GW170817: gravitational waves from the merger of two neutron stars - - PowerPoint PPT Presentation

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GW170817: gravitational waves from the merger of two neutron stars - - PowerPoint PPT Presentation

May 12, 2023 282 likes •778 views

GW170817: gravitational waves from the merger of two neutron stars Photo credit: Mike Fyffe NSF/LIGO/Sonoma State University/A. Simonnet Dr. Jess McIver for the LIGO-Virgo Collaboration Caltech/JPL Association for Gravitational-Wave Research

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Photo credit: Mike Fyffe

GW170817: gravitational waves

LIGO DCC G1702114

  • Dr. Jess McIver for the LIGO-Virgo Collaboration

Caltech/JPL Association for Gravitational-Wave Research Seminar Oct 24, 2017

from the merger of two neutron stars

NSF/LIGO/Sonoma State University/A. Simonnet

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NASA

Gravitational waves

Ripples in the fabric of spacetime

generated by the acceleration of matter

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Indirect evidence of gravitational waves

LIGO/Caltech

Weisburg, Nice & Taylor, 2010

Hulse-Taylor Binary Pulsar PSR B1913+16

GR prediction

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Gravitational wave propagation

Spacetime strain h(t) measured as

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LIGO DCC P1500072

Observing GWs with interferometry

5 McIver

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How does LIGO detect gravitational waves?

LIGO/Caltech

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Kai Staats

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LIGO/Caltech

How sensitive is the LIGO experiment?

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Where are the LIGO detectors?

LIGO/Caltech

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Matched Filter Analysis

ˆ L ~ S1 ~ S2 1,2 ∝ ~ S1,2 · ˆ L

Matched filter signal-to-noise ratio

  • Phys. Rev. X 6 (2016)

Template Bank

Slide adapted from S. Caudill

  • B. P. Abbott et al. Phys. Rev. X (2016)

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O1 results

2σ 3σ 4σ 5σ > 5σ 2σ 3σ 4σ 5σ > 5σ

8 10 12 14 16 18 20 22 24

Detection statistic ˆ ρc

10−8 10−7 10−6 10−5 10−4 10−3 10−2 10−1 100 101 102 103 104

Number of events

GW150914 Search Result Search Background Background excluding GW150914

  • B. P. Abbott et al. Phys. Rev. X (2016)

GW150914 GW151226 LVT151012

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Observed black hole mergers to date

LIGO/Caltech/MIT/LSC

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LIGO/Caltech

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Sky localization

arXiv 1304.0670

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Sky localization of BBHs with LIGO

LIGO/Caltech/MIT/Singer/Mellinger

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A three interferometer network

LIGO/Caltech

and EM observer partners

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Sky localization with three detectors

LIGO/Caltech/MIT/Singer/Mellinger

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Prior to the Advanced LIGO’s second observing run (O2), no BNS mergers were observed.

The first observing run (O1) placed upper limits on the rate of BNS mergers that did not yet rule out any astrophysical predictions (as high as ~ 10,000 Gpc yr )

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NASA/Goddard Space Flight Center/CI Lab

130 million years ago, two neutron stars merged

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LIGO/Virgo/Lovelace, Brown, Macleod, McIver, Nitz

GW170817: Gravitational waves from a binary neutron star merger

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B.P. Abbott et al PRL. (2017)

A glitch in LIGO-Livingston

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LIGO/University of Oregon/Ben Farr

GW170817 and GWs from binary black holes

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B.P. Abbott et al PRL. (2017)

From GWs: inferring the component masses

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LIGO-Virgo/Frank Elavsky/Northwestern University

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B.P. Abbott et al PRL. (2017)

From GWs: constraining NS EoS

Tidal deformability

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B.P. Abbott et al. PRL (2017)

From GWs: sky localization

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LIGO-Virgo

Sky localization with GWs and gamma rays

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LIGO-Virgo/Greco, Arnaud, Vicerè

Virgo’s role in localization

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B.P. Abbott et al. Ap. J. Letters (2017)

Prompt emission: GWs and gamma rays

t(seconds) t(days)

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B.P. Abbott et al. Ap. J. Letters (2017)

GW γ-ray X-ray

LIGO, Virgo Fermi, INTEGRAL, Astrosat, IPN, Insight-HXMT, Swift, AGILE, CALET, H.E.S.S., HAWC, Konus-Wind

SALT ESO-NTT SOAR ESO-VLT 7000o 4000o t-tc

(days)

1.2 1.4 2.4

wavelength (A) normalized Fλ 4000 6000 10000 20000

  • INTEGRAL/SPI-ACS

Fermi/GBM

t-tc (s)

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2 4 6 counts/s (arb. scale) frequency (Hz) 500 400 300 200 100 50

LIGO - Virgo

Prompt emission: GWs and gamma rays

t(seconds) t(days)

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B.P. Abbott et al. Ap. J. Letters (2017)

  • 100 -50

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GW γ-ray X-ray UV Optical IR Radio

