We made R-band polarization measurements of 234 stars towards the direction of MBM 33-39 cloud complex. The distance of MBM 33-39 complex was determined as $120\pm10$ pc using polarization results and near-infrared photometry from the 2MASS survey. The magnetic field geometry of the individual cloud inferred from our polarimetric results reveals that the field lines are in general consistent with the global magnetic field geometry of the region obtained from the previous studies. This implies that the clouds in the complex are permeated by the interstellar magnetic field. Multi-wavelength polarization measurements of a few stars projected on the complex suggest that the size of the dust grains in these clouds is similar to those found in the normal interstellar medium of the Milky Way. We studied a possible formation scenario of MBM 33-39 complex by combining the polarization results from our study and from the literature and by identifying the distribution of ionized, atomic and molecular (dust) components of material in the region.
B-Fields and Star Formation across Scales with TRAO (B-FROST): CO Abundances, Dynamics and Relative Orientations in the Translucent High Latitude Cloud MBM12
University of Helsinki（赫尔辛基大学）；Institut UTINAM – UMR 6213 – CNRS – Univ. Bourgogne Franche Comté（UTINAM研究所-法国国家科学研究中心-勃艮第弗朗什孔泰大学）；Ecole Normale Supérieure, Université PSL, CNRS, Sorbonne Université, Université de Paris（巴黎高等师范学院、巴黎文理研究大学、法国国家科学研究中心、索邦大学、巴黎大学）；IRAP, Université de Toulouse, CNRS（图卢兹大学空间物理研究所、法国国家科学研究中心）；Nazarbayev University（纳扎尔巴耶夫大学）；Nanjing University（南京大学）；Key Laboratory of Modern Astronomy and Astrophysics (Nanjing), Ministry of Education（教育部现代天文与天体物理重点实验室（南京））；Korea Astronomy and Space Science Institute（韩国天文与空间科学研究院）；Seoul National University（首尔国立大学）；University of Science and Technology, Korea (UST)（韩国科学技术院）
HI, CO, and Planck/IRAS dust properties in the high-latitude-cloud complex, MBM 53, 54, 55 and HLCG 92-35; Possible evidence for an optically thick HI envelope around the CO clouds
Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. II. Mass Mapping and Overdensity Characterization
IPAC, California Institute of Technology（加州理工学院 IPAC）；Korea Astronomy and Space Science Institute (KASI)（韩国天体宇宙科学研究所）；SPACE Institute, University of California（加州大学 SPACE 研究所）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天文研究所）；Department of Physics, Duke University（杜克大学物理系）；Department of Astronomy, Yonsei University（延世大学天文学系）；Department of Physics and Astronomy, University of California, Davis（加州大学戴维斯分校物理与天文学系）；Center for Cosmology and Astroparticle Physics, The Ohio State University（俄亥俄州立大学宇宙学与高能粒子物理中心）；Department of Physics, The Ohio State University（俄亥俄州立大学物理系）；Department of Astronomy, The Ohio State University（俄亥俄州立大学天文学系）
