adsabs/AstroCLIMB huggingface dataset:
Paper: Early Planet Formation in Embedded Disks (eDisk). IX. High-resolution ALMA Observations of the Class 0 Protostar R CrA IRS5N and Its Surroundings
Authors: Rajeeb Sharma, Jes K. Jørgensen, Sacha Gavino, Nagayoshi Ohashi, John J. Tobin, Zhe-Yu Daniel Lin, Zhi-Yun Li, Shigehisa Takakuwa, Chang Won Lee, Jinshi Sai (Insa Choi), Woojin Kwon, Itziar de Gregorio-Monsalvo, Alejandro Santamaría-Miranda, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Shih-Ping Lai, Jeong-Eun Lee, Leslie W. Looney, Nguyen Thi Phuong, Travis J. Thieme, Jonathan P. Williams
Figure caption: Same as Figure 10, but for tje IRS5a binary source with the model made with a single-Gaussian peak for each continuum emission observed.
Paper: Ho’oleilana: An Individual Baryon Acoustic Oscillation?
Authors: R. Brent Tully, Cullan Howlett, Daniel Pomarède
Figure caption: BAO detection using the BAO wavelet with different radii (r BAO) and widths (s BAO). The top panel of this figure shows the average values of the differences in the detection coefficient B  r,s  between the BAO and no-BAO simulations weighted by the variance. The vertical green line is the expected BAO radius in the mocks. The middle panel shows the average over the variance for only the no-BAO simulations. The bottom panel shows the same applied to the data. In all cases, the contours simply follow the color map, where the solid contour corresponds to a value of zero while the dashed (dotted) lines correspond to positive (negative) 0.5σ and 1.0σ values. Dashed lines/red regions hence indicate values of the wavelet parameters with stronger BAO-like features. Finally, the green cross in the bottom panel indicates the wavelet parameters with the single largest BAO weight W  r,s , which coincides closely with the center, width, and radius of Ho’oleilana derived via other means.
Paper: Ho’oleilana: An Individual Baryon Acoustic Oscillation?
Authors: R. Brent Tully, Cullan Howlett, Daniel Pomarède
Figure caption: Top panel: a composite of single BAO features found in the 256 simulations we explore, restricting to simulations with positive BAO detections B  r,s  > 0, where we have scaled the radius of the BAO shell by the parameter α to align them for clarity. The red line shows the BAO model averaged over each of the fits to the individual detections. The dashed vertical line is the expected BAO radius given the input cosmology of the simulation. Middle panel: a histogram of the recovered α values from fitting these single BAO features with the model from Section 2.1.1, where the solid line is a Gaussian fit to the distribution with the mean given by the dotted line. Bottom panel: a histogram of the standard deviation in best-fit α measured from features within each single mock (i.e., we measure 256 values of the standard deviation from our 256 mocks). The black shaded region shows our baseline error on α from Ho’oleilana, while the dashed line is the standard deviation measured from across all features and mocks (i.e., all the measurements shown in the middle panel).
Paper: Ho’oleilana: An Individual Baryon Acoustic Oscillation?
Authors: R. Brent Tully, Cullan Howlett, Daniel Pomarède
Figure caption: Cosmological constraints from fitting Ho’oleilana with a BAO model using the uncertainty from Ho’oleilana alone allowing for uncertainty in the central location (blue) or using the the scatter seen in BAO simulations as the uncertainty fixing to our most likely center for Ho’oleilana (red). α is our BAO scaling parameter, D  v /r drag is the ratio between the distance to the center of Ho’oleilana and its size, while z is the redshift to its center. From these pieces of information, and assuming constraints on r drag from early Universe physics, we obtain constraints on the matter content Ω m  and present-day expansion rate of the Universe H 0 that favor other local direct measurements (orange band) rather than that propagated from models of the early Universe (green band).
Paper: Ho’oleilana: An Individual Baryon Acoustic Oscillation?
Authors: R. Brent Tully, Cullan Howlett, Daniel Pomarède
Figure caption: A normalized histogram of the number of galaxies as a function of distance from the center of Ho’oleilana. Error bars are computed using simulations fully reproducing the selection function of the data. Ho’oleilana, at a distance ﹩r\approx 150\,{h}_{75}^{-1}\,\mathrm{Mpc}﹩ from the central location, is well fit by a physical BAO model (red line). Compared to the expectations for a random field of galaxies (blue line), Ho’oleilana is detected at greater than 6σ significance as shown by the relative difference in χ 2 statistic.
