Optical, X-ray, and Radio Telescopes Seek Explosive Sources of Gravitational Waves
Observing astronomical events with both light and gravitational waves will tell us more about the cause of the events than either observation would alone. In order to take advantage of this potential, LIGO and Virgo have established partnerships with scientists who operate telescopes around the world and developed the systems needed to quickly analyze gravitational wave data and send alerts to the telescopes. A recent publication, which is summarized below, details the benefits of following-up on possible gravitational wave events with light observations, the partnerships formed, the analysis methods used, and the potential light observability of a candidate gravitational wave detection.
Because gravitational waves are created by the acceleration of matter, they carry information about the motion of matter in the event’s system. However, observing gravitational waves alone can currently only localize their source from tens to hundreds of square degrees of area on the sky (5 full moons fill about 1 square degree). Detecting a new source of light in this area of the sky would improve the source localization to a much higher precision and allow the measurement of the light’s redshift, which indicates the distance to the source. Observing both gravitational waves and light from the same source can also help us identify what causes different kinds of gamma-ray bursts or allow for the observation of certain supernovae from their earliest moments (which can only done by chance with light observations alone).
This study was performed during the 2009-2010 LIGO-Virgo joint run and used three gravitational wave data analysis methods: two to detect bursts and another to detect compact binary inspirals. These methods measured both the strength of a candidate detection and estimated areas on the sky where the signal most likely originated. If the event was strong enough to have a low false alarm probability, the source information was then processed through software that produced observing plans for the partner telescopes. These observing plans suggested the best areas to observe based on where galaxies were located, how much area each could observe and how many pointings (images) they allowed. The event, observing plan and state of the detectors were then reviewed by on-call experts before being sent to the telescopes for observation.
Because of the large area produced in the gravitational wave source localization, most of the partner telescopes were ones that observed large areas of the sky (wide-field) in optical light including the Palomar Transient Factory, Pi of the Sky, QUEST, ROTSE III, SkyMapper, and TAROT. Optical telescopes with narrower fields of view included the Zadko Telescope and the Liverpool Telescope. The LOFAR observatory observed large areas of the sky in radio waves and the Swift satellite observed narrower fields in both X-ray and UV/optical light. (Although not used in the prompt follow-up of candidate gravitational waves in this study, the Expanded Very Large Array also made radio observations within 3 to 5 weeks of some events.)
Ultimately, it was shown that the rapid follow-up of candidate gravitational wave detections is feasible with candidate gravitational wave events being successfully evaluated by humans and sent out to telescopes in about a half an hour's time. Also, it was found through simulations that the correct portion of the sky would be observed for a strong event with ~50% or greater probability with a few wide-field pointings. The results of observations made through this work will be published in the future. These findings and the experience gained from the project are now being used to plan a better, expanded follow-up campaign for when the Advanced LIGO and Advanced Virgo detectors begin operation in a few years.
- Freely readable preprint of the paper describing this work: "Implementation and testing of the first prompt search for gravitational wave transients with electromagnetic counterparts" by J. Abadie et al. (the LIGO Scientific Collaboration and the Virgo Collaboration)
- burst gravitational waves: gravitational waves of short duration from unanticipated sources or from known sources where we can't be sure what the gravitational waves will look like.
- compact binary inspiral: the orbit of two dense objects (like neutron stars and/or black holes) as the distance between the lessens until they merge into one object. This situation is a strong candidate for producing detectable gravitational waves. Read more in these science summaries: Low-latency Search and Low Mass Search.
- electromagnetic (EM) waves: waves composed of coupled electric and magnetic fields. These waves are commonly known as light, although only a small portion of EM wavelengths can be seen by the human eye. In order of increasing wavelength, the kinds of EM light mentioned in this recent paper are: Gamma-rays, X-rays, UV (ultraviolet), visible (optical), radio.
- false alarm probability: the probability that a detector noise fluctuation could produce an event similar to a candidate being considered.
- gamma-ray bursts: extremely energetic explosions of gamma-ray light from astrophysical sources very far away. The exact cause of these bursts is not known. Read more in this science summary.
- redshift: the lengthening of the wavelength of light as it travels through the Universe due to the expansion of the Universe. Measuring the redshift and knowing the observed expansion of the Universe produces an estimate of the distance the light has traveled from where it was produced.
- square degrees: used to measure an area on a sphere and used in astronomy to measure area on the sky. The entire sky (both the day and the night parts) yields about 41,253 square degrees of area.
- supernova (pl. supernovae): the violent explosion of a massive star's outer layers at the end of its life. This releases very bright light as the exploded material expands and can be observed on Earth as a "new star" in the sky that fades over weeks or months.
Figures from the Publication
For more information on the meaning of these figures, see the preprint at arXiv.org.