adsabs/AstroCLIMB huggingface dataset:
Paper: Rest-frame Optical Spectroscopy of z ∼ 2 Quasars with Steep Hard X-Ray Spectral Shapes: X-Ray Selection of Super-Eddington Accretion and Verification
Authors: Y. Chen, B. Luo, J. Huang
Figure caption: IR-to-X-ray SEDs for our sources. The IR–UV photometric data were collected from WISE, NEOWISE, 2MASS, SDSS, GALEX, and XMM-Newton OM. For NEOWISE, average measurements are displayed. Our P200/Tspec spectra are also included as red curves; for J0838, the HST UV spectra are displayed. Some of the error bars are smaller than the symbol size. The green dashed curve illustrates the mean quasar SED from C. M. Krawczyk et al. (2013), normalized at the 2500 Å luminosity interpolated from the SDSS photometric data. The X-ray component of the mean quasar SED is determined from the αOX–L2500 Å relation in A. T. Steffen et al. (2006). These photometric and spectroscopic data might be affected by mild variability effects. Overall, our quasars show typical IR-to-X-ray SEDs.
Paper: Is Dark Energy Changing? Probing the Universe’s Expansion with Present and Future Astronomical Probes
Authors: Mehdi Rezaei, Supriya Pan, Weiqiang Yang, David F. Mota
Figure caption: One-dimensional marginalized posterior distributions and two-dimensional joint contours at 1σ and 2σ considering some of the model parameters are shown for nonflat Padé-I using the combined data sets SN+BAO+BBN+H(z), SN+BAO+BBN+H(z)+GW, SN+BAO+BBN+H(z)+CMB, and SN+BAO+BBN+H(z)+CMB+GW. The solid lines through w1 = 0 and w2 = 0 correspond to the ΛCDM cosmology, which is also considered as the fiducial model for generating the GW mock data set.
Paper: Is Dark Energy Changing? Probing the Universe’s Expansion with Present and Future Astronomical Probes
Authors: Mehdi Rezaei, Supriya Pan, Weiqiang Yang, David F. Mota
Figure caption: One-dimensional marginalized posterior distributions and two-dimensional joint contours at 1σ and 2σ considering some of the model parameters are shown for flat Padé-I using the combined data sets SN+BAO+BBN+H(z), SN+BAO+BBN+H(z)+GW, SN+BAO+BBN+H(z)+CMB, and SN+BAO+BBN+H(z)+CMB+GW. The solid lines through w1 = 0 and w2 = 0 correspond to the ΛCDM cosmology, which is also considered as the fiducial model for generating the GW mock data set.
Paper: Is Dark Energy Changing? Probing the Universe’s Expansion with Present and Future Astronomical Probes
Authors: Mehdi Rezaei, Supriya Pan, Weiqiang Yang, David F. Mota
Figure caption: One-dimensional marginalized posterior distributions and two-dimensional joint contours at 1σ and 2σ considering some of the model parameters are shown for flat SPadé-I using the combined data sets SN+BAO+BBN+H(z), SN+BAO+BBN+H(z)+GW, SN+BAO+BBN+H(z)+CMB, and SN+BAO+BBN+H(z)+CMB+GW. The solid line through w2 = 0 corresponds to the ΛCDM cosmology, which is also considered as the fiducial model for generating the GW mock data set.
Paper: Rest-frame Optical Spectroscopy of z ∼ 2 Quasars with Steep Hard X-Ray Spectral Shapes: X-Ray Selection of Super-Eddington Accretion and Verification
Authors: Y. Chen, B. Luo, J. Huang
Figure caption:  ﹩\mathrm{log}\,{L}_{[{\rm{O}}\,{\rm{III}}]}﹩ vs. ﹩\mathrm{log}\,{L}_{2-10\,{\rm{keV}}}﹩ for our targets (red stars) and data collected from literature (gray dots). The dotted–dashed, dotted, and dashed lines represent the best-fit relations from F. Panessa et al. (2006), M. Meléndez et al. (2008), and Y. Ueda et al. (2015), respectively. Our quasars do not display significantly weaker L[O III] compared to the other quasars with similar X-ray luminosities.
