adsabs/AstroCLIMB huggingface dataset:
Paper: Ho’oleilana: An Individual Baryon Acoustic Oscillation?
Authors: R. Brent Tully, Cullan Howlett, Daniel Pomarède
Figure caption: Top panel: the power spectrum of the SDSS PV data compared to the average from sets of simulations with similar large-scale structure and selection effects, with and without the presence of BAOs. Our method for populating the simulations with mock galaxies is tuned to this data, so we also report the χ 2 difference for the two sets of simulations. Bottom panel: the average of the ratio of the power spectra for our BAO and no-BAO simulations. For reference, the black dotted line shows the linear theory model smoothed with a nonlinear damping of 13 ﹩{h}_{75}^{-1}﹩ Mpc (see Section 2.1.1), which clearly demonstrates that the BAO is being suppressed in the no-BAO simulations. Note that the linear theory model has not been corrected for selection effects and galaxy bias so is not expected to match the amplitude of the data.
Paper: Ho’oleilana: An Individual Baryon Acoustic Oscillation?
Authors: R. Brent Tully, Cullan Howlett, Daniel Pomarède
Figure caption: Top panel: supergalactic SGX−SGZ projection of all northern Cosmicflows-4 galaxies with 19,000 < V cmb < 26,000 km s−1. Bottom panel: same as the top panel with the addition in red of a circle of radius 11,300 km s−1 centered at SGX c  = −400 km s−1, SGZ c  = 5000 km s−1 and blue crosses at the locations of Abell clusters A1781, A1795, A1825, and A1831.
Paper: Ho’oleilana: An Individual Baryon Acoustic Oscillation?
Authors: R. Brent Tully, Cullan Howlett, Daniel Pomarède
Figure caption: Top panel: histogram of numbers of galaxies in the systemic velocity window 19,000−26,000 km s−1 as a function of radius from a center at SGX c  = –400 km s−1, SGZ c  = 5000 km s−1 in 100 km s−1 bins. Numbers are normalized by the area within each 100 km s−1 bin. Bottom panel: histogram of velocities in 100 km s−1 bins of groups that are projected into a ring of width with bounds 10,600−12,000 km s−1 centered at SGX c  = –400 km s−1, SGZ c  = 5000 km s−1.
Paper: Ho’oleilana: An Individual Baryon Acoustic Oscillation?
Authors: R. Brent Tully, Cullan Howlett, Daniel Pomarède
Figure caption: Zoom of Figure 21 from Tully et al. (2023) in the galactic north sector showing the distribution of Cosmicflows-4 galaxy groups in supergalactic coordinates.
Paper: The Sun’s Magnetic Power Spectra over Two Solar Cycles. I. Calibration between SDO/HMI and SOHO/MDI Magnetograms
Authors: Yukun Luo, Jie Jiang, Ruihui Wang
Figure caption: The same as Figure 2, but for CR 2100 (left) and CR 2102 (right).
Paper: The Sun’s Magnetic Power Spectra over Two Solar Cycles. I. Calibration between SDO/HMI and SOHO/MDI Magnetograms
Authors: Yukun Luo, Jie Jiang, Ruihui Wang
Figure caption: The same as Figure 2, but for CR 2103 (left) and CR 2104 (right).
Paper: Analysis of Solar-like X-class Flare on Wolf 359 Observed Simultaneously with TESS and XMM-Newton
Authors: M. Pietras, R. Falewicz, M. Siarkowski, A. Kepa, K. Bicz, P. Preś
Figure caption: Upper panel: average observed spectrum of the analyzed flare (in black). Gray stripes correspond to the spectral bands used for the DEM determination. The colors show the spectra calculated based on DEM distribution (Figure 4) using two abundance sets from Scott et al. ( 2015a, 2015b), in blue and Fuhrmeister et al. (2007), in red. Bottom left: DEM distributions determined based on unperturbed line fluxes (colors) and the 100 Monte Carlo realizations of DEM calculations (gray) when elemental abundances by Fuhrmeister et al. (2007) were used. Red and blue colors represent the results obtained using two abundance sets from Scott et al. (2015a, 2015b) and Fuhrmeister et al. (2007), respectively. Bottom right: the O VII triplet in the RGS spectrum on 2021 December 21. Red lines denote the Gaussian profiles fitted for each line.
