adsabs/AstroCLIMB huggingface dataset:
Paper: Physical Environments of the Luminosity Outburst Source NGC 6334I Traced by Thermal and Maser Lines of Multiple Molecules 
Authors: Jiong-Heng Wu, Xi Chen, Yan-Kun Zhang, Simon P. Ellingsen, Andrej M. Sobolev, Zhang Zhao, Shi-Ming Song, Zhi-Qiang Shen, Bin Li, Bo Xia, Rong-Bin Zhao, Jing-Qing Wang, Ya-Jun Wu
Figure caption: The left and right panels exhibit the spectra of the detected class I and II CH3OH maser (or maser candidate) transitions with TMRT, respectively. The frequencies, transitions, and observing date are given in each panel. If the spectra were only taken with the TMRT wide-band mode, we marked them with “wide” in the panel. Upward arrows in the panels are indications of the possible weak and narrow maser features.
Paper: Physical Environments of the Luminosity Outburst Source NGC 6334I Traced by Thermal and Maser Lines of Multiple Molecules 
Authors: Jiong-Heng Wu, Xi Chen, Yan-Kun Zhang, Simon P. Ellingsen, Andrej M. Sobolev, Zhang Zhao, Shi-Ming Song, Zhi-Qiang Shen, Bin Li, Bo Xia, Rong-Bin Zhao, Jing-Qing Wang, Ya-Jun Wu
Figure caption: An overview of the source structure of the observed high-mass star-forming region NGC 6334I traced by the 2.2 mm continuum emission produced from ALMA data ADS/JAO.ALMA#2017.1.00661.S. The peak of the continuum emission is 56 mJy beam−1. The pointing position of our TMRT observation is denoted with a red star.
Paper: Rubin LSST Observing Strategies to Maximize Volume and Uniformity Coverage of Star-forming Regions in the Galactic Plane
Authors: Loredana Prisinzano, Rosaria Bonito, Alessandro Mazzi, Francesco Damiani, Sabina Ustamujic, Peter Yoachim, Rachel Street, Mario Giuseppe Guarcello, Laura Venuti, William Clarkson, Lynne Jones, Leo Girardi
Figure caption: Map of the number of visits per HEALPix planned for the four representative OpSim relevant for our science case. The small yellow patches are the Deep Drilling Fields (DDFs) to which a higher number of observations is assigned. Note the Rubin LSST footprint of the baselines (panels (a) and (b)) is significantly different with respect to that of the vary_gp_gpfrac1.00_v2.0_10yr and the plane_priority_priority0.3_pbt_v2.1_10yr OpSim (panels (c) and (d)), where the number of visits at the WFD level is also assigned to the high dust extinction GP area. The sky is shown in the equal-area Mollweide projection in equatorial coordinates and the HEALPix grid resolution is N side = 64.
Paper: Rubin LSST Observing Strategies to Maximize Volume and Uniformity Coverage of Star-forming Regions in the Galactic Plane
Authors: Loredana Prisinzano, Rosaria Bonito, Alessandro Mazzi, Francesco Damiani, Sabina Ustamujic, Peter Yoachim, Rachel Street, Mario Giuseppe Guarcello, Laura Venuti, William Clarkson, Lynne Jones, Leo Girardi
Figure caption: Map of the number of detectable YSOs per HEALPix computed with our metric, using the baseline_v2.0_10yr, the 3D dust map and the crowding metric. The sky is shown in the equal-area Mollweide projection in equatorial coordinates and the HEALPix grid resolution is N side = 64.
Paper: Rubin LSST Observing Strategies to Maximize Volume and Uniformity Coverage of Star-forming Regions in the Galactic Plane
Authors: Loredana Prisinzano, Rosaria Bonito, Alessandro Mazzi, Francesco Damiani, Sabina Ustamujic, Peter Yoachim, Rachel Street, Mario Giuseppe Guarcello, Laura Venuti, William Clarkson, Lynne Jones, Leo Girardi
Figure caption: Map of the number of YSOs per HEALPix as computed by our metric, adopting the OpSim surveys listed in Table 1 and indicated by the names superimposed on top of each panel. The sky is shown in the equal-area Mollweide projection in equatorial coordinates and the HEALPix grid resolution is N side = 64. Note that the map in panel (a) is identical to the map shown in Figure 2.
