GW151226: Observation of Gravitational Waves from a 22 Solar-mass Binary Black Hole Coalescence

Figure 1. (Adapted from figure 1 of our publication). The gravitational wave event GW151226 as observed by the twin Advanced LIGO instruments: LIGO Hanford (left) and LIGO Livingston (right). The images show the data recorded by the detectors during the last second before merger as the signal varies as a function of time (in seconds) and frequency (in Hertz or the number of wave cycles per second). To be certain that a real gravitational wave has been observed, we compare the data from the detectors against a pre-defined set of models for merging binaries. This allows us to find gravitational wave signals which are buried deep in the noise from the instruments and nearly impossible to find by eye. The animation shows the detector data with and without removing the best-matching model gravitational-wave signal, making it much easier to identify. The signal can be seen sweeping up in frequency as the two black holes spiral together. This signal is much more difficult to spot by eye than the first detection GW150914!

Figure 1. (Adapted from figure 1 of our publication). The gravitational wave event GW151226 as observed by the twin Advanced LIGO instruments: LIGO Hanford (left) and LIGO Livingston (right). The images show the data recorded by the detectors during the last second before merger as the signal varies as a function of time (in seconds) and frequency (in Hertz or the number of wave cycles per second). To be certain that a real gravitational wave has been observed, we compare the data from the detectors against a pre-defined set of models for merging binaries. This allows us to find gravitational wave signals which are buried deep in the noise from the instruments and nearly impossible to find by eye. The animation shows the detector data with and without removing the best-matching model gravitational-wave signal, making it much easier to identify. The signal can be seen sweeping up in frequency as the two black holes spiral together. This signal is much more difficult to spot by eye than the first detection GW150914!

A few months after the first detection of gravitational waves from the black hole merger event GW150914, the Laser Interferometer Gravitational-Wave Observatory (LIGO) has made another observation of gravitational waves from the collision and merger of a pair of black holes. This signal, called GW151226, arrived at the LIGO detectors on 26 December 2015 at 03:38:53 UTC.

The signal, which came from a distance of around 1.4 billion light-years, was an example of a compact binary coalescence, when two extremely dense objects merge. Binary systems like this are one of many sources of gravitational waves for which the LIGO detectors are searching. Gravitational waves are ripples in space-time itself and carry energy away from such a binary system, causing the two objects to spiral towards each other as they orbit. This inspiral brings the objects closer and closer together until they merge. The gravitational waves produced by the binary stretch and squash space-time as they spread out through the universe. It is this stretching and squashing that can be detected by observatories like Advanced LIGO, and used to reveal information about the sources which created the gravitational waves.

GW151226 is the second definitive observation of a merging binary black hole system detected by the LIGO Scientific Collaboration and Virgo Collaboration. Together with GW150914, this event marks the beginning of gravitational-wave astronomy as a revolutionary new means to explore the frontiers of our Universe….

Read more at: http://www.ligo.org/science/Publication-GW151226/index.php#sthash.GM0EB4ib.dpuf>

Relativity Gets Thorough Vetting from LIGO

The gravitational wave signal observed by the LIGO detectors shows no deviation from what general relativity predicts.

Figure 1: The signal from one of the LIGO detectors in Hanford, Washington, is shown with two representations of the best-fit numerical relativity (NR) waveform. The filtered NR waveform illustrates how the raw waveform is perceived by the detector, showing that for GW150914 the instrument was most sensitive to the late-inspiral, merger, and ringdown of the event (data and analysis scripts from Ref.[9]).

The signal from one of the LIGO detectors in Hanford, Washington, is shown with two representations of the best-fit numerical relativity (NR) waveform. The filtered NR waveform illustrates how the raw waveform is perceived by the detector, showing that for GW150914 the instrument was most sensitive to the late-inspiral, merger, and ringdown of the event

Read more at http://physics.aps.org/articles/v9/52

Detecting “Christodoulou memory effect” with LIGO

Detecting gravitational-wave memory with LIGO: implications of GW150914

 Gravitational-wave strain time series using parameters consistent with GW150914

Gravitational-wave strain time series using parameters consistent with GW150914

Paul D. Lasky, Eric Thrane, Yuri Levin, Jonathan Blackman, Yanbei Chen

It may soon be possible for Advanced LIGO to detect hundreds of binary black hole mergers per year. We show how the accumulation of many such measurements will allow for the detection of gravitational-wave memory: a permanent displacement of spacetime that comes from strong-field, general relativistic effects. We estimate that Advanced LIGO operating at design sensitivity may be able to make a signal-to-noise ratio 3(5) detection of memory with 35(90) events with masses and distance similar to GW150914. Given current merger rate estimates (of one such event per 16 days), this could happen in as few as 1.5(4) years of coincident data collection. We highlight the importance of incorporating higher-order gravitational-wave modes for parameter estimation of binary black hole mergers, and describe how our methods can also be used to detect higher-order modes themselves before Advanced LIGO reaches design sensitivity.

