Deep photometry of grb 041006 afterglow

Hypernova bump at redshift z = 0.716

K. Z. Stanek, P. M. Garnavich, P. A. Nutzman, J. D. Hartman, A. Garg, K. Adelberger, P. Berlind, A. Z. Bonanos, M. L. Calkins, P. Challis, B. S. Gaudi, M. J. Holman, R. P. Kirshner, B. A. Mcleod, D. Osip, T. Pimenova, T. H. Reiprich, W. Romanishin, T. Spahr, Stephen C Tegler & 1 others X. Zhao

Research output: Contribution to journalArticle

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Abstract

We present deep optical photometry of the afterglow of gamma-ray burst (GRB) 041006 and its associated hypernova obtained over 65 days after detection (55 R-band epochs on 10 different nights). Our early data (t < 4 days) joined with published GCN data indicate a steepening decay, approaching Fv oc r-0.6 at early times (t ≪ 1 day) and Fv ∞ t-1.3 at late times. The break at tb = 0.16 ± 0.04 days is the earliest reported jet break among all GRB afterglows. During our first night, we obtained 39 exposures spanning 2,. 15 hr from 0.62 to 0.71 days after the burst that reveal a smooth afterglow, with an rms deviation of 0.024 mag from the local power-law fit, consistent with photometric errors. After t ∼ 4 days, the decay slows considerably, and the light curve remains approximately flat at R ∼ 24 mag for a month before decaying by another magnitude to reach R ∼ 25 mag 2 months after the burst. This "bump" is well fit by a k-corrected light curve of supernova SN 1998bw, but only if stretched by a factor of 1.38 in time. In comparison with the other GRB-related SN bumps, GRB 041006 stakes out new parameter space for GRBs/SNe, with a very bright and significantly stretched late-time SN light curve. Within a small sample of fairly well observed GRB/ SN bumps, we see a hint of a possible correlation between their peak luminosity and their "stretch factor," broadly similar to the well-studied Phillips relation for the Type la Supernovae.

Original languageEnglish (US)
JournalAstrophysical Journal
Volume626
Issue number1 II
DOIs
StatePublished - Jun 10 2005

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afterglows
gamma ray bursts
photometry
light curve
night
supernovae
bursts
decay
power law
luminosity
time measurement
deviation

Keywords

  • Galaxies: Distances and redshifts
  • Gamma rays: Bursts
  • Supernovae: General

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Stanek, K. Z., Garnavich, P. M., Nutzman, P. A., Hartman, J. D., Garg, A., Adelberger, K., ... Zhao, X. (2005). Deep photometry of grb 041006 afterglow: Hypernova bump at redshift z = 0.716. Astrophysical Journal, 626(1 II). https://doi.org/10.1086/431361

Deep photometry of grb 041006 afterglow : Hypernova bump at redshift z = 0.716. / Stanek, K. Z.; Garnavich, P. M.; Nutzman, P. A.; Hartman, J. D.; Garg, A.; Adelberger, K.; Berlind, P.; Bonanos, A. Z.; Calkins, M. L.; Challis, P.; Gaudi, B. S.; Holman, M. J.; Kirshner, R. P.; Mcleod, B. A.; Osip, D.; Pimenova, T.; Reiprich, T. H.; Romanishin, W.; Spahr, T.; Tegler, Stephen C; Zhao, X.

In: Astrophysical Journal, Vol. 626, No. 1 II, 10.06.2005.

Research output: Contribution to journalArticle

Stanek, KZ, Garnavich, PM, Nutzman, PA, Hartman, JD, Garg, A, Adelberger, K, Berlind, P, Bonanos, AZ, Calkins, ML, Challis, P, Gaudi, BS, Holman, MJ, Kirshner, RP, Mcleod, BA, Osip, D, Pimenova, T, Reiprich, TH, Romanishin, W, Spahr, T, Tegler, SC & Zhao, X 2005, 'Deep photometry of grb 041006 afterglow: Hypernova bump at redshift z = 0.716', Astrophysical Journal, vol. 626, no. 1 II. https://doi.org/10.1086/431361
Stanek KZ, Garnavich PM, Nutzman PA, Hartman JD, Garg A, Adelberger K et al. Deep photometry of grb 041006 afterglow: Hypernova bump at redshift z = 0.716. Astrophysical Journal. 2005 Jun 10;626(1 II). https://doi.org/10.1086/431361
Stanek, K. Z. ; Garnavich, P. M. ; Nutzman, P. A. ; Hartman, J. D. ; Garg, A. ; Adelberger, K. ; Berlind, P. ; Bonanos, A. Z. ; Calkins, M. L. ; Challis, P. ; Gaudi, B. S. ; Holman, M. J. ; Kirshner, R. P. ; Mcleod, B. A. ; Osip, D. ; Pimenova, T. ; Reiprich, T. H. ; Romanishin, W. ; Spahr, T. ; Tegler, Stephen C ; Zhao, X. / Deep photometry of grb 041006 afterglow : Hypernova bump at redshift z = 0.716. In: Astrophysical Journal. 2005 ; Vol. 626, No. 1 II.
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abstract = "We present deep optical photometry of the afterglow of gamma-ray burst (GRB) 041006 and its associated hypernova obtained over 65 days after detection (55 R-band epochs on 10 different nights). Our early data (t < 4 days) joined with published GCN data indicate a steepening decay, approaching Fv oc r-0.6 at early times (t ≪ 1 day) and Fv ∞ t-1.3 at late times. The break at tb = 0.16 ± 0.04 days is the earliest reported jet break among all GRB afterglows. During our first night, we obtained 39 exposures spanning 2,. 15 hr from 0.62 to 0.71 days after the burst that reveal a smooth afterglow, with an rms deviation of 0.024 mag from the local power-law fit, consistent with photometric errors. After t ∼ 4 days, the decay slows considerably, and the light curve remains approximately flat at R ∼ 24 mag for a month before decaying by another magnitude to reach R ∼ 25 mag 2 months after the burst. This {"}bump{"} is well fit by a k-corrected light curve of supernova SN 1998bw, but only if stretched by a factor of 1.38 in time. In comparison with the other GRB-related SN bumps, GRB 041006 stakes out new parameter space for GRBs/SNe, with a very bright and significantly stretched late-time SN light curve. Within a small sample of fairly well observed GRB/ SN bumps, we see a hint of a possible correlation between their peak luminosity and their {"}stretch factor,{"} broadly similar to the well-studied Phillips relation for the Type la Supernovae.",
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T1 - Deep photometry of grb 041006 afterglow

