adsabs/AstroCLIMB huggingface dataset:
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-370 (Kepler-145). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-295 (Kepler-134). Left: there is a marginally detected trend in the RVs (ΔBIC = –54).
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-365 (Kepler-538). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-321 (Kepler-406). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-305 (Kepler-99). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-299 (Kepler-98). No nontransiting companions are detected.
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Coverage in the mass–metallicity plane (center). The x-axis is the initial Z of a model relative to solar, and the y-axis is M ZAMS of a model relative to solar. Six metallicities, each marked with a different color, and 70 masses at each metallicity (circles) span the mass–metallicity plane. The nuclear reaction network for low-mass (left) and high-mass (right) models is illustrated. These x-axes are the difference in the number of neutrons and protons in an isotope. Positive values indicate neutron-rich isotopes, the zero value is marked by the red vertical line, and negative values indicate proton-rich isotopes. These y-axes are the number of protons in an isotope, labeled by their chemical element names. Isotopes in the reaction network are shown by purple squares. Reactions between isotopes are shown by gray lines. Note Fe in the low-mass reaction network does not react with other isotopes. Fe is included for a more consistent specification of the initial composition, hence any microphysics that depends upon the composition including the opacity, equation of state, element diffusion, and neutrino emission.
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Low-mass tracks in a γHRD (left panels) and a νHRD (right panels) for Z = 1 Z ⊙ over 0.2–2.0 M ⊙ (top row) and 2.0–7.0 M ⊙(bottom row). Tracks are colored by evolutionary phase and labeled. WD cooling tracks are suppressed for visual clarity. Luminosities are normalized to L ⊙ = 3.828 × 1033 erg s−1 (Prša et al. 2016). The 1 M ⊙ and 3 M ⊙ tracks are highlighted in black as they are analyzed in detail as examples of low-mass models that do and do not undergo the He flash, respectively.
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Light curves for photons (left) and neutrinos (right). Tracks span 0.2–150 M ⊙ for Z = 1 Z ⊙ and are labeled. Key phases of evolution including the ZAMS (black circles), TAMS (black circles), core He flashes (light green), thermal pulses, and pre-supernova stage are also labeled. The PMS light curves are suppressed for visual clarity. L  ν  during the nitrogen flash (He flash for photons) and thermal pulses for the M < 8 M ⊙ light curves can exceed L  γ . At and beyond core C burning, L  ν  dominates the evolution of the M ≥ 8 M ⊙ light curves. Luminosities are normalized to L ⊙ = 3.828 × 1033 erg s−1 (Prša et al. 2016).
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Tracks in a γHRD (left panels) and νHRD (right panels) for M ZAMS = 1 M ⊙ (top row) and 3 M ⊙ (bottom row) across all six metallicities. Luminosities are normalized to the current solar photon luminosity L ⊙ = 3.828 × 1033 erg s−1 (Prša et al. 2016). Metal-poor tracks are generally bluer and more luminous than metal-rich tracks.
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Ratio of L  ν  to L  ν  of the Z = 1 Z ⊙ model vs. M ZAMS for all six metallicities at ZAMS (top panel), TAMS (second panel), and core He depletion (CHeD; third panel). The ratio of E  ν  to E  ν  of the Z = 1 Z ⊙ model versus M ZAMS for all six metallicities at TAMS (fourth panel), CHeD (fifth panel), and final fate (bottom panel). Each panel is colored by the final fate given by the legend.
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Total energy emitted in photons and neutrinos over the lifetime of a model (top) and their ratio (bottom) across the mass–metallicity plane. Transitions between different final fates occur at local extrema, indicated by the colored panels and labels.
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Components of L  ν  over the lifetimes of a 1 M ⊙, 1 Z ⊙ model (top) and a 3 M ⊙, 1 Z ⊙ model (bottom). The x-axis is the sequential model number, a nonlinear proxy for time, which begins on the left at core H depletion and ends on the right as a cool WD at each metallicity. Phases of evolution are marked by the colored regions, and the time spent in each phase is labeled. Curves show the luminosities from nuclear and thermal processes and their subcomponents, and are smoothed with a 50 model moving-average filter. Luminosities are normalized to L ⊙ = 3.828 × 1033 erg s−1 (Prša et al. 2016).
