adsabs/AstroCLIMB huggingface dataset:
Paper: Advancing Stellar Parameter Estimation: Uncertainty-Aware Astrophysical Fusion Network for Red Giant Ages and Abundances from Ultra-low-resolution Spectra—Applications to Galactic Archaeology
Authors: Jingzhen Sun, Yude Bu, Mengmeng Zhang, Jiangchuan Zhang, ShanShan Li, Yuhang Zhang, Ke Wang, Zhenping Yi, Xiaoming Kong, Meng Liu, Minglei Wu
Figure caption: [Fe/H] distributions of the individual subsamples, The [Fe/H] ratios of the high-α “young” stars are similar to those of the high-α old stars, while low-α young stars are obviously different from the former two subsamples.
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: Distributions of (a) log Wr[O III] and (b) RFe II for our sample (red solid histograms) and the GNIRS sub-A (blue histograms) and sub-B (green histograms) comparison samples. For the Wr[O III] distributions, upper limits are depicted using leftward arrows with the y-axis value representing the number of sources. Our objects show weaker [O III] and marginally stronger Fe II emission than the full GNIRS sample, and the differences are enhanced if the GNIRS sub-B sample is compared to it.
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: Similar to Figure 3, displaying the combined XMM-Newton pn and MOS spectra for J0223 overlaid with the best-fit simple power-law model. The XMM-Newton pn, MOS1, and MOS2 spectra and their corresponding best-fit models are shown in green, black, and blue, respectively. The bottom panel displays the residuals between the spectral data and the best-fit model, normalized by the errors.
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: (a) MBH,Fe II and (b) λEdd,Fe II vs. monochromatic luminosity at 5100 Å (L5100). Our sample is represented by the red stars, while the GNIRS sub-A and sub-B samples are shown as the blue and green triangles, respectively. Our quasars show overall lower luminosities and smaller SMBH masses than the comparison samples. But their λEdd,Fe II distribution is similar to that of the full comparison sample.
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: MBH,Fe II vs. λEdd,Fe II for our sample (red stars) and the comparison samples (blue and green triangles). The dashed line corresponds to a constant bolometric luminosity of 1047.2 erg s−1, the median bolometric luminosity of the GNIRS sample. There is no significant difference between the λEdd,Fe II distributions of our sample and the GNIRS sample.
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. (a) Wr[O III] and (b) RFe II for our objects. There is no clear negative correlation between Γ vs. Wr[O III] or positive correlation between Γ vs. RFe II, probably affected by the limited sample size and the large Γ errors.
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: Comparison of the Hβ-based virial SMBH masses with the Mg II-based virial SMBH masses for eight of the nine quasars; J0223 does not have a Mg II-based virial mass. The error bars represent only measurement uncertainties. The black line represents the line of equality.
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: log Wr[O III] vs. log Wr(C IV) for our sample (red stars), the WLQs from Y. Chen et al. (2024) (purple stars), and the GNIRS non-WLQs (green dots). Upper limits are indicated by downward arrows. WLQs predominantly occupy the bottom-left corner of the diagram.
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. λEdd,Fe II for our sample (red stars) and the super- (gray triangles) and sub-Eddington (light gray triangles) accreting quasars in H. Liu et al. (2021). The best-fit relation from H. Liu et al. (2021) is displayed as the solid line. Our quasars are generally consistent with the expectation from the H. Liu et al. (2021) relation.
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: Histograms showing the distributions of λEdd based on three different estimates of MBH: MBH, MBH,Fe II, and MBH,Mg II.
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-II 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: 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 distribution of the clusters analyzed in this work in the celestial sphere. Gray points correspond to star clusters cataloged in E. Bica et al. (2008). The inset plot shows a composite image of the LMC in optical filters from A. Mellinger (2009). The bottom panel shows the distribution of clusters as a function of their position angles around the center of the galaxy. The colored histogram corresponds to the clusters analyzed in this work. The gray, hashed histogram includes all clusters cataloged in E. Bica et al. (2008), in the vicinity of our sample.
