259 research outputs found
The distance to a star forming region in the Outer arm of the Galaxy
We performed astrometric observations with the VLBA of WB89-437, an H2O maser
source in the Outer spiral arm of the Galaxy. We measure an annual parallax of
0.167 +/- 0.006 mas, corresponding to a heliocentric distance of 6.0 +/- 0.2
kpc or a Galactocentric distance of 13.4 +/- 0.2 kpc. This value for the
heliocentric distance is considerably smaller than the kinematic distance of
8.6 kpc. This confirms the presence of a faint Outer arm toward l = 135
degrees. We also measured the full space motion of the object and find a large
peculiar motion of ~20 km/s toward the Galactic center. This peculiar motion
explains the large error in the kinematic distance estimate. We also find that
WB89-437 has the same rotation speed as the LSR, providing more evidence for a
flat rotation curve and thus the presence of dark matter in the outer Galaxy.Comment: The Astrophysical Journal, accepted, 16 pages, 4 Figure
A model for soap film dynamics with evolving thickness
Previous research on animations of soap bubbles, films, and foams largely focuses on the motion and geometric shape of the bubble surface. These works neglect the evolution of the bubble’s thickness, which is normally responsible for visual phenomena like surface vortices, Newton’s interference patterns, capillary waves, and deformation-dependent rupturing of films in a foam. In this paper, we model these natural phenomena by introducing the film thickness as a reduced degree of freedom in the Navier-Stokes equations and deriving their equations of motion. We discretize the equations on a nonmanifold triangle mesh surface and couple it to an existing bubble solver. In doing so, we also introduce an incompressible fluid solver for 2.5D films and a novel advection algorithm for convecting fields across non-manifold surface junctions. Our simulations enhance state-of-the-art bubble solvers with additional effects caused by convection, rippling, draining, and evaporation of the thin film
Trigonometric Parallax of W51 Main/South
We report measurement of the trigonometric parallax of W51 Main/South using
the Very Long Baseline Array (VLBA). We measure a value of 0.185 +/- 0.010 mas,
corresponding to a distance of 5.41 (+0.31/-0.28) kpc. W51 Main/South is a
well-known massive star-forming region near the tangent point of the
Sagittarius spiral arm of the Milky Way. Our distance to W51 yields an estimate
of the distance to the Galactic center of Ro = 8.3 +/- 0.46 (statistical) +/-
1.0 (systematic) kpc by simple geometry. Combining the parallax and proper
motion measurements for W51, we obtained the full-space motion of this massive
star forming region. We find W51 is in a nearly circular orbit about the
Galactic center. The H2O masers used for our parallax measurements trace four
powerful bipolar outflows within a 0.4 pc size region, some of which are
associated with dusty molecular hot cores and/or hyper- or ultra-compact HII
regions.Comment: Accepted to ApJ; 32 pages; 6 tables; 5 figure
A Precise Distance to IRAS 00420+5530 via H2O Maser Parallax with the VLBA
We have used the VLBA to measure the annual parallax of the H2O masers in the
star-forming region IRAS 00420+5530. This measurement yields a direct distance
estimate of 2.17 +/- 0.05 kpc (<3%), which disagrees substantially with the
standard kinematic distance estimate of ~4.6 kpc (according to the rotation
curve of Brand and Blitz 1993), as well as most of the broad range of distances
(1.7-7.7 kpc) used in various astrophysical analyses in the literature. The
3-dimensional space velocity of IRAS 00420+5530 at this new, more accurate
distance implies a substantial non-circular and anomalously slow Galactic
orbit, consistent with similar observations of W3(OH) (Xu et al., 2006;
Hachisuka et al. 2006), as well as line-of-sight velocity residuals in the
rotation curve analysis of Brand and Blitz (1993). The Perseus spiral arm of
the Galaxy is thus more than a factor of two closer than previously presumed,
and exhibits motions substantially at odds with axisymmetric models of the
rotating Galaxy.Comment: 33 pages, 12 figures; Accepted by ApJ (to appear March 2009
Improved VLBI astrometry of OH maser stars
Aims: Accurate distances to evolved stars with high mass loss rates are
needed for studies of many of their fundamental properties. However, as these
stars are heavily obscured and variable, optical and infrared astrometry is
unable to provide enough accuracy.
