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The 30 year search for the compact object in SN 1987A

Alp, Dennis, Larsson, Josefin, Fransson, Claes, Indebetouw, Remy, Jerkstrand, Anders, Ahola, Antero, Burrows, David, Challis, Peter, Cigan, Phil, Cikota, Aleksandar, Kirshner, Robert P., van Loon, Jacco Th., Mattila, Seppo, Ng, C.-Y., Park, Sangwook, Spyromilio, Jason, Woosley, Stan, Baes, Maarten, Bouchet, Patrice, Chevalier, Roger, Frank, Kari A., Gaensler, B. M., Gomez, Haley, Janka, Hans-Thomas, Leibundgut, Bruno, Lundqvist, Peter, Marcaide, Jon, Matsuura, Mikako, Sollerman, Jesper, Sonneborn, George, Staveley-Smith, Lister, Zanardo, Giovanna, Gabler, Michael, Taddia, Francesco and Wheeler, J. Craig 2018. The 30 year search for the compact object in SN 1987A. Astrophysical Journal 864 (2) , 174. 10.3847/1538-4357/aad739

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Abstract

Despite more than 30 years of searching, the compact object in Supernova (SN) 1987A has not yet been detected. We present new limits on the compact object in SN 1987A using millimeter, near-infrared, optical, ultraviolet, and X-ray observations from ALMA, VLT, HST, and Chandra. The limits are approximately 0.1 mJy ($0.1 imes {10}^{-26}$ erg s−1 cm−2 Hz−1) at 213 GHz, 1 L ⊙ ($6 imes {10}^{-29}$ erg s−1 cm−2 Hz−1) in the optical if our line of sight is free of ejecta dust, and 1036 erg s−1 ($2 imes {10}^{-30}$ erg s−1 cm−2 Hz−1) in 2–10 keV X-rays. Our X-ray limits are an order of magnitude less constraining than previous limits because we use a more realistic ejecta absorption model based on three-dimensional neutrino-driven SN explosion models. The allowed bolometric luminosity of the compact object is 22 L ⊙ if our line of sight is free of ejecta dust, or 138 L ⊙ if dust-obscured. Depending on assumptions, these values limit the effective temperature of a neutron star (NS) to $lt 4$–8 MK and do not exclude models, which typically are in the range 3–4 MK. For the simplest accretion model, the accretion rate for an efficiency η is limited to $lt {10}^{-11},{eta }^{-1}$ M ⊙ yr−1, which excludes most predictions. For pulsar activity modeled by a rotating magnetic dipole in vacuum, the limit on the magnetic field strength (B) for a given spin period (P) is $Blesssim {10}^{14},{P}^{2}$ G s−2, which firmly excludes pulsars comparable to the Crab. By combining information about radiation reprocessing and geometry, we infer that the compact object is a dust-obscured thermally emitting NS, which may appear as a region of higher-temperature ejecta dust emission.

Item Type: Article
Date Type: Publication
Status: Published
Schools: Physics and Astronomy
Publisher: American Astronomical Society
ISSN: 0004-637X
Date of First Compliant Deposit: 28 September 2018
Date of Acceptance: 28 July 2018
Last Modified: 02 Oct 2018 22:08
URI: http://orca.cf.ac.uk/id/eprint/115321

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