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INTEGRAL serendipitous upper limits on FRB180301

ATel #11386; Savchenko, V. (ISDC, University of Geneva, CH); Panessa, F. (IAPS/INAF, Italy); Ferrigno, C.(ISDC, University of Geneva, CH); Keane, E. (Jodrell Bank Observatory, UK); Bazzano, A. (IAPS/INAF, Italy); Burgay, M. (OAC/INAF, Italy); Kuulkers, E. (ESA/ESTEC, The Netherlands); Petroff, E. (ASTRON, The Netherlands); Ubertini, P. (IAPS/INAF, Italy); Diehl, R. (MPE, Germany); the SUPERB team
on 9 Mar 2018; 11:40 UT
Credential Certification: Francesca Panessa (francesca.panessa@iaps.inaf.it)

Subjects: Gamma Ray, Fast Radio Burst

On March 1 at T0 = 07:34:19.76 (UTC), a Fast Radio Burst (FRB180301) was detected during Breakthrough Listen observations with the 21-cm multibeam receiver of the CSIRO Parkes radio telescope (see ATel #11376).

FRB180301 occurred at an angle of 15.6 deg from the INTEGRAL pointing axis at the time of the event, only 0.5 deg from the edge of the IBIS/ISGRI Field of View (FoV). Unfortunately, at this orientation it is not possible to exploit direct coded-mask imaging with IBIS/ISGRI (nor with JEM-X).

We searched the rates of the INTEGRAL "all-sky detectors" (see Savchenko et al. 2017, A&A 603, A46) for any impulsive transients at the time of the FRB. For the given FRB source location, the best sensitivity is achieved with IBIS/ISGRI or SPI-ACS, depending on the source spectrum. The background within +/-300 seconds around the event was very stable. We do not detect any significant counterparts.

We estimate a 3-sigma upper limit on the 75-2000 keV fluence of 4.0e-7 erg/cm^2 for a burst lasting less than 1 s with a characteristic short GRB spectrum (an exponentially cut-off power-law with alpha=-0.5 and Ep=600 keV) occurring at any time in the interval within 300 s around T0. For a typical long GRB spectrum (Band function with alpha=-1, beta=-2.5, and Ep=300 keV), the derived fluence upper limit in 8 s is 1.1e-6 erg/cm^2 in the 75-2000 keV energy range.

FRB180301 was in the FoV of IBIS/ISGRI in the pointings immediately before and after the event. This allows us to derive the following upper limits from these data:

Before the event (UTC 2018-03-01 06:15:33 - 07:11:07):

20 - 40 keV : 290 mCrab or 2.2e-9 erg/cm2/s

40 - 80 keV : 453 mCrab or 3.3e-9 erg/cm2/s

After the event (UTC 2018-03-01 08:11:03 - 09:06:37):

20 - 40 keV : 88 mCrab or 6.8e-10 erg/cm2/s

40 - 80 keV : 146 mCrab or 1.0e-9 erg/cm2/s

INTEGRAL serendipitous upper limits on FRB180301