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Global VLBA Observations of NGC 3079

Published online by Cambridge University Press:  14 August 2015

Satoko Satoh ,
M. Inoue ,
N. Nakai ,
K.M. Shibata ,
S. Kameno ,
V. Migenes  and
P. J. Diamond
Satoko Satoh
Affiliation:
National Astronomical Observatory2-21-1 Osawa, Mitaka, Tokyo, 181Japan
M. Inoue
Affiliation:
National Astronomical Observatory2-21-1 Osawa, Mitaka, Tokyo, 181Japan
N. Nakai
Affiliation:
National Astronomical Observatory2-21-1 Osawa, Mitaka, Tokyo, 181Japan
K.M. Shibata
Affiliation:
National Astronomical Observatory2-21-1 Osawa, Mitaka, Tokyo, 181Japan
S. Kameno
Affiliation:
National Astronomical Observatory2-21-1 Osawa, Mitaka, Tokyo, 181Japan
V. Migenes
Affiliation:
National Astronomical Observatory2-21-1 Osawa, Mitaka, Tokyo, 181Japan
P. J. Diamond
Affiliation:
National Radio Astronomical ObservatoryPO Box O Socorro, NM 87801, USA

Extract

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NGC 3079 has very luminous water megamaser from the nucleus, the peak of the spectrum being blueshifted by 180 km s-1 from the systemic velocity of the galaxy (Vsys = 1131 km s-1) (Henkel et al. 1984, Haschick & Baan 1985). Core-jet like continuum structure is also found in the nuclear region (Irwin & Seaquist 1988). No velocity drift for main features of water maser (VLSR — 941-975 km s1) has been shown (Nakai et al. 1995). However, the drift was recently detected for the maser of 1190 km s-1 (Nakai 1997). HI and OH absorptions were detected in the nucleus (Haschick & Baan 1985, Irwin & Seaquist 1991). Thus this galaxy is very unique object to investigate water masers, continuum structure and absorption features all together with VLBI.

Type
II. Joint Discussions
Information
Highlights of Astronomy , Volume 11 , Issue 2: Highlights of Astronomy. As presented at the XXIIIrd General Assembly of the IAU (Part B), 1997 , 1998 , pp. 972 - 973
Copyright
Copyright © Kluwer 1998

References

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