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.
<Astrophys. J., 795, 105 (2014)>
=2014ApJ...795..105S 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 deg2 in 2015 to ∼200 deg2
in 2016. A few distinct scenarios for the first LIGO/Virgo detections
emerge from our simulations.
Description:
Aasi et al. (2013, 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☉ 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:
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FileName Lrecl Records Explanations
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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
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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
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Bytes Format Units Label Explanations
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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
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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 2001PhRvD..63d2003A).
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Byte-by-byte Description of file: table3.dat table5.dat
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Bytes Format Units Label Explanations
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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
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Note (3): Blank if SNR<4 or detector is not online.
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Global notes:
Note (G1): Identifier for detection candidate. This is the same value as the
coinceventid column in the GSTLAL output database and the OBJECT
cards in sky map FITS headers, with the 'coincevent:coincevent_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
'siminspiral:simulationid:' prefix stripped.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 22-May-2017