adsabs/AstroCLIMB huggingface dataset:
Paper: A Hide-and-seek Game: Looking for Population III Stars during the Epoch of Reionization through the He II λ1640 Line
Authors: Alessandra Venditti, Volker Bromm, Steven L. Finkelstein, Antonello Calabrò, Lorenzo Napolitano, Luca Graziani, Raffaella Schneider
Figure caption: Number of potentially observable He II-emitting Pop III systems N HeII as a function of the effective survey volume V eff at z = 8.1 (see text for details). Vertical dashed lines indicate the effective volume of selected JWST surveys and their cumulative volume at z ≃ 8, with Δz = 1 (filled circles; see text for details); the number of Pop III systems found in our six dustyGadget cubes is also indicated in the plot (DG, empty squares). A horizontal dashed line further indicates the reference value of 1 system per volume. The black line refers to the number found in all halos with ﹩7.5\lt \mathrm{Log}({M}_{\star }/{M}_{\odot })\leqslant 9.5﹩, while the colored lines refer to the number found in halos of different stellar mass bins (see Figure 4).
Paper: Theoretical Modeling of the Exceptional GRB 221009A Afterglow
Authors: Luca Foffano, Marco Tavani, Giovanni Piano
Figure caption: Calculated lightcurves for different energy bands. As in Figure 1, we include optical data (pink diamonds), Swift-XRT X-ray data (orange triangles, multiplied by 100), AGILE GRID GeV data (red squares, multiplied by 10), and LHAASO TeV data (blue circles). The TeV calculated lightcurve is shown after the EBL deabsorption.
Paper: Theoretical Modeling of the Exceptional GRB 221009A Afterglow
Authors: Luca Foffano, Marco Tavani, Giovanni Piano
Figure caption: Time evolution of the calculated characteristic frequencies of the model of the GRB 221009A afterglow: the cooling frequency ν  c  is shown with a dashed blue line, and the minimum frequency ﹩{\nu }_{\min }﹩ as a dashed–dotted orange line.
Paper: Cautionary Tales on Heating-rate Prescriptions in Kilonovae
Authors: Nikhil Sarin, Stephan Rosswog
Figure caption: Simulated data from the Vera Rubin Observatory for different bands using a two-component kilonova simulated with the updated heating-rate prescription and 95% credible-interval fit with old heating-rate prescription (O. Korobkin et al. 2012; left panel) and the updated prescription (S. Rosswog & O. Korobkin 2024; right panel).
Paper: Cautionary Tales on Heating-rate Prescriptions in Kilonovae
Authors: Nikhil Sarin, Stephan Rosswog
Figure caption: Recovered posteriors from old (orange) and updated (blue) heating-rate prescriptions. The black crosses indicate the true input of the simulated data.
Paper: Quartz Clouds in the Dayside Atmosphere of the Quintessential Hot Jupiter HD 189733 b
Authors: Julie Inglis, Natasha E. Batalha, Nikole K. Lewis, Tiffany Kataria, Heather A. Knutson, Brian M. Kilpatrick, Anna Gagnebin, Sagnick Mukherjee, Maria M. Pettyjohn, Ian J. M. Crossfield, Trevor O. Foote, David Grant, Gregory W. Henry, Maura Lally, Laura K. McKemmish, David K. Sing, Hannah R. Wakeford, Juan C. Zapata Trujillo, Robert T. Zellem
Figure caption: (a) Our joint eclipse spectrum, converted to brightness temperature, plotted against the best-fit Picaso forward model and 3σ upper limits. We show the same model with the contribution from the quartz (SiO2[s]) grains (purple) and H2O (blue) opacities removed. (b) The best-fit pressure–temperature (P–T) profile predicted by forward models and maximum dayside temperature compared to condensation curves of major silicate cloud species. (c) Our joint eclipse spectrum plotted against the best-fit petitRADTRANs free retrieval. We additionally compare to our best-fit model from a retrieval with fosterite (Mg2SiO4[s]) as the condensate species instead of SiO2 (pink). We show the same model with opacities from the gas-phase molecules detected in our retrievals, including H2S (brown) and H2O (blue), removed. (d) The best-fit retrieved P–T profile from the free retrievals and 1σ limits compared to condensation curves.
