adsabs/AstroCLIMB huggingface dataset:
Paper: TESS Spots a Super-puff: The Remarkably Low Density of TOI-1420b
Authors: Stephanie Yoshida, Shreyas Vissapragada, David W. Latham, Allyson Bieryla, Daniel P. Thorngren, Jason D. Eastman, Mercedes López-Morales, Khalid Barkaoui, Charles Beichman, Perry Berlind, Lars A. Buchave, Michael L. Calkins, David R. Ciardi, Karen A. Collins, Rosario Cosentino, Ian J. M. Crossfield, Fei Dai, Victoria DiTomasso, Nicholas Dowling, Gilbert A. Esquerdo, Raquel Forés-Toribio, Adriano Ghedina, Maria V. Goliguzova, Eli Golub, Erica J. Gonzales, Ferran Grau Horta, Jesus Higuera, Nora Hoch, Keith Horne, Steve B. Howell, Jon M. Jenkins, Jessica Klusmeyer, Didier Laloum, Jack J. Lissauer, Sarah E. Logsdon, Luca Malavolta, Rachel A. Matson, Elisabeth C. Matthews, Kim K. McLeod, Jennifer V. Medina, Jose A. Muñoz, Hugh P. Osborn, Boris Safonov, Joshua Schlieder, Michael Schmidt, Heidi Schweiker, Sara Seager, Alessandro Sozzetti, Gregor Srdoc, Guđmundur Stefánsson, Ivan A. Strakhov, Stephanie Striegel, Joel Villaseñor, Joshua N. Winn
Figure caption: Phase-folded light curve of TESS transits (left) and phase-folded HARPS-N and NEID RVs of TOI-1420 (right) with residuals. The black data points are the observations and the red lines are the overlaying best-fit models from ExoFASTv2.
Paper: TESS Spots a Super-puff: The Remarkably Low Density of TOI-1420b
Authors: Stephanie Yoshida, Shreyas Vissapragada, David W. Latham, Allyson Bieryla, Daniel P. Thorngren, Jason D. Eastman, Mercedes López-Morales, Khalid Barkaoui, Charles Beichman, Perry Berlind, Lars A. Buchave, Michael L. Calkins, David R. Ciardi, Karen A. Collins, Rosario Cosentino, Ian J. M. Crossfield, Fei Dai, Victoria DiTomasso, Nicholas Dowling, Gilbert A. Esquerdo, Raquel Forés-Toribio, Adriano Ghedina, Maria V. Goliguzova, Eli Golub, Erica J. Gonzales, Ferran Grau Horta, Jesus Higuera, Nora Hoch, Keith Horne, Steve B. Howell, Jon M. Jenkins, Jessica Klusmeyer, Didier Laloum, Jack J. Lissauer, Sarah E. Logsdon, Luca Malavolta, Rachel A. Matson, Elisabeth C. Matthews, Kim K. McLeod, Jennifer V. Medina, Jose A. Muñoz, Hugh P. Osborn, Boris Safonov, Joshua Schlieder, Michael Schmidt, Heidi Schweiker, Sara Seager, Alessandro Sozzetti, Gregor Srdoc, Guđmundur Stefánsson, Ivan A. Strakhov, Stephanie Striegel, Joel Villaseñor, Joshua N. Winn
Figure caption: Posterior distributions on the planetary mass, bulk metallicity, and age from the planet evolution model described in the text.
