NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-04-22 T19:33:51 PDT
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For refcode 2015PASJ...67....5M:
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Copyright by Astronomical Society of Japan. 2015PASJ...67....5M Hot ammonia in the center of the Seyfert 2 galaxy NGC 3079 Miyamoto, Yusuke; Nakai, Naomasa; Seta, Masumichi; Salak, Dragan; Hagiwara, Kenzaburo; Nagai, Makoto; Ishii, Shun; Yamauchi, Aya Abstract. We present the results of ammonia observations toward the center of NGC 3079. The NH_3_(J, K) = (1, 1) and (2, 2) inversion lines were detected in absorption with the Tsukuba 32 m telescope, and the NH_3_(1, 1) through (6, 6) lines with the VLA, although the profile of NH_3_(3, 3) was in emission in contrast to the other transitions. The background continuum source, whose flux density was ~ 50 mJy, could not be resolved with the VLA beam of <~ 0{^"_._}09 x 0{^"_._}08. All ammonia absorption lines have two distinct velocity components: one is at the systemic velocity and the other is blueshifted, and both components are aligned along the nuclear jets. For the systemic components, the relatively low temperature gas is extended more than the high temperature gas. The blueshifted NH_3_(3, 3) emission can be regarded as ammonia masers associated with shocks by strong winds probably from newly formed massive stars or supernova explosions in dense clouds in the nuclear megamaser disk. Using para-NH_3_(1, 1), (2, 2), (4, 4), and (5, 5) lines with VLA, we derived the rotational temperature T_rot_ = 120 +/- 12 K and 157 +/- 19 K for the systemic and blueshifted components, respectively. The total column densities of NH_3_(0, 0)-(6, 6), assuming T_ex_ ~ T_rot_, were (8.85 +/- 0.70) x 10^16^ cm^-2^ and (4.47 +/- 0.78) x 10^16^ cm^-2^ for the systemic and blueshifted components, respectively. The fractional abundance of NH_3_ relative to molecular hydrogen H_2_ for the systemic and blueshifted was [NH_3_]/[H_2_] = 1.3 x 10^-7^ and 6.5 x 10^-8^, respectively. We also found the F = 4-4 and F = 5-5 doublet lines of OH ^2^Pi_3/2_ J = 9/2 in absorption, which could be fitted by two velocity components, systemic and redshifted components. The rotational temperature of OH was estimated to be T_rot, OH_ >= 175 K, tracing hot gas associated with the interaction of the fast nuclear outflow with dense molecular material around the nucleus. Key words: galaxies: individual (NGC 3079), galaxies: ISM, radio lines: galaxies, radio lines: ISM
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