scholarly journals A challenge to identify an optical counterpart of the gravitational wave event GW151226 with Hyper Suprime-Cam†

2017 ◽  
Vol 70 (1) ◽  
Author(s):  
Yousuke Utsumi ◽  
Nozomu Tominaga ◽  
Masaomi Tanaka ◽  
Tomoki Morokuma ◽  
Michitoshi Yoshida ◽  
...  
Keyword(s):  
Gravitational Wave ◽  
Optical Counterpart ◽  
Wave Event

scholarly journals A DECAM SEARCH FOR AN OPTICAL COUNTERPART TO THE LIGO GRAVITATIONAL-WAVE EVENT GW151226

2016 ◽  
Vol 826 (2) ◽  
pp. L29 ◽  
Author(s):  
P. S. Cowperthwaite ◽  
E. Berger ◽  
M. Soares-Santos ◽  
J. Annis ◽  
D. Brout ◽  
...  
Keyword(s):  
Gravitational Wave ◽  
Optical Counterpart ◽  
Wave Event

scholarly journals Search for the optical counterpart of the GW170814 gravitational wave event with the VLT Survey Telescope

2019 ◽  
Vol 492 (2) ◽  
pp. 1731-1754 ◽  
Author(s):  
A Grado ◽  
E Cappellaro ◽  
S Covino ◽  
F Getman ◽  
G Greco ◽  
...  
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Optical Radiation ◽  
Laser Interferometer ◽  
Time Interval ◽  
Optical Counterpart ◽  
Binary Black Hole ◽  
Transient Source ◽  
Wave Event ◽  
Observational Strategy

ABSTRACT We report on the search for the optical counterpart of the gravitational event GW170814, which was carried out with the VLT Survey Telescope (VST) by the GRAvitational Wave Inaf TeAm. Observations started 17.5 h after the Laser Interferometer Gravitational-wave Observatory (LIGO) and Virgo alert and we covered an area of 99 deg2 that encloses $\sim 77{{\ \rm per\ cent}}$ and $\sim 59{{\ \rm per\ cent}}$ of the initial and refined localization probability regions, respectively. A total of six epochs were secured over nearly two months. The survey reached an average limiting magnitude of 22 AB mag in the r band. After assuming the model described in Perna, Lazzati & Farr, that derives as possible optical counterpart of a BBH (binary black hole) event a transient source declining in about one day, we have computed a survey efficiency of about $5{{\ \rm per\ cent}}$. This paper describes the VST observational strategy and the results obtained by our analysis pipelines developed to search for optical transients in multi-epoch images. We report the catalogue of the candidates with possible identifications based on light-curve fitting. We have identified two dozens of SNe, nine AGNs, and one QSO. Nineteen transients characterized by a single detection were not classified. We have restricted our analysis only to the candidates that fall into the refined localization map. None out of 39 left candidates could be positively associated with GW170814. This result implies that the possible emission of optical radiation from a BBH merger had to be fainter than r ∼ 22 (Loptical ∼ 1.4 × 1042 erg s−1) on a time interval ranging from a few hours up to two months after the gravitational wave event.

scholarly journals A DARK ENERGY CAMERA SEARCH FOR AN OPTICAL COUNTERPART TO THE FIRST ADVANCED LIGO GRAVITATIONAL WAVE EVENT GW150914

2016 ◽  
Vol 823 (2) ◽  
pp. L33 ◽  
Author(s):  
M. Soares-Santos ◽  
R. Kessler ◽  
E. Berger ◽  
J. Annis ◽  
D. Brout ◽  
...  
Keyword(s):  
Dark Energy ◽  
Gravitational Wave ◽  
Optical Counterpart ◽  
Wave Event

scholarly journals A SEARCH FOR AN OPTICAL COUNTERPART TO THE GRAVITATIONAL-WAVE EVENT GW151226

2016 ◽  
Vol 827 (2) ◽  
pp. L40 ◽  
Author(s):  
S. J. Smartt ◽  
K. C. Chambers ◽  
K. W. Smith ◽  
M. E. Huber ◽  
D. R. Young ◽  
...  
Keyword(s):  
Gravitational Wave ◽  
Optical Counterpart ◽  
Wave Event

scholarly journals Virgo and Gravitational-Wave Computing in Europe

2020 ◽  
Vol 245 ◽  
pp. 07050
Author(s):  
Stefano Bagnasco
Keyword(s):  
Gravitational Wave ◽  
Current Status ◽  
Low Latency ◽  
Observational Period ◽  
Compact Binaries ◽  
The Third ◽  
Compact Binary ◽  
Continuous Waves ◽  
The Us ◽  
Wave Event

Advanced Virgo is an interferometer for the detection of gravitational waves at the European Gravitational Observatory in Italy. Along with the two Advanced LIGO interferometers in the US, Advanced Virgo is being used to collect data from astrophysical sources such as compact binary coalescences and is currently running the third observational period, collecting gravitational wave event candidates at a rate of more than once per week. Data from the interferometer are processed by running search pipelines for several expected signals, from coalescing compact binaries to continuous waves and burst events. Furthermore, detector characterisation studies are run. Some of the processing needs to be done with low latency, to be able to provide triggers for other observatories and make multi-messenger observations possible. Deep searches are run offline on external computing centres. Thus, data needs also to be reliably and promptly distributed from the EGO site to computer centres in Europe and the US for further analysis and archival storage. Two of the defining characteristics of Virgo computing are the heterogeneity of the activities and the need to interoperate with LIGO. A very wide array of analysis pipelines differing in scientific target, implementation details and running environment assumptions have to be allowed to run ubiquitously and uniformly on dedicated resources and, in perspective, on heterogeneous infrastructures. The current status, possible strategies and outlook of Virgo computing are discussed.

