Measurements for the Performance of the Digital Autocorrelation Spectrometer

Injecting phase calibration (PCAL) signals to the feed horn of the observation sys- tem and analyzing the output response signals of the spectrometer, we measured the working performance of a 4096-channel digital autocalibration spectrometer. The results demonstrate that the spectrometer has a fine working performance: (1) the channels are distributed uni- formly in the spectrometer; (2) line drift produces little effect on the observation results; (3) spectral resolution shows little changes with observation time. The distribution of the fre- quency resolution in an 80 MHz bandwidth was measured. A trial observation on the two molecular spectral lines of H2CO and H110α taken with this spectrometer is described.     

~(12)CO,~(13)CO and C~(18)O observations along the major axes of nearby bright infrared galaxies

We present simultaneous observations of 12CO,13CO and C18O J=1-0 emission in 11 nearby(cz<1000 km s-1) bright infrared galaxies.Both 12CO and 13CO are detected in the centers of all the galaxies,except for 13CO in NGC 3031. We have also detected C18O,CSJ=2-1 and HCO+J=1-0 emission in the nuclear regions of M82 and M51.These are the first systematical extragalactic detections of 12CO and its isotopes from the PMO 14 m telescope.We have conducted half-beam-spaced mapping of M82 over an area of 4×2.5 and major...     

Molecular Cores in Different Evolutionary Stages near Luminous IRAS Sources and UC HII Regions

We report the results of 12CO and 13CO J=1–0 observations of eight candidates of Ultra-Compact (UC) HII regions with the Purple Mountain Observatory (PMO) Qinghai 13.7-m telescope, which resulted in revealing 11 molecular cores. Their masses range from 130 to 1.7×104 M , with different spatial scales (1 ～ 6 pc). Also presented are the relevant HCO J=1–0 maps, which enabled us to investigate more detailed structures of these cores. Further comparisons show that four of the cores deviated from the centers of infrared (MIR) emission of Midcourse Space Experiment (MSX), while others correspond either to bright MIR sources or diffuse MIR background. This indicates various evolutionary phases of the cores, including quite early ones for those without MIR sources.     

Pilot HI survey of Planck Galactic Cold Clumps with FAST

We present a pilot HI survey of 17 Planck Galactic Cold Clumps(PGCCs)with the Five-hundred-meter Aperture Spherical radio Telescope(FAST).HI Narrow Self-Absorption(HINSA)is an effective method to detect cold HI being mixed with molecular hydrogen H2 and improves our understanding of the atomic to molecular transition in the interstellar medium.HINSA was found in 58%PGCCs that we observed.The column density of HINSA was found to have an intermediate correlation with that of 13CO,following log(N(HINSA))=(0.52±0.26)log(N13CO)+(10±4.1).HI abundance relative to total hydrogen[HI]/[H]has an average value of 4.4×10-3,which is about 2.8 times of the average value of previous HINSA surveys toward molecular clouds.For clouds with total column density NH>5×1020 cm-2,an inverse correlation between HINSA abundance and total hydrogen column density is found,confirming the depletion of cold HI gas during molecular gas formation in more massive clouds.Nonthermal line width of 13CO is about 0-0.5 kms-1 larger than that of HINSA.One possible explanation of narrower non-thermal width of HINSA is that HINSA region is smaller than that of 13CO.Based on an analytic model of H2 formation and H2 dissociation by cosmic ray,we found the cloud ages to be within 106.7-107.0 yr for five sources.     

Multiwavelength study of low-luminosity 6.7-GHz methanol masers

We present results of 13CO(1-0),C18O(1-0),and HCO+(1-0) map observations and N2H+(1-0) single point observations directed towards a sample of nine low-luminosity 6.7-GHz masers.N2H + line emission has been detected from six out of nine sources,C18O line emission has been detected from eight out of nine sources,and HCO + and 13CO emission has been detected in all sources.In particular,a blue profile of the HCO + spectrum,a signature of inflow,is found towards one source.From integrated intensity emission map...     

Associations of decimetric type Ⅲ bursts with coronal mass ejections and Hα flares

We present a statistical study of decimetric type Ⅲ radio bursts,coronal mass ejections(CMEs),and Hα flares observed in the period from July 2000 to March2005.In total,we investigated 395 decimetric type Ⅲ radio burst events,21% of which showed apparent correlation to CMEs that were associated with Hα flares.We noticed that the Hα flares which were strongly associated with CMEs were gradual events,and82% of them took place before CMEs appeared in the field of view of LASCO C2;that most of the CME-associated radio bursts started in the frequency range around750 MHz with a frequency drifting rate of several hundred MHz s-1,of which both positive and negative ones were recognized; and that the correlation of type Ⅲ radio bursts to CMEs without associated flares is fairly vague,less than 9%.     

Submillimeter/millimeter observations of the high-mass star forming region IRAS 22506+5944

The mapping observations of CO J = 2-1, CO J = 3-2, 13 CO J = 2-1 and 13 CO J = 3-2 lines in the direction of IRAS 22506+5944 have been made. The results show that the cores in the J = 2-1 transition lines have a similar morphology to those in the J = 3-2 transition lines. Bipolar molecular outflows are verified. The prior IRAS 22506+5944 observations indicated that two IRAS sources and three H 2 O masers were located close to the peak position of the core. One of the IRAS sources may be the driving source ...     

