adsabs/AstroCLIMB huggingface dataset:
Paper: High-altitude Spider-type Prominence above the Magnetic Null Point
Authors: Boris Filippov
Figure caption: Distribution of the curvature radius of field lines along the dipped section of the PIL marked with small green circles in Figure 5(c).
Paper: Neutral Hydrogen (H I) 21 cm as a Probe: Investigating Spatial Variations in Interstellar Turbulent Properties
Authors: Amit Kumar Mittal, Brian L. Babler, Snežana Stanimirović, Nickolas Pingel
Figure caption: The H I SPS slope, averaged in 2° latitude bins, as a function of Galactic latitude. Green points show results from previous studies: (1) Pingel et al. (2013); (2) Kalberla et al. (2017); (3) Miville-Deschênes et al. (2003); (4) Blagrave et al. (2017); (5) Martin et al. (2015); (6) Khalil et al. (2006); (7) Dickey et al. (2001); (8) Kalberla & Haud (2019); (9) Marchal & Miville-Deschênes (2021); (10) Chepurnov et al. (2010); (11) Pingel et al. (2018); (12) Choudhuri & Roy (2019).
Paper: Neutral Hydrogen (H I) 21 cm as a Probe: Investigating Spatial Variations in Interstellar Turbulent Properties
Authors: Amit Kumar Mittal, Brian L. Babler, Snežana Stanimirović, Nickolas Pingel
Figure caption: Top three panels: the standard deviation of the radiometer noise due to receiver temperature (σ rx), the standard deviation due to the H I brightness temperature (σ HI), and the standard deviation due to both receiver and H I brightness temperature (σ rx+HI). Bottom three panels: the noise contribution to the H I column density image: random fluctuations due to receiver temperature plus the systematic scanning uncertainty (N off), the contribution due to the brightness temperature that is velocity dependent (N on−HI), and the sum of these two contributions (N total).
Paper: Neutral Hydrogen (H I) 21 cm as a Probe: Investigating Spatial Variations in Interstellar Turbulent Properties
Authors: Amit Kumar Mittal, Brian L. Babler, Snežana Stanimirović, Nickolas Pingel
Figure caption: Top: the GALFA-H I rolling SPS slope, where the SPS slope is calculated for each 3° kernel and rolled across R.A. and decl. by stepping every ﹩8^{\prime} ﹩ to cover the entire GALFA-H I region. The SPS slope was determined only for regions where the SPS power is ≥9 × noise power, and the fitting was conducted over the range of 1.°5 to 16′. Pixels that do not satisfy this criterion are left blank (NaN). The Galactic coordinate grid is overlaid as black dashed lines. Middle: the uncertainty in the fitted SPS slope. Bottom: the χ 2 map of the single power-law SPS fit.
Paper: Neutral Hydrogen (H I) 21 cm as a Probe: Investigating Spatial Variations in Interstellar Turbulent Properties
Authors: Amit Kumar Mittal, Brian L. Babler, Snežana Stanimirović, Nickolas Pingel
Figure caption: Top panel: the H I column density integrated over the ±40 km s−1 velocity range multiplied by ﹩\sin | b| ﹩ is shown as black data points with respect to ﹩\sin | b| ﹩. Bottom panel: the SPS slope of the ﹩N({\rm{H}}\,{\rm\small{I}})\times \sin | b| ﹩ distribution, averaged in 2° latitude bins, as a function of ﹩\sin | b| ﹩.
Paper: Neutral Hydrogen (H I) 21 cm as a Probe: Investigating Spatial Variations in Interstellar Turbulent Properties
Authors: Amit Kumar Mittal, Brian L. Babler, Snežana Stanimirović, Nickolas Pingel
Figure caption: The SPS for three H I column density images shown in Figure 3. The fitting range, shown by the gray area, covers a range of angular scales from ∼20° to 16′, which corresponds to spatial frequencies k = 10−3 arcmin−1 to ∼6 × 10−2 arcmin−1.
Paper: Neutral Hydrogen (H I) 21 cm as a Probe: Investigating Spatial Variations in Interstellar Turbulent Properties
Authors: Amit Kumar Mittal, Brian L. Babler, Snežana Stanimirović, Nickolas Pingel
Figure caption: The histogram (shown in green) of the SPS slope image shown in the top panel of Figure 5. The on-plane histogram corresponds to latitudes ∣b∣ ≤ 10° and is shown in blue, whereas the off-plane histogram pertains to latitudes ∣b∣ ≥ 70° and is shown in orange. The vertical dashed lines represent the mean value for the three samples.
