adsabs/AstroCLIMB huggingface dataset:
Paper: High-resolution Simulation of Coronal Mass Ejection–Corotating Interaction Region Interactions: Mesoscale Solar Wind Structure Formation Observable by the SWIFT Constellation
Authors: W. B. Manchester, Nishtha Sachdeva, Emilia Kilpua, Matti Ala-Lahti, Shirsh Lata Soni, Zhenguang Huang, Hongfan Chen, Aniket Jivani, Bart van der Holst, Adam Szabo, Mojtaba Akhavan-Tafti
Figure caption: The early structure of the CME in the SC domain. Panels (a) and (b) show the CME at t = 10 minutes with the plasma velocity and Bz components shown on the (x-z) plane, respectively. Panels (c)–(f) show the system at t = 1 hr, viewed on the equatorial (x–y) plane with plasma velocity, Bz, proton density, and temperature shown, respectively. In all cases, magnetic field lines are shown in gray and the inner boundary of the SC component is colored to show Br. Note that the outer extremity of the flux rope expands rapidly into the open magnetic field of the fast wind.
Paper: High-resolution Simulation of Coronal Mass Ejection–Corotating Interaction Region Interactions: Mesoscale Solar Wind Structure Formation Observable by the SWIFT Constellation
Authors: W. B. Manchester, Nishtha Sachdeva, Emilia Kilpua, Matti Ala-Lahti, Shirsh Lata Soni, Zhenguang Huang, Hongfan Chen, Aniket Jivani, Bart van der Holst, Adam Szabo, Mojtaba Akhavan-Tafti
Figure caption: Schematic illustration of unique tetrahedral configuration of SWIFT along the Sun–Earth line beyond the Lagrangian point L1 (sub-L1) in combination with L1.
Paper: Impact of Gravity on Changing Magnetic Field Orientations in a Sample of Massive Protostellar Clusters Observed with ALMA
Authors: Qizhou Zhang, Junhao Liu, Lingzhen Zeng, J. D. Soler, Huei-Ru Vivien Chen, Tao-Chung Ching, Paul T. P. Ho, Josep Miquel Girart, Patrick M. Koch, Shih-Ping Lai, Shanghuo Li, Zhi-Yun Li, Hauyu Baobab Liu, Keping Qiu, Ramprasad Rao
Figure caption: Magnetic field orientations in NGC 6334 In made from the C43-1, C43-4, and C43-4-restricted data that exclude visibilities with projected baseline lengths < 250 m. The Stokes I emission is shown in contours and gray scales. The red line segments represent the PAs of the plane-of-the-sky component of magnetic fields. The synthesized beam is marked at the lower-left corner of each panel. The horizontal bars at the lower-right corner of each panel represent a linear scale of 0.05 pc. The dotted line marks the 50% sensitivity level of the observations.
Paper: Impact of Gravity on Changing Magnetic Field Orientations in a Sample of Massive Protostellar Clusters Observed with ALMA
Authors: Qizhou Zhang, Junhao Liu, Lingzhen Zeng, J. D. Soler, Huei-Ru Vivien Chen, Tao-Chung Ching, Paul T. P. Ho, Josep Miquel Girart, Patrick M. Koch, Shih-Ping Lai, Shanghuo Li, Zhi-Yun Li, Hauyu Baobab Liu, Keping Qiu, Ramprasad Rao
Figure caption: Normalized PRS of ROs of magnetic fields between the C43-1 and the C43-4-restricted data that excludes visibilities with UV distances < 250 m vs. column densities for NGC 6334.
Paper: Impact of Gravity on Changing Magnetic Field Orientations in a Sample of Massive Protostellar Clusters Observed with ALMA
Authors: Qizhou Zhang, Junhao Liu, Lingzhen Zeng, J. D. Soler, Huei-Ru Vivien Chen, Tao-Chung Ching, Paul T. P. Ho, Josep Miquel Girart, Patrick M. Koch, Shih-Ping Lai, Shanghuo Li, Zhi-Yun Li, Hauyu Baobab Liu, Keping Qiu, Ramprasad Rao
Figure caption: ROs of magnetic field PAs between the C43-1 and the C43-4 data excluding visibilities with UV distances < 250 m. The left panel shows the combined RO distribution of NGC 6334 I, In, IV, and V. The right panel shows the combined RO distribution of G14.
