Two Years of Nonthermal Emission from the Binary Neutron Star Merger GW170817: Rapid Fading of the Jet Afterglow and First Constraints on the Kilonova Fastest Ejecta

Hajela, A.; Margutti, R.; Alexander, K. D.; Kathirgamaraju, Adithan; Baldeschi, A.; Guidorzi, C.; Giannios, Dimitrios; Fong, W.; Wu, Y.; MacFadyen, Andrew; Paggi, A.; Berger, E.; Blanchard, P. K.; Chornock, R.; Coppejans, D. L.; Cowperthwaite, P. S.; Eftekhari, T.; Gómez, Sebastián; Hosseinzadeh, G.; Laskar, T.; Metzger, Brian D.; Nicholl, M.; Paterson, K.; Radice, David; Sironi, Lorenzo; Terreran, G.; Villar, V. Ashley; Williams, Peter K. G.; Xie, Xiaoyi; Zrake, Jonathan

doi:10.3847/2041-8213/ab5226

Cited by 170 publications

(159 citation statements)

References 70 publications

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“…Within the associated uncertainties, these results are consistent with the broadband evolution of AT 2017gfo (e.g. Alexander et al 2018;Lamb et al 2019;Troja et al 2019;Hajela et al 2019).…”

supporting

confidence: 88%

“…The fitted radio spectral index α 1 from this study is −0.53 ± 0.04, consistent with broadband spectral indices determined using radio, optical and X-ray data at various epochs, where the typical value is approximately −0.58 (e.g. Margutti et al 2018;Troja et al 2018Troja et al , 2019Alexander et al 2018;Hajela et al 2019). Mooley et al (2018c) also found power-law dependencies for the rise and decay phases of approximately t 0.8 and t −2.4 , respectively, where t is the time since the merger.…”

supporting

confidence: 87%

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LOFAR 144-MHz follow-up observations of GW170817

Broderick

Shimwell

Gourdji

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present low-radio-frequency follow-up observations of AT 2017gfo, the electromagnetic counterpart of GW170817, which was the first binary neutron star merger to be detected by Advanced LIGO-Virgo. These data, with a central frequency of 144 MHz, were obtained with LOFAR, the Low-Frequency Array. The maximum elevation of the target is just 13. • 7 when observed with LOFAR, making our observations particularly challenging to calibrate and significantly limiting the achievable sensitivity. On timescales of 130-138 and 371-374 days after the merger event, we obtain 3σ upper limits for the afterglow component of 6.6 and 19.5 mJy beam −1 , respectively. Using our best upper limit and previously published, contemporaneous higher-frequency radio data, we place a limit on any potential steepening of the radio spectrum between 610 and 144 MHz: the two-point spectral index α 610 144 −2.5. We also show that LOFAR can detect the afterglows of future binary neutron star merger events occurring at more favourable elevations.

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supporting

confidence: 88%

supporting

confidence: 87%

LOFAR 144-MHz follow-up observations of GW170817

Broderick

Shimwell

Gourdji

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…We calculate the medians for the parameters, = (Figure 4). Motivated by the low value of ò B ≈10 −4 -10 −2 derived for GW170817ʼs afterglow (e.g., Wu & MacFadyen 2018;Hajela et al 2019), as well as those derived for Swift SGRBs (Santana et al 2014;Zhang et al 2015), we explore the possibility of a low value of ò B and find that the allowed parameter space is completely ruled out for ò B 10 −3 (for ò e =0.1). In summary, we derive E K,iso ≈0.13-0.14×10 52 erg and n≈0.04-1.10 cm −3 for GRB 181123B.…”

Section: Afterglow Propertiesmentioning

confidence: 96%

Discovery of the Optical Afterglow and Host Galaxy of Short GRB 181123B at z = 1.754: Implications for Delay Time Distributions

