GRAVITATIONAL-WAVE OBSERVATIONS BY ADVANCED LIGO AND VIRGO LIGO - - PowerPoint PPT Presentation

SLIDE 1

GRAVITATIONAL-WAVE OBSERVATIONS BY ADVANCED LIGO AND VIRGO

PATRICIA SCHMIDT

ON BEHALF OF THE LIGO SCIENTIFIC AND VIRGO COLLABORATIONS TAUP 2019 TOYAMA, JAPAN - SEPTEMBER 9, 2019 LIGO DCC-G1901751 Birmingham Institute for Gravitational Wave Astronomy

SLIDE 2

GW SPECTRUM

THE GRAVITATIONAL WAVE SPECTRUM

2 stellar-mass compact binary mergers

Image credits: WMAP, NASA, P. Mösta

stellar mass

SLIDE 3

GW DETECTORS

LASER INTERFEROMETERS

3

Credit: Johan Jarnestad/The Royal Swedish Academy of Sciences

∆L ∼ 10−18 m

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SLIDE 4

GW DETECTOR NETWORK

A GLOBAL GW NETWORK

A global consortium with more than 2000 scientist involved!

4

Virgo GEO 600

? ?

• Simultaneous detection increases detection confidence
• Improved sky localisation & polarisation
• Increased duty cycle

SLIDE 5

GWS FROM COMPACT BINARIES

MORPHOLOGY OF COMPACT BINARIES

▸ Signal „sweeps“ through the detector’s

sensitivity band: “chirp”

▸ GWs carry characteristic information

about the binary

5

Merger Ringdown Inspiral the orbit shrinks … … until they collide … and form a single black hole

[LVC, PRL 116 (2016)]

SLIDE 6

PARAMETER ESTIMATION

BINARY PARAMETERS

▸ Intrinsic: ▸ Masses ▸ Spins ▸ Tidal deformability (neutron stars)

6

▸ Extrinsic: ▸ Inclination, distance, polarisation ▸ Sky location ▸ Time, reference phase

SLIDE 7

THE FIRST TWO OBSERVING RUNS

O1 & O2

▸ O1: Sept 12,2015 - Jan 30, 2016 ▸ HL coincident time: 48.6 days ▸ O2: Nov 30, 2016 - Aug 25, 2017 ▸ Virgo joined on Aug 1, 2017 ▸ 25Mpc BNS range ▸ HL-coincident time: 118 days ▸ HLV-coincident time: 15 days

7

Montana earthquake Representative best performance

GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs LVC, PRX 9 (2019)

SLIDE 8

DETECTIONS: GWTC-1

GW DETECTIONS IN O1&O2:GWTC-1

▸ 11 confident GW detections from compact binaries: ▸ FAR ≤ ~1 per month & probability of astrophysical origin > 50% ▸ 10 binary black holes & 1 binary neutron star

8

32 128 512 Frequency [Hz] 10 40 20 30 Frequency [Hz]

GRAVITATIONAL-WAVE TRANSIENT CATALOG-1

32 128 512 FREQUENCY [HZ] 32 128 512 FREQUENCY [HZ] 32 128 512 FREQUENCY [HZ] 0.1 0.4 0.2 0.3 0.1 0.4 0.2 0.3 TIME [SECONDS] TIME [SECONDS] TIME [SECONDS] EINSTEIN’S THEORY 0.1 0.4 0.2 0.3 0.1 0.4 0.2 0.3 WAVELET (UNMODELED)

• S. GHONGE, K. JANI | GEORGIA TECH

LIGO-VIRGO DATA: HTTPS://DOI.ORG/10.7935/82H3-HH23

GW150914 GW151012 GW151226 GW170104 GW170608 GW170729 GW170809 GW170814 GW170818 GW170823 GW170817 : BINARY NEUTRON STAR

SLIDE 9

DETECTIONS: GWTC-1

GW DETECTIONS

▸ Four new binary black hole mergers

identified: GW170729 (HL), GW170809 (HL), GW170818 (HLV), GW170823 (HL)