Paper: TESS Spots a Super-puff: The Remarkably Low Density of TOI-1420b
Authors: Stephanie Yoshida, Shreyas Vissapragada, David W. Latham, Allyson Bieryla, Daniel P. Thorngren, Jason D. Eastman, Mercedes López-Morales, Khalid Barkaoui, Charles Beichman, Perry Berlind, Lars A. Buchave, Michael L. Calkins, David R. Ciardi, Karen A. Collins, Rosario Cosentino, Ian J. M. Crossfield, Fei Dai, Victoria DiTomasso, Nicholas Dowling, Gilbert A. Esquerdo, Raquel Forés-Toribio, Adriano Ghedina, Maria V. Goliguzova, Eli Golub, Erica J. Gonzales, Ferran Grau Horta, Jesus Higuera, Nora Hoch, Keith Horne, Steve B. Howell, Jon M. Jenkins, Jessica Klusmeyer, Didier Laloum, Jack J. Lissauer, Sarah E. Logsdon, Luca Malavolta, Rachel A. Matson, Elisabeth C. Matthews, Kim K. McLeod, Jennifer V. Medina, Jose A. Muñoz, Hugh P. Osborn, Boris Safonov, Joshua Schlieder, Michael Schmidt, Heidi Schweiker, Sara Seager, Alessandro Sozzetti, Gregor Srdoc, Guđmundur Stefánsson, Ivan A. Strakhov, Stephanie Striegel, Joel Villaseñor, Joshua N. Winn
Figure caption: TESS 2 minutes cadence PDCSAP light curves for TOI-1420. Transit events are visible roughly every 7 days.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Observational Properties and Chemical Abundance Ratio between CO and its Isotopologues
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qing-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption:                    ﹩{N}_{{}^{13}\mathrm{CO}}﹩ vs. ﹩{X}_{{}^{13}\mathrm{CO}}/{X}_{{{\rm{C}}}^{18}{\rm{O}}}﹩ pixel by pixel measured in 32 clouds. The color coding shows the excitation temperature derived from the 12CO peak intensity. The two dashed lines show the mean threshold of C18O 7.0 × 1014 cm−2 and the terrestrial ratio ﹩{X}_{{}^{13}\mathrm{CO}}/{X}_{{{\rm{C}}}^{18}{\rm{O}}}﹩ 5.5 (Wilson & Matteucci 1992), respectively. The two red rectangles present two typical distribution regions of the Type I and Type II clouds classified in Wang et al. (2019). The gray lines show the error bar for each pixel.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Observational Properties and Chemical Abundance Ratio between CO and its Isotopologues
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qing-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: Left: flux (12CO) vs. flux (13CO) measured cloud by cloud in the 1197-cloud catalog. The flux (12CO) and flux (13CO) are calculated toward the same areas, where both 12CO and 13CO emissions are detected. Right: flux (13CO) vs. flux (C18O) measured in the 32-cloud catalog. The flux (13CO) and flux (C18O) are calculated toward the same areas, where both 13CO and C18O emissions are detected. The colors indicate different types of MCs, based on excitation temperature.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Observational Properties and Chemical Abundance Ratio between CO and its Isotopologues
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qing-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption:  12CO area vs. 13CO area cloud by cloud, measured in the 1197-cloud catalog. The color coding is the same as in Figure 1. The red line represents a linear fit with a ratio of 0.38. The fitting is calculated by utilizing the OLS function in the Python package Statsmodels (https://www.statsmodels.org/dev/generated/statsmodels.regression.linear_model.OLS.html), assuming a zero intercept and no weighting. The dashed black line is the limit with a ratio of 0.7 proposed by Yuan et al. (2022).
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Observational Properties and Chemical Abundance Ratio between CO and its Isotopologues
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qing-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: Peak intensity distribution and peak intensity ratio pixel by pixel measured in the 12CO, 13CO, and C18O catalog. The color coding represents the distribution of the probability density functions of the pixels with 13CO emission (2D probability density functions), which are calculated by utilizing kernel density estimation through Gaussian kernels in the Python package scipy.stats.Gaussian_kde (https://docs.scipy.org/doc/scipy/reference/generated/scipy.stats.Gaussian_kde.html).
