Difference: GCNCIRCULAR21550 ( vs. 1)

P.A. Evans (U. Leicester), J.A. Kennea (PSU), A.A. Breeveld (UCL-MSSL), S. Campana (INAF-OAB), S.B. Cenko (NASA/GSFC), E. Troja (NASA/GSFC/UMCP), P.T. O'Brien (U. Leicester), S.D. Barthelmy (NASA/GSFC), A.P. Beardmore (U. Leicester), D.N. Burrows (PSU), G. Cusumano (INAF-IASF PA), A. D'Ai (INAF-IASFPA), P. D'Avanzo (INAF-OAB), V.D'Elia(ASDC), S.W.K. Emery (UCL-MSSL), P. Giommi (ASI), C. Gronwall (PSU), H.A. Krimm (CRESST/GSFC/USRA), N.P.M. Kuin (UCL-MSSL), A.Y. Lien (GSFC/UMBC), F.E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB), J.A. Nousek (PSU), S.R. Oates (U. Warwick), J.P. Osborne (U. Leicester), C. Pagani (U. Leicester), K.L. Page (U.Leicester), D.M. Palmer (LANL), M. Perri (ASDC), J.L. Racusin (NASA/GSFC), B. Sbarufatti (INAF-OAB/PSU), M.H. Siegel (PSU), G. Tagliaferri (INAF-OAB), A. Tohuvavohu (PSU) report on behalf of the Swift team:

Swift has performed ToO observations of the proposed optical counterpart of LIGO/Virgo G298048 (Coulter et al. LVC GCN 21529). We obtained 2 ks of data from 53.8 to 55.8 ks after the LVC trigger.

No X-ray source is detected at the location of the transient reported by Coulter et al. The 3-sigma upper limit at this location is 4.5e-3 ct/sec. For a typical GRB spectrum this corresponds to 1.8e-13 erg/cm^2/s (0.3-10 keV). Assuming a distance of 40 Mpc this corresponds to a 0.3-10 keV luminosity of 3.5e40 erg/s.

D'Avanzo et al (2014, MNRAS, 442, 2342) compiled the observed 2-10 keV luminosity at 11 hours post-trigger for a complete sample of Swift-detected short GRBs; these were typically of order 1e41-1e43 erg/s. Our measurement corresponds to a 2-10 keV luminosity of 2.3e40 erg/s, ~an order of magnitude fainter than all of the other sGRBs in that paper apart from GRB 080905. However those authors also showed a correlation between Eiso and X-ray afterglow luminosity, so given the low Eiso (Goldstein et al., LVC Circ. 21528) this may not be surprising.

The afterglow is detected in the Swift-UVOT data. Analysis is complicated by the nearby presence the galaxy NGC4993, but we obtain the following magnitudes:

Filter Magnitude Start time Stop time

We note that it is very unusual for an optical counterpart to be found but no X-ray counterpart, especially given the brightness of the optical counterpart. Therefore, if this object is a GRB afterglow, it is atypical compared to the sample of Swift-BAT triggered objects observed to date. We suggest therefore that the object may be a blue (i.e. lanthanide-free) kilonova.

This circular is an official product of the Swift team.

-- ShaonGhosh - 18 Aug 2017