TITLE: GCN CIRCULAR NUMBER: 24624 SUBJECT: LIGO/Virgo S190521g: No counterpart candidates in INTEGRAL SPI/ACS & IBIS/PICsIT prompt observations DATE: 19/05/21 05:51:57 GMT FROM: Maeve Doyle at U College Dublin, Ireland Maeve Doyle (UCD, Ireland), Enrico Bozzo, V. Savchenko, C. Ferrigno (ISDC/UniGE, Switzerland) J. Rodi (IAPS-Roma, Italy) A. Coleiro (APC, France) S. Mereghetti (INAF IASF-Milano, Italy) 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 S190521g (GCN 24621). At the time of the event (2019-05-21 03:02:29 UTC, hereafter T0), INTEGRAL was operating in nominal mode. The peak of the event localization probability was at an angle of 23 deg with respect to the spacecraft pointing axis. This orientation implies strongly suppressed (16% of optimal) response of ISGRI, strongly suppressed (25% of optimal) response of IBIS/Veto, and somewhat suppressed (56% of optimal) response of SPI-ACS. This orientation was relatively favorable for an IBIS/PICsIT observation, which is why we have performed a search for any impulsive signal near the time of the event in INTEGRAL IBIS/PICsIT data. We do not find any significant signal in this data. Furthermore, a fraction of the LIGO/Virgo GW localization probability occurred within the FoV of the coded mask imager IBIS/ISGRI, which is inspected by the INTEGRAL Burst Alert System (IBAS). No IBAS trigger occurred around the time of the event. The background within +/-300 seconds around the event was very stable (excess variance 1.1). We have performed a search for any impulsive events in INTEGRAL SPI- ACS (as described in Savchenko et al. 2012, A&A 541A, 122S) data. We do not detect any significant counterparts and estimate a 3-sigma upper limit on the 75-2000 keV fluence of 1.7e-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 ~1.4e-07 (5.2e-08) erg/cm^2/s at 1 s (8 s) time scale in 75-2000 keV energy range.