adsabs/AstroCLIMB huggingface dataset:
Paper: The California Legacy Survey. IV. Lonely, Poor, and Eccentric: A Comparison between Solitary and Neighborly Gas Giants
Authors: Lee J. Rosenthal, Andrew W. Howard, Heather A. Knutson, Benjamin J. Fulton
Figure caption: Occurrence with respect to semimajor axis for single giant planets and multiple giant planets. The steps and dots are median values, while the vertical lines are 15.9%–84.1% confidence intervals. The single giant planets display a pileup of very hot Jupiters within 0.06 au, tentatively not shared by the multiple giant planets.
Paper: The California Legacy Survey. IV. Lonely, Poor, and Eccentric: A Comparison between Solitary and Neighborly Gas Giants
Authors: Lee J. Rosenthal, Andrew W. Howard, Heather A. Knutson, Benjamin J. Fulton
Figure caption: Lonely and neighborly warm Jupiters, described in Section 4.3. 11 systems have lonely warm Jupiters, while 10 systems host both a warm Jupiter and at least one detected outer giant companion. This does not refute the synthetically driven claim by Jackson et al. (2021) of secular warm Jupiter migration.
Paper: The California Legacy Survey. IV. Lonely, Poor, and Eccentric: A Comparison between Solitary and Neighborly Gas Giants
Authors: Lee J. Rosenthal, Andrew W. Howard, Heather A. Knutson, Benjamin J. Fulton
Figure caption: Cumulative ﹩M\sin i﹩ distributions for multiple giants within 3 au and single giants split across an eccentricity of 0.2. While the single and circular giants are >4σ separated from the multiples, eccentric giants are inconclusively more massive. Note that this may be a selection effect for more eccentric detections with greater mass.
Paper: The California Legacy Survey. IV. Lonely, Poor, and Eccentric: A Comparison between Solitary and Neighborly Gas Giants
Authors: Lee J. Rosenthal, Andrew W. Howard, Heather A. Knutson, Benjamin J. Fulton
Figure caption: Occurrence as a function of ﹩M\sin i﹩ for single and multiple giants. The steps and dots are median values, while the vertical lines are 15.9%–84.1% confidence intervals. The two distributions are not ≤2σ separated in all four considered ranges.
Paper: The California Legacy Survey. IV. Lonely, Poor, and Eccentric: A Comparison between Solitary and Neighborly Gas Giants
Authors: Lee J. Rosenthal, Andrew W. Howard, Heather A. Knutson, Benjamin J. Fulton
Figure caption: Observed semimajor axis ratio distribution of two-giant systems. The curve is a kernel density estimation of the distribution, while the vertical ticks show the observed set of axis ratios. The horizontal bar shows the kernel width.
Paper: The California Legacy Survey. IV. Lonely, Poor, and Eccentric: A Comparison between Solitary and Neighborly Gas Giants
Authors: Lee J. Rosenthal, Andrew W. Howard, Heather A. Knutson, Benjamin J. Fulton
Figure caption: Observed multiplicity of giant planets in the CLS sample. Half as many systems contain two or more giants as contain only one giant.
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: Galaxy number counts for sources identified from our LW detection image and measured in total magnitudes from F150W, F160W, F356W, and F444W. Stars and objects with unreliable photometry are removed. Effects of blending at intermediate brightness are shown by the colored curves where we allow Kron aperture corrections for blended sources. Literature F160W-selected counts in A2744 by Shipley et al. (2018) and Kokorev et al. (2022) are shown by the unfilled gray boxes and diamonds, respectively; note that bCGs have been excluded. Error bars denote 1σ Poisson uncertainties. Counts are not corrected for magnification.
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: The selection of stars and spurious objects (bad pixels or model residuals) is determined from the flux ratio in large to small apertures above a limiting magnitude threshold. Stars are identified from the JWST/F200W image (blue) at positions corresponding to the catalog, and/or directly from the HST/F160W image (yellow) to account for high proper motion. We also include any star that contributed to PSF models in any band (green) that has a match to an object in the catalog. Some artifacts such as bCG model residuals can also be similarly flagged (red).
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: Schematic of the depth variation across the noise-equalized LW coadded detection image aggregated from the DDT (gray), GLASS (blue), and UNCOVER programs. Combining F277W, F356W, and F444W, the 5σ depths in our LW detection band measured in 0.″32 apertures span 28.5–30.0 mag. Poisson contributions of the brightest objects feature prominently in our JWST weight maps. Although provided in our mosaic release, the UNCOVER NIRISS parallel imaging is not yet cataloged and so is not shown.