Paper: Rubin LSST Observing Strategies to Maximize Volume and Uniformity Coverage of Star-forming Regions in the Galactic Plane
Authors: Loredana Prisinzano, Rosaria Bonito, Alessandro Mazzi, Francesco Damiani, Sabina Ustamujic, Peter Yoachim, Rachel Street, Mario Giuseppe Guarcello, Laura Venuti, William Clarkson, Lynne Jones, Leo Girardi
Figure caption: Map of the number of detectable YSOs per HEALPix computed with our metric, using the 2D dust map (left panel) and the 3D dust map (right panel). In both cases the baseline_v2.0_10yr has been adopted. The sky is shown in the equal-area Mollweide projection in equatorial coordinates and the HEALPix grid resolution is N side = 64.
Paper: Rubin LSST Observing Strategies to Maximize Volume and Uniformity Coverage of Star-forming Regions in the Galactic Plane
Authors: Loredana Prisinzano, Rosaria Bonito, Alessandro Mazzi, Francesco Damiani, Sabina Ustamujic, Peter Yoachim, Rachel Street, Mario Giuseppe Guarcello, Laura Venuti, William Clarkson, Lynne Jones, Leo Girardi
Figure caption: Number of detected YSOs as a function of the distance for the four OpSim indicated in Table 1.
Paper: The Study of the Circumgalactic Medium with Quasar Pairs 
Authors: Zhi-Fu Chen, Huan-Chang Qin, Jin-Ting Cai, Yu-Tao Zhou, Zhe-Geng Chen, Ting-Ting Pang, Zhi-Wen Wang, Kang-Fa Cheng
Figure caption: Examples of two pairs of quasars. Left panels show the SDSS spectra of quasars. Red solid lines are the fitting pseudocontinuum, blue dashed lines label the positions of Mg II emission lines of foreground quasars, and the shaded yellow regions label the spectral regions used to search for associated Mg  II absorption lines of foreground quasars. For the quasar pair of J231156.65 + 043522.9 and J231156.86 + 043550.6, having a projected distance of d p = 201.3  kpc, an obvious Mg  II absorption line is displayed in the spectra of foreground quasars, but not in the spectra of background quasars. For the quasar pair of J084331.09 + 111234.3 and J084331.84 + 111235.3, having a projected distance of d p = 79  kpc, an obvious Mg  II absorption line is displayed in the spectra of background quasars, but not in the spectra of foreground quasars. Right panels show the SDSS images of the fields around the foreground quasars. The background and foreground quasars are labeled as Q  B  and Q  F , respectively. The purple lines at the top left of images are 10″ in length.
Paper: The Study of the Circumgalactic Medium with Quasar Pairs 
Authors: Zhi-Fu Chen, Huan-Chang Qin, Jin-Ting Cai, Yu-Tao Zhou, Zhe-Geng Chen, Ting-Ting Pang, Zhi-Wen Wang, Kang-Fa Cheng
Figure caption: The incident rate of detected TRA Mg  II absorption lines as a function of projected distance. Horizontal solid lines represent incident rates of detected LOS Mg  II absorption lines, and dotted–dashed lines represent ±1σ error of the incident rates of detected LOS Mg  II absorption lines. Note that these fractions for the LOS Mg  II are averaged over the entire velocity bin considered. Panel (a) is for all the quasar pairs, where f c = 8.554% ± 0.381% for the LOS Mg  II absorption lines. (b) Black symbols (circles and horizonal lines) are for the quasar pairs whose foreground quasars have LogL bol ≤ 45.66 erg s−1, and the red symbols (stars and horizonal lines) are for the quasar pairs whose foreground quasars have LogL bol > 45.66 erg s−1. For the LOS Mg  II absorption lines, faint foreground quasars have f c = 11.919% ± 0.633%, and luminous quasars have f c = 5.283% ± 0.433%.
Paper: The Study of the Circumgalactic Medium with Quasar Pairs 
Authors: Zhi-Fu Chen, Huan-Chang Qin, Jin-Ting Cai, Yu-Tao Zhou, Zhe-Geng Chen, Ting-Ting Pang, Zhi-Wen Wang, Kang-Fa Cheng
Figure caption: Mg  II rest equivalent width, the sum of Mg II λ2796 and Mg II λ2803 lines, as a function of projected distance for the TRA absorption lines. (a) Black filled circles are for all the quasar pairs; green and orange unfilled squares are for the quasar pairs whose foreground quasars have z em(fg) < 1.5 and z em(fg) < 0.8, respectively; blue filled triangles and red unfilled triangles are for the TRA Mg  II absorption lines around the emission line galaxies and luminous red galaxies from Lan & Mo (2018), respectively. (b) Black circles are for the quasar pairs whose foreground quasars have ﹩\mathrm{Log}{L}_{\mathrm{bol}}\leqslant 45.66﹩ erg s−1, and the red stars are for the quasar pairs whose foreground quasars have ﹩\mathrm{Log}{L}_{\mathrm{bol}}\gt 45.66﹩ erg s−1, where the ﹩\mathrm{Log}{L}_{\mathrm{bol}}=45.66﹩ erg s−1 is the median value of the bolometric luminosities of foreground quasars.