Paper: Analysis of Solar-like X-class Flare on Wolf 359 Observed Simultaneously with TESS and XMM-Newton
Authors: M. Pietras, R. Falewicz, M. Siarkowski, A. Kepa, K. Bicz, P. Preś
Figure caption: Left panel: the TESS light curve of Wolf 359 (sectors 45 and 46). Detected flares are marked with orange triangles, XMM-Newton observational interval in green, and the analyzed flare in red. Right panel: the light curve of the flare on Wolf 359 in white light, UV, and X-ray (0.2–12 keV). TESS 2 minute cadence data are shown in black and XMM-Newton data binned to 2 minutes are in violet and red. The vertical colored lines mark the maximum of the flare in different energy ranges (black–white light, violet–UV, red–X-rays). The maximum of the flare in the white-light range was at 11:28 UT, in the ultraviolet at 11:26 UT, and in X-rays at 11:33 UT. The pre-flare is marked as red arrows.
Paper: Analysis of Solar-like X-class Flare on Wolf 359 Observed Simultaneously with TESS and XMM-Newton
Authors: M. Pietras, R. Falewicz, M. Siarkowski, A. Kepa, K. Bicz, P. Preś
Figure caption: The location of the analyzed flare on the diagram EM vs. heating (E  H ). The added X-class solar flares are marked in red. The flare on Wolf 359 is marked with a blue star. The solid line shows the new EM–E  H  relationship based on all flares.
Paper: Analysis of Solar-like X-class Flare on Wolf 359 Observed Simultaneously with TESS and XMM-Newton
Authors: M. Pietras, R. Falewicz, M. Siarkowski, A. Kepa, K. Bicz, P. Preś
Figure caption: Left: the light curves and flare profiles in two X-ray ranges. The range from 0.2–1 keV is shown in dark blue, and 1–4 keV in light blue. The time binning of the data was 100 s. Right: the flare EPIC-pn profiles (light and dark blue) and the TESS 100 s light curve (red) compared with the average flare single profile from Pietras et al. (2022) (black).
Paper: Analysis of Solar-like X-class Flare on Wolf 359 Observed Simultaneously with TESS and XMM-Newton
Authors: M. Pietras, R. Falewicz, M. Siarkowski, A. Kepa, K. Bicz, P. Preś
Figure caption: The diagnostic diagram of the flare (﹩\mathrm{log}\sqrt{\mathrm{EM}}﹩ vs. ﹩\mathrm{log}{T}_{\mathrm{obs}}﹩). The emission measure and temperature are expressed in cm−3 and K, respectively. Quantities in logarithms are dimensionless. The green line shows the best fit with the slope ζ = 0.39 ± 0.24 for the decay phase (red stars) and the red line represents the slope of the quasi-stationary decay (ζ QSS = 0.35). The green-shaded region shows the confidence interval.
Paper: Analysis of Solar-like X-class Flare on Wolf 359 Observed Simultaneously with TESS and XMM-Newton
Authors: M. Pietras, R. Falewicz, M. Siarkowski, A. Kepa, K. Bicz, P. Preś
Figure caption: Relationship between the GOES flare class and the half-length of the flare loops for 24 solar events analyzed in Warmuth & Mann (2013) represented by red squares. At each point, there is also a description of the GOES flare class. The error ranges are marked in blue and the L 0 value for the analyzed flare on the star Wolf 359 is marked with the diamond symbol.
Paper: Analysis of Solar-like X-class Flare on Wolf 359 Observed Simultaneously with TESS and XMM-Newton
Authors: M. Pietras, R. Falewicz, M. Siarkowski, A. Kepa, K. Bicz, P. Preś
Figure caption: Left panel: the best fit to the light curve of the rise phase. The data are binned every 50 s. The estimated thermodynamical time is τ th = 106.6 ± 12.6 s and the saturation flux F ss = 6.47 ± 0.35  cts s−1. The black dots indicate the points used in the fit function for the rise phase. Right panel: the best fit of the exponential decay to the light curve of the decay phase. The data are binned every 50 s. The estimated thermodynamical time should not be greater than τ th = 104.7  s. The black dots indicate the points used in the fit function for the decay phase.
