<i>Mary</i>, a Pipeline to Aid Discovery of Optical Transients

Andreoni, Igor; Jacobs, Colin; Hegarty, Sarah; Cooke, Jeff; Ryder, S. D.

doi:10.1017/pasa.2017.33

Cited by 65 publications

(72 citation statements)

References 38 publications

(56 reference statements)

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“…The first binary neutron star merger event, GW170817, was indeed accompanied by a macronova (Abbott et al 2017). The light curves and spectra of this macronova are largely consistent with r-process-powered macronova models (Andreoni et al 2017;Arcavi et al 2017;Coulter et al 2017;Cowperthwaite et al 2017;Drout et al 2017;Evans et al 2017;Kasliwal et al 2017;Pian et al 2017;Smartt et al 2017;Tanvir et al 2017;Utsumi et al 2017).…”

Section: Introductionsupporting

confidence: 63%

Radioactive Heating Rate of r-process Elements and Macronova Light Curve

Hotokezaka

Nakar

2020

ApJ

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We study the heating rate of r-process nuclei and thermalization of decay products in neutron star merger ejecta and macronova (kilonova) light curves. Thermalization of charged decay products, i.e., electrons, α-particles, and fission fragments is calculated according to their injection energy. The γ-ray thermalization processes are also properly calculated by taking the γ-ray spectrum of each decay into account. We show that the β-decay heating rate at later times approaches a powerlaw decline as ∝ t −2.8 , which agrees with the result of Waxman et al. (2019). We present a new analytic model to calculate macronova light curves, in which the density structure of the ejecta is accounted for. We demonstrate that the observed bolometric light curve and temperature evolution of the macronova associated with GW170817 are reproduced well by the β-decay heating rate with the solar r-process abundance pattern. We interpret the break in the observed bolometric light curve around a week as a result of the diffusion wave crossing a significant part of the ejecta rather than a thermalization break. We also show that the time-weighted integral of the bolometric light curve (Katz integral) is useful to provide an estimate of the total r-process mass from the observed data, which is independent of the highly uncertain radiative transfer. For the macronova in GW170817, the ejecta mass is robustly estimated as ≈ 0.05M for A min ≤ 72 and 85 ≤ A min ≤ 130 with the solar r-process abundance pattern. The code for computation of the heating rate and light curve for given initial nuclear abundances is publicly available.

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Section: Introductionsupporting

confidence: 63%

Radioactive Heating Rate of r-process Elements and Macronova Light Curve

Hotokezaka

Nakar

2020

ApJ

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“…The simultaneous detection of gravitational waves (GWs) from a neutron star-neutron star (NS-NS) merger (Abbott et al 2017a) and its electromagnetic (EM) counterparts opened a new window of the multimessenger astronomy. EM counterparts to GW170817 were observed over the entire wavelength range, from gamma-ray to radio wavelengths (Abbott et al 2017b;Andreoni et al 2017;Arcavi et al 2017;Coulter et al 2017;Cowperthwaite et al 2017;Díaz et al 2017;Drout et al 2017;Evans et al 2017;Hu et al 2017;Valenti et al 2017;Kasliwal et al 2017;Lipunov et al 2017;Pian et al 2017;Pozanenko et al 2018;Smartt et al 2017;Tanvir et al 2017;Troja et al 2017;Utsumi et al 2017;Mooley et al 2018;Hallinan et al 2017). In particular, a counterpart in optical and infrared wavelengths (named as SSS17a, AT 2017gfo or DLT17ck), is identified as the emission so-called a kilonova (also known as macronova).…”

Section: Introductionmentioning

confidence: 99%

Diversity of Kilonova Light Curves

Kawaguchi

Shibata

Tanaka

2020

ApJ

137

151

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We perform radiative transfer simulations for kilonova in various situations, including the cases of prompt collapse to a black hole from neutron-star mergers, high-velocity ejecta possibly accelerated by magnetars, and a black hole-neutron star merger. Our calculations are done employing ejecta profiles predicted by numerical-relativity simulations and a new line list for all the r-process elements. We found that (i) the optical emission for binary neutron stars promptly collapsing to a black hole would be fainter by 1-2 mag than that found in GW170817, while the infrared emission could be as bright as that in GW170817 if the post-merger ejecta is as massive as ≈ 0.01 M ; (ii) the kilonova would be brighter than that observed in GW170817 for the case that the ejecta is highly accelerated by the electromagnetic energy injection from the remnant, but it would decline rapidly and the magnitude would become fainter than in GW170817 within a few days; (iii) the optical emission from a black hole-neutron star merger ejecta could be as bright as that observed in GW170817 for the case that sufficiently large amount of matter is ejected ( 0.02 M ), while the infrared brightness would be brighter by 1-2 mag at the same time. We show that the difference in the ejecta properties would be imprinted in the differences in the peak brightness and time of peak. This indicates that we may be able to infer the type of the central engine for kilonovae by observation of the peak in the multiple band.

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“…The discovery, about 12 hours after the GBM trigger, of the associated optical transient AT2017gfo (Coulter et al 2017;Valenti et al 2017) triggered an intense ultraviolet, optical and infrared (UVOIR) follow up campaign (e.g. Andreoni et al 2017;Arcavi et al 2017;Chornock et al 2017;Covino et al 2017;Díaz et al 2017;Drout et al 2017;Evans et al 2017;Hal-1 Similar results were obtained by an independent analysis by Zhang et al (2018) linan et al 2017; Pian et al 2017;Pozanenko et al 2018;Smartt et al 2017;Utsumi et al 2017) -whose results have been collected and homogenized in Villar et al (2017) -which characterised with unprecedented details the emission and color evolution of the first ever spectroscopically confirmed (e.g. Pian et al 2017;Cowperthwaite et al 2017;Gall et al 2017;Kilpatrick et al 2017;McCully et al 2017;Nicholl et al 2017;Smartt et al 2017) kilonova (KN), i.e.…”

Section: Introductionmentioning

confidence: 99%

On-axis view of GRB 170817A

Salafia

Ghirlanda

Ascenzi

et al. 2019

A&A

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The peculiar short gamma-ray burst GRB 170817A has been firmly associated to the gravitational wave event GW170817, which has been unaninmously interpreted as due to the coalescence of a double neutron star binary. The unprecedented behaviour of the non-thermal afterglow led to a debate about its nature, which was eventually settled by high-resolution VLBI observations, which strongly support the off-axis structured jet scenario. Using information on the jet structure derived from multi-wavelength fitting of the afterglow emission and of the apparent VLBI image centroid motion, we compute the appearance of a GRB 170817A-like jet as seen by an on-axis observer and we compare it to the previously observed population of SGRB afterglows and prompt emission events. We find that the intrinsic properties of the GRB 170817A jet are representative of a typical event in the SGRB population, hinting at a quasi-universal jet structure. The diversity in the SGRB afterglow population could therefore be ascribed in large part to extrinsic (redshift, density of the surrounding medium, viewing angle) rather than intrinsic properties. Although more uncertain, the comparison can be extended to the prompt emission properties, leading to similar conclusions.

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Mary, a Pipeline to Aid Discovery of Optical Transients

Cited by 65 publications

References 38 publications

Radioactive Heating Rate of r-process Elements and Macronova Light Curve

Radioactive Heating Rate of r-process Elements and Macronova Light Curve

Diversity of Kilonova Light Curves

On-axis view of GRB 170817A

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