Paper: The Study of the Circumgalactic Medium with Quasar Pairs 
Authors: Zhi-Fu Chen, Huan-Chang Qin, Jin-Ting Cai, Yu-Tao Zhou, Zhe-Geng Chen, Ting-Ting Pang, Zhi-Wen Wang, Kang-Fa Cheng
Figure caption: Distributions of projected distances of quasar pairs, which have been normalized by the circular area spanned by each annulus. Black symbols are for all the quasar pairs, and red symbols are only for quasar pairs with detected TRA Mg  II absorption lines in the background quasar spectra.
Paper: The Study of the Circumgalactic Medium with Quasar Pairs 
Authors: Zhi-Fu Chen, Huan-Chang Qin, Jin-Ting Cai, Yu-Tao Zhou, Zhe-Geng Chen, Ting-Ting Pang, Zhi-Wen Wang, Kang-Fa Cheng
Figure caption: (a) Velocity dispersions of gas clouds traced by Mg  II absorption lines. Black solid line and red dashed lines are for the TRA and LOS Mg  II absorption lines, respectively. The thick horizontal line is for the mean uncertainty of line widths, accounting for the typical spectral resolution of the SDSS/BOSS. (b) Velocity dispersions of gas clouds traced by TRA Mg  II absorption lines as a function of projected distances.
Paper: The Study of the Circumgalactic Medium with Quasar Pairs 
Authors: Zhi-Fu Chen, Huan-Chang Qin, Jin-Ting Cai, Yu-Tao Zhou, Zhe-Geng Chen, Ting-Ting Pang, Zhi-Wen Wang, Kang-Fa Cheng
Figure caption: Velocity distributions of Mg  II absorption lines relative to foreground quasar systemic redshifts. Black solid line and red dashed lines are for the TRA and LOS Mg  II absorption lines, respectively.
Paper: The Study of the Circumgalactic Medium with Quasar Pairs 
Authors: Zhi-Fu Chen, Huan-Chang Qin, Jin-Ting Cai, Yu-Tao Zhou, Zhe-Geng Chen, Ting-Ting Pang, Zhi-Wen Wang, Kang-Fa Cheng
Figure caption: Redshift distributions. The black solid line and red dashed line are for background and foreground quasars, respectively.
Paper: The CAMELS Project: Public Data Release
Authors: Francisco Villaescusa-Navarro, Shy Genel, Daniel Anglés-Alcázar, Lucia A. Perez, Pablo Villanueva-Domingo, Digvijay Wadekar, Helen Shao, Faizan G. Mohammad, Sultan Hassan, Emily Moser, Erwin T. Lau, Luis Fernando Machado Poletti Valle, Andrina Nicola, Leander Thiele, Yongseok Jo, Oliver H. E. Philcox, Benjamin D. Oppenheimer, Megan Tillman, ChangHoon Hahn, Neerav Kaushal, Alice Pisani, Matthew Gebhardt, Ana Maria Delgado, Joyce Caliendo, Christina Kreisch, Kaze W. K. Wong, William R. Coulton, Michael Eickenberg, Gabriele Parimbelli, Yueying Ni, Ulrich P. Steinwandel, Valentina La Torre, Romeel Dave, Nicholas Battaglia, Daisuke Nagai, David N. Spergel, Lars Hernquist, Blakesley Burkhart, Desika Narayanan, Benjamin Wandelt, Rachel S. Somerville, Greg L. Bryan, Matteo Viel, Yin Li, Vid Irsic, Katarina Kraljic, Federico Marinacci, Mark Vogelsberger
Figure caption: In this plot, we illustrate the similarities and differences between the IllustrisTNG and SIMBA suites considering eight different properties of the subhalos: (1) stellar mass, M *, (2) gas mass, M g, (3) black hole mass, M BH, (4) stellar half-mass–radius, R *, (5) stellar metallicity, Z *, (6) gas metallicity, Z g, (7) maximum circular velocity, ﹩{V}_{\max }﹩, and (8) star formation rate, SFR. We show the 1D and 2D distribution of these properties for all galaxies in the LH sets of the IllustrisTNG (orange) and SIMBA (green) suites. Masses are in units of 1010/(M ⊙ h −1), R * in kiloparsecs per hour, ﹩{V}_{\max }﹩ in kilometers per second, and SFR in M ⊙ yr−1.