Paper: Is Dark Energy Changing? Probing the Universe’s Expansion with Present and Future Astronomical Probes
Authors: Mehdi Rezaei, Supriya Pan, Weiqiang Yang, David F. Mota
Figure caption: Redshift distribution of the SN, H(z), and GW samples using the normalized histogram description. Note that in the redshift regions (3–4) and (4–5) only the GW data are present; in particular, only a few data points of the GW sample are in the latter region, and hence the vertical bar in this redshift region is barely visible.
Paper: Rest-frame Optical Spectroscopy of z ∼ 2 Quasars with Steep Hard X-Ray Spectral Shapes: X-Ray Selection of Super-Eddington Accretion and Verification
Authors: Y. Chen, B. Luo, J. Huang
Figure caption: Γ vs. L2−10 keV distributions for the 21 Γ > 2 quasars. Our final sample objects (nine quasars) are in red, and the other 12 quasars without NIR observations are in purple. The Γ and L2−10 keV distributions are overall consistent between the two groups.
Paper: The VISCACHA Survey XV: Tracing the 3D Structure and Chemical Evolution of the Outskirts of the Large Magellanic Cloud from Star Clusters
Authors: Bernardo P. L. Ferreira, João F. C. Santos Jr., Bruno Dias, Francisco F. S. Maia, Saroon Sasi, Pieter Westera, Raphael A. P. Oliveira, Stefano O. Souza, José G. Fernández-Trincado, Leandro Kerber, Bruno Quint, David Sanmartim, Luciano Fraga, Tina Armond
Figure caption: The top left panel shows an edge-on projection of the LMC for the star clusters analyzed in this work, with respect to the axis xg (see text for details). The bottom panel shows a moving average of the zp values of the clusters, in intervals of 1.5 kpc. The position of cluster SL 2 (analyzed in Paper XII) is shown as the red-bordered circle. The second and third panels show similar plots for fields of RC stars analyzed in S. Saroon & S. Subramanian (2022), considering their full sample (second panel) and only fields within 10 arcmin of our clusters (third). The color scales indicate the number of stars within each observed field, and the moving averages were weighed by this number. The final panels show the combined sample. The inset plot shows a similar face-on view of the galaxy with the red arrow indicating the projected direction of the viewing angle (which is opposite to the increase of xg).
Paper: The VISCACHA Survey XV: Tracing the 3D Structure and Chemical Evolution of the Outskirts of the Large Magellanic Cloud from Star Clusters
Authors: Bernardo P. L. Ferreira, João F. C. Santos Jr., Bruno Dias, Francisco F. S. Maia, Saroon Sasi, Pieter Westera, Raphael A. P. Oliveira, Stefano O. Souza, José G. Fernández-Trincado, Leandro Kerber, Bruno Quint, David Sanmartim, Luciano Fraga, Tina Armond
Figure caption: Face-on view of the LMC. Gray dots correspond to extended objects in the galaxy cataloged by E. Bica et al. (2008), assuming that they lie in the plane of the galaxy. Colored circles correspond to clusters analyzed in this work. Arrows indicate the projected directions of the Sun (leaving the page) and the SMC (entering the page) from the center of the galaxy (red star). The thin, black circles indicate ρ = 4, 5, 6 kpc. The position of cluster SL 2 (analyzed in Paper XII) is shown as the red-bordered circle.
Paper: The VISCACHA Survey XV: Tracing the 3D Structure and Chemical Evolution of the Outskirts of the Large Magellanic Cloud from Star Clusters
Authors: Bernardo P. L. Ferreira, João F. C. Santos Jr., Bruno Dias, Francisco F. S. Maia, Saroon Sasi, Pieter Westera, Raphael A. P. Oliveira, Stefano O. Souza, José G. Fernández-Trincado, Leandro Kerber, Bruno Quint, David Sanmartim, Luciano Fraga, Tina Armond
Figure caption: For each panel, we show, on the top, the values of the ages obtained for each cluster as a function of their galactocentric distances r, distances to the LMC plane ∣zp∣, and galactocentric distances projected in the LMC plane ρ, respectively. On the bottom, we show histograms with the distribution of each pair of parameters and the average age taken in intervals of 1.0 kpc (for r and ∣zp∣) and 0.5 kpc (for ρ). The inset displays a face-on view of the LMC, similar to Figure 7.