Paterson

Fong

Nugent

et al. 2020

ApJL

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We present the discovery of the optical afterglow and host galaxy of the Swift short-duration gamma-ray burst (SGRB) GRB 181123B. Observations with Gemini-North starting ≈9.1 hr after the burst reveal a faint optical afterglow with i≈25.1 mag at an angular offset of 0 59±0 16 from its host galaxy. Using grizYJHK observations, we measure a photometric redshift of the host galaxy of =-+ z 1.77 0.17 0.30. From a combination of Gemini and Keck spectroscopy of the host galaxy spanning 4500-18000 Å, we detect a single emission line at 13390 Å, inferred as Hβ at z=1.754±0.001 and corroborating the photometric redshift. The host galaxy properties of GRB 181123B are typical of those of other SGRB hosts, with an inferred stellar mass of ≈9.1×10 9 M e , a mass-weighted age of ≈0.9 Gyr, and an optical luminosity of ≈0.9L *. At z=1.754, GRB 181123B is the most distant secure SGRB with an optical afterglow detection and one of only three at z>1.5. Motivated by a growing number of high-z SGRBs, we explore the effects of a missing z>1.5 SGRB population among the current Swift sample on delay time distribution (DTD) models. We find that lognormal models with mean delay times of ≈4-6 Gyr are consistent with the observed distribution but can be ruled out to 95% confidence, with an additional ≈one to five Swift SGRBs recovered at z>1.5. In contrast, power-law models with ∝t −1 are consistent with the redshift distribution and can accommodate up to ≈30 SGRBs at these redshifts. Under this model, we predict that ≈1/3 of the current Swift population of SGRBs is at z>1. The future discovery or recovery of existing high-z SGRBs will provide significant discriminating power on their DTDs and thus their formation channels.

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“…An X-ray signal (Troja et al 2017;Margutti et al 2017;Haggard et al 2017;Ruan et al 2018;Pooley et al 2017) and a radio signal (Hallinan et al 2017;Alexander et al 2017;Mooley et al 2018) were discovered at the position of the optical transient after $ 9 days and $ 16 days, respectively. A slow multi-wavelength flux-rise of the non-thermal emission was observed until $ 150 days (Lyman et al 2018;Margutti et al 2018;Troja et al 2018) before entering a flattening-decaying phase (D'Avanzo et al 2018;Dobie et al 2018;Alexander et al 2018;Hajela et al 2019;Fong et al 2019). Very Long Baseline Interferometry observations enabled measurement of the superluminal proper motion of the radio counterpart (Mooley et al 2018) and constrained the apparent size of the source (Ghirlanda et al 2019), proving that a relativistic and narrowlycollimated jet successfully emerged from the neutron star merger.…”

Section: The O1 and O2 Follow-up Programmentioning

confidence: 99%

Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA

et al. 2020

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We present our current best estimate of the plausible observing scenarios for the Advanced LIGO, Advanced Virgo and KAGRA gravitational-wave detectors over the next several years, with the intention of providing information to facilitate planning for multi-messenger astronomy with gravitational waves. We estimate the sensitivity of the network to transient gravitational-wave signals for the third (O3), fourth (O4) and fifth observing (O5) runs, including the planned upgrades of the Advanced LIGO and Advanced Virgo detectors. We study the capability of the network to determine the sky location of the source for gravitational-wave signals from the inspiral of binary systems of compact objects, that is binary neutron star, neutron star–black hole, and binary black hole systems. The ability to localize the sources is given as a sky-area probability, luminosity distance, and comoving volume. The median sky localization area (90% credible region) is expected to be a few hundreds of square degrees for all types of binary systems during O3 with the Advanced LIGO and Virgo (HLV) network. The median sky localization area will improve to a few tens of square degrees during O4 with the Advanced LIGO, Virgo, and KAGRA (HLVK) network. During O3, the median localization volume (90% credible region) is expected to be on the order of $$10^{5}, 10^{6}, 10^{7}\mathrm {\ Mpc}^3$$ 10 5 , 10 6 , 10 7 Mpc 3 for binary neutron star, neutron star–black hole, and binary black hole systems, respectively. The localization volume in O4 is expected to be about a factor two smaller than in O3. We predict a detection count of $$1^{+12}_{-1}$$ 1 - 1 + 12 ($$10^{+52}_{-10}$$ 10 - 10 + 52 ) for binary neutron star mergers, of $$0^{+19}_{-0}$$ 0 - 0 + 19 ($$1^{+91}_{-1}$$ 1 - 1 + 91 ) for neutron star–black hole mergers, and $$17^{+22}_{-11}$$ 17 - 11 + 22 ($$79^{+89}_{-44}$$ 79 - 44 + 89 ) for binary black hole mergers in a one-calendar-year observing run of the HLV network during O3 (HLVK network during O4). We evaluate sensitivity and localization expectations for unmodeled signal searches, including the search for intermediate mass black hole binary mergers.

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Two Years of Nonthermal Emission from the Binary Neutron Star Merger GW170817: Rapid Fading of the Jet Afterglow and First Constraints on the Kilonova Fastest Ejecta

Cited by 170 publications

References 70 publications

LOFAR 144-MHz follow-up observations of GW170817

LOFAR 144-MHz follow-up observations of GW170817

Discovery of the Optical Afterglow and Host Galaxy of Short GRB 181123B at z = 1.754: Implications for Delay Time Distributions

Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA

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