Journal articles: 'Gravitational Wave Counterparts'

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WEN, LINQING. "DETECTING GRAVITATIONAL WAVES AND THEIR ELECTROMAGNETIC COUNTERPARTS." International Journal of Modern Physics D 20, no. 10 (September 2011): 1883–90. http://dx.doi.org/10.1142/s021827181101989x.

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In the next decade, we expect a first detection of gravitational waves predicted by Einstein's general theory of relativity. A detection of their electromagnetic counterparts will significantly contribute to our confidence in a first time detection and identification of the source. We discuss the challenges in using gravitational-wave events as triggers for prompt follow-up electromagnetic observations. We demonstrate that wide-field cameras are desirable for follow-up observations of gravitational wave sources and that a larger gravitational wave detector network, e.g. adding AIGO detector in Australia, can significantly help pinpoint the direction of gravitational wave sources. We also argue that low-latency real-time detection methods and hardware acceleration using graphics processing units will help generate prompt gravitational-wave triggers within the time frames allowed for electromagnetic follow-ups in the era of advanced detectors.

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Unatlokov, I. B., I. M. Dzaparova, M. G. Kostyuk, M. M. Kochkarov, A. N. Kurenya, Yu F. Novoseltsev, R. V. Novoseltseva, V. B. Petkov, P. S. Striganov, and A. F. Yanin. "Search for neutrino counterparts of LIGO/Virgo gravitational-wave events." Journal of Physics: Conference Series 2156, no. 1 (December 1, 2021): 012142. http://dx.doi.org/10.1088/1742-6596/2156/1/012142.

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Abstract The LIGO/Virgo collaborations have reported the results of their searches for gravitational-waves from the first half of their third observing run. 39 events were combined into the second Gravitational-Wave Transient Catalog (GWTC-2), reaching the total number of 50. In addition to these, two neutron star - black hole merger events were also confirmed. The search for neutrino counterparts of LIGO/Virgo gravitational-wave events was performed on the Baksan Underground Scintillation Telescope. The processing algorithm and the results of the counterpart search are described.

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Nuttall, Laura K., and Christopher P. L. Berry. "Electromagnetic counterparts of gravitational-wave signals." Astronomy & Geophysics 62, no. 4 (August 1, 2021): 4.15–4.21. http://dx.doi.org/10.1093/astrogeo/atab077.

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Kostrzewa-Rutkowska, Z., P. G. Jonker, S. T. Hodgkin, D. Eappachen, D. L. Harrison, S. E. Koposov, G. Rixon, et al. "Electromagnetic counterparts to gravitational wave events from Gaia." Monthly Notices of the Royal Astronomical Society 493, no. 3 (February 13, 2020): 3264–73. http://dx.doi.org/10.1093/mnras/staa436.

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ABSTRACT The recent discoveries of gravitational wave events and in one case also its electromagnetic (EM) counterpart allow us to study the Universe in a novel way. The increased sensitivity of the LIGO and Virgo detectors has opened the possibility for regular detections of EM transient events from mergers of stellar remnants. Gravitational wave sources are expected to have sky localization up to a few hundred square degrees, thus Gaia as an all-sky multi-epoch photometric survey has the potential to be a good tool to search for the EM counterparts. In this paper, we study the possibility of detecting EM counterparts to gravitational wave sources using the Gaia Science Alerts system. We develop an extension to current used algorithms to find transients and test its capabilities in discovering candidate transients on a sample of events from the observation periods O1 and O2 of LIGO and Virgo. For the gravitational wave events from the current run O3, we expect that about 16 (25) per cent should fall in sky regions observed by Gaia 7 (10) d after gravitational wave. The new algorithm will provide about 21 candidates per day from the whole sky.

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Lazio, Joseph, Katie Keating, F. A. Jenet, and N. E. Kassim. "Search for Electromagnetic Counterparts to LIGO-Virgo Candidates: Expanded Very Large Array Observations." Proceedings of the International Astronomical Union 7, S285 (September 2011): 67–70. http://dx.doi.org/10.1017/s1743921312000245.

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AbstractThis paper summarizes a search for radio-wavelength counterparts to candidate gravitational-wave events. The identification of an electromagnetic counterpart could provide a more complete understanding of a gravitational-wave event, including such characteristics as the location and the nature of the progenitor. We used the Expanded Very Large Array (EVLA) to search six galaxies which were identified as potential hosts for two candidate gravitational-wave events. We summarize our procedures and discuss preliminary results.

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Coughlin, Michael W., Sarah Antier, David Corre, Khalid Alqassimi, Shreya Anand, Nelson Christensen, David A. Coulter, et al. "Optimizing multitelescope observations of gravitational-wave counterparts." Monthly Notices of the Royal Astronomical Society 489, no. 4 (September 7, 2019): 5775–83. http://dx.doi.org/10.1093/mnras/stz2485.

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ABSTRACT The ever-increasing sensitivity of the network of gravitational-wave detectors has resulted in the accelerated rate of detections from compact binary coalescence systems in the third observing run of Advanced LIGO and Advanced Virgo. Not only has the event rate increased, but also the distances to which phenomena can be detected, leading to a rise in the required sky volume coverage to search for counterparts. Additionally, the improvement of the detectors has resulted in the discovery of more compact binary mergers involving neutron stars, revitalizing dedicated follow-up campaigns. While significant effort has been made by the community to optimize single telescope observations, using both synoptic and galaxy-targeting methods, less effort has been paid to coordinated observations in a network. This is becoming crucial, as the advent of gravitational-wave astronomy has garnered interest around the globe, resulting in abundant networks of telescopes available to search for counterparts. In this paper, we extend some of the techniques developed for single telescopes to a telescope network. We describe simple modifications to these algorithms and demonstrate them on existing network examples. These algorithms are implemented in the open-source software gwemopt, used by some follow-up teams, for ease of use by the broader community.

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Steele, Iain A., Chris M. Copperwheat, and Andrzej S. Piascik. "Spectroscopy of candidate electromagnetic counterparts to gravitational wave sources." Proceedings of the International Astronomical Union 12, S324 (September 2016): 283–86. http://dx.doi.org/10.1017/s1743921316012515.

