Volume 461, Number 3, January III 2007
|Page(s)||1013 - 1018|
|Section||Interstellar and circumstellar matter|
|Published online||16 October 2006|
Radio spectrum and distance of the SNR HB9
Department of Physics & Astronomy, University of Calgary, Calgary, Alberta T2N 1N4, Canada e-mail: email@example.com
2 National Astronomical Observatories, CAS, Beijing 100012, PR China
Accepted: 13 September 2006
New images are presented of the supernova remnant (SNR) HB9 based on 408 MHz and 1420 MHz continuum emission and HI-line emission data from the Canadian Galactic Plane Survey (CGPS). Two different T-T plot methods and new integrated flux densities give spectral index ( ν) for the whole of HB9 of 0.48 ± 0.03; 0.49; and 0.47 ± 0.06, respectively. These values are lower than the previous spectral index estimated for HB9 (α = 0.61). The change is mainly due to improved 1420 MHz data. No difference in spectral index is detected between strong and weak filaments. A new result is that the spectral index for interior regions is steeper than for the rim. This can be explained by a standard curved interstellar electron energy spectrum combined with lower interior magnetic field compared to that near the outer shock. This results in a larger proportion of steep spectrum emission for lines-of-sight through the central body of the SNR. HI observations show structures probably associated with the SNR in the radial velocity range -3 to -9 km s-1, suggesting a kinematic distance of 0.8 ± 0.4 kpc for the SNR. This is consistent with the distance to the radio pulsar PSR B0458+46, offset from the center of HB9 by 23′. However the pulsar spindown and kinematic ages are significantly greater than estimates of the SNR age: the Sedov age for HB9 is 6600 yr and the evaporative cloud model yields ages of 4000–7000 yr.
Key words: radio continuum: ISM / radio lines: ISM / ISM: supernova remnants
© ESO, 2007
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