Formation of cyanoallene （buta-2, 3-dienenitrile） in theinterstellar medium： a quantum chemical and spectroscopicstudy

The interstellar medium, filling the vast space between stars, is a rich reser-voir of molecular material ranging from simple diatomic molecules to more com-plex, astrobiologically important molecules such as vinylcyanide, methylcyanodiac-cetylene, cyanoaUene, etc. Interstellar molecular cyanoallene is one of the most stableisomers of methylcynoacetylene. An attempt has been made to explore the possibilityof forming cyanoallene in interstellar space by radical-radical and radical-moleculeinteraction schemes in the gaseous phase. The formation of cyanoallene starting fromsome simple, neutral interstellar molecules and radicals has been studied using densityfunctional theory. The reaction energies and structures of the reactants and productsshow that the formation of cyanoallene is possible in the gaseous phase. Both of theconsidered reaction paths are totally exothermic and barrierless, thus giving rise to ahigh probability of occurrence. Rate constants for each step in the formation processof cyanoallene in both the reaction paths are estimated. A full vibrational analysishas been attempted for cyanoallene in the harmonic and anharmonic approximations.Anharmonic spectroscopic parameters such as rotational constants, rotation-vibrationcoupling constants and centrifugal distortion constants have been calculated.     

CO Clouds around SNR G21.8-0.6 and G32.8-0.1

We made the first CO(I—0) mapping to SNR G21.8-0.6 and SNR G32.8-0.1, both associated with OH 1720 MHz maser.Based on the morphological correspondence and velocity and position agreement between the radio remnant and the CO clouds,we tentatively identify the clouds that are respectively interacting with the two SNRs.     

Submillimeter/millimeter observations of the molecular clouds associated with Tycho's supernova remnant

We have carried out CO J = 2-1 and CO J = 3-2 observations toward Tycho's supernova remnant(SNR) using the KOSMA 3m-telescope.From these observations,we identified three molecular clouds(MCs) around the SNR.The small cloud in the southwest was discovered for the first time.In the north and east,two MCs(Cloud A and Cloud B) adjacent in space display a bow-shaped morphology,and have broad emission lines,which provide some direct evidences of the SNR-MCs interaction.The MCs are revealed at-69--59 km s-1,coinci...     

Possible radio precursors/signatures of the CMEs onset:radio type Ⅲ bursts and fine structures in the centimeter-metric wavelength region

Seventy-one occurrences of coronal mass ejections(CMEs) associated with radio bursts,seemingly associated with type Ⅲ bursts/fine structures(FSs),in the centimeter-metric frequency range during 2003-2005,were obtained with the spectrometers at the National Astronomical Observatories,Chinese Academy of Sciences(NAOC) and the Culgoora radio spectrometer and are presented.The statistical results of 68 out of 71 events associated with the radio type III bursts or FSs during the initiation or early stages of the...     

A Survey and Statistics of Interstellar OH and H_2O Masers

We present a statistical analysis of a sky survey of interstellar H2O and OH masers. These masers can be classified into three categories: isolated H2O masers, isolated OH masers, and simple OH/H2O maser associations. The total number of sources in each category is of the same order of magnitude, and as an evolutionary phase they can maintain -105 yr. An improved radiative pumping mechanism is proposed. This model avoids some of the deficiencies of previous radiative models, such as shortage of exciting photons. The statistical results obtained from the survey can be interpreted by the new mechanism together with the evolutionary model in which the gravitational force of the central stellar objects is responsible for the HII region.     

H2CO and H110α observations towards NH3 sources

We observed the H₂CO(1₁₀–1₁₁) absorption lines and H_110α radio recombination lines (RRL) toward 180 NH₃ sources using the Nanshan 25-m radio telescope. In our observation, 138 sources were found to have H₂CO lines and 36 have H_110α RRLs. Among the 138 detected H₂CO sources, 38 sources were first detected. The detection rates of H₂CO have a better correlation with extinction than with background continuum radiation. Line center velocities of H₂CO and NH₃ agree well. The line width ratios of H₂CO and NH₃ are generally larger than unity and are similar to that of ¹³CO. The correlation between column densities of H₂CO and extinction is better than that between NH₃ and extinction. These line width relation and column density relation indicate H₂CO is distributed on a larger scale than that of NH₃, being similar to the regions of ¹³CO. The abundance ratios between NH₃ and H₂CO were found to be different in local clouds and other clouds.     

A Search for High—velocity Gas Associated H2O Masers and Ultracompact HⅡ Regions

With the objective of studying the relationships between high-velocity gas and water maser emission the results of a search from 95 IRAS sources for high-velocity gas associated with star forming molecular clouds are reported. 21 sources have been identified as molecular outflow candidates.     

Multifrequency emission analysis of TeV blazars H 2356–309 and 1ES 1218+304

The multiband nonthermal emissions in radio, X-ray, and very high-energy(VHE) γ-ray bands from two distant blazars, H 2356–309 and 1ES 1218+304, havebeen detected, and, especially from recent observations with the Suzaku, MAGICand VERITAS telescopes, clearly reveal nonthermal power-law spectra. We study thebroadband nonthermal spectra of the two sources by using a combination of a one-zone homogeneous synchrotron self-Compton (SSC) model and an inhomogeneousconical jet model, where the new external backgrou...     

Searches for HH-objects and emission stars in star-formation regions. VIII. Stars with Hα emission in the vicinity of the nebula GM 2-41

43 stellar objects with Hα emission are discovered by slitless spectroscopy in a 14’ × 14' area near the nebula GM 2-41 located in the HII region DR 15 at the southern edge of the Cyg OB2 association. Emission is detected for the first time for 30 of these objects. Based on VI and JHK photometric data, the overwhelming majority of these objects are classified as young stellar objects in spectral classes F7-M3 with ages of ~1 Myr. The stars are distributed nonuniformly and form two groups which have the same coordinates as the UCHII regions G0.79 + 0.3 and G79.2 + 0.4.