2,443 research outputs found
A multi-transition submillimeter water maser study of evolved stars - detection of a new line near 475 GHz
Context: Maser emission from the H2O molecule probes the warm, inner
circumstellar envelopes of oxygen-rich red giant and supergiant stars.
Multi-maser transition studies can be used to put constraints on the density
and temperature of the emission regions.
Aims: A number of known H2O maser lines were observed toward the long period
variables R Leo and W Hya and the red supergiant VY CMa. A search for a new,
not yet detected line near 475 GHz was conducted toward these stars.
Methods: The Atacama Pathfinder Experiment telescope was used for a
multi-transition observational study of submillimeter H2O lines.
Results: The 5_33-4_40 transition near 475 GHz was clearly detected toward VY
CMa and W Hya. Many other H2O lines were detected toward all three target
stars. Relative line intensity ratios and velocity widths were found to vary
significantly from star to star.
Conclusions: Maser action is observed in all but one line for which it was
theoretically predicted. In contrast, one of the strongest maser lines, in R
Leo by far the strongest, the 437 GHz 7_53-6_60 transition, is not predicted to
be inverted. Some other qualitative predictions of the model calculations are
at variance with our observations. Plausible reasons for this are discussed.
Based on our findings for W Hya and VY CMa, we find evidence that the H2O
masers in the AGB star W Hya arise from the regular circumstellar outflow,
while shock excitation in a high velocity flow seems to be required to excite
masers far from the red supergiant VY CMa.Comment: 9 pages, 4 figures, Astronomy and Astrophyics (in press
Aluminium oxide in the optical spectrum of VY Canis Majoris
We report the first identification of the optical bands of the B-X system of
AlO in the red supergiant VY CMa. In addition to TiO, VO, ScO, and YO, which
were recognized in the optical spectrum of the star long time ago, AlO is
another refractory molecule which displays strong emission bands in this
peculiar star. Simulating the bands of AlO, we derive a rotational temperature
of the circumstellar gas of Trot=700K. By resolving individual rotational
components of the bands, we derive the kinematical characteristics of the gas,
finding that the emission is centered at the stellar radial velocity and its
intrinsic width is 13.5 km/s (full width at half maximum). It is the narrowest
emission among all (thermal) features observed in VY CMa so far. The
temperature and line widths suggest that the emission arises in gas located
within ~20 stellar radii, where the outflow is still being accelerated. This
result contradicts equilibrium-chemistry models which predict substantial AlO
abundances only to within a few stellar radii. We argue that non-equilibrium
models involving propagation of shocks are needed to explain the observations.Comment: to appear in A&
New Measurements of the Radio Photosphere of Mira based on Data from the JVLA and ALMA
We present new measurements of the millimeter wavelength continuum emission
from the long period variable Mira ( Ceti) at frequencies of 46 GHz, 96 GHz,
and 229 GHz (~7 mm, 3 mm, and 1 mm) based on observations obtained
with the Jansky Very Large Array (JVLA) and the Atacama Large
Millimeter/submillimeter Array (ALMA). The measured millimeter flux densities
are consistent with a radio photosphere model derived from previous
observations, where flux density, . The stellar disk
is resolved, and the measurements indicate a decrease in the size of the radio
photosphere at higher frequencies, as expected if the opacity decreases at
shorter wavelengths. The shape of the radio photosphere is found to be slightly
elongated, with a flattening of ~10-20%. The data also reveal evidence for
brightness non-uniformities on the surface of Mira at radio wavelengths. Mira's
hot companion, Mira B was detected at all three observed wavelengths, and we
measure a radius for its radio-emitting surface of
cm. The data presented here highlight the power of the JVLA and ALMA for the
study of the atmospheres of evolved stars.Comment: Accepted to ApJ; 27 pages, 7 figure
The cometary HII regions of DR 21: Bow shocks or champagne flows or both?
We present deep Very Large Array H66 radio recombination line (RRL)
observations of the two cometary HII regions in DR 21. With these sensitive
data, we test the "hybrid" bow shock/champagne flow model previously proposed
for the DR 21 HII regions. The ionized gas down the tail of the southern HII
region is redshifted by up to ~30 km/s with respect to the ambient molecular
gas, as expected in the hybrid scenario. The RRL velocity structure, however,
reveals the presence of two velocity components in both the northern and
southern HII regions. This suggests that the ionized gas is flowing along
cone-like shells, swept-up by stellar winds. The observed velocity structure of
the well-resolved southern HII region is most consistent with a picture that
combines a stellar wind with stellar motion (as in bow shock models) along a
density gradient (as in champagne flow models). The direction of the implied
density gradient is consistent with that suggested by maps of dust continuum
and molecular line emission in the DR 21 region.Comment: 22 pages, 9 figures, 2 tables, accepted for publication in A&
Detection of a new methanol maser line with the Kitt Peak 12-m telescope by remote observing from Moscow
A new methanol maser line 6(-1)-5(0)E at 133 GHz was detected with the 12-m
Kitt Peak radio telescope using remote observation mode from Moscow. Moderately
strong, narrow maser lines were found in DR21(OH), DR21-W, OMC-2, M8E, NGC2264,
L379, W33-Met. The masers have similar spectral features in other transitions
of methanol-E at 36 and 84 GHz, and in transitions of methanol-A at 44 and 95
GHz. All these are Class I transitions, and the new masers also belong to Class
I. In two other methanol transitions near 133 GHz, 5(-2)-6(-1)E and
6(2)-7(1)A+, only thermal emission was detected in some sources. Several other
sources with wider lines in the transition 6(-1)-5(0)E also may be masers,
since they do not show any emission at the two other methanol transitons near
133 GHz. These are NGC2071, S231, S255, GGD27, also known as Class I masers.
The ratio of intensities and line widths of the 133 GHz masers and 44 GHz
masers is consistent with the saturated maser model, in which the line
rebroadening with respect to unsaturated masers is suppressed by cross
relaxation due to elastic collisions.Comment: 4 pages, AASTeX text, uses aasms4.sty, 2 Postscript figures, to be
published in Ap
Exciting Maser Science with New Instruments - the Promise of the EVLA
In the near future, the Expanded Very Large Array (EVLA) will allow surveys
for maser sources with unprecedented sensitivity, spectral coverage and
spectroscopic capabilities. In particular, comprehensive surveys for many maser
species with simultaneous sensitive continuum imaging and absorption studies
will give a comprehensive radio picture of star formation in the Galactic plane
and elsewhere. Very efficient EVLA surveys for H2O megamasers in Active Galacic
Nuclei will be possible to practically arbitrary redshifts.
EVLA and Atacama Large Millimeter Array (ALMA) studies of H2O and SiO masers
will serve as high resolution probes of the innermost envelopes of oxygen-rich
evolved stars and HCN masers of carbon-rich stars.
Farther in the future, the Square Kilometer Array (SKA) promises the
detection of OH gigamasers at all conceivable redshifts and maser astrometry
with unprecedented accuracy.Comment: 10 pages, incl. 4 figures, iaus.cls, to appear the Procedings of IAU
Symp. 242 (Astrophysical masers and their environments) eds. J. Chapman & W.
Baan Replaced version with a few typos correcte
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