Paper: Neutral Hydrogen (H I) 21 cm as a Probe: Investigating Spatial Variations in Interstellar Turbulent Properties
Authors: Amit Kumar Mittal, Brian L. Babler, Snežana Stanimirović, Nickolas Pingel
Figure caption: Examples of the noise SPS spectra for different kernels. The raw SPS data points, P noise(k), are shown as black data points. The parameterized noise SPS, Q(k, sd), is shown in yellow, while the final parameterized noise SPS, C × Q(k, sd), is shown in blue. The SPS samples the range of angular scales from 3° to 8′, which corresponds to spatial frequencies k = 5 × 10−3 arcmin–1 to 10−1 arcmin−1.
Paper: Neutral Hydrogen (H I) 21 cm as a Probe: Investigating Spatial Variations in Interstellar Turbulent Properties
Authors: Amit Kumar Mittal, Brian L. Babler, Snežana Stanimirović, Nickolas Pingel
Figure caption: The logarithmic power for the noise SPS, P noise(k), as a function of the logarithm of σ(N total) for the first 20 binned k values obtained for all the 3° kernels, shown as gray data points. The mean values are overplotted in black. For each k, a linear function Q(sd) was fitted to the data.
Paper: Neutral Hydrogen (H I) 21 cm as a Probe: Investigating Spatial Variations in Interstellar Turbulent Properties
Authors: Amit Kumar Mittal, Brian L. Babler, Snežana Stanimirović, Nickolas Pingel
Figure caption: The parameterized noise SPS, Q(k, sd), for different values of σ(N total).
Paper: Early Planet Formation in Embedded Disks (eDisk). VIII. A Small Protostellar Disk around the Extremely Low Mass and Young Class 0 Protostar IRAS 15398–3359
Authors: Travis J. Thieme, Shih-Ping Lai, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Jinshi Sai (Insa Choi), Yusuke Aso, Jonathan P. Williams, Yoshihide Yamato, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Adele L. Plunkett, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Hsi-Wei Yen
Figure caption: Same as Figure 3, but for the SB-only maps of the representative molecular lines.
Paper: Early Planet Formation in Embedded Disks (eDisk). VIII. A Small Protostellar Disk around the Extremely Low Mass and Young Class 0 Protostar IRAS 15398–3359
Authors: Travis J. Thieme, Shih-Ping Lai, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Jinshi Sai (Insa Choi), Yusuke Aso, Jonathan P. Williams, Yoshihide Yamato, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Adele L. Plunkett, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Hsi-Wei Yen
Figure caption: Gallery of SB+LB continuum images from our eDisk observations of IRAS15398 with asinh (a = 0.001) scaling. Each robust value made by the imaging script is shown from largest angular resolution (robust = +2.0) on the left to smallest angular resolution (robust = −2.0) on the right. A large-scale view is shown in the top row, while a zoomed-in view is shown in the bottom row. The blue and red arrows represent the overall blue- and redshifted outflow directions found by Vazzano et al. (2021), respectively. The contours in both maps are shown in steps (3, 5, 7, 9, 12, 15, 20, 50, 100)σ rms, where σ rms is the rms noise of each map.
Paper: Early Planet Formation in Embedded Disks (eDisk). VIII. A Small Protostellar Disk around the Extremely Low Mass and Young Class 0 Protostar IRAS 15398–3359
Authors: Travis J. Thieme, Shih-Ping Lai, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Jinshi Sai (Insa Choi), Yusuke Aso, Jonathan P. Williams, Yoshihide Yamato, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Adele L. Plunkett, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Hsi-Wei Yen
Figure caption: Channel map of the SB+LB 12CO (J = 2 → 1) molecular line data. The channel velocities are shown in the upper right corner of the panels. The yellow star denotes the central position of IRAS15398 from the 2D Gaussian fitting. The scale bar is shown in the bottom left panel. Contours are shown in steps (3, 5, 7, 9, 12, 15, 20, 50, 100)σ rms, where σ rms is the rms noise of the map. The channel map is centered at 5.41 km s−1, which is the channel closest to the previously derived system velocity of 5.24 km s−1 (Yen et al. 2017a).
Paper: Early Planet Formation in Embedded Disks (eDisk). VIII. A Small Protostellar Disk around the Extremely Low Mass and Young Class 0 Protostar IRAS 15398–3359
Authors: Travis J. Thieme, Shih-Ping Lai, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Jinshi Sai (Insa Choi), Yusuke Aso, Jonathan P. Williams, Yoshihide Yamato, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Adele L. Plunkett, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Hsi-Wei Yen
Figure caption: Same as Figure 4, but for the SB-only maps of the representative molecular lines.
