Multi-messenger Observations of a Binary Neutron Star Merger

LIGO Scientific Collaboration; Virgo Collaboration; GBM Fermi; null INTEGRAL; IceCube Collaboration; AstroSat Cadmium Zinc Telluride Imager Team; IPN Collaboration; The Insight-Hxmt Collaboration; ANTARES Collaboration; The Swift Collaboration; AGILE Team; The 1M2H Team; The Dark Energy Camera GW-EM Collaboration; the DES Collaboration; The DLT40 Collaboration; null GRAWITA; GRAvitational Wave Inaf TeAm; The Fermi Large Area Telescope Collaboration; null ATCA; Australia Telescope Compact Array; null ASKAP; Australian SKA Pathfinder; Las Cumbres Observatory Group; null OzGrav; null DWF; null AST3; CAASTRO Collaborations; The VINROUGE Collaboration; MASTER Collaboration; null J-GEM; null GROWTH; null JAGWAR; NRAO Caltech-; null TTU-NRAO; NuSTAR Collaborations; null Pan-STARRS; The MAXI Team; TZAC Consortium; KU Collaboration; Nordic Optical Telescope; null ePESSTO; null GROND; Texas Tech University; SALT Group; null TOROS; Transient Robotic Observatory of the South Collaboration; The BOOTES Collaboration; null MWA; Murchison Widefield Array; The CALET Collaboration; IKI-GW Follow-up Collaboration; H. E. S. S. Collaboration; LOFAR Collaboration; null LWA; Long Wavelength Array; HAWC Collaboration; The Pierre Auger Collaboration; ALMA Collaboration; Euro VLBI Team; Pi of the Sky Collaboration; The Chandra Team at McGill University; null DFN; Desert Fireball Network; null ATLAS; High Time Resolution Universe Survey; null RIMAS; null RATIR; SKA South Africa/MeerKAT; Hendrik Van Eerten

doi:10.3847/2041-8213/aa91c9

Multi-messenger Observations of a Binary Neutron Star Merger

LIGO Scientific Collaboration, Virgo Collaboration, GBM Fermi, INTEGRAL, IceCube Collaboration, AstroSat Cadmium Zinc Telluride Imager Team, IPN Collaboration, The Insight-Hxmt Collaboration, ANTARES Collaboration, The Swift Collaboration, AGILE Team, The 1M2H Team, The Dark Energy Camera GW-EM Collaboration, the DES Collaboration, The DLT40 Collaboration, GRAWITA, GRAvitational Wave Inaf TeAm, The Fermi Large Area Telescope Collaboration, ATCA, Australia Telescope Compact ArrayASKAP, Australian SKA Pathfinder, Las Cumbres Observatory Group, OzGrav, DWF, AST3, CAASTRO Collaborations, The VINROUGE Collaboration, MASTER Collaboration, J-GEM, GROWTH, JAGWAR, NRAO Caltech-, TTU-NRAO, NuSTAR Collaborations, Pan-STARRS, The MAXI Team, TZAC Consortium, KU Collaboration, Nordic Optical Telescope, ePESSTO, GROND, Texas Tech University, SALT Group, TOROS, Transient Robotic Observatory of the South Collaboration, The BOOTES Collaboration, MWA, Murchison Widefield Array, The CALET Collaboration, IKI-GW Follow-up Collaboration, H. E. S. S. Collaboration, LOFAR Collaboration, LWA, Long Wavelength Array, HAWC Collaboration, The Pierre Auger Collaboration, ALMA Collaboration, Euro VLBI Team, Pi of the Sky Collaboration, The Chandra Team at McGill University, DFN, Desert Fireball Network, ATLAS, High Time Resolution Universe Survey, RIMAS, RATIR, SKA South Africa/MeerKAT, Hendrik Van Eerten

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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 $\sim$1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg$^2$ 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 Msun. 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 $\sim$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 $\sim$10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position $\sim$9 and $\sim$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. (Abridged)

Original language	English
Article number	L12
Number of pages	59
Journal	Astrophysical Journal Letters
Volume	848
Issue number	2
DOIs	https://doi.org/10.3847/2041-8213/aa91c9
Publication status	Published - 16 Oct 2017

Bibliographical note

This is a reproduction of the article published in the Astrophysical Journal Letters, under the terms of the Creative Commons Attribution 3.0 licence