Paper: Analysis of Solar-like X-class Flare on Wolf 359 Observed Simultaneously with TESS and XMM-Newton
Authors: M. Pietras, R. Falewicz, M. Siarkowski, A. Kepa, K. Bicz, P. Preś
Figure caption: Left: the temperature estimated during the analyzed flare from EPIC-pn X-ray data. The straight line before the beginning of the flare shows the mean temperature. The actual values could not be reliably determined due to the high data noise. Right: the emission measure estimated during the analyzed flare from EPIC-pn X-ray data. The straight line before the beginning of the flare shows the mean emission measure. The actual values could not be reliably determined due to the high data noise.
Paper: An Unsupervised Machine Learning-based Algorithm for Detecting Weak Impulsive Narrowband Quiet Sun Emissions and Characterizing Their Morphology
Authors: Shabbir Bawaji, Ujjaini Alam, Surajit Mondal, Divya Oberoi, Ayan Biswas
Figure caption: Top left-hand panel: Δχ 2 is plotted against the distance of the point from the centroid of the reference cluster in the t-SNE plane. Top right-hand panel: histogram of Δχ 2 for three chosen clusters, yellow (adjacent to the reference cluster), black (farthest cluster from the reference cluster), and purple (a cluster at an intermediate distance). Bottom panel: shows the fraction of good fits. The X-axis corresponds to the fitting results shown in the manuscript where the fitting window is chosen based on the mean hyper-parameters of the cluster to which the point belongs. The Y-axis corresponds to the case when the same fitting window is used for all points. The orange line defines the case where the original fit and reference fit are identical. The color scheme for all panels is the same as that in Figure 9.
Paper: An Unsupervised Machine Learning-based Algorithm for Detecting Weak Impulsive Narrowband Quiet Sun Emissions and Characterizing Their Morphology
Authors: Shabbir Bawaji, Ujjaini Alam, Surajit Mondal, Divya Oberoi, Ayan Biswas
Figure caption: The figure shows a zoomed in view of an example WINQSE to demonstrate the quality of Gaussian fit. The left-hand panel shows the contours of the actual image in black and those corresponding to the best-fit Gaussian model are shown in white. The middle panel shows the residual of the Gaussian fit. The contours mark 78.3%, 85.6%, 90.5%, and 95.4% of the peak. The residuals lie in the range ±5% in the regions where the Gaussian has a significant amplitude and increase to ±10% toward the edges of the image. Right-hand panel: Distribution of the reduced χ 2 for peaks in the three chosen groups from Figure 9.
Paper: An Unsupervised Machine Learning-based Algorithm for Detecting Weak Impulsive Narrowband Quiet Sun Emissions and Characterizing Their Morphology
Authors: Shabbir Bawaji, Ujjaini Alam, Surajit Mondal, Divya Oberoi, Ayan Biswas
Figure caption: The purple circles mark the actual regions used by M20 for detecting WINQSEs. The red and black dots show two example locations of WINQSEs chosen to demonstrate the weaknesses of the detection method employed by M20.
Paper: An Unsupervised Machine Learning-based Algorithm for Detecting Weak Impulsive Narrowband Quiet Sun Emissions and Characterizing Their Morphology
Authors: Shabbir Bawaji, Ujjaini Alam, Surajit Mondal, Divya Oberoi, Ayan Biswas
Figure caption: Histograms of characteristics for the 20200620 data set with frequency 120.52 MHz. Blue denotes all the peaks fitted, orange denotes the peaks that are dissimilar to the psf.
Paper: An Unsupervised Machine Learning-based Algorithm for Detecting Weak Impulsive Narrowband Quiet Sun Emissions and Characterizing Their Morphology
Authors: Shabbir Bawaji, Ujjaini Alam, Surajit Mondal, Divya Oberoi, Ayan Biswas
Figure caption: Histograms of characteristics for the 20171127 data set with frequency 132 MHz for peaks dissimilar to the psf.
