Alp, D, Larsson, J, Fransson, C, Indebetouw, R, Jerkstrand, A, Ahola, A, Burrows, D, Challis, P, Cigan, P, Cikota, A, Kirshner, RP, van Loon, JT ORCID: https://orcid.org/0000-0002-1272-3017, Mattila, S, Ng, C-Y, Park, S, Spyromilio, J, Woosley, S, Baes, M, Bouchet, P, Chevalier, R, Frank, KA, Gaensler, BM, Gomez, H, Janka, H-T, Leibundgut, B, Lundqvist, P, Marcaide, J, Matsuura, M, Sollerman, J, Sonneborn, G, Staveley-Smith, L, Zanardo, G, Gabler, M, Taddia, F and Wheeler, JC (2018) The 30 Year Search for the Compact Object in SN 1987A. Astrophysical Journal, 864 (2). 174 -174.

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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 ( erg s−1 cm−2 Hz−1) at 213 GHz, 1 L ⊙ ( 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 ( 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 –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 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 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
Additional Information: This is the final published version of the article (version of record). It first appeared online via IOP Science at https://doi.org/10.3847/1538-4357/aad739 - please refer to any applicable terms of use of the publisher.
Subjects: Q Science > QB Astronomy > QB460 Astrophysics
Divisions: Faculty of Natural Sciences > School of Chemical and Physical Sciences
Depositing User: Symplectic
Date Deposited: 27 Sep 2018 09:03
Last Modified: 05 Mar 2019 16:08
URI: http://eprints.keele.ac.uk/id/eprint/5370

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