adsabs/AstroCLIMB huggingface dataset:
Paper: Systematic KMTNet Planetary Anomaly Search. IX. Complete Sample of 2016 Prime-field Planets
Authors: In-Gu Shin, Jennifer C. Yee, Weicheng Zang, Hongjing Yang, Kyu-Ha Hwang, Cheongho Han, Andrew Gould, Andrzej Udalski, Ian A. Bond, Michael D. Albrow, Sun-Ju Chung, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof A. Rybicki, Patryk Iwanek, Krzysztof Ulaczyk, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Light curve of KMT-2016-BLG-1751 with degenerate models.
Paper: Systematic KMTNet Planetary Anomaly Search. IX. Complete Sample of 2016 Prime-field Planets
Authors: In-Gu Shin, Jennifer C. Yee, Weicheng Zang, Hongjing Yang, Kyu-Ha Hwang, Cheongho Han, Andrew Gould, Andrzej Udalski, Ian A. Bond, Michael D. Albrow, Sun-Ju Chung, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof A. Rybicki, Patryk Iwanek, Krzysztof Ulaczyk, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: The APRX distributions of OGLE-2016-BLG-1850.
Paper: Visual Orbits and Alignments of Planet-hosting Binary Systems
Authors: Kathryn V. Lester, Steve B. Howell, Rachel A. Matson, Elise Furlan, Crystal L. Gnilka, Colin Littlefield, David R. Ciardi, Mark E. Everett, Sergio B. Fajardo-Acosta, Catherine A. Clark
Figure caption: Critical semimajor axis (a crit) vs. planet semimajor axis (a  pl ) for the planet candidates in our sample. Holman & Wiegert (1999) predict that planets with a crit > a  pl  would be dynamically stable in binary systems. All systems in our sample lie above the 1:1 line (dotted) and therefore are expected to be dynamically stable, though two planets (labeled) are close to their critical separation.
Paper: Visual Orbits and Alignments of Planet-hosting Binary Systems
Authors: Kathryn V. Lester, Steve B. Howell, Rachel A. Matson, Elise Furlan, Crystal L. Gnilka, Colin Littlefield, David R. Ciardi, Mark E. Everett, Sergio B. Fajardo-Acosta, Catherine A. Clark
Figure caption: Example visual orbit for the planet-hosting binary KOI 1961. The primary star is positioned at the origin (black cross), and the relative positions of the secondary component are marked with colored points. A random subset of the orbital solutions from orbitize! are shown in gray.
Paper: Visual Orbits and Alignments of Planet-hosting Binary Systems
Authors: Kathryn V. Lester, Steve B. Howell, Rachel A. Matson, Elise Furlan, Crystal L. Gnilka, Colin Littlefield, David R. Ciardi, Mark E. Everett, Sergio B. Fajardo-Acosta, Catherine A. Clark
Figure caption: Alignment between the planetary and binary orbital inclinations (﹩\sin | 90-i| ﹩). A random inclination distribution would result in uniform histograms, but instead our binary host star orbits are often well aligned with the planets’ orbits. This is consistent with numerical simulations of planet formation, which found it more difficult to form planets in protoplanetary disks with a highly misaligned stellar companion (Quintana et al. 2002).
Paper: Visual Orbits and Alignments of Planet-hosting Binary Systems
Authors: Kathryn V. Lester, Steve B. Howell, Rachel A. Matson, Elise Furlan, Crystal L. Gnilka, Colin Littlefield, David R. Ciardi, Mark E. Everett, Sergio B. Fajardo-Acosta, Catherine A. Clark
Figure caption: Example corner plot of the orbital solution for KOI 1961. The diagonal frames show posterior histograms for each orbital parameter, and the off-diagonal frames show the covariance between different pairs of parameters.
Paper: Visual Orbits and Alignments of Planet-hosting Binary Systems
Authors: Kathryn V. Lester, Steve B. Howell, Rachel A. Matson, Elise Furlan, Crystal L. Gnilka, Colin Littlefield, David R. Ciardi, Mark E. Everett, Sergio B. Fajardo-Acosta, Catherine A. Clark
Figure caption: Left: visual orbit solutions for KOI 270. The primary star is positioned at the origin (black cross), and the relative positions of the secondary component are marked with colored points. A random subset of the accepted orbital solutions from orbitize! are shown in gray. The green arrow shows the Gaia proper motion of the primary star (in a single year), which is inconsistent with the observed motion of the secondary. Right: the observed changes in position angle and relative separation over time, plotted against the possible orbital solutions.