Paper: Quartz Clouds in the Dayside Atmosphere of the Quintessential Hot Jupiter HD 189733 b
Authors: Julie Inglis, Natasha E. Batalha, Nikole K. Lewis, Tiffany Kataria, Heather A. Knutson, Brian M. Kilpatrick, Anna Gagnebin, Sagnick Mukherjee, Maria M. Pettyjohn, Ian J. M. Crossfield, Trevor O. Foote, David Grant, Gregory W. Henry, Maura Lally, Laura K. McKemmish, David K. Sing, Hannah R. Wakeford, Juan C. Zapata Trujillo, Robert T. Zellem
Figure caption: Our fitted spectroscopic secondary-eclipse depths from 5 to 12 μm are plotted for both visits from our Eureka! reductions. The Spitzer 8 μm band response curve is shown in black. We compare our MIRI LRS emission spectrum to the Spitzer/IRS spectrum from K. O. Todorov et al. (2014, gray), with an applied offset of 0.06%. The misfit between eclipses at 10–11 μm matches the area of the detector where the ramp behavior differs the most significantly between visits (see Section 3.4).
Paper: Quartz Clouds in the Dayside Atmosphere of the Quintessential Hot Jupiter HD 189733 b
Authors: Julie Inglis, Natasha E. Batalha, Nikole K. Lewis, Tiffany Kataria, Heather A. Knutson, Brian M. Kilpatrick, Anna Gagnebin, Sagnick Mukherjee, Maria M. Pettyjohn, Ian J. M. Crossfield, Trevor O. Foote, David Grant, Gregory W. Henry, Maura Lally, Laura K. McKemmish, David K. Sing, Hannah R. Wakeford, Juan C. Zapata Trujillo, Robert T. Zellem
Figure caption: The fitted spectroscopic coefficients for three of our detrending parameters, PSF width, linear slope with time, and ramp amplitude, for each of our two secondary-eclipse observations from our Eureka! reduction. While the best-fit systematics differ between our two secondary-eclipse observations, the shape of the emission spectrum is mostly consistent between the two visits at the 2σ level. The largest differences between visits occur where the linear component of the ramp varies most. The linear component of the ramp also switches sign between visits from 10 to 11 μm. This suggests that this could lead to small offsets in eclipse depth (see Section 3.4).
Paper: Quartz Clouds in the Dayside Atmosphere of the Quintessential Hot Jupiter HD 189733 b
Authors: Julie Inglis, Natasha E. Batalha, Nikole K. Lewis, Tiffany Kataria, Heather A. Knutson, Brian M. Kilpatrick, Anna Gagnebin, Sagnick Mukherjee, Maria M. Pettyjohn, Ian J. M. Crossfield, Trevor O. Foote, David Grant, Gregory W. Henry, Maura Lally, Laura K. McKemmish, David K. Sing, Hannah R. Wakeford, Juan C. Zapata Trujillo, Robert T. Zellem
Figure caption: A sample of spectroscopic light curves from our Eureka! reduction for each of our two secondary-eclipse observations. For our fits, we trim 100 integrations at the beginning of each observation to remove the sharp “hook” which cannot quite be captured by an exponential, shown in the gray shaded region. The best-fit combined instrumental and eclipse models are overplotted in black.
Paper: Quartz Clouds in the Dayside Atmosphere of the Quintessential Hot Jupiter HD 189733 b
Authors: Julie Inglis, Natasha E. Batalha, Nikole K. Lewis, Tiffany Kataria, Heather A. Knutson, Brian M. Kilpatrick, Anna Gagnebin, Sagnick Mukherjee, Maria M. Pettyjohn, Ian J. M. Crossfield, Trevor O. Foote, David Grant, Gregory W. Henry, Maura Lally, Laura K. McKemmish, David K. Sing, Hannah R. Wakeford, Juan C. Zapata Trujillo, Robert T. Zellem
Figure caption: (a) Measured 8 μm eclipse depths colored by eclipse depth for the seven Spitzer eclipses from E. Agol et al. (2010) as compared to our two JWST 8 μm eclipse depths (orange, blue). (b) The ramps for the corresponding Spitzer eclipses from (a) are plotted, colored according to their depths.