Paper: Ho’oleilana: An Individual Baryon Acoustic Oscillation?
Authors: R. Brent Tully, Cullan Howlett, Daniel Pomarède
Figure caption: Histograms of the χ 2 difference between models for the radial distributions of galaxies with and without the BAO feature fit to the central location with the largest value of W  r,s  in each no-BAO mock. The dashed line shows the value from fitting Ho’oleilana in Section 2.1.1. The blue histogram shows results allowing for any value of r BAO and s BAO. The red histogram is conditioned on ﹩{r}_{\mathrm{BAO}}=155\,{{\rm{h}}}_{75}^{-1}\,\mathrm{Mpc}﹩ and ﹩{s}_{\mathrm{BAO}}=27\,{{\rm{h}}}_{75}^{-1}\,\mathrm{Mpc}﹩, the radius and width that returns the largest value of W  r,s  in the data, corresponding Ho’oleilana.
Paper: Ho’oleilana: An Individual Baryon Acoustic Oscillation?
Authors: R. Brent Tully, Cullan Howlett, Daniel Pomarède
Figure caption: A histogram of the weights W  r,s  for a BAO wavelet with radius ﹩{r}_{\mathrm{BAO}}=155\,{{\rm{h}}}_{75}^{-1}\,\mathrm{Mpc}﹩ and width ﹩{s}_{\mathrm{BAO}}=27\,{{\rm{h}}}_{75}^{-1}\,\mathrm{Mpc}﹩. The weights are normalized by the standard deviation across the full sample, and positive values correspond to grid locations that demonstrate an overabundance of galaxies distributed within a BAO-like shell. There is a clear excess of positive weights in the data (black) compared to the average and standard deviation of the no-BAO mocks (blue). The dotted line shows a Gaussian distribution—both the BAO and no-BAO mocks display a non-Gaussian tail of large overdensities. The largest positive weight corresponds to Ho’oleilana.
Paper: Ho’oleilana: An Individual Baryon Acoustic Oscillation?
Authors: R. Brent Tully, Cullan Howlett, Daniel Pomarède
Figure caption: A comparison of the expansion rate of the Universe as a function of redshift from Ho’oleilana compared to other statistical BAO measurements (Beutler et al. 2011; Ross et al. 2015; Alam et al. 2017), assuming a prior on the BAO size from early Universe physics. Bright and faint points represent our measurements using the uncertainty from Ho’oleilana alone, or taking the scatter from BAO simulations as the error, respectively. The solid band shows the predicted expansion rate for a ΛCDM cosmological model from Planck Collaboration et al. (2020).
Paper: Fast Radio Bursts as Probes of Magnetic Fields in Galaxies at z < 0.5
Authors: Alexandra G. Mannings, Rüdiger Pakmor, J. Xavier Prochaska, Freeke van de Voort, Sunil Simha, R. M. Shannon, Nicolas Tejos, Adam Deller, Marc Rafelski
Figure caption: RM and DM distributions for lines of sight from matched host galaxies in Auriga. The name of the matched FRB host and the number of matching Auriga galaxies found are listed above each panel. Shown are histograms of the DM values (solid red lines) and absolute RM values (solid purple lines) along each line of sight. The vertical red and purple lines indicate the observed or derived RMhost and ﹩{\mathrm{DM}}_{\mathrm{host}}^{\mathrm{Macquart}}﹩ values. We also show histograms of absolute RM values that include only lines of sight with a consistent DM value (dashed yellow lines; absent in panels where no consistent DM was found). The RM distributions predicted from the Auriga galaxies are generally in good agreement with the observed values, with the glaring exception of FRB20121102A whose RM value is far away from any lines of sight we find in Auriga. The modeled RM pdf for FRB20190608B is also noticeably lower than the observed value. The derived ﹩{\mathrm{DM}}_{\mathrm{host}}^{\mathrm{Macquart}}﹩ value for FRB20180924B is negative; therefore, there is no vertical line shown here.
Paper: Fast Radio Bursts as Probes of Magnetic Fields in Galaxies at z < 0.5
Authors: Alexandra G. Mannings, Rüdiger Pakmor, J. Xavier Prochaska, Freeke van de Voort, Sunil Simha, R. M. Shannon, Nicolas Tejos, Adam Deller, Marc Rafelski
Figure caption: RMhost and DMhost,ISM with lines of constant magnetic field strength (1 μG, dashed; 5 μG, dotted; 10 μG, dashed–dotted). We calculate the value of B ∥ for each of the FRBs using Equation (8). The majority of the values are less than 5 μG, with many even falling below 1 μG. There is one outlier, with a field magnitude far exceeding 10 μG. These values are relatively consistent with microgauss fields, but are at the lower end of the range of 1–15 μG.
