Target-of-opportunity Observations of Gravitational-wave Events with Vera C. Rubin Observatory

Andreoni, Igor; Margutti, R.; Salafia, O. S.; Parazin, B.; Villar, V. Ashley; Coughlin, M. W.; Yoachim, Peter; Mortensen, Kris; Brethauer, Daniel; Smartt, S. J.; Kasliwal, Mansi M.; Alexander, K. D.; Anand, S.; Berger, E.; Bernardini, M. G.; Bianco, Federica; Blanchard, P. K.; Bloom, J.; Brocato, E.; Bulla, Mattia; Cartier, R.; Cenko, S. Bradley; Chornock, R.; Copperwheat, C. M.; Corsi, A.; D’Ammando, F.; D’Avanzo, P.; Datrier, L. E. H.; Foley, R. J.; Ghirlanda, G.; Goobar, A.; Grindlay, Jonathan E.; Hajela, A.; Holz, D. E.; Karambelkar, Viraj; Kool, Erik C.; Lamb, Gavin P.; Laskar, T.; Levan, A. J.; Maguire, K.; May, M.; Melandri, A.; Milisavljevic, Dan; Miller, A. A.; Nicholl, M.; Nissanke, S.; Palmese, A.; Piranomonte, S.; Rest, A.; Sagues-Carracedo, Ana; Siellez, K.; Singer, L. P.; Smith, M.; Steeghs, D.; Tanvir, N. R.

doi:10.3847/1538-4365/ac617c

Cited by 36 publications

(16 citation statements)

References 156 publications

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“…For a more realistic picture regarding the number of KN detections, we use a TOO strategy for Rubin which is similar to the approaches discussed in Ref. [103]. To claim a KN detection with Rubin, it has to be observed in the g + i filters on two consecutive nights.…”

Section: Kilonova Detectionmentioning

confidence: 99%

Neutron star-black hole mergers in next generation gravitational-wave observatories

Gupta¹,

Borhanian²,

Dhani³

et al. 2023

Preprint

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Observations by the current generation of gravitational-wave detectors have been pivotal in expanding our understanding of the universe. Although tens of exciting compact binary mergers have been observed, neutron star-black hole (NSBH) mergers remained elusive until they were first confidently detected in 2020. The number of NSBH detections is expected to increase with sensitivity improvements of the current detectors and the proposed construction of new observatories over the next decade. In this work, we explore the NSBH detection and measurement capabilities of these upgraded detectors and new observatories using the following metrics: network detection efficiency and detection rate as a function of redshift, distributions of the signal-to-noise ratios, the measurement accuracy of intrinsic and extrinsic parameters, the accuracy of sky position measurement, and the number of early-warning alerts that can be sent to facilitate the electromagnetic follow-up. Additionally, we evaluate the prospects of performing multi-messenger observations of NSBH systems by reporting the number of expected kilonova detections with the Vera C. Rubin Observatory and the Nancy Grace Roman Space Telescope. We find that as many as O(10) kilonovae can be detected by these two telescopes every year, depending on the population of the NSBH systems and the equation of state of neutron stars.

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Section: Kilonova Detectionmentioning

confidence: 99%

Neutron star-black hole mergers in next generation gravitational-wave observatories

Gupta¹,

Borhanian²,

Dhani³

et al. 2023

Preprint

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show abstract

“…Our model shows that while kilonovae from BHNS mergers at this distance are likely not detectable by the current generation of survey telescopes like the Zwicky Transient Facility (ZTF; Bellm et al 2019), the Asteroid Terrestrial Impact Last Alert System (ATLAS; Tonry et al 2018) or the Gravitational-wave Optical Transient Observer (GOTO; Dyer et al 2020;Steeghs et al 2022), these events are expected to be detectable by the Vera Rubin Observatory (Ivezić et al 2019;Andreoni et al 2022). Such a finding is in line with the non-detections of BHNS merger candidates during O3 (Hosseinzadeh et al 2019;Lundquist et al 2019;Ackley et al 2020;Andreoni et al 2020;Antier et al 2020;Gompertz et al 2020a;Anand et al 2021b;Oates et al 2021;Paterson et al 2021), though GW-triggered events are likely to be probed to greater depths than untriggered survey observations.…”