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: Differential source counts at 1.4 GHz. The MALS source counts corrected for the 5σ detection threshold, shown for both the katbeam (red filled circles) and plumber (black filled diamonds) beam models and the raw source counts (magenta filled triangles pointing downwards), have been scaled to 1.4 GHz using α  =  −0.74. The counts from NVSS (blue filled triangles pointing to the right; Condon et al. 1998) and MeerKAT-DEEP2 (scaled from 1.266 GHz using α  =  −0.7 and displayed using blue filled circles; Mauch et al. 2020) presented in Matthews et al. (2021), FIRST (empty green asterisks; White et al. 1997), the Lockman hole project (green filled triangles pointing up; Prandoni et al. 2018), and the MIGHTEE COSMOS (empty teal triangles pointing left) and XMM-LSS (empty orange boxes) counts based on the modified SKADS model (Hale et al. 2023) are also shown.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: Integrated flux density comparison at 1.38 GHz of 345 central targets and 64 gain calibrators from MALS with NVSS (left) and 1150 compact sources (S/N > 8) detected in four twice-observed MALS fields (right). The dashed lines mark median offsets. In the right panel, sources with 8 ≤ S/N ≤15 are color coded.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: MALS SPW9 to NVSS flux density ratio for 15,834 sources. The scatter plot is for flux densities corrected using the katbeam. The circles and diamonds with error bars (1σ) correspond to ratios (3′ bins) based on beam models from katbeam and plumber, respectively. The NVSS flux densities have been scaled to 1380 MHz using α = −0.7 for this analysis. The horizontal dashed lines represent median values for the whole sample.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: Distributions of integrated flux densities (S) in linear and log scales (top panels), and apparent and deconvolved (DC) major axis of sources (bottom panels). The insets show CDF.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: Astrometric comparison of 5990 sources from MALS with FIRST. The remaining details are the same as in Figure 12.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: Ratios (katbeam / plumber) of primary beams for SPW9 (left) and SPW2 (right). The extent of these images is the same as the primary beam-corrected MALS images. The dashed circles mark beam FWHMs of 62.′5 (SPW9) and 85.′7 (SPW2) from Mauch et al. (2020).
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: Sky distribution of MALS pointings—the points have been color coded on the basis of median astrometric offsets between MALS and NVSS. The MALS pointings at δ < −40° do not overlap with NVSS and, hence, are absent in this plot.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: Sky distribution of MALS pointings for median flux density ratios between MALS and NVSS. The remaining details are the same as in Figure 14.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: Flux density comparison at 1.38 GHz of 15,834 compact and isolated sources from MALS with NVSS.
Paper: The UNCOVER Survey: A First-look HST + JWST Catalog of 60,000 Galaxies near A2744 and beyond
Authors: John R. Weaver, Sam E. Cutler, Richard Pan, Katherine E. Whitaker, Ivo Labbé, Sedona H. Price, Rachel Bezanson, Gabriel Brammer, Danilo Marchesini, Joel Leja, Bingjie Wang, 冰洁 王, Lukas J. Furtak, Adi Zitrin, Hakim Atek, Iryna Chemerynska, Dan Coe, Pratika Dayal, Pieter van Dokkum, Robert Feldmann, Natascha M. Förster Schreiber, Marijn Franx, Seiji Fujimoto, Yoshinobu Fudamoto, Karl Glazebrook, Anna de Graaff, Jenny E. Greene, Stéphanie Juneau, Susan Kassin, Mariska Kriek, Gourav Khullar, Michael V. Maseda, Lamiya A. Mowla, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, Camilla Pacifici, Casey Papovich, David J. Setton, Alice E. Shapley, Heath V. Shipley, Renske Smit, Mauro Stefanon, Edward N. Taylor, Andrea Weibel, Christina C. Williams
Figure caption: Effective catalog depths over the A2744 JWST footprint for the 15 available photometric bands and their transmission curves. The effective depth of our LW detection image is also included. Depths are quoted in 0.″32 diameter apertures and correspond to the area-weighted 50th (median) and 10th percentiles (dashed and solid lines, respectively). Areas in HST imaging without JWST coverage are not considered. See the text for details.