Keywords

astro-ph.HE
gr-qc

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1710.05833v2Final published version, 3.12 MBLicence: CC BY

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Collaboration, LIGO. S., Collaboration, V., Fermi, GBM., INTEGRAL, Collaboration, I., Team, A. C. Z. T. I., Collaboration, IPN., Collaboration, T. I.-H., Collaboration, ANTARES., Collaboration, T. S., Team, AGILE., Team, T. MH., Collaboration, T. D. E. C. GW.-EM., Collaboration, T. DES., Collaboration, T. DLT., GRAWITA, TeAm, GRA. W. I., Collaboration, T. F. L. A. T., ATCA, ... Van Eerten, H. (2017). Multi-messenger Observations of a Binary Neutron Star Merger. Astrophysical Journal Letters, 848(2), Article L12. https://doi.org/10.3847/2041-8213/aa91c9

Collaboration, LIGOS, Collaboration, V, Fermi, GBM, INTEGRAL, Collaboration, I, Team, ACZTI, Collaboration, IPN, Collaboration, TI-H, Collaboration, ANTARES, Collaboration, TS, Team, AGILE, Team, TMH, Collaboration, TDECGW-EM, Collaboration, TDES, Collaboration, TDLT, GRAWITA, TeAm, GRAWI, Collaboration, TFLAT, ATCA, Array, ATC, ASKAP, Pathfinder, ASKA, Group, LCO, OzGrav, DWF, AST3, Collaborations, CAASTRO, Collaboration, TVINROUGE, Collaboration, MASTER, J-GEM, GROWTH, JAGWAR, Caltech-, NRAO, TTU-NRAO, Collaborations, NTAR, Pan-STARRS, Team, TMAXI, Consortium, TZAC, Collaboration, KU, Telescope, NO, ePESSTO, GROND, University, TT, Group, SALT, TOROS, Collaboration, TROOTS, Collaboration, TBOOTES, MWA, Array, MW, Collaboration, TCALET, Collaboration, IKI-GWF, Collaboration, HESS, Collaboration, LOFAR, LWA, Array, LW, Collaboration, HAWC, Collaboration, TPA, Collaboration, ALMA, Team, EVLBI, Collaboration, POTS, University, TCTAM, DFN, Network, DF, ATLAS, Survey, HTRU, RIMAS, RATIR, Africa/MeerKAT, SKAS & Van Eerten, H 2017, 'Multi-messenger Observations of a Binary Neutron Star Merger', Astrophysical Journal Letters, vol. 848, no. 2, L12. https://doi.org/10.3847/2041-8213/aa91c9

@article{9362b97740dd4f35b06b5cbdba2adcf4,

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 $\sim$1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg$^2$ 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 Msun. 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 $\sim$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 $\sim$10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position $\sim$9 and $\sim$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. (Abridged)",

keywords = "astro-ph.HE, gr-qc",

author = "Collaboration, {LIGO Scientific} and Virgo Collaboration and GBM Fermi and INTEGRAL and IceCube Collaboration and Team, {AstroSat Cadmium Zinc Telluride Imager} and IPN Collaboration and Collaboration, {The Insight-Hxmt} and ANTARES Collaboration and Collaboration, {The Swift} and AGILE Team and Team, {The 1M2H} and Collaboration, {The Dark Energy Camera GW-EM} and Collaboration, {the DES} and Collaboration, {The DLT40} and GRAWITA and TeAm, {GRAvitational Wave Inaf} and Collaboration, {The Fermi Large Area Telescope} and ATCA and Array, {Australia Telescope Compact} and ASKAP and Pathfinder, {Australian SKA} and Group, {Las Cumbres Observatory} and OzGrav and DWF and AST3 and CAASTRO Collaborations and Collaboration, {The VINROUGE} and MASTER Collaboration and J-GEM and GROWTH and JAGWAR and NRAO Caltech- and TTU-NRAO and NuSTAR Collaborations and Pan-STARRS and Team, {The MAXI} and TZAC Consortium and KU Collaboration and Telescope, {Nordic Optical} and ePESSTO and GROND and University, {Texas Tech} and SALT Group and TOROS and Collaboration, {Transient Robotic Observatory of the South} and Collaboration, {The BOOTES} and MWA and Array, {Murchison Widefield} and Collaboration, {The CALET} and Collaboration, {IKI-GW Follow-up} and Collaboration, {H. E. S. S.} and LOFAR Collaboration and LWA and Array, {Long Wavelength} and HAWC Collaboration and Collaboration, {The Pierre Auger} and ALMA Collaboration and Team, {Euro VLBI} and Collaboration, {Pi of the Sky} and University, {The Chandra Team at McGill} and DFN and Network, {Desert Fireball} and ATLAS and Survey, {High Time Resolution Universe} and RIMAS and RATIR and Africa/MeerKAT, {SKA South} and {Van Eerten}, Hendrik",

