Ian Harry Why were excited by compact binary mergers Short - - PowerPoint PPT Presentation

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Ian Harry Why were excited by compact binary mergers Short - - PowerPoint PPT Presentation

Nov 18, 2022 18 likes •551 views

Ian Harry Why were excited by compact binary mergers Short introduction to gravitational waves and gravitational-wave observatories Observing compact binary mergers with gravitational-wave facilities What can we learn from

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Ian Harry

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  • Why we’re excited by compact binary mergers
  • Short introduction to gravitational waves and

gravitational-wave observatories

  • Observing compact binary mergers with

gravitational-wave facilities

  • What can we learn from gravitational-wave
  • bservations of compact binary mergers?
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Image credit: NRAO and Chandra.harvard.edu

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0.0 0.5 1.0 1.5 2.0 2.5 Neutron star mass [M ]

J0737-3039A J0737-3039B J1518+4904 J1518+4904comp. B1534+12 B1534+12comp. J1756-2251 J1756-2251comp. J1811-1736 J1811-1736comp. J1829+2456 J1829+2456comp. J1906+0746 J1906+0746comp. B1913+16 B1913+16comp. B2127+11C B2127+11comp. J0024-7204H(47TucH)* J0437-4715 J0514-4002A* J0621+1002 J0751+1807 J1012+5307 J1141-6545 B1516+02B* J1614-2230 J1713+0747 J1748-2446I(Ter5I)* J1748-2446J(Ter5J)* B1802-07* J1802-2124 B1855+09 J1909-3744 B1911-5958A* B2303+46

0.0 0.5 1.0 1.5 2.0 2.5 0.0 0.5 1.0 1.5 2.0 2.5

Double neutron star systems Neutron star-white dwarf systems

Kiziltan et al. arXiv:1011.4291

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0.0 0.5 1.0 1.5 2.0 2.5 Neutron star mass [M ]

J0737-3039A J0737-3039B J1518+4904 J1518+4904comp. B1534+12 B1534+12comp. J1756-2251 J1756-2251comp. J1811-1736 J1811-1736comp. J1829+2456 J1829+2456comp. J1906+0746 J1906+0746comp. B1913+16 B1913+16comp. B2127+11C B2127+11comp. J0024-7204H(47TucH)* J0437-4715 J0514-4002A* J0621+1002 J0751+1807 J1012+5307 J1141-6545 B1516+02B* J1614-2230 J1713+0747 J1748-2446I(Ter5I)* J1748-2446J(Ter5J)* B1802-07* J1802-2124 B1855+09 J1909-3744 B1911-5958A* B2303+46

0.0 0.5 1.0 1.5 2.0 2.5 0.0 0.5 1.0 1.5 2.0 2.5

Double neutron star systems Neutron star-white dwarf systems

Kalogera et al. ApJ. 601, L179 (2004) 83 binary neutron star mergers in our galaxy every 1 million years

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  • Binary pulsar PSR1913+16
  • Pulsar provides a very

accurate clock

  • Ideal “laboratory” for

testing general relativity

  • Binary is losing energy as

gravitational waves at precisely the rate predicted by general relativity

Figure from Weisberg+Taylor (2004).

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Image credit: ESA (left) NASA/ESA/Felix Mirabel (right) Low mass X-ray binary (LMXRB) High mass X-ray binary (HMXRB)

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Image credit: J. Orosz

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Farr et al. ApJ 741, 103

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Abbott et al. CQG 27, 173001 (2010)

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Simulation courtesy of the Simulating eXtreme Spacetimes (SXS) collaboration

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LIGO Hanford, WA LIGO Livingston, LA

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Virgo Cascina Italy

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  • Initial LIGO operated between 2002-2010
  • Initial Virgo between 2007-2011
  • No observations were made
  • Advanced LIGO will become is operational this year
  • Advanced Virgo will follow next year
  • At design sensitivity will be 10x more sensitive
  • 10x distance = 1000x more volume
  • Observatories in Japan and India hope to join in the

2020+ timescale.

  • The first direct observations of gravitational wave

sources from colliding black holes and/or neutron stars are expected soon!