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: Performance of z phot assessed by comparison with known z spec, described in Section 2.4. Outlier sources with z phot wrong by more than 0.15Δz/(1 + z spec) are colored red. The lower panel shows residuals in normalized units of σ away from z spec. N = 372 sources are compared finding 40 outliers (10.8%), an overall tightness σ NMAD = 0.0359 and an outlier-removed σ NMAD = 0.0301. z phot are derived from super catalog SEDs fit with EA z Y using the SFHz_CORR template set.
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: Depth as a function of cumulative area for each filter mosaic as well as the LW detection image. Measurements are taken from 10,000 empty apertures of 0.″32 diameter, per filter. Gray dotted lines mark depths at 27, 28, 29, and 30 AB mag.
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: PSF growth curves for each filter before (top) and after (bottom) matching to F444W. After matching, all filters have deviations below the 1% level at the smallest aperture diameter used (0.″32). Growth curves are shown relative to the F444W growth curve; a value of 1 indicates perfect matching with F444W. Dashed lines indicate the ±1% deviations from exact matching (solid black line). Dotted lines indicate the location of 0.″32 and 0.″70 aperture diameters.
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: Zoom-in view around the two primary cluster cores of A2744 in F444W. The bCGs and ICL visible in the input image (left) are removed by subtracting fitted models (middle), with the models themselves on the right.
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: Color composite image of the JWST footprint of A2744, with three cluster cores highlighted. bCGs and ICL have been subtracted. Apertures consistent with our super photometric catalog are shown in green for reliable objects (see Section 4.6).
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: Photometric uncertainty as a function of magnitude shown by log10-scaled 2D histograms for total fluxes derived in 0.″32 diameter apertures. Catalog depths for each filter measured in the same aperture size corresponding to the 50th and 10th percentile areas are indicated by the dashed and solid lines, respectively.
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: HIP 94931; KOI-3158 (Kepler-444). Left: RVs from Keck-HIRES. Panels include (top to bottom) the full RV time series, RV residuals, and the RVs phase-folded to the orbits of the individual planets (after subtracting the contributions from the other known planets). The phase-folded plots include weighted mean RVs binned by orbital phase (red circles). Right: periodograms of the HIRES RVs, before (top) and after (bottom) subtracting the best-fit model that includes the transiting planets and one nontransiting stellar companion modeled as an RV trend.
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-41 (Kepler-100). The best-fit model (blue line) includes a nontransiting planet, Kepler-100 e, at 60 days (orbit details inset in phase-folded panel). The periodograms in the right column are of the RVs (top) and the RVs after the best-fit model has been subtracted (bottom).
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-94 (Kepler-89). 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-72 (Kepler-10). Left: the RVs were taken at Keck-HIRES (black circles) and TNG-HARPS-N (maroon triangles). A planet candidate is marginally detected at 25 days (ΔBIC = –18).
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-85 (Kepler-65). Left: the best-fit model (blue line) includes a nontransiting planet, Kepler-65 e (orbit details inset in phase-folded panel). The periodograms in the right column are of the RVs (top) and the RVs after the best-fit model has been subtracted (bottom).
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-82 (Kepler-102). Left: the RVs were taken at Keck-HIRES (black circles) and TNG-HARPS-N (maroon triangles). 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-70 (Kepler-20). Left: the RVs were taken at Keck-HIRES (black circles) and TNG-HARPS-N (maroon triangles). The best-fit model includes a nontransiting planet, Kepler-20 g, at 35 days (orbital parameters inset in phase-folded panel).
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-84 (Kepler-19). Left: the RVs were taken at Keck-HIRES (black circles) and TNG-HARPS-N (maroon triangles). The best-fit model includes a nontransiting planet, Kepler-19 c, at 28.54 days (orbital parameters inset in phase-folded panel).
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-69 (Kepler-93). Left: the RVs were taken at Keck-HIRES (black circles) and TNG-HARPS-N (maroon triangles). The best-fit model includes a stellar companion modeled as an RV trend.
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-316 (Kepler-139). The best-fit model includes a nontransiting planet at 1800 days, although the automated KGPS algorithm did not detect this planet owing to the unusual time sampling. Right: periodograms of the RVs after removing a model of the transiting planets only (top) and our best-fit model including a giant planet at 1800 days (bottom).
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-351 (Kepler-90). Left: this system has eight transiting planets, of which only the most massive is detected in the RVs. Right: periodogram of the RVs after removing the best model with all transiting planets. 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-377 (Kepler-9). Left: RVs are from HIRES (black dots) and HARPS-N (maroon triangles). The most recent RV is consistent with a moderate upward trend and/or curvature.