T2 - Hypernova bump at redshift z = 0.716

AU - Stanek, K. Z.

AU - Garnavich, P. M.

AU - Nutzman, P. A.

AU - Hartman, J. D.

AU - Garg, A.

AU - Adelberger, K.

AU - Berlind, P.

AU - Bonanos, A. Z.

AU - Calkins, M. L.

AU - Challis, P.

AU - Gaudi, B. S.

AU - Holman, M. J.

AU - Kirshner, R. P.

AU - Mcleod, B. A.

AU - Osip, D.

AU - Pimenova, T.

AU - Reiprich, T. H.

AU - Romanishin, W.

AU - Spahr, T.

AU - Tegler, Stephen C

AU - Zhao, X.

PY - 2005/6/10

Y1 - 2005/6/10

N2 - We present deep optical photometry of the afterglow of gamma-ray burst (GRB) 041006 and its associated hypernova obtained over 65 days after detection (55 R-band epochs on 10 different nights). Our early data (t < 4 days) joined with published GCN data indicate a steepening decay, approaching Fv oc r-0.6 at early times (t ≪ 1 day) and Fv ∞ t-1.3 at late times. The break at tb = 0.16 ± 0.04 days is the earliest reported jet break among all GRB afterglows. During our first night, we obtained 39 exposures spanning 2,. 15 hr from 0.62 to 0.71 days after the burst that reveal a smooth afterglow, with an rms deviation of 0.024 mag from the local power-law fit, consistent with photometric errors. After t ∼ 4 days, the decay slows considerably, and the light curve remains approximately flat at R ∼ 24 mag for a month before decaying by another magnitude to reach R ∼ 25 mag 2 months after the burst. This "bump" is well fit by a k-corrected light curve of supernova SN 1998bw, but only if stretched by a factor of 1.38 in time. In comparison with the other GRB-related SN bumps, GRB 041006 stakes out new parameter space for GRBs/SNe, with a very bright and significantly stretched late-time SN light curve. Within a small sample of fairly well observed GRB/ SN bumps, we see a hint of a possible correlation between their peak luminosity and their "stretch factor," broadly similar to the well-studied Phillips relation for the Type la Supernovae.

AB - We present deep optical photometry of the afterglow of gamma-ray burst (GRB) 041006 and its associated hypernova obtained over 65 days after detection (55 R-band epochs on 10 different nights). Our early data (t < 4 days) joined with published GCN data indicate a steepening decay, approaching Fv oc r-0.6 at early times (t ≪ 1 day) and Fv ∞ t-1.3 at late times. The break at tb = 0.16 ± 0.04 days is the earliest reported jet break among all GRB afterglows. During our first night, we obtained 39 exposures spanning 2,. 15 hr from 0.62 to 0.71 days after the burst that reveal a smooth afterglow, with an rms deviation of 0.024 mag from the local power-law fit, consistent with photometric errors. After t ∼ 4 days, the decay slows considerably, and the light curve remains approximately flat at R ∼ 24 mag for a month before decaying by another magnitude to reach R ∼ 25 mag 2 months after the burst. This "bump" is well fit by a k-corrected light curve of supernova SN 1998bw, but only if stretched by a factor of 1.38 in time. In comparison with the other GRB-related SN bumps, GRB 041006 stakes out new parameter space for GRBs/SNe, with a very bright and significantly stretched late-time SN light curve. Within a small sample of fairly well observed GRB/ SN bumps, we see a hint of a possible correlation between their peak luminosity and their "stretch factor," broadly similar to the well-studied Phillips relation for the Type la Supernovae.

KW - Galaxies: Distances and redshifts

KW - Gamma rays: Bursts

KW - Supernovae: General

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