Paper: Quartz Clouds in the Dayside Atmosphere of the Quintessential Hot Jupiter HD 189733 b
Authors: Julie Inglis, Natasha E. Batalha, Nikole K. Lewis, Tiffany Kataria, Heather A. Knutson, Brian M. Kilpatrick, Anna Gagnebin, Sagnick Mukherjee, Maria M. Pettyjohn, Ian J. M. Crossfield, Trevor O. Foote, David Grant, Gregory W. Henry, Maura Lally, Laura K. McKemmish, David K. Sing, Hannah R. Wakeford, Juan C. Zapata Trujillo, Robert T. Zellem
Figure caption: Comparison of our Eureka! and SPARTA reductions for each of our two secondary-eclipse observations. The systematic differences between reductions are due to the different linearity corrections. Shortwards of 5.5 μm, the difference is increased by the partially saturated detector.
Paper: Quartz Clouds in the Dayside Atmosphere of the Quintessential Hot Jupiter HD 189733 b
Authors: Julie Inglis, Natasha E. Batalha, Nikole K. Lewis, Tiffany Kataria, Heather A. Knutson, Brian M. Kilpatrick, Anna Gagnebin, Sagnick Mukherjee, Maria M. Pettyjohn, Ian J. M. Crossfield, Trevor O. Foote, David Grant, Gregory W. Henry, Maura Lally, Laura K. McKemmish, David K. Sing, Hannah R. Wakeford, Juan C. Zapata Trujillo, Robert T. Zellem
Figure caption: Left: raw spectroscopic light curves from the Eureka! reduction for each of our MIRI LRS secondary eclipses. Right: residuals after subtracting the best-fit eclipse and instrumental ramp model. The strong wavelength-dependent instrumental ramp is visible at the beginning of the raw light curves for both observations.
Paper: The Stellar Distribution in Ultrafaint Dwarf Galaxies Suggests Deviations from the Collisionless Cold Dark Matter Paradigm
Authors: Jorge Sánchez Almeida, Ignacio Trujillo, Angel R. Plastino
Figure caption: Stellar surface density profiles for six UFDs from Richstein et al. (2024), pieced together by rescaling in x and y using a least-square fit that gives the scales and assumes the same polynomial shape for all galaxies. The symbols represent different galaxies and reductions, as labeled, whereas the solid line shows the best-fitting polynomial. The dashed line corresponds to a linear fit to the innermost points of the profile. The best-fitting polynomial is close to a simple y = 1/(1 + x 2) law (not shown). χ 2/ν stands for the reduced χ 2 of the fit with rms representing its root mean square.
Paper: The Stellar Distribution in Ultrafaint Dwarf Galaxies Suggests Deviations from the Collisionless Cold Dark Matter Paradigm
Authors: Jorge Sánchez Almeida, Ignacio Trujillo, Angel R. Plastino
Figure caption: Observed stellar surface density (the symbols) and its best fit assuming a Schuster–Plummer potential (the red solid line). The plot shows the mass surface density that gives rise to the best fitting Schuster–Plummer potential (the blue dashed line), the NFW potential (the green dashed line), and the ρ 230 potential (the magenta dashed line). The vertical scaling was chosen to be representative of the UFDs, so that the mass creating the potential is 500 times the observed stellar mass. The contribution from the stars to the overall potential has been subtracted out in the solid yellow–green line. The result is virtually indistinguishable from the original profile (the green dashed line), showing the self-gravity of the stars to be negligible.
Paper: The Stellar Distribution in Ultrafaint Dwarf Galaxies Suggests Deviations from the Collisionless Cold Dark Matter Paradigm
Authors: Jorge Sánchez Almeida, Ignacio Trujillo, Angel R. Plastino
Figure caption: Summary plot used to estimate confidence limits. (a) Histograms with the innermost slopes for the fits with the three gravitational potentials explored in the work (see the inset). The red histogram represents the observed value (Equation (1)). (b) Distribution of χ 2 of the fits for the three potentials when forcing f ≥ 0. The arrows represent the χ 2 of the best fit obtained with unconstrained f(ϵ). The color code is the same in (a) and (b).
Paper: The Stellar Distribution in Ultrafaint Dwarf Galaxies Suggests Deviations from the Collisionless Cold Dark Matter Paradigm
Authors: Jorge Sánchez Almeida, Ignacio Trujillo, Angel R. Plastino
Figure caption: (a) Fits to the data in Figure 1 using f(ϵ) as free parameter and assuming the galaxies to reside in a Schuster–Plummer gravitational potential. The best fit is shown as a solid red line. The fits forced to have f ≥ 0 are shown as colored solid lines, where the color code represents the innermost slope (﹩d\mathrm{log}{\rm{\Sigma }}/d\mathrm{log}R﹩ when R → 0) as indicated in the color bar. (b) f(ϵ) corresponding to the fits in (a) and using the same color code. Note that the best unconstrained fit yields f ≥ 0 everywhere.
