Paper: Impact of Gravity on Changing Magnetic Field Orientations in a Sample of Massive Protostellar Clusters Observed with ALMA
Authors: Qizhou Zhang, Junhao Liu, Lingzhen Zeng, J. D. Soler, Huei-Ru Vivien Chen, Tao-Chung Ching, Paul T. P. Ho, Josep Miquel Girart, Patrick M. Koch, Shih-Ping Lai, Shanghuo Li, Zhi-Yun Li, Hauyu Baobab Liu, Keping Qiu, Ramprasad Rao
Figure caption:                         (a) Continuum emission at 225 GHz and magnetic fields for NGC 6334 I, In, IV, and V. The Stokes I emission is shown in contours and in gray scales. The red line segments represent the PA of the magnetic field plane-of-the-sky component, produced using a cutoff threshold of 3σ in Stokes Q and U intensities. The synthesized beam is marked at the lower-left corner of each panel. The horizontal bars at the lower-right corner of each panel represent a linear scale of 0.05 pc. The dotted line marks the 50% sensitivity level of the observations. Unless stated otherwise, all images in Figure 1 were made from combined visibilities from the configuration C43-1 and C43-4. The Stokes I intensities are contoured at (±3, ±6, 10, 20, 40, 60, 100) × σ, where σ values are listed in Table 2. (b) Continuum emission at 225 GHz and magnetic fields for G14. The Stokes I emission is shown in contours and gray scales. The red line segments represent the PAs of the plane-of-the-sky component of magnetic fields. The synthesized beam is marked at the lower-left corner of each panel. The horizontal bars at the lower-right corner of each panel represent a linear scale of 0.05 pc. The dotted line marks the 50% sensitivity level of the observations. (c) Continuum emission at 225 GHz for NGC 6334IR, G14-N.4, G14-N.5, and G14-N.6. The Stokes I emission is shown in contours and in gray scales. The red line segments represent the PAs of the plane-of-the-sky component of magnetic fields. The synthesized beam is marked at the lower-left corner of each panel. The horizontal bars at the lower-right corner of each panel represent a linear scale of 0.05 pc. The dotted line marks the 50% sensitivity level of the observations. Images were made from visibilities from the configuration C43-1 only. (d) Continuum emission at 225 GHz and magnetic fields for G34. The Stokes I emission is shown in contours and gray scales. The red line segments represent the PAs of the plane-of-the-sky component of magnetic fields. The synthesized beam is marked at the lower-left corner of each panel. The horizontal bars at the lower-right corner of each panel represent a linear scale of 0.05 pc. The dotted line marks the 50% sensitivity level of the coverage. (e) Continuum emission at 225 GHz and magnetic fields for G35.2N. The Stokes I emission is shown in contours and gray scales. The red line segments represent the PAs of the plane-of-the-sky component of magnetic fields. The synthesized beam is marked at the lower-left corner of each panel. The horizontal bars at the lower-right corner of each panel represent a linear scale of 0.05 pc. The dotted line marks the 50% sensitivity level of the observations. (f) Continuum emission at 225 GHz and magnetic fields for IRAS 18360 and IRDC G28.34. The Stokes I emission is shown in contours and gray scales. The red line segments represent the PAs of the plane-of-the-sky component of magnetic fields. The synthesized beam is marked at the lower-left corner of each panel. The horizontal bars at the lower-right corner of each panel represent a linear scale of 0.05 pc. The dotted line marks the 50% sensitivity level of the observations.