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Observational Properties and Chemical Abundance Ratio between CO and its Isotopologues
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qing-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption:                    ﹩{N}_{{}^{13}\mathrm{CO}}﹩ vs. ﹩{N}_{{{\rm{C}}}^{18}{\rm{O}}}﹩ pixel by pixel measured in 32 clouds. The color coding shows the excitation temperature derived from the 12CO peak intensity. The two dashed lines show the mean threshold of the integrated intensity noise, which corresponds to ﹩{N}_{{}^{13}\mathrm{CO}}﹩ and ﹩{N}_{{{\rm{C}}}^{18}{\rm{O}}}﹩ of 4.5 × 1015 cm−2 and 7.0 × 1014 cm−2, respectively. The gray lines show the error bar for each pixel.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Observational Properties and Chemical Abundance Ratio between CO and its Isotopologues
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qing-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: Intensity distribution between 12CO, 13CO, and C18O, pixel by pixel. The color coding is the same as in Figure 1.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Observational Properties and Chemical Abundance Ratio between CO and its Isotopologues
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qing-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: Optical depth τ vs. velocity-integrated intensity I, pixel by pixel, measured in the 12CO, 13CO, and C18O catalog. The color coding is the same as in Figure 1.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Observational Properties and Chemical Abundance Ratio between CO and its Isotopologues
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qing-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: Left: flux (12CO) vs. flux (13CO) measured cloud by cloud in the 1197-cloud catalog. The flux (12CO) and flux (13CO) are calculated toward the entire cloud. Right: flux (13CO) vs. flux (C18O) measured in the 32-cloud catalog. The flux (13CO) and flux (C18O) are calculated toward the entire cloud. The colors indicate different types of MCs, based on excitation temperature. The dashed line shows the result of a weighted linear fit to the data.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Observational Properties and Chemical Abundance Ratio between CO and its Isotopologues
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qing-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: The ratio of ﹩{N}_{{}^{18}}^{\mathrm{LTE}}﹩/﹩{N}_{{}^{18}}^{\mathrm{corrected}}﹩ vs. ﹩{T}_{\mathrm{ex}}^{12}﹩. ﹩{N}_{{}^{18}}^{\mathrm{LTE}}﹩ is the 18CO column density under the LTE assumption, while ﹩{N}_{{}^{18}}^{\mathrm{corrected}}﹩ is the corrected 18CO column density based on the corrected 18CO excitation temperature and correlation T ex(13CO)/T ex(C18O) = 1.3. ﹩{T}_{\mathrm{ex}}^{12}﹩ is the excitation temperature from the 12CO spectrum under the LTE assumption. The color shows the intensity of 18CO.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Observational Properties and Chemical Abundance Ratio between CO and its Isotopologues
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qing-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: The ratio of ﹩{N}_{{}^{13}}^{\mathrm{LTE}}﹩/﹩{N}_{{}^{13}}^{\mathrm{corrected}}﹩ vs. ﹩{T}_{\mathrm{ex}}^{12}﹩. ﹩{N}_{{}^{13}}^{\mathrm{LTE}}﹩ is the 13CO column density under the LTE assumption, while ﹩{N}_{{}^{13}}^{\mathrm{corrected}}﹩ is the corrected 13CO column density, based on the corrected 13CO excitation temperature and the correlation T ex(12CO)/T ex(13CO) = 1.7. ﹩{T}_{\mathrm{ex}}^{12}﹩ is the excitation temperature from the 12CO spectrum under the LTE assumption. The color shows the intensity of 13CO.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Observational Properties and Chemical Abundance Ratio between CO and its Isotopologues
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qing-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption:  12CO flux ﹩{F}_{12}^{\mathrm{tot}}﹩ vs. flux proportion of the 12CO-only region in the 1197-cloud catalog. ﹩{F}_{12}^{\mathrm{tot}}﹩ is calculated toward the entire cloud.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Observational Properties and Chemical Abundance Ratio between CO and its Isotopologues
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qing-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: Histogram distribution of the filling factors η and sensitivity clip factors ξ for 12CO, 13CO, and C18O in the cloud catalog.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Observational Properties and Chemical Abundance Ratio between CO and its Isotopologues
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qing-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption:  η-corrected ﹩{N}_{{}^{13}\mathrm{CO}}﹩ vs. ﹩{X}_{{}^{13}\mathrm{CO}}/{X}_{{{\rm{C}}}^{18}{\rm{O}}}﹩ pixel by pixel measured in 32 clouds. All the symbols and colors are same as in Figure 7, except the values of ﹩{N}_{{}^{13}\mathrm{CO}}﹩ and ﹩{X}_{{}^{13}\mathrm{CO}}/{X}_{{{\rm{C}}}^{18}{\rm{O}}}﹩ are corrected by the fill factor η.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Observational Properties and Chemical Abundance Ratio between CO and its Isotopologues
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qing-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: Left: corrected flux (12CO) vs. flux (13CO) cloud by cloud. Right: corrected flux (13CO) vs. flux (C18O) cloud by cloud. Different than Figure 5, the flux here is corrected based on the sensitivity clip factor ξ. The colors indicate different types of MCs, based on excitation temperature.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Observational Properties and Chemical Abundance Ratio between CO and its Isotopologues
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qing-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: Histogram distribution of the column density of 13CO and C18O under the LTE assumption with or without the filling factor η being corrected.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Observational Properties and Chemical Abundance Ratio between CO and its Isotopologues
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qing-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: The histogram of the intensity-weighted average excitation temperatures from 12CO data.