Paper: An Unsupervised Machine Learning-based Algorithm for Detecting Weak Impulsive Narrowband Quiet Sun Emissions and Characterizing Their Morphology
Authors: Shabbir Bawaji, Ujjaini Alam, Surajit Mondal, Divya Oberoi, Ayan Biswas
Figure caption: Distribution of ΔF/F for WINQSEs detected within the solar boundary for the 20200620 data set at 120.52 MHz, 128.2 MHz, 135.9 MHz and 143.6MHz.
Paper: An Unsupervised Machine Learning-based Algorithm for Detecting Weak Impulsive Narrowband Quiet Sun Emissions and Characterizing Their Morphology
Authors: Shabbir Bawaji, Ujjaini Alam, Surajit Mondal, Divya Oberoi, Ayan Biswas
Figure caption: Histograms of best-fit Gaussian parameters for the 20200620 data set for 120.52 MHz, 128.20 MHz, 135.90 MHz, and 143.60 MHz (top to bottom) for peaks dissimilar to the psf.
Paper: An Unsupervised Machine Learning-based Algorithm for Detecting Weak Impulsive Narrowband Quiet Sun Emissions and Characterizing Their Morphology
Authors: Shabbir Bawaji, Ujjaini Alam, Surajit Mondal, Divya Oberoi, Ayan Biswas
Figure caption: Shows the data presented in Figure 7 at a resolution similar to that shown in M23.
Paper: An Unsupervised Machine Learning-based Algorithm for Detecting Weak Impulsive Narrowband Quiet Sun Emissions and Characterizing Their Morphology
Authors: Shabbir Bawaji, Ujjaini Alam, Surajit Mondal, Divya Oberoi, Ayan Biswas
Figure caption: Distribution of the reduced χ 2 for WINQSEs detected within the solar boundary for the 20200620 data set at 120.52 MHz.
Paper: Alignments between Galaxies and the Cosmic Web at z ∼ 1–2 in the IllustrisTNG Simulations
Authors: Benjamin Zhang, Khee-Gan Lee, Alex Krolewski, Jingjing Shi, Benjamin Horowitz, Robin Kooistra
Figure caption:  Z1_FID                         ﹩\langle | \cos \theta | \rangle ﹩ summary box plot for the true density field and mock reconstruction stages for shape alignments. The 3D mean alignments are shown in the top row, while the projected mean alignments are shown in the bottom row. The null distribution’s ﹩\langle | \cos \theta | \rangle ﹩ is marked with a dashed line for both rows. The box plot whiskers have been modified to display 16th and 84th percentiles ﹩\langle | \cos \theta | \rangle ﹩.
Paper: Alignments between Galaxies and the Cosmic Web at z ∼ 1–2 in the IllustrisTNG Simulations
Authors: Benjamin Zhang, Khee-Gan Lee, Alex Krolewski, Jingjing Shi, Benjamin Horowitz, Robin Kooistra
Figure caption: The PDF of ﹩| \cos \theta | ﹩ between true and TARDIS-reconstructed eigenvectors for each point in the reconstructed IllustrisTNG volume. Along with the z = 1 and joint z = 2 reconstructions used for the final analysis, we include a Lyα forest–only reconstruction at z = 2 for comparison. Each viewing angle’s reconstruction is separately plotted as a semitransparent line. In the case of a perfect reconstruction, the PDF would be a delta function at ﹩| \cos \theta | =1﹩ for each of the panels.
Paper: Alignments between Galaxies and the Cosmic Web at z ∼ 1–2 in the IllustrisTNG Simulations
Authors: Benjamin Zhang, Khee-Gan Lee, Alex Krolewski, Jingjing Shi, Benjamin Horowitz, Robin Kooistra
Figure caption: The TNG300-1 ﹩{\hat{{\boldsymbol{e}}}}_{{\bf{3}}}﹩–shape mean alignment at z = 1 as a function of density smoothing scale. We use the magnitude-selected Z1_FID galaxy sample but do not apply any mock observational effects. Errors are derived from bootstrap resampling (but do not include any viewing-angle effects).