Paper: Visual Orbits and Alignments of Planet-hosting Binary Systems
Authors: Kathryn V. Lester, Steve B. Howell, Rachel A. Matson, Elise Furlan, Crystal L. Gnilka, Colin Littlefield, David R. Ciardi, Mark E. Everett, Sergio B. Fajardo-Acosta, Catherine A. Clark
Figure caption: Left: visual orbit solutions for KOI 2124. The primary star is positioned at the origin (black cross), and the relative positions of the secondary component are marked with colored points. A random subset of the accepted orbital solutions from orbitize! are shown in gray. The green arrow shows the Gaia proper motion of the primary star (in a single year), which is inconsistent with the observed motion of the secondary. Right: the observed changes in position angle and relative separation over time, plotted against the possible orbital solutions.
Paper: Visual Orbits and Alignments of Planet-hosting Binary Systems
Authors: Kathryn V. Lester, Steve B. Howell, Rachel A. Matson, Elise Furlan, Crystal L. Gnilka, Colin Littlefield, David R. Ciardi, Mark E. Everett, Sergio B. Fajardo-Acosta, Catherine A. Clark
Figure caption: Left: visual orbit solutions for KOI 1961. The primary star is positioned at the origin (black cross), and the relative positions of the secondary component are marked with colored points. A random subset of the accepted orbital solutions from orbitize! are shown in gray. The green arrow shows the Gaia proper motion of the primary star (in a single year), which is inconsistent with the observed motion of the secondary. Right: the observed changes in position angle and relative separation over time, plotted against the possible orbital solutions.
Paper: Visual Orbits and Alignments of Planet-hosting Binary Systems
Authors: Kathryn V. Lester, Steve B. Howell, Rachel A. Matson, Elise Furlan, Crystal L. Gnilka, Colin Littlefield, David R. Ciardi, Mark E. Everett, Sergio B. Fajardo-Acosta, Catherine A. Clark
Figure caption: Left: visual orbit solutions for KOI 1613. The primary star is positioned at the origin (black cross), and the relative positions of the secondary component are marked with colored points. A random subset of the accepted orbital solutions from orbitize! are shown in gray. The green arrow shows the Gaia proper motion of the primary star (in a single year), which is inconsistent with the observed motion of the secondary. Right: the observed changes in position angle and relative separation over time, plotted against the possible orbital solutions.
Paper: Visual Orbits and Alignments of Planet-hosting Binary Systems
Authors: Kathryn V. Lester, Steve B. Howell, Rachel A. Matson, Elise Furlan, Crystal L. Gnilka, Colin Littlefield, David R. Ciardi, Mark E. Everett, Sergio B. Fajardo-Acosta, Catherine A. Clark
Figure caption: Left: visual orbit solutions for KOI 307. The primary star is positioned at the origin (black cross), and the relative positions of the secondary component are marked with colored points. A random subset of the accepted orbital solutions from orbitize! are shown in gray. The green arrow shows the Gaia proper motion of the primary star (in a single year), which is inconsistent with the observed motion of the secondary. Right: the observed changes in position angle and relative separation over time, plotted against the possible orbital solutions.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: Evolution of mass-less test particles (i.e., exomoons) around TOI-199 b, under gravitational perturbation of the outer planet. Shown are the position of TOI-199 b (blue dot), the planetary Roche limit (gray dashed line), and the planetary 0.5 R Hill (blue dashed line), which scales with (1 – e  b ) due to the dynamical perturbations of TOI-199 c.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: Corner plot of the posterior distributions of the instrumental RV parameters for the joint modeling of the TESS and ASTEP TTVs, and the HARPS, FEROS, CHIRON, and CORALIE RVs. The distributions are explored using nested sampling. The red crosses indicate the median values, and the black contour lines the 1σ, 2σ, and 3σ confidence levels. Subindex H refers to HARPS, F to FEROS, CH to CHIRON, and CO to CORALIE.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: Corner plot of the posterior distributions of the derived planet parameters for the joint modeling of the TESS and ASTEP TTVs, and the HARPS, FEROS, CHIRON, and CORALIE RVs. The distributions are explored using nested sampling. The red crosses indicate the median values, and the black contour lines the 1σ, 2σ, and 3σ confidence levels.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: Same as in Figure D1, but for TOI-199 c.
Paper: A Solution to Continuous RFI in Narrowband Radio SETI with FAST: The MultiBeam Point-source Scanning Strategy
Authors: Bo-Lun Huang, Zhen-Zhao Tao, Tong-Jie Zhang
Figure caption: (a) The relative positions for the 19 beams of FAST with rotation angle = 0° at the starting point of the MBPS observation are shown with gray circles. Beam 1 is placed at the origin, and the five yellow shaded beams are the OTBs, where the diameter of each circle is the HPBW of each beam. The positions of the blue circles represent the relative coordinates when MBPS observation ends. The star represents the position of the target, which is placed at (17.22, 0) relative to beam 1. The cyan arrow indicates the direction of the telescope slew. (b) A zoom-in plot of (a) around the target. The lengths of the red, green, and orange shaded regions in the x-axis represent the beam’s HPBW, ASAB, and angular separation between HPBWs of adjacent beams, respectively.
