المؤلفون: Andreoni, Igor, Goldstein, Daniel A., Kasliwal, Mansi M., Nugent, Peter E., Zhou, Rongpu, Newman, Jeffrey A., Bulla, Mattia, Foucart, Francois, Hotokezaka, Kenta, Nakar, Ehud, Nissanke, Samaya, Raaijmakers, Geert, Bloom, Joshua S., De, Kishalay, Jencson, Jacob E., Ward, Charlotte, Ahumada, Tomás, Anand, Shreya, Buckley, David A. H., Caballero-García, María Dolores, Castro-Tirado, Alberto J., Copperwheat, Christopher M., Coughlin, Michael W., Cenko, S. Bradley, Gromadzki, Mariusz, Hu, Youdong, Karambelkar, Viraj R., Perley, Daniel A., Sharma, Yashvi, Valeev, Azamat F., Cook, David O., Fremling, U. Christoffer, Kumar, Harsh, Taggart, Kirsty, Bagdasaryan, Ashot, Cooke, Jeff, Dahiwale, Aishwarya, Dhawan, Suhail, Dobie, Dougal, Gatkine, Pradip, Golkhou, V. Zach, Goobar, Ariel, Chaves, Andreas Guerra, Hankins, Matthew, Kaplan, David L., Kong, Albert K. H., Kool, Erik C., Mohite, Siddharth, Sollerman, Jesper, Tzanidakis, Anastasios, Webb, Sara, Zhang, Keming

المساهمون: National Science Foundation (US), Hubble Space Telescope, Space Telescope Science Institute (US), National Aeronautics and Space Administration (US), Department of Energy (US), Amazon, Simons Foundation, Knut and Alice Wallenberg Foundation, Gordon and Betty Moore Foundation, National Research Foundation (South Africa), Netherlands Organization for Scientific Research, Australian Government, China Scholarship Council, Ministry of Science and Technology (Taiwan), University of Washington, Washington Research Foundation, National Science Centre (Poland)

مصطلحات موضوعية: On 2019 August 14, the Advanced LIGO and Virgo interferometers detected the high-significance gravitational wave (GW) signal S190814bv. The GW data indicated that the event resulted from a neutron star-black hole (NSBH) merger, or potentially a low-mass binary BH merger. Due to the low false-alarm rate and the precise localization (23 deg2 at 90%), S190814bv presented the community with the best opportunity yet to directly observe an optical/near-infrared counterpart to an NSBH merger. To search for potential counterparts, the GROWTH Collaboration performed real-time image subtraction on six nights of public Dark Energy Camera images acquired in the 3 weeks following the merger, covering >98% of the localization probability. Using a worldwide network of follow-up facilities, we systematically undertook spectroscopy and imaging of optical counterpart candidates. Combining these data with a photometric redshift catalog, we ruled out each candidate as the counterpart to S190814bv and placed deep, uniform limits on the optical emission associated with S190814bv. For the nearest consistent GW distance, radiative transfer simulations of NSBH mergers constrain the ejecta mass of S190814bv to be M ej < 0.04 M o&dot, at polar viewing angles, or M ej < 0.03 M o&dot, if the opacity is κ < 2 cm2g-1. Assuming a tidal deformability for the NS at the high end of the range compatible with GW170817 results, our limits would constrain the BH spin component aligned with the orbital momentum to be χ < 0.7 for mass ratios Q < 6, with weaker constraints for more compact NSs. © 2020. The American Astronomical Society. All rights reserved

Relation: Postprint; http://dx.doi.org/10.3847/1538-4357/ab6a1b; Sí; e-issn: 1538-4357; Astrophysical Journal 890(2): 131 (2020); http://hdl.handle.net/10261/218992; http://dx.doi.org/10.13039/100000893; http://dx.doi.org/10.13039/100013757; http://dx.doi.org/10.13039/100007812; http://dx.doi.org/10.13039/100001906; http://dx.doi.org/10.13039/501100004543; http://dx.doi.org/10.13039/100000015; http://dx.doi.org/10.13039/100000936; http://dx.doi.org/10.13039/501100004063; http://dx.doi.org/10.13039/100000104; http://dx.doi.org/10.13039/501100001321; http://dx.doi.org/10.13039/501100004281; http://dx.doi.org/10.13039/100000001

الاتاحة: http://hdl.handle.net/10261/218992
https://doi.org/10.3847/1538-4357/ab6a1b
https://doi.org/10.13039/100000893
https://doi.org/10.13039/100013757
https://doi.org/10.13039/100007812
https://doi.org/10.13039/100001906
https://doi.org/10.13039/501100004543
https://doi.org/10.13039/100000015
https://doi.org/10.13039/100000936
https://doi.org/10.13039/501100004063

المؤلفون: AA Chrimes, AJ Levan, AS Fruchter, PJ Groot, C Kouveliotou, JD Lyman, NR Tanvir, K Wiersema

مصطلحات موضوعية: Uncategorized, Astronomy & Astrophysics, DISCOVERY, GIANT FLARE, IR VARIABILITY, NEAR-INFRARED COUNTERPART, NEUTRON-STARS, OPTICAL PULSATIONS, Physical Sciences, PULSAR, Science & Technology, SOFT GAMMA-REPEATERS, stars: magnetars, XMM-NEWTON, X-RAY-EMISSION

Relation: 2381/25029200.v1; https://figshare.com/articles/journal_contribution/New_candidates_for_magnetar_counterparts_from_a_deep_search_with_the_Hubble_Space_Telescope/25029200