note = "This is a reproduction of the article published in the Astrophysical Journal Letters, under the terms of the Creative Commons Attribution 3.0 licence",

year = "2017",

month = oct,

day = "16",

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

language = "English",

volume = "848",

journal = "Astrophysical Journal Letters",

issn = "2041-8205",

publisher = "IOP Publishing",

number = "2",

}

TY - JOUR

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

AU - Collaboration, LIGO Scientific

AU - Collaboration, Virgo

AU - Fermi, GBM

AU - INTEGRAL, null

AU - Collaboration, IceCube

AU - Team, AstroSat Cadmium Zinc Telluride Imager

AU - Collaboration, IPN

AU - Collaboration, The Insight-Hxmt

AU - Collaboration, ANTARES

AU - Collaboration, The Swift

AU - Team, AGILE

AU - Team, The 1M2H

AU - Collaboration, The Dark Energy Camera GW-EM

AU - Collaboration, the DES

AU - Collaboration, The DLT40

AU - GRAWITA, null

AU - TeAm, GRAvitational Wave Inaf

AU - Collaboration, The Fermi Large Area Telescope

AU - ATCA, null

AU - Array, Australia Telescope Compact

AU - ASKAP, null

AU - Pathfinder, Australian SKA

AU - Group, Las Cumbres Observatory

AU - OzGrav, null

AU - DWF, null

AU - AST3, null

AU - Collaborations, CAASTRO

AU - Collaboration, The VINROUGE

AU - Collaboration, MASTER

AU - J-GEM, null

AU - GROWTH, null

AU - JAGWAR, null

AU - Caltech-, NRAO

AU - TTU-NRAO, null

AU - Collaborations, NuSTAR

AU - Pan-STARRS, null

AU - Team, The MAXI

AU - Consortium, TZAC

AU - Collaboration, KU

AU - Telescope, Nordic Optical

AU - ePESSTO, null

AU - GROND, null

AU - University, Texas Tech

AU - Group, SALT

AU - TOROS, null

AU - Collaboration, Transient Robotic Observatory of the South

AU - Collaboration, The BOOTES

AU - MWA, null

AU - Array, Murchison Widefield

AU - Collaboration, The CALET

AU - Collaboration, IKI-GW Follow-up

AU - Collaboration, H. E. S. S.

AU - Collaboration, LOFAR

AU - LWA, null

AU - Array, Long Wavelength

AU - Collaboration, HAWC

AU - Collaboration, The Pierre Auger

AU - Collaboration, ALMA

AU - Team, Euro VLBI

AU - Collaboration, Pi of the Sky

AU - University, The Chandra Team at McGill

AU - DFN, null

AU - Network, Desert Fireball

AU - ATLAS, null

AU - Survey, High Time Resolution Universe

AU - RIMAS, null

AU - RATIR, null

AU - Africa/MeerKAT, SKA South

AU - Van Eerten, Hendrik

N1 - This is a reproduction of the article published in the Astrophysical Journal Letters, under the terms of the Creative Commons Attribution 3.0 licence

PY - 2017/10/16

Y1 - 2017/10/16

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 $\sim$1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg$^2$ 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 Msun. 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 $\sim$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 $\sim$10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position $\sim$9 and $\sim$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. (Abridged)

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 $\sim$1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg$^2$ 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 Msun. 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 $\sim$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 $\sim$10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position $\sim$9 and $\sim$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. (Abridged)

KW - astro-ph.HE

KW - gr-qc

U2 - 10.3847/2041-8213/aa91c9

DO - 10.3847/2041-8213/aa91c9

M3 - Article

SN - 2041-8205

VL - 848

JO - Astrophysical Journal Letters

JF - Astrophysical Journal Letters

IS - 2

M1 - L12

ER -

Multi-messenger Observations of a Binary Neutron Star Merger

Abstract

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