J/ApJ/795/105 Electromagnetic follow-up with LIGO/Virgo (Singer+, 2014) ================================================================================ The first two years of electromagnetic follow-up with advanced LIGO and Virgo. Singer L.P., Price L.R., Farr B., Urban A.L., Pankow C., Vitale S., Veitch J., Farr W.M., Hanna C., Cannon K., Downes T., Graff P., Haster C.-J., Mandel I., Sidery T., Vecchio A. =2014ApJ...795..105S (SIMBAD/NED BibCode) ================================================================================ ADC_Keywords: Stars, double and multiple ; Polarization ; Stars, distances ; Stars, masses ; Surveys ; Interferometry Keywords: gravitational waves - stars: neutron - surveys Abstract: We anticipate the first direct detections of gravitational waves (GWs) with Advanced LIGO and Virgo later this decade. Though this groundbreaking technical achievement will be its own reward, a still greater prize could be observations of compact binary mergers in both gravitational and electromagnetic channels simultaneously. During Advanced LIGO and Virgo's first two years of operation, 2015 through 2016, we expect the global GW detector array to improve in sensitivity and livetime and expand from two to three detectors. We model the detection rate and the sky localization accuracy for binary neutron star (BNS) mergers across this transition. We have analyzed a large, astrophysically motivated source population using real-time detection and sky localization codes and higher-latency parameter estimation codes that have been expressly built for operation in the Advanced LIGO/Virgo era. We show that for most BNS events, the rapid sky localization, available about a minute after a detection, is as accurate as the full parameter estimation. We demonstrate that Advanced Virgo will play an important role in sky localization, even though it is anticipated to come online with only one-third as much sensitivity as the Advanced LIGO detectors. We find that the median 90% confidence region shrinks from ~500 deg^2^ in 2015 to ~200 deg^2^ in 2016. A few distinct scenarios for the first LIGO/Virgo detections emerge from our simulations. Description: Aasi et al. (2013, arXiv:1304.0670) outline five observing scenarios representing the evolving configuration and capability of the Advanced GW detector array, from the first observing run in 2015, to achieving final design sensitivity in 2019, to adding a fourth detector at design sensitivity by 2022. In this study, we focus on the first two epochs. The first, in 2015, is envisioned as a three-month science run. LIGO Hanford (H) and LIGO Livingston (L) Observatories are operating with an averaged (1.4, 1.4) M_{sun}_ BNS range between 40 and 80 Mpc. The second, in 2016-2017, is a six-month run with H and L operating between 80 and 120 Mpc and the addition of Advanced Virgo (V) with a range between 20 and 60 Mpc. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table2.dat 99 630 Simulated BNS signals for 2015 scenario table3.dat 103 630 Detections and sky localization areas for 2015 scenario table4.dat 99 475 Simulated BNS signals for 2016 scenario table5.dat 103 475 Detections and sky localization areas for 2016 scenario -------------------------------------------------------------------------------- See also: J/ApJ/760/12 : LIGO/Virgo gravitational-wave (GW) bursts with GRBs (Abadie+, 2012) J/ApJ/804/114 : Parameter-estimation performance with LIGO (Berry+, 2015) J/ApJ/813/39 : LIGO gravitational-wave (GW) searches from SNRs (Aasi+, 2015) Byte-by-byte Description of file: table2.dat table4.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 7 A7 --- dID Detection ID (G1) 9- 13 I5 --- sID Simulation ID (G2) 15- 25 F11.5 d MJD MJD of simulated signal (3) 27- 31 F5.1 deg RAdeg Right Ascension; decimal degrees (J2000) 33- 37 F5.1 deg DEdeg Declination; decimal degrees (J2000) 39- 41 I3 deg Inc Binary orbital inclination angle 43- 45 I3 deg PA [] Polarization angle (4) 47- 49 I3 deg Phase Orbital phase at coalescence 51- 53 I3 Mpc Dist Distance 55- 58 F4.2 Msun Mass1 Mass of binary component 1 60- 63 F4.2 Msun Mass2 Mass of binary component 2 65- 69 F5.2 --- Spin1x Spin of binary component 1, x-axis 71- 75 F5.2 --- Spin1y Spin of binary component 1, y-axis 77- 81 F5.2 --- Spin1z Spin of binary component 1, z-axis 83- 87 F5.2 --- Spin2x Spin of binary component 2, x-axis 89- 93 F5.2 --- Spin2y Spin of binary component 2, y-axis 95- 99 F5.2 --- Spin2z Spin of binary component 2, z-axis -------------------------------------------------------------------------------- Note (3): Time of arrival at geocenter of gravitational waves from last stable orbit. Note (4): According to convention in Appendix B of Anderson et al. (2001PhRvD..63d2003A). -------------------------------------------------------------------------------- Byte-by-byte Description of file: table3.dat table5.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 7 A7 --- dID Detection ID (G1) 9- 13 I5 --- sID Simulation ID (G2) 15- 17 A3 --- network Detector network 19- 23 F5.1 --- SNR-net Network signal-to-noise ratio 25- 28 F4.1 --- SNR-H ? Signal-to-noise ratio in H (3) 30- 33 F4.1 --- SNR-L ? Signal-to-noise ratio in L (3) 35- 38 F4.1 --- SNR-V ? Signal-to-noise ratio in V (only in table5.dat) (3) 40- 43 F4.2 Msun Mass1 Recovered mass 1 45- 48 F4.2 Msun Mass2 Recovered mass 2 50- 56 F7.3 deg2 Area50 50% area, BAYESTAR 58- 64 F7.2 deg2 Area90 90% area, BAYESTAR 66- 76 F11.5 deg2 Area Searched area, BAYESTAR 78- 84 F7.3 deg2 pe-area50 ? 50% area, LALINFERENCE_NEST 86- 93 F8.3 deg2 pe-area90 ? 90% area, LALINFERENCE_NEST 95-103 F9.4 deg2 pe-area ? Searched area, LALINFERENCE_NEST -------------------------------------------------------------------------------- Note (3): Blank if SNR<4 or detector is not online. -------------------------------------------------------------------------------- Global notes: Note (G1): Identifier for detection candidate. This is the same value as the coinc_event_id column in the GSTLAL output database and the OBJECT cards in sky map FITS headers, with the 'coinc_event:coinc_event_id:' prefix stripped. Note (G2): Identifier for simulated signal. This is the same value as the simulation_id column in the GSTLAL output database, with the 'sim_inspiral:simulation_id:' prefix stripped. -------------------------------------------------------------------------------- History: From electronic version of the journal ================================================================================ (End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 22-May-2017