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dc.contributor.authorHalpern, J. P.
dc.contributor.authorGotthelf, E. V.
dc.contributor.authorMirabal, N.
dc.contributor.authorCamilo, F.
dc.date.accessioned2020-09-09T17:26:41Z
dc.date.available2020-09-09T17:26:41Z
dc.date.issued2002-06-02
dc.description.abstractWe describe Chandra, Hubble Space Telescope (HST), and radio observations that reveal a radio-quiet but magnetospherically active neutron star in the error circle of the high-energy γ-ray source 3EG J1835+5918, the brightest of the unidentified EGRET sources at high Galactic latitude. A Chandra ACIS-S spectrum of the ultrasoft X-ray source RX J1836.2+5925, suggested by Mirabal & Halpern as the neutron star counterpart of 3EG J1835+5918, requires two components: a blackbody of T∞ ≈ 3 × 10⁵ K and a hard tail that can be parameterized as a power law of photon index Γ ≈ 2. An upper limit of d < 800 pc can be derived from the blackbody fit under an assumption of R∞ = 10 km. Deep optical imaging with the HST Space Telescope Imaging Spectrograph CCD failed to detect this source to a limit of V > 28.5, and thus fX/fV > 6000 and d > 250 pc assuming the X-ray-fitted temperature for the full surface. Repeated observations with the 76 m Lovell telescope at Jodrell Bank place an upper limit of less than 0.1 mJy on the flux density at 1400 MHz for a pulsar with P > 0.1 s and less than 0.25 mJy for a ~10 ms pulsar at the location of RX J1836.2+5925. All of this evidence points to an older, possibly more distant version of the highly efficient γ-ray pulsar Geminga as the origin of the γ-rays from 3EG J1835+5918.en_US
dc.description.sponsorshipWe thank Andrew Lyne for obtaining the radio data at Jodrell Bank, and the referee Patrizia Caraveo for helpful suggestions. This work was supported by grants SAO GO2-3071X and HST GO-09278.01A. The ability to obtain coordinated Chandra and HST observations under a joint proposal opportunity enabled us to achieve these results in a timely and efficient manner.en_US
dc.description.urihttps://iopscience.iop.org/article/10.1086/341967en_US
dc.format.extent4 pagesen_US
dc.genrejournal articles preprintsen_US
dc.identifierdoi:10.13016/m2co8i-svzg
dc.identifier.citationJ. P. Halpern, E. V. Gotthelf, N. Mirabal, and F. Camilo, The Next Geminga: Deep Multiwavelength Observations of a Neutron Star Identified with 3EG J1835+5918, ApJ 573 L41 (2002), doi: https://doi.org/10.1086/341967en_US
dc.identifier.urihttps://doi.org/10.1086/341967
dc.identifier.urihttp://hdl.handle.net/11603/19620
dc.language.isoen_USen_US
dc.publisherIOPen_US
dc.relation.isAvailableAtThe University of Maryland, Baltimore County (UMBC)
dc.relation.ispartofUMBC Physics Department Collection
dc.relation.ispartofUMBC Joint Center for Earth Systems Technology (JCET)
dc.relation.ispartofUMBC Center for Space Sciences and Technology (CSST) / Center for Research and Exploration in Space Sciences & Technology II (CRSST II)
dc.rightsThis item is likely protected under Title 17 of the U.S. Copyright Law. Unless on a Creative Commons license, for uses protected by Copyright Law, contact the copyright holder or the author.
dc.rights© 2002. The American Astronomical Society. All rights reserved.
dc.titleThe Next Geminga: Deep Multiwavelength Observations of a Neutron Star Identified with 3EG J1835+5918en_US
dc.typeTexten_US


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