adsabs/AstroCLIMB huggingface dataset:
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: Our spectra for stars from the SSPS sample of Hamuy et al. (1992, 1994). The presentation follows that of Figure 17.
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: Our spectra of space-based CALSPEC stars that were not used as primary calibrators or had observations on two or fewer nights. The presentation follows that of Figure 17.
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: Our spectra for stars from Oke (1990) that were used as secondary calibrators. The presentation follows that of Figure 17.
Paper: Statistical Study and Live Catalog of Multispacecraft 3He-rich Time Periods over Solar Cycles 23, 24, and 25
Authors: S. T. Hart, M. A. Dayeh, R. Bučík, M. I. Desai, R. W. Ebert, G. C. Ho, G. Li, G. M. Mason
Figure caption: Same format as Figure 1, but for an ISEP event observed by STEREO-A at the start of 2010 August 24. Note again that the Fe and O flux temporal profiles overlap in (a). Comparing (b) to Figure 1(b), it is clear that the mass resolution of STEREO/SIT is broader than that of ACE/ULEIS. To help clarify the 3He enhancement, we include the time-integrated mass histogram (d) of the contents within the green box to highlight the 3He “shoulder” next to the 4He peak. For more detailed images, see Section 3.2.2.
Paper: Statistical Study and Live Catalog of Multispacecraft 3He-rich Time Periods over Solar Cycles 23, 24, and 25
Authors: S. T. Hart, M. A. Dayeh, R. Bučík, M. I. Desai, R. W. Ebert, G. C. Ho, G. Li, G. M. Mason
Figure caption: (a) Hourly flux values of 4He, O, and Fe at 0.19 MeV nucleon−1, clearly showing an overlapping flux temporal profile of Fe and O commonly observed in 3He-rich SEP events. (b) Mass spectrogram between 2 and 80 amu with an energy range of 0.32–3.6 MeV nucleon−1. The most common species are labeled on the right side of the plot. Starting at DOY 273.3 (dashed vertical line), the mass spectrogram shows an enhancement of all of the most common species, most notably 3He, signaling an observation of a 3He-rich SEP event that lasts for a few days. (c) One-over-ion speed plot of masses 10–80 amu. The red axis on the right side of the plot shows the energy per nucleon that corresponds to the inverse speed. The slanted red line shows the approximate arrival times of particles with different energies. The dispersion’s intersection with the time axis yields the injection time (red arrow), and the slope reveals the path length of the ion travel to 1 au.
Paper: PROBES. I. A Compendium of Deep Rotation Curves and Matched Multiband Photometry
Authors: Connor Stone, Stéphane Courteau, Nikhil Arora, Matthew Frosst, Thomas H. Jarrett
Figure caption: Comparison of SB errors for the multiband GALEX, DESI-LIS, and unWISE photometry as a function of SB depth. Scatter points were taken from every profile in the PROBES photometry sample, while contours were used in high-density regions. Most SB profiles reach at least 26  mag arcsec−2  before errors start to rise; some profiles reach 30  mag arcsec−2  with small errors. This deep multiband photometry critically maximizes the scientific potential of the PROBES photometric data set.
Paper: PROBES. I. A Compendium of Deep Rotation Curves and Matched Multiband Photometry
Authors: Connor Stone, Stéphane Courteau, Nikhil Arora, Matthew Frosst, Thomas H. Jarrett
Figure caption: Example r-band SB profile for ESO143-G028 with various radial metrics indicated with arrows. For instance, isophotal radii correspond to SB levels ranging from 22 to 26 mag arcsec−2  in steps of 0.5 mag arcsec−2 ; see text for details. These radii are evaluated for all galaxies in the PROBES photometry sample, most other structural parameters are evaluated at all of these radii. Errors on the SB profiles are not shown as they are too small.
