The journal paper:
Phys. Rev. Lett. 116, 061102 (2016) - Observation of Gravitational Waves from a Binary Black Hole Merger
Its abstract:
On September 14, 2015 at 09:50:45 UTC the two detectors of the Laser Interferometer Gravitational-Wave Observatory simultaneously observed a transient gravitational-wave signal. The signal sweeps upwards in frequency from 35 to 250 Hz with a peak gravitational-wave strain of 1.0×10^−21. It matches the waveform predicted by general relativity for the inspiral and merger of a pair of black holes and the ringdown of the resulting single black hole. The signal was observed with a matched-filter signal-to-noise ratio of 24 and a false alarm rate estimated to be less than 1 event per 203 000 years, equivalent to a significance greater than 5.1σ. The source lies at a luminosity distance of 410+160−180 Mpc corresponding to a redshift z=0.09+0.03−0.04. In the source frame, the initial black hole masses are 36+5−4 M⊙ and 29+4−4 M⊙, and the final black hole mass is 62+4−4 M⊙, with 3.0+0.5−0.5 M⊙c^2 radiated in gravitational waves. All uncertainties define 90% credible intervals. These observations demonstrate the existence of binary stellar-mass black hole systems. This is the first direct detection of gravitational waves and the first observation of a binary black hole merger.
It was detected with the two detectors of
LIGO, one at Hanford, WA, and the other at Livingston LA. The similar signals observed at both sites helped rule out the hypothesis that the observed signal was noise. The Europeans'
VIRGO interferometer was not operating at the time, but it should be later this year. It is a single detector near Pisa, Italy, and it will be operated in collaboration with LIGO.
Since only two detectors "saw" it, the delay between them constrains the source direction to a circle in the sky. It may be possible to get a further constraint from the relative intensities of the signals, but I'm not sure if the LIGO team did that. However, one may get some combination of (source direction) and (source orientation).
Now that this detector evidently saw something, I think that that will make it easier for other G-wave research teams to get support for their efforts. There's already an under-construction one in Japan (KAGRA) and a proposed one in India (INDIGO).
Here's a table of results:
What | Mass (Msun) | Spin (relative)
Primary | 36 +5-4 | < 0.7
Secondary | 29 +4-4 | poorly constrained
Final | 62 +4-4 | 0.67 +0.05-0.07
About 3 +0.5-0.5 solar masses of energy was radiated as G-waves.
Its peak G-wave luminosity was (3.6 +0.5−0.4)×10^56 erg/s, equivalent to 200 +30−20 solar masses / second. The Sun has a luminosity of 3.9 * 10^26 watts in the electromagnetic spectrum -- that gives about 10^23 solar luminosities for this event, or somewhere around the combined luminosity of every star in the observable Universe.
The progenitors of those two black holes were likely very massive stars with relatively weak stellar winds, meaning that they retained much of their original mass before collapsing. Their metallicity or heavy-element content was likely <~ 1/2 that of the Sun. "Heavy" being everything heavier than helium. So their protostellar nebula(e) was not as enriched as the Sun's was. This is consistent with their being very old stars whose black holes then spiraled in over the lifetime of the Universe. Or else with much younger ones that formed in a metal-poor galaxy with star formation (there are some such galaxies).
The observation suggests an event rate somewhere within various estimates of the rates of mergers of massive black holes. It is only one observation, so it will be necessary to observe more events to get a better fix.
Identifying the event's home galaxy will be more difficult, since it will likely require G-wave detectors in outer space outside of low Earth orbit. That's what's necessary to get a good baseline to get a good fix on an event's position.