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AbstractA programme of worldwide, multi-wavelength electromagnetic follow-up of sources detected by gravitational wave detectors is in place. Following the discovery of GW150914 and GW151226, wide field imaging of their sky localisations identified a number of candidate optical counterparts which were then spectrally classified. The majority of candidates were found to be supernovae at redshift ranges similar to the GW events and were thereby ruled out as a genuine counterpart. Other candidates ruled out include AGN and Solar System objects. Given the GW sources were black hole binary mergers, the lack of an identified electromagnetic counterpart is not surprising. However the observations show that it is possible to organise and execute a campaign that can eliminate the majority of potential counterparts. Finally we note the existence of a “classification gap” with a significant fraction of candidates going unclassified.

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JinJun, GENG, XIAO Di, WANG ShanQin, and DAI ZiGao. "Electromagnetic counterparts to the gravitational wave event GW170817." SCIENTIA SINICA Physica, Mechanica & Astronomica 48, no. 7 (June 11, 2018): 079802. http://dx.doi.org/10.1360/sspma2018-00096.

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Salmon, L., L. Hanlon, R. M. Jeffrey, and A. Martin-Carrillo. "Web application for galaxy-targeted follow-up of electromagnetic counterparts to gravitational wave sources." Astronomy & Astrophysics 634 (January 31, 2020): A32. http://dx.doi.org/10.1051/0004-6361/201936573.

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The Laser Interferometer Gravitational Wave Observatory (LIGO) and Virgo Collaboration’s Observing Run 3 has demanded the development of widely-applicable tools for gravitational wave follow-up. These tools must address the main challenges of the multi-messenger era, namely covering large localisation regions and quickly identifying decaying transients. To address these challenges, we present a public web interface to assist astronomers in conducting galaxy-targeted follow-up of gravitational wave events by offering a fast and public list of targets post-gravitational wave trigger. After a gravitational wave trigger, the back-end galaxy retrieval algorithm identifies and scores galaxies based on the LIGO and Virgo computed probabilities and properties of the galaxies taken from the Galaxy List for the Advanced Detector Era V2 galaxy catalogue. Within minutes, the user can retrieve, download, and limit ranked galaxy lists from the web application. The algorithm and website have been tested on past gravitational wave events, and execution times have been analysed. The algorithm is being triggered automatically during Observing Run 3 and its features will be extended if needed. The web application was developed using the Python based Flask web framework.

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Coughlin, Michael W., Duo Tao, Man Leong Chan, Deep Chatterjee, Nelson Christensen, Shaon Ghosh, Giuseppe Greco, et al. "Optimizing searches for electromagnetic counterparts of gravitational wave triggers." Monthly Notices of the Royal Astronomical Society 478, no. 1 (April 26, 2018): 692–702. http://dx.doi.org/10.1093/mnras/sty1066.

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Stachie, Cosmin, Michael W. Coughlin, Tim Dietrich, Sarah Antier, Mattia Bulla, Nelson Christensen, Reed Essick, et al. "Predicting electromagnetic counterparts using low-latency gravitational-wave data products." Monthly Notices of the Royal Astronomical Society 505, no. 3 (June 23, 2021): 4235–48. http://dx.doi.org/10.1093/mnras/stab1492.

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ABSTRACT Searches for gravitational-wave counterparts have been going in earnest since GW170817 and the discovery of AT2017gfo. Since then, the lack of detection of other optical counterparts connected to binary neutron star or black hole–neutron star candidates has highlighted the need for a better discrimination criterion to support this effort. At the moment, low-latency gravitational-wave alerts contain preliminary information about binary properties and hence whether a detected binary might have an electromagnetic counterpart. The current alert method is a classifier that estimates the probability that there is a debris disc outside the black hole created during the merger as well as the probability of a signal being a binary neutron star, a black hole–neutron star, a binary black hole, or of terrestrial origin. In this work, we expand upon this approach to both predict the ejecta properties and provide contours of potential light curves for these events, in order to improve the follow-up observation strategy. The various sources of uncertainty are discussed, and we conclude that our ignorance about the ejecta composition and the insufficient constraint of the binary parameters by low-latency pipelines represent the main limitations. To validate the method, we test our approach on real events from the second and third Advanced Laser Interferometer Gravitational-Wave Observatory (LIGO)–Virgo observing runs.

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Centrella, Joan, Samaya Nissanke, and Roy Williams. "Gravitational Waves and Time-Domain Astronomy." Proceedings of the International Astronomical Union 7, S285 (September 2011): 191–98. http://dx.doi.org/10.1017/s1743921312000592.

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AbstractThe gravitational-wave window onto the universe will open in roughly five years, when Advanced LIGO and Virgo achieve the first detections of high-frequency gravitational waves, most likely coming from compact binary mergers. Electromagnetic follow-up of these triggers, using radio, optical, and high energy telescopes, promises exciting opportunities in multi-messenger time-domain astronomy. In the decade, space-based observations of low-frequency gravitational waves from massive black hole mergers, and their electromagnetic counterparts, will open up further vistas for discovery. This two-part workshop featured brief presentations and stimulating discussions on the challenges and opportunities presented by gravitational-wave astronomy. Highlights from the workshop, with the emphasis on strategies for electromagnetic follow-up, are presented in this report.

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Lamb, Gavin P., and Shiho Kobayashi. "Electromagnetic counterparts to structured jets from gravitational wave detected mergers." Monthly Notices of the Royal Astronomical Society 472, no. 4 (September 11, 2017): 4953–64. http://dx.doi.org/10.1093/mnras/stx2345.

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KAMBLE, ATISH, and DAVID L. A. KAPLAN. "ELECTROMAGNETIC COUNTERPARTS OF GRAVITATIONAL WAVE SOURCES: MERGERS OF COMPACT OBJECTS." International Journal of Modern Physics D 22, no. 01 (January 2013): 1341011. http://dx.doi.org/10.1142/s0218271813410113.

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Mergers of compact objects are considered prime sources of gravitational waves (GW) and will soon be targets of GW observatories such as the Advanced-LIGO and VIRGO. Finding electromagnetic counterparts of these GW sources will be important to understand their nature. We discuss possible electromagnetic signatures of the mergers. We show that the BH–BH mergers could have luminosities which exceed Eddington luminosity from unity to several orders of magnitude depending on the masses of the merging BHs. As a result these mergers could be explosive, release up to 1051 erg of energy and shine as radio transients. At any given time we expect about a few such transients in the sky at GHz frequencies, which could be detected to be about 300 Mpc. It has also been argued that these radio transients would look alike radio supernovae with comparable detection rates. Multi-band follow-up could, however, distinguish between the mergers and supernovae.