Paper: The VISCACHA Survey XV: Tracing the 3D Structure and Chemical Evolution of the Outskirts of the Large Magellanic Cloud from Star Clusters
Authors: Bernardo P. L. Ferreira, João F. C. Santos Jr., Bruno Dias, Francisco F. S. Maia, Saroon Sasi, Pieter Westera, Raphael A. P. Oliveira, Stefano O. Souza, José G. Fernández-Trincado, Leandro Kerber, Bruno Quint, David Sanmartim, Luciano Fraga, Tina Armond
Figure caption: The top panel shows the variation of the coordinate zp with the azimuthal angle φ for the clusters analyzed in this work. The bottom panel shows the average value for zp in 30° intervals. The position of the cluster SL 2 (analyzed in Paper XII) is shown as the red-bordered circle.
Paper: The VISCACHA Survey XV: Tracing the 3D Structure and Chemical Evolution of the Outskirts of the Large Magellanic Cloud from Star Clusters
Authors: Bernardo P. L. Ferreira, João F. C. Santos Jr., Bruno Dias, Francisco F. S. Maia, Saroon Sasi, Pieter Westera, Raphael A. P. Oliveira, Stefano O. Souza, José G. Fernández-Trincado, Leandro Kerber, Bruno Quint, David Sanmartim, Luciano Fraga, Tina Armond
Figure caption: Each pair of panels shows, on the top, the AMR obtained for star clusters analyzed in this work and G. I. Perren et al. (2017), W. Narloch et al. (2022), and A. P. Milone et al. (2023), as indicated in the legends. On the bottom, the metallicity is averaged over 0.5 Gyr intervals. The insets show the positions of the clusters in the celestial sphere, superimposed with a composite image of the LMC by A. Mellinger (2009), as seen in Figures 1 and 2.
Paper: The VISCACHA Survey XV: Tracing the 3D Structure and Chemical Evolution of the Outskirts of the Large Magellanic Cloud from Star Clusters
Authors: Bernardo P. L. Ferreira, João F. C. Santos Jr., Bruno Dias, Francisco F. S. Maia, Saroon Sasi, Pieter Westera, Raphael A. P. Oliveira, Stefano O. Souza, José G. Fernández-Trincado, Leandro Kerber, Bruno Quint, David Sanmartim, Luciano Fraga, Tina Armond
Figure caption: The top panels show the AMR of star clusters from different components of the Magellanic System, obtained by different works of the VISCACHA collaboration: left for the LMC (this work), middle for the Magellanic Bridge (R. A. P. Oliveira et al. 2023), and right for the SMC (B. Dias et al. 2021; S. Saroon et al. 2025). Hollowed points correspond from the literature adopted by S. Saroon et al. (2025) for the clusters Lindsay 3 (B. Dias et al. 2014) and Lindsay 7 (M. C. Parisi et al. 2009, 2014). The bottom panel shows the spatial distribution of the clusters. Gray dots correspond to extended objects cataloged by E. Bica et al. (2008).
Paper: The VISCACHA Survey XV: Tracing the 3D Structure and Chemical Evolution of the Outskirts of the Large Magellanic Cloud from Star Clusters
Authors: Bernardo P. L. Ferreira, João F. C. Santos Jr., Bruno Dias, Francisco F. S. Maia, Saroon Sasi, Pieter Westera, Raphael A. P. Oliveira, Stefano O. Souza, José G. Fernández-Trincado, Leandro Kerber, Bruno Quint, David Sanmartim, Luciano Fraga, Tina Armond
Figure caption: The large panel shows the AMR of the studied clusters with the red dotted line corresponding to the bursting model of B. E. J. Pagel & G. Tautvaisiene (1998). The bottom panel shows an average AMR in intervals of 0.5 Gyr. The top and right panels display the distribution of the ages and metallicities. On the top right, a face-on view of the LMC, similar to Figure 7 is exhibited.
