Optical follow-up of the neutron star–black hole mergers S200105ae and S200115j

Anand, S.; Coughlin, M. W.; Kasliwal, M. M.; Bulla, Mattia; Ahumada, Tomás; Carracedo, Ana Sagués; Almualla, Mouza; Andreoni, Igor; Stein, R.; Foucart, François; Singer, L. P.; Sollerman, J.; Bellm, Eric C.; Bolin, Bryce; Caballero‐García, M. D.; Castro‐Tirado, Alberto J.; Cenko, S. Bradley; De, Kishalay; Dekany, Richard; Duev, Dmitry A.; Feeney, Michael; Fremling, C.; Goldstein, Daniel A.; Golkhou, V. Z.; Graham, M. J.; Guessoum, Nidhal; Hankins, Matthew J.; Hu, Y. D.; Kong, Albert; Kool, Erik C.; Kulkarni, S. R.; Kumar, Harsh; Laher, Russ R.; Masci, Frank J.; Mróz, P.; Nissanke, S.; Porter, Michael; Reusch, Simeon; Riddle, Reed; Rosnet, P.; Rusholme, B.; Serabyn, Eugene; Sánchez-Ramírez, R.; Rigault, M.; Shupe, D. L.; Smith, Roger; Soumagnac, Maayane T.; Walters, Richard; Valeev, A. F.

doi:10.1038/s41550-020-1183-3

Cited by 106 publications

(92 citation statements)

References 62 publications

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“…In 2013, the Palomar Transient Factory (PTF) 67 used a 7 deg 2 camera on the Palomar 48 inch Oschin telescope (P48) to discover the first optical afterglow of a GRB based solely on a Fermi GBM localization 68 and subsequently found afterglows of 7 other LGRBs 69 . Now, the Zwicky Transient Facility (ZTF 10, 71, 72 ), a 47 deg 2 camera mounted at the P48 telescope, has enabled searches an order of magnitude faster in areal and volumetric survey speed and has been used to search the coarse error regions of Fermi GBM SGRBs 73 and LIGO/Virgo events [74][75][76][77] .…”

Section: Methods 1 Discoverymentioning

confidence: 99%

Discovery and confirmation of the shortest gamma-ray burst from a collapsar

et al. 2021

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Gamma-ray bursts (GRBs) are among the brightest and most energetic events in the universe.The duration and hardness distribution of GRBs has two clusters 1 , now understood to reflect (at least) two different progenitors 2 . Short-hard GRBs (SGRBs; T 90 <2 s) arise from compact binary mergers, while long-soft GRBs (LGRBs; T 90 >2 s) have been attributed to the collapse of peculiar massive stars (collapsars) 3 . The discovery of SN 1998bw/GRB 980425 4 marked the first association of a LGRB with a collapsar and AT 2017gfo 5 /GRB 170817A/GW170817 6 marked the first association of a SGRB with a binary neutron star merger, producing also gravitational wave (GW). Here, we present the discovery of ZTF20abwysqy (AT2020scz), a fast-fading optical transient in the Fermi Satellite and the InterPlanetary Network (IPN) localization regions of GRB 200826A; X-ray and radio emission further confirm that this is the afterglow. Follow-up imaging (at rest-frame 16.5 days) reveals excess emission above the afterglow that cannot be explained as an underlying kilonova (KN), but is consistent with being the supernova (SN). Despite the GRB duration being short (rest-frame T 90 of 0.65 s), our panchromatic follow-up data confirms a collapsar origin. GRB 200826A is the shortestLGRB found with an associated collapsar; it appears to sit on the brink between a successful and a failed collapsar. Our discovery is consistent with the hypothesis that most collapsars fail to produce ultra-relativistic jets.

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Section: Methods 1 Discoverymentioning

confidence: 99%

Discovery and confirmation of the shortest gamma-ray burst from a collapsar

et al. 2021

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“…wavelength-dependent opacities as direct input. For the BHNS case, we use the grid presented in Anand et al (2021) and restrict to ejecta masses that are consistent with the distribution of ejecta masses computed in Section 2, i.e., M dyn = 0.01, 0.02, 0.03 M e and M wind = 0.01, 0.02, 0.03 M e . The distance is varied in the range 120−200 Mpc, corresponding to the 1σ range of the luminosity distance measure inferred in Abbott et al (2020a).…”