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Aasi, J., J. Abadie, B. P. Abbott, R. Abbott, T. Abbott, M. R. Abernathy, T. Accadia, et al. "FIRST SEARCHES FOR OPTICAL COUNTERPARTS TO GRAVITATIONAL-WAVE CANDIDATE EVENTS." Astrophysical Journal Supplement Series 211, no. 1 (February 11, 2014): 7. http://dx.doi.org/10.1088/0067-0049/211/1/7.

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Verrecchia, Francesco, Marco Tavani, Andrea Bulgarelli, Martina Cardillo, Claudio Casentini, Immacolata Donnarumma, Francesco Longo, et al. "AGILE search for gamma-ray counterparts of gravitational wave events." Rendiconti Lincei. Scienze Fisiche e Naturali 30, S1 (November 5, 2019): 71–77. http://dx.doi.org/10.1007/s12210-019-00854-0.

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Möller, A., B. E. Tucker, P. Armstrong, S. W. Chang, N. Lowson, C. A. Onken, F. Panther, et al. "First Results of the SkyMapper Transient Survey." Proceedings of the International Astronomical Union 14, S339 (November 2017): 3–6. http://dx.doi.org/10.1017/s1743921318002077.

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AbstractThe SkyMapper Transient survey (SMT) is exploring variability in the southern sky by performing (a) a rolling search to discover and study supernovæ, and (b) a Target of Opportunity programme that uses the robotic SkyMapper Telescope at Siding Spring Observatory. The supernova survey is obtaining a non-targeted sample of Type Ia supernovæ (SNe Ia) at low redshifts, z < 0.1, and studying other interesting transients found with the search strategy. We have a Target of Opportunity programme with an automatic response mechanism to search for optical counterparts to gravitational-wave and fast radio-burst events; it benefits from SkyMapper’s large field of view of 5.7 sq. deg. and a rapid data reduction pipeline.We present first results of the SMT survey. The SMT pipeline can process and obtain potential candidates within 12 hours of observation. It disentangles real transients from processing artefacts using a machine-learning algorithm. To date, SMT has discovered over 60 spectroscopically confirmed supernovæ, several peculiar objects, and over 40 SNe Ia including one (SNIa 2016hhd) which was found within the first few days of explosion. We have also participated in searches for optical counterparts of gravitational waves, fast radio bursts and other transients, and have published observations of the optical counterpart of the gravitational-wave event GW170817. We also participate in coordinated observations with the Deeper Wider Faster programme, and the Kepler K2 cosmology project.

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Salmon, L., L. Hanlon, R. M. Jeffrey, and A. Martin-Carrillo. "GALAXY-TARGETED ROBOTIC TELESCOPE FOLLOW-UP OF GRAVITATIONAL WAVE EVENTS." Revista Mexicana de Astronomía y Astrofísica Serie de Conferencias 53 (September 2021): 67–74. http://dx.doi.org/10.22201/ia.14052059p.2021.53.17.

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Robotic telescopes and networks are well equipped to respond rapidly to transient events. However, the era of multi-messenger astronomy presents new challenges in the search for electromagnetic counterparts to gravitational wave events. Specifically, these sources can be distant, faint, poorly localised, and quickly decaying. Effciently searching for counterparts requires coverage of large localisation regions and/or targeted observations. This paper presents a galaxy retrieval and ranking algorithm for targeted observations, and a public web interface to retrieve ranked galaxy lists following a gravitational wave event. The website is publicly available at https://gwtool.watchertelescope.ie/.

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Chatterjee, Deep, Gautham Narayan, Patrick D. Aleo, Konstantin Malanchev, and Daniel Muthukrishna. "El-CID: a filter for gravitational-wave electromagnetic counterpart identification." Monthly Notices of the Royal Astronomical Society 509, no. 1 (October 20, 2021): 914–30. http://dx.doi.org/10.1093/mnras/stab3023.

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ABSTRACT As gravitational-wave (GW) interferometers become more sensitive and probe ever more distant reaches, the number of detected binary neutron star mergers will increase. However, detecting more events farther away with GWs does not guarantee corresponding increase in the number of electromagnetic counterparts of these events. Current and upcoming wide-field surveys that participate in GW follow-up operations will have to contend with distinguishing the kilonova (KN) from the ever increasing number of transients they detect, many of which will be consistent with the GW sky-localization. We have developed a novel tool based on a temporal convolutional neural network architecture, trained on sparse early-time photometry and contextual information for Electromagnetic Counterpart Identification (El-CID). The overarching goal for El-CID is to slice through list of new transient candidates that are consistent with the GW sky localization, and determine which sources are consistent with KNe, allowing limited target-of-opportunity resources to be used judiciously. In addition to verifying the performance of our algorithm on an extensive testing sample, we validate it on AT2017gfo – the only EM counterpart of a binary neutron star merger discovered to date – and AT2019npv – a supernova that was initially suspected as a counterpart of the GW event, GW190814, but was later ruled out after further analysis.

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Dobie, Dougal, Tara Murphy, David L. Kaplan, Kenta Hotokezaka, Juan Pablo Bonilla Ataides, Elizabeth K. Mahony, and Elaine M. Sadler. "Radio afterglows from compact binary coalescences: prospects for next-generation telescopes." Monthly Notices of the Royal Astronomical Society 505, no. 2 (May 22, 2021): 2647–61. http://dx.doi.org/10.1093/mnras/stab1468.

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ABSTRACT The detection of gravitational waves from a neutron star merger, GW170817, marked the dawn of a new era in time-domain astronomy. Monitoring of the radio emission produced by the merger, including high-resolution radio imaging, enabled measurements of merger properties including the energetics and inclination angle. In this work, we compare the capabilities of current and future gravitational wave facilities to the sensitivity of radio facilities to quantify the prospects for detecting the radio afterglows of gravitational wave events. We consider three observing strategies to identify future mergers – wide field follow-up, targeting galaxies within the merger localization and deep monitoring of known counterparts. We find that while planned radio facilities like the Square Kilometre Array will be capable of detecting mergers at gigaparsec distances, no facilities are sufficiently sensitive to detect mergers at the range of proposed third-generation gravitational wave detectors that would operate starting in the 2030s.