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 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: 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: The redshift evolution of w(z) with its 68% CL region for different DE parameterizations (Padé-I, SPadé-I, Padé-II). In the upper panels we show the evolution of w(z) assuming the flat universe while in the lower panels we show the evolution of w(z) considering the nonflat universe. The left panels correspond to SN+BAO+BBN+H(z) and the right panels correspond to SN+BAO+BBN+H(z)+CMB.
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 panel shows a comparison between PARSEC+COLIBRI isochrones of the same age and metallicity ([Fe/H] = −0.5) that do not include rotation and that do, with an initial angular velocity of 90% of the critical value. The inclination angle refers to the separation between the line of sight and the rotation axis. Therefore, an inclination of 0° (90°) corresponds to a pole-on (equator-on) view of the star. Specific versions of the PARSEC code are the same as those described in the text.
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 panel shows a comparison between the ages, metallicities, distances, color excesses, binary fractions, and average posterior probabilities obtained between the fits performed in this work using nonrotating and rotating (ωi = 0.90ωc) models. The orange line indicates equality between results. For the bottom right panel, values from the fits were subtracted for a better visualization.
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: Color excess obtained from the CMD fitting performed for the clusters in this work with nonrotating (left) and rotating (right) models as a function of those used as priors from the dust maps of D. J. Schlegel et al. (1998). The black dashed line indicates the position where both values are equal.
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: Top panel: Filament 1 inferred B-field vectors overlaid on the Herschel-derived column density map, with contours for this figure and in Appendix A at [0.63, 0.75, 1.3, 1.8, 2.5, 5.0, 7.5] × 1022 cm−2. Bright red and yellow vectors have measurements of Pfrac/﹩{\sigma }_{{P}_{{\rm{frac}}}}﹩ > 3 and 2 ≤ Pfrac/﹩{\sigma }_{{P}_{{\rm{frac}}}}﹩≤ 3, respectively; faded vectors indicate where Pfrac > 0.15. Filled blue and green circles mark known Class I and II YSOs, respectively (Section 2.5). Vectors are spaced by 2 HAWC+ pixels (9﹩\mathop{.}\limits^{^{\prime\prime} }﹩1), near Nyquist sampling. Bottom panel: LIC map overlaid on column density, where the wavy pattern shows the B-field direction for Pfrac/﹩{\sigma }_{{P}_{{\rm{frac}}}}﹩ > 1.5 and I/σI > 10. The spine’s polynomial fit is the solid line. The white beam (top right; 36﹩\mathop{.}\limits^{^{\prime\prime} }﹩4) shows the resolution for the column density map, and the orange beam (bottom right; 18﹩\mathop{.}\limits^{^{\prime\prime} }﹩7) shows the resolution for SOFIA/HAWC+.
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: Ngas vs. ∣θB − θfil∣ for each bone, shown for every other HAWC+ pixel (approximately Nyquist sampled). Only data within 23″ of the bone (two spine pixels) are considered. The data is binned into 10 equal Ngas ranges, and box plots are shown if there are at least four points in the bin. The box plots show the first and third quartiles in black and the median in orange. A red vertical line is shown for the first Ngas box plot bin where ∣θB − θfil∣ > 60°, which indicates the first sign of perpendicularity with Ngas. Filled blue and green circles show the Ngas and ∣θB − θfil∣ values at the nearest pixel for the known Class I and II YSOs, respectively.
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: Sliding box results for each bone, where Bpos, λ, αvir, and ϵ for the sliding box along the spine are shown in color scale, and the gray scale shows the gas column density, Ngas. Color scales for λ is a linear scale, while the others are on a square root scale. A black forward slash “/” through a point indicates that the velocity dispersions are likely overestimated, as they were measured with a low-density tracer (see Section 2.4). Black and white points are locations where we were unable to make estimates (see the text). The box size is shown in each panel, which was allowed to rotate as it slid across the spine. The top right of each panel shows the median for all points and for those using only high-density (HD) tracers. Figure 1 gives the beam sizes, and Figure 1 and the figures in Appendix A quantify the gray scale for each bone.
