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The Astrophysics of the Binary Neutron Star Merger GW170817/GRB170817A

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The Astrophysics of the Binary Neutron Star Merger GW170817/GRB170817A Black and Gold The Astrophysics of the Binary Neutron Star Merger GW170817/GRB170817A Leo P. Singer, Research Astrophysicist NASA Goddard Space Flight Center 1st GammaSIG Teleconference Outline 1. LIGO/Virgo 2. Discovery, Observing Strategies 3. Optical and Near Infrared Observations 4. Interpretation, Radio 5. A Few Open Questions 1. LIGO / Virgo VIRGO CASCINA, ITALY Upgrades completed and Advanced Virgo ADVANCED VIRGO became operational in August 2017. Main commences observations enhancements over initial Virgo: • Increased finesse of arm cavities 20 Test masses heavier, lower absorption, 10− Virgo • higher surface quality Hanford Livingston • Size of beam doubled (vacuum system and 21 input/output optics modified accordingly) 10− Hz) p • More robust control of final pendulum stage 22 Not in this talk: LIGO/Virgo sensitivity 10− improvements in software developed and Strain (1/ deployed in O2 23 10− • Feed-forward noise subtraction • Glitch removal by masking or subtraction 100 1000 LVC 2017, PRL • Fully coherent rapid localization for Frequency (Hz) inhomogeneous networks of detectors Advanced GW Detectors LIGO Hanford Operational since 2015/08 Advanced GW Detectors LIGO Hanford Operational since 2015/08 LIGO Livingston Advanced GW Detectors Operational since 2015/08 LIGO Hanford Virgo Operational since 2015/08 Operational since 2017/08 LIGO Livingston Advanced GW Detectors Operational since 2015/08 AUGUST 14, 2017, 10:30:43 UTC: the first BBH signal observed with Virgo Hanford Livingston Virgo 14 12 LVC 2017, PRL • Signal arrived first at Livingston, 10 then 8.4 ms later at Hanford, then 8 SNR 6 6.6 ms later at Virgo 4 2 • Clearly visible chirp trace in Hanford 0 5.0 and Livingston spectrograms; faint 4.5 256 4.0 telltale visible in Virgo 3.5 128 3.0 •2.5 Independently detected in low 64 2.0 1.5 latency within 30s of data Frequency [Hz] 32 1.0 0.5 acquisition by two real-time Normalized Amplitude 16 0.0 ] 1.0 searches for compact binary inspiral -21 2 5 5 signals: GstLAL (see C. Hanna’s 0.5 colloquium at GSFC on October 31) 0.0 0 0 0 noise and PyCBC σ 0.5 − 5 Initial matched-filter signal to noise 5 − 2• − − Whitened Strain [10 1.0 − 0.46 0.48 0.50 0.52 0.54 0.56 0.46 0.48 0.50 0.52 0.54 0.56 0.46 0.48 0.50 0.52 0.54 0.56 ratios in H/L/V: 7.3/13.7/4.4 Time [s] Time [s] Time [s] OCTOBER 14, 2017, 10:30:43 UTC: the first GW signal observed with Virgo • A 31 on 25 M⊙ binary black hole merger • Thanks to additional detector baseline, localized to 60 deg2 • First measurement of gravitational-wave polarization: confirmation of tensor nature of gravitational waves as predicted by GR • More detailed tests of GR in progress Credit: LIGO/Virgo/NASA/Leo Singer PHYSICAL REVIEW LETTERS week ending PRL 119, 161101 (2017) AUGUST20 OCTOBER 17, 2017 2017, 12∶41:04 UTC ∼100 s (calculated starting from 24 Hz) in the detectors’ sensitive band, the inspiral signal ended at 12 41:04.4 UTC. the first gravitational wave signal from a binary neutron star merger In addition, a γ-ray burst was observed 1.7∶ s after the coalescence time [39–45]. The combination of data from Detected in low latency in Hanford data. Chirp track clearly the LIGO and Virgo detectors allowed a precise sky • position localization to an area of 28 deg2. This measure- visible, long duration immediately implied a low mass binary PHYSICAL REVIEW LETTERS week ending PRL 119, 161101ment enabled (2017) an electromagnetic follow-up campaign that 20 OCTOBERmerger 2017 ! identified a counterpart near the galaxy NGC 4993, con- PHYSICAL REVIEW LETTERS week ending sistent with the localization and distance inferred from PRL 119, 161101 (2017) 20 OCTOBER 2017 Additionally, a short instrumental noise transient gravitational-wave data [46–50]. Additionally, a short instrumental noise transient • Chirp visible in Livingston too, but did not trigger due to a appeared in theFrom LIGO-Livingston the gravitational-wave detector signal, 1.1 the best s before measured appeared in the LIGO-Livingston detector 1.1 s before photodiode saturation glitch. the coalescencecombination time of GW170817 of the masses as is shown the chirp in Fig. mass2.[51] the coalescence time of GW170817 as shown in Fig. 2. 