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Kanner, Jonah, Tracy L. Huard, Szabolcs Márka, David C. Murphy, Jennifer Piscionere, Molly Reed, and Peter Shawhan. "LOOC UP: locating and observing optical counterparts to gravitational wave bursts." Classical and Quantum Gravity 25, no. 18 (September 2, 2008): 184034. http://dx.doi.org/10.1088/0264-9381/25/18/184034.

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Sylvestre, Julien. "Prospects for the Detection of Electromagnetic Counterparts to Gravitational Wave Events." Astrophysical Journal 591, no. 2 (July 10, 2003): 1152–56. http://dx.doi.org/10.1086/375505.

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Levan, Andrew J., and Peter G. Jonker. "Electromagnetic counterparts of gravitational wave sources at the Very Large Telescope." Nature Reviews Physics 2, no. 9 (July 16, 2020): 455–57. http://dx.doi.org/10.1038/s42254-020-0216-2.

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Gompertz, B. P., R. Cutter, D. Steeghs, D. K. Galloway, J. Lyman, K. Ulaczyk, M. J. Dyer, et al. "Searching for electromagnetic counterparts to gravitational-wave merger events with the prototype Gravitational-Wave Optical Transient Observer (GOTO-4)." Monthly Notices of the Royal Astronomical Society 497, no. 1 (July 3, 2020): 726–38. http://dx.doi.org/10.1093/mnras/staa1845.

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ABSTRACT We report the results of optical follow-up observations of 29 gravitational-wave (GW) triggers during the first half of the LIGO–Virgo Collaboration (LVC) O3 run with the Gravitational-wave Optical Transient Observer (GOTO) in its prototype 4-telescope configuration (GOTO-4). While no viable electromagnetic (EM) counterpart candidate was identified, we estimate our 3D (volumetric) coverage using test light curves of on- and off-axis gamma-ray bursts and kilonovae. In cases where the source region was observable immediately, GOTO-4 was able to respond to a GW alert in less than a minute. The average time of first observation was 8.79 h after receiving an alert (9.90 h after trigger). A mean of 732.3 square degrees were tiled per event, representing on average 45.3 per cent of the LVC probability map, or 70.3 per cent of the observable probability. This coverage will further improve as the facility scales up alongside the localization performance of the evolving GW detector network. Even in its 4-telescope prototype configuration, GOTO is capable of detecting AT2017gfo-like kilonovae beyond 200 Mpc in favourable observing conditions. We cannot currently place meaningful EM limits on the population of distant ($\hat{D}_L = 1.3$ Gpc) binary black hole mergers because our test models are too faint to recover at this distance. However, as GOTO is upgraded towards its full 32-telescope, 2 node (La Palma & Australia) configuration, it is expected to be sufficiently sensitive to cover the predicted O4 binary neutron star merger volume, and will be able to respond to both northern and southern triggers.

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Duque, R., F. Daigne, and R. Mochkovitch. "Radio afterglows of binary neutron star mergers: a population study for current and future gravitational wave observing runs." Astronomy & Astrophysics 631 (October 17, 2019): A39. http://dx.doi.org/10.1051/0004-6361/201935926.

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Following the historical observations of GW170817 and its multi-wavelength afterglow, more radio afterglows from neutron star mergers are expected in the future as counterparts to gravitational wave inspiral signals. Our aim is to describe these events using our current knowledge of the population of neutron star mergers based on gamma-ray burst science, and taking into account the sensitivities of current and future gravitational wave and radio detectors. We combined analytical models for the merger gravitational wave and radio afterglow signals to a population model prescribing the energetics, circum-merger density and other relevant parameters of the mergers. We reported the expected distributions of observables (distance, orientation, afterglow peak time and flux, etc.) for future events and studied how these can be used to further probe the population of binary neutron stars, their mergers and related outflows during future observing campaigns. In the case of the O3 run of the LIGO-Virgo Collaboration, the radio afterglow of one third of gravitational-wave-detected mergers should be detectable (and detected if the source is localized thanks to the kilonova counterpart) by the Very Large Array. Furthermore, these events should have viewing angles similar to that of GW170817. These findings confirm the radio afterglow as a powerful insight into these events, although some key afterglow-related techniques, such as very long baseline interferometry imaging of the merger remnant, may no longer be feasible as the gravitational wave horizon increases.

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Lamb, Gavin P., and Shiho Kobayashi. "Revealing Short GRB Jet Structure and Dynamics with Gravitational Wave Electromagnetic Counterparts." Proceedings of the International Astronomical Union 13, S338 (October 2017): 1–8. http://dx.doi.org/10.1017/s1743921318000169.

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AbstractCompact object mergers are promising candidates for the progenitor system of short gamma-ray bursts (GRBs). Using gravitational wave (GW) triggers to identify a merger, any electromagnetic (EM) counterparts from the jet can be used to constrain the dynamics and structure of short GRB jets. GW triggered searches could reveal a hidden population of optical transients associated with the short-lived jets from the merger object. If the population of merger-jets is dominated by low-Lorentz-factors, then a GW triggered search will reveal the on-axis orphan afterglows from these failed GRBs. By considering the EM counterparts from a jet, with or without the prompt GRB, the jet structure and dynamics can be constrained. By modelling the afterglow of various jet structures with viewing angle, we provide observable predictions for the on- and off- axis EM jet counterparts. The predictions provide an indication for the various features expected from the proposed jet structure models.

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van Baal, Bart F. A., Frank R. N. Chambers, and Anna L. Watts. "Waves in thin oceans on oblate neutron stars." Monthly Notices of the Royal Astronomical Society 496, no. 2 (June 15, 2020): 2098–106. http://dx.doi.org/10.1093/mnras/staa1699.

