TY - JOUR
T1 - Discovery of two radio transients at a high galactic latitude in a 1.4 ghz drift-scan survey
AU - Niinuma, K.
AU - Daishido, T.
AU - Matsumura, N.
AU - Takefuji, K.
AU - Kuniyoshi, M.
AU - Asuma, K.
AU - Kida, S.
AU - Tanaka, T.
AU - Aoki, T.
AU - Ishikawa, S.
AU - Hirano, K.
AU - Uehara, H.
AU - Nakagawa, S.
PY - 2009
Y1 - 2009
N2 - We report two new radio transients at high Galactic latitude, WJN J0951+3300 (α = 09h51m22s 10s, δ = 33°00′ 0°.4, b = 50°542) and WJN J1039+3300 (α = 10h39m26s 10s, δ = 33°00′ 0°.4, b = 60°585), which were detected by interferometric drift-scan observations at 1.4 GHz at the Waseda Nasu Pulsar Observatory. WJN J0951+3300 was detected at 16:49:32 UT on 2006 January 12 with the flux density of approximately 1760.5 265.9 mJy, and WJN J1039+3300 was detected at 17:13:32 UT on 2006 January 18 with the flux density of approximately 2242.5 228.7 mJy. Both of them lasted for a short duration (≤2 days). The possibility that the distribution of the WJN radio transients is isotropic was suggested in a previous study. Having re-evaluated the log N-log S relation with the addition of the two new objects reported in this paper, we find that the slope is consistent with a slope of -1.5 and the previous result. Additionally, although there are several counterparts to WJN radio transients, we found that one of the quasar counterparts within the positional error of WJN J0951+3300 could be a radio-loud quasar. We have discussed whether or not WJN J0951+3300 could be of this quasar origin.
AB - We report two new radio transients at high Galactic latitude, WJN J0951+3300 (α = 09h51m22s 10s, δ = 33°00′ 0°.4, b = 50°542) and WJN J1039+3300 (α = 10h39m26s 10s, δ = 33°00′ 0°.4, b = 60°585), which were detected by interferometric drift-scan observations at 1.4 GHz at the Waseda Nasu Pulsar Observatory. WJN J0951+3300 was detected at 16:49:32 UT on 2006 January 12 with the flux density of approximately 1760.5 265.9 mJy, and WJN J1039+3300 was detected at 17:13:32 UT on 2006 January 18 with the flux density of approximately 2242.5 228.7 mJy. Both of them lasted for a short duration (≤2 days). The possibility that the distribution of the WJN radio transients is isotropic was suggested in a previous study. Having re-evaluated the log N-log S relation with the addition of the two new objects reported in this paper, we find that the slope is consistent with a slope of -1.5 and the previous result. Additionally, although there are several counterparts to WJN radio transients, we found that one of the quasar counterparts within the positional error of WJN J0951+3300 could be a radio-loud quasar. We have discussed whether or not WJN J0951+3300 could be of this quasar origin.
KW - Radio continuum: general
KW - Stars: variables: other
KW - Techniques: interferometric
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U2 - 10.1088/0004-637X/704/1/652
DO - 10.1088/0004-637X/704/1/652
M3 - Article
AN - SCOPUS:70549094320
SN - 0004-637X
VL - 704
SP - 652
EP - 660
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
ER -