Статья

Results from a Systematic Survey of X-Ray Emission from Hydrogen-poor Superluminous SNe

R. MarguttiCenter for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208, USAR. ChornockAstrophysical Institute, Department of Physics and Astronomy, 251B Clippinger Lab, Ohio University, Athens, OH 45701, USABrian D. MetzgerColumbia Astrophysics Laboratory, Columbia University, Pupin Hall, New York, NY 10027, USAD. L. CoppejansCenter for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208, USAC. GuidorziDepartment of Physics and Earth Science, University of Ferrara, via Saragat 1, I-44122, Ferrara, ItalyGiulia MiglioriLaboratoire AIM (CEA/IRFU—CNRS/INSU—Universite Paris Diderot), CEA DSM/SAp, F-91191 Gif-sur-Yvette, FranceD. MilisavljevicHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAE. BergerHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAM. NichollHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAB. A. ZaudererCenter for Cosmology and Particle Physics, New York University, 4 Washington Place, New York, NY 10003, USAR. LunnanDepartment of Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USAA. KambleHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAM. DroutCarnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USAM. ModjazCenter for Cosmology and Particle Physics, New York University, 4 Washington Place, New York, NY 10003, USA

2018en

ABI

Аннотация

Abstract We present the results from a sensitive X-ray survey of 26 nearby hydrogen-poor superluminous supernovae (SLSNe-I) with Swift , Chandra, and XMM . This data set constrains the SLSN evolution from a few days until ∼2000 days after explosion, reaching a luminosity limit L x ∼ 10 40 erg s −1 and revealing the presence of significant X-ray emission possibly associated with PTF 12dam. No SLSN-I is detected above , suggesting that the luminous X-ray emission L x ∼ 10 45 erg s −1 associated with SCP 60F6 is not common among SLSNe-I. We constrain the presence of off-axis gamma-ray burst (GRB) jets, ionization breakouts from magnetar engines and the density in the sub-parsec environments of SLSNe-I through inverse Compton emission. The deepest limits rule out the weakest uncollimated GRB outflows, suggesting that if the similarity of SLSNe-I with GRB/SNe extends to their fastest ejecta, then SLSNe-I are either powered by energetic jets pointed far away from our line of sight ( θ > 30°), or harbor failed jets that do not successfully break through the stellar envelope. Furthermore, if a magnetar central engine is responsible for the exceptional luminosity of SLSNe-I, our X-ray analysis favors large magnetic fields G and ejecta masses , in agreement with optical/UV studies. Finally, we constrain the pre-explosion mass-loss rate of stellar progenitors of SLSNe-I. For PTF 12dam we infer , suggesting that the SN shock interaction with an extended circumstellar medium is unlikely to supply the main source of energy powering the optical transient and that some SLSN-I progenitors end their lives as compact stars surrounded by a low-density medium similar to long GRBs and type Ib/c SNe.

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Идентификаторы

DOI: 10.3847/1538-4357/aad2df

Цитирования и источники

Цитирований: 2Использованных источников: 0

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