10-2 t-tc (s) t-tc (days) 10-1 100 101

LIGO, Virgo Fermi, INTEGRAL, Astrosat, IPN, Insight-HXMT, Swift, AGILE, CALET, H.E.S.S., HAWC, Konus-Wind Swift, MAXI/GSC, NuSTAR, Chandra, INTEGRAL Swift, HST Swope, DECam, DLT40, REM-ROS2, HST, Las Cumbres, SkyMapper, VISTA, MASTER, Magellan, Subaru, Pan-STARRS1, HCT, TZAC, LSGT, T17, Gemini-South, NTT, GROND, SOAR, ESO-VLT, KMTNet, ESO-VST, VIRT, SALT, CHILESCOPE, TOROS, BOOTES-5, Zadko, iTelescope.Net, AAT, Pi of the Sky, AST3-2, ATLAS, Danish Tel, DFN, T80S, EABA REM-ROS2, VISTA, Gemini-South, 2MASS,Spitzer, NTT, GROND, SOAR, NOT, ESO-VLT, Kanata Telescope, HST ATCA, VLA, ASKAP, VLBA, GMRT, MWA, LOFAR, LWA, ALMA, OVRO, EVN, e-MERLIN, MeerKAT, Parkes, SRT, Effelsberg

Chandra 9d J VLA 16.4d Radio Las Cumbres 11.57h w DECam 11.40h iz MASTER 11.31h W VISTA 11.24h YJKs X-ray DLT40 11.08h h 1M2H Swope 10.86h i

Electromagnetic follow-up

SALT ESO-NTT SOAR ESO-VLT 7000o 4000o t-tc

(days)

1.2 1.4 2.4

wavelength (A) normalized Fλ 4000 6000 10000 20000

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counts/s (arb. scale)

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What we’ve learned from GW170817

From gravitational waves:

  • Astrophysical rate of BNS mergers R = 1540 Gpc yr
  • Stochastic background from BNS and BBH mergers should be

detectable with current generation of detectors at design sensitivity!

  • Limits on dynamical ejecta in the associated kilonova.
  • To come: improved constraints on deviations from general relativity

using much longer duration waveform.

  • To come: insight on the remnant object from the post-merger GW

signal.

Companion papers:

1. GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral. B.P. Abbott et al. PRL 119 161101 (2017) 2. GW170817: Implications for the Stochastic Gravitational-Wave Background from Compact Binary Coalescences. arXiv 1710.05837 3. Estimating the Contribution of Dynamical Ejecta in the Kilonova Associated with

  • GW170817. arXiv 1710.05836
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+3200

  • 1220
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What we’ve learned from GW170817

From multi-messenger observations:

  • Confirmation of association between short GRBs and BNS mergers.
  • Independent measurement of the Hubble constant consistent with

prior measurements.

  • Speed of gravity is consistent with speed of light to one part in 10 .
  • Improved Lorentz invariance limits; constrained to one part in 10 .
  • New insights into physics of gamma-ray burst events.
  • Constraints on progenitors and the evolution of the BNS pair.
  • BNS mergers as producers of heavy elements confirmed.
  • More to come - see Kasliwal/Hallinan CaJAGWR seminar on Nov 7!

Companion papers:

1. Multi-Messenger Observations of a Binary Neutron Star Merger. B.P. Abbott et al. Ap. J. Letters 848, 2 (2017) 2. Gravitational Waves and Gamma-Rays from a Binary Neutron Star Merger: GW170817 and GRB

  • 170817A. B.P. Abbott et al. Ap. J. Letters 848, 2 (2017)

3. A gravitational-wave standard siren measurement of the Hubble constant. B.P. Abbott et al. Nature (2017) 4. On the Progenitor of Binary Neutron Star Merger GW170817. arXiv 1710.05838 5. Search for High-energy Neutrinos from Binary Neutron Star Merger GW170817 with ANTARES, IceCube, and the Pierre Auger Observatory. arXiv 1710.05839

13 15

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B.P. Abbott et al. Nature (2017)

Independent measurement of the Hubble constant

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Future challenges: targeting transient noise

gravityspy.org

Zevin et al, CQG (2017)

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LIGO-Livingston h(t)

LIGO-Livingston transient noise during the second observing run

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Understanding the impact of transient noise on estimation of source properties

Minimum 90% confidence sky area (2 seconds before the scattering noise feature): 300 sq. deg. Maximum 90% confidence sky area: (During the first 0.5 seconds of the scattering noise): 540 sq. deg. Parameter estimation produced with the lalinference pipeline: arXiv 1409.7215

McIver et al. (in prep)

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gravitational wave astronomy

The future of

SXS

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Roadmap to design sensitivity

39 arXiv 1304.0670

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Future prospects: the global GW network

LIGO/Caltech

2020 2021 2022 2025

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Future prospects for terrestrial gravitational wave astronomy

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  • B. P. Abbott et al. CQG 34 (2017)
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Beyond terrestrial detectors

ESA

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Pulsar Timing Arrays

David J Champion

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The International Pulsar Timing Array

IPTA

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LIGO Scientific Collaboration

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The future of gravitational wave astrophysics is bright!

NSF/LIGO/Sonoma State University/A. Simonnet

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LIGO/Caltech

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