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Multi-wavelength Observations of the Radio Magnetar PSR J1622–4950 and Discovery of Its Possibly Associated Supernova Remnant

Anderson, Gemma E. and Gaensler, B. M. and Slane, Patrick O. and Rea, Nanda and Kaplan, David L. and Posselt, Bettina and Levin, Lina and Johnston, Simon and Murray, Stephen S. and Brogan, Crystal L. and Bailes, Matthew and Bates, Samuel and Benjamin, Robert A. and Bhat, N. D. Ramesh and Burgay, Marta and Burke-Spolaor, Sarah and Chakrabarty, Deepto and D'Amico, Nichi and Drake, Jeremy J. and Esposito, Paolo and Grindlay, Jonathan E. and Hong, Jaesub and Israel, G. L. and Keith, Michael J. and Kramer, Michael and Lazio, T. Joseph W. and Lee, Julia C. and Mauerhan, Jon C. and Milia, Sabrina and Possenti, Andrea and Stappers, Ben and Steeghs, Danny T. H. (2012) Multi-wavelength Observations of the Radio Magnetar PSR J1622–4950 and Discovery of Its Possibly Associated Supernova Remnant. Astrophysical Journal, 751 (1). Art. No. 53. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20120601-113248553

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Abstract

We present multi-wavelength observations of the radio magnetar PSR J1622-4950 and its environment. Observations of PSR J1622-4950 with Chandra (in 2007 and 2009) and XMM (in 2011) show that the X-ray flux of PSR J1622-4950 has decreased by a factor of ~50 over 3.7 years, decaying exponentially with a characteristic time of τ = 360 ± 11 days. This behavior identifies PSR J1622-4950 as a possible addition to the small class of transient magnetars. The X-ray decay likely indicates that PSR J1622-4950 is recovering from an X-ray outburst that occurred earlier in 2007, before the 2007 Chandra observations. Observations with the Australia Telescope Compact Array show strong radio variability, including a possible radio flaring event at least one and a half years after the 2007 X-ray outburst that may be a direct result of this X-ray event. Radio observations with the Molonglo Observatory Synthesis Telescope reveal that PSR J1622-4950 is 8' southeast of a diffuse radio arc, G333.9+0.0, which appears non-thermal in nature and which could possibly be a previously undiscovered supernova remnant (SNR). If G333.9+0.0 is an SNR then the estimates of its size and age, combined with the close proximity and reasonable implied velocity of PSR J1622-4950, suggest that these two objects could be physically associated.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/751/1/53DOIArticle
http://iopscience.iop.org/0004-637X/751/1/53/PublisherArticle
ORCID:
AuthorORCID
Gaensler, B. M.0000-0002-3382-9558
Kaplan, David L.0000-0001-6295-2881
Brogan, Crystal L.0000-0002-6558-7653
Bailes, Matthew0000-0003-3294-3081
Burke-Spolaor, Sarah0000-0003-4052-7838
Chakrabarty, Deepto0000-0001-8804-8946
Additional Information:© 2012 American Astronomical Society. Received 2011 September 15; accepted 2012 March 9; published 2012 May 4. We thank the referee for their careful reading of the manuscript and constructive suggestions. G.E.A acknowledges the support of an Australian Postgraduate Award. B.M.G. acknowledges the support of an Australian Laureate Fellowship. P.O.S. acknowledges partial support from NASA Contract NAS8-03060. N.R. is supported by a Ramon y Cajal Research Fellowship to CSIC, and grants AYA2009-07391 and SGR2009-811, as well as the Formosa Program TW2010005. J.J.D was supported by NASA contract NAS8-39073 to the Chandra X-ray Center (CXC). P.E. acknowledges financial support from the Autonomous Region of Sardinia through a research grant under the program PO Sardegna FSE 2007–2013, L.R. 7/2007. D.T.H.S. acknowledges an STFC Advanced Fellowship. Support for this work was also provided by NASA through Chandra Award Number GO9-0155X issued by the CXC, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA. This research makes use of data obtained with the Chandra X-ray Observatory, and software provided by the CXC in the application packages CIAO. This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. MOST is operated with the support of the Australian Research Council and the Science Foundation for Physics within the University of Sydney. ATCA and Parkes, part of the Australia Telescope, are funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. Observing time on the 6.5 m Baade Magellan Telescope, located at Las Campanas Observatory, was allocated through the Harvard-Smithsonian Center for Astrophysics. 2MASS is a joint project of the University of Massachusetts and the IPAC/Caltech, funded by the NASA and NFS. GLIMPSE survey data are part of the Spitzer Legacy Program. The Spitzer Space Telescope is operated by the JPL/Caltech under a contract with NASA. This research has made use of NASA’s Astrophysics Data System. Facilities: ASCA, ATCA, CXO (ACIS), Magellan:Baade (PANIC), Molonglo Observatory, Parkes, XMM (EPIC)
Group:TAPIR
Funders:
Funding AgencyGrant Number
Australian Postgraduate AwardUNSPECIFIED
Australian Research CouncilUNSPECIFIED
NASANAS8-03060
Ramón y Cajal ProgrammeAYA2009-07391
Ramón y Cajal ProgrammeSGR2009-811
Formosa ProgramTW2010005
NASANAS8-39073
Autonomous Region of Sardinia PO Sardegna ProgramFSE 2007-2013, L.R. 7/2007
Science and Technology Facilities Council (STFC)UNSPECIFIED
NASAGO9-0155X
University of Sydney Science Foundation for PhysicsUNSPECIFIED
Commonwealth of AustraliaUNSPECIFIED
NSFUNSPECIFIED
NASA/JPL/CaltechUNSPECIFIED
Subject Keywords: ISM: individual objects (G333.9+0.0); ISM: supernova remnants; pulsars: individual (PSR J1622-4950); radio continuum: stars; stars: neutron; X-rays: stars
Issue or Number:1
Record Number:CaltechAUTHORS:20120601-113248553
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20120601-113248553
Official Citation:Multi-wavelength Observations of the Radio Magnetar PSR J1622–4950 and Discovery of Its Possibly Associated Supernova Remnant Gemma E. Anderson et al. 2012 ApJ 751 53
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:31773
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:01 Jun 2012 20:37
Last Modified:06 Nov 2019 21:06

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