54 research outputs found
SiO Maser Survey off the Galactic Plane: A Signature of Streaming Motion
A group of Mira variables in the solar neighborhood show unusual spatial
motion in the Galaxy. To study this motion in a much larger scale in the
Galaxy, we newly surveyed 134 evolved stars off the Galactic plane by SiO maser
lines, obtaining accurate radial velocities of 84 detected stars. Together with
the past data of SiO maser sources, we analyzed the radial velocity data of a
large sample of sources distributing in a distance range of about 0.3 -- 6 kpc
in the first Galactic quadrant. At the Galactic longitudes between 20 and 40
deg, we found a group of stars with large negative radial velocities, which
deviate by more than 100 km s^{-1} from the Galactic rotation. We show that
these deviant motions of maser stars are created by periodic gravitational
perturbation of the Bulge bar, and that the effect appears most strongly at
radii between corotation and outer Lindblad resonances. The resonance effect
can explain the displacement of positions from the Galactic plane as well.Comment: 14 pages, 11 figures, PASJ, 62. No. 3 in press high resolution
figures available from
http://www.nro.nao.ac.jp/~lib_pub/report/data/no675.pd
A Search for Water Masers in the Saturnian System
We searched for H2O 6(1,6)-5(2,3) maser emission at 22.235 GHz from several
Saturnian satellites with the Nobeyama 45m radio telescope in May 2009.
Observations were made for Titan, Hyperion, Enceladus and Atlas, for which
Pogrebenko et al. (2009) had reported detections of water masers at 22.235 GHz,
and in addition for Iapetus and other inner satellites. We detected no emission
of the water maser line for all the satellites observed, although sensitivities
of our observations were comparable or even better than those of Pogrebenko et
al.. We infer that the water maser emission from the Saturnian system is
extremely weak, or sporadic in nature. Monitoring over a long period and
obtaining statistical results must be made for the further understanding of the
water maser emission in the Saturnian system.Comment: 8 pages, 2 figures, accepted for publication in PASJ (Letter
Interaction between Northern Coal Sack in the Cyg OB 7 cloud complex and the multiple super nova remnants including HB 21
We report possible interaction between multiple super nova remnants (SNRs)
and Northern Coal Sack (NCS) which is a massive clump (~1000 Mo) in the Cyg OB
7 cloud complex and is forming a massive Class 0 object. We performed molecular
observations of the 12CO(J=1-0), 13CO(J=1-0), and C18O(J=1-0) emission lines
using the 45m telescope at the Nobeyama Radio Observatory, and we found that
there are mainly four velocity components at Vlsr=-20, -6, -4, and 10 km/s. The
-6 and -4 km/s components correspond to the systemic velocities of NCS and the
Cygnus OB 7 complex, respectively, and the other velocity components originate
from distinct smaller clouds. Interestingly, there are apparent correlations
and anti-correlations among the spatial distributions of the four components,
suggesting that they are physically interacting with one another. On a larger
scale, we find that a group of small clouds belonging to the -20 and 10 km/s
components are located along two different arcs around some SNRs including HB
21 which has been suggested to be interacting with the Cyg OB 7 cloud complex,
and we also find that NCS is located right at the interface of the arcs. The
small clouds are likely to be the gas swept up by the stellar wind of the
massive stars which created the SNRs. We suggest that the small clouds alined
along the two arcs recently encountered NCS and the massive star formation in
NCS was triggered by the strong interaction with the small clouds.Comment: To appear in the Publications of the Astronomical Society of Japan
(PASJ
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