▸ Not all events were found by all

pipelines

9

FAR [y−1] Network SNR Event UTC Time PyCBC GstLAL cWB PyCBC GstLAL cWB GW150914 09:50:45.4 < 1.53 × 10−5 < 1.00 × 10−7 < 1.63 × 10−4 23.6 24.4 25.2 GW151012 09:54:43.4 0.17 7.92 × 10−3 – 9.5 10.0 – GW151226 03:38:53.6 < 1.69 × 10−5 < 1.00 × 10−7 0.02 13.1 13.1 11.9 GW170104 10:11:58.6 < 1.37 × 10−5 < 1.00 × 10−7 2.91 × 10−4 13.0 13.0 13.0 GW170608 02:01:16.5 < 3.09 × 10−4 < 1.00 × 10−7 1.44 × 10−4 15.4 14.9 14.1 GW170729 18:56:29.3 1.36 0.18 0.02 9.8 10.8 10.2 GW170809 08:28:21.8 1.45 × 10−4 < 1.00 × 10−7 – 12.2 12.4 – GW170814 10:30:43.5 < 1.25 × 10−5 < 1.00 × 10−7 < 2.08 × 10−4 16.3 15.9 17.2 GW170817 12:41:04.4 < 1.25 × 10−5 < 1.00 × 10−7 – 30.9 33.0 – GW170818 02:25:09.1 – 4.20 × 10−5 – – 11.3 – GW170823 13:13:58.5 < 3.29 × 10−5 < 1.00 × 10−7 2.14 × 10−3 11.1 11.5 10.8

GstLAL

SLIDE 10

SOURCE PROPERTIES

MASSES

▸ Wide range of masses ▸ More BBH towards the heavy end but none in either mass gap ▸ GW170729: heaviest, furthest away

10 20 40 60 80 m1(M) 10 20 30 40 50 m2(M) q

1/2 1/4 1/8

GW170817 GW170608 GW151226 GW151012 GW170104 GW170814 GW170809 GW170818 GW150914 GW170823 GW170729

[LVC, PRX 9 (2019)]

SLIDE 11

SOURCE PROPERTIES

SPINS

▸ Key signatures to discriminate black hole populations ▸ GW170729 has clear indication for a net positive spin ▸ Precession remains unconstrained for all events

11

GW170817 GW170608 GW151226 GW151012 GW170104 GW170814 GW170809 GW170818 GW150914 GW170823 GW170729

−1.0 −0.5 0.0 0.5 1.0 χeff

eff = (m1~ 1 + m2~ 2) · ˆ LN M

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[LVC, PRX 9 (2019)]

SLIDE 12

GW BINARIES IN CONTEXT

THE STELLAR GRAVEYARD

12

SLIDE 13

GW MULTIMESSENGER ASTRONOMY

GW170817: A NEW ERA IS BORN

▸ On August 17, 2017 at 12:41:04

UTC the signal from a binary neutron star was detected

▸ Fermi detects sGRB 1.7s after the

GW

▸ GCN alert sent ~27 minutes after GW

detection

▸ Localised to ~30deg2 ▸ First observation of an optical

counterpart ~11h later by the Swope telescope

13

[Astrophys. J. 848 (2017) L12]

First GW + EM observation!!

SLIDE 14

MATTER AT ITS EXTREME

GW170817: PROBING MATTER AT ITS EXTREME

▸

Neutron stars: densest objects in the universe

▸

O(1000s) observed to date

14

early universe

phases of QCD

Temperature quark-gluon plasma

Baryon Density

RHIC, LHC hadrons

nuclear experiments

? ? ? ? ?

neutron stars

NS mergers

Credit: F. Linde

?

crust ~ km neutron rich ions, free neutrons

• uter core ~ few km

uniform liquid

deep core ~2-10x nuclear density Exotic states of matter?

debris from a supernova explosion in 1054 Crab Pulsar

What is the nature of matter under such extreme conditions? What is the nuclear equation of state?

Credit:NASA

SLIDE 15

FIRST NUCLEAR PHYSICS CONSTRAINTS FROM GWS

NUCLEAR PHYSICS WITH GW170817

▸ GWs are unique probes of the neutron star interior ▸ Tidal deformability:

15

200 400 600 800 1000 1200 1400 1600

˜ Λ

0.0000 0.0005 0.0010 0.0015 0.0020 0.0025 0.0030 0.0035

PDF

WFF1 APR4 SLy MPA1 H4 MS1b MS1

IMRPhenomPv2NRT SEOBNRv4NRT SEOBNRv4T TEOBResumS TaylorF2 Prior

˜ Λ = 16 13 (m1 + 12m2)m4

1 Λ1 + (m2 + 12m1)m4 2 Λ2

(m1 + m2)5

8 10 12 14

R (km)