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ABSTRACT Waves in thin fluid layers are important in various stellar and planetary problems. Due to rapid rotation such systems will become oblate, with a latitudinal variation in the gravitational acceleration across the surface of the object. In the case of accreting neutron stars, rapid rotation could lead to a polar radius smaller than the equatorial radius by a factor ∼0.8. We investigate how the oblateness and a changing gravitational acceleration affect different hydrodynamic modes that exist in such fluid layers through analytic approximations and numerical calculations. The wave vectors of g modes and Yanai modes increase for more oblate systems compared to spherical counterparts, although the impact of variations in the changing gravitational acceleration is effectively negligible. We find that for increased oblateness, Kelvin modes show less equatorial confinement and little change in their wave vector. For r modes, we find that for more oblate systems the wave vector decreases. The exact manner of these changes for the r modes depends on the model for the gravitational acceleration across the surface.

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Wang, Jieshuang, and Liangduan Liu. "Electromagnetic Precursors of Short Gamma-Ray Bursts as Counterparts of Gravitational Waves." Galaxies 9, no. 4 (November 15, 2021): 104. http://dx.doi.org/10.3390/galaxies9040104.

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Precursor emissions are found in some short gamma-ray bursts (SGRBs). In this paper, we review the theories and observations of the SGRB precursor and discuss its prospect as an electromagnetic counterpart of the gravitational wave event produced by neutron star (NS) mergers. The observed luminosity, spectrum, and duration of precursors are explained by the magnetospheric interaction model during the inspiral or the cocoon/jet shock breakout model during the jet propagation. In general, these two models predict that the precursor will be weaker than the main GRB, but will be of a larger opening angle, which makes it an advantageous gamma-ray counterpart for NS mergers in the local Universe, especially for NS - black hole mergers with very low mass ratios, in which the main GRBs are not expected. The joint observation of the precursor, SGRB, and gravitational wave will help to reveal the jet launch mechanism and post-merger remnant.

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Adriani, O., Y. Akaike, K. Asano, Y. Asaoka, M. G. Bagliesi, E. Berti, G. Bigongiari, et al. "Search for GeV Gamma-Ray Counterparts of Gravitational Wave Events by CALET." Astrophysical Journal 863, no. 2 (August 20, 2018): 160. http://dx.doi.org/10.3847/1538-4357/aad18f.

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Perna, Rosalba, Davide Lazzati, and Will Farr. "Limits on Electromagnetic Counterparts of Gravitational-wave-detected Binary Black Hole Mergers." Astrophysical Journal 875, no. 1 (April 16, 2019): 49. http://dx.doi.org/10.3847/1538-4357/ab107b.

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Stachie, Cosmin, Michael W. Coughlin, Nelson Christensen, and Daniel Muthukrishna. "Using machine learning for transient classification in searches for gravitational-wave counterparts." Monthly Notices of the Royal Astronomical Society 497, no. 2 (June 23, 2020): 1320–31. http://dx.doi.org/10.1093/mnras/staa1776.

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ABSTRACT The large sky localization regions offered by the gravitational-wave interferometers require efficient follow-up of the many counterpart candidates identified by the wide field-of-view telescopes. Given the restricted telescope time, the creation of prioritized lists of the many identified candidates becomes mandatory. Towards this end, we use astrorapid, a multiband photometric light-curve classifier, to differentiate between kilonovae, supernovae, and other possible transients. We demonstrate our method on the photometric observations of real events. In addition, the classification performance is tested on simulated light curves, both ideally and realistically sampled. We show that after only a few days of observations of an astronomical object, it is possible to rule out candidates as supernovae and other known transients.

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Nuttall, L. K., W. Zheng, and C. Akerlof. "The Analysis of ROTSE Images of Potential Counterparts to Gravitational Wave Events." Journal of Physics: Conference Series 363 (June 1, 2012): 012033. http://dx.doi.org/10.1088/1742-6596/363/1/012033.

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Ghosh, Shaon, Deep Chatterjee, David L. Kaplan, Patrick R. Brady, and Angela Van Sistine. "Hunting Electromagnetic Counterparts of Gravitational-wave Events Using the Zwicky Transient Facility." Publications of the Astronomical Society of the Pacific 129, no. 981 (September 18, 2017): 114503. http://dx.doi.org/10.1088/1538-3873/aa884f.

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Mastrogiovanni, S., R. Duque, E. Chassande-Mottin, F. Daigne, and R. Mochkovitch. "The potential role of binary neutron star merger afterglows in multimessenger cosmology." Astronomy & Astrophysics 652 (July 30, 2021): A1. http://dx.doi.org/10.1051/0004-6361/202040229.

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Binary neutron star mergers offer a new and independent means of measuring the Hubble constant H0 by combining the gravitational-wave inferred source luminosity distance with its redshift obtained from electromagnetic follow-up. This method is limited by the intrinsic degeneracy between the system distance and orbital inclination in the gravitational-wave signal. Observing the afterglow counterpart to a merger can further constrain the inclination angle, allowing this degeneracy to be partially lifted and improving the measurement of H0. In the case of the binary neutron star merger GW170817, afterglow light-curve and imaging modeling thus allowed the H0 measurement to be improved by a factor of three. However, systematic access to afterglow data is far from guaranteed. In fact, though each one allows a leap in H0 precision, these afterglow counterparts should prove rare in forthcoming multimessenger campaigns. We combine models for emission and detection of gravitational-wave and electromagnetic radiation from binary neutron star mergers with realistic population models and estimates for afterglow inclination angle constraints. Using these models, we quantify how fast H0 will be narrowed down by successive multimessenger events with and without the afterglow. We find that because of its rareness and though it greatly refines angle estimates, the afterglow counterpart should not significantly contribute to the measurement of H0 in the long run.

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Friedman, John L. "Gravitational-wave astrophysics from neutron star inspiral and coalescence." International Journal of Modern Physics D 27, no. 11 (August 2018): 1843018. http://dx.doi.org/10.1142/s0218271818430186.

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Prior to the observation of a double neutron star inspiral and merger, its possible implications were striking. Events whose light and gravitational waves are simultaneously detected could resolve the 50-year mystery of the origin of short gamma-ray bursts; they might provide strong evidence for (or against) mergers as the main source of half the heaviest elements (the [Formula: see text]-process elements); and they could give an independent measurement of the Hubble constant. The closest events can also address a primary goal of gravitational-wave astrophysics: From the imprint of tides on inspiral waveforms, one can find the radius and tidal distortion of the inspiraling stars and infer the behavior of cold matter above nuclear density. Remarkably, the first observation of the inspiral and coalescence of a double neutron star system was accompanied by a gamma-ray burst and then an array of electromagnetic counterparts, and the combined effort of the gravitational-wave and astronomy communities has led to dramatic advances along all of these anticipated avenues of multimessenger astrophysics.

