adsabs/AstroCLIMB huggingface dataset:
Paper: Early Planet Formation in Embedded Disks (eDisk). XVII. A Compact but Structured Keplerian Disk and Large-scale Streamers Revealed in the Class I Protostellar System IRAS 04169+2702
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Leslie W. Looney, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Patrick M. Koch, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Jinshi Sai, Travis J. Thieme, Jonathan P. Williams, Sacha Gavino, Miyu Kido, Shih-Ping Lai, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Hsi-Wei Yen
Figure caption: Top: channel maps for the SO (65–54) emission of the SBLB data. The emission above the 3σSBLB level is detected from 2.68 to 9.70 km s−1. The white contours indicate the 3σSBLB levels of the emission, where 1σSBLB corresponds to 1.88 mJy beam−1. The red ellipse in the lower left denotes the synthesized beam of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩188 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩152 (PA = 8﹩\mathop{.}\limits^{^\circ }﹩6). Note that this velocity range overlaps with the range where the spiral arms are detected in C18O (Figures A5 and A6). Bottom: channel maps for the H2CO (30,3–20,2) emission of the SBLB data. The emission above the 3σSBLB level is detected from 3.4 to 8.76 km s−1. The black dashed and solid contours indicate the −3σSBLB and 3σSBLB levels of the emission, respectively, where 1σSBLB corresponds to 0.52 mJy beam−1. The red ellipse in the lower left denotes the synthesized beam of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩186 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩148 (PA = 5﹩\mathop{.}\limits^{^\circ }﹩5). Note that the spiral structure is seen in the two channels from 6.08 to 7.42 km s−1.
Paper: Early Planet Formation in Embedded Disks (eDisk). XVII. A Compact but Structured Keplerian Disk and Large-scale Streamers Revealed in the Class I Protostellar System IRAS 04169+2702
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Leslie W. Looney, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Patrick M. Koch, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Jinshi Sai, Travis J. Thieme, Jonathan P. Williams, Sacha Gavino, Miyu Kido, Shih-Ping Lai, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Hsi-Wei Yen
Figure caption: Top: channel maps for the C18O (2–1) emission of the SB-only data. The emission above the 3σSB level is detected from 3.18 to 9.86 km s−1. The black contours indicate the 3σSB levels of the emission, where 1σSB corresponds to 3.17 mJy beam−1. The red ellipse in the lower left denotes the synthesized beam of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩482 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩343 (PA = −2﹩\mathop{.}\limits^{^\circ }0﹩). Bottom: channel maps for the C18O (2–1) emission of the LB-only data. The emission above the 3σLB level is detected from 3.35 to 9.86 km s−1. The black dashed and solid contours indicate the −3σLB and 3σLB levels of the emission, respectively, where 1σLB corresponds to 1.75 mJy beam−1. The red ellipse in the lower left denotes the synthesized beam of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩133 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩111 (PA = 14﹩\mathop{.}\limits^{^\circ }2﹩).
Paper: Early Planet Formation in Embedded Disks (eDisk). XVII. A Compact but Structured Keplerian Disk and Large-scale Streamers Revealed in the Class I Protostellar System IRAS 04169+2702
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Leslie W. Looney, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Patrick M. Koch, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Jinshi Sai, Travis J. Thieme, Jonathan P. Williams, Sacha Gavino, Miyu Kido, Shih-Ping Lai, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Hsi-Wei Yen
Figure caption: Channel maps for the 12CO (2–1) emission of the LB-only data. The emission above the 3σLB emission is detected from −7.93 to 18.11 km s−1, and the black dashed and solid contours indicate the −3σLB and 3σLB levels of the emission, respectively, where 1σLB corresponds to 1.07 mJy beam−1. The red ellipse in the lower left denotes the synthesized beam of this emission, which is 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩129 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩109 (PA = 12﹩\mathop{.}\limits^{^\circ }﹩9). In addition, the LB-only dust continuum emission is represented as white contours with levels of {3, 150, 190} × σLB, where 1σLB corresponds to 18.8 μJy beam−1, and its synthesized beam of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩044 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩034 (PA = 19﹩\mathop{.}\limits^{^\circ }﹩1) is denoted as a white ellipse in the lower left.