Paper: The VISCACHA Survey XV: Tracing the 3D Structure and Chemical Evolution of the Outskirts of the Large Magellanic Cloud from Star Clusters
Authors: Bernardo P. L. Ferreira, João F. C. Santos Jr., Bruno Dias, Francisco F. S. Maia, Saroon Sasi, Pieter Westera, Raphael A. P. Oliveira, Stefano O. Souza, José G. Fernández-Trincado, Leandro Kerber, Bruno Quint, David Sanmartim, Luciano Fraga, Tina Armond
Figure caption: Same as Figure 13, but for the metallicity instead of the age.
Paper: The VISCACHA Survey XV: Tracing the 3D Structure and Chemical Evolution of the Outskirts of the Large Magellanic Cloud from Star Clusters
Authors: Bernardo P. L. Ferreira, João F. C. Santos Jr., Bruno Dias, Francisco F. S. Maia, Saroon Sasi, Pieter Westera, Raphael A. P. Oliveira, Stefano O. Souza, José G. Fernández-Trincado, Leandro Kerber, Bruno Quint, David Sanmartim, Luciano Fraga, Tina Armond
Figure caption: Distribution of the binary fraction obtained for the clusters analyzed in this work.
Paper: The VISCACHA Survey XV: Tracing the 3D Structure and Chemical Evolution of the Outskirts of the Large Magellanic Cloud from Star Clusters
Authors: Bernardo P. L. Ferreira, João F. C. Santos Jr., Bruno Dias, Francisco F. S. Maia, Saroon Sasi, Pieter Westera, Raphael A. P. Oliveira, Stefano O. Souza, José G. Fernández-Trincado, Leandro Kerber, Bruno Quint, David Sanmartim, Luciano Fraga, Tina Armond
Figure caption: The left panel shows a similar face-on view of the LMC as Figure 7 for the clusters analyzed in A. Pieres et al. (2016) and in this work. The green shaded sector corresponds to a common region between both works. The middle panel shows, on the top, the AMR of the clusters found in both works, considering only objects in the common region. On the bottom, the metallicity is given as an average over 0.5 Gyr intervals. The black dashed line corresponds to the bursting model from B. E. J. Pagel & G. Tautvaisiene (1998). The right panel shows a similar plot for zp as a function of xp, with the black line corresponding to the LMC plane at zp = 0. The averages shown in the bottom panel were taken over intervals of 1.5 kpc
Paper: The VISCACHA Survey XV: Tracing the 3D Structure and Chemical Evolution of the Outskirts of the Large Magellanic Cloud from Star Clusters
Authors: Bernardo P. L. Ferreira, João F. C. Santos Jr., Bruno Dias, Francisco F. S. Maia, Saroon Sasi, Pieter Westera, Raphael A. P. Oliveira, Stefano O. Souza, José G. Fernández-Trincado, Leandro Kerber, Bruno Quint, David Sanmartim, Luciano Fraga, Tina Armond
Figure caption: Same as Figure 8 (top), the left panels of Figure 9 (bottom), and Figure 10 (bottom) for the results obtained using models that include rotation.
Paper: The VISCACHA Survey XV: Tracing the 3D Structure and Chemical Evolution of the Outskirts of the Large Magellanic Cloud from Star Clusters
Authors: Bernardo P. L. Ferreira, João F. C. Santos Jr., Bruno Dias, Francisco F. S. Maia, Saroon Sasi, Pieter Westera, Raphael A. P. Oliveira, Stefano O. Souza, José G. Fernández-Trincado, Leandro Kerber, Bruno Quint, David Sanmartim, Luciano Fraga, Tina Armond
Figure caption: Comparison between the results found in this work (with nonrotating models on the left and rotating models on the right) with spectroscopic and empirical evaluations of the metallicities of some of the clusters analyzed in this work (as listed in Table 3). The black dashed line indicates equality between the values. For E. W. Olszewski et al. (1991) and A. J. Grocholski et al. (2006), the colors of each point correspond to the number of stars used in the CaT analysis, as indicated in the colorbars.
