TY - JOUR
T1 - Sloan digital sky survey multicolor observations of GRB 010222
AU - Lee, Brian C.
AU - Tucker, Douglas L.
AU - Vanden Berk, Daniel E.
AU - Yanny, Brian
AU - Reichart, Daniel E.
AU - Adelman, Jennifer
AU - Chen, Bing
AU - Harvanek, Mike
AU - Henden, Arne
AU - Ivezić, Željko
AU - Kleinman, Scot
AU - Lamb, Don
AU - Long, Dan
AU - Mcmillan, Russet
AU - Newman, Peter R.
AU - Nitta, Atsuko
AU - Palunas, Povilas
AU - Schneider, Donald P.
AU - Snedden, Steph
AU - York, Don
AU - Briggs, John W.
AU - Brinkmann, J.
AU - Csabai, Istvan
AU - Hennessy, Greg S.
AU - Kent, Stephen
AU - Lupton, Robert
AU - Newberg, Heidi Jo
AU - Stoughton, Chris
PY - 2001/11/1
Y1 - 2001/11/1
N2 - The discovery of an optical counterpart to GRB 010222 (detected by BeppoSAX) was announced 4.4 hr after the burst by Henden. The Sloan Digital Sky Survey's 0.5 m photometric telescope (PT) and 2.5 m survey telescope were used to observe the afterglow of GRB 010222 starting 4.8 hr after the gamma-ray burst. The 0.5 m PT observed the afterglow in five 300 s g*-band exposures over the course of half an hour, measuring a temporal decay rate in this short period of Fv ∝ t-1±0.5. The 2.5 m camera imaged the counterpart nearly simultaneously in five filters (u*, g*, r*, i*, z*), with r* = 18.74 ± 0.02 at 12:10 UT. These multicolor observations, corrected for reddening and the afterglow's temporal decay, are well-fitted by the power law Fv ∝ v-0.90±0.03 with the exception of the u*-band UV flux which is 20% below this slope. We examine possible interpretations of this spectral shape, including source extinction in a star-forming region.
AB - The discovery of an optical counterpart to GRB 010222 (detected by BeppoSAX) was announced 4.4 hr after the burst by Henden. The Sloan Digital Sky Survey's 0.5 m photometric telescope (PT) and 2.5 m survey telescope were used to observe the afterglow of GRB 010222 starting 4.8 hr after the gamma-ray burst. The 0.5 m PT observed the afterglow in five 300 s g*-band exposures over the course of half an hour, measuring a temporal decay rate in this short period of Fv ∝ t-1±0.5. The 2.5 m camera imaged the counterpart nearly simultaneously in five filters (u*, g*, r*, i*, z*), with r* = 18.74 ± 0.02 at 12:10 UT. These multicolor observations, corrected for reddening and the afterglow's temporal decay, are well-fitted by the power law Fv ∝ v-0.90±0.03 with the exception of the u*-band UV flux which is 20% below this slope. We examine possible interpretations of this spectral shape, including source extinction in a star-forming region.
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U2 - 10.1086/322981
DO - 10.1086/322981
M3 - Article
AN - SCOPUS:0035510949
SN - 0004-637X
VL - 561
SP - 183
EP - 188
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1 PART 1
ER -