Paper: The UNCOVER Survey: A First-look HST + JWST Catalog of 60,000 Galaxies near A2744 and beyond
Authors: John R. Weaver, Sam E. Cutler, Richard Pan, Katherine E. Whitaker, Ivo Labbé, Sedona H. Price, Rachel Bezanson, Gabriel Brammer, Danilo Marchesini, Joel Leja, Bingjie Wang, 冰洁 王, Lukas J. Furtak, Adi Zitrin, Hakim Atek, Iryna Chemerynska, Dan Coe, Pratika Dayal, Pieter van Dokkum, Robert Feldmann, Natascha M. Förster Schreiber, Marijn Franx, Seiji Fujimoto, Yoshinobu Fudamoto, Karl Glazebrook, Anna de Graaff, Jenny E. Greene, Stéphanie Juneau, Susan Kassin, Mariska Kriek, Gourav Khullar, Michael V. Maseda, Lamiya A. Mowla, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, Camilla Pacifici, Casey Papovich, David J. Setton, Alice E. Shapley, Heath V. Shipley, Renske Smit, Mauro Stefanon, Edward N. Taylor, Andrea Weibel, Christina C. Williams
Figure caption: Astrometric performance of the imaging data set based on the positions of bright stars in HST/F160W compared to Gaia DR3. 1 and 4 pixel areas are shown by the solid and dashed squares, respectively. Filled purple and gray elliptical contours enclose roughly 50% and 90% of bright stars, respectively. The median deviation (purple cross) and the standard deviation of the absolute median deviation are quoted for each axis corresponding to the innermost 50% of stars.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: KGPS algorithm. This algorithm was applied to 63 systems to search for nontransiting giant planets while accounting for the known (transiting) planets.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: The masses (or ﹩M\sin i﹩ values or mass estimates) vs. semimajor axes of the KGPS I transiting planets and companions. For systems with a giant planet (﹩M\sin i\gt 0.3{M}_{{\rm{J}}}﹩), the circle fill color corresponds to the maximum detected companion mass in the system (capped at 100 Jupiter masses), and the edge color encircling each point corresponds to the planetary system. Black circles correspond to transiting planets in our survey for which giant planets were not detected. Planet masses or ﹩M\sin i﹩ values are reported where they are measured, but mass estimates are used for m ≲ 3 × 10−2 M J (see text for details). Companions that have eccentric, stellar-mass companions at large separations (KOI-2169 and KOI-3158; yellow) have planets that are smaller and closer to their stars than the typical transiting planets from the KGPS sample, whereas transiting planets that have giant planet companions (nonyellow colors) have comparable sizes and orbits to the transiting planets without detected giant planet companions.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Architectures of the KGPS I planetary systems. Systems are ranked by the semimajor axis of the innermost known (transiting) planet. Point sizes scale with the square root of planet masses, ﹩M\sin i﹩ values, or mass estimates from the Weiss & Marcy (2014) mass–radius relationship. Colors correspond to eccentricities (if measured); low-mass planets are assumed to have circular orbits.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Left: the eccentricity vs. semimajor axis of companions with ﹩M\sin i\gt 0.3{M}_{{\rm{J}}}﹩ in KGPS (blue) and CLS (Rosenthal et al. 2021, gray). The eccentricities of the KGPS transiting planets are assumed to be zero. The point size scales with the square root of the companion ﹩M\sin i﹩ (see legend). Right: the cumulative distribution function of the KGPS and CLS companions for a > 1 au, with Kolmogorov–Smirnov and Anderson–Darling p-values shown.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Observed rms scatter of the RVs vs. expected rms from jitter. The jitter is computed based on the average of the Mount Wilson S HK index, the stellar mass, the stellar rotation, and photon limits. The vertical axis for triangles shows the rms of the unfit (raw) RVs, and the vertical axis for circles shows the rms of the residuals to the best-fit model that includes transiting planets and any detected nontransiting planets and companions. The RVs for some systems had significant reductions in their rms (factor of 5 or more) when the model included a massive companion (blue).