Paper: Alignments between Galaxies and the Cosmic Web at z ∼ 1–2 in the IllustrisTNG Simulations
Authors: Benjamin Zhang, Khee-Gan Lee, Alex Krolewski, Jingjing Shi, Benjamin Horowitz, Robin Kooistra
Figure caption: Standard deviation of projected z = 1 real-space mean alignment σ VA computed from 64 viewing angles of the same subvolumes, plotted as a function of subvolume side length. As we divide the TNG300 volume into nonoverlapping subvolumes, we can also plot the error on σ VA. The data are consistent with a power law with fixed exponent β = −1.5, which is equivalent to a β = −0.5 power law against volume.
Paper: Alignments between Galaxies and the Cosmic Web at z ∼ 1–2 in the IllustrisTNG Simulations
Authors: Benjamin Zhang, Khee-Gan Lee, Alex Krolewski, Jingjing Shi, Benjamin Horowitz, Robin Kooistra
Figure caption: Cumulative density function of alignment between the spin and three shape ellipsoid axes of TNG300-1 and TNG100-1 galaxies at z = 1. The TNG galaxy sample is the same as Figure 3, with a minimum-mass cut of M * > 108.06 h −1 M ⊙ to match Codis et al. (2015).
Paper: Alignments between Galaxies and the Cosmic Web at z ∼ 1–2 in the IllustrisTNG Simulations
Authors: Benjamin Zhang, Khee-Gan Lee, Alex Krolewski, Jingjing Shi, Benjamin Horowitz, Robin Kooistra
Figure caption: Cartoon illustrating viewing-angle variance on alignments caused by cosmic variance. For the small simulation volume depicted here with a filament running through it, galaxies are highly aligned with the filament in 3D. This extends to the projected alignment when looking “side-on” to the filament (left panel). However, if we view the volume “face-on” to the filament (right panel), the projected alignment is nearly random.
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: Intensity profiles of the 1.3 mm continuum emission of IRS5N shown in Figure 1(b) and the double-Gaussian component model shown in Figure 9. The solid line represents the observed emission, and the dashed line represents the model. The blue lines indicate the intensity along the major axes, and the orange lines represent the intensity along the minor axes. The smaller plot at the bottom shows the residual intensity after subtracting the model from the observation. The shaded region and the horizontal dotted lines indicate ±3σ uncertainties with σ = 0.016 mJy beam−1.
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: Zoomed-in moment-0 maps of 12CO emission (a) around the IRS5 binary source and 13CO emission (b) around the IRS5 binary source. The crosses represent the peak position of the continuum emission of IRS5a and IRS5b sources. The maps are created by integrating over the velocity ranges of −4.75–14.93 km s−1 and 2.85–9.86 km s−1 for 12CO and 13CO, respectively. The synthesized beam is shown in black in the bottom right corner of each image.
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: Channel maps showing the 12CO emission around the two sources of the IRS5 system. The yellow and green stars show the peak position of the continuum emission of IRS5a and IRS5b, respectively. The numbers at the top show the corresponding velocity of each channel map. The synthesized beam is shown in black in the bottom right corner of the final channel map.
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: IRS5N disk model (left) and residual (right) created using double-Gaussian components. The contours show the 3σ, 6σ, 12σ, 24σ, and 48σ. The dashed contours indicate negative intensity. The white ellipse in the bottom right corner of each image shows the synthesized beam.
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: Zoomed-in moment-0 (left) and moment-1 (right) maps of 12CO (top) and 13CO (bottom) emission. The maps are created by integrating over the velocity ranges of −5.38 to 20.65 km s−1 and 0.51–12.03 km s−1 for 12CO and 13CO , respectively. The cross represents the peak position of the IRS5N continuum. The synthesized beam is shown in black in the bottom right corner of each image.
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: Selected channel maps showing the C18O (2–1) emission around IRS5N. The numbers at the top show the corresponding velocity of each channel map. The cross shows the peak position of the IRS5N continuum. The synthesized beam is shown in black in the bottom right corner of the final channel.
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 5, but for H2CO (30,3–20,2). The maps are created by integrating over the velocity ranges of 2.06–8.76 km s−1.
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: PV diagram of C18O emission toward IRS5N cut along its major axis. The points derived using the edge and ridge methods and their corresponding rotation curves are shown in blue and red, respectively. The black contours start at the 3σ level and increase every 2σ. The dashed contours show the corresponding negative contours.