scholarly journals GRANDMA: A NETWORK TO COORDINATE THEM ALL

2021 ◽  
Vol 53 ◽  
pp. 198-205
Author(s):  
S. Agayeva ◽  
S. Alishov ◽  
S. Antier ◽  
V. R. Ayvazian ◽  
J. M. Bai ◽  
...  
Keyword(s):  
Organizational Structure ◽  
Gravitational Wave ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
International Project ◽  
Optical Counterpart ◽  
Transient Source ◽  
Transient Sources ◽  
Imaging Strategy ◽  
Initial Results

GRANDMA is an international project that coordinates telescope observations of transient sources with large localization uncertainties. Such sources include gravitational wave events, gamma-ray bursts and neutrino events. GRANDMA currently coordinates 25 telescopes (70 scientists), with the aim of optimizing the imaging strategy to maximize the probability of identifying an optical counterpart of a transient source. This paper describes the motivation for the project, organizational structure, methodology and initial results.

scholarly journals A comparison between short GRB afterglows and kilonova AT2017gfo: shedding light on kilonovae properties

2020 ◽  
Vol 493 (3) ◽  
pp. 3379-3397 ◽  
Author(s):  
A Rossi ◽  
G Stratta ◽  
E Maiorano ◽  
D Spighi ◽  
N Masetti ◽  
...  
Keyword(s):  
Gravitational Wave ◽  
Gamma Ray ◽  
Light Curves ◽  
Optical Counterpart ◽  
Wave Source ◽  
Gamma Ray Burst ◽  
Nir Light ◽  
First Time ◽  
Short Grbs

ABSTRACT Multimessenger astronomy received a great boost following the discovery of kilonova (KN) AT2017gfo, the optical counterpart of the gravitational wave source GW170817 associated with the short gamma-ray burst GRB 170817A. AT2017gfo was the first KN that could be extensively monitored in time using both photometry and spectroscopy. Previously, only few candidates have been observed against the glare of short GRB afterglows. In this work, we aim to search the fingerprints of AT2017gfo-like KN emissions in the optical/NIR light curves of 39 short GRBs with known redshift. For the first time, our results allow us to study separately the range of luminosity of the blue and red components of AT2017gfo-like kilonovae in short GRBs. In particular, the red component is similar in luminosity to AT2017gfo, while the blue KN can be more than 10 times brighter. Finally, we exclude a KN as luminous as AT2017gfo in GRBs 050509B and 061201.

scholarly journals Strong lensing as a giant telescope to localize the host galaxy of gravitational wave event

2020 ◽  
Vol 497 (1) ◽  
pp. 204-209 ◽  
Author(s):  
Hai Yu ◽  
Pengjie Zhang ◽  
Fa-Yin Wang
Keyword(s):  
Gravitational Wave ◽  
Host Galaxy ◽  
Observational Constraints ◽  
Host Galaxies ◽  
Einstein Telescope ◽  
Strong Lensing ◽  
Potential Applications ◽  
Wave Event ◽  
Localization Uncertainty ◽  
Better Than

ABSTRACT Standard siren cosmology of gravitational wave (GW) merger events relies on the identification of host galaxies and their redshifts. But this can be highly challenging due to numerous candidates of galaxies in the GW localization area. We point out that the number of candidates can be reduced by orders of magnitude for strongly lensed GW events, due to extra observational constraints. For the next-generation GW detectors like Einstein Telescope (ET), we estimate that this number is usually significantly less than one, as long as the GW localization uncertainty is better than $\sim 10\, \rm deg^2$. This implies that the unique identification of the host galaxy of lensed GW event detected by ET and Cosmic Explorer (CE) is possible. This provides us a promising opportunity to measure the redshift of the GW event and facilitate the standard siren cosmology. We also discuss its potential applications in understanding the evolution process and environment of the GW event.

scholarly journals Observations with Wide-band Gravitational Radiation Detectors

1974 ◽  
Vol 64 ◽  
pp. 37-37
Author(s):  
R. W. P. Drever ◽  
J. Hough ◽  
R. Bland ◽  
G. W. Lessnoff
Keyword(s):  
Gravitational Wave ◽  
Gravitational Radiation ◽  
Wide Band ◽  
Radiation Detectors ◽  
Upper Limit ◽  
Wave Event

The principles and operation of wide-band gravitational radiation detectors are described. In 7 months of coincidence observations, one signal which fulfills requirements set for a gravitational wave event was recorded, and details are presented. The experiment sets an upper limit to millisecond pulses of gravitational radiation of 0.9±2.1 per month at a 25% threshold of 0.3kT in 300 kG bars, which appears inconsistent with the flux implied by Weber's 1970 results if these are due to such pulses.

scholarly journals A First Search for Prompt Radio Emission from a Gravitational-wave Event

2019 ◽  
Vol 877 (2) ◽  
pp. L39 ◽  
Author(s):  
Thomas A. Callister ◽  
Marin M. Anderson ◽  
Gregg Hallinan ◽  
Larry R. D’addario ◽  
Jayce Dowell ◽  
...  
Keyword(s):  
Radio Emission ◽  
Gravitational Wave ◽  
Wave Event
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