Magnier, E. A., Smith, I. A., Wainscoat, R., Coulter, D. A., Jones, D. O., Kilpatrick, C. D., McGill, P., Ramirez-Ruiz, E., Lee, K.-S., Narayan, G., Ramakrishnan, V., Ridden-Harper, R., Singh, A., Wang, Q., Kong, A. K. H., Ngeow, C.-C., Pan, Y.-C., Yang, S., Davis, K. W., Piro, A. L., Rojas-Bravo, C., Sommer, J., Yadavalli, S. K.
Format Journal Article
LanguageEnglish
Published Austin The American Astronomical Society 01.03.2023
IOP Publishing
Subjects
Afterglows
Ejecta
Extinction
Fluctuations
Gamma ray bursts
Gamma rays
Light curve
Light curves
Milky Way
Nickel
Optical astronomy
Photometry
Power law
Red shift
Supernova
Supernovae
Synchrotrons
Type Ic supernovae
X-ray astronomy
X-ray fluxes
X-ray photometry
X-rays
Online AccessGet full text
ISSN2041-8205
2041-8213
2041-8213
DOI10.3847/2041-8213/acc101

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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 × 10 52 erg.
AbstractList 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 × 10 52 erg.
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 ${M}_{\mathrm{ej}}={7.1}_{-1.7}^{+2.4}$ M _⊙ , ${M}_{\mathrm{Ni}}={1.0}_{-0.4}^{+0.6}$ M _⊙ , and ${v}_{\mathrm{ej}}={{\rm{33,900}}}_{-5700}^{+5900}$ km s ^−1 , for the ejecta mass, nickel mass, and ejecta velocity respectively, inferring an explosion energy of E _kin ≃ 2.6–9.0 × 10 ^52 erg.
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 <img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?M_%7Bej%7D=7.1_%7B-1.7%7D%5E%7B+2.4%7DM_%7B%5Codot%7D,M_%7BNi%7D=1.0%5E%7B+0.6%7D_%7B-0.4%7DM_%7B%5Codot%7D" data-classname="equation" />, and <img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?v_%7Bej%7D=33,900%5E%7B+5900%7D_%7B-5700%7D" data-classname="equation" data-title="" /> km s −1 , for the ejecta mass, nickel mass, and ejecta velocity respectively, inferring an explosion energy of  E kin  ≃ 2.6–9.0  ×  10 52  erg.
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 Mg = −19.8 ± 0.6 and Mr = − 19.4 ± 0.3 and Mz = −20.1 ± 0.3. If this is an SN component, then Bayesian modeling of the excess flux would imply explosion parameters of Mej=7.1−1.7+2.4 M⊙, MNi=1.0−0.4+0.6 M⊙, and vej=33,900−5700+5900 km s−1, for the ejecta mass, nickel mass, and ejecta velocity respectively, inferring an explosion energy of Ekin ≃ 2.6–9.0 × 1052 erg.
Author Zenati, Y.
Piro, A. L.
Kilpatrick, C. D.
Smith, K. W.
Smith, I. A.
Singh, A.
Sim, S. A.
de Boer, T.
Villar, V. A.
Ridden-Harper, R.
Moore, T.
Lin, C.-C.
Gao, H.
Lowe, T.
Rojas-Bravo, C.
Lee, K.-S.
Wang, Q.
Coulter, D. A.
Chambers, K. C.
Wainscoat, R.
Kong, A. K. H.
Fairlamb, J.
Smartt, S. J.
Davis, K. W.
Hjorth, J.
Chen, T.-W.
Nicholl, M.
Srivastav, S.
Ramakrishnan, V.
Rhodes, L.
McGill, P.
Huber, M. E.
Izzo, L.
Foley, R. J.
Narayan, G.
Young, D. R.
Magnier, E. A.
Pan, Y.-C.
Ramirez-Ruiz, E.
Schultz, A. S. B.
Rest, A.
Bright, J.
Yang, S.
Fulton, M. D.
Ngeow, C.-C.
Yadavalli, S. K.
Jones, D. O.
Sommer, J.
Bulger, J.
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BackLink https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-234230$$DView record from Swedish Publication Index
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Snippet 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)...
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SubjectTerms Afterglows
Ejecta
Extinction
Fluctuations
Gamma ray bursts
Gamma rays
Light curve
Light curves
Milky Way
Nickel
Optical astronomy
Photometry
Power law
Red shift
Supernova
Supernovae
Synchrotrons
Type Ic supernovae
X-ray astronomy
X-ray fluxes
X-ray photometry
X-rays
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Title The Optical Light Curve of GRB 221009A: The Afterglow and the Emerging Supernova
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