Paper: The VISCACHA Survey XV: Tracing the 3D Structure and Chemical Evolution of the Outskirts of the Large Magellanic Cloud from Star Clusters
Authors: Bernardo P. L. Ferreira, João F. C. Santos Jr., Bruno Dias, Francisco F. S. Maia, Saroon Sasi, Pieter Westera, Raphael A. P. Oliveira, Stefano O. Souza, José G. Fernández-Trincado, Leandro Kerber, Bruno Quint, David Sanmartim, Luciano Fraga, Tina Armond
Figure caption: Same as Figure 13 but for the variation of age with the azimuthal angle φ. In the top panel, points are colored according to their distance to the galactic plane ∣zp∣. In the bottom, averages were taken in a 30° interval, and points are colored following the value of φ.
Paper: The VISCACHA Survey XV: Tracing the 3D Structure and Chemical Evolution of the Outskirts of the Large Magellanic Cloud from Star Clusters
Authors: Bernardo P. L. Ferreira, João F. C. Santos Jr., Bruno Dias, Francisco F. S. Maia, Saroon Sasi, Pieter Westera, Raphael A. P. Oliveira, Stefano O. Souza, José G. Fernández-Trincado, Leandro Kerber, Bruno Quint, David Sanmartim, Luciano Fraga, Tina Armond
Figure caption: Same as Figure A1, but for characterizations of the clusters’ ages and distances that do not use isochrone fitting.
Paper: The VISCACHA Survey XV: Tracing the 3D Structure and Chemical Evolution of the Outskirts of the Large Magellanic Cloud from Star Clusters
Authors: Bernardo P. L. Ferreira, João F. C. Santos Jr., Bruno Dias, Francisco F. S. Maia, Saroon Sasi, Pieter Westera, Raphael A. P. Oliveira, Stefano O. Souza, José G. Fernández-Trincado, Leandro Kerber, Bruno Quint, David Sanmartim, Luciano Fraga, Tina Armond
Figure caption: Distance to the LMC center for the clusters investigated in this work as a function of the zp coordinate and the heliocentric distance.
Paper: The VISCACHA Survey XV: Tracing the 3D Structure and Chemical Evolution of the Outskirts of the Large Magellanic Cloud from Star Clusters
Authors: Bernardo P. L. Ferreira, João F. C. Santos Jr., Bruno Dias, Francisco F. S. Maia, Saroon Sasi, Pieter Westera, Raphael A. P. Oliveira, Stefano O. Souza, José G. Fernández-Trincado, Leandro Kerber, Bruno Quint, David Sanmartim, Luciano Fraga, Tina Armond
Figure caption: Same as Figure 13, for the results obtained using models that include rotation.
Paper: The VISCACHA Survey XV: Tracing the 3D Structure and Chemical Evolution of the Outskirts of the Large Magellanic Cloud from Star Clusters
Authors: Bernardo P. L. Ferreira, João F. C. Santos Jr., Bruno Dias, Francisco F. S. Maia, Saroon Sasi, Pieter Westera, Raphael A. P. Oliveira, Stefano O. Souza, José G. Fernández-Trincado, Leandro Kerber, Bruno Quint, David Sanmartim, Luciano Fraga, Tina Armond
Figure caption: Comparison between the results found in this work (using nonrotating models) and previous characterizations of the same clusters using isochrone fitting (as listed in Table 3). The black dashed line indicates equality between the values for each parameter.
Paper: The VISCACHA Survey XV: Tracing the 3D Structure and Chemical Evolution of the Outskirts of the Large Magellanic Cloud from Star Clusters
Authors: Bernardo P. L. Ferreira, João F. C. Santos Jr., Bruno Dias, Francisco F. S. Maia, Saroon Sasi, Pieter Westera, Raphael A. P. Oliveira, Stefano O. Souza, José G. Fernández-Trincado, Leandro Kerber, Bruno Quint, David Sanmartim, Luciano Fraga, Tina Armond
Figure caption: Same as Figure 16 but for the variation of metallicity.