Paper: Early Planet Formation in Embedded Disks (eDisk). XVII. A Compact but Structured Keplerian Disk and Large-scale Streamers Revealed in the Class I Protostellar System IRAS 04169+2702
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Leslie W. Looney, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Patrick M. Koch, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Jinshi Sai, Travis J. Thieme, Jonathan P. Williams, Sacha Gavino, Miyu Kido, Shih-Ping Lai, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Hsi-Wei Yen
Figure caption: Channel maps for the 12CO (2–1) emission of the SBLB data. The emission above the 3σSBLB level is detected from −13.01 to 18.75 km s−1. The black contours indicate the 3σSBLB level of the emission, where 1σSBLB corresponds to 0.95 mJy beam−1. The red ellipse in the lower left denotes the synthesized beam of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩182 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩147 (PA = 6﹩\mathop{.}\limits^{^\circ }﹩5). The two perpendicular gray lines show the directions of the disk’s major (PA = 140°) and minor (PA = 50°) axes measured in the LB-only dust continuum image (Figure 1(c)). A bipolar outflow feature is clearly seen along the disk’s minor axis, i.e., along the northeast–southwest direction. Notably, the redshifted components exhibit complicated shapes with multiple parabolic shells and are not well aligned with the disk’s minor axis.
Paper: Early Planet Formation in Embedded Disks (eDisk). XVII. A Compact but Structured Keplerian Disk and Large-scale Streamers Revealed in the Class I Protostellar System IRAS 04169+2702
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Leslie W. Looney, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Patrick M. Koch, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Jinshi Sai, Travis J. Thieme, Jonathan P. Williams, Sacha Gavino, Miyu Kido, Shih-Ping Lai, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Hsi-Wei Yen
Figure caption: Channel maps for the C18O (2–1) emission of the SBLB data. The emission above the 3σSBLB level is detected from 3.18 to 10.20 km s−1. The black contours indicate the 3σSBLB levels of the emission, where 1σSBLB corresponds to 1.57 mJy beam−1. The red ellipse in the lower left denotes the synthesized beam of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩188 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩149 (PA = ﹩6\mathop{.}\limits^{^\circ }6﹩).
Paper: Early Planet Formation in Embedded Disks (eDisk). XVII. A Compact but Structured Keplerian Disk and Large-scale Streamers Revealed in the Class I Protostellar System IRAS 04169+2702
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Leslie W. Looney, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Patrick M. Koch, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Jinshi Sai, Travis J. Thieme, Jonathan P. Williams, Sacha Gavino, Miyu Kido, Shih-Ping Lai, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Hsi-Wei Yen
Figure caption: Channel maps for the 13CO (2–1) emission of the LB-only data. The emission above the 3σLB level is detected from 2.18 to 10.20 km s−1. The black dashed and solid contours indicate the −3σLB and 3σLB levels of the emission, respectively, where 1σLB corresponds to 2.35 mJy beam−1. The red ellipse in the lower left denotes the synthesized beam of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩132 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩111 (PA = 10﹩\mathop{.}\limits^{^\circ }8﹩).
Paper: Early Planet Formation in Embedded Disks (eDisk). XVII. A Compact but Structured Keplerian Disk and Large-scale Streamers Revealed in the Class I Protostellar System IRAS 04169+2702
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Leslie W. Looney, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Patrick M. Koch, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Jinshi Sai, Travis J. Thieme, Jonathan P. Williams, Sacha Gavino, Miyu Kido, Shih-Ping Lai, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Hsi-Wei Yen
Figure caption: Channel maps for the 13CO (2–1) emission of the SBLB data. The emission above the 3σSBLB level is detected from 1.01 to 11.37 km s−1. The black contours indicate the 3σSBLB level of the emission, where 1σSBLB corresponds to 2.09 mJy beam−1. The red ellipse in the lower left denotes the synthesized beam of the emission, which is 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩189 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩151 (PA = ﹩4\mathop{.}\limits^{^\circ }0﹩).
Paper: The Significant Contribution of Supersoft X-Ray Sources to Nebular He II Line Emission
Authors: Dian P. Triani, Rosanne Di Stefano, Tiger Yu-Yang Hsiao, Lisa J. Kewley
Figure caption: He II/Hβ as a function of blackbody temperature for the MAPPINGS model with pure blackbody spectra as an input. The bolometric luminosity is kept constant at L = 1039erg s−1. Symbols with different colors mark different ionization parameters as indicated in the colorbar. Crosses mark the MAPPINGS output from the 1 Myr stellar population synthesis from BPASS with a metallicity of 0.4Z⊙ . The gas-phase metallicity is assumed to be similar to the stellar metallicity and the ionization parameter of the BPASS model is kept at a similar range with the pure blackbody model. The blue shaded region shows the 16th and 84th percentile of the He II/Hβ ratio observed in the SDSS sample and the orange shaded regions shows the 16th and 84th percentile in the NIRSpec sample.
