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Results from the 1st Advanced LIGO observing run and their astrophysical implicationsTyson B. Littenberg for the LIGO & Virgo Scientific Collaborations NASA Marshall Space Flight Center
https://ntrs.nasa.gov/search.jsp?R=20160013425 2020-06-16T15:49:45+00:00Z
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The chirp heard ‘round the world
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Phys. Rev. Lett. 116, 061102
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LIGO’s First Observing Run (O1)
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Binary black holes in O1
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Naming GW events: XXYYMMDD
LVT=candidate GW=confirmed
Date of detection
Phys. Rev. X 6, 041015 (2016)
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Finding BBHs in the data
• GW150914 and GW151226 were both > 5-sigma detections
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Phys. Rev. X 6, 041015 (2016)
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BBH CharacterizationMass & Spin
S1
S2
m1
m2
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BBH Characterization — Masses
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component masses [measured]
remnant mass & spin [~predicted]
Phys. Rev. X 6, 041015 (2016)
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primary secondary
magnitude
misalignment
BBH Characterization — Spins
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• Spin will typically be difficult to pin down precisely except for ideally oriented systems (edge-on)
• GW151226 shows evidence for non-negligible spin of m1, not anti-aligned with L
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GW150914 LVT151012 GW151226
Phys. Rev. X 6, 041015 (2016)
BBH Characterization — Spins
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Why is spin so important?
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Creating binary black holes
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“Field” “Cluster”L
S1 S2
L
S1
S2
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LS1 S2
L
S1
S2
Creating binary black holes
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Why is spin so important?Spin alignment is a window into the BBH formation channel
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BBH Localization
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BBH Localization
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Phys. Rev. X 6, 041015 (2016)
• Position reconstruction is a challenge for 2-detector networks.
• This will improve as Virgo and others join the network at comparable sensitivity [see Living Rev. Relativity 19 (2016), 1].
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Testing GR
Image credit: NASA/GSFC
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Testing GR — consistency tests
• GW150914 signal was dominated by merger which facilitated some interesting tests: • Detectable by excess power searches, enabling analysis of residuals after GR
model was removed from data. • Consistency tests for final mass and spin of remnant black hole
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Phys. Rev. Lett. 116, 221101 (2016)
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Testing GR — parameterized tests• Inspiral waveforms computed using post-Newtonian (PN) expansion.
Analyses search for departures from the GR values of PN coefficients.
• Additional modification parameters included for late-inspiral, merger, and ringdown stage of the signal.
• So far, measurements are consistent with GR
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post-Newtonian (inspiral) late inspiral, merger & ringdown
Phys. Rev. X 6, 041015 (2016)
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Astrophysics Rates of Compact Mergers
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arXiv:1607.07456 [astrop-ph.HE]
Upper limits on BNS (left)NSBH (right)
Inferred rates for BBH
Phys. Rev. X 6, 041015 (2016)
Assuming
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In Summary What did we learn about the Universe from O1?
• O1 significantly added to the zoo of known stellar-mass black holes
• GW150914 contained the largest stellar-mass black holes ever detected.
• So far, the observed gravitational waves are consistent with Einstein’s general theory of relativity.
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What to expect from O2
What we will be asking about black hole mergers:
• How & where are the black holes formed?
• How large can black holes be? How small?
• Are the waves consistent with Einstein’s theory?
• Do they produce any electromagnetic signals?
N > 10N > 35
N > 70
Space-time volume observed [relative to O1]
Prob
abili
ty o
f det
ectin
g >
N
high
ly si
gnifi
cant
eve
nts
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What to expect from O2
Image credit: NASA/GSFC
Image credit: NASA/AEI/ZIB/M. Koppitz and L. Rezzolla
Mosta et al (2014)
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What we will be asking about other transient sources:
• What is the rate of binary neutron star mergers? NSBH?
• Do binary neutron star mergers create GRBs?
• What other sources of GW transients are out there?
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Gravitational wave
detectors