Read more at http://arxiv.org/pdf/1605.01415v1.pdf

Citizen scientists take on latest gravitational-wave data

Einstein@home project will target neutron stars, some of the most mysterious objects in astrophysics.

Fermi spotted that the Crab Nebula, once thought to be constant, flares violently with gamma rays

At the centre of the Crab Nebula (pictured) is a pulsar, a type of neutron star, that may emit gravitational waves.

Davide Castelvecchi
The next discovery of gravitational waves could come from citizen scientists. The Einstein@home project, which uses the idle time on the computers of volunteers who have downloaded a screen saver, is about to start analysing the data from the recently-upgraded Laser Interferometer Gravitational-Wave Observatory (LIGO), a US-led experiment that made history last month with its announcement that it had detected ripples in spacetime.

Since Einstein@home began in 2005, the network has analysed previous data collected by LIGO and its Franco-Italian-led counterpart Virgo near Pisa, Italy, but has so far seen nothing.

On 9 March, the project is due to start analysing data that the upgraded observatory, known as Advanced LIGO, collected between September and January, says Maria Alessandra Papa, a LIGO astrophysicist at the Max Planck Institute for Gravitational Physics in Hannover, Germany. The upgrade vastly increased the volume of sky that LIGO could scan for signals, and led to the discovery of gravitational waves, which was announced on 11 February.

The Einstein@home screen saver automatically downloads and searches chunks of LIGO data, and then sends its results back to the central server, a model inherited from the SETI@home project, which searches radio-astronomy data for messages sent by alien civilizations.

Slow-burn signals

Rather than looking for dramatic sources of gravitational waves, such as the black-hole merger that LIGO detected on 14 September, Einstein@home looks for quieter, slow-burn signals that might be emitted by fast-spinning objects such as some neutron stars. These remnants of supernova explosions are some of the least well understood objects in astrophysics: such searches could help to reveal their nature.

Because they produce a weaker signal than mergers, rotating sources require more computational power to detect. This makes them well-suited to a distributed search. “Einstein@home is used for the deepest searches, the ones that are computationally most demanding,” Papa says. The hope is to extract the weak signals from the background noise by observing for long stretches of time. “The beauty of a continuous signal is that the signal is always there,” she says.

Albert Einstein’s general theory of relativity predicts that a rotating object will produce gravitational waves as long as it is not perfectly symmetrical around its axis of rotation. Neutron stars are thought to be highly symmetrical because their gravity is very intense. But some researchers have theorized that they could have regions of different densities or bumpy surfaces, causing them to emit gravitational waves and slow down their rotation in the process. Observations that some pulsars, a type of neutron star that emits radio-frequency blips, have shown that the stars do slow down, although effects other than gravitational waves are known to contribute to this. If Einstein@home spots gravitational waves from a neutron star, it would suggest that the objects can be asymmetrical.

Mysterious structure

The magnitude of the waves would also allow physicists to determine how hilly or inhomogeneous the neutron star is, which in turn would provide clues about their internal structure. Although neutron stars get their name because their high density means that any protons and electrons present may have been crunched together to form neutrons, astrophysicists don’t know for sure what they are made of, nor how the known laws of physics apply to them. “We call them neutron stars, but we don’t even have overwhelming evidence that they’re made of neutrons. They could be made of more exotic materials,” says Graham Woan, a LIGO astrophysicist at the University of Glasgow, UK.

As it scans its first tranche of data, Einstein@home will look for neutron stars that are emitting waves with frequencies of between 20 hertz and 100 hertz (corresponding to rotation rates of between 10 hertz and 50 hertz), a range where LIGO’s sensitivity has improved dramatically following the US$200 million upgrade.

The professionals aren’t leaving all the work to citizen-scientists, though. Whereas Einstein@home will look for signals that could be coming from anywhere in the Milky Way, scientists at LIGO and Virgo are planning to target known pulsars. Such targeted searches are computationally less intensive than the Einstein@home scans, so can run on a lab’s computer. But they can also be very powerful. “They are probably the most sensitive observations which LIGO makes,” Woan says.

Read more at www.nature.com