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Herner, Kenneth, James Annis, Alyssa Garcia, Marcelle Soares-Santos, Dillon Brout, Noemi Glaeser, Nora Sherman, et al. "The updated DESGW processing pipeline for the third LIGO/VIRGO observing run." EPJ Web of Conferences 245 (2020): 01008. http://dx.doi.org/10.1051/epjconf/202024501008.

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The DESGW group seeks to identify electromagnetic counterparts of gravitational wave events seen by the LIGO-VIRGO network, such as those expected from binary neutron star mergers or neutron star-black hole mergers. DESGW was active throughout the first two LIGO observing seasons, following up several binary black hole mergers and the first binary neutron star merger, GW170817. This work describes the modifications to the observing strategy generation and image processing pipeline between the second (ending in August 2017) and third (beginning in April 2019) LIGO observing seasons. The modifications include a more robust observing strategy generator, further parallelization of the image reduction software and difference imaging processing pipeline, data transfer streamlining, and a web page listing identified counterpart candidates that updates in real time. Taken together, the additional parallelization steps enable the identification of potential electromagnetic counterparts within fully calibrated search images in less than one hour, compared to the 3-5 hours it would typically take during the first two seasons. These performance improvements are critical to the entire EM follow-up community, as rapid identification (or rejection) of candidates enables detailed and rapid spectroscopic follow-up by multiple instruments, leading to more information about the environment immediately following such gravitational wave events.

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de Jaeger, T., B. J. Shappee, C. S. Kochanek, K. Z. Stanek, J. F. Beacom, T. W.-S. Holoien, Todd A. Thompson, A. Franckowiak, and S. Holmbo. "ASAS-SN search for optical counterparts of gravitational-wave events from the third observing run of Advanced LIGO/Virgo." Monthly Notices of the Royal Astronomical Society 509, no. 3 (November 1, 2021): 3427–40. http://dx.doi.org/10.1093/mnras/stab3141.

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ABSTRACT We report on the search for electromagnetic counterparts to the nine gravitational-wave events with a >60 per cent probability of containing a neutron star during the third observing run (O3) of the Laser Interferometer Gravitational-Wave Observatory (LIGO)–Virgo Collaboration (LVC) with the All-Sky Automated Survey for SuperNovae (ASAS-SN). No optical counterparts associated with a gravitational-wave event were found. However, thanks to its network of telescopes, the average area visible to at least one ASAS-SN site during the first 10 h after the trigger contained ∼30 per cent of the integrated source location probability. Through a combination of normal operations and target-of-opportunity observations, ASAS-SN observations of the highest probability fields began within 1 h of the trigger for four of the events. After 24 h, ASAS-SN observed >60 per cent of total probability for three events and >40 per cent for all but one of the events. This is the largest area coverage to a depth of g = 18.5 mag from any survey with published coverage statistics for seven of the nine events. With its observing strategy, five sites around the world, and a large field of view, ASAS-SN will be one of the leading surveys to optically search for nearby neutron star mergers during LVC fourth observation run (O4).

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Bartos, I., K. R. Corley, N. Gupte, N. Ash, Z. Márka, and S. Márka. "Gravitational-wave follow-up with CTA after the detection of GRBs in the TeV energy domain." Monthly Notices of the Royal Astronomical Society 490, no. 3 (October 10, 2019): 3476–82. http://dx.doi.org/10.1093/mnras/stz2848.

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ABSTRACT The recent discovery of TeV emission from gamma-ray bursts (GRBs) by the MAGIC and H.E.S.S. Cherenkov telescopes confirmed that emission from these transients can extend to very high energies. The TeV energy domain reaches the most sensitive band of the Cherenkov Telescope Array (CTA). This newly anticipated, improved sensitivity will enhance the prospects of gravitational-wave follow-up observations by CTA to probe particle acceleration and high-energy emission from binary black hole and neutron star mergers, and stellar core-collapse events. Here we discuss the implications of TeV emission on the most promising strategies of choice for the gravitational-wave follow-up effort for CTA and Cherenkov telescopes more broadly. We find that TeV emission (i) may allow more than an hour of delay between the gravitational-wave event and the start of CTA observations; (ii) enables the use of CTA’s small size telescopes that have the largest field of view. We characterize the number of pointings needed to find a counterpart. (iii) We compute the annual follow-up time requirements and find that prioritization will be needed. (iv) Even a few telescopes could detect sufficiently nearby counterparts, raising the possibility of adding a handful of small-sized or medium-sized telescopes to the network at diverse geographic locations. (v) The continued operation of VERITAS/H.E.S.S./MAGIC would be a useful compliment to CTA’s follow-up capabilities by increasing the sky area that can be rapidly covered, especially in the United States and Australia, in which the present network of gravitational-wave detectors is more sensitive.

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Becerra, R. L., S. Dichiara, A. M. Watson, E. Troja, N. R. Butler, M. Pereyra, E. Moreno Méndez, et al. "DDOTI observations of gravitational-wave sources discovered in O3." Monthly Notices of the Royal Astronomical Society 507, no. 1 (July 21, 2021): 1401–20. http://dx.doi.org/10.1093/mnras/stab2086.

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ABSTRACT We present optical follow-up observations with the Deca-Degree Optical Transient Imager (DDOTI) telescope of gravitational-wave (GW) events detected during the Advanced LIGO and Advanced Virgo O3 observing run. DDOTI is capable of responding to an alert in a few minutes, has an instantaneous field of about 69 deg2, and obtains 10σ upper limits of wlim = 18.5–20.5 AB mag in 1000 s of exposure, depending on the conditions. We observed 54 per cent (26 out of 48) of the unretracted GW alerts and did not find any electromagnetic counterparts. We compare our upper limits to various possible counterparts: the kilonova AT 2017gfo, models of radioactive- and magnetar-powered kilonovae, short gamma-ray burst afterglows, and active galactic nucleus (AGN) flares. Although the large positional uncertainties of GW sources do not allow us to place strong constraints during O3, DDOTI observations of well-localized GW events in O4 and beyond could meaningfully constrain models of compact binary mergers. We show that DDOTI is able to detect kilonovae similar to AT 2017gfo up to about 200 Mpc and magnetar-powered kilonovae up to 1 Gpc. We calculate that nearby (≲200 Mpc) afterglows have a high chance (≈70 per cent) to be detected by rapid (≲3 h) DDOTI observations if observed on-axis, whereas off-axis afterglows are unlikely to be seen. Finally, we suggest that long-term monitoring of massive BBH events with DDOTI could confirm or rule out late AGN flares associated with these events.