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: B-field and spine angle difference, ∣θB − θfil∣, shown in color scale for Pfrac/﹩{\sigma }_{{P}_{\,\rm{frac}\,}}\gt 2﹩ for six of the bones (the other four are in Figure 3). Open squares show the spine pixels of the bones, and the gray line shows the polynomial fit to these pixels (Section 2.3). Black vectors have measurements of Pfrac/﹩{\sigma }_{{P}_{{\rm{frac}}}}﹩ > 3, while faded black (gray) vectors have 2 ≤ Pfrac/﹩{\sigma }_{{P}_{{\rm{frac}}}}﹩≤ 3. Filled blue and green circles show the location of known Class I and II YSOs, respectively (Section 2.5). The black beam on the top right is the column density resolution (36﹩\mathop{.}\limits^{^{\prime\prime} }﹩4), while the green beam on the bottom right is the SOFIA resolution (18﹩\mathop{.}\limits^{^{\prime\prime} }﹩7). Vectors are shown are separated by 5 HAWC+ pixels (22﹩\mathop{.}\limits^{^{\prime\prime} }﹩75 or ∼1.25 beams) to help better visualize the B-field morphology.
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: CDF of the angle difference between each bone’s spine and B-field direction, ∣θB − θfil∣. Only pixels within 23″ of the spine are considered. The red line in each panel shows the results for that particular bone. The blue lines in each panel show a Monte Carlo simulation of the expected distribution of projected angles if the spine and B-field directions in 3D are mostly parallel (within 0°–20°; dashed blue line), mostly perpendicular (within 70°–90°; dashed–dotted blue line), or random (solid blue line). The cyan lines show the expected projected angles if the bone is fixed in the plane of the sky for mostly parallel (dashed cyan line) and mostly perpendicular (dashed–dotted cyan line).
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: B-field and spine angle difference, ∣θB − θfil∣, for four of the bones. The caption is the same as that of Figure 2, which shows the other six of the 10 bones.
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 Figures 15 (left), 16 (center), and 17 (right), 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: Same as Figure 14, for the results obtained using models that include rotation.
Paper: The SDSS-V Black Hole Mapper Reverberation Mapping Project: Light Echoes of the Coronal-line Region in a Luminous Quasar
Authors: Theodore B. Smith, Logan B. Fries, Jonathan R. Trump, Catherine J. Grier, Yue Shen, Scott F. Anderson, W. N. Brandt, Megan C. Davis, Tom Dwelly, P. B. Hall, Keith Horne, Y. Homayouni, J. McKaig, Sean Morrison, Hugh W. Sharp, Roberto J. Assef, Franz E. Bauer, Anton M. Koekemoer, Donald P. Schneider, Benny Trakhtenbrot, Hector Javier Ibarra-Medel, Castalia Alenka Negrete Peñaloza
Figure caption: Gaussian fit parameters of the [O III] λ5007 emission line in COS168 (line flux, line center, and line width) as well as the median over all epochs for each parameter (black line) and the normalized median absolute deviation (gray areas). The line center and line width are stable, so we use line flux as a flux calibrator.
Paper: The SDSS-V Black Hole Mapper Reverberation Mapping Project: Light Echoes of the Coronal-line Region in a Luminous Quasar
Authors: Theodore B. Smith, Logan B. Fries, Jonathan R. Trump, Catherine J. Grier, Yue Shen, Scott F. Anderson, W. N. Brandt, Megan C. Davis, Tom Dwelly, P. B. Hall, Keith Horne, Y. Homayouni, J. McKaig, Sean Morrison, Hugh W. Sharp, Roberto J. Assef, Franz E. Bauer, Anton M. Koekemoer, Donald P. Schneider, Benny Trakhtenbrot, Hector Javier Ibarra-Medel, Castalia Alenka Negrete Peñaloza
Figure caption: Median (top) and rms flux (bottom) spectra for COS168. The left panels show the full wavelength range of the SDSS-V spectra, and the right panels show the region around the [Ne V] λ3427 line. The full rms spectrum is boxcar smoothed by 13 pixels.