Paper: The Stellar Distribution in Ultrafaint Dwarf Galaxies Suggests Deviations from the Collisionless Cold Dark Matter Paradigm
Authors: Jorge Sánchez Almeida, Ignacio Trujillo, Angel R. Plastino
Figure caption: Same as Figure 2 but assuming the galaxies to reside in a NFW potential. The color code is the same as that employed in Figure 2. Note that the best fit requires an unphysical f < 0 (the red solid line in panel (b)) and that the fits forced to have f ≥ 0, contrarily to the observation, present quite negative inner slopes ω (the coloring is green–yellow rather than orange–red).
Paper: The H I Reservoir in Central Spiral Galaxies and the Implied Star Formation Process 
Authors: Jing Dou, Yingjie Peng, Qiusheng Gu, Alvio Renzini, Luis C. Ho, Filippo Mannucci, Emanuele Daddi, Chengpeng Zhang, Jiaxuan Li, Yong Shi, Tao Wang, Dingyi Zhao, Cheqiu Lyu, Di Li, Feng Yuan, Roberto Maiolino, Yulong Gao
Figure caption: The SFEH I –sSFR relation (upper panels) and μ H I –sSFR relation (lower panels) of central spiral galaxies in the ALFALFA-SDSS matched sample with incompleteness corrections. Left: the distribution of galaxies on the SFEH I –sSFR and μ H I –sSFR planes. The size of each point represents the weight used for incompleteness correction. Middle: the median SFEH I  and μ H I  as a function of sSFR in different stellar mass bins, determined by using a moving median with a sliding window of 0.5 dex in sSFR. Error bars on each line indicate the 5% and 95% percentiles of the distribution. As discussed in Appendix C and Figure 6, these one-dimensional analyses can be heavily affected by the shape of the sample distribution and lead to biased results. Right: average stellar mass on the SFEH I –sSFR and μ H I –sSFR planes, calculated with a moving box of 0.5 dex in both sSFR and SFEH I  (or μ H I ). The contour lines mark the equal stellar mass distribution. In each panel, the black diagonal lines indicate three different values of a constant μ H I  of 0.2, 0.7, and 4 (upper panels), or a SFEH I  of 0.01, 0.1, and 1 Gyr−1 (lower panels). The gray thick lines indicate the fundamental formation relation (FFR) of molecular gas found in J. Dou et al. (2021a), corresponding to ﹩{\mu }_{{{\rm{H}}}_{2}}﹩ on the y-axis.
Paper: The H I Reservoir in Central Spiral Galaxies and the Implied Star Formation Process 
Authors: Jing Dou, Yingjie Peng, Qiusheng Gu, Alvio Renzini, Luis C. Ho, Filippo Mannucci, Emanuele Daddi, Chengpeng Zhang, Jiaxuan Li, Yong Shi, Tao Wang, Dingyi Zhao, Cheqiu Lyu, Di Li, Feng Yuan, Roberto Maiolino, Yulong Gao
Figure caption: The distribution function of R 90/R 50 in the r band (upper-left panel), the mass-weighted B/T (upper-right panel), the Sérsic index in the r band (lower-left panel), and the probability of a galaxy being a late-type disk galaxy with T-type > 0 using the machine learning (ML) morphology catalog from H. DomÍnguez Sánchez et al. (2018; lower-right panel) for central galaxies with 1010 M ⊙ < M * < 1010.3 M ⊙ and 0.02 < z < 0.05 in the SDSS. In each panel, blue, red, and gray histograms indicate the visual morphological classification of spiral, elliptical, and uncertain galaxies defined from the Galaxy Zoo project. Clearly, a significant amount of central visually defined spiral galaxies have large values of R 90/R 50, B/T, and Sérsic index, and will be classified as “elliptical” according to their structural parameters. On the other hand, many visually classified “uncertain” galaxies have small values of R 90/R 50, B/T, and Sérsic index, and a large value of P                          disk                       with T-type > 0, and will be classified as “spiral” according to their structural parameters or morphological classification from ML.
