{ "id": "1501.03225", "version": "v1", "published": "2015-01-14T00:48:54.000Z", "updated": "2015-01-14T00:48:54.000Z", "title": "X-ray analysis of the proper motion and pulsar wind nebula for PSR J1741-2054", "authors": [ "Katie Auchettl", "Patrick Slane", "Roger W. Romani", "Bettina Posselt", "George G. Pavlov", "Oleg Kargaltsev", "C-Y Ng", "Tea Temim", "Martin. C. Weisskopf", "Andrei Bykov", "Douglas A. Swartz" ], "comment": "9 pages, 5 figures, 4 Tables; Submitted to ApJ", "categories": [ "astro-ph.HE" ], "abstract": "We obtained six observations of PSR J1741-2054 using the $Chandra$ ACIS-S detector totaling $\\sim$300 ks. By registering this new epoch of observations to an archival observation taken 3.2 years earlier using X-ray point sources in the field of view, we have measured the pulsar proper motion at $\\mu =109 \\pm 10$ mas/yr. The spectrum of the pulsar can be described by an absorbed power law with photon index $\\Gamma$=2.68$\\pm$0.04, plus a blackbody with an emission radius of (4.5$^{+3.2}_{-2.5})d_{0.38}$ km, for a DM-estimated distance of $0.38d_{0.38}$ kpc and a temperature of $61.7\\pm3.0$ eV. Emission from the compact nebula is well described by an absorbed power law model with a photon index of $\\Gamma$ = 1.67$\\pm$0.06, while the diffuse emission seen as a trail extending northeast of the pulsar shows no evidence of synchrotron cooling. We also looked for extended features that might represent a jet or torus-like structure using image deconvolution and PSF-subtraction but we find no conclusive evidence of such features immediately surrounding the pulsar.", "revisions": [ { "version": "v1", "updated": "2015-01-14T00:48:54.000Z" } ], "analyses": { "keywords": [ "pulsar wind nebula", "x-ray analysis", "photon index", "archival observation taken", "x-ray point sources" ], "publication": { "doi": "10.1088/0004-637X/802/1/68" }, "note": { "typesetting": "TeX", "pages": 9, "language": "en", "license": "arXiv", "status": "editable", "inspire": 1339230 } } }