Paper: The CAMELS Project: Public Data Release
Authors: Francisco Villaescusa-Navarro, Shy Genel, Daniel Anglés-Alcázar, Lucia A. Perez, Pablo Villanueva-Domingo, Digvijay Wadekar, Helen Shao, Faizan G. Mohammad, Sultan Hassan, Emily Moser, Erwin T. Lau, Luis Fernando Machado Poletti Valle, Andrina Nicola, Leander Thiele, Yongseok Jo, Oliver H. E. Philcox, Benjamin D. Oppenheimer, Megan Tillman, ChangHoon Hahn, Neerav Kaushal, Alice Pisani, Matthew Gebhardt, Ana Maria Delgado, Joyce Caliendo, Christina Kreisch, Kaze W. K. Wong, William R. Coulton, Michael Eickenberg, Gabriele Parimbelli, Yueying Ni, Ulrich P. Steinwandel, Valentina La Torre, Romeel Dave, Nicholas Battaglia, Daisuke Nagai, David N. Spergel, Lars Hernquist, Blakesley Burkhart, Desika Narayanan, Benjamin Wandelt, Rachel S. Somerville, Greg L. Bryan, Matteo Viel, Yin Li, Vid Irsic, Katarina Kraljic, Federico Marinacci, Mark Vogelsberger
Figure caption: This scheme shows the generic structure of CAMELS data. The top level represents the type of data it contains (power spectra in this case). Inside that folder, there are typically four folders containing the data for the three different simulation suites: IllustrisTNG, SIMBA, and their N-body counterparts (IllustrisTNG_DM and SIMBA_DM). Within each of those folders, there are numerous folders, containing the data from the different simulations belonging to each suite; i.e., the simulations from the four sets: LH, 1P, CV, and EX. Finally, inside each of those folders, the user can find the data products themselves. In this particular case, the power spectra for the different component.
Paper: The CAMELS Project: Public Data Release
Authors: Francisco Villaescusa-Navarro, Shy Genel, Daniel Anglés-Alcázar, Lucia A. Perez, Pablo Villanueva-Domingo, Digvijay Wadekar, Helen Shao, Faizan G. Mohammad, Sultan Hassan, Emily Moser, Erwin T. Lau, Luis Fernando Machado Poletti Valle, Andrina Nicola, Leander Thiele, Yongseok Jo, Oliver H. E. Philcox, Benjamin D. Oppenheimer, Megan Tillman, ChangHoon Hahn, Neerav Kaushal, Alice Pisani, Matthew Gebhardt, Ana Maria Delgado, Joyce Caliendo, Christina Kreisch, Kaze W. K. Wong, William R. Coulton, Michael Eickenberg, Gabriele Parimbelli, Yueying Ni, Ulrich P. Steinwandel, Valentina La Torre, Romeel Dave, Nicholas Battaglia, Daisuke Nagai, David N. Spergel, Lars Hernquist, Blakesley Burkhart, Desika Narayanan, Benjamin Wandelt, Rachel S. Somerville, Greg L. Bryan, Matteo Viel, Yin Li, Vid Irsic, Katarina Kraljic, Federico Marinacci, Mark Vogelsberger
Figure caption: We show two images of the gas distribution of two distinct IllustrisTNG simulations. The one on the top displays the results for a simulation with high supernova feedback strength, while the one on the bottom is from a simulation with low supernova feedback. The color represents gas temperature, while its brightness corresponds to the gas density. Finally, we apply an extinction based on gas metallicity. As can be seen, the effect of feedback is very pronounced: it not only affects the gas abundance and temperature on the smallest galaxies but also changes the gas distribution in the most massive galaxies.
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: Same format as Figure 4, but for the B_H model (#4 in Table 1) and B ranges from 0.03 to 30.
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: Same format as Figure 4, but for the B_L model (#3 in Table 1). The gray dashed line represents B ∝ ρ normalized at (0,0).
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: Same format as Figure 4, but for the ρ 2_L model (#5 in Table 1).
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: Same format as Figure 4, but for the R 2_L model (#7 in Table 1).
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: Same format as Figure 4, but for the R 2_H model (#8 in Table 1).
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: Same format as Figure 4, but for the η_H model (#2 in Table 1).