Paper: The Significant Contribution of Supersoft X-Ray Sources to Nebular He II Line Emission
Authors: Dian P. Triani, Rosanne Di Stefano, Tiger Yu-Yang Hsiao, Lisa J. Kewley
Figure caption: He II/Hβ as a function of blackbody temperature for the MAPPINGS model with a combination of a stellar population spectrum and a blackbody as an input. The bolometric luminosity is kept constant at L = 1039erg s−1 and the ionization parameter is kept at ﹩{\mathrm{log}}\,U=-3﹩. Symbols with different colors mark different luminosity fractions of blackbody to the BPASS spectra as indicated in the legend. The red cross marks the MAPPINGS output from the 1 Myr stellar population synthesis from BPASS with a metallicity of ﹩12+{\mathrm{log}}\,({\rm{O}}/{\rm{H}})=8.47﹩ and the gas-phase metallicity is assumed to be similar to the stellar metallicity. The blue shaded region shows the range of the He II/Hβ ratio observed in the SDSS sample and the orange shaded regions shows the observed range in the NIRSpec sample.
Paper: Global Distribution of the Key Species on the Surface of Europa
Authors: Jiazheng Li, Yinsi Shou, Cheng Li, Xianzhe Jia
Figure caption: The incoming energy fluxes of the six major components on the surface of Europa as functions of latitude and longitude. (a) Thermal O+. (b) Energetic O+. (c) Thermal S++. (d) Energetic S++. (e) Energetic H+. (f) Electrons.
Paper: The Significant Contribution of Supersoft X-Ray Sources to Nebular He II Line Emission
Authors: Dian P. Triani, Rosanne Di Stefano, Tiger Yu-Yang Hsiao, Lisa J. Kewley
Figure caption: The SED of binary stellar populations from BPASS with ages of 1 Myr–1 Gyr. The vertical lines show the ionization potential of HI(13.59eV), HeI(24.59eV), OII(35.12eV), and He II (54.42eV).
Paper: The Significant Contribution of Supersoft X-Ray Sources to Nebular He II Line Emission
Authors: Dian P. Triani, Rosanne Di Stefano, Tiger Yu-Yang Hsiao, Lisa J. Kewley
Figure caption: The SED of a 1 Myr stellar population from BPASS (blue, showing emission and absorption lines) and blackbody spectra of kT = 5, 10, 20, 30, 50, 80, and 100 eV (purple to yellow, as indicated in the legend). The total luminosity of each blackbody is set equal to the luminosity of the 1 Myr stellar population from BPASS, assuming a total stellar mass of 106M⊙ . The vertical lines show the ionization potential of HI(13.59 eV), HeI(24.59 eV), OII(35.12 eV), and He II (54.42 eV).
Paper: The Significant Contribution of Supersoft X-Ray Sources to Nebular He II Line Emission
Authors: Dian P. Triani, Rosanne Di Stefano, Tiger Yu-Yang Hsiao, Lisa J. Kewley
Figure caption: Number of observed supersoft sources as a function of temperature in eV based on J. Greiner’s (1996) catalog.
Paper: Gas-induced Perturbations on the Gravitational Wave Inspiral of Live Post-Newtonian LISA Massive Black Hole Binaries
Authors: Mudit Garg, Alessia Franchini, Alessandro Lupi, Matteo Bonetti, Lucio Mayer
Figure caption: Gas torques onto the binary in terms of ξ as a function of the SMA for gas+PN 2.5 simulation (light blue lines). We show average ξ values for gas+PN 2.5 (solid blue line; ﹩{\bar{\xi }}_{{\rm{gas}}+{\rm{PN\; 2}}.5}\approx -19.5﹩) and gas+PN 2 (dashed red line; ﹩{\bar{\xi }}_{{\rm{gas}}+{\rm{PN\; 2}}}\approx -24.5﹩) cases. Note that we have not done any smoothing in plotting ξ for the gas+PN 2.5 run but only interpolation between snapshots.