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Gourdji, K., A. Rowlinson, R. A. M. J. Wijers, J. W. Broderick, A. Shulevski, and P. G. Jonker. "Searching for low radio-frequency gravitational wave counterparts in wide-field LOFAR data." Monthly Notices of the Royal Astronomical Society 509, no. 4 (November 9, 2021): 5018–29. http://dx.doi.org/10.1093/mnras/stab3197.

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ABSTRACT The electromagnetic counterparts to gravitational wave (GW) merger events are highly sought after, but difficult to find owing to large localization regions. In this study, we present a strategy to search for compact object merger radio counterparts in wide-field data collected by the Low-Frequency Array (LOFAR). In particular, we use multi-epoch LOFAR observations centred at 144 MHz spanning roughly 300 deg2 at optimum sensitivity of a since retracted neutron star–black hole merger candidate detected during O2, the second Advanced Ligo–Virgo GW observing run. The minimum sensitivity of the entire (overlapping) 1809 deg2 field searched is 50 mJy and the false negative rate is 0.1 per cent above 200 mJy. We do not find any transients and thus place an upper limit at 95 per cent confidence of 0.02 transients per square degree above 20 mJy on one, two, and three month time-scales, which are the most sensitive limits available to date. Finally, we discuss the prospects of observing GW events with LOFAR in the upcoming GW observing run and show that a single multibeam LOFAR observation can probe the full projected median localization area of binary neutron star mergers down to a median sensitivity of at least 8 mJy.

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Nissanke, Samaya, Mansi Kasliwal, and Alexandra Georgieva. "IDENTIFYING ELUSIVE ELECTROMAGNETIC COUNTERPARTS TO GRAVITATIONAL WAVE MERGERS: AN END-TO-END SIMULATION." Astrophysical Journal 767, no. 2 (April 4, 2013): 124. http://dx.doi.org/10.1088/0004-637x/767/2/124.

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Duque, Raphaël, Paz Beniamini, Frédéric Daigne, and Robert Mochkovitch. "Probing binary neutron star mergers in dense environments using afterglow counterparts." Astronomy & Astrophysics 639 (July 2020): A15. http://dx.doi.org/10.1051/0004-6361/201937115.

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The only binary neutron star merger gravitational wave event with detected electromagnetic counterparts recorded to date is GRB170817A. This merger occurred in a rarefied medium with a density smaller than 10−3 − 10−2 cm−3. Since kicks are imparted to neutron star binaries upon formation, and due to their long delay times before merger, such low-density circum-merger media are generally expected. However, there is some indirect evidence for fast-merging or low-kick binaries, which would coalesce in denser environments. Nonetheless, present astronomical data are largely inconclusive on the possibility of these high-density mergers. We describe a method to directly probe this hypothetical population of high-density mergers through multi-messenger observations of binary neutron star merger afterglows, exploiting the high sensitivity of these signals to the density of the merger environment. This method is based on a sample of merger afterglows that has yet to be collected. Its constraining power is large, even with a small sample of events. We discuss the method’s limitations and applicability. In the upcoming era of third-generation gravitational wave detectors, this method’s potential will be fully realized as it will allow us to probe mergers that occurred soon after the peak of cosmic star formation, provided the follow-up campaigns are able to locate the sources.

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Abedi, Jahed, Niayesh Afshordi, Naritaka Oshita, and Qingwen Wang. "Quantum Black Holes in the Sky." Universe 6, no. 3 (March 10, 2020): 43. http://dx.doi.org/10.3390/universe6030043.

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Black Holes are possibly the most enigmatic objects in our universe. From their detection in gravitational waves upon their mergers, to their snapshot eating at the centres of galaxies, black hole astrophysics has undergone an observational renaissance in the past four years. Nevertheless, they remain active playgrounds for strong gravity and quantum effects, where novel aspects of the elusive theory of quantum gravity may be hard at work. In this review article, we provide an overview of the strong motivations for why “Quantum Black Holes” may be radically different from their classical counterparts in Einstein’s General Relativity. We then discuss the observational signatures of quantum black holes, focusing on gravitational wave echoes as smoking guns for quantum horizons (or exotic compact objects), which have led to significant recent excitement and activity. We review the theoretical underpinning of gravitational wave echoes and critically examine the seemingly contradictory observational claims regarding their (non-)existence. Finally, we discuss the future theoretical and observational landscape for unraveling the “Quantum Black Holes in the Sky”.

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Coughlin, Michael W., Tim Dietrich, Sarah Antier, Mouza Almualla, Shreya Anand, Mattia Bulla, Francois Foucart, et al. "Implications of the search for optical counterparts during the second part of the Advanced LIGO’s and Advanced Virgo’s third observing run: lessons learned for future follow-up observations." Monthly Notices of the Royal Astronomical Society 497, no. 1 (July 6, 2020): 1181–96. http://dx.doi.org/10.1093/mnras/staa1925.

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ABSTRACT Joint multimessenger observations with gravitational waves and electromagnetic (EM) data offer new insights into the astrophysical studies of compact objects. The third Advanced LIGO and Advanced Virgo observing run began on 2019 April 1; during the 11 months of observation, there have been 14 compact binary systems candidates for which at least one component is potentially a neutron star. Although intensive follow-up campaigns involving tens of ground and space-based observatories searched for counterparts, no EM counterpart has been detected. Following on a previous study of the first six months of the campaign, we present in this paper the next five months of the campaign from 2019 October to 2020 March. We highlight two neutron star–black hole candidates (S191205ah and S200105ae), two binary neutron star candidates (S191213g and S200213t), and a binary merger with a possible neutron star and a ‘MassGap’ component, S200115j. Assuming that the gravitational-wave (GW) candidates are of astrophysical origin and their location was covered by optical telescopes, we derive possible constraints on the matter ejected during the events based on the non-detection of counterparts. We find that the follow-up observations during the second half of the third observing run did not meet the necessary sensitivity to constrain the source properties of the potential GW candidate. Consequently, we suggest that different strategies have to be used to allow a better usage of the available telescope time. We examine different choices for follow-up surveys to optimize sky localization coverage versus observational depth to understand the likelihood of counterpart detection.

