Skip to main content
Testing. You are viewing the public testing version of GCN. For the production version, go to https://gcn.nasa.gov.
New Announcement Feature, Code of Conduct, Circular Revisions. See news and announcements

GCN Circular 16139

Subject
GRB 140419A: Continued RATIR Optical and NIR Observations
Date
2014-04-21T19:19:13Z (10 years ago)
From
Owen Littlejohns at Az State U <olittlej@asu.edu>
Owen Littlejohns (ASU), Nat Butler (ASU), Alan M. Watson (UNAM),
Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer
(UNAM), Chris Klein (UCB), Ori Fox (UCB), J. Xavier Prochaska (UCSC),
Josh Bloom (UCB), Antonino Cucchiara (ORAU/GSFC), Eleonora Troja
(GSFC), Enrico Ramirez-Ruiz (UCSC), Jos�� A. de Diego (UNAM), Leonid
Georgiev (UNAM), Jes��s Gonz��lez (UNAM), Carlos Rom��n-Z����iga (UNAM),
Neil Gehrels (GSFC), and Harvey Moseley (GSFC) report:

We observed the field of GRB 140419A (Marshall, et al., GCN 16118) with
the Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on
the 1.5m Harold Johnson Telescope at the Observatorio Astron��mico Nacional
on Sierra San Pedro M��rtir from 2014/04 21.14 to 2014/04 21.29 UTC (47.30
to 50.93 hours after the BAT trigger), obtaining a total of 2.49 hours
exposure in the r and i bands and 1.04 hours exposure in the Z, Y, J, and
H bands.

We continue to detect the UVOT optical transient (Zheng, et al., GCN 16116;
Guver et al., GCN 16120). For a source located at the position of the KAIT
optical counterpart candidate (Zheng, et al., GCN 16119), in comparison with
the SDSS DR9 and 2MASS, we obtain the following detections and upper limit
(3-sigma):

  r     21.92 +/- 0.07
  i     21.77 +/- 0.07
  Z     21.74 +/- 0.13
  Y     21.58 +/- 0.19
  J     21.54 +/- 0.21
  H     > 21.66

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB. In comparison to the first two
epochs of RATIR observations (Littlejohns, et al., GCN 16136; Butler, et
al., GCN 16121) we note that the decay in the NIR bands appears steeper,
now consistent with 1.4 < alpha < 1.6 in the i, Z, Y, J and H bands (see
also; Xu et al., GCN 16138). The XRT data for this GRB
(http://www.swift.ac.uk/xrt_curves/00596426/) may support a temporal break
at low significance after 100 ks. Further XRTdata can constrain this
possibility.

Conversely, the decay observed in the r band has become shallower, with
alpha = 0.8. This shallow decay in the r band could be attributed to the
presence of an underlying host galaxy or contamination from the nearby
bright star.

We thank the staff of the Observatorio Astron��mico Nacional in San Pedro
M��rtir.
Looking for U.S. government information and services? Visit USA.gov