Paper: Early Planet Formation in Embedded Disks (eDisk). VIII. A Small Protostellar Disk around the Extremely Low Mass and Young Class 0 Protostar IRAS 15398–3359
Authors: Travis J. Thieme, Shih-Ping Lai, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Jinshi Sai (Insa Choi), Yusuke Aso, Jonathan P. Williams, Yoshihide Yamato, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Adele L. Plunkett, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Hsi-Wei Yen
Figure caption: Same as Figure B1, but for 13CO (J = 2 → 1). The channel map is centered at 5.19 km s−1.
Paper: Early Planet Formation in Embedded Disks (eDisk). VIII. A Small Protostellar Disk around the Extremely Low Mass and Young Class 0 Protostar IRAS 15398–3359
Authors: Travis J. Thieme, Shih-Ping Lai, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Jinshi Sai (Insa Choi), Yusuke Aso, Jonathan P. Williams, Yoshihide Yamato, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Adele L. Plunkett, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Hsi-Wei Yen
Figure caption: Same as Figure B1, but for C18O (J = 2 → 1). The channel map is centered at 5.19 km s−1.
Paper: Early Planet Formation in Embedded Disks (eDisk). VIII. A Small Protostellar Disk around the Extremely Low Mass and Young Class 0 Protostar IRAS 15398–3359
Authors: Travis J. Thieme, Shih-Ping Lai, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Jinshi Sai (Insa Choi), Yusuke Aso, Jonathan P. Williams, Yoshihide Yamato, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Adele L. Plunkett, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Hsi-Wei Yen
Figure caption: Zoomed-in version of Figure B4 for SO (J  N  = 65 → 54) showing velocities from 3.52 to 6.86 km s−1. The channel map is centered at 5.19 km s−1.
Paper: Early Planet Formation in Embedded Disks (eDisk). VIII. A Small Protostellar Disk around the Extremely Low Mass and Young Class 0 Protostar IRAS 15398–3359
Authors: Travis J. Thieme, Shih-Ping Lai, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Jinshi Sai (Insa Choi), Yusuke Aso, Jonathan P. Williams, Yoshihide Yamato, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Adele L. Plunkett, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Hsi-Wei Yen
Figure caption: Same as Figure B1, but for SO (J  N  = 65 → 54). The channel map is centered at 5.19 km s−1.
Paper: Early Planet Formation in Embedded Disks (eDisk). VIII. A Small Protostellar Disk around the Extremely Low Mass and Young Class 0 Protostar IRAS 15398–3359
Authors: Travis J. Thieme, Shih-Ping Lai, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Jinshi Sai (Insa Choi), Yusuke Aso, Jonathan P. Williams, Yoshihide Yamato, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Adele L. Plunkett, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Hsi-Wei Yen
Figure caption: A dynamical schematic of the IRAS15398 protostellar system.
Paper: Early Planet Formation in Embedded Disks (eDisk). VIII. A Small Protostellar Disk around the Extremely Low Mass and Young Class 0 Protostar IRAS 15398–3359
Authors: Travis J. Thieme, Shih-Ping Lai, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Jinshi Sai (Insa Choi), Yusuke Aso, Jonathan P. Williams, Yoshihide Yamato, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Adele L. Plunkett, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Hsi-Wei Yen
Figure caption: Integrated intensity maps of the representative molecular lines for IRAS15398. Each column is labeled with the respective molecular line. On the left, we show the large-scale structure of 12CO (panel (a)). On the right, we show C18O, 13CO, and SO, with a large-scale view in the top row (panels (b), (d), and (e)) and a zoomed-in view in the bottom row (panels (c), (e), and (g)). The yellow star represents the protostellar position. The beam sizes are shown as the gray circles in the lower left corner of each map, and scale bars are shown in the lower right corner of the 12CO map, as well as the rightmost SO maps for different physical scales. The solid and dashed gray lines indicate the deconvolved position angle of the continuum major and minor axes, respectively. The blue and red arrows represent the overall blue- and redshifted outflow directions found by Vazzano et al. (2021), respectively. The black contours show the integrated intensity in steps (3, 5, 7, 9, 12, 15, 20, 50, 100)σ rms, where σ rms is the rms noise of the respective integrated intensity map.