Paper: Observational Signatures of Electron-driven Chromospheric Evaporation in a White-light Flare
Authors: Dong Li, Chuan Li, Ye Qiu, Shihao Rao, Alexander Warmuth, Frederic Schuller, Haisheng Zhao, Fanpeng Shi, Jun Xu, Zongjun Ning
Figure caption: Panels (a) and (b): STIX 16−28 keV and AIA 94 Å maps during the solar flare. The magenta contours represent HXR emissions at levels of 70% and 90%. The dashed white lines indicate latitude–longitude grids, and the solid white line marks the solar limb. The green circle is a visibility forward fit for the HXR source area. The cyan dashed line outlines the IRIS slit, the blue and red contours denote Hα and Fe I kernels. Panel (c): STIX X-ray spectrum between 4 and 28 keV with an integrated time of 20 s, the fitted thermal (green) and nonthermal (blue) components, as well as the sum of both components (red). The low-energy cutoff (E  c ), spectral index (δ), and the chi-squared residual (χ 2) are labeled. Panel (d): the magnetic configuration from the SDO viewpoint with a potential field source surface (PFSS) model. The white and purple lines represent the closed and open magnetic fields, respectively. The gold arrow indicates the short flare loop.
Paper: Observational Signatures of Electron-driven Chromospheric Evaporation in a White-light Flare
Authors: Dong Li, Chuan Li, Ye Qiu, Shihao Rao, Alexander Warmuth, Frederic Schuller, Haisheng Zhao, Fanpeng Shi, Jun Xu, Zongjun Ning
Figure caption: Time–distance images of line intensity, Doppler velocity, and line width from IRIS spectra, e.g., Fe XXI, C I, and Si IV. Two short black lines outline the flare region used to integrate the time series in Figure 8. Green and cyan contours represent the CHASE observations at Fe I and Hα. A logarithmic scale is used for the line intensity.
Paper: Observational Signatures of Electron-driven Chromospheric Evaporation in a White-light Flare
Authors: Dong Li, Chuan Li, Ye Qiu, Shihao Rao, Alexander Warmuth, Frederic Schuller, Haisheng Zhao, Fanpeng Shi, Jun Xu, Zongjun Ning
Figure caption: Time series of the Doppler velocity in Fe XXI (black) and Si IV (red), and the normalized HXR fluxes at GECAM 20−60 keV (cyan) and STIX 15−25 keV (green), and the normalized white-light flux at CHASE Fe I (brown). The blue and magenta dots mark these HXR points used to perform the correlation analysis. Panel (b): scatterplots of Doppler velocities of Fe XXI (circles) and Si IV (diamonds) depend on the HXR fluxes observed by GECAM (fill) and STIX (hollow). Their Pearson correlation coefficients (cc.) are labeled.
Paper: Observational Signatures of Electron-driven Chromospheric Evaporation in a White-light Flare
Authors: Dong Li, Chuan Li, Ye Qiu, Shihao Rao, Alexander Warmuth, Frederic Schuller, Haisheng Zhao, Fanpeng Shi, Jun Xu, Zongjun Ning
Figure caption: Time–distance images along the solar jet, which are performed from SDO and IRIS maps at wavelengths of AIA 304 Å (a), 171 Å (b), 193 Å (c), 211 Å (d), and 335 Å (e), and SJI 1400 Å (f). The black and cyan arrows indicate the rise and fall speeds of the solar jet.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: (a) 1.3 mm continuum emission map with a robust parameter of 0.0. The contours levels are 3, 6, 12, 24, ... ×σ, where σ = 0.020 mJy beam−1. Dashed boxes show the zoom-in areas, shown in panels (c) and (d). (b) 1.3 mm continuum emission map with a robust parameter of 2.0. The contour level is 3σ, where σ = 0.018 mJy beam−1. (c) Zoom-in view of the continuum emission associated with Ced110 IRS4A with a robust parameter of 0.0. The contour levels are the same as in panel (a). (d) Zoom-in view of the continuum emission associated with Ced110 IRS4B with a robust parameter of 0.0. The contour levels are 3, 6, 9, 12, 15, ... ×σ. Note that the color scales are in an asinh stretch in panels (a) and (b) to cover a wide dynamic range, while they are in a linear scale in panels (c) and (d). In all panels, white ellipses at the bottom left corners denote the synthesized beam size.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Moment zero and one maps of the C18O J = 2–1 emission (color) overlaid with the 1.3 mm continuum maps (contours). Panels (a) and (c) show zoom-in and wide views of the moment zero map, and panels (b) and (d) show zoom-in and wide views of the moment one map, respectively. The 1.3 mm continuum maps with robust parameters of 0.0 and 2.0 are overlaid on the zoom-in and wide views of the moment maps, respectively. The contour levels are the same as those of Figure 1(a) and (b). The filled and opened ellipses at the bottom left corners represent the synthesized beam sizes of the C18O and continuum maps, respectively.