{
  "bibcode": "2008GCN..7762....1P",
  "body": "K.L. Page, A.P. Beardmore (U. Leicester) and S.T. Holland \n(CRESST/USRA/GSFC) report on behalf of the Swift-XRT and UVOT teams:\n\nA follow-up observation of GRB 080515 was performed about 1.5 days after \nthe initial trigger (Holland et al., GCN Circ. 7721), when the burst was \nno longer Sun-constrained. An X-ray source was identified within the BAT \nground-calculated error circle (Fenimore et al., GCN Circ. 7726). A \nfurther observation, 3.5 days later, confirmed that the source is fading, \nwith alpha = 1.0 +0.7/-0.5. We therefore believe this is the X-ray \nafterglow of the GRB.\n\nThe position of this source is RA, Dec = 3.16343, 32.57894, which is \nequivalent to:\n\nRA(J2000) =   00 12 39.22\nDec(J2000) = +32 34 44.2\n\nwith an uncertainty of 3.8 arcsec (radius, 90% containment). This is 54 \narcsec from the BAT position given by Fenimore et al. in GCN Circ. 7726.\n\nA spectrum of the source can be fitted with a power-law of Gamma = 1.95 \n+/- 0.34, absorbed by the Galactic column of 4.65x10^20 cm^-2. This \nspectrum, averaged over 1.5-6.6 days after the burst, has an observed \n(unabsorbed) flux of 2.28x10^-13 (2.59x10^-13) erg cm^-2 s^-1.\n\nThe field was observed by UVOT with the v filter for 6262 s between \n~1.5 and 2.4 days after the BAT trigger.  The XRT error circle is\nlocated in the scattered light halo of the B = 11.4 star TYC 2264-1051-1, \nso it is not possible to constrain the presence of an afterglow in the \nUVOT data.\n\nThis circular is an official product of the Swift-XRT and UVOT teams.",
  "circularId": 7762,
  "createdOn": 1211464730000,
  "email": "kpa@star.le.ac.uk",
  "subject": "GRB 080515: Swift-XRT position and analysis",
  "submitter": "Kim Page at U.of Leicester  <kpa@star.le.ac.uk>",
  "eventId": "GRB 080515"
}