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: Same format as Figure 4, but for the T_H model (#10 in Table 1).
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: Same format as Figure 4, but for the T_L model (#9 in Table 1).
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: Same format as Figure 4, but for the ρ 2_H model (#6 in Table 1).
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: Distribution of the “ringiness” parameter for the 20 random projections of the last time step of the different simulations. The parameter gives the number of detected rings with inner radii between 5 and 20 pixels and a radius ratio between 1.2 and 1.4 multiplied by their contrast relative to a filled circle with the same outer radius. The distributions are given as whisker plots like in Figure 21.
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: Distribution of the most prominent structure widths detected in 20 random projections of the last time step (1 Myr) of the different simulations through the anisotropic wavelet analysis. The distributions are given as whisker plots giving the two central quartiles of the distributions as boxes and the extremes (outer quartiles, like error bars) if they fall within 1.5 times the total span of the inner quartiles. Outliers beyond that limit are shown as individual circles. For simulation #14 (v  z _H) the upper quartile is truncated extending up to 165 pixels.
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: Same format as Figure 4, but for the v  x _H model (#12 in Table 1). The gray dashed line represents B ∝ ρ normalized at (0,0).
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: Same format as Figure 4, but for the v  z _H model (#14 in Table 1).
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: Same format as Figure 4, but for the v  z _L model (#13 in Table 1).
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: Same format as Figure 4, but for the v  x _L model (#11 in Table 1).
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: MRCOL results (model #0 in Table 1). Each row shows the results from a time step labeled in the leftmost panel. The first column shows the ρ-PDF from 5 × 10−5 to 5 × 102. The middle three columns show the RT images at different projections. They have the same color scale (linear) and range (0–100 MJy sr−1). No noise is implemented. The fifth column shows the B–ρ relation as a 2D histogram. ρ ranges from 10−3 to 103, and B ranges from 0.014 to 15. The color scale is in probability density in logarithmic scale (10−2 to 102).
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: An illustration of CMR in two viewing angles. (a) A view in the x–y plane. The Cartesian coordinate system (red) centers at the collision point. The x-axis points rightward, and the y-axis points to the top. The z-axis points toward us as indicated by the red circled points. The clouds have colliding velocities v 1,x  and v 2,x. The B-field points toward us (marked as black circled points) for x < 0 and away from us (marked as black circled crosses) for x > 0. After collision, the filament (orange) forms along the y-axis. (b) A view in the z–x projection. In this view, the B-field is parallel to the plane of the sky. The y-axis points toward us as indicated by the red circled point. After collision, the filament (orange) forms along the y-axis, which points toward us. The green ellipse marks the location of the compression pancake if there are no B-fields. With antiparallel fields and CMR, the field reconnects at two tips of the pancake and forms a loop (black dashed arrow curve) around the pancake. Due to the magnetic tension force, the pancake is squeezed into the central axis (y-axis), becoming a filament. The fiducial model parameters in code units are shown in both panels (see row 1 in Table 1).
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: 3D illustration of the field topology around the CMR filament. The color plot shows the isosurface of the filament at a density of 10 (﹩{n}_{{{\rm{H}}}_{2}}=8400﹩ cm−3). The black lines are B-field streamlines. The streamline seeding and length are limited so as to avoid too much crowdedness. See Figure 5 for an illustration of the 3D geometry.
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: Same format as Figure 4, but for the η_L model (#1 in Table 1).
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: Top row: isosurface of B-magnitude at t = 0.1 in MRCOL. The left panel shows B = 3.5, and the right panel shows B = 5. Bottom row: isosurface of B-magnitude at t = 0.5 in MRCOL. The left panel shows B = 2, and the right panel shows B = 3.
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: Illustration of the ring-finding results for the projection of the fiducial model, MRCOL, that shows most ring and fork structures. The left panel shows the column density map, where the centers of the 37 detected rings are marked by diamonds. The shade of gray of the diamond characterizes the contrast of the ring changing from 0.02 for almost black symbols to 0.4 for the strongest ring marked by a white diamond. The right panel visualizes the rings by showing only that fraction of the column density map that falls within the corresponding ring annuli.
Paper: CMR Exploration. I. Filament Structure with Synthetic Observations
Authors: Shuo Kong, 朔 孔, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu
Figure caption: Top row: isosurface of density at t = 0.1 in MRCOL. The left panel shows ρ = 0.5, and the right panel shows ρ = 1. Bottom row: isosurface of density at t = 0.5 in MRCOL. The left panel shows ρ = 0.5, and the right panel shows ρ = 1.