Paper: Gas-induced Perturbations on the Gravitational Wave Inspiral of Live Post-Newtonian LISA Massive Black Hole Binaries
Authors: Mudit Garg, Alessia Franchini, Alessandro Lupi, Matteo Bonetti, Lucio Mayer
Figure caption: Average torque value (blue cross) expressed in terms of ﹩\bar{\xi }﹩ over initial 100 orbits of gas+PN 2.5 simulations for three different resolutions: LR with Δx[3a] = 1.31 rs, MR with Δx[3a] = 1.07 rs, and HR with Δx[3a] = 0.66 rs.
Paper: Gas-induced Perturbations on the Gravitational Wave Inspiral of Live Post-Newtonian LISA Massive Black Hole Binaries
Authors: Mudit Garg, Alessia Franchini, Alessandro Lupi, Matteo Bonetti, Lucio Mayer
Figure caption: The 2D projected gravitational torque (Tgrav) distribution between −5a and 5a in both axes averaged over 100 snapshots between the 100th and 110th orbits. We show results from the gas+PN 2.5 run (left panel), the gas+PN 2 run (middle panel), and their difference (right panel). The third panel clearly shows that the gas+PN 2.5 run has slightly more positive torque than the gas+PN 2 simulation.
Paper: Gas-induced Perturbations on the Gravitational Wave Inspiral of Live Post-Newtonian LISA Massive Black Hole Binaries
Authors: Mudit Garg, Alessia Franchini, Alessandro Lupi, Matteo Bonetti, Lucio Mayer
Figure caption: Column density (Σ) plots at three SMAs—54.5 rs (left panel), 52 rs (middle panel), and 49.5 rs (right panel)—for the binary evolution under both GW and gas. Here Σ varies between ∼103 and 107 g cm−2. Both the binary (green dots) and the cavity shrink with time. Moreover, gas inflow inside the cavity creates short-lived minidisks.
Paper: The Hourglass-shaped Magnetic Fields and Dust Filaments in the HH 211 Protostellar Envelope
Authors: Youngwoo Choi, Woojin Kwon, Leslie W. Looney, Ian W. Stephens, Zhi-Yun Li, Floris F. S. van der Tak, John J. Tobin
Figure caption: Left: inferred magnetic field orientations around HH 211 from the Band 3 polarized continuum with a robust parameter of 2.0. The line segments represent plane-of-sky magnetic field directions, with green for PI > 2σPI and red for 1.5σPI < PI < 2σPI. The black lines are the Band 3 dust continuum with a robust parameter of 2, showing 3, 10, 20, 50, 100, 200, and 500 times the rms noise level. Right: inferred magnetic field orientations around HH 211 from the Band 6 polarized continuum with a robust parameter of 0.5. Green segments represent plane-of-sky magnetic field directions with PI > 3σPI. The blue and red contours indicate CO (2-1) integrated intensities in velocity ranges from 0 to 8 and from 10 to 18 km s−1, respectively (K.-S. Jhan & C.-F. Lee 2021). The blue and red contour levels are 0.03, 0.035, 0.05, 0.1, and 0.2 Jy beam−1 km s−1. The black lines are the Band 6 dust continuum with a robust parameter of 0.5, showing 5, 10, 20, 50, 100, 200, and 500 times the rms noise level. The synthesized beam size and spatial scale bar are shown in the bottom left and bottom right of both panels, respectively.
Paper: The Hourglass-shaped Magnetic Fields and Dust Filaments in the HH 211 Protostellar Envelope
Authors: Youngwoo Choi, Woojin Kwon, Leslie W. Looney, Ian W. Stephens, Zhi-Yun Li, Floris F. S. van der Tak, John J. Tobin
Figure caption: CMU model trajectories in the southern region of the HH 211 envelope. The red line shows the case with θ0 = 90° and  ϕ0 = 90°, while the orange lines represent models with 80∘ < θ0 < 90° and 90∘ < ϕ0 < 95°. All other features are the same as in the right panel of Figure 4.
