Multi-epoch VERA Observations of H2O masers in OH 43.8-0.1

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dc.creatorHonma, M.
dc.creatorBushimata, T.
dc.creatorChoi, Y. K.
dc.creatorFujii, T.
dc.creatorHirota, T.
dc.creatorHoriai, K.
dc.creatorImai, H.
dc.creatorInomata, N.
dc.creatorIshitsuka, J.
dc.creatorIwadate, K.
dc.creatorJike, T.
dc.creatorKameya, O.
dc.creatorKamohara, R.
dc.creatorKan-ya, Y.
dc.creatorKawaguchi, N.
dc.creatorKijima, M.
dc.creatorKobayashi, H.
dc.creatorKuji, S.
dc.creatorKurayama, T.
dc.creatorManabe, S.
dc.creatorMiyaji, T.
dc.creatorNakagawa, A.
dc.creatorNakashima, K.
dc.creatorOh, C. S.
dc.creatorOmodaka, T.
dc.creatorOyama, T.
dc.creatorRioja, M.
dc.creatorSakai, S.
dc.creatorSato, K.
dc.creatorSasao, T.
dc.creatorShibata, K. M.
dc.creatorShimizu, R.
dc.creatorSora, K.
dc.creatorSuda, H.
dc.creatorTamura, Y.
dc.creatorYamashita, K.
dc.date2005-05-10
dc.date.accessioned2026-07-07T02:17:35Z
dc.date.available2026-07-07T02:17:35Z
dc.descriptionWe report on the multi-epoch observations of H2O maser emission in star forming region OH 43.8-0.1 carried out with VLBI Exploration of Radio Astrometry (VERA). The large-scale maser distributions obtained by single-beam VLBI mapping reveal new maser spots scattered in area of 0.7 x 1.0 arcsec, in addition to a `shell-like' structure with a scale of 0.3 x 0.5 arcsec which was previously mapped by Downes et al.(1979). Proper motions are also obtained for 43 spots based on 5-epoch monitoring with a time span of 281 days. The distributions of proper motions show a systematic outflow in the north-south direction with an expansion velocity of ~8 km/s, and overall distributions of maser spots as well as proper motions are better represented by a bipolar flow plus a central maser cluster with a complex structure, rather than a shell with a uniform expansion such as those found in Cep A R5 and W75N VLA2. The distance to OH 43.8-0.1 is also estimated based on the statistical parallax, yielding D = 2.8 +/- 0.5 kpc. This distance is consistent with a near kinematic distance and rules out a far kinematics distance (~9 kpc), and the LSR velocity of OH 43.8-0.1 combined with the distance provides a constraint on the flatness of the galactic rotation curve, that there is no systematic difference in rotation speeds at the Sun and at the position of OH 43.8-0.1, which is located at the galacto-centric radius of ~6.3 kpc.
dc.description10 pages, 2 figures and 2 tables included, to appear in PASJ (vol. 57, #4, 2005, August)
dc.identifierhttps://arxiv.org/abs/astro-ph/0505180
dc.identifierhttp://arxiv.org/abs/astro-ph/0505180
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/9224
dc.subjectAstrophysics
dc.titleMulti-epoch VERA Observations of H2O masers in OH 43.8-0.1
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