Paper: A Solution to Continuous RFI in Narrowband Radio SETI with FAST: The MultiBeam Point-source Scanning Strategy
Authors: Bo-Lun Huang, Zhen-Zhao Tao, Tong-Jie Zhang
Figure caption: Four examples of simulated RFI that could be identified by MBPS. The colored bar indicates the power with arbitrary units. (a) Signal that appears for a fraction of the observation but with constant intensity. (b) Intermittent signal over a long duration. (c) Signal that is continuous throughout the observation. (d) Signal that appears simultaneously at different beams but with the same central frequency.
Paper: A Solution to Continuous RFI in Narrowband Radio SETI with FAST: The MultiBeam Point-source Scanning Strategy
Authors: Bo-Lun Huang, Zhen-Zhao Tao, Tong-Jie Zhang
Figure caption: Examples of RFI in the observation of TRAPPIST-1. (a) The signal is visible throughout the full observation time in beam 14 but not in any other beam. (b) The signal only appears in beam 2 for a fraction of the observation but shows constant intensity. (c) The signal occupies a fraction of the observation and shows variation in intensity but is visible in all OTBs and exhibits the same central frequency. (d) The signal shows intensity falling during the entire observation in all OTBs simultaneously.
Paper: A Solution to Continuous RFI in Narrowband Radio SETI with FAST: The MultiBeam Point-source Scanning Strategy
Authors: Bo-Lun Huang, Zhen-Zhao Tao, Tong-Jie Zhang
Figure caption: (a) Waterfall plots for a simulated ETI signal in the five OTBs across the full observation time. (b) Waterfall plots for a simulated ETI signal in the five OTBs during their five OTWs, each with a length of 181 s. (c) Waterfall plots for a simulated ETI signal in the five OTBs during their OTWs with corrected frequencies. The colored bar indicates the power with arbitrary units.
Paper: A Solution to Continuous RFI in Narrowband Radio SETI with FAST: The MultiBeam Point-source Scanning Strategy
Authors: Bo-Lun Huang, Zhen-Zhao Tao, Tong-Jie Zhang
Figure caption: (a) The intensity response of a beam in the 19-beam receiver of FAST; the origin represents the center of a beam. (b) The predicted intensity variation of a sky-localized signal inside an OTW. The gray line is the response when the received signal is at a frequency of 1.05 GHz, and the blue line is the response when the signal is at 1.45 GHz (the frequency band we use for SETI observation at FAST is 1.05–1.45 GHz).
Paper: Estimating Distances from Parallaxes. VI. A Method for Inferring Distances and Transverse Velocities from Parallaxes and Proper Motions Demonstrated on Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: Demonstration of how the likelihood—prior product, P(μ∣r, v)P(v∣r), shown as the gray curves, sum to make the unnormalized distance posterior (black dashed line) via Equation (A1). The gray curves are shown just for 10 velocities from 5 to 50 km s−1 in steps of 5 km s−1, but some are so flat as to be invisible. In all panels, the measured proper motion is 1 mas yr−1. The top row is for a proper motion S/N of 4, and the bottom for 16. The right column is for a narrower prior with half the standard deviation of that in the left column. None of the functions shown are probability density functions in r. The gray ones have been normalized to unit area over the range plotted. The black dashed curve has been scaled to have the same maximum as the largest gray peak.
Paper: The Comprehensive Archive of Substellar and Planetary Accretion Rates
Authors: S. K. Betti, K. B. Follette, K. Ward-Duong, A. E. Peck, Y. Aoyama, J. Bary, B. Dacus, S. Edwards, G.-D. Marleau, K. Mohamed, J. Palmo, C. Plunkett, C. Robinson, H. Wang
Figure caption: Literature Database of accreting objects. Top: accretion rate vs. mass colored by accretion diagnostic. The dashed gray lines indicate objects with multiple accretion-rate and mass estimates. The best-fit relation, ﹩\dot{M}\sim {M}^{2.16}﹩, is shown with a black solid line, with the 1σ upper limit in gray. Bound PMCs are indicated by thicker-edged squares, while stars are indicated by circles and BDs by diamonds. Upper limits are shown by downward arrows. Bottom: accretion rate vs. mass for separate accretion diagnostics—continuum excess (light blue), Hα photometric luminosity (dark red), line luminosity (salmon), and line profile (green). The solid lines show the best fit for each diagnostic, with the black/gray line indicating the overall fit from the top panel. The vertical gray lines indicate the HBL and DBL. Overall, the literature database follows similar trends to previous surveys, while highlighting the strong scatter and variation in accretion rate and mass resulting from different methodologies.