Paper: Impact of Gravity on Changing Magnetic Field Orientations in a Sample of Massive Protostellar Clusters Observed with ALMA
Authors: Qizhou Zhang, Junhao Liu, Lingzhen Zeng, J. D. Soler, Huei-Ru Vivien Chen, Tao-Chung Ching, Paul T. P. Ho, Josep Miquel Girart, Patrick M. Koch, Shih-Ping Lai, Shanghuo Li, Zhi-Yun Li, Hauyu Baobab Liu, Keping Qiu, Ramprasad Rao
Figure caption: Normalized PRS analysis of ROs between directions of local gravity and magnetic fields for NGC 6334.
Paper: Impact of Gravity on Changing Magnetic Field Orientations in a Sample of Massive Protostellar Clusters Observed with ALMA
Authors: Qizhou Zhang, Junhao Liu, Lingzhen Zeng, J. D. Soler, Huei-Ru Vivien Chen, Tao-Chung Ching, Paul T. P. Ho, Josep Miquel Girart, Patrick M. Koch, Shih-Ping Lai, Shanghuo Li, Zhi-Yun Li, Hauyu Baobab Liu, Keping Qiu, Ramprasad Rao
Figure caption: ROs of magnetic field PAs between the C43-1 and the C43-4-restricted data that excludes visibilities with UV distances < 250 m.
Paper: Impact of Gravity on Changing Magnetic Field Orientations in a Sample of Massive Protostellar Clusters Observed with ALMA
Authors: Qizhou Zhang, Junhao Liu, Lingzhen Zeng, J. D. Soler, Huei-Ru Vivien Chen, Tao-Chung Ching, Paul T. P. Ho, Josep Miquel Girart, Patrick M. Koch, Shih-Ping Lai, Shanghuo Li, Zhi-Yun Li, Hauyu Baobab Liu, Keping Qiu, Ramprasad Rao
Figure caption: ROs of magnetic field PAs between the C43-1 and the C43-4-restricted data, which excludes visibilities with projected baselines < 250 m. The histogram includes data from NGC 6334, G14, G34.43, and G35.2N.
Paper: paired: A Statistical Framework for Detecting Stellar Binarity with Gaia RVs. I. Sensitivity to Unresolved Binaries
Authors: Quadry Chance, Daniel Foreman-Mackey, Sarah Ballard, Andrew R. Casey, Trevor J. David, Adrian M. Price-Whelan
Figure caption: Top panel: In an effort to determine if our pipeline robustly recovers the correct K, we run it on a population of binary stars described in Section 2.2. We inject the same estimated per-measurement uncertainties for each color and magnitude bin. The size of the circles indicates the ratio of the recovered signal to this uncertainty. Recovering the correct semi-amplitude mostly depends on how uncertain the RV noise estimate is of stars in the same bin. The recovered semi-amplitude tends to be biased high for two reasons: because we are also sampling over eccentricity with bounds of 0–1 and the heavy tails of the K probability distribution are weighted toward larger K. The remaining nonrandom scatter depends on the eccentricity of the binary orbit. Bottom panel: The same as the top panel with a 50% uncertainty added to the estimated per-transit measurement uncertainty. Sources with a high SNR remain unaffected, but those with low SNR systematically underestimate the semi-amplitude.
Paper: paired: A Statistical Framework for Detecting Stellar Binarity with Gaia RVs. I. Sensitivity to Unresolved Binaries
Authors: Quadry Chance, Daniel Foreman-Mackey, Sarah Ballard, Andrew R. Casey, Trevor J. David, Adrian M. Price-Whelan
Figure caption: A histogram of the number of RV observations (transits) of sources in the Gaia RV sample.
Paper: paired: A Statistical Framework for Detecting Stellar Binarity with Gaia RVs. I. Sensitivity to Unresolved Binaries
Authors: Quadry Chance, Daniel Foreman-Mackey, Sarah Ballard, Andrew R. Casey, Trevor J. David, Adrian M. Price-Whelan
Figure caption: Top panel: Color–magnitude diagram of the difference between p-values calculated in this work vs. p-values from Gaia DR3 (D. Katz et al. 2023). Sources for which there is more disagreement between the paired p-value and rv_chisqu_pvalue cluster in locations on the HR diagram that are more sparsely sampled. Bottom panel: The difference between paired p-value and rv_chisqu_pvalue as a function of the number of stars in that portion of color–magnitude space. There is broad agreement where N ≳ 103, but where paired is calibrated on fewer stars, our quantification of “excess” noise deviates more from DR3.
