Two-component Magnetic Field along the Line of Sight to the Perseus Molecular Cloud: Contribution of the Foreground Taurus Molecular Cloud

• Published in: The Astrophysical journal Vol. 914; no. 2; pp. 122 - 137
• Main Authors: Doi, Yasuo, Hasegawa, Tetsuo, Bastien, Pierre, Tahani, Mehrnoosh, Arzoumanian, Doris, Coudé, Simon, Matsumura, Masafumi, Sadavoy, Sarah, Hull, Charles L. H., Shimajiri, Yoshito, Furuya, Ray S., Johnstone, Doug, Plume, Rene, Inutsuka, Shu-ichiro, Kwon, Jungmi, Tamura, Motohide
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01.06.2021; IOP Publishing; American Astronomical Society
• Subjects: Astrophysics; Dust; Dust clouds; Interstellar clouds; Interstellar magnetic fields; Line of sight; Magnetic fields; Molecular clouds; Polarimetry; Polarization; Sciences of the Universe; Starlight polarization; Starlight polarization; Astrophysics - Astrophysics of Galaxies; 1278; Interstellar magnetic fields; 834; 1571; 845; Interstellar clouds; Polarimetry
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/abfcc5

Abstract Optical stellar polarimetry in the Perseus molecular cloud direction is known to show a fully mixed bimodal distribution of position angles across the cloud. We study the Gaia trigonometric distances to each of these stars and reveal that the two components in position angles trace two different dust clouds along the line of sight. One component, which shows a polarization angle of −37.°6 ± 35.°2 and a higher polarization fraction of 2.0 ± 1.7 %, primarily traces the Perseus molecular cloud at a distance of 300 pc. The other component, which shows a polarization angle of +66.°8 ± 19.°1 and a lower polarization fraction of 0.8 ± 0.6 %, traces a foreground cloud at a distance of 150 pc. The foreground cloud is faint, with a maximum visual extinction of ≤1 mag. We identify that foreground cloud as the outer edge of the Taurus molecular cloud. Between the Perseus and Taurus molecular clouds, we identify a lower-density ellipsoidal dust cavity with a size of 100–160 pc. This dust cavity is located at l = 170°, b = −20°, and d = 240 pc, which corresponds to an H I shell generally associated with the Per OB2 association. The two-component polarization signature observed toward the Perseus molecular cloud can therefore be explained by a combination of the plane-of-sky orientations of the magnetic field both at the front and at the back of this dust cavity.