Methods: Astrometry using masers in the circumstellar envelopes can be used
to overcome this problem. We have observed the OH masers of a number of
Asymptotic Giant Branch (AGB) stars for approximately 1 year with the Very Long
Baseline Array (VLBA). We have used the technique of phase referencing with
in-beam calibrators to test the improvements this technique can provide to Very
Long Baseline Interferometry (VLBI) OH maser astrometric observations.
Results: We have significantly improved the parallax and proper motion
measurements of the Mira variable stars U Her, S CrB and RR Aql.
Conclusions: It is shown that both in-beam phase-referencing and a decrease
in solar activity during the observations significantly improves the accuracy
of the astrometric observations. The improved distances to S CrB (418 +21 -18
pc) and RR Aql (633 +214 -128 pc) are fully consistent with published P-L
relations, but the distance to U Her (266 +32 -28 pc) is significantly smaller.
We conclude that for sources that are bright and have a nearby in-beam
calibrator, VLBI OH maser astrometry can be used to determine distances to OH
masing stars of up to ~2 kpc.Comment: 15 pages, 10 figures; accepted for publication in A&A; for a version
with high-resolution figures see
http://www.astro.uni-bonn.de/~wouter/papers/astrom/astrom.shtm
A Trigonometric Parallax of Sgr B2
We have measured the positions of water masers in Sgr B2, a massive star
forming region in the Galactic center, relative to an extragalactic radio
source with the Very Long Baseline Array. The positions measured at 12 epochs
over a time span of one year yield the trigonometric parallax of Sgr B2 and
hence a distance to the Galactic center of Ro=7.9 (+0.8/-0.7) kpc. The proper
motion of Sgr B2 relative to Sgr A* suggests that Sgr B2 is about 0.13 kpc
nearer than the Galactic center, assuming a low-eccentricity Galactic orbit.Comment: Submitted to ApJ; 4 tables; 3 figures. Version 2 corrects Fig. 2
which was missing some dat
Trigonometric Parallaxes of Massive Star Forming Regions: III. G59.7+0.1 and W 51 IRS2
We report trigonometric parallaxes for G59.7+0.1 and W 51 IRS2, corresponding
to distances of 2.16^{+0.10}_{-0.09} kpc and 5.1^{+2.9}_{-1.4} kpc,
respectively. The distance to G59.7+0.1 is smaller than its near kinematic
distance and places it between the Carina-Sagittarius and Perseus spiral arms,
probably in the Local (Orion) spur. The distance to W 51 IRS2, while subject to
significant uncertainty, is close to its kinematic distance and places it near
the tangent point of the Carina-Sagittarius arm. It also agrees well with a
recent estimate based on O-type star spectro/photometry. Combining the
distances and proper motions with observed radial velocities gives the full
space motions of the star forming regions. We find modest deviations of 5 to 10
km/s from circular Galactic orbits for these sources, both counter to Galactic
rotation and toward the Galactic center.Comment: 16 pages, 6 figures; to appear in the Astrophysical Journa
Trigonometric Parallaxes of 6.7 GHz Methanol Masers
Emission from the 6.7 GHz methanol maser transition is very strong, is
relatively stable, has small internal motions, and is observed toward numerous
massive star-forming regions in the Galaxy. Our goal is to perform
high-precision astrometry using this maser transition to obtain accurate
distances to their host regions. Eight strong masers were observed during five
epochs of VLBI observations with the European VLBI Network between 2006 June,
and 2008 March. We report trigonometric parallaxes for five star-forming
regions, with accuracies as good as as. Distances to these
sources are kpc for ON 1, kpc
for L 1206, kpc for L 1287,
kpc for NGC 281-W, and kpc for S 255. The distances and
proper motions yield the full space motions of the star-forming regions hosting
the masers, and we find that these regions lag circular rotation on average by
17 km s, a value comparable to those found recently by similar
studies.Comment: 17 pages, 21 figures, 5 tables, accepted for publication in A&A,
corrected typo
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