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High-Energy Observations of PSR B1259-63/LS 2883 Through the 2014 Periastron Passage: Connecting X-Rays to the GeV Flare

Tam, P. H. T. and Li, K. L. and Takata, J. and Okazaki, A. T. and Hui, C. Y. and Kong, A. K. H. (2015) High-Energy Observations of PSR B1259-63/LS 2883 Through the 2014 Periastron Passage: Connecting X-Rays to the GeV Flare. Astrophysical Journal Letters, 798 (1). L26-L31. ISSN 2041-8205. http://resolver.caltech.edu/CaltechAUTHORS:20150824-164910021

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Abstract

The binary system PSR B1259–63/LS 2883 is well sampled in radio, X-rays, and TeV γ-rays, and shows orbital-phase-dependent variability in these frequencies. The first detection of GeV γ-rays from the system was made around the 2010 periastron passage. In this Letter, we present an analysis of X-ray and γ-ray data obtained by the Swift/XRT, NuSTAR/FPM, and Fermi/LAT, through the recent periastron passage which occurred on 2014 May 4. While PSR B1259–63/LS 2883 was not detected by the Large Area Telescope before and during this passage, we show that the GeV flares occurred at a similar orbital phase as in early 2011, thus establishing the repetitive nature of the post-periastron GeV flares. Multiple flares each lasting for a few days have been observed and short-term variability is seen as well. We also found X-ray flux variation contemporaneous with the GeV flare for the first time. Strong evidence of the keV-to-GeV connection came from the broadband high-energy spectra, which we interpret as synchrotron radiation from the shocked pulsar wind.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/2041-8205/798/1/L26DOIArticle
http://iopscience.iop.org/2041-8205/798/1/L26/PublisherArticle
ORCID:
AuthorORCID
Tam, P. H. T.0000-0002-1262-7375
Li, K. L.0000-0001-8229-2024
Takata, J.0000-0002-8731-0129
Hui, C. Y.0000-0003-1753-1660
Kong, A. K. H.0000-0002-5105-344X
Additional Information:© 2015. The American Astronomical Society. Received 2014 October 7, accepted for publication 2014 December 5. Published 2014 December 19. We acknowledge the use of data and software facilities from the FSSC, managed by the HEASARC at the Goddard Space Flight Center. P.H.T. and K.L.L. are supported by the Ministry of Science and Technology (MOST) of the Republic of China (Taiwan) through grant 101-2112-M-007-022-MY3. A.K.H.K. is supported by MOST through grants 100-2628-M-007-002-MY3, 100-2923-M-007-001-MY3, and 103-2628-M-007-003-MY3. J.T. is supported by a 2014 GRF grant of Hong Kong Government under HKU 17300814P. C.Y.H. is supported by the National Research Foundation of Korea through grant 2014R1A1A2058590.
Group:NuSTAR
Funders:
Funding AgencyGrant Number
Ministry of Science and Technology (Taipei)101-2112-M-007-022-MY3
Ministry of Science and Technology (Taipei)100-2628- M-007-002-MY3
Ministry of Science and Technology (Taipei)100-2923-M-007-001-MY3
Ministry of Science and Technology (Taipei)100-2628- M-007-002-MY3
Ministry of Science and Technology (Taipei)100-2923-M-007-001-MY3
Ministry of Science and Technology (Taipei)103-2628- M-007-003-MY3
General Research Fund (Hong Kong)HKU 17300814P
National Research Foundation of Korea2014R1A1A2058590
Record Number:CaltechAUTHORS:20150824-164910021
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20150824-164910021
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:59866
Collection:CaltechAUTHORS
Deposited By: Joy Painter
Deposited On:25 Aug 2015 01:20
Last Modified:22 Mar 2019 16:52

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