Paper: The Hourglass-shaped Magnetic Fields and Dust Filaments in the HH 211 Protostellar Envelope
Authors: Youngwoo Choi, Woojin Kwon, Leslie W. Looney, Ian W. Stephens, Zhi-Yun Li, Floris F. S. van der Tak, John J. Tobin
Figure caption: Dust continuum images with similar beam sizes in Band 3 (left) and Band 6 (middle). The beam sizes are matched by adjusting the uv-coverage of the Band 3 and Band 6 observations. The resulting beam sizes are 0. ﹩\mathop{.}\limits^{\unicode{x02033}}﹩774 × 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩727 (PA = 35﹩\mathop{.}\limits^{\unicode{x000b0}}﹩9) in Band 3 and 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩759 ×  0﹩\mathop{.}\limits^{\unicode{x02033}}﹩717 (PA = 2﹩\mathop{.}\limits^{\unicode{x000b0}}﹩9) in Band 6. Contour levels are at 5, 10, 20, 50, 100, 200, and 500 times the rms noise level in each observation. The spectral index map is made with these images (right).
Paper: The Hourglass-shaped Magnetic Fields and Dust Filaments in the HH 211 Protostellar Envelope
Authors: Youngwoo Choi, Woojin Kwon, Leslie W. Looney, Ian W. Stephens, Zhi-Yun Li, Floris F. S. van der Tak, John J. Tobin
Figure caption: Spectral index components between 97.5 and 233 GHz frequencies. Left: spectral index of the Planck function as a function of temperature. It converges to 2 at high temperatures. Right: ﹩\beta ^{\prime} ({\tau }_{\nu })﹩ as a function of optical depth at 233 GHz when β is 1.5. It converges to β in the optically thin limit and 0 in the optically thick limit.
Paper: The Hourglass-shaped Magnetic Fields and Dust Filaments in the HH 211 Protostellar Envelope
Authors: Youngwoo Choi, Woojin Kwon, Leslie W. Looney, Ian W. Stephens, Zhi-Yun Li, Floris F. S. van der Tak, John J. Tobin
Figure caption: Polarized intensity around the HH 211 envelope in Band 3 with a robust parameter of 2.0 (left) and in Band 6 with a robust parameter of 0.5 (right). The black lines represent Stokes I intensity levels with 3 (left)/5 (right), 10, 20, 50, 100, 200, and 500 times the rms noise level in each observation. The synthesized beam size and spatial scale bar are shown in the bottom left and bottom right of both panels, respectively.
Paper: The Hourglass-shaped Magnetic Fields and Dust Filaments in the HH 211 Protostellar Envelope
Authors: Youngwoo Choi, Woojin Kwon, Leslie W. Looney, Ian W. Stephens, Zhi-Yun Li, Floris F. S. van der Tak, John J. Tobin
Figure caption: The estimated line-of-sight averaged temperature (left) and column density (right) of the HH 211 envelope. Note that calculations are uncertain in the central region due to the embedded disk emission.
Paper: The Hourglass-shaped Magnetic Fields and Dust Filaments in the HH 211 Protostellar Envelope
Authors: Youngwoo Choi, Woojin Kwon, Leslie W. Looney, Ian W. Stephens, Zhi-Yun Li, Floris F. S. van der Tak, John J. Tobin
Figure caption: A cartoon illustrating the observation of a protostellar envelope. The dust continuum traces not only the material closest to the protostar (A), but also the cooler background (B) and foreground (C) material, resulting in a line-of-sight averaged temperature lower than the temperature at location A.
Paper: The Hourglass-shaped Magnetic Fields and Dust Filaments in the HH 211 Protostellar Envelope
Authors: Youngwoo Choi, Woojin Kwon, Leslie W. Looney, Ian W. Stephens, Zhi-Yun Li, Floris F. S. van der Tak, John J. Tobin
Figure caption: Polarization fraction around the HH 211 envelope in Band 3 with a robust parameter of 2.0 (left) and in Band 6 with a robust parameter of 0.5 (right). The black lines represent Stokes I intensity levels with 3 (left)/5 (right), 10, 20, 50, 100, 200, and 500 times the rms noise level in each observation. The synthesized beam size and spatial scale bar are shown in the bottom left and bottom right of both panels, respectively.
Paper: The Hourglass-shaped Magnetic Fields and Dust Filaments in the HH 211 Protostellar Envelope
Authors: Youngwoo Choi, Woojin Kwon, Leslie W. Looney, Ian W. Stephens, Zhi-Yun Li, Floris F. S. van der Tak, John J. Tobin
Figure caption: Defined possible southern stream region used to estimate the mass infall rate along the southern filament. The magenta line indicates the ballistic infalling model trajectory within the defined region. All other features are the same as in the right panel of Figure 4.