0.5 1.0 1.5 2.0 2.5 3.0

m (M)

WFF1 APR4 SLy MPA1 H4

BH limit Buchdahl limit

1 1

R1 = 10.8+2.0

−1.7 km

R2 = 10.7+2.1

−1.5 km

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[LVC, PRL 121 (2018)] Credit: T. Hinder & T. Dietrich [LVC, PRX 9 (2019)]

SLIDE 16

FUNDAMENTAL PHYSICS

FUNDAMENTAL PHYSICS WITH GWS

▸ Propagation of gravitational waves

(dispersion) [LVC, arXiv:1903.04467]

▸ Generation of gravitational waves

(parameterised tests) [LVC, arXiv:1903.04467]

▸ Polarisation tests [LVC, PRL (2017)] ▸ Tests of the nature of the remnant [LVC,

arXiv:1903.04467]

▸ Speed of gravity [LVC, Fermi &Integral, ApJL

(2017)]

16

−3 × 10−15 ≤ ∆v vEM ≤ 7 × 10−16

mg ≤ 5.0 × 10−23 eV/c2

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Φ=M/L

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R

1/2=(M/L 3) 1/2 [km

• 1]

Double Binary Pulsar Lunar Laser Ranging GW150914 Perihelion Precession of Mercury LAGEOS Pulsar Timing Arrays Cassini GW151226 (Orbital Decay) Double Binary Pulsar (Shapiro Delay)

Yunes et al., PRD 2016

• Î
• Î
• +
• Î
• Î

SLIDE 17

POPULATION INFERENCE

ASTROPHYSICAL RATES

▸ Merger rates (based on fixed populations):

17

LVC, PRD 85 (2012) LVC, PRX 9 (2019) LVC, 1811.12940

BBH: 9.7 - 101 Gpc-3 y-1 BNS: 110 - 3840 Gpc-3 y-1 NSBH 90% upper limit: 610 Gpc-3 y-1

S5 upper limits S6 upper limits

SLIDE 18

SUMMARY

SUMMARY & OTHER ANALYSES

▸ In O1&O2 LIGO and Virgo have confidently detected GWs from 10 BBH

and one BNS

▸ During O1 & O2, we observed one GW event every 15 days of

searched data

▸ Updated merger rates for BNS, BBH and NSBH ▸ No signs of precession, exotic physics, violations of GR ▸ Many more analyses, e.g. sub-solar mass compact binaries, sub-

threshold GW events, intermediate mass black hole binaries, eccentric black hole binaries, continuous waves, supernovae, stochastic GW background

▸ Data available from the GW Open Science Center: https://www.gw-

• penscience.org/catalog/

18

SLIDE 19

THIRD OBSERVING RUN

NO APRIL FOOL’S

▸ O3 began on April 1st,

2019 @ 15:00 UTC

▸ Five months of

• bservations

▸ HLV coincidence duty

cycle ~45%; double coincidence 81%; no IFO time < 3%

19

https://www.gw-openscience.org/detector_status/day/20190501/

SLIDE 20

THIRD OBSERVING RUN

O3 SO FAR: OPEN PUBLIC ALERTS

▸ 26 GW candidates:

20

https://gracedb.ligo.org

SLIDE 21

O3 SO FAR

SELECTED HIGHLIGHTS

21

S190425z: BNS candidate S190814bv: S190829j & S190829l: two BHs within ~20 minutes https://gracedb.ligo.org/superevents/public/O3/ Public alerts guide: https://emfollow.docs.ligo.org/ userguide/index.html

SLIDE 22

INTO THE FUTURE

BEYOND O3

▸ O3 to last ~1 year ▸ KAGRA (almost) ready to join

O3

▸ Possible 5 detector network

~2026

▸ O5: LIGO A+ and Advanced

Virgo+

▸ 3G: Einstein Telescope, Cosmic

Explorer

▸ Space-based GW missions e.g.

LISA

22

[LVC, 1304.0670-v7]

SLIDE 23

INTO THE FUTURE

READY FOR NEW DISCOVERIES

23

The future is loud & bright!

neutron star - black hole mergers intermediate mass black holes core-collapse supernovae spinning neutron stars astrophysical cosmological background The Unknown

Image credits: NASA, PI, CQG