Paper: PROBES. I. A Compendium of Deep Rotation Curves and Matched Multiband Photometry
Authors: Connor Stone, Stéphane Courteau, Nikhil Arora, Matthew Frosst, Thomas H. Jarrett
Figure caption: Distribution of velocity residuals (top), normalized by the error of the velocity measurement (bottom), for the C97 model fit to each RC in the PROBES photometry sample. Radii are normalized by the isophotal radius, R 23.5. The dashed purple lines give the 68% band of data. The axis limits are truncated to show the main trends.
Paper: PROBES. I. A Compendium of Deep Rotation Curves and Matched Multiband Photometry
Authors: Connor Stone, Stéphane Courteau, Nikhil Arora, Matthew Frosst, Thomas H. Jarrett
Figure caption: Example r-band profile truncated at the noise floor for ESO143-G028. The dashed purple lines give the exponential disk fit to the outer profile (blue points) and the SB floor (gray points). The data beyond the intersection of the exponential disk and the SB floor are ignored for further analysis. Error bars are multiplied by 5 for visibility.
Paper: PROBES. I. A Compendium of Deep Rotation Curves and Matched Multiband Photometry
Authors: Connor Stone, Stéphane Courteau, Nikhil Arora, Matthew Frosst, Thomas H. Jarrett
Figure caption: Linear least-squares fits for the inclination correction schemes applied to the PROBES magnitudes. Every point in the corresponding PROBES photometry sample SB profiles is represented in the scatter plot. Fits only include data points beyond R e. The least-squares fitted slopes give the correction factor γ  λ , and the dashed line shows the corrected trend. The bottom right panel shows that the W2–W1 color is essentially independent of inclination.
Paper: PROBES. I. A Compendium of Deep Rotation Curves and Matched Multiband Photometry
Authors: Connor Stone, Stéphane Courteau, Nikhil Arora, Matthew Frosst, Thomas H. Jarrett
Figure caption: Triangle plot giving the distribution of a selection of structural parameters for the PROBES photometry sample. (Lower triangle) The intersection of each row and column is a scatter plot of the relation between the two corresponding parameters; all parameters are shown in log scale. The diagonal gives a histogram for each parameter. (Upper triangle) The density plots show the distribution where scatter points overlap in the lower triangle. Velocities are determined with the C97 model.
Paper: PROBES. I. A Compendium of Deep Rotation Curves and Matched Multiband Photometry
Authors: Connor Stone, Stéphane Courteau, Nikhil Arora, Matthew Frosst, Thomas H. Jarrett
Figure caption: Example RCs from PROBES over a broad range of stellar masses, ﹩{M}_{26}^{* }﹩, with C97 and tanh model fits. Data points are taken directly from PROBES profiles, and the errors are scaled by a factor of 2 for visibility. PROBES RCs display a great range of shapes and sampling densities (see also Frosst et al. 2022).
Paper: PROBES. I. A Compendium of Deep Rotation Curves and Matched Multiband Photometry
Authors: Connor Stone, Stéphane Courteau, Nikhil Arora, Matthew Frosst, Thomas H. Jarrett
Figure caption: Truncated SB profiles of all seven photometric bands for ESO143-G028. Thanks to the forced photometry, each profile is evaluated using exactly the same isophotes, though each profile achieves different depths. Error bars are multiplied by 2 for visibility.
Paper: PROBES. I. A Compendium of Deep Rotation Curves and Matched Multiband Photometry
Authors: Connor Stone, Stéphane Courteau, Nikhil Arora, Matthew Frosst, Thomas H. Jarrett
Figure caption: Typical SEDs taken from the PROBES structural parameters table for a representative range of galaxy morphologies.
Paper: PROBES. I. A Compendium of Deep Rotation Curves and Matched Multiband Photometry
Authors: Connor Stone, Stéphane Courteau, Nikhil Arora, Matthew Frosst, Thomas H. Jarrett
Figure caption: Distribution of morphological T-types for the PROBES photometric sample. The legend gives the surveys in order of total number of galaxies. The distribution is peaked for Sb and Sc types, with significant contributions from the Mathewson and SCII samples. A small number of galaxies have no known morphology in NED.
