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2 results on '"Collaboration, Pi of the Sky"'

1. Multi-messenger Observations of a Binary Neutron Star Merger

Author

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

Subjects
Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
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), Comment: This is a reproduction of the article published in the Astrophysical Journal Letters, under the terms of the Creative Commons Attribution 3.0 licence

Published
2017
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2. Multi-messenger Observations of a Binary Neutron Star Merger

Author

Collaboration, LIGO Scientific, Collaboration, Virgo, Fermi, GBM, INTEGRAL, Collaboration, IceCube, Team, AstroSat Cadmium Zinc Telluride Imager, Collaboration, IPN, Collaboration, The Insight-Hxmt, Collaboration, ANTARES, Collaboration, The Swift, Team, AGILE, Team, The 1M2H, Collaboration, The Dark Energy Camera GW-EM, Collaboration, the DES, Collaboration, The DLT40, GRAWITA, TeAm, GRAvitational Wave Inaf, Collaboration, The Fermi Large Area Telescope, ATCA, Array, Australia Telescope Compact, ASKAP, Pathfinder, Australian SKA, Group, Las Cumbres Observatory, OzGrav, DWF, AST3, Collaborations, CAASTRO, Collaboration, The VINROUGE, Collaboration, MASTER, J-GEM, GROWTH, JAGWAR, Caltech-, NRAO, TTU-NRAO, Collaborations, NuSTAR, Pan-STARRS, Team, The MAXI, Consortium, TZAC, Collaboration, KU, Telescope, Nordic Optical, ePESSTO, GROND, University, Texas Tech, Group, SALT, TOROS, Collaboration, Transient Robotic Observatory of the South, Collaboration, The BOOTES, MWA, Array, Murchison Widefield, Collaboration, The CALET, Collaboration, IKI-GW Follow-up, Collaboration, H. E. S. S., Collaboration, LOFAR, LWA, Array, Long Wavelength, Collaboration, HAWC, Collaboration, The Pierre Auger, Collaboration, ALMA, Team, Euro VLBI, Collaboration, Pi of the Sky, University, The Chandra Team at McGill, DFN, Network, Desert Fireball, ATLAS, Survey, High Time Resolution Universe, RIMAS, RATIR, Africa/MeerKAT, SKA South, Van Eerten, Hendrik, Calloni, E., DE ROSA, Rosario, Garufi, F., De Laurentis, M., Di Girolamo, T., Milano, L., Barbato, F., Colalillo, R., Guarino, Fausto, Valore, L., Allocca, Annalisa, Fermi, Gbm, 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 and the DES Collaboration, The DLT40 Collaboration, GRAWITA: GRAvitational Wave Inaf TeAm, The Fermi Large Area Telescope Collaboration, ATCA: Australia Telescope Compact Array, ASKAP: Australian SKA Pathfinder, Las Cumbres Observatory Group, Ozgrav, Dwf, (Deeper, Wider, Faster, Program), Ast3, and CAASTRO Collaborations, The VINROUGE Collaboration, Master, Collaboration, J-GEM, Growth, Jagwar, Caltech-, Nrao, TTU-NRAO, and NuSTAR Collaborations, Pan-STARRS, The MAXI Team, Tzac, Consortium, Collaboration, Ku, 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, Collaboration, H. E. S. S., 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 and RATIR, and SKA South Africa/MeerKAT, and Pinto, Innocenzo

Subjects
astro-ph.HE, Astrophysics::High Energy Astrophysical Phenomena, gr-qc, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
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 $\sim 1.7\,{\rm{s}}$ 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 $\,{M}_{\odot }$. 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 $\sim 40\,{\rm{Mpc}}$) 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 $\sim 9$ 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. 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.

Published
2017
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