RIGHT: R:2700s smoothed image (ca. 1x1 arcmin, N up/left, E left/down) taken with DK-1.5m+DFOSC at June 21, 2006 UT. Seeing is ~1".
The marked position is: (RA,Dec)(J2000.0) = (21:23:32.13, -53:01:36.5).
The circle indicates the refined 3.7" XRT error circle Mangano et al. (GCN 5254).
 

NUMBER:  5277
SUBJECT: GRB060614: Detection of the host galaxy but no supernova emission 
DATE:    06/06/22 

J. P.U. Fynbo, C. C. Thoene, B. L. Jensen, J. Hjorth, J. Sollerman, D. Watson, D. Xu (DARK Cosmology Centre), J.-E. Ovaldsen (Oslo University), U. G. Joergensen, T. Hinse, K. Woller (NBI Copenhagen) report:

We have obtained further imaging of the optical afterglow of GRB060614 (GCN 5252) with the Danish 1.54m telescope and DFOSC on La Silla in the R-band at June 19-21. The afterglow has flattened from the power-law decay reported by Thoene et al. (GCN 5272). Also, the source is clearly resolved in the latest imaging. Hence, the host galaxy is most likely now contributing most of the detected flux. There is not yet any sign of an emerging supernova. Given the low redshift of GRB060614 (GCN 5275, GCN 5276) we can conclude that if there is a supernova associated with GRB060614 it is either intrinsically about 2 magnitudes fainter than SN2006aj (associated with GRB060218) at a similar time or there is substantial dust absorption along the line of sigth to the afterglow.

A plot of the data and fit is available at:
http://www.astro.ku.dk/~brian_j/grb/grb060614/ "

NUMBER:  5271
SUBJECT: GRB060614: optical observations
DATE:    06/06/18 

Christina C. Thoene, Johan P.U. Fynbo, Brian L. Jensen, J. Hjorth, D. Xu (DARK Cosmology Centre), Uffe G. Joergensen, Kristian Woller (NBI Copenhagen) report:

We observed the OT of GRB060614 (GCN 5252) with the Danish 1.54m telescope and DFOSC on La Silla in the R-band at several epochs on June 15-18. A fit to our data leads to a powerlaw decay with a temporal decay index of 1.50. Compared to other data reported in the GCNs is seems that the afterglow in the R- band had a rising lightcurve during the first about 12 hours after the burst and then started the more regular powerlaw decay. In this way the burst qualitatively resembles GRB970508 (Pedersen et al. 1998, ApJ 496, 311).

A plot of the data and fit is available at:
http://www.astro.ku.dk/~brian_j/grb/grb060614/ "