Section: Light-curve Modelingmentioning

confidence: 99%

“…Recent GW events potentially involving NSs-GW190425 (Abbott et al 2020a), GW190426 (Abbott et al 2021), and GW190814 (Abbott et al 2020c)-have all led to similar largescale searches for an EM counterpart (Coughlin et al 2019b;Goldstein et al 2019;Andreoni et al 2020;Antier et al 2020;Gompertz et al 2020;Page et al 2020). These searches have not resulted in any successful detections so far, though the absence of a counterpart can add weak additional constraints on the binary parameters of the system (Coughlin et al 2020a(Coughlin et al , 2020bAckley et al 2020;Anand et al 2021). The absence of a detection could be due to the low S/N of some of these events, e.g., GW190425 with a combined S/N of 12.9, producing much larger skymaps compared to GW170817.…”

Section: Introductionmentioning

confidence: 99%

The Challenges Ahead for Multimessenger Analyses of Gravitational Waves and Kilonova: A Case Study on GW190425

Raaijmakers

Nissanke

Foucart

et al. 2021

ApJ

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In recent years, there have been significant advances in multimessenger astronomy due to the discovery of the first, and so far only confirmed, gravitational wave event with a simultaneous electromagnetic (EM) counterpart, as well as improvements in numerical simulations, gravitational wave (GW) detectors, and transient astronomy. This has led to the exciting possibility of performing joint analyses of the GW and EM data, providing additional constraints on fundamental properties of the binary progenitor and merger remnant. Here, we present a new Bayesian framework that allows inference of these properties, while taking into account the systematic modeling uncertainties that arise when mapping from GW binary progenitor properties to photometric light curves. We extend the relative binning method presented in Zackay et al. to include extrinsic GW parameters for fast analysis of the GW signal. The focus of our EM framework is on light curves arising from r-process nucleosynthesis in the ejected material during and after merger, the so-called kilonova, and particularly on black hole−neutron star systems. As a case study, we examine the recent detection of GW190425, where the primary object is consistent with being either a black hole or a neutron star. We show quantitatively how improved mapping between binary progenitor and outflow properties, and/or an increase in EM data quantity and quality are required in order to break degeneracies in the fundamental source parameters.

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“…those from LSST WFD) and/or fast-evolving. One important application is the potential to inform optimal follow-up of LIGO gravitationalwave kilonova counterparts [17,2], constrain H 0 [1,28,19] or discriminate between binary neutron star and neutron star-neutron star LC models [15,27,3]. Given the high survey data volumes, limited expert time and follow-up resources, delegating autonomous systems to handle data acquisition would free up time to not only further improve the science return for the particular field being targeted, but also for other science cases outside the purview of machine intelligence.…”

Section: Discussionmentioning

confidence: 99%

Autonomous real-time science-driven follow-up of survey transients

Sravan¹,

Graham²,

Fremling³

et al. 2021

Preprint

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Astronomical surveys continue to provide unprecedented insights into the time-variable Universe and will remain the source of groundbreaking discoveries for years to come. However, their data throughput has overwhelmed the ability to manually synthesize alerts for devising and coordinating necessary follow-up with limited resources. The advent of Rubin Observatory, with alert volumes an order of magnitude higher at otherwise sparse cadence, presents an urgent need to overhaul existing human-centered protocols in favor of machine-directed infrastructure for conducting science inference and optimally planning expensive follow-up observations. We present the first implementation of autonomous real-time sciencedriven follow-up using value iteration to perform sequential experiment design. We demonstrate it for strategizing photometric augmentation of Zwicky Transient Facility Type Ia supernova light-curves given the goal of minimizing SALT2 parameter uncertainties. We find a median improvement of 2-6% for SALT2 parameters and 3-11% for photometric redshift with 2-7 additional data points in g, r and/or i compared to random augmentation. The augmentations are automatically strategized to complete gaps and for resolving phases with high constraining power (e.g. around peaks). We suggest that such a technique can deliver higher impact during the era of Rubin Observatory for precision cosmology at high redshift and can serve as the foundation for the development of general-purpose resource allocation systems.

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Optical follow-up of the neutron star–black hole mergers S200105ae and S200115j

Cited by 106 publications

References 62 publications

Discovery and confirmation of the shortest gamma-ray burst from a collapsar

Discovery and confirmation of the shortest gamma-ray burst from a collapsar

The Challenges Ahead for Multimessenger Analyses of Gravitational Waves and Kilonova: A Case Study on GW190425

Autonomous real-time science-driven follow-up of survey transients

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