الاتاحة: https://figshare.com/articles/journal_contribution/New_candidates_for_magnetar_counterparts_from_a_deep_search_with_the_Hubble_Space_Telescope/25029200

المؤلفون: S. Bradley Cenko, Anastasios Tzanidakis, Chris M. Copperwheat, Mariusz Gromadzki, Jeffrey A. Newman, Keming Zhang, A. F. Valeev, David O. Cook, Aishwarya S. Dahiwale, M. D. Caballero-Garcia, Kenta Hotokezaka, Jesper Sollerman, A. J. Castro-Tirado, Samaya Nissanke, Yashvi Sharma, S. R. Mohite, Ashot Bagdasaryan, David L. Kaplan, Peter Nugent, Mansi M. Kasliwal, Ariel Goobar, Suhail Dhawan, Tomas Ahumada, Charlotte Ward, Jacob E. Jencson, M. Hankins, Kaushik De, Sara Webb, Igor Andreoni, Erik C. Kool, U. Christoffer Fremling, Dougal Dobie, Jeff Cooke, Harsh Kumar, V. Zach Golkhou, Daniel A. Perley, David A. H. Buckley, Mattia Bulla, Andreas Guerra Chaves, Francois Foucart, Kirsty Taggart, Daniel A. Goldstein, Shreya Anand, Michael W. Coughlin, Pradip Gatkine, Ehud Nakar, Joshua S. Bloom, Y. D. Hu, Albert K. H. Kong, Rongpu Zhou, Geert Raaijmakers, Viraj Karambelkar

المساهمون: National Science Foundation (US), Hubble Space Telescope, Space Telescope Science Institute (US), National Aeronautics and Space Administration (US), Department of Energy (US), Amazon, Simons Foundation, Knut and Alice Wallenberg Foundation, Gordon and Betty Moore Foundation, National Research Foundation (South Africa), Netherlands Organization for Scientific Research, Australian Government, China Scholarship Council, Ministry of Science and Technology (Taiwan), University of Washington, Washington Research Foundation, National Science Centre (Poland)

المصدر: Digital.CSIC. Repositorio Institucional del CSIC
instname
Astrophysical Journal, vol 890, iss 2
The Astrophysical Journal, vol 890, iss 2

مصطلحات موضوعية: 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Binary stars, Atomic, Physical Chemistry, NO, Neutron stars, Gravitational waves, Vaccine Related, Particle and Plasma Physics, Binary black hole, 0103 physical sciences, Radiative transfer, Nuclear, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Photometric redshift, QB, Physics, Gravitational wave sources, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), if the opacity is κ < 2 cm2g-1. Assuming a tidal deformability for the NS at the high end of the range compatible with GW170817 results, our limits would constrain the BH spin component aligned with the orbital momentum to be χ < 0.7 for mass ratios Q < 6, with weaker constraints for more compact NSs. © 2020. The American Astronomical Society. All rights reserved, Gravitational wave, Molecular, Astronomy and Astrophysics, Black hole physics, 16. Peace & justice, Observational astronomy, LIGO, Transient sources, Black hole, Photometry (astronomy), Neutron star, Space and Planetary Science, Neutron stars, Binary stars, Gravitational wave sources, Gravitational waves, Transient sources, Black hole physics, Observational astronomy, at polar viewing angles, or M ej < 0.03 M o&dot, Astrophysics - High Energy Astrophysical Phenomena, Astronomical and Space Sciences, On 2019 August 14, the Advanced LIGO and Virgo interferometers detected the high-significance gravitational wave (GW) signal S190814bv. The GW data indicated that the event resulted from a neutron star-black hole (NSBH) merger, or potentially a low-mass binary BH merger. Due to the low false-alarm rate and the precise localization (23 deg2 at 90%), S190814bv presented the community with the best opportunity yet to directly observe an optical/near-infrared counterpart to an NSBH merger. To search for potential counterparts, the GROWTH Collaboration performed real-time image subtraction on six nights of public Dark Energy Camera images acquired in the 3 weeks following the merger, covering >98% of the localization probability. Using a worldwide network of follow-up facilities, we systematically undertook spectroscopy and imaging of optical counterpart candidates. Combining these data with a photometric redshift catalog, we ruled out each candidate as the counterpart to S190814bv and placed deep, uniform limits on the optical emission associated with S190814bv. For the nearest consistent GW distance, radiative transfer simulations of NSBH mergers constrain the ejecta mass of S190814bv to be M ej < 0.04 M o&dot, Physical Chemistry (incl. Structural)

وصف الملف: application/pdf

URL الوصول: https://explore.openaire.eu/search/publication?articleId=doi_dedup___::0965b1c3200ae4ba9cf1e8c16dc9cb5e
http://arxiv.org/abs/1910.13409

المؤلفون: Shi, Y, Xu, RX

المساهمون: Shi, Y (reprint author), Peking Univ, Sch Phys, Beijing 100871, Peoples R China., Peking Univ, Sch Phys, Beijing 100871, Peoples R China.

المصدر: SCI

مصطلحات موضوعية: pulsars : general, pulsars : individual (1E 1207.4-5209), stars : neutron, X-RAY PULSAR, NEAR-INFRARED COUNTERPART, SPIN-DOWN, STRANGE STARS, FALLBACK DISK, 1E 2259+586, BLACK-HOLE, SUPERNOVA, G296.5+10.0

Relation: ASTROPHYSICAL JOURNAL.2003,596,(1),L75-L78.; 1007812; http://hdl.handle.net/20.500.11897/298306; WOS:000185814500019

الاتاحة: https://hdl.handle.net/20.500.11897/298306
https://doi.org/10.1086/379111