The afterglow and the host galaxy of GRB 011211

P. Jakobsson, J. Hjorth, J. P U Fynbo, J. Gorosabel, K. Pedersen, I. Burud, A. Levan, C. Kouveliotou, N. Tanvir, A. Fruchter, J. Rhoads, T. Grav, M. W. Hansen, R. Michelsen, M. I. Andersen, B. L. Jensen, H. Pedersen, B. Thomsen, M. Weidinger, S. G. BhargaviR. Cowsik, S. B. Pandey

Research output: Contribution to journalArticle

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Abstract

We present optical, near-infrared, and X-ray observations of the optical afterglow (OA) of the X-ray rich, long-duration gamma-ray burst GRB 011211. Hubble Space Telescope (HST) data obtained 14, 26, 32, and 59 days after the burst, show the host galaxy to have a morphology that is fairly typical of blue galaxies at high redshift. We measure its magnitude to be R = 24.95 ± 0.11. We detect a break in the OA R-band light curve which is naturally accounted for by a collimated outflow geometry. By fitting a broken power-law to the data we find a best fit with a break 1.56 ± 0.02 days after the burst, a pre-break slope of α1 = -0.95 ± 0.02, and a post-break slope of α2 = -2.11 ± 0.07. The UV-optical spectral energy distribution (SED) around 14 hours after the burst is best fit with a power-law with index β = -0.56 ± 0.19 reddened by an SMC-like extinction law with a modest Av = 0.08 ± 0.08 mag. By comparison, from the XMM-Newton X-ray data at around the same time, we find a decay index of αx = -1.62 ± 0.36 and a spectral index of βx = -1.21-0.15 +0.10. Interpolating between the UV-optical and X-ray implies that the cooling frequency is located close to ∼ 1016 Hz in the observer frame at the time of the observations. We argue, using the various temporal and spectral indices above, that the most likely afterglow model is that of a jet expanding into an external environment that has a constant mean density rather than a wind-fed density structure. We estimate the electron energy index for this burst to be p ∼ 2.3.

Original languageEnglish (US)
Pages (from-to)941-947
Number of pages7
JournalAstronomy and Astrophysics
Volume408
Issue number3
DOIs
StatePublished - Sep 2003
Externally publishedYes

Fingerprint

afterglows
galaxies
bursts
power law
x rays
slopes
XMM-Newton telescope
spectral energy distribution
gamma ray bursts
Hubble Space Telescope
newton
light curve
energy
near infrared
extinction
outflow
index
electron energy
cooling
geometry

Keywords

  • Cosmology: Observations
  • Gamma rays: bursts
  • ISM: dust, extinction
  • Stars: supernovae: general

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Jakobsson, P., Hjorth, J., Fynbo, J. P. U., Gorosabel, J., Pedersen, K., Burud, I., ... Pandey, S. B. (2003). The afterglow and the host galaxy of GRB 011211. Astronomy and Astrophysics, 408(3), 941-947. https://doi.org/10.1051/0004-6361:20031044

The afterglow and the host galaxy of GRB 011211. / Jakobsson, P.; Hjorth, J.; Fynbo, J. P U; Gorosabel, J.; Pedersen, K.; Burud, I.; Levan, A.; Kouveliotou, C.; Tanvir, N.; Fruchter, A.; Rhoads, J.; Grav, T.; Hansen, M. W.; Michelsen, R.; Andersen, M. I.; Jensen, B. L.; Pedersen, H.; Thomsen, B.; Weidinger, M.; Bhargavi, S. G.; Cowsik, R.; Pandey, S. B.

In: Astronomy and Astrophysics, Vol. 408, No. 3, 09.2003, p. 941-947.