Paper: PROBES. I. A Compendium of Deep Rotation Curves and Matched Multiband Photometry
Authors: Connor Stone, Stéphane Courteau, Nikhil Arora, Matthew Frosst, Thomas H. Jarrett
Figure caption: Median RCs in the PROBES compendium in stellar mass and concentration bins specified by the top and right labels. The radii and velocities were normalized (before stacking) by the r-band isophotal radius R 23.5 and velocities measured at R 23.5, V 23.5, respectively. The number of galaxies included in each bin and the mean V 23.5 of the median stack are shown as a text inset at the upper left and right sides of each panel. The radial scale is limited to 2.5R/R 23.5 to emphasize the range of shapes in the inner RCs, though many RCs extend beyond this point.
Paper: PROBES. I. A Compendium of Deep Rotation Curves and Matched Multiband Photometry
Authors: Connor Stone, Stéphane Courteau, Nikhil Arora, Matthew Frosst, Thomas H. Jarrett
Figure caption: Distribution of RC extent in the PROBES data set. The RC extent is the radial value of the last data point in each RC. The distribution is given (top axis) in physical size (kpc) or normalized (lower axis) by a fiducial radius (R e and R 23.5). Most RC profiles extend beyond 2R  e  or beyond R 23.5. The nominal extents of MaNGA and CALIFA galaxies are shown for reference.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: Example rest-frame SEDs fitted by normal-galaxy (top left), AGN (top right), quenching-galaxy (bottom left), and bursting-galaxy (bottom right) templates. The blue points and downward triangles are the observed photometry and upper limits, respectively. The orange stars are the best-fit modeled photometry in the given bands, and the thick gray lines are the best-fit models. The bottom subpanel of each panel shows the logarithm of the ratios of the observed fluxes over the model fluxes. The best-fit model for the AGN example in the top right panel is decomposed into an AGN component (green) and a galaxy component (red). In the panels other than the top left one, we also show the best-fit models with normal-galaxy templates as cyan dashed lines, and they cannot provide acceptable fits to the data. The abscissa axes of the bottom panels are truncated in the UV to help focus on the difference between the BQ and normal-galaxy models, for which the X-ray data cannot provide useful constraints. The inset plots in the bottom panels compare the best-fit SFHs of the BQ-galaxy model (gray) and normal-galaxy model (cyan). For the quenching galaxy in the bottom-left panel, the normal-galaxy model tends to assign most star formation to an early stage, and thus it cannot explain its blue optical color and red UV color simultaneously. Its quenching SFH indicates that it is generally star forming before the quenching but the SFR has dropped significantly recently. For the bursting galaxy in the bottom-right panel, the normal-galaxy model predicts that all the stars were formed recently and hence cannot explain the excess NIR emission; in contrast, the bursting model retains low-level star formation before the burst (i.e., the part of the gray SFH that visually overlaps with the abscissa axis), which contributes to the NIR emission. Another feature of this bursting galaxy is that it has a strong Hα line dominating its fourth photometric data point (counted from left to right), and we found that the normal-galaxy model cannot fully explain the excess. Hα represents the star formation activity within ∼10 Myr, and this excessive Hα feature does support a strong recent starburst (e.g., Broussard et al. 2019).
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: The distributions of sources in the UVJ color–color plane. The large points are likely quenching galaxies color-coded by their median stellar age, the blue points are likely bursting galaxies, and the cyan points, plotted as a comparison, are our whole sample in W-CDF-S. The solid line is the boundary expected to enclose quiescent galaxies in Muzzin et al. (2013) at z > 1. The dashed line is the post-starburst region in Belli et al. (2019), which is defined as the region for which the expected median stellar age is between 300 and 800 Myr, as labeled in the figure. The likely quenching galaxies are generally in the star-forming region but on top of the main star-forming locus and have an age gradient toward the quiescent region. The likely bursting galaxies are scattered across the star-forming region.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: The purity (blue) and completeness (red) of AGNs for a sample with ΔBIC2(AGN) > δ as a function of the threshold δ. The purity and completeness points are calculated by calibration over the CDF-S data, and the associated error bars represent their binomial proportion confidence intervals. The black horizontal line marks a purity of 75%, which is roughly the plateau that the purity can reach when δ is large. The red curves are the completeness of retrieving X-ray or MIR AGNs in the whole W-CDF-S field using the criterion of ΔBIC2(AGN) > δ, where “MIR” means all the sources satisfying any criterion in Stern et al. (2005), Lacy et al. (2007), or Donley et al. (2012), while “MIR; Donley et al. (2012)” means only for MIR AGNs satisfying Donley et al. (2012).
