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Title: SNR G349.7+0.2: A γ-RAY SOURCE IN THE FAR 3 kpc ARM OF THE GALACTIC CENTER

We analyze the H I absorption profile for TeV supernova remnant (SNR) G349.7+0.2 based on updated knowledge of the inner Galaxy's structure. We significantly revise its kinematic distance from the previous ∼22 kpc to ∼11.5 kpc, indicating it is in the far 3 kpc arm of the Galactic center. We give a revised age of ∼1800 yr for G349.7+0.2 which has a low explosion energy of ∼2.5 × 10{sup 50} erg. This removes G349.7+0.2 from the set of brightest SNRs in radio and X-ray to γ-ray wavebands and helps us to better understand γ-ray emission originating from this remnant. However, one needs to use caution when discussing old kinematic distances of Galactic objects (e.g., SNRs, pulsars, and H II regions) in the range of –12° ≤ l ≤ 12° with distance estimates of ≥5.5 kpc.
Authors:
 [1] ;  [2]
  1. National Astronomical Observatories, CAS, Beijing 100012 (China)
  2. Department of Physics and Astronomy, University of Calgary, Calgary, Alberta T2N 1N4 (Canada)
Publication Date:
OSTI Identifier:
22363971
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal Letters; Journal Volume: 783; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ABSORPTION; COSMIC GAMMA SOURCES; COSMIC PHOTONS; DISTANCE; MILKY WAY; PHOTON EMISSION; PULSARS; SUPERNOVA REMNANTS; TEV RANGE; X RADIATION