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Coughlin, Michael W., Tim Dietrich, Sarah Antier, Mattia Bulla, Francois Foucart, Kenta Hotokezaka, Geert Raaijmakers, Tanja Hinderer, and Samaya Nissanke. "Implications of the search for optical counterparts during the first six months of the Advanced LIGO’s and Advanced Virgo’s third observing run: possible limits on the ejecta mass and binary properties." Monthly Notices of the Royal Astronomical Society 492, no. 1 (December 10, 2019): 863–76. http://dx.doi.org/10.1093/mnras/stz3457.

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ABSTRACT GW170817 showed that neutron star mergers not only emit gravitational waves but also can release electromagnetic signatures in multiple wavelengths. Within the first half of the third observing run of the Advanced LIGO and Virgo detectors, there have been a number of gravitational wave candidates of compact binary systems for which at least one component is potentially a neutron star. In this article, we look at the candidates S190425z, S190426c, S190510g, S190901ap, and S190910h, predicted to have potentially a non-zero remnant mass, in more detail. All these triggers have been followed up with extensive campaigns by the astronomical community doing electromagnetic searches for their optical counterparts; however, according to the released classification, there is a high probability that some of these events might not be of extraterrestrial origin. Assuming that the triggers are caused by a compact binary coalescence and that the individual source locations have been covered during the EM follow-up campaigns, we employ three different kilonova models and apply them to derive possible constraints on the matter ejection consistent with the publicly available gravitational-wave trigger information and the lack of a kilonova detection. These upper bounds on the ejecta mass can be related to limits on the maximum mass of the binary neutron star candidate S190425z and to constraints on the mass-ratio, spin, and NS compactness for the potential black hole–neutron star candidate S190426c. Our results show that deeper electromagnetic observations for future gravitational wave events near the horizon limit of the advanced detectors are essential.

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Almualla, Mouza, Michael W. Coughlin, Shreya Anand, Khalid Alqassimi, Nidhal Guessoum, and Leo P. Singer. "Dynamic scheduling: target of opportunity observations of gravitational wave events." Monthly Notices of the Royal Astronomical Society 495, no. 4 (June 1, 2020): 4366–71. http://dx.doi.org/10.1093/mnras/staa1498.

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ABSTRACT The simultaneous detection of electromagnetic and gravitational waves from the coalescence of two neutron stars (GW170817 and GRB170817A) has ushered in a new era of ‘multimessenger’ astronomy, with electromagnetic detections spanning from gamma to radio. This great opportunity for new scientific investigations raises the issue of how the available multimessenger tools can best be integrated to constitute a powerful method to study the transient Universe in particular. To facilitate the classification of possible optical counterparts to gravitational wave events, it is important to optimize the scheduling of observations and the filtering of transients, both key elements of the follow-up process. In this work, we describe the existing workflow whereby telescope networks such as GRANDMA and GROWTH are currently scheduled; we then present modifications we have developed for the scheduling process specifically, so as to face the relevant challenges that have appeared during the latest observing run of Advanced LIGO and Advanced Virgo. We address issues with scheduling more than one epoch for multiple fields within a skymap, especially for large and disjointed localizations. This is done in two ways: by optimizing the maximum number of fields that can be scheduled and by splitting up the lobes within the skymap by right ascension to be scheduled individually. In addition, we implement the ability to take previously observed fields into consideration when rescheduling. We show the improvements that these modifications produce in making the search for optical counterparts more efficient, and we point to areas needing further improvement.

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Butler, Robert E., M. Soares-Santos, J. Annis, and K. Herner. "DESGW Optical Follow-up of BBH LIGO-Virgo Events with DECam." Proceedings of the International Astronomical Union 13, S338 (October 2017): 61–64. http://dx.doi.org/10.1017/s1743921318003599.

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AbstractThe DESGW program is a collaboration between members of the Dark Energy Survey, the wider astronomical community, and the LIGO-Virgo Collaboration to search for optical counterparts of gravitational wave events, such as those expected from binary neutron star mergers or neutron star-black hole mergers. While binary black hole (BBH) events are not expected to produce an electromagnetic (EM) signature, emission is certainly not impossible. The DESGW program has performed follow-up observations of four BBH events detected by LIGO in order to search for any possible EM counterpart. Failure to find such counterparts is still relevant in that it produces limits on optical emission from such events. This is a review of follow-up results from O1 BBH events and a discussion of the status of ongoing uniform re-analysis of all BBH events that DESGW has followed up to date.

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Lamb, Gavin P., and Shiho Kobayashi. "LOW-Γ JETS FROM COMPACT STELLAR MERGERS: CANDIDATE ELECTROMAGNETIC COUNTERPARTS TO GRAVITATIONAL WAVE SOURCES." Astrophysical Journal 829, no. 2 (September 28, 2016): 112. http://dx.doi.org/10.3847/0004-637x/829/2/112.

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Nederlander, Richard, and Frits Paerels. "Detecting and Locating Electromagnetic Counterparts to Gravitational Wave Sources Using Galactic Dust Scattering Halos." Astrophysical Journal 890, no. 2 (February 21, 2020): 135. http://dx.doi.org/10.3847/1538-4357/ab6dc5.

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Yu, Hao, Bao-Min Gu, Fa Peng Huang, Yong-Qiang Wang, Xin-He Meng, and Yu-Xiao Liu. "Probing extra dimension through gravitational wave observations of compact binaries and their electromagnetic counterparts." Journal of Cosmology and Astroparticle Physics 2017, no. 02 (February 21, 2017): 039. http://dx.doi.org/10.1088/1475-7516/2017/02/039.

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Journal articles on the topic 'Gravitational Wave Counterparts'

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