Paper: paired: A Statistical Framework for Detecting Stellar Binarity with Gaia RVs. I. Sensitivity to Unresolved Binaries
Authors: Quadry Chance, Daniel Foreman-Mackey, Sarah Ballard, Andrew R. Casey, Trevor J. David, Adrian M. Price-Whelan
Figure caption: Detection efficiency using RV errors as a function of injected separation and mass ratio. The color bar is the recovered fraction of binaries over the entire magnitude range of our sample. The contours indicate the threshold where 99% of binaries to the left of the dotted lines are recovered. This threshold goes to lower mass ratios and larger separations as a function of magnitude. Our recovered fraction decreases in the upper left corner, as sources with RV error greater than 40 km s−1 are culled from the data release.
Paper: paired: A Statistical Framework for Detecting Stellar Binarity with Gaia RVs. I. Sensitivity to Unresolved Binaries
Authors: Quadry Chance, Daniel Foreman-Mackey, Sarah Ballard, Andrew R. Casey, Trevor J. David, Adrian M. Price-Whelan
Figure caption: Top panel: Hertzsprung–Russell diagram of our sample, comprising ∼30 million sources. Colors and absolute magnitudes have not been corrected for extinction. Bins with fewer than 100 sources have been excluded. The color corresponds to the mean p-value of the bin, with darker colors indicating a higher fraction of binaries. The inset histograms are the distribution of p-values for sources in the marked area. Bottom panel: The same sources, with color now assigned based on the fraction of sources with paired p-value <0.001, which is our cutoff for “excess” noise.
Paper: paired: A Statistical Framework for Detecting Stellar Binarity with Gaia RVs. I. Sensitivity to Unresolved Binaries
Authors: Quadry Chance, Daniel Foreman-Mackey, Sarah Ballard, Andrew R. Casey, Trevor J. David, Adrian M. Price-Whelan
Figure caption: Top: A histogram of the p-values of 724 M dwarfs from E. R. Newton et al. (2017), split by Hα activity. Active M dwarfs are more likely to have excess RV noise than their inactive counterparts. Bottom: A histogram of the natural log of the per-transit RV measurement uncertainty (see Appendix B). This value is larger for active M dwarfs, leading to more outliers when compared to a random sample of similar stars that includes both active and inactive M dwarfs.
Paper: paired: A Statistical Framework for Detecting Stellar Binarity with Gaia RVs. I. Sensitivity to Unresolved Binaries
Authors: Quadry Chance, Daniel Foreman-Mackey, Sarah Ballard, Andrew R. Casey, Trevor J. David, Adrian M. Price-Whelan
Figure caption: The completeness of our detection method as a function of the observable parameters of simulated binaries. The completeness drops at extreme semi-amplitudes, as sources with reported RV errors greater than 40 km s−1 are culled from the catalog.
Paper: paired: A Statistical Framework for Detecting Stellar Binarity with Gaia RVs. I. Sensitivity to Unresolved Binaries
Authors: Quadry Chance, Daniel Foreman-Mackey, Sarah Ballard, Andrew R. Casey, Trevor J. David, Adrian M. Price-Whelan
Figure caption: Histogram of difference between p-values calculated in this work vs. p-values from Gaia DR3. (D. Katz et al. 2023).
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Spectra of the molecular lines observed toward the dust peak of L1544. HC17O+ is included from previous work (J. Ferrer Asensio et al. 2022). The vertical dotted gray line represents the LSR velocity of L1544 (7.2 km s−1). The misalignment between the SO (2, 3–1, 2) and c-C3H2 (21,2–10,1) line centers and the LSR of L1544 lies within the laboratory-measured transition frequency uncertainties.