Paper: The H I Reservoir in Central Spiral Galaxies and the Implied Star Formation Process 
Authors: Jing Dou, Yingjie Peng, Qiusheng Gu, Alvio Renzini, Luis C. Ho, Filippo Mannucci, Emanuele Daddi, Chengpeng Zhang, Jiaxuan Li, Yong Shi, Tao Wang, Dingyi Zhao, Cheqiu Lyu, Di Li, Feng Yuan, Roberto Maiolino, Yulong Gao
Figure caption: H I detection fraction (DF) as a function of stellar mass and star formation rate (SFR) for different samples. These are obtained by using a moving box of size 0.5 dex in SFR and 0.5 dex in M *. In all panels, the dashed line indicates the position of the star-forming main sequence defined in A. Renzini & Y.-j. Peng (2015). The dotted lines indicate ±0.4 dex scatter around the main sequence. Contour lines connect points that have the same DF. The gray shades in the middle panels indicate the region with M * < 109 M ⊙, where the sample becomes incomplete even with corrections. Left: H I DF in the ALFALFA-SDSS matched sample for all galaxies (upper-left panel) and central spiral galaxies (lower-left panel) without incompleteness corrections. Middle: same as left panels, but with incompleteness corrections. Right: H I DF in the xGASS sample for all galaxies (upper-right panel) and central spiral galaxies defined by visual morphology (lower-right panel).
Paper: The H I Reservoir in Central Spiral Galaxies and the Implied Star Formation Process 
Authors: Jing Dou, Yingjie Peng, Qiusheng Gu, Alvio Renzini, Luis C. Ho, Filippo Mannucci, Emanuele Daddi, Chengpeng Zhang, Jiaxuan Li, Yong Shi, Tao Wang, Dingyi Zhao, Cheqiu Lyu, Di Li, Feng Yuan, Roberto Maiolino, Yulong Gao
Figure caption: The detection limits of the SDSS spectroscopic and ALFALFA samples. Left: stellar mass (M *) distribution for the SDSS sample in a narrow redshift bin of 0.02 < z < 0.05. The galaxies with log sSFR < −1.8 Gyr−1 (the measurements of stellar masses and SFRs are described in Section 2.5) are defined to be passive and denoted as red dots. Right: atomic gas mass M H I  distribution for the ALFALFA sample in the same redshift bin. The galaxies with W 50 > 100, 200, and 400 km s−1 are denoted as blue, green, and red dots, respectively. Evidently, both the SDSS and ALFALFA samples are strongly biased and sample incompleteness corrections are necessary for any statistical analysis.
Paper: The H I Reservoir in Central Spiral Galaxies and the Implied Star Formation Process 
Authors: Jing Dou, Yingjie Peng, Qiusheng Gu, Alvio Renzini, Luis C. Ho, Filippo Mannucci, Emanuele Daddi, Chengpeng Zhang, Jiaxuan Li, Yong Shi, Tao Wang, Dingyi Zhao, Cheqiu Lyu, Di Li, Feng Yuan, Roberto Maiolino, Yulong Gao
Figure caption: As for Figure 1, using the ALFALFA-SDSS matched sample with incompleteness correction. The upper two panels are for all central galaxies with B/T < 0.3 (upper-left panel) and B/T < 0.5 (upper-right panel). The lower two panels are for central, visually defined “uncertain” galaxies (lower-left panel) and central, visually defined “elliptical” galaxies (lower-right panel) from the Galaxy Zoo project. In each panel, the average H I DF for the given subsample above the completeness mass of M * ∼ 109 M ⊙ is given in the legend.
