Detection of 40-48 GHz dust continuum linear polarization towards the Class 0 young stellar object IRAS 16293-2422
文献类型：期刊论文
| 作者 | Liu, Hauyu Baobab1; Hasegawa, Yasuhiro2; Ching, Tao-Chung3; Lai, Shih-Ping4,5; Hirano, Naomi6; Rao, Ramprasad6 |
| 刊名 | ASTRONOMY & ASTROPHYSICS
 |
| 出版日期 | 2018-09-12 |
| 卷号 | 617页码:15 |
| 关键词 | radiation mechanisms: thermal stars: formation radio continuum: ISM ISM: magnetic fields |
| ISSN号 | 1432-0746 |
| DOI | 10.1051/0004-6361/201832699 |
| 英文摘要 | Aims. The aims of this work are to test the feasibility of observing dust polarization at frequencies lower than 50 GHz, which is the optically thinner part of the modified black body spectrum, and to clarify whether or not the polarization mechanism is identical or similar to that for (sub) millimeter observations. Methods. We performed the new Karl G. Jansky Very Large Array (JVLA) full polarization observations at 40-48 GHz (6.3-7.5 mm) towards the nearby (d = 147 +/- 3.4 pc) Class 0 young stellar object (YSO) IRAS 16293-2422, and compared these with the previous Submillimeter Array (SMA) observations. We observed the quasar J1407+2827, which is weakly polarized and can be used as a leakage term calibrator for <9 GHz observations, to gauge the potential residual polarization leakage after calibration. Results. We did not detect Stokes Q, U, and V intensities from the observations of J1407+2827, and constrain (3 sigma) the residual polarization leakage after calibration to be less than or similar to 0.3%. Limited by thermal noise, we only detected linear polarization from one of the two binary components of our target source, IRAS 16293-2422 B. The measured polarization percentages range from less than one percent to a few tens of percent. The derived polarization position angles from our observations are in excellent agreement with those detected from the previous observations of the SMA, implying that on the spatial scale we are probing (similar to 50-1000 au), the physical mechanisms for polarizing the continuum emission do not vary significantly over the wavelength range of similar to 0.88-7.5 mm. Conclusions. We hypothesize that the observed polarization position angles trace the magnetic field, which converges from large scale to an approximately face-on rotating accretion flow. In this scenario, magnetic field is predominantly poloidal on >100 au scales, and becomes toroidal on smaller scales. However, this interpretation remains uncertain due to the high dust optical depths at the central region of IRAS 16293-2422 B and the uncertain temperature profile. We suggest that dust polarization at wavelengths comparable or longer than 7 mm may still trace interstellar magnetic field. Future sensitive observations of dust polarization in the fully optically thin regime will have paramount importance for unambiguously resolving the magnetic field configuration. |
| WOS关键词 | MAGNETIC-FIELD ; PROTOPLANETARY DISKS ; HOT CORE ; POLARIMETRY ; EMISSION ; STAR ; IRAS-16293-2422 ; ALIGNMENT ; ALMA |
| 资助项目 | Smithsonian Institution ; Academia Sinica ; Jet Propulsion Laboratory, California Institute of Technology ; National Aeronautics and Space Administration ; Ministry of Science and Technology of Taiwan[MOST 106-2119-M-007-021-MY3] |
| WOS研究方向 | Astronomy & Astrophysics |
| 语种 | 英语 |
| WOS记录号 | WOS:000444602700003 |
| 出版者 | EDP SCIENCES S A |
| 资助机构 | Smithsonian Institution ; Smithsonian Institution ; Academia Sinica ; Academia Sinica ; Jet Propulsion Laboratory, California Institute of Technology ; Jet Propulsion Laboratory, California Institute of Technology ; National Aeronautics and Space Administration ; National Aeronautics and Space Administration ; Ministry of Science and Technology of Taiwan ; Ministry of Science and Technology of Taiwan ; Smithsonian Institution ; Smithsonian Institution ; Academia Sinica ; Academia Sinica ; Jet Propulsion Laboratory, California Institute of Technology ; Jet Propulsion Laboratory, California Institute of Technology ; National Aeronautics and Space Administration ; National Aeronautics and Space Administration ; Ministry of Science and Technology of Taiwan ; Ministry of Science and Technology of Taiwan ; Smithsonian Institution ; Smithsonian Institution ; Academia Sinica ; Academia Sinica ; Jet Propulsion Laboratory, California Institute of Technology ; Jet Propulsion Laboratory, California Institute of Technology ; National Aeronautics and Space Administration ; National Aeronautics and Space Administration ; Ministry of Science and Technology of Taiwan ; Ministry of Science and Technology of Taiwan ; Smithsonian Institution ; Smithsonian Institution ; Academia Sinica ; Academia Sinica ; Jet Propulsion Laboratory, California Institute of Technology ; Jet Propulsion Laboratory, California Institute of Technology ; National Aeronautics and Space Administration ; National Aeronautics and Space Administration ; Ministry of Science and Technology of Taiwan ; Ministry of Science and Technology of Taiwan |
| 源URL | [http://ir.bao.ac.cn/handle/114a11/22749]  |
| 专题 | 中国科学院国家天文台 |
| 通讯作者 | Liu, Hauyu Baobab |
| 作者单位 | 1.ESO, Karl Schwarzschild Str 2, D-85748 Garching, Germany 2.CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA 3.Chinese Acad Sci, Natl Astron Observ, Beijing, Peoples R China 4.Natl Tsing Hua Univ, Inst Astron, Hsinchu, Taiwan 5.Natl Tsing Hua Univ, Dept Phys, Hsinchu, Taiwan 6.Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan |
| 推荐引用方式 GB/T 7714 | Liu, Hauyu Baobab,Hasegawa, Yasuhiro,Ching, Tao-Chung,et al. Detection of 40-48 GHz dust continuum linear polarization towards the Class 0 young stellar object IRAS 16293-2422[J]. ASTRONOMY & ASTROPHYSICS,2018,617:15. |
| APA | Liu, Hauyu Baobab,Hasegawa, Yasuhiro,Ching, Tao-Chung,Lai, Shih-Ping,Hirano, Naomi,&Rao, Ramprasad.(2018).Detection of 40-48 GHz dust continuum linear polarization towards the Class 0 young stellar object IRAS 16293-2422.ASTRONOMY & ASTROPHYSICS,617,15. |
| MLA | Liu, Hauyu Baobab,et al."Detection of 40-48 GHz dust continuum linear polarization towards the Class 0 young stellar object IRAS 16293-2422".ASTRONOMY & ASTROPHYSICS 617(2018):15. |
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来源：国家天文台
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