Paper: SPar: Estimating Stellar Parameters from Multiband Photometries with Empirical Stellar Libraries
Authors: Mingxu Sun, Bingqiu Chen, Helong Guo, He Zhao, Ming Yang, Wenyuan Cui
Figure caption: Left panel: Gaia observed color–magnitude diagram. Middle panel: Gaia dereddened color–magnitude diagram. Right panel: Gaia HR diagram.
Paper: SPar: Estimating Stellar Parameters from Multiband Photometries with Empirical Stellar Libraries
Authors: Mingxu Sun, Bingqiu Chen, Helong Guo, He Zhao, Ming Yang, Wenyuan Cui
Figure caption: The HRDs plotted with our final sample stars (left) and the resultant gridded stellar library (right). The color scales represent the mean metallicities of each T eff − M  G  bin.
Paper: Iron-rich Metal-poor Stars and the Astrophysics of Thermonuclear Events Observationally Classified as Type Ia Supernovae. I. Establishing the Connection
Authors: Henrique Reggiani, Kevin C. Schlaufman, Andrew R. Casey
Figure caption: Abundances of the light odd-Z elements sodium, aluminum, and scandium. We plot as dark-blue stars the three IRMP stars in our sample. We plot as black-bordered light-green squares inner-halo metal-poor stars from Reggiani et al. (2017) and H. R. Reggiani et al. (2023, in preparation); as dark-gray triangles, squares, and circles thick-disk, low-α, and high-α stars from Nissen & Schuster (2010), respectively; as black-bordered light-blue triangles stars from the dSph galaxies Carina, Fornax, Sagittarius, and Sculptor (Shetrone et al. 2003; Geisler et al. 2005; Monaco et al. 2005; Letarte et al. 2010; Hill et al. 2019; Skúladóttir et al. 2019); and as dark-green pentagons outer-halo metal-poor stars from Cayrel et al. (2004) and Jacobson et al. (2015). By construction, our three IRMP stars have low [Na/Fe] abundances. Consistent with the implications of subsolar [Ti/Fe] abundances, subsolar [Sc/Fe] abundances generally disfavor double detonations in thick helium envelopes.
Paper: Iron-rich Metal-poor Stars and the Astrophysics of Thermonuclear Events Observationally Classified as Type Ia Supernovae. I. Establishing the Connection
Authors: Henrique Reggiani, Kevin C. Schlaufman, Andrew R. Casey
Figure caption: Abundances of the neutron-capture elements strontium, yttrium, barium, and europium. We plot as black-bordered light-green squares inner-halo metal-poor stars from Reggiani et al. (2017) and H. R. Reggiani et al. (2023, in preparation); as dark-gray triangles, squares, and circles thick-disk, low-α, and high-α stars from Nissen & Schuster (2010), respectively; as black-bordered light-blue triangles stars from the dSph galaxies Carina, Fornax, Sagittarius, and Sculptor (Shetrone et al. 2003; Geisler et al. 2005; Monaco et al. 2005; Letarte et al. 2010; Hill et al. 2019; Skúladóttir et al. 2019); and as dark-green pentagons outer-halo metal-poor stars from Cayrel et al. (2004) and Jacobson et al. (2015). As essentially no neutron-capture elements are synthesized in thermonuclear explosions, the low neutron-capture abundances relative to iron we infer support the idea that the iron-peak elements in IRMP stars were mostly synthesized in thermonuclear events without the additional neutron-capture elements expected under more typical chemical evolution scenarios.