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Intensity profiles of the 1.3 mm continuum emission associated with Ced110 IRS4A along the (a) major and (b) minor axes. A 1σ uncertainty in the intensity is comparable to the width of the solid lines. The bars at the bottom right corners denote the FWHMs of the synthesized beam along the directions of the slices.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Intensity profiles of the 1.3 mm continuum emission associated with Ced110 IRS4B along the major and minor axes. The shaded regions indicate the 1σ uncertainties. The horizontal dashed line indicates the 3σ level. The purple and green bars at the bottom right corner denote the FWHMs of the synthesized beam along the major and minor axes, respectively.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Comparison between the smooth model and the observed continuum map of Ced110 IRS4A. (a) The model image before the beam convolution and (b) the residual image normalized by σ. The contours start from 3σ and increase in steps of 3σ. The dashed contours indicate the negative residuals. The dashed lines across the maps show the directions of the continuum major and minor axes. The white ellipse at the bottom left corner in panel (b) denotes the synthesized beam size. (c) One-dimensional intensity and residual profiles along the continuum major axis with a cut width corresponding to the size of one pixel (∼1/10 beam size). The horizontal dashed lines indicate ±3σ. The bar in the bottom right corner represents the FWHM of the synthesized beam along the continuum major axis.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Results of the fitting of a two-dimensional Gaussian function to the dust continuum emission of Ced110 IRS4B. (a) Image of the deconvolved Gaussian and (b) residual image normalized by σ. The solid and dashed contours indicate 3σ and −3σ, respectively. The white ellipse at the bottom left corner denotes the synthesized beam size. The dashed lines across the maps in panels (a) and (b) show the directions of the continuum major and minor axes. (c) One-dimensional intensity and residual profiles along the continuum major axis with a cut width corresponding to the size of one pixel (∼1/10 beam size). The horizontal dashed lines indicate ±3σ. The bar in the bottom right corner represents the FWHM of the synthesized beam along the continuum major axis.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Position–velocity diagrams of (a) C18O and (b) 13CO emission of Ced110 IRS4A cut along its continuum major axis. The contour levels are from 3σ to 12σ in steps of 3σ. The dashed contours represent negative intensities. The round and triangle markers denote the determined ridges and edges, respectively. The color of the marker indicates the properties of the data points: blue and red markers show measurements of positions at a given velocity; cyan and pink markers show measurements of velocities at a given offset; blue and cyan markers indicate measurements at blueshifted velocity; and red and pink markers indicate measurements at redshifted velocity. The solid and dashed curves show the power-law functions representing the best fits to the ridges and edges, respectively. The vertical and horizontal bars in the bottom left corners represent the FWHM of the synthesized beam and the velocity resolution, respectively.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Position–velocity diagrams of (a) C18O and (b) 13CO emission of Ced110 IRS4B cut along its continuum major axis. The contour levels are from 3σ to 12σ in steps of 3σ. The dashed contours represent negative intensities. The solid and dashed curves correspond to Keplerian rotation with a central mass of 0.02 and 0.05 M ⊙, respectively, without correction of the inclination angle. The vertical and horizontal bars in the bottom left corners represent the FWHM of the synthesized beam and the velocity resolution, respectively.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Spectra of the C18O and 13CO J = 2–1 lines measured within a radius of 0.″15 around Ced110 IRS4B. The curves show the best-fit Gaussian functions.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: (a) Moment zero and (b) one maps of the SO emission (color) overlaid with the 1.3 mm continuum maps with a robust parameter of 2.0 (contours). The contour levels are as the same as those of Figure 1(b). The filled and opened ellipses at the bottom left corners represent the synthesized beam sizes of the SO and continuum maps, respectively.