Paper: The H I Reservoir in Central Spiral Galaxies and the Implied Star Formation Process 
Authors: Jing Dou, Yingjie Peng, Qiusheng Gu, Alvio Renzini, Luis C. Ho, Filippo Mannucci, Emanuele Daddi, Chengpeng Zhang, Jiaxuan Li, Yong Shi, Tao Wang, Dingyi Zhao, Cheqiu Lyu, Di Li, Feng Yuan, Roberto Maiolino, Yulong Gao
Figure caption: The distribution of central spiral galaxies in the ALFALFA-SDSS sample on the SFEH I –sSFR plane, split into three different stellar mass bins. In each panel, the black diagonal lines indicate three constant μ H I . The gray thick lines indicate the molecular gas FFR for reference. Blue dots in the upper three panels are individual galaxies. Level contours for the number density of galaxies are shown in the lower three panels, with colors ranging from blue to red as a function of logarithm of the number density, applied with sample incompleteness correction. The blue lines show the average SFEH I  (at a given sSFR) as a function of sSFR, calculated with a moving average of 0.5 dex in sSFR. The red lines show the best fits to the data using the ODR fitting method, with the slope given in the legend, which is around unity (i.e., galaxies distributed following the diagonal constant H I gas-to-mass ratio line) for all three mass bins. While the blue line has, on average, a shallower slope than unity, indicating that when sSFR decreases, the H I gas-to-mass ratio also decreases, i.e., galaxies become more H I-poor. Evidently, the red line better traces the ridge of the contour lines than the blue line, and hence the ODR fitting that considers the variations in both the x- and y-axes represents a more accurate fit to the data, in particular for the case of the low-mass bin where the scatter is larger.
Paper: The H I Reservoir in Central Spiral Galaxies and the Implied Star Formation Process 
Authors: Jing Dou, Yingjie Peng, Qiusheng Gu, Alvio Renzini, Luis C. Ho, Filippo Mannucci, Emanuele Daddi, Chengpeng Zhang, Jiaxuan Li, Yong Shi, Tao Wang, Dingyi Zhao, Cheqiu Lyu, Di Li, Feng Yuan, Roberto Maiolino, Yulong Gao
Figure caption: As for Figure 3, but using SFRs derived from the SED fitting of UV, optical, and mid-IR bands (S. Salim et al. 2018). The H2 FFR is also derived from the SED SFRs, correspondingly. The range of the galaxy distribution in sSFR is narrower compared to Figure 3, but the general trends shown in the right two panels (which are more accurate representations of the true underlying trends compared to the one-dimensional analysis shown in the middle two panels, as illustrated in Figure 6) are similar to those in Figure 3.
Paper: The Formation of Milky Way “Bones”: Ubiquitous HI Narrow Self-absorption Associated with CO Emission
Authors: Shenglan Sun, Ke Wang, Xunchuan Liu, Fengwei Xu
Figure caption: Left: 12CO-integrated intensity contours overlaid on H2 column density from K. A. Marsh et al. (2017) for G28 (top) and G47 (bottom). The contours are at 6, 9, and 12 × 104K km s−1 and 4, 8,and 12 × 104K km s−1, respectively. The magenta solid circles are ON-filament regions, and the green dashed circles are OFF-filament regions, both with a diameter of FAST beam (﹩\sim 2\buildrel{\,\prime}\over{.} 9﹩). Right: HINSA fitting and CO spectra toward representative regions of G28 (top, region ON 1) and G47 (bottom, region ON 1). For each region, the recovered HI background T HI (blue) and observed HI spectra T r (black) are in the top half. Fitted spectra of HINSA features T ab = T HI − T r (red), 12CO (green), and 13CO (gold) are in the second half. The temperatures of 13CO are magnified three times.
Paper: The Formation of Milky Way “Bones”: Ubiquitous HI Narrow Self-absorption Associated with CO Emission
Authors: Shenglan Sun, Ke Wang, Xunchuan Liu, Fengwei Xu
Figure caption: Boxplot comparing the spectral line parameters of HINSA and 13CO of ON and OFF regions in G28 and G47. (a) Boxplot of the difference between the central velocities of HINSA and 13CO. (b) Boxplot of the ratio of the nonthermal velocity dispersion of HINSA to that of 13CO. The horizontal lines connect minimal to maximum values, and each data point of V lsr(HINSA) − V lsr(13CO) in panel (a) or ﹩{\sigma }_{\mathrm{nt},\mathrm{HINSA}}-{\sigma }_{\mathrm{nt}{,}^{13}\mathrm{CO}}﹩ in panel (b) is marked as a small open circle. The filled boxes encompass 25th percentile Q 1 to 75th percentile Q 3 of the corresponding V lsr(HINSA) − V lsr(13CO) or ﹩{\sigma }_{\mathrm{nt},\mathrm{HINSA}}-{\sigma }_{\mathrm{nt}{,}^{13}\mathrm{CO}}﹩ data set, and the red vertical lines in the boxes mark median values.