Paper: Measuring Dust Masses of Protoplanetary Disks in Serpens and L1641/L1647 with ALMA
Authors: Luisa F. Zamudio-Ruvalcaba, Catherine C. Espaillat, Álvaro Ribas, Enrique Macías
Figure caption: Posterior distributions of the 160 individual successfully modeled sources of the L1641/L1647 sample (top panels) and ensemble distribution (bottom panels) for the following parameters (from top left to bottom right): α (disk viscosity), ﹩\dot{M}﹩ (mass accretion rate), Rdisk (outer disk radius), ϵ (dust settling), amax,midplane (maximum grain size in the midplane), and amax,upper (maximum grain size in the upper layers of the disk). The error bars denote the 16th and 84th percentiles; the bottom panels’ histograms use 20 bins. Posterior distributions of the 160 individual successfully modeled sources of the L1641/L1647 sample (top panels) and ensemble distribution (bottom panels) for the following parameters (from left to right): Mdisk/M* (disk mass fraction to host star mass) and M* (host star mass).
Paper: Measuring Dust Masses of Protoplanetary Disks in Serpens and L1641/L1647 with ALMA
Authors: Luisa F. Zamudio-Ruvalcaba, Catherine C. Espaillat, Álvaro Ribas, Enrique Macías
Figure caption: Posterior distributions of the 18 individual successfully modeled sources of the Serpens sample (top panels) and ensemble distribution (bottom panels) for the following parameters (from top left to bottom right): α (disk viscosity), ﹩\dot{M}﹩ (mass accretion rate), Rdisk (outer disk radius), ϵ (dust settling), amax,midplane (maximum grain size in the midplane), and amax,upper (maximum grain size in the upper layers of the disk). The error bars denote the 16th and 84th percentiles; the bottom panels’ histograms use 20 bins. Posterior distributions of the 18 individual successfully modeled sources of the Serpens sample (top panels) and ensemble distribution (bottom panels) for the following parameters (from left to right): Mdisk/M* (disk mass fraction to host star mass) and M* (host star mass).
Paper: Measuring Dust Masses of Protoplanetary Disks in Serpens and L1641/L1647 with ALMA
Authors: Luisa F. Zamudio-Ruvalcaba, Catherine C. Espaillat, Álvaro Ribas, Enrique Macías
Figure caption: Comparison of this work’s Mdust calculated from SED modeling and Mdust derived from millimeter fluxes from the literature. Serpens (A. R. Anderson et al. 2022) and L1641/L1647 (S. E. van Terwisga et al. 2022) data correspond to this work, while data for the remaining 10 star-forming regions are gathered from A. M. Rilinger et al. (2023), where the same methodology was applied to calculate the masses. The solid orange line displays the linear fit to the recalculated dust masses, assuming a constant dust temperature of 20 K. The black dashed line denotes a one-to-one relation.
Paper: Measuring Dust Masses of Protoplanetary Disks in Serpens and L1641/L1647 with ALMA
Authors: Luisa F. Zamudio-Ruvalcaba, Catherine C. Espaillat, Álvaro Ribas, Enrique Macías
Figure caption: Comparison of this work’s disk dust masses calculated from SED modeling and disk dust masses derived from millimeter fluxes from the literature. The left panel corresponds to the Serpens sample (A. R. Anderson et al. 2022), and the right panel corresponds to the L1641/L1647 sample (S. E. van Terwisga et al. 2022; A. M. Rilinger et al. 2023). Both panels show a one-to-one relation (dotted black line) and a linear fit (solid orange line) that assumes a constant dust temperature of 20 K. The corresponding equation is noted for each linear fit.