Paper: paired: A Statistical Framework for Detecting Stellar Binarity with Gaia RVs. I. Sensitivity to Unresolved Binaries
Authors: Quadry Chance, Daniel Foreman-Mackey, Sarah Ballard, Andrew R. Casey, Trevor J. David, Adrian M. Price-Whelan
Figure caption: Top: A sensitivity map of the paired p-value vs. the DR3 field rv_renormalised_gof. The color bar corresponds to the number of sources in each bin. rv_renormalised_gof is largely uncorrelated with the paired p-value outside the 0 p-value bin in this figure. Bottom: The distribution of rv_renormalised_gof for sources with paired p-values greater than 0 (in purple) and equal to 0 (in green). Sources that our catalog identifies as binaries have a rv_renormalised_gof distribution that peaks well past the rv_renormalised_gof = 4 threshold identifies in D. Katz et al. (2023) as an indicator of RV variability.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: The 1D prestellar core physical model profiles used for the radiative transfer modeling. The model described in E. Keto et al. (2015) is plotted between 0 and 0.32 pc. The vertical dotted black line marks the radius at 0.32 pc. The physical profiles between 0.32 and 1 pc correspond to an “external layer” used for some of the transition modeling. The physical parameters in this external layer are constant profiles with values equal to the value at the edge (0.32 pc) of the prestellar core model in E. Keto et al. (2015). The molecular hydrogen column density, ﹩{n}_{{{\rm{H}}}_{2}}﹩, is plotted logarithmically with a black solid line. The gas temperature, T, is plotted with a blue dashed line. Finally, the velocity profile is plotted with an orange dashed–dotted line.
Paper: paired: A Statistical Framework for Detecting Stellar Binarity with Gaia RVs. I. Sensitivity to Unresolved Binaries
Authors: Quadry Chance, Daniel Foreman-Mackey, Sarah Ballard, Andrew R. Casey, Trevor J. David, Adrian M. Price-Whelan
Figure caption: A comparison of the semi-amplitude K inferred by paired vs. the semi-amplitude inferred from ground-based radial velocity surveys of binaries. Top panel: A comparison of the semi-amplitude inferred by paired vs. the value measured with mid-resolution RV survey APOGEE (M. Kounkel et al. 2021). Bottom panel: A comparison of the semi-amplitude inferred by paired vs. the value from the spectroscopic binary catalog SB9 (D. Pourbaix et al. 2004). There is a tight agreement for high semi-amplitudes that starts to loosen as K approaches the Gaia noise floor of ∼1 km s−1.
Paper: paired: A Statistical Framework for Detecting Stellar Binarity with Gaia RVs. I. Sensitivity to Unresolved Binaries
Authors: Quadry Chance, Daniel Foreman-Mackey, Sarah Ballard, Andrew R. Casey, Trevor J. David, Adrian M. Price-Whelan
Figure caption: The expected per-transit RV measurement uncertainty as a function of Gaia color and magnitude, computed based on the Gaia DR3 RV error measurements and an iterative sigma-clipping method. This figure shows these estimates smoothed and interpolated using a maximum likelihood Gaussian Process model in two dimensions.
Paper: paired: A Statistical Framework for Detecting Stellar Binarity with Gaia RVs. I. Sensitivity to Unresolved Binaries
Authors: Quadry Chance, Daniel Foreman-Mackey, Sarah Ballard, Andrew R. Casey, Trevor J. David, Adrian M. Price-Whelan
Figure caption: Left: The cumulative density function (CDF) of the p-values of DR3 sources with two-body orbit solutions (Gaia Collaboration et al. 2023). The red dashed line is our p < 0.001 threshold. The intersection of this line with the CDFs is the proportion of the sample that are flagged as binaries. Right: Identical plot for the only sources flagged as SB 1 in the table.​​​​​​
Paper: paired: A Statistical Framework for Detecting Stellar Binarity with Gaia RVs. I. Sensitivity to Unresolved Binaries
Authors: Quadry Chance, Daniel Foreman-Mackey, Sarah Ballard, Andrew R. Casey, Trevor J. David, Adrian M. Price-Whelan
Figure caption: Left: CDF of p-values of KTL crossmatch and Villanova Kepler Eclipsing binary catalog (B. Kirk et al. 2016). The red dashed line is our p < 0.001 threshold. The intersection of this line with the CDFs is the proportion of the sample that are flagged as binaries. Right: Identical plot for the TESS Community Target List and Villanova TESS Eclipsing binary catalog (A. Prša et al. 2022). Eclipsing binaries from both catalogs have excess RV noise that meets our threshold in ∼70% of stars, compared to the “field” rate of ∼15%–20%.