Paper: Iron-rich Metal-poor Stars and the Astrophysics of Thermonuclear Events Observationally Classified as Type Ia Supernovae. I. Establishing the Connection
Authors: Henrique Reggiani, Kevin C. Schlaufman, Andrew R. Casey
Figure caption: Abundances of titanium and the α-elements magnesium, silicon, and calcium. We plot as dark-blue stars the three IRMP stars in our sample. We plot as black-bordered light-green squares inner-halo metal-poor stars from Reggiani et al. (2017) and H. R. Reggiani et al. (2023, in preparation); as dark-gray triangles, squares, and circles thick-disk, low-α, and high-α stars from Nissen & Schuster (2010), respectively; as black-bordered light-blue triangles stars from the dSph galaxies Carina, Fornax, Sagittarius, and Sculptor (Shetrone et al. 2003; Geisler et al. 2005; Monaco et al. 2005; Letarte et al. 2010; Hill et al. 2019; Skúladóttir et al. 2019); and as dark-green pentagons outer-halo metal-poor stars from Cayrel et al. (2004) and Jacobson et al. (2015). By construction, our three IRMP stars have low [Mg/Fe] abundances. Their low [Ca/Fe] and [Ti/Fe] abundances generally disfavor spot- or belt-like double detonations with either especially thin or especially thick helium envelopes. Direct white dwarf collisions are also disfavored.
Paper: Iron-rich Metal-poor Stars and the Astrophysics of Thermonuclear Events Observationally Classified as Type Ia Supernovae. I. Establishing the Connection
Authors: Henrique Reggiani, Kevin C. Schlaufman, Andrew R. Casey
Figure caption: Abundances of the iron-peak elements chromium, manganese, cobalt, nickel, and zinc. We plot as dark-blue stars the three IRMP stars in our sample. We plot as dark-blue stars the three IRMP stars in our sample. We plot as black-bordered light-green squares inner-halo metal-poor stars from Reggiani et al. (2017) and H. R. Reggiani et al. (2023, in preparation); as dark-gray triangles, squares, and circles thick-disk, low-α, and high-α stars from Nissen & Schuster (2010), respectively; as black-bordered light-blue triangles stars from the dSph galaxies Carina, Fornax, Sagittarius, and Sculptor (Shetrone et al. 2003; Geisler et al. 2005; Monaco et al. 2005; Letarte et al. 2010; Hill et al. 2019; Skúladóttir et al. 2019); and as dark-green pentagons outer-halo metal-poor stars from Cayrel et al. (2004) and Jacobson et al. (2015). By construction, our three IRMP stars have low [Co/Fe]. The high [Mn/Fe] abundances we infer support the idea that the iron-peak elements in IRMP stars were mostly synthesized in thermonuclear supernovae.
Paper: Iron-rich Metal-poor Stars and the Astrophysics of Thermonuclear Events Observationally Classified as Type Ia Supernovae. I. Establishing the Connection
Authors: Henrique Reggiani, Kevin C. Schlaufman, Andrew R. Casey
Figure caption: Observed elemental abundances and predicted thermonuclear event yields from models that best fit the observed data. We plot as blue circles our observed elemental abundances and as black-bordered white squares connected by solid black lines the theoretical yields predicted by the model that best reproduces our observations. The best model in each panel is depicted as black open squares, and the inferred stellar abundances are shown as blue circles. The abundances of BD +80°245 and HE 0533–5340 are best fit by Bravo et al. (2019) models for the detonation of sub-Chandrasekhar-mass CO white dwarfs with M WD = 1.1 M ⊙, a standard C/O ratio, and metallicities of Z = 9 × 10−3 and Z = 2.25 × 10−3, respectively. The abundances of SMSS J034249.53–284216.0 are best fit by the Leung & Nomoto (2020a) sub-Chandrasekhar-mass double-detonation model 110-050-2-S50.
