Mapping observations were made towards IRAS 201109-3321 using the Nobeyama 45 m and the Delingha 13.7m radio telescopes. The high angular resolution （- 21″） image with the 45m telescope shows that there is a highve...Mapping observations were made towards IRAS 201109-3321 using the Nobeyama 45 m and the Delingha 13.7m radio telescopes. The high angular resolution （- 21″） image with the 45m telescope shows that there is a highvelocity bipolar molecular outflow in this region, which is in the NW-SE direction with a collimation factor of 2.2. The outflow has significantly higher mass loss rate and mechanical luminosity than those from low mass YSOs, indicating that the outflow is driven by the IRAS source. A dense massive core was detected by mapping C180 （J = 1 - 0） line in the area with the 13.7m telescope. The IRAS source lies within the core but slightly offsets from its emission peak.展开更多
IRAS 22475＋5939 has been we can still discover new characteristics well studied by previous astronomers, but about it, using the first observations of the lines from CO J=2-1, 13C0 J=2-1 and 13CO J=3-2 by the KOSMA 3...IRAS 22475＋5939 has been we can still discover new characteristics well studied by previous astronomers, but about it, using the first observations of the lines from CO J=2-1, 13C0 J=2-1 and 13CO J=3-2 by the KOSMA 3m telescope. The mapping of the intensity ratio of 13CO J=3-2 and 13CO J=2-1 shows that the distribution of the temperature has two peaks, neither of which coincide with the IRAS 22475＋5939 source or the center of the HII region, but rather are located at the edge of the HII region. Overlays of the Spitzer IRAC 8 p.m with CO contours indicate that they are associated with each other and that the strongest polycyclic aro- matic hydrocarbon （PAH） emission is at the IRAS 22475＋5939 source position. The IRAS LRS spectrum at 7μm-23 μm and the PHT-s spectrum at 2μm-12μm of the IRAS 22475＋5939 source also exhibit strong PAH emission characteristics in the main PAH bands： The diversity of the PAH family should be responsible for the plateaus in the PAH emission in the PHT-s and IRAS-LRS spectra. Analysis and mod- eling in the infrared bands suggest that IRAS 22475＋5939 is more likely to be a class I young stellar object. Where this is the case, the star is likely to have a tempera- ture of Tefr-9995.8K, mass-15.34Mo, luminosity -1.54×104 L- and age 1.54-104 yr. The model shows that circumstellar disc emission is important for wavelengths between 1 and 10μm, otherwise, the envelope fluctuates for A 〉 10μm. Bipolar outflow is confirmed in the molecular cloud, and the excited star of the HII region could be the driving source of the outflow. High resolution is required fm better results.展开更多
基金Supported in part by the National Natural Science Foundation of China under Grant No 10573029, and the 0ne Hundred Talents Programme of Chinese Academy of Sciences.
文摘Mapping observations were made towards IRAS 201109-3321 using the Nobeyama 45 m and the Delingha 13.7m radio telescopes. The high angular resolution （- 21″） image with the 45m telescope shows that there is a highvelocity bipolar molecular outflow in this region, which is in the NW-SE direction with a collimation factor of 2.2. The outflow has significantly higher mass loss rate and mechanical luminosity than those from low mass YSOs, indicating that the outflow is driven by the IRAS source. A dense massive core was detected by mapping C180 （J = 1 - 0） line in the area with the 13.7m telescope. The IRAS source lies within the core but slightly offsets from its emission peak.
文摘IRAS 22475＋5939 has been we can still discover new characteristics well studied by previous astronomers, but about it, using the first observations of the lines from CO J=2-1, 13C0 J=2-1 and 13CO J=3-2 by the KOSMA 3m telescope. The mapping of the intensity ratio of 13CO J=3-2 and 13CO J=2-1 shows that the distribution of the temperature has two peaks, neither of which coincide with the IRAS 22475＋5939 source or the center of the HII region, but rather are located at the edge of the HII region. Overlays of the Spitzer IRAC 8 p.m with CO contours indicate that they are associated with each other and that the strongest polycyclic aro- matic hydrocarbon （PAH） emission is at the IRAS 22475＋5939 source position. The IRAS LRS spectrum at 7μm-23 μm and the PHT-s spectrum at 2μm-12μm of the IRAS 22475＋5939 source also exhibit strong PAH emission characteristics in the main PAH bands： The diversity of the PAH family should be responsible for the plateaus in the PAH emission in the PHT-s and IRAS-LRS spectra. Analysis and mod- eling in the infrared bands suggest that IRAS 22475＋5939 is more likely to be a class I young stellar object. Where this is the case, the star is likely to have a tempera- ture of Tefr-9995.8K, mass-15.34Mo, luminosity -1.54×104 L- and age 1.54-104 yr. The model shows that circumstellar disc emission is important for wavelengths between 1 and 10μm, otherwise, the envelope fluctuates for A 〉 10μm. Bipolar outflow is confirmed in the molecular cloud, and the excited star of the HII region could be the driving source of the outflow. High resolution is required fm better results.