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: Venn diagrams comparing our reliable SED AGNs (see, Equations (18) and (19)) in CDF-S (left) and W-CDF-S (right). The purity of our reliable SED AGNs is (76 ± 7)%, according to the CDF-S calibration, and 69% of these sources are also identified as X-ray or MIR AGNs in W-CDF-S.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption:  f AGN vs. ΔBIC2(AGN) for refined SED AGN candidates. The red line is the LOESS curve of the points. The apparent horizontal point density does not reflect source number because we intentionally increase the point size and opacity at larger ΔBIC2(AGN) for better visualization. There is only a weak positive correlation between the two parameters, and f AGN scatters across a wide range because it can hardly be constrained well by the available data.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: The i-band magnitude distributions of AGNs selected by different methods. The legend “X-ray & MIR & SED” means refined SED AGN candidates that are also identified by the X-ray and MIR selections, and “X-ray (MIR) only” refers to those only identified by X-ray (MIR) but not other methods. The X-ray- or MIR-only AGNs are generally fainter.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption:  r SFR vs. ΔBIC2(BQ) for our BQ-galaxy candidates. The r SFR distribution is bimodal. The black horizontal lines represent r SFR = 0.2 and 10, from which we empirically select quenching or bursting subpopulations.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: A Venn diagram comparing our refined SED AGN candidates with the ground-truth 7 Ms X-ray sources in CDF-S. The overlap between our refined candidates and the X-ray AGNs is limited, indicating that both the purity and the completeness are not high for the refined candidates.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: The rest-frame UVJ (left) and FUVVJ (right) color–color diagrams of our sources, color-coded by their logsSFR per year. The FUVVJ diagram has a larger dynamical range to separate quiescent galaxies with different levels of sSFR.
Paper: Gas Column Density Distribution of Molecular Clouds in the Third Quadrant of the Milky Way
Authors: Yuehui Ma, Hongchi Wang, Miaomiao Zhang, Chen Wang, Shaobo Zhang, Yao Liu, Chong Li, Yuqing Zheng, Lixia Yuan, Ji Yang
Figure caption: Top: relationship between the dispersion of the normalized column density, ﹩{\sigma }_{N/\left\langle N\right\rangle }﹩, and sonic Mach number, ﹩{ \mathcal M }﹩, of the clouds. Bottom: relationship between σ  s  and ﹩{ \mathcal M }﹩. The green, blue, and red dashed curves show the case [A = 0.16, b = 1/2], [A = 0.12, b = 1/2], and [A = 0.11, b = 1/3], corresponding to the Taurus, IC 5146, and simulated molecular clouds, respectively (Burkhart 2018). The dark-blue dotted–dashed lines in the top and bottom panels are the best fit of the relation ﹩{\sigma }_{N/\left\langle N\right\rangle }=\sqrt{{({b}^{2}{{ \mathcal M }}^{2}+1)}^{A}-1}﹩ and ﹩{\sigma }_{s}=\sqrt{A\mathrm{ln}(1+{b}^{2}{{ \mathcal M }}^{2})}﹩, respectively, while the orange straight line is the best fit of the linear relation of ﹩{\sigma }_{N/\left\langle N\right\rangle }-{ \mathcal M }﹩. The gray solid and dashed curves represent the relations ﹩{\sigma }_{s}={{ \mathcal M }}^{0.18}﹩ and ﹩{\sigma }_{s}={{ \mathcal M }}^{0.31}﹩, respectively.
