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GCN Circular 24381

Subject
IceCube-190503A: INTEGRAL prompt observation
Date
2019-05-03T21:42:22Z (5 years ago)
From
James Rodi at IAPS-INAF <james.rodi@inaf.it>
James Rodi (IAPS-Roma, Italy), Sandro Mereghetti (INAF IASF-Milano, Italy)
V. Savchenko, C. Ferrigno (ISDC/UniGE, Switzerland) A. Coleiro (APC, France)

on behalf of the INTEGRAL multi-messenger collaboration:
https://www.astro.unige.ch/cdci/integral-multimessenger-collaboration

Using combination of INTEGRAL all-sky detectors (following Savchenko
et al. 2017, A&A 603, A46): SPI/ACS, IBIS/Veto, and IBIS  we have
performed a search for a prompt gamma-ray counterpart of
IceCube190503A (GCN 24378).

At the time of the event (2019-05-03 17:23:08 UTC, hereafter T0),
INTEGRAL was operating in nominal mode. The peak of the event
localization probability was at an angle of 170 deg with respect to
the spacecraft pointing axis. This orientation implies strongly
suppressed (3% of optimal) response of ISGRI, near-optimal (84% of
optimal) response of IBIS/Veto, and strongly suppressed (38% of
optimal) response of SPI-ACS.



https://analyse.reproducible.online/transients/dashboard/event?utc=2019-...
<https://analyse.reproducible.online/transients/dashboard/event?utc=2019-05-03T17:23:08.72&ra_deg=120.304&dec_deg=6.3568&notice_key=received-1556904219-hash-b82233148e2c3f8a635819b5055c4fff-random-OJANNL2D&parsed=%7B%22dec_deg%22%3A%206.3568%2C%20%22eventid%22%3A%20%22unknown%22%2C%20%22ivorn%22%3A%20%22ivo%3A//nasa.gsfc.gcn/AMON%23ICECUBE_EHE_Event2019-05-03T17%3A23%3A08.72_132508_042419327-463%22%2C%20%22location_kind%22%3A%20%22position%22%2C%20%22lvc_data%22%3A%20%7B%7D%2C%20%22observatory%22%3A%20%22AMON%20%28via%20VO-TAN%29%22%2C%20%22ra_deg%22%3A%20120.304%2C%20%22role%22%3A%20%22observation%22%2C%20%22utc_isot%22%3A%20%222019-05-03T17%3A23%3A08.72%22%7D&integral=%7B%22observations%22%3A%20%7B%22data_readiness%22%3A%20%22NO%20DATA%22%2C%20%22data_readiness_fraction%22%3A%200%2C%20%22hist_png%22%3A%20%22ohist.png%22%2C%20%22history_png%22%3A%20%22ohistory.png%22%2C%20%22in_15deg_fov_ks%22%3A%200%2C%20%22last_cons%22%3A%207045.12982358209%2C%20%22nearest_cons%22%3A%207045.12982358209%2C%20%22orientation_comment%22%3A%20%22bottom%22%2C%20%22sc_phi%22%3A%2010.770955906339958%2C%20%22sc_theta%22%3A%20170.37286701883434%2C%20%22summary_card%22%3A%20%22summary_card.html%22%2C%20%22t0_ijd%22%3A%207062.725207222222%2C%20%22t0_utc%22%3A%20%222019-05-03T17%3A23%3A08.72%22%2C%20%22telapse_cons%22%3A%200%2C%20%22telapse_nrt%22%3A%20856298.7028505537%7D%2C%20%22planning_advice%22%3A%20%7B%22advices%22%3A%20%5B%7B%22importance%22%3A%20%22high%22%2C%20%22reason%22%3A%20%22small%20region%22%7D%5D%2C%20%22distance%22%3A%20null%2C%20%22followup_grade%22%3A%20%22high%22%2C%20%22hasNS%22%3A%200%2C%20%22recommended_action%22%3A%20%7B%22comment%22%3A%20%22small%20region%20%28high%29%22%2C%20%22destination%22%3A%20%5B%22shift%22%2C%20%22core%22%5D%2C%20%22route%22%3A%20%22email%22%7D%2C%20%22visibility_data%22%3A%20%7B%7D%7D%2C%20%22revnum%22%3A%20%222086%22%2C%20%22scwid%22%3A%20%22208600510021%22%2C%20%22visibility%22%3A%20%7B%22visible%22%3A%200.9999999999999999%7D%7D&event_uid=b397a521147cd75e45c864325729d4fb44b002f8b2f658f643695bbe>

The background within +/-300 seconds around the event was very stable
(excess variance 1.2).We have performed a search for any impulsive events
in INTEGRAL SPI-
ACS (as described in Savchenko et al. 2012, A&A 541A, 122S), IBIS, and
IBIS/Veto data.We do not detect any significant counterparts and estimate a
3-sigma
upper limit on the 75-2000 keV fluence of 4e-07 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 peak flux upper limit is ~4.1e-07 (9e-08)
erg/cm^2/s at 1 s (8 s) time scale in 75-2000 keV energy range.
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