Paper: A Comparison of the Composition of Planets in Single-planet and Multiplanet Systems Orbiting M dwarfs
Authors: Romy Rodríguez Martínez, David V. Martin, B. Scott Gaudi, Joseph G. Schulze, Anusha Pai Asnodkar, Kiersten M. Boley, Sarah Ballard
Figure caption: Left: Histograms of the bulk densities of planets in single-planet systems (blue), and multiplanet systems (red) for our entire sample of planets (top) and for planets with R  p  < 6 R ⊕ (bottom). The red dashed line shows the median density of the multis while the blue dashed line shows the median density of the singles. Right: Bootstrapped empirical cumulative distribution functions (CDF) for our entire sample of planets (top) and for planets with R  p  < 6 R ⊕ (bottom). The Kolmogorov–Smirnov statistic values, or p values, of the original distributions are overplotted. f threshold is explained in Section 4.3. We note that removal of the dense outliers at ∼12 g cm−3 and ∼18 g cm−3 does not considerably affect the observed differences in the density distributions.
Paper: A Comparison of the Composition of Planets in Single-planet and Multiplanet Systems Orbiting M dwarfs
Authors: Romy Rodríguez Martínez, David V. Martin, B. Scott Gaudi, Joseph G. Schulze, Anusha Pai Asnodkar, Kiersten M. Boley, Sarah Ballard
Figure caption: Representation of the interior structure and core/water mass fractions of planets with M  p  < 10 M ⊕. The gray circles are the liquid iron cores and the blue and orange circles represent water and rocky layers, respectively. The relative sizes of the circles are proportional to the planet/core/water masses. The numbers above each planet are the derived water/core mass fractions. The systems are sorted by planet multiplicity from low (top) to high (bottom) multiplicity.
Paper: A Comparison of the Composition of Planets in Single-planet and Multiplanet Systems Orbiting M dwarfs
Authors: Romy Rodríguez Martínez, David V. Martin, B. Scott Gaudi, Joseph G. Schulze, Anusha Pai Asnodkar, Kiersten M. Boley, Sarah Ballard
Figure caption: Orbital architectures of representative planetary systems in our sample. The x-axis shows the orbital periods. The symbol sizes are proportional to the planets’ radii, and they are color coded by planet mass. The circles are planets with masses determined from radial velocity measurements while the triangles represent planets with masses from transit timing variations (TTV). All of them are transiting exoplanets. They are sorted by planet multiplicity from top to bottom, with systems with a higher number of planets at the top.
Paper: A Comparison of the Composition of Planets in Single-planet and Multiplanet Systems Orbiting M dwarfs
Authors: Romy Rodríguez Martínez, David V. Martin, B. Scott Gaudi, Joseph G. Schulze, Anusha Pai Asnodkar, Kiersten M. Boley, Sarah Ballard
Figure caption: Left: Histograms of the bulk density normalized by the density that an Earth-like planet (i.e., a rocky planet with ∼0.32 core mass fraction) would have at that mass. Single planets are shown in blue and multis in red; all planets have R  p  < 6 R ⊕. Right: bootstrapped cumulative distributions; f threshold is explained in Section 4.3.
Paper: A Comparison of the Composition of Planets in Single-planet and Multiplanet Systems Orbiting M dwarfs
Authors: Romy Rodríguez Martínez, David V. Martin, B. Scott Gaudi, Joseph G. Schulze, Anusha Pai Asnodkar, Kiersten M. Boley, Sarah Ballard
Figure caption: Mass–radius diagram of the planets in our sample with R  p  < 6 R ⊕. The colored lines represent mass–radius composition curves from Zeng et al. (2019). Earth and Venus are also plotted for reference. The circles represent planets in multiplanet systems and the squares are singles. The majority of planets above the 100% water line are single.