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1

10

2

10

3

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−24

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−23

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frequency (Hz) strain noise amplitude (Hz−1/2) Advanced Virgo Early (2016−17, 20 − 60 Mpc) Mid (2017−18, 60 − 85 Mpc) Late (2018−20, 65 − 115 Mpc) Design (2021, 130 Mpc) BNS−optimized (145 Mpc) 10

1

10

2

10

3

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frequency (Hz) strain noise amplitude (Hz−1/2) Advanced LIGO Early (2015, 40 − 80 Mpc) Mid (2016−17, 80 − 120 Mpc) Late (2017−18, 120 − 170 Mpc) Design (2019, 200 Mpc) BNS−optimized (215 Mpc)

Aasi et al. 1304.0670 100 Mpc = 326Mly = redshift (z) of 0.024

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Image credit: Stevenson et al. 1504.07802 Mass ratio 4:1 2:1 1:1 ~ Average mass of the two components

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  • Gravitational wave detectors

are sensitive to sources from many directions

  • Do not require “pointing”
  • Makes source localization difficult

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LIGO Hanford LIGO Livingston GEO Virgo

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1 2 3 4 5×10−3

  • prob. per deg2

Singer et al. ApJ 795 (2014), 2, 105

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0.0 0.5 1.0 1.5×10−2

  • prob. per deg2

Singer et al. ApJ 795 (2014), 2, 105

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Aasi et al. 1304.0670 2016 2017-8 2018 - ?? With a fourth observatory

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Aasi et al. 1304.0670 Abbott et al. CQG 27, 173001 (2010)

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1.5 2.0 2.5 3.0 3.5 0.6 0.8 1.0 1.2 1.4 m2M m1M

ΧNS 0 ΧNS 0.05

1.5 2.0 2.5 3.0 0.05 0.00 0.05 0.10 0.15 0.20 0.25 0.30 m2M Χ

Hannam, IH, et al. Astrophys.J. 766 (2013) L14

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1.5 2.0 2.5 3.0 3.5 0.6 0.8 1.0 1.2 1.4 m2M m1M

ΧNS 0 ΧNS 0.05

1.5 2.0 2.5 3.0 0.05 0.00 0.05 0.10 0.15 0.20 0.25 0.30 m2M Χ

Hannam, IH, et al. Astrophys.J. 766 (2013) L14

M = (m1 + m2) × (m1 × m2) (m1 + m2)2 3/5

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1.219 0.871 1.741 2.786

1.0,1.0

  • 1.35,1.35
  • 2,2

3.2,3.2

1:2 1:4 1:10

2 4 6 8 10 0.0 0.5 1.0 1.5 2.0 2.5 3.0 m2M m1M

Hannam, IH, et al. Astrophys.J. 766 (2013) L14

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2 4 6 8 10 12 14 2 3 4 5 6 7 8 m2M m1M

BBH region

7.3,7.3 Inspiral only

  • 5.7,5.7

Merger ringdown

  • Hannam, IH, et al. Astrophys.J. 766 (2013) L14
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5 10 15 20 25 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 m2M m1M

0.5 1.0 1.5 2.0 2.5 0.60 0.65 0.70 0.75 0.80 0.85 0.90 m1M Χ2

  • Hannam, IH, et al. Astrophys.J. 766 (2013) L14
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5 10 15 20 25 30 1 2 3 4 5 6

m1 m2

0.2 0.4 0.6 0.8 1

2

Littenberg, et al. 1503.03179

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100 110 120 130 140 150 160 170 180

mz

1 [M]

40 50 60 70 80 90 100 110 120

mz

2 [M]

Ghosh et al. arXiv: 1505.0560

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Vitale et al. PRL 112, 251101 (2014)

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Mandel et al. MNRAS 450, L85

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Stevenson et al. 1504.07802

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  • W. Del Pozzo, Phys. Rev. D 86, 043011 (2012)
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−40 −20 20 40 60 80 100 120 140 ln OmodGR

GR

0.00 0.01 0.02 0.03 0.04 0.05 0.06 0.07 0.08 P(ln OmodGR

GR

)

TaylorT4 + all (70 catalogs) δχ3 = −0.1 (30 catalogs)

  • M. Agathos et al., Phys. Rev. D 89, 082001 (2014)
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  • We expect gravitational-wave astronomy to begin

in the next years

  • Compact binary mergers are a key target for these

systems

  • I hope to have given you a flavour of what we can

learn from observing such systems

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Any questions?

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  • Gravity is described as a

warping of space and time

  • Caused by the mass and energy

in the universe

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Black hole space-time

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Image: T. Carnahan (NASA GSFC)

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  • How would we know when there is a black hole

signal in data from LIGO and Virgo?

  • PROBLEM: The data is contaminated by other noise

sources: seismic, thermal, human ….

  • PROBLEM: Unless the black holes are really close,

data with a signal in it will look indistinguishable from data with no signal in it.

  • SOLUTION: Matched-filtering

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  • Optimal if looking for a known signal buried in noise.

50 Wainstein and Zubakov “Extraction of signals from noise”, 1962 Allen et al. Phys.Rev. D85 (2012) 122006 Babak, … ,IH, et al. Phys.Rev. D87 (2013) 024033

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Time-frequency spectrograms showing power

Loud simulated black hole merger A noise artifact

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  • Flag times of poor data quality
  • Use a variety of monitors to identify

instrumental misbehaviour

  • Require “coincident” signal in several

detectors

  • Make use of signal consistency tests

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