scholarly journals All-sky search for short gravitational-wave bursts in the third Advanced LIGO and Advanced Virgo run

2021 ◽  
Vol 104 (12) ◽  
Author(s):  
R. Abbott ◽  
T. D. Abbott ◽  
F. Acernese ◽  
K. Ackley ◽  
C. Adams ◽  
...  
2021 ◽  
Vol 104 (10) ◽  
Author(s):  
R. Abbott ◽  
T. D. Abbott ◽  
F. Acernese ◽  
K. Ackley ◽  
C. Adams ◽  
...  

2021 ◽  
Vol 104 (4) ◽  
Author(s):  
Anuradha Samajdar ◽  
Justin Janquart ◽  
Chris Van Den Broeck ◽  
Tim Dietrich

2020 ◽  
Vol 245 ◽  
pp. 07050
Author(s):  
Stefano Bagnasco

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.


2018 ◽  
Vol 97 (10) ◽  
Author(s):  
Margaret Millhouse ◽  
Neil J. Cornish ◽  
Tyson Littenberg

2020 ◽  
Vol 493 (3) ◽  
pp. 4333-4341 ◽  
Author(s):  
M Renzo ◽  
R J Farmer ◽  
S Justham ◽  
S E de Mink ◽  
Y Götberg ◽  
...  

ABSTRACT Gravitational-wave detections are now probing the black hole (BH) mass distribution, including the predicted pair-instability mass gap. These data require robust quantitative predictions, which are challenging to obtain. The most massive BH progenitors experience episodic mass ejections on time-scales shorter than the convective turnover time-scale. This invalidates the steady-state assumption on which the classic mixing length theory relies. We compare the final BH masses computed with two different versions of the stellar evolutionary code $\tt{MESA}$: (i) using the default implementation of Paxton et al. (2018) and (ii) solving an additional equation accounting for the time-scale for convective deceleration. In the second grid, where stronger convection develops during the pulses and carries part of the energy, we find weaker pulses. This leads to lower amounts of mass being ejected and thus higher final BH masses of up to ∼$5\, \mathrm{M}_\odot$. The differences are much smaller for the progenitors that determine the maximum mass of BHs below the gap. This prediction is robust at $M_{\rm BH, max}\simeq 48\, \mathrm{M}_\odot$, at least within the idealized context of this study. This is an encouraging indication that current models are robust enough for comparison with the present-day gravitational-wave detections. However, the large differences between individual models emphasize the importance of improving the treatment of convection in stellar models, especially in the light of the data anticipated from the third generation of gravitational-wave detectors.


2003 ◽  
Vol 67 (6) ◽  
Author(s):  
Nicolas Arnaud ◽  
Matteo Barsuglia ◽  
Marie-Anne Bizouard ◽  
Violette Brisson ◽  
Fabien Cavalier ◽  
...  

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