Multi-messenger Observations of a Binary Neutron Star Merger

B.P. Abbott; R. Abbott; T. D. Abbott; F. Acernese; K. Ackley; C. Adams; T Adams; P. Addesso; R.X. Adhikari; V.B. Adya; C. Affeldt; M. Afrough; Bina Agarwal; M. Agathos; K. Agatsuma; Neha Aggarwal; O. D. Aguiar; Leslie Aiello; A. Ain; P. Ajith; Allen G. Collins; A. Allocca; Johan Peter Uldall Fynbo; Daniele Malesani; Morten Ankersen Medici; Michael James Larson; D. Jason Koskinen; Subir Sarkar; Markus Ahlers; Jorge Enrico Ramirez-Ruiz; Uffe Gråe Jørgensen; M.H. Gibby; T. Cline

doi:10.3847/2041-8213/aa91c9

Multi-messenger Observations of a Binary Neutron Star Merger

B.P. Abbott, R. Abbott, T. D. Abbott, F. Acernese, K. Ackley, C. Adams, T Adams, P. Addesso, R.X. Adhikari, V.B. Adya, C. Affeldt, M. Afrough, Bina Agarwal, M. Agathos, K. Agatsuma, Neha Aggarwal, O. D. Aguiar, Leslie Aiello, A. Ain, P. AjithAllen G. Collins, A. Allocca, Johan Peter Uldall Fynbo, Daniele Malesani, Morten Ankersen Medici, Michael James Larson, D. Jason Koskinen, Subir Sarkar, Markus Ahlers, Jorge Enrico Ramirez-Ruiz, Uffe Gråe Jørgensen, M.H. Gibby, T. Cline

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Abstract

On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg² at a luminosity distance of 40_- ⁺ ₈ ⁸ Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 M_☉. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ∼10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta.

Original language	English
Article number	L12
Journal	Astrophysics Journal Letters
Volume	848
Issue number	2
ISSN	2041-8205
DOIs	https://doi.org/10.3847/2041-8213/aa91c9
Publication status	Published - 1 Jan 2017

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Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Afrough, M., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., ... Cline, T. (2017). Multi-messenger Observations of a Binary Neutron Star Merger. Astrophysics Journal Letters, 848(2), [L12]. https://doi.org/10.3847/2041-8213/aa91c9

Abbott, BP, Abbott, R, Abbott, TD, Acernese, F, Ackley, K, Adams, C, Adams, T, Addesso, P, Adhikari, RX, Adya, VB, Affeldt, C, Afrough, M, Agarwal, B, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, OD, Aiello, L, Ain, A, Ajith, P, Collins, AG, Allocca, A, Fynbo, JPU , Malesani, D, Medici, MA, Larson, MJ, Koskinen, DJ, Sarkar, S, Ahlers, M, Ramirez-Ruiz, JE, Jørgensen, UG, Gibby, MH & Cline, T 2017, 'Multi-messenger Observations of a Binary Neutron Star Merger', Astrophysics Journal Letters, vol. 848, no. 2, L12. https://doi.org/10.3847/2041-8213/aa91c9

@article{fd9ee2fa2c244f69b9def0a93567a432,

title = "Multi-messenger Observations of a Binary Neutron Star Merger",

abstract = "On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of 40- + 8 8 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 M☉. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ∼10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta.",

author = "B.P. Abbott and R. Abbott and Abbott, {T. D.} and F. Acernese and K. Ackley and C. Adams and T Adams and P. Addesso and R.X. Adhikari and V.B. Adya and C. Affeldt and M. Afrough and Bina Agarwal and M. Agathos and K. Agatsuma and Neha Aggarwal and Aguiar, {O. D.} and Leslie Aiello and A. Ain and P. Ajith and Collins, {Allen G.} and A. Allocca and Fynbo, {Johan Peter Uldall} and Daniele Malesani and Medici, {Morten Ankersen} and Larson, {Michael James} and Koskinen, {D. Jason} and Subir Sarkar and Markus Ahlers and Ramirez-Ruiz, {Jorge Enrico} and J{\o}rgensen, {Uffe Gr{\aa}e} and M.H. Gibby and T. Cline",

year = "2017",

month = jan,

day = "1",

doi = "10.3847/2041-8213/aa91c9",

language = "English",

volume = "848",

journal = "The Astrophysical Journal Letters",

issn = "2041-8205",

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TY - JOUR

T1 - Multi-messenger Observations of a Binary Neutron Star Merger

AU - Abbott, B.P.

AU - Abbott, R.

AU - Abbott, T. D.

AU - Acernese, F.

AU - Ackley, K.

AU - Adams, C.

AU - Adams, T

AU - Addesso, P.

AU - Adhikari, R.X.

AU - Adya, V.B.

AU - Affeldt, C.

AU - Afrough, M.

AU - Agarwal, Bina

AU - Agathos, M.

AU - Agatsuma, K.

AU - Aggarwal, Neha

AU - Aguiar, O. D.

AU - Aiello, Leslie

AU - Ain, A.

AU - Ajith, P.

AU - Collins, Allen G.

AU - Allocca, A.

AU - Fynbo, Johan Peter Uldall

AU - Malesani, Daniele

AU - Medici, Morten Ankersen

AU - Larson, Michael James

AU - Koskinen, D. Jason

AU - Sarkar, Subir

AU - Ahlers, Markus

AU - Ramirez-Ruiz, Jorge Enrico

AU - Jørgensen, Uffe Gråe

AU - Gibby, M.H.

AU - Cline, T.

PY - 2017/1/1

Y1 - 2017/1/1

N2 - On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of 40- + 8 8 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 M☉. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ∼10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta.

AB - On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of 40- + 8 8 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 M☉. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ∼10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta.

U2 - 10.3847/2041-8213/aa91c9

DO - 10.3847/2041-8213/aa91c9

M3 - Journal article

SN - 2041-8205

VL - 848

JO - The Astrophysical Journal Letters

JF - The Astrophysical Journal Letters

IS - 2

M1 - L12

ER -

Multi-messenger Observations of a Binary Neutron Star Merger

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