منابع مشابه
Vlbi Observations of Sn 2008d
We report on two epochs of VLBI observations of the Type Ib/c supernova SN 2008D, which was associated with the X-ray outburst XRF 080109, At our first epoch, at t = 30 days after the explosion, we observed at 22 and 8.4 GHz, and at our second, at t = 133 days, at 8.4 and 5.0 GHz. The VLBI observations allow us to accurately measure the source’s size and position at each epoch, and thus constra...
متن کامل23 Ghz Vlbi Observations of Sn 2008ax 23 Ghz Vlbi Observations of Sn 2008ax (research Note)
We report on phase-referenced 23 GHz Very-Long-Baseline-Interferometry (VLBI) observations of the type IIb supernova SN 2008ax, made with the Very Long Baseline Array (VLBA) on 2 April 2008 (33 days after explosion). These observations resulted in a marginal detection of the supernova. The total flux density recovered from our VLBI image is 0.8±0.3 mJy (one standard deviation). As it appears, t...
متن کاملVLBI Observations of SN 2008 ax ( Research Note )
We report on phase-referenced 23 GHz Very-Long-Baseline-Interferometry (VLBI) observations of the type IIb supernova SN 2008ax, made with the Very Long Baseline Array (VLBA) on 2 April 2008 (33 days after explosion). These observations resulted in a marginal detection of the supernova. The total flux density recovered from our VLBI image is 0.8±0.3 mJy (one standard deviation). As it appears, t...
متن کاملHigh-resolution Radio Imaging of Young Supernovae
The high resolution obtained through the use of VLBI gives an unique opportunity to directly observe the interaction of an expanding radio supernova with its surrounding medium. We present here results from our VLBI observations of the young supernovae SN 1979C, SN 1986J, and SN 2001gd.
متن کاملLate-Time Optical and UV Spectra of SN 1979C and SN 1980K
A low-dispersion Keck I spectrum of SN 1980K taken in August 1995 (t = 14.8 yr after explosion) and a November 1997 MDM spectrum (t = 17.0 yr) show broad 5500 km s emission lines of Hα, [O I] 6300,6364 Å, and [O II] 7319,7330 Å. Weaker but similarly broad lines detected include [Fe II] 7155 Å, [S II] 4068,4072 Å, and a blend of [Fe II] lines at 5050–5400 Å. The presence of strong [S II] 4068,40...
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ژورنال
عنوان ژورنال: International Astronomical Union Colloquium
سال: 2005
ISSN: 0252-9211
DOI: 10.1017/s0252921100009052