Paper: Early Planet Formation in Embedded Disks (eDisk). VIII. A Small Protostellar Disk around the Extremely Low Mass and Young Class 0 Protostar IRAS 15398–3359
Authors: Travis J. Thieme, Shih-Ping Lai, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Jinshi Sai (Insa Choi), Yusuke Aso, Jonathan P. Williams, Yoshihide Yamato, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Adele L. Plunkett, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Hsi-Wei Yen
Figure caption: The PV plots of the SLAM fitting results for SO. The red and blue circles represent the red- and blueshifted points fit with the edge method, respectively, while the magenta and cyan triangles represent the red- and blueshifted points fit with the ridge method, respectively. The black solid and dashed lines show the best-fit edge and ridge models, respectively. The contours in the PV map are shown in steps (3, 5, 7, 9, 12, 15, 20, 50, 100)σ rms, where σ rms is the rms noise in the PV map.
Paper: Early Planet Formation in Embedded Disks (eDisk). VIII. A Small Protostellar Disk around the Extremely Low Mass and Young Class 0 Protostar IRAS 15398–3359
Authors: Travis J. Thieme, Shih-Ping Lai, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Jinshi Sai (Insa Choi), Yusuke Aso, Jonathan P. Williams, Yoshihide Yamato, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Adele L. Plunkett, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Hsi-Wei Yen
Figure caption: Same as Figure 3, but for the intensity-weighted velocity maps of the representative molecular lines.
Paper: Early Planet Formation in Embedded Disks (eDisk). VIII. A Small Protostellar Disk around the Extremely Low Mass and Young Class 0 Protostar IRAS 15398–3359
Authors: Travis J. Thieme, Shih-Ping Lai, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Jinshi Sai (Insa Choi), Yusuke Aso, Jonathan P. Williams, Yoshihide Yamato, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Adele L. Plunkett, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Hsi-Wei Yen
Figure caption: PV diagrams of C18O (left), 13CO (middle), and SO (right). All cuts were made with a width of 1 beam. The offset axis goes from west (negative) to east (positive). The color bar scale is normalized by the peak intensity (﹩{I}_{\nu }^{\mathrm{peak}}﹩). The emission is also shown with black contours in steps (3, 5, 7, 9, 12, 15, 20, 50, 100)σ rms, where σ rms is the rms noise of the respective PV map. The blue and orange lines represent the Keplerian curves for the protostellar masses, system velocities, and disk inclination angles reported by Okoda et al. (2018) and Yen et al. (2017a), respectively.
Paper: Early Planet Formation in Embedded Disks (eDisk). VIII. A Small Protostellar Disk around the Extremely Low Mass and Young Class 0 Protostar IRAS 15398–3359
Authors: Travis J. Thieme, Shih-Ping Lai, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Jinshi Sai (Insa Choi), Yusuke Aso, Jonathan P. Williams, Yoshihide Yamato, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Adele L. Plunkett, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Hsi-Wei Yen
Figure caption: The RV plots of the SLAM fitting results for SO. The colored points and black lines have the same meaning as in Figure 6. The best-fit power-law equations are shown in the lower left corner.
Paper: Early Planet Formation in Embedded Disks (eDisk). VIII. A Small Protostellar Disk around the Extremely Low Mass and Young Class 0 Protostar IRAS 15398–3359
Authors: Travis J. Thieme, Shih-Ping Lai, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Jinshi Sai (Insa Choi), Yusuke Aso, Jonathan P. Williams, Yoshihide Yamato, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Adele L. Plunkett, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Hsi-Wei Yen
Figure caption: Representative 1.3  mm dust continuum maps of IRAS15398 with asinh (a = 0.001) scaling. Left: the robust = 0.5 map showing an overall view of the extended dust emission. The blue and red arrows represent the overall blue- and redshifted outflow directions found by Vazzano et al. (2021), respectively. Right: the robust = −0.5 map showing a zoomed-in view of the central compact structure. The contours in both maps are shown in steps (3, 5, 7, 9, 12, 15, 20, 50, 100)σ rms, where σ rms is the rms noise of each map.
Paper: Early Planet Formation in Embedded Disks (eDisk). VIII. A Small Protostellar Disk around the Extremely Low Mass and Young Class 0 Protostar IRAS 15398–3359
Authors: Travis J. Thieme, Shih-Ping Lai, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Jinshi Sai (Insa Choi), Yusuke Aso, Jonathan P. Williams, Yoshihide Yamato, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Adele L. Plunkett, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Hsi-Wei Yen
Figure caption: The 2D Gaussian fitting results of IRAS15398. Left: the robust = −0.5 map as shown in Figure 1. Middle: the 2D Gaussian fitting model results. The solid and dashed gray lines indicate the deconvolved position angle of the continuum major and minor axes, respectively. Right: the residual map made by subtracting the model from the observations. The contours are shown in steps (3, 5, 7, 9, 12, 15, 20, 50, 100)σ rms, where σ rms is the rms noise in the robust = −0.5 map.