Paper: Magnetic Fields in the Bones of the Milky Way
Authors: Ian W. Stephens, Simon Coudé, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Andrés E. Guzmán, Alyssa Goodman, Takayoshi Kusune, Miaomiao Zhang, Nicole Karnath, Jessy Marin
Figure caption: Values of Bpos, λ, αvir, and ϵ for the sliding box analysis plotted against their respective gas density, ngas, color coded for each bone. Filled and open circles show where the velocity dispersion was estimated by high- and low-density tracers, respectively. αvir is shown as filled/open circles only where there is also a Bpos estimate, and as × or + symbols where there is no Bpos estimate, yet some SOFIA data still exists in the sliding box. The × and + symbols are for αvir parameters measured with high- and low-density tracers, respectively. Dashed lines in the bottom three panels are at y = 1. Bones are typically magnetically subcritical (fields are dominant), but have virial parameters that are above 1, implying gravity along much of the bones may be insufficient for collapse.
Paper: Magnetic Fields in the Bones of the Milky Way
Authors: Ian W. Stephens, Simon Coudé, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Andrés E. Guzmán, Alyssa Goodman, Takayoshi Kusune, Miaomiao Zhang, Nicole Karnath, Jessy Marin
Figure caption: Figure caption is the same as that of Figure 1, except now for Filament 2.
Paper: Magnetic Fields in the Bones of the Milky Way
Authors: Ian W. Stephens, Simon Coudé, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Andrés E. Guzmán, Alyssa Goodman, Takayoshi Kusune, Miaomiao Zhang, Nicole Karnath, Jessy Marin
Figure caption: Figure caption is the same as that of Figure 1, except now for Filament 8.
Paper: Magnetic Fields in the Bones of the Milky Way
Authors: Ian W. Stephens, Simon Coudé, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Andrés E. Guzmán, Alyssa Goodman, Takayoshi Kusune, Miaomiao Zhang, Nicole Karnath, Jessy Marin
Figure caption: Figure caption is the same as that of Figure 1, except now for Filament 5.
Paper: Magnetic Fields in the Bones of the Milky Way
Authors: Ian W. Stephens, Simon Coudé, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Andrés E. Guzmán, Alyssa Goodman, Takayoshi Kusune, Miaomiao Zhang, Nicole Karnath, Jessy Marin
Figure caption: Figure caption is the same as that of Figure 1, except now for Filament 4.
Paper: Magnetic Fields in the Bones of the Milky Way
Authors: Ian W. Stephens, Simon Coudé, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Andrés E. Guzmán, Alyssa Goodman, Takayoshi Kusune, Miaomiao Zhang, Nicole Karnath, Jessy Marin
Figure caption: Figure caption is the same as that of Figure 1, except now for the Snake.
Paper: Magnetic Fields in the Bones of the Milky Way
Authors: Ian W. Stephens, Simon Coudé, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Andrés E. Guzmán, Alyssa Goodman, Takayoshi Kusune, Miaomiao Zhang, Nicole Karnath, Jessy Marin
Figure caption: Ratio in measured velocity dispersions of the high-density tracer (δvlos,ld) and low-density tracer (δvlos,hd) as a function of gas column density Ngas for each bone. Data are binned in four equal-width intervals in Ngas, with black crosses showing the median ratio per bin. The dashed line marks a ratio of unity. The overall median ratio is indicated in the upper right of each panel. Comparisons are only shown where Pfrac/﹩{\sigma }_{{P}_{{\rm{frac}}}}﹩ > 2 and pixels are no more than 23″ from the spine.
Paper: Magnetic Fields in the Bones of the Milky Way
Authors: Ian W. Stephens, Simon Coudé, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Andrés E. Guzmán, Alyssa Goodman, Takayoshi Kusune, Miaomiao Zhang, Nicole Karnath, Jessy Marin
Figure caption: Caption is the same as that of Figure 5, but now only showing data in the first quartile (lowest values) for column density.
Paper: Magnetic Fields in the Bones of the Milky Way
Authors: Ian W. Stephens, Simon Coudé, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Andrés E. Guzmán, Alyssa Goodman, Takayoshi Kusune, Miaomiao Zhang, Nicole Karnath, Jessy Marin
Figure caption: Figure caption is the same as that of Figure 1, except now for G49.