Section: Light Curves Of Electromagnetic Counterpartsmentioning

confidence: 86%

Mechanisms for high spin in black-hole neutron-star binaries and kilonova emission: inheritance and accretion

Steinle¹,

Gompertz²,

Nicholl³

2022

Preprint

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Black-hole neutron-star binary mergers, whose existence has been confirmed by gravitational-wave detectors, can lead to an electromagnetic counterpart called a kilonova if the neutron star is disrupted prior to merger. The observability of a kilonova depends crucially on the amount of neutron star ejecta, which is sensitive to the aligned component of the black hole spin. These binaries likely originate from the evolution of isolated stellar binaries. We explore the dependence of the ejected mass on two main mechanisms that provide high black hole spin. When the black hole inherits a high spin from a Wolf-Rayet star that was born with least ∼ 10% of its breakup spin under weak stellar core-envelope coupling, which is relevant for all formation pathways, the median of the ejected mass is 10 −2 M . Though only possible for certain formation pathways, similarly large ejected mass results when the BH accretes 20% of its companion's envelope to gain a high spin, and a more massive stellar progenitor provides smaller ejected mass compared to when the black hole inherits high spin. Together, these signatures suggest that a population analysis of black hole masses and spins in black-hole neutron-star binary mergers may help distinguish between mechanisms for spin and possible formation pathways. Using a novel kilonova light curve model we show that current capabilities are unlikely to observe a counterpart, however future facilities such as the Vera Rubin Observatory will likely detect counterparts even if the aligned dimensionless spin of the disrupting black hole is as low as ∼ 0.2. Our model predicts kilonovae as bright as M i ∼ −14.5 for an aligned black hole spin of ∼ 0.9.

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“…Lastly, combinations with ZTF [33] or Vera C. Rubin [34] surveys and Target of Opportunity programs may help pinpoint candidate host galaxies for observed binary mergers, and allow more detailed analyses using the electromagnetic information and the environment characterisation as inputs for the prediction and constraint of the neutrino emission. More generally, there are still only a few models on the processes leading to neutrino production during binary merger events in the literature [3-5, 25, 28], and further theoretical developments in the coming years may bring new light to past, present, and future observations.…”

Section: Discussionmentioning

confidence: 99%

Search for neutrino counterparts of gravitational-wave events detected by LIGO and Virgo during run O2 with the ANTARES telescope

et al. 2020

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An offline search for a neutrino counterpart to gravitational-wave (GW) events detected during the second observation run (O2) of Advanced-LIGO and Advanced-Virgo performed with ANTARES data is presented. In addition to the search for long tracks induced by ν μ (ν μ) charged current interactions, a search for showering events induced by interactions of neutrinos of any flavour is conducted. The severe spatial and time coincidence provided by the gravitational-wave alert allows regions above the detector horizon to be probed, extending the ANTARES sensitivity over the entire sky. The results of this all-neutrino-flavour and all-sky time dependent analysis are presented. The search for prompt neutrino emission within ±500 s around the time of six GW events yields no neutrino counterparts. Upper limits on the neutrino spectral fluence and constraints on the isotropic energy radiated via high-energy neutrinos (from a few TeV to a few tens of PeV) are set for each GW event analysed.

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Target-of-opportunity Observations of Gravitational-wave Events with Vera C. Rubin Observatory

Cited by 36 publications

References 156 publications

Neutron star-black hole mergers in next generation gravitational-wave observatories

Neutron star-black hole mergers in next generation gravitational-wave observatories

Mechanisms for high spin in black-hole neutron-star binaries and kilonova emission: inheritance and accretion

Search for neutrino counterparts of gravitational-wave events detected by LIGO and Virgo during run O2 with the ANTARES telescope

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