2,472 research outputs found
Proper Motions of H2O Masers in the Water Fountain Source IRAS 19190+1102
We report on the results of two epochs of Very Long Baseline Array (VLBA)
observations of the 22 GHz water masers toward IRAS 19190+1102. The water maser
emission from this object shows two main arc-shaped formations perpendicular to
their NE-SW separation axis. The arcs are separated by ~280 mas in position,
and are expanding outwards at an angular rate of 2.35 mas/yr. We detect maser
emission at velocities between -53.3 km/s to +78.0 km/s and there is a distinct
velocity pattern where the NE masers are blueshifted and the SW masers are
redshifted. The outflow has a three-dimensional outflow velocity of 99.8 km/s
and a dynamical age of about 59 yr. A group of blueshifted masers not located
along the arcs shows a change in velocity of more than 35 km/s between epochs,
and may be indicative of the formation of a new lobe. These observations show
that IRAS 19190+1102 is a member of the class of "water fountain"'
pre-planetary nebulae displaying bipolar structureComment: Accepted for publication in ApJ, corrected typo
The enigmatic B[e]-star Henize 2-90: The non-spherical mass loss history from an analysis of forbidden lines
(abridged) We study the optical spectrum of the exciting B[e] star Hen 2-90
based on new high-resolution observations that cover the innermost 2". Our
investigation is splitted in two parts, a qualitative study of the presence of
the numerous emission lines and the classification of their line profiles which
indicate a circumstellar environment of high complexity, and a quantitative
analysis of numerous forbidden lines, e.g. [OI], [OII], [OIII], [SII], [SIII],
[ArIII], [ClII], [ClIII] and [NII]. We find a correlation between the different
ionization states of the elements and the velocities derived from the line
profiles: the highly ionized atoms have the highest outflow velocity while the
neutral lines have the lowest outflow velocity. The recent HST image of Hen
2-90 reveals a bipolar, highly ionized region, a neutral disk-like structure
and an intermediate region of moderate ionization. It seems that a
non-spherical stellar wind model is a good option to explain the ionization and
spatial distribution of the circumstellar material. We modelled the forbidden
lines under the assumption of a non-spherically symmetric wind based on the HST
image. We find that in order to fit the observed line luminosities, the mass
flux, surface temperature, and terminal wind velocities need to be latitude
dependent, which might be explained in terms of a rapidly rotating central
star. A rotation speed of 75-80 % of the critical velocity has been derived.
The total mass loss rate of the star was determined to be of order 3 10^{-5}
M_sun/yr. Such a wind scenario and the fact that compared to solar abundances
C, O, and N seem to be underabundant while S, Ar and Cl have solar abundances,
might be explained in terms of a rapidly rotating post-AGB star.Comment: 16 pages, 13 figures, accepted for publication in A&A. Table 4 is
included at the end of the paper. This table will only be available in the
online version of the paper and will not appear in the printed versio
Shocked and Scorched: The Tail of a Tadpole in an Interstellar Pond
We report multi-wavelength observations of the far-infrared source IRAS
20324+4057, including high-resolution optical imaging with HST, and
ground-based near-infrared, millimeter-wave and radio observations. These data
show an extended, limb-brightened, tadpole-shaped nebula with a bright,
compact, cometary nebula located inside the tadpole head. Our molecular line
observations indicate that the Tadpole is predominantly molecular, with a total
gas mass exceeding 3.7 Msun. Our radio continuum imaging, and archival Spitzer
IRAC images, show the presence of additional tadpole-shaped objects in the
vicinity of IRAS 20324+4057 that share a common E-W head-tail orientation: we
propose that these structures are small, dense molecular cores that originated
in the Cygnus cloud and are now being (i) photoevaporated by the ultraviolet
radiation field of the Cyg OB2 No. 8 cluster located to the North-West, and
(ii) shaped by ram pressure of a distant wind source or sources located to the
West, blowing ablated and photoevaporated material from their heads eastwards.
The ripples in the tail of the Tadpole are interpreted in terms of
instabilities at the interface between the ambient wind and the dense medium of
the former.Comment: (accepted by the Astrophysical Journal
Dynamical Seasonal Prediction of Indian Summer Monsoon using AGCM: Weighted Ensemble Mean Approach
This study examines the fidelity of portable unified model's Atmospheric General Circulation Model in ensemble seasonal prediction of Indian Summer Monsoons of 1999-2004, driven by May SST anomaly persistent boundary conditions. Simple Ensemble-mean (EM) is inappropriate due to the presence of large deviation among the ensemble members in simulation of Indian Summer Monsoon Rainfall (ISMR). Thus 'Weighted Ensemble Mean' (WEM) method is used in the present study. In WEM method, weights are determined for all ensemble members at each model grid point using daily precipitation anomaly to distinguish the most reliable members and outliers among the ensemble members. Ensemble-mean then obtained by weighted combinations of all ensemble members is referred as 'Weighted Ensemble Mean'. The WEM prediction of ISMR better matches with observations than EM in majority of the monsoons. Further, WEM estimated using monthly and seasonal mean weights are assessed with respect to WEM from daily mean weights. WEM with monthly/seasonal weighting is found to be similar to EM in most of the monsoons and hence daily weighting is more suited approach than monthly/seasonal weighting
The Illumination and Growth of CRL 2688: An Analysis of New & Archival HST Observations
We present four-color images of CRL 2688 obtained in 2009 using the
Wide-Field Camera 3 on HST. The F606W image is compared with archival images in
very similar filters to monitor the proper motions of nebular structure. We
find that the bright N-S lobes have expanded uniformly by 2.5% and that the
ensemble of rings has translated radially by 0.07 in 6.65 y. The rings were
ejected every 100y for ~4 millennia until the lobes formed 250y ago. Starlight
scattered from the edges of the dark E-W dust lane is coincident with extant H2
images and leading tips of eight pairs of CO outflows. We interpret this as
evidence that fingers lie within geometrically opposite cones of opening angles
{\approx} 30{\circ} like those in CRL618. By combining our results of the rings
with 12CO absorption from the extended AGB wind we ascertain that the rings
were ejected at ~18 km s-1 with very little variation and that the distance to
CRL2688, v_{exp}{\dot\theta}_exp$, is 300 - 350 pc. Our 2009 imaging
program included filters that span 0.6 to 1.6{\mu}m. We constructed a
two-dimensional dust scattering model of stellar radiation through CRL2688 that
successfully reproduces the details of the nebular geometry, its integrated
spectral energy distribution, and nearly all of its color variations. The model
implies that the optical opacity of the lobes >~ 1, the dust particle density
in the rings decreases as radius^{-3} and that the mass and momentum of the AGB
winds and their rings have increased over time.Comment: (51 pages, 6 figures; accepted by ApJ
- …