Dust Polarization of Prestellar and Protostellar Sources in OMC-3
We present the Atacama Large Millimeter/submillimeter Array observations of linearly polarized 1.1 mm continuum emission at ∼0.″14 (55 au) resolution and CO ( J = 2−1) emission at ∼1.″5 (590 au) resolution toward one prestellar (MMS 4), four Class 0 (MMS 1, MMS 3, MMS 5, and MMS 6), one Class I (MMS...
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2024-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/ad182d |
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| author | Yuhua Liu Satoko Takahashi Masahiro Machida Kohji Tomisaka Josep Miquel Girart Paul T. P. Ho Kouichiro Nakanishi Asako Sato |
| author_facet | Yuhua Liu Satoko Takahashi Masahiro Machida Kohji Tomisaka Josep Miquel Girart Paul T. P. Ho Kouichiro Nakanishi Asako Sato |
| author_sort | Yuhua Liu |
| collection | DOAJ |
| description | We present the Atacama Large Millimeter/submillimeter Array observations of linearly polarized 1.1 mm continuum emission at ∼0.″14 (55 au) resolution and CO ( J = 2−1) emission at ∼1.″5 (590 au) resolution toward one prestellar (MMS 4), four Class 0 (MMS 1, MMS 3, MMS 5, and MMS 6), one Class I (MMS 7), and one flat-spectrum (MMS 2) sources in the Orion Molecular Cloud 3 region. The dust disk-like structures and clear CO outflows are detected toward all sources except for MMS 4. The diameters of these disk-like structures, ranging from 16 to 97 au, are estimated based on the deconvolved full width half maximum (FWHM) values obtained from the multi-Gaussian fitting. Polarized emissions are detected toward MMS 2, MMS 5, MMS 6, and MMS 7, while no polarized emission is detected toward MMS 1, MMS 3, and MMS 4. MMS 2, MMS 5, and MMS 7 show organized polarization vectors aligned with the minor axes of the disk-like structures, with mean polarization fractions ranging from 0.6% to 1.2%. The strongest millimeter source, MMS 6, exhibits complex polarization orientations and a remarkably high polarization fraction of ∼10% around the Stokes I peak, and 15%–20% on the arm-like structure, as reported by Takahashi et al. (2019). The origins of the polarized emission, such as self-scattering and dust alignment due to the magnetic field or radiative torque, are discussed for individual sources. Some disk-like sources exhibit a polarized intensity peak shift toward the nearside of the disk, which supports that the polarized emission originates from self-scattering. |
| format | Article |
| id | doaj-art-a4d17e4f548647a0bbc83df708c834ec |
| institution | DOAJ |
| issn | 1538-4357 |
| language | English |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-a4d17e4f548647a0bbc83df708c834ec2025-08-20T03:15:08ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01963210410.3847/1538-4357/ad182dDust Polarization of Prestellar and Protostellar Sources in OMC-3Yuhua Liu0https://orcid.org/0009-0009-2263-5502Satoko Takahashi1https://orcid.org/0000-0002-7287-4343Masahiro Machida2https://orcid.org/0000-0002-0963-0872Kohji Tomisaka3https://orcid.org/0000-0003-2726-0892Josep Miquel Girart4https://orcid.org/0000-0002-3829-5591Paul T. P. Ho5https://orcid.org/0000-0002-3412-4306Kouichiro Nakanishi6https://orcid.org/0000-0002-6939-0372Asako Sato7https://orcid.org/0000-0001-5817-6250Department of Earth and Planetary Sciences, Graduate School of Science, Kyushu University , Fukuoka 819-0395, Japan ; liu.yuhua.519@s.kyushu-u.ac.jpNational Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Astronomical Science Program, School of Physical Sciences, The Graduate University for Advanced Studies , SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanDepartment of Earth and Planetary Sciences, Faculty of Science, Kyushu University , Fukuoka 819-0395, JapanNational Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Astronomical Science Program, School of Physical Sciences, The Graduate University for Advanced Studies , SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanInstitut de Ciències de l’Espai (ICE, CSIC) , Can Magrans s/n, E-08193 Cerdanyola del Vallès, Catalonia, Spain; Institut d’Estudis Espacials de Catalunya (IEEC) , E-08034 Barcelona, Catalonia, SpainInstitute of Astronomy and Astrophysics , Academia Sinica, 11F of Astronomy-Mathematics Building, AS/NTU No. 1, Sec. 4, Roosevelt Rd, Taipei 10617, Taiwan, R.O.C.; East Asian Observatory , 660 N. A’ohoku Place, Hilo, HI 96720, USANational Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Astronomical Science Program, School of Physical Sciences, The Graduate University for Advanced Studies , SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanDepartment of Earth and Planetary Sciences, Graduate School of Science, Kyushu University , Fukuoka 819-0395, Japan ; liu.yuhua.519@s.kyushu-u.ac.jpWe present the Atacama Large Millimeter/submillimeter Array observations of linearly polarized 1.1 mm continuum emission at ∼0.″14 (55 au) resolution and CO ( J = 2−1) emission at ∼1.″5 (590 au) resolution toward one prestellar (MMS 4), four Class 0 (MMS 1, MMS 3, MMS 5, and MMS 6), one Class I (MMS 7), and one flat-spectrum (MMS 2) sources in the Orion Molecular Cloud 3 region. The dust disk-like structures and clear CO outflows are detected toward all sources except for MMS 4. The diameters of these disk-like structures, ranging from 16 to 97 au, are estimated based on the deconvolved full width half maximum (FWHM) values obtained from the multi-Gaussian fitting. Polarized emissions are detected toward MMS 2, MMS 5, MMS 6, and MMS 7, while no polarized emission is detected toward MMS 1, MMS 3, and MMS 4. MMS 2, MMS 5, and MMS 7 show organized polarization vectors aligned with the minor axes of the disk-like structures, with mean polarization fractions ranging from 0.6% to 1.2%. The strongest millimeter source, MMS 6, exhibits complex polarization orientations and a remarkably high polarization fraction of ∼10% around the Stokes I peak, and 15%–20% on the arm-like structure, as reported by Takahashi et al. (2019). The origins of the polarized emission, such as self-scattering and dust alignment due to the magnetic field or radiative torque, are discussed for individual sources. Some disk-like sources exhibit a polarized intensity peak shift toward the nearside of the disk, which supports that the polarized emission originates from self-scattering.https://doi.org/10.3847/1538-4357/ad182dPolarimetryDust continuum emissionYoung stellar objects |
| spellingShingle | Yuhua Liu Satoko Takahashi Masahiro Machida Kohji Tomisaka Josep Miquel Girart Paul T. P. Ho Kouichiro Nakanishi Asako Sato Dust Polarization of Prestellar and Protostellar Sources in OMC-3 The Astrophysical Journal Polarimetry Dust continuum emission Young stellar objects |
| title | Dust Polarization of Prestellar and Protostellar Sources in OMC-3 |
| title_full | Dust Polarization of Prestellar and Protostellar Sources in OMC-3 |
| title_fullStr | Dust Polarization of Prestellar and Protostellar Sources in OMC-3 |
| title_full_unstemmed | Dust Polarization of Prestellar and Protostellar Sources in OMC-3 |
| title_short | Dust Polarization of Prestellar and Protostellar Sources in OMC-3 |
| title_sort | dust polarization of prestellar and protostellar sources in omc 3 |
| topic | Polarimetry Dust continuum emission Young stellar objects |
| url | https://doi.org/10.3847/1538-4357/ad182d |
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