Hint of quantum gravity effects from LIGO data

Slides used to present the paper https://arxiv.org/abs/1612.00266 at the Black Hole Club.

Transcript

1. arXiv:1612.00266
4. Let’s add the membrane near the event horizon
5. r ⇡ lP
6. bined signal-to- g at the time of eing upgraded, nsitive to detect n observational urce position is rival time and 600 deg2 (90% int to it being ack holes—i.e., quent final black ses in frequency o 150 Hz, where most plausible l of two orbiting ave emission. At characterized by Y S I C A L R E V I E W L E T T E R S week ending 12 FEBRUARY 2016 bined signal-to- g at the time of eing upgraded, nsitive to detect n observational urce position is rival time and 600 deg2 (90% int to it being ack holes—i.e., quent final black ses in frequency o 150 Hz, where most plausible l of two orbiting ave emission. At characterized by −11=3 _ f  3=5 ; FIG. 2. Top: Estimated gravitational-wave strain amplitude from GW150914 projected onto H1. This shows the full bandwidth of the waveforms, without the filtering used for Fig. 1. The inset images show numerical relativity models of the black LIGO PRL 2016
7. bined signal-to- g at the time of eing upgraded, nsitive to detect n observational urce position is rival time and 600 deg2 (90% int to it being ack holes—i.e., quent final black ses in frequency o 150 Hz, where most plausible l of two orbiting ave emission. At characterized by Y S I C A L R E V I E W L E T T E R S week ending 12 FEBRUARY 2016 bined signal-to- g at the time of eing upgraded, nsitive to detect n observational urce position is rival time and 600 deg2 (90% int to it being ack holes—i.e., quent final black ses in frequency o 150 Hz, where most plausible l of two orbiting ave emission. At characterized by −11=3 _ f  3=5 ; FIG. 2. Top: Estimated gravitational-wave strain amplitude from GW150914 projected onto H1. This shows the full bandwidth of the waveforms, without the filtering used for Fig. 1. The inset images show numerical relativity models of the black LIGO PRL 2016
8. event 1st echo 2nd echo time r * membrane / firewall tmerger techo Δtecho angular momentum barrier FIG. 1: Spacetime depiction of gravitational wave echoes from a membrane/firewall on the stretched horizon, following a black hole merger event. flected w have op For a eter a , t techo = = where r distance The p given by 2 +
9. ded by other rd and t ) and 096 Hz sists of nstruct or the cessive , fixed angu- ). which merger mplate Template with echoes t tmerger ( s ) techo
   
   tmerger techo FIG. 2: LIGO original template for GW150914, along with our best fit template for the echoes.
10. V I E W L E T T E R S week ending 12 FEBRUARY 2016 FIG. 2. Top: Estimated gravitational-wave strain amplitude from GW150914 projected onto H1. This shows the full bandwidth of the waveforms, without the filtering used for Fig. 1. The inset images show numerical relativity models of the black Templatewithechoes techo
    
    tme
11. op: Estimated gravitational-wave strain amplitude 50914 projected onto H1. This shows the full of the waveforms, without the filtering used for Fig. 1. mages show numerical relativity models of the black ns as the black holes coalesce. Bottom: The Keplerian ack hole separation in units of Schwarzschild radii =c2) and the effective relative velocity given by the nian parameter v=c ¼ ðGMπf=c3Þ1=3, where f is the l-wave frequency calculated with numerical relativity e total mass (value from Table I). T T E R S week ending 12 FEBRUARY 2016 33], a modified Michelson interferometer (see t measures gravitational-wave strain as a differ- gth of its orthogonal arms. Each arm is formed mirrors, acting as test masses, separated by L ¼ 4 km. A passing gravitational wave effec- op: Estimated gravitational-wave strain amplitude 50914 projected onto H1. This shows the full of the waveforms, without the filtering used for Fig. 1. mages show numerical relativity models of the black ns as the black holes coalesce. Bottom: The Keplerian ack hole separation in units of Schwarzschild radii =c2) and the effective relative velocity given by the nian parameter v=c ¼ ðGMπf=c3Þ1=3, where f is the l-wave frequency calculated with numerical relativity e total mass (value from Table I). T T E R S week ending 12 FEBRUARY 2016 t tm e rg e r ( s ) techo
    
    tmerger techo G. 2: LIGO original template for GW150 with our b est fit template for the ec h IG. 3: Amplitude Sp ectral Densities (ASD st fit ec ho template (Eq. 9) and the main W150914. Since w e ha v e a quasi-p erio dic m are resonances in the sp ectrum. The ASD uare ro ot of the p o w er sp ectral densities, v erages of the square of the fast F ourier t FFTs) of the data. The noise sp ectra from and Livingston detectors are also sho ere the term ( 1)n +1 is due to the phase truncated mo del in eac h reflection. Fig b est fit for this template for GW150914 ameter space describ ed ab o v e, along wit ger ev en t. In the frequency domain w e ex onances of these ec ho es (Fig. 3). Results: Our strategy is to searc h for the ec ho template (9), b y maximizing its sig
12. Fig. 4 from paper (need help)
13. Hanford, WA, and Livingston, LA, observatories detected tions reported here. Occurring within the 10-ms intersite FIG. 1. The gravitational-wave event GW150914 observed by the LIGO Hanford (H1, left column panels) and Livingston (L1, right ⌫ = t 1 echo = 3.4 Hz
14. On September 14, 2015 at 09:50:45 UTC, the LIGO Hanford, WA, and Livingston, LA, observatories detected most significant event from each detector for the observa- tions reported here. Occurring within the 10-ms intersite ⌫ = t 1 echo = 3.4 Hz we should see the echoes in the CWT, if they are really there