Optical/Infrared Telescopes Follow Gravitational Waves to Treasure
October 16, 2017
Astronomers have tracked down the source of a gravitational wave and discovered the first observed kilonova: a nuclear furnace 100 million times brighter than the Sun producing thousands of times the entire mass of the Earth in heavy elements such as precious metals.
On August 17, 2017 the LIGO-Virgo collaboration alerted more than 90 astronomy teams around the world, that they had detected a signal (GW170817) consistent with the inspiral and merger of two neutron stars. Dr. Raffaele Flaminio (NAOJ and CNRS/LAPP), a scientist from the Virgo and KAGRA collaborations, explains that "Thanks to the combination of the data from the LIGO detectors in the US and the Virgo detector in Europe, this was the best ever localized gravitational wave source."
J-GEM (Japanese collaboration of Gravitational wave Electro-Magnetic follow-up) is a research project to search for optical counterparts of gravitational wave sources because optical observations give us different information than gravitational wave observations. Indeed multi-messenger astronomy, observing the same phenomenon with both gravitational waves and normal light, is needed to paint the full picture of the phenomenon.
Neutron star mergers are expected to have strong optical and infrared light emissions, so J-GEM sprang in to action. Using a network of telescopes around the world, including the Subaru Telescope in Hawai'i and the 1.4-m IRSF telescope in South Africa (run by Nagoya University and Kagoshima University), they observed the source located 130 million light-years away in the constellation Hydra, trying to discern its true nature. As they watched the object change day by day, they realized that they were observing the first ever confirmed kilonova.
Astronomers have long searched for sites in the Universe where the heavy elements were produced by rapid neutron capture (r-process) reactions. One possible candidate was kilonova explosions which are predicted to produce 10,000 times the mass of the Earth in rare earth elements and precious metals.
The time evolution of the color and brightness of the object at the origin of the gravitational waves were too rapid to be a supernova, but matched the simulations of a kilonova made by the ATERUI supercomputer at the National Astronomical Observatory of Japan.
"We were so excited to see the rapid brightness evolution revealed day by day through observations at facilities operated by Japanese institutes distributed all over the world." said Dr. Yousuke Utsumi (Hiroshima University), a scientist in the J-GEM collaboration.
Moive: The optical and near-infrared counterpart of GW170817 capture by HSC mounted on the Subaru Telescope. (Credit: NAOJ)
Two papers on this research will be published in Publications of the Astronomical Society of Japan (PASJ) on October 16, 2017 (Utsumi et al., "J-GEM observations of an electromagnetic counterpart to the neutron star merger GW170817", and Tanaka et al., "Kilonova from post-merger ejecta as an optical and near-infrared counterpart of GW170817"). Another paper is also submitted to PASJ (Tominaga et al., "Subaru Hyper Suprime-Cam survey for an optical counterpart of GW170817").
- Subaru / Hyper Suprime-Cam image for the optical follow-up to GW170817 (J-GEM Project)
- Press release from CfCA, NAOJ
- Press release from Gravitational Wave Project Office, NAOJ
- Press release from School of Science, University of Tokyo
- Press release from Nagoya University
- Press release from Hiroshima University