Paper: paired: A Statistical Framework for Detecting Stellar Binarity with Gaia RVs. I. Sensitivity to Unresolved Binaries
Authors: Quadry Chance, Daniel Foreman-Mackey, Sarah Ballard, Andrew R. Casey, Trevor J. David, Adrian M. Price-Whelan
Figure caption: Here, we compare our results with 177,410 spectroscopic binary RV semi-amplitudes reported in Gaia DR3. The left panel is the comparison of our estimated semi-amplitude to the reported semi-amplitude colored by magnitude. There is tight agreement across the magnitude range. The right panel is the comparison of estimated semi-amplitudes for the same sources, this time colored by the estimated RV uncertainty for each source.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Top panel: comparison of the C34S (2–1) spectra computed with different models. The spectrum computed with the LOC + MCMC approach is plotted with a red solid line (model 0). The spectrum computed with the pyRate abundance profile and the resulting LOC + MCMC fv and σturb values is plotted with a dotted gray line (model 1). The C34S spectrum computed with the pyRate fractional abundance profile and the prestellar core physical model velocity profile (E. Keto et al. 2015) and σturb = 0.075 km s−1 is plotted with a gray dashed line (model 2). Finally, the observations are plotted with a black solid line. Bottom panel: the C34S fractional abundance profile obtained from the LOC + MCMC modeling of the observed line profile is plotted as a solid white line over a red solid band, indicating the model uncertainties. This is compared with the fractional abundance profile obtained from pyRate, plotted with a gray dashed–dotted line.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Schematics of the abundance profiles used for the radiative transfer modeling. The vertical axis represents the abundance, and the horizontal axis is the radius in units of parsecs. From the center of the core (left) to the parameter r, we have the inner fractional abundance ain, and from r to 0.32 pc, there is the outer fractional abundance aout. This constitutes the spatial extent of the nonextended model, as indicated by the red stripe at the bottom of the plot. From 0.32 to 1 pc, we have the shaded blue area representing the external layer characterized by an external fractional abundance aext, which we set to the molecular fractional abundance found toward diffuse clouds. Thus, the extended model (from the center to 1 pc) is indicated by the blue stripe at the bottom of the plot. The parameters framed in a box (ain, aout, and r) are those explored by the MCMC.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Same as Figure 4 but for the 34SO (2, 3–1, 2) transition.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Same as Figure 4 but for the H2CO (21,2–11,1) transition. Notice that in this case, the extended model is presented; thus, model 0 as well as the abundance profile uncertainties are plotted in blue. In the same way as for Figure 9, the abundance line profile computed with the LOC + MCMC is plotted with a sky blue color for better contrast.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Same as Figure 4 but for the HC17O+ (1–0) transition.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Same as Figure 4 but for the SO (2, 3–1, 2) transition.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Same as Figure 4 but for the HCO+ (1–0) transition. Notice that in this case, as the extended model was used, both the model 0 spectrum as well as the abundance profile uncertainty bands are plotted in blue. For better contrast, the white line showing the abundance profile is plotted in this case with a sky blue color.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Same as Figure 4 but for the CS (2–1) transition nonextended model.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Same as for Figure 4 but for the H2CO (21,2–11,1) transition.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Same as Figure 4 but for the c-C3H2 (21,2–10,1) transition. Notice that in this case, the extended model is presented; thus, model 0 as well as the abundance profile uncertainties are plotted in blue. In the same way as for Figure 9, the abundance line profile computed with the LOC + MCMC is plotted with a sky blue color for better contrast.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: The observed C34S (2–1) transition is plotted in black, the LOC + MCMC spectrum is plotted in red, and the optical depth (τ) is plotted with a gray dashed line. An additional y-axis (right) indicating the optical depth is included.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Same as Figure 4 but for the c-C3H2 (21,2–10,1) transition.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Schematics of the L1544 layers traced by the different molecular transitions presented in the previous sections.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Same as Figure 15 but for the CS (2–1) transition.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Corner plot of the HC17O+ (1–0) parameters used for the LOC + MCMC in Figure 6.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Corner plot of the 34SO (2, 3–1, 2) parameters used for the LOC + MCMC in Figure 5.