Paper: Polarization Evolution of Fast Radio Burst Sources in Binary Systems
Authors: Zhao-Yang Xia, Yuan-Pei Yang, Qiao-Chu Li, Fa-Yin Wang, Bo-Yang Liu, Zi-Gao Dai
Figure caption: Comparison between the model and observations of PSR B1744-24A. (a) The CP evolution with orbital phase near the spin phase 0.34. (b) The CP evolution with orbital phase near the spin phase 0.32. (c) The DM evolution with orbital phase. The red line represents the fitting line based on the model, and the black points denote observation data. The residuals of the model and data are shown in the bottom panels, where the red horizontal dashed line is at zero residual. We take the binary parameters with R orb = 0.85R ⊙, R c = 0.12R ⊙, B c = 300 G, n w,0 = 4.5 × 107 cm−3, and V i = 0.5, θ L = 5/12π, α = 0.
Paper: Polarization Evolution of Fast Radio Burst Sources in Binary Systems
Authors: Zhao-Yang Xia, Yuan-Pei Yang, Qiao-Chu Li, Fa-Yin Wang, Bo-Yang Liu, Zi-Gao Dai
Figure caption: The evolution of RM with orbital phase for different magnetic inclination angles α in HMCBs. The pulsar is located in superior conjunction at ϕ orb = 1.25.
Paper: Polarization Evolution of Fast Radio Burst Sources in Binary Systems
Authors: Zhao-Yang Xia, Yuan-Pei Yang, Qiao-Chu Li, Fa-Yin Wang, Bo-Yang Liu, Zi-Gao Dai
Figure caption: The evolution of RM with orbital phase in LMCBs. (a) P c = 10 day, for different α = 0, π/12, and 5π/12. (b) α = 5π/12, for different P c = 10, 50, and 100 days over five orbital periods.
Paper: Polarization Evolution of Fast Radio Burst Sources in Binary Systems
Authors: Zhao-Yang Xia, Yuan-Pei Yang, Qiao-Chu Li, Fa-Yin Wang, Bo-Yang Liu, Zi-Gao Dai
Figure caption: The characteristic Faraday transition frequency ν T as a function of the orbital period P orb (day) and the rate of mass loss ﹩\dot{M}({M}_{\odot }\,{\mathrm{yr}}^{-1})﹩ of the companion star. The dashed line corresponds to the radio frequency ν ∼ GHz, and strong FCs are expected in the region below this line. The red dots indicate the characteristic transition frequencies of the two binary systems.
Paper: Polarization Evolution of Fast Radio Burst Sources in Binary Systems
Authors: Zhao-Yang Xia, Yuan-Pei Yang, Qiao-Chu Li, Fa-Yin Wang, Bo-Yang Liu, Zi-Gao Dai
Figure caption: (a) The value of V f/V i as the function of θ L for R orb = 16R c. (b) The value of V f/V i as the function of R orb for θ L = π/4. The strong FC can be generated even for LMCBs, as shown by the orange-shaded region.
Paper: Polarization Evolution of Fast Radio Burst Sources in Binary Systems
Authors: Zhao-Yang Xia, Yuan-Pei Yang, Qiao-Chu Li, Fa-Yin Wang, Bo-Yang Liu, Zi-Gao Dai
Figure caption: The geometric configuration of binary systems involving FRB sources, where the XYZ coordinate system is chosen with the orbital plane lying in the XY plane and the rotation axis Ω of the companion star lying in the XZ plane. The angles with the Z-axis and the magnetic axes are denoted by θ Ω and α, respectively.
Paper: Polarization Evolution of Fast Radio Burst Sources in Binary Systems
Authors: Zhao-Yang Xia, Yuan-Pei Yang, Qiao-Chu Li, Fa-Yin Wang, Bo-Yang Liu, Zi-Gao Dai
Figure caption: The evolution of polarization (V, L) and B  z  with distance along LOS at different orbital phases in HMCBs.
Paper: Polarization Evolution of Fast Radio Burst Sources in Binary Systems
Authors: Zhao-Yang Xia, Yuan-Pei Yang, Qiao-Chu Li, Fa-Yin Wang, Bo-Yang Liu, Zi-Gao Dai
Figure caption: The evolution of polarization (V, L) with frequency at different orbital phases in HMCBs.