Paper: Gas Column Density Distribution of Molecular Clouds in the Third Quadrant of the Milky Way
Authors: Yuehui Ma, Hongchi Wang, Miaomiao Zhang, Chen Wang, Shaobo Zhang, Yao Liu, Chong Li, Yuqing Zheng, Lixia Yuan, Ji Yang
Figure caption: Variations of the widths of the N-pdfs with (a) the average column densities and (b) mass of the molecular clouds. The dashed lines are the fitted scaling relations between ﹩\mathrm{log}{\sigma }_{s}﹩ and ﹩\mathrm{log}{N}_{{{\rm{H}}}_{2}}﹩ in panel (a) and ﹩\mathrm{log}{\sigma }_{s}﹩ and ﹩\mathrm{log}M﹩ in panel (b). The blue and light blue colors correspond to the clouds in the LN and LN+PL categories in this work, while the orange, magenta, and green colors correspond to the results obtained by K09, and Ma et al. (2020, 2021), respectively. The average column density for each cloud in this work is calculated above the median detection limit of the cloud.
Paper: Gas Column Density Distribution of Molecular Clouds in the Third Quadrant of the Milky Way
Authors: Yuehui Ma, Hongchi Wang, Miaomiao Zhang, Chen Wang, Shaobo Zhang, Yao Liu, Chong Li, Yuqing Zheng, Lixia Yuan, Ji Yang
Figure caption: (a) Histograms of the virial parameters of the clouds and the subregions of molecular clouds with column densities in the PL part of the N-pdfs. The vertical dashed line represents α vir = 2. (b) A zoom-in histogram of the virial parameters within 0 < α vir < 10 with bin widths of 0.5. (c) Histograms of the area and mass fraction of the molecular gas of column density in the PL part of the N-pdfs.
Paper: Gas Column Density Distribution of Molecular Clouds in the Third Quadrant of the Milky Way
Authors: Yuehui Ma, Hongchi Wang, Miaomiao Zhang, Chen Wang, Shaobo Zhang, Yao Liu, Chong Li, Yuqing Zheng, Lixia Yuan, Ji Yang
Figure caption: Relationships between (a) velocity dispersion and radius, (b) the factor ﹩{\sigma }_{v}^{2}/R﹩ and surface density, and (c) mass and radius of the clouds. The red color and the blue color correspond to the clouds in the LN and LN+PL categories, respectively. The dashed blue lines in panels (a) and (c) are the fitted linear relations for the ﹩\mathrm{log}{\sigma }_{v}-\mathrm{log}R﹩ and ﹩\mathrm{log}M-\mathrm{log}R﹩ correlations, respectively.
Paper: Gas Column Density Distribution of Molecular Clouds in the Third Quadrant of the Milky Way
Authors: Yuehui Ma, Hongchi Wang, Miaomiao Zhang, Chen Wang, Shaobo Zhang, Yao Liu, Chong Li, Yuqing Zheng, Lixia Yuan, Ji Yang
Figure caption: Corner maps of the fitted parameters in the relationships of (a) ﹩{\sigma }_{N/\left\langle N\right\rangle }=\sqrt{{({b}^{2}{{ \mathcal M }}^{2}+1)}^{A}-1}﹩ and (b) ﹩{\sigma }_{s}=\sqrt{A\mathrm{ln}(1+{b}^{2}{{ \mathcal M }}^{2})}﹩, respectively. The numbers in the marginalized distributions present the median value and the 16th and 84th percentiles of the parameters A and b. The vertical lines represent the 16th and 84th percentiles.
Paper: Gas Column Density Distribution of Molecular Clouds in the Third Quadrant of the Milky Way
Authors: Yuehui Ma, Hongchi Wang, Miaomiao Zhang, Chen Wang, Shaobo Zhang, Yao Liu, Chong Li, Yuqing Zheng, Lixia Yuan, Ji Yang
Figure caption: Distribution of (a) μ, (b) σ  s , (c) b  r , and (d) α in Equations (5)–(6). The red dashed line and the blue dashed line in panel (b) represent the median σ  s  for the LN and LN+PL categories, respectively.