0.004 This transient noise, or glitch [71], produced a very brief This transientM noise,1.188 or−þ glitch0.002 M [71]. From, produced the union a of very 90% brief credible (less than 5 ms) saturation in the digital-to-analog converter ¼ ⊙ • No chirp visible in Virgo. (less than 5 ms)intervals saturation obtained in the using digital-to-analog different waveform converter models (see of the feedback signal controlling the position of the test Sec. IV for details), the total mass of the system is between masses. Similar glitches are registered roughly once every of the feedback2.73 signal and 3.29 controllingM . The individual the position masses of are the in the test broad few hours in each of the LIGO detectors with no temporal • H/L/V signal to noise ratio after noise subtraction and glitch ⊙ correlation between the LIGO sites. Their cause remains masses. Similarrange glitches of 0.86 are to 2.26 registeredM , due to roughly correlations once between every their unknown. To mitigate the effect on the results presented in ⊙ removal: 18.8/26.4/2.0 few hours in eachuncertainties. of the LIGO This suggests detectors a BNS with as no the temporal source of the Sec. III, the search analyses applied a window function to gravitational-wave signal, as the total masses of known zero out the data around the glitch [72,73], following the correlation between the LIGO sites. Their cause remains treatment of other high-amplitude glitches used in the BNS systems are between 2.57 and 2.88 M with compo- • Component masses: 1.4–1.6 on 1.2—1.4 M⊙ unknown. To mitigate the effect on the results presented⊙ in O1 analysis [74]. To accurately determine the properties nents between 1.17 and ∼1.6 M [52]. Neutron stars in of GW170817 (as reported in Sec. IV) in addition to the Sec. III, the searchgeneral analyses have precisely applied measured a window masses⊙ as function large as 2 to.01 noise subtraction described above, the glitch was modeled 2 zero out the data0.04 aroundM [53], the whereas glitch stellar-mass[72,73], black following holes found the Æ in with a time-frequency wavelet reconstruction [75] and • Localized to only 30 deg and 26–48 Mpc despite weak/ binaries⊙ in our galaxy have masses substantially greater subtracted from the data, as shown in Fig. 2. unresolved signal in Virgo due to proximity to antenna treatment of other high-amplitude glitches used in the Following the procedures developed for prior gravita- than the components of GW170817 [54 56]. O1 analysis [74]. To accurately determine the– properties tional-waveLVC detections 2017,[29,78], we concludePRL there is no pattern null Gravitational-wave observations alone are able to mea- environmental disturbance observed by LIGO environmen- of GW170817sure (as the reported masses of in the Sec. two objectsIV) in and addition set a lower to limit the on tal sensors [79] that could account for the GW170817 FIG. 2. Mitigation of the glitch in LIGO-Livingston data. Times their compactness, but the results presented here do not signal. are shown relative to August 17, 2017 12 41:04 UTC. Top panel: noise subtraction described above, the glitch was modeled ∶ exclude objects more compact than neutron stars such as The Virgo data, used for sky localization and an A time-frequency representation [65] of the raw LIGO-Living- with a time-frequency wavelet reconstruction [75] and estimation of the source properties, are shown in the ston data used in the initial identification of GW170817 [76]. The FIG. 1. Time-frequency representations [65] of data containing subtracted fromquark the stars, data, black as shown holes, or in more Fig. exotic2. objects [57–61]. bottom panel of Fig. 1. The Virgo data are nonstationary coalescence time reported by the search is at time 0.4 s in this The detection of GRB 170817A and subsequent electro- the gravitational-waveabove 150 Hz due to scattered event light from the GW170817, output optics figure and observed the glitch occurs 1.1 by s before the this time. LIGO- The time- Following themagnetic procedures emission developed demonstrates for the prior presence gravita- of matter. Hanford (top),modulated by LIGO-Livingston alignment fluctuations and below 30 Hz due (middle),frequency track and of GW170817 Virgo is clearly visible (bottom) despite the detectors.to Times seismic noise are from anthropogenic shown activity. relative Occasional topresence August of the glitch. 17,Bottom 2017panel: The raw 12 LIGO-Livingston41:04 tional-wave detectionsMoreover, although[29,78] a, neutron we conclude star black hole there system is no is not strain data (orange curve) showing the glitch in the time domain. – UTC. Thenoise amplitude excess around the European scale power in mains each frequency detector is normalized∶ to that ruled out, the consistency of the mass estimates with the of 50 Hz is also present. No noise subtraction was applied To mitigate the glitch in the rapid reanalysis that produced the sky environmental disturbance observed by LIGO environmen- detector’s noise amplitude spectral density.map shown in Fig. 3 In [77], the the raw detector LIGO data were multiplied data, dynamically measured masses of known neutron stars in to the Virgo data prior to this analysis.
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