Research output: Contribution to journalArticle

Jakobsson, P, Hjorth, J, Fynbo, JPU, Gorosabel, J, Pedersen, K, Burud, I, Levan, A, Kouveliotou, C, Tanvir, N, Fruchter, A, Rhoads, J, Grav, T, Hansen, MW, Michelsen, R, Andersen, MI, Jensen, BL, Pedersen, H, Thomsen, B, Weidinger, M, Bhargavi, SG, Cowsik, R & Pandey, SB 2003, 'The afterglow and the host galaxy of GRB 011211', Astronomy and Astrophysics, vol. 408, no. 3, pp. 941-947. https://doi.org/10.1051/0004-6361:20031044
Jakobsson P, Hjorth J, Fynbo JPU, Gorosabel J, Pedersen K, Burud I et al. The afterglow and the host galaxy of GRB 011211. Astronomy and Astrophysics. 2003 Sep;408(3):941-947. https://doi.org/10.1051/0004-6361:20031044
Jakobsson, P. ; Hjorth, J. ; Fynbo, J. P U ; Gorosabel, J. ; Pedersen, K. ; Burud, I. ; Levan, A. ; Kouveliotou, C. ; Tanvir, N. ; Fruchter, A. ; Rhoads, J. ; Grav, T. ; Hansen, M. W. ; Michelsen, R. ; Andersen, M. I. ; Jensen, B. L. ; Pedersen, H. ; Thomsen, B. ; Weidinger, M. ; Bhargavi, S. G. ; Cowsik, R. ; Pandey, S. B. / The afterglow and the host galaxy of GRB 011211. In: Astronomy and Astrophysics. 2003 ; Vol. 408, No. 3. pp. 941-947.
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abstract = "We present optical, near-infrared, and X-ray observations of the optical afterglow (OA) of the X-ray rich, long-duration gamma-ray burst GRB 011211. Hubble Space Telescope (HST) data obtained 14, 26, 32, and 59 days after the burst, show the host galaxy to have a morphology that is fairly typical of blue galaxies at high redshift. We measure its magnitude to be R = 24.95 ± 0.11. We detect a break in the OA R-band light curve which is naturally accounted for by a collimated outflow geometry. By fitting a broken power-law to the data we find a best fit with a break 1.56 ± 0.02 days after the burst, a pre-break slope of α1 = -0.95 ± 0.02, and a post-break slope of α2 = -2.11 ± 0.07. The UV-optical spectral energy distribution (SED) around 14 hours after the burst is best fit with a power-law with index β = -0.56 ± 0.19 reddened by an SMC-like extinction law with a modest Av = 0.08 ± 0.08 mag. By comparison, from the XMM-Newton X-ray data at around the same time, we find a decay index of αx = -1.62 ± 0.36 and a spectral index of βx = -1.21-0.15 +0.10. Interpolating between the UV-optical and X-ray implies that the cooling frequency is located close to ∼ 1016 Hz in the observer frame at the time of the observations. We argue, using the various temporal and spectral indices above, that the most likely afterglow model is that of a jet expanding into an external environment that has a constant mean density rather than a wind-fed density structure. We estimate the electron energy index for this burst to be p ∼ 2.3.",
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AU - Jakobsson, P.

AU - Hjorth, J.

AU - Fynbo, J. P U

AU - Gorosabel, J.

AU - Pedersen, K.

AU - Burud, I.

AU - Levan, A.

AU - Kouveliotou, C.

AU - Tanvir, N.

AU - Fruchter, A.

AU - Rhoads, J.

AU - Grav, T.

AU - Hansen, M. W.

AU - Michelsen, R.

AU - Andersen, M. I.

AU - Jensen, B. L.

AU - Pedersen, H.

AU - Thomsen, B.

AU - Weidinger, M.

AU - Bhargavi, S. G.

AU - Cowsik, R.

AU - Pandey, S. B.

PY - 2003/9

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N2 - We present optical, near-infrared, and X-ray observations of the optical afterglow (OA) of the X-ray rich, long-duration gamma-ray burst GRB 011211. Hubble Space Telescope (HST) data obtained 14, 26, 32, and 59 days after the burst, show the host galaxy to have a morphology that is fairly typical of blue galaxies at high redshift. We measure its magnitude to be R = 24.95 ± 0.11. We detect a break in the OA R-band light curve which is naturally accounted for by a collimated outflow geometry. By fitting a broken power-law to the data we find a best fit with a break 1.56 ± 0.02 days after the burst, a pre-break slope of α1 = -0.95 ± 0.02, and a post-break slope of α2 = -2.11 ± 0.07. The UV-optical spectral energy distribution (SED) around 14 hours after the burst is best fit with a power-law with index β = -0.56 ± 0.19 reddened by an SMC-like extinction law with a modest Av = 0.08 ± 0.08 mag. By comparison, from the XMM-Newton X-ray data at around the same time, we find a decay index of αx = -1.62 ± 0.36 and a spectral index of βx = -1.21-0.15 +0.10. Interpolating between the UV-optical and X-ray implies that the cooling frequency is located close to ∼ 1016 Hz in the observer frame at the time of the observations. We argue, using the various temporal and spectral indices above, that the most likely afterglow model is that of a jet expanding into an external environment that has a constant mean density rather than a wind-fed density structure. We estimate the electron energy index for this burst to be p ∼ 2.3.

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KW - Cosmology: Observations

KW - Gamma rays: bursts

KW - ISM: dust, extinction

KW - Stars: supernovae: general

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