75 research outputs found
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
Class I methanol masers in low-mass star formation regions
Four Class I maser sources were detected at 44, 84, and 95 GHz toward
chemically rich outflows in the regions of low-mass star formation NGC 1333I4A,
NGC 1333I2A, HH25, and L1157. One more maser was found at 36 GHz toward a
similar outflow, NGC 2023. Flux densities of the newly detected masers are no
more than 18 Jy, being much lower than those of strong masers in regions of
high-mass star formation. The brightness temperatures of the strongest peaks in
NGC 1333I4A, HH25, and L1157 at 44 GHz are higher than 2000 K, whereas that of
the peak in NGC 1333I2A is only 176 K. However, rotational diagram analysis
showed that the latter source is also a maser. The main properties of the newly
detected masers are similar to those of Class I methanol masers in regions of
massive star formation. The former masers are likely to be an extension of the
latter maser population toward low luminosities of both the masers and the
corresponding YSOs.Comment: 5 pages, 1 figure, Proc. IAU Symp. 287 "Cosmic Masers: from OH to
H0". LSR velocities of the HH25 masers, which are presented in Table 1, are
correcte
Non-equilibrium excitation of methanol in Galactic molecular clouds: multi-transitional observations at 2 mm
We observed 14 methanol transitions near lambda=2 mm in Galactic star-forming
regions. Broad, quasi-thermal J(0)-J(-1)E methanol lines near 157 GHz were
detected toward 73 sources. Together with the 6(-1)-5(0)E and 5(-2)-6(-1)E
lines at 133 GHz and the 7(1)-7(0)E line at 165 GHz, they were used to study
the methanol excitation. In the majority of the observed objects, the Class I
6(-1)-5(0)E transition is inverted, and the Class II 5(-2)-6(-1)E and
6(0)-6(-1)E transitions are overcooled. This is exactly as predicted by models
of low gain Class I masers. The absence of the inversion of Class II
transitions 5(-2)-6(-1)E and 6(0)-6(-1)E means that quasi-thermal methanol
emission in all objects arises in areas without a strong radiation field, which
is required for the inversion.Comment: 23 pages paper (uses aasms4.sty), 12 pages tables (uses apjpt4.sty),
10 Jpeg figures, submitted to the ApJ
Spectral Survey of the Star Formation Region DR21OH in the 4 mm Wavelength Range
The results of a spectral survey of the region of massive star formation
DR21OH in the 4-mm wavelength range are presented. Sixty-nine molecules and
their isotopologues have been detected, ranging from simple diatomic or
triatomic species such as SO, SiO and CCH, to complex organic molecules such as
CHOCHO or CHOCH. The obtained results qualitatively repeat the
results of the survey of the same source at 3~mm. The inventories of molecules
found at 3mm and 4mm overlap to a great extent. However, at 4 mm we found a
number of species that have no allowed transitions in the 3-mm wavelength
range, e.g. DCN, DNC, or SO. The bulk of the molecules detected at 4~mm are
those that are common for dense cores, e.g., HCN or CHCCH, but some of
the detected species are typical for hot cores. The latter include complex
organic molecules CHOCHO, CHCHOH, CHOCH, etc. However, the
detected emission of these molecules probably arises in a gas heated to 30 K
only. Nine molecules, including complex species CHCN, CHCHCN,
CHCOCH, were found by spectral line stacking. This demonstrates the
prospects of the method in the study of molecular clouds.Comment: 36 pages, 4 figure
The detection of Class I methanol masers towards regions of low-mass star formation
Six young bipolar outflows in regions of low-to-intermediate-mass star
formation were observed in the 7_0-6_1A+, 8_0-7_1A+, and 5_{-1}-4_0E methanol
lines at 44, 95, and 84 GHz, respectively. Narrow features were detected
towards NGC 1333IRAS4A, HH 25MMS, and L1157 B1. Flux densities of the detected
lines are no higher than 11 Jy, which is much lower than the flux densities of
strong maser lines in regions of high-mass star formation. Analysis shows that
most likely the narrow features are masers.Comment: 12 pages, 6 figures, to be published in Astronomy Report
Modeling of the formation of complex molecules in protostellar objects
The results of molecular composition modeling are presented for the well studied low-mass star-forming region TMC-1 and the massive star-forming region DR21(OH), which is poorly studied from a chemical point of view. The column densities of dozens of molecules, ranging from simple diatomic to complex organic molecules, are reproduced to within an order of magnitude using a one-dimensional model for the physical and chemical structure of these regions. The chemical ages of the regions are approximately 105 years in both cases. The main desorption mechanisms that are usually included in chemical models (photodesorption, thermal desorption, and cosmic-ray-induced desorption) do not provide sufficient gasphase abundances of molecules that are synthesized in surface reactions; however, this shortcoming can be removed by introducing small amount of reactive desorption into the model. It is possible to reproduce the properties of the TMC-1 chemical composition in a standard model, without requiring additional assumptions about an anomalous C/O ratio or the recent accretion of matter enriched with atomic carbon, as has been proposed by some researchers. © 2013 Pleiades Publishing, Ltd
- …