Paper: The Comprehensive Archive of Substellar and Planetary Accretion Rates
Authors: S. K. Betti, K. B. Follette, K. Ward-Duong, A. E. Peck, Y. Aoyama, J. Bary, B. Dacus, S. Edwards, G.-D. Marleau, K. Mohamed, J. Palmo, C. Plunkett, C. Robinson, H. Wang
Figure caption: Comparison between the Literature Database physical parameters and those rederived in CASPAR colored by accretion diagnostic. The black line indicates 1–1. For masses, we show the HBL at M = 0.075 M ⊙ with the dashed black lines; under a uniform methodology, objects in the lower right quadrant decreased in mass from stellar to substellar, while in the upper left, the reverse occurred. We find 50%−89% of CASPAR parameters are within a factor of 2 of the literature value.
Paper: The Comprehensive Archive of Substellar and Planetary Accretion Rates
Authors: S. K. Betti, K. B. Follette, K. Ward-Duong, A. E. Peck, Y. Aoyama, J. Bary, B. Dacus, S. Edwards, G.-D. Marleau, K. Mohamed, J. Palmo, C. Plunkett, C. Robinson, H. Wang
Figure caption: Mass function (dN/d                   ﹩\mathrm{log}M﹩) of the 793 objects in CASPAR colored by stellar age (stacked histogram). The IMF for multiple systems from Chabrier (2005) and the field BD IMF from Kirkpatrick et al. (2021) are shown for comparison. Herbig Ae/Be stars are purposely excluded from CASPAR, as we are primarily focused on substellar objects.
Paper: The Comprehensive Archive of Substellar and Planetary Accretion Rates
Authors: S. K. Betti, K. B. Follette, K. Ward-Duong, A. E. Peck, Y. Aoyama, J. Bary, B. Dacus, S. Edwards, G.-D. Marleau, K. Mohamed, J. Palmo, C. Plunkett, C. Robinson, H. Wang
Figure caption: All-sky map indicating all objects in CASPAR colored by SFR or association overlaid on a 65 μm all-sky map (Doi et al. 2015; Takita et al. 2015). Insets: enlarged views of several nearby SFRs.
Paper: The Comprehensive Archive of Substellar and Planetary Accretion Rates
Authors: S. K. Betti, K. B. Follette, K. Ward-Duong, A. E. Peck, Y. Aoyama, J. Bary, B. Dacus, S. Edwards, G.-D. Marleau, K. Mohamed, J. Palmo, C. Plunkett, C. Robinson, H. Wang
Figure caption: Distribution of spectral types in ρ Ophiuchus from the complete census survey (black) and systems with optically thick disks (gray) from Esplin & Luhman (2020; binned as in their Figure 22). Overlaid in yellow are the CASPAR ρ Ophiuchus objects.
Paper: The Comprehensive Archive of Substellar and Planetary Accretion Rates
Authors: S. K. Betti, K. B. Follette, K. Ward-Duong, A. E. Peck, Y. Aoyama, J. Bary, B. Dacus, S. Edwards, G.-D. Marleau, K. Mohamed, J. Palmo, C. Plunkett, C. Robinson, H. Wang
Figure caption: Accretion rate vs. mass for the star and BD populations colored by specific ages. The solid lines and bands show the best linear fits and 1σ  standard deviations, where age and mass are both free parameters for each mass population. The dashed lines are extrapolations to the DBL.
Paper: The Comprehensive Archive of Substellar and Planetary Accretion Rates
Authors: S. K. Betti, K. B. Follette, K. Ward-Duong, A. E. Peck, Y. Aoyama, J. Bary, B. Dacus, S. Edwards, G.-D. Marleau, K. Mohamed, J. Palmo, C. Plunkett, C. Robinson, H. Wang
Figure caption: Top: CASPAR accretion rates vs. mass colored by age with best linear fits for each age and mass population (BDs and stars). We combined the BD ≤1 and (1–3] Myr populations to improve statistical number counts (brown pentagons). We extend the stellar fits into the BD regime indicated by the dashed lines. Bottom: residuals for the best linear fits for each age and mass population. The colors and markers are as in Figure 13.
Paper: The Comprehensive Archive of Substellar and Planetary Accretion Rates
Authors: S. K. Betti, K. B. Follette, K. Ward-Duong, A. E. Peck, Y. Aoyama, J. Bary, B. Dacus, S. Edwards, G.-D. Marleau, K. Mohamed, J. Palmo, C. Plunkett, C. Robinson, H. Wang
Figure caption: Absolute difference between the literature and CASPAR-derived temperatures/spectral types as a function of CASPAR temperature/spectral type (top) and the ratio between the literature and CASPAR-derived masses as a function of CASPAR mass (bottom) for objects with accretion rates derived from Hα emission profile modeling. The estimated accretion rates do not vary with rederived masses and radii if the spectral types are within one subclass (<200 K difference) and masses are within a factor of 2 of the original values. We find all values in CASPAR to be within those parameters.