TITLE: GCN CIRCULAR NUMBER: 24141 SUBJECT: LIGO/Virgo S190421ar: Identification of a GW compact binary merger candidate DATE: 19/04/22 17:37:44 GMT FROM: Deep Chatterjee at University of Wisconsin, Milwaukee The LIGO Scientific Collaboration and the Virgo Collaboration report: We identified the compact binary merger candidate S190421ar during real-time processing of data from LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1) at 2019-04-21 21:38:56.251 UTC (GPS time: 1239917954.251). The candidate was found by the PyCBC Live [1], CWB [2], GstLAL [3], MBTAOnline [4], and spiir [5] analysis pipelines. S190421ar is an event of interest because its false alarm rate, as determined by the online analysis, is 1.5e-08 Hz, or about one in 2 years. The event's properties can be found at this URL: https://gracedb.ligo.org/superevents/S190421ar The classification of the GW signal, in order of descending probability, is Terrestrial (96%), BBH (4%), BNS (<1%), NSBH (<1%), or MassGap (<1%). We think that BBH probability may be underestimated and the Terrestrial probability may be overestimated; we are reviewing it and will provide an update when available. Assuming the candidate is astrophysical in origin, there is strong evidence against the lighter compact object having a mass < 3 solar masses (HasNS: <1%). Using the masses and spins inferred from the signal, there is strong evidence against matter outside the final compact object (HasRemnant: <1%). One skymap is available at this time and can be retrieved from the GraceDB event page:  * bayestar.fits.gz, an updated localization generated by BAYESTAR [6], distributed via GCN notice about 18 hours after the candidate For the bayestar.fits.gz skymap, the 90% credible region is 1917 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 2281 +/- 697 Mpc (a posteriori mean +/- standard deviation). For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo Public Alerts User Guide .  [1] Nitz et al. PRD 98, 024050 (2018)  [2] Klimenko et al. PRD 93, 042004 (2016)  [3] Messick et al. PRD 95, 042001 (2017)  [4] Adams et al. CQG 33, 175012 (2016)  [5] Hooper et al. PRD 86, 024012 (2012)  [6] Singer & Price PRD 93, 024013 (2016)