adsabs/AstroCLIMB huggingface dataset:
Paper: PhotoD with LSST: Stellar Photometric Distances Out to the Edge of the Galaxy
Authors: Lovro Palaversa, Željko Ivezić, Neven Caplar, Karlo Mrakovčić, Bob Abel, Oleksandra Razim, Filip Matković, Connor Yablonski, Toni Šarić, Tomislav Jurkić, Sandro Campos, Melissa DeLucchi, Derek Jones, Konstantin Malanchev, Alex I. Malz, Sean McGuire, Mario Jurić
Figure caption: The variation of the difference between the true and estimated values (left: Mr, middle: [Fe/H]) with u-band magnitude. The binned background map shows the same simulated sample as in Figure 11. The symbols show binned medians and the dashed lines show robust standard deviation around the medians. At about u = 23, the scatter for both Mr and [Fe/H] starts increasing due to increasing u-band measurement error. The dataset was generated assuming a u-band 5σ limiting depth of 25.73 for coadded LSST photometry (F. B. Bianco et al. 2022). The right panel illustrates a strong anticorrelation between the differences.
Paper: PhotoD with LSST: Stellar Photometric Distances Out to the Edge of the Galaxy
Authors: Lovro Palaversa, Željko Ivezić, Neven Caplar, Karlo Mrakovčić, Bob Abel, Oleksandra Razim, Filip Matković, Connor Yablonski, Toni Šarić, Tomislav Jurkić, Sandro Campos, Melissa DeLucchi, Derek Jones, Konstantin Malanchev, Alex I. Malz, Sean McGuire, Mario Jurić
Figure caption: Analysis of the difference between Gaia's photometric (color-based) absolute magnitudes and photometric magnitudes derived from SDSS colors. Symbols show a sample of 165,834 stars with absolute magnitude Mr,Pho > 4, and SDSS-based u < 21 and 0.2 < g − r < 0.6. The median magnitude difference is −0.05 mag, with a scatter of 0.32 mag. The four panels illustrate the variation of the binned median (red circles) and scatter (red lines) with the u-band magnitude, SDSS u − g and g − r colors, and photometric metallicity.
Paper: PhotoD with LSST: Stellar Photometric Distances Out to the Edge of the Galaxy
Authors: Lovro Palaversa, Željko Ivezić, Neven Caplar, Karlo Mrakovčić, Bob Abel, Oleksandra Razim, Filip Matković, Connor Yablonski, Toni Šarić, Tomislav Jurkić, Sandro Campos, Melissa DeLucchi, Derek Jones, Konstantin Malanchev, Alex I. Malz, Sean McGuire, Mario Jurić
Figure caption: Analysis of the difference between Gaia's geometric (trigonometric) absolute magnitudes and the photometric magnitudes derived from SDSS colors. Symbols show a sample of 33,186 stars with a parallax signal-to-noise ratio above 10, absolute magnitude Mr,Geo > 4 and Mr,Pho > 4 , and SDSS-based u < 21 and 0.2 < g − r < 0.6. The median magnitude difference is −0.01 mag, with a scatter of 0.28 mag. The four panels illustrate variations of the binned median (red circles) and scatter (red lines) with the u-band magnitude, the parallax signal-to-noise ratio, SDSS g − r color, and photometric metallicity.
Paper: PhotoD with LSST: Stellar Photometric Distances Out to the Edge of the Galaxy
Authors: Lovro Palaversa, Željko Ivezić, Neven Caplar, Karlo Mrakovčić, Bob Abel, Oleksandra Razim, Filip Matković, Connor Yablonski, Toni Šarić, Tomislav Jurkić, Sandro Campos, Melissa DeLucchi, Derek Jones, Konstantin Malanchev, Alex I. Malz, Sean McGuire, Mario Jurić
Figure caption: Color-coded maps show the best-fit Ar (dust extinction along the line of sight) per pixel for the SDSS-SEGUE strip centered on l = 110° (modeled after Figure 25 from M. Berry et al. 2012). Each pixel, defined in Galactic coordinates, shows the median Ar according to the legend below each panel. The three panels correspond to distance slices of 0.3–1 kpc (left), 1–1.5 kpc (middle), and 2–2.5 kpc (right). Note that the median extinction increases rapidly with distance. In the right panel, there are no stars in the white regions in the center because extinction makes them fainter than the sample magnitude limit.
Paper: Peering into the Black Box: Forward Modeling of the Uncertainty Budget of High-resolution Spectroscopy of Exoplanet Atmospheres
Authors: Arjun B. Savel, Megan Bedell, Eliza M.-R. Kempton, Peter C. B. Smith, Jacob L. Bean, Lily L. Zhao, Kaze W. K. Wong, Jorge A. Sanchez, Michael R. Line
Figure caption: Schematic of scope pipeline. This example uses a planetary emission spectrum calculated with the CHIMERA (M. R. Line et al. 2013) atmospheric model as input. This simulation is meant to reconstruct the IGRINS data set used to identify the emission of WASP-77Ab by M. R. Line et al. (2021). The slight discontinuity in the planetary emission tracks is due to a gap in exposures corresponding to these observations. The SNR of this simulation matches the SNR of the M. R. Line et al. 2021 observations (SNR = 12.8); nine other noise realizations span SNRs from 11.0 to 19.0.
Paper: Peering into the Black Box: Forward Modeling of the Uncertainty Budget of High-resolution Spectroscopy of Exoplanet Atmospheres
Authors: Arjun B. Savel, Megan Bedell, Eliza M.-R. Kempton, Peter C. B. Smith, Jacob L. Bean, Lily L. Zhao, Kaze W. K. Wong, Jorge A. Sanchez, Michael R. Line
Figure caption: The eigenweights of our PCA decomposition for IGRINS standard-star observations for a single order (order 5 in the H band). In this case, the first two components clearly covary with air mass, and multiple components exhibit subtle substructure as a function of date.
Paper: Peering into the Black Box: Forward Modeling of the Uncertainty Budget of High-resolution Spectroscopy of Exoplanet Atmospheres
Authors: Arjun B. Savel, Megan Bedell, Eliza M.-R. Kempton, Peter C. B. Smith, Jacob L. Bean, Lily L. Zhao, Kaze W. K. Wong, Jorge A. Sanchez, Michael R. Line
Figure caption: Simulated telluric spectra, zoomed in on a narrow spectral region to display the effect of changing air mass (top) and date (bottom). Air mass is clearly the first-order effect, but some lines are particularly time variable.
Paper: LAMOST Reveals Long-lived Protoplanetary Disks
Authors: Xiao-Long Wang, Min Fang, Yao Liu, Miao-Miao Zhang, Wen-Yuan Cui
Figure caption: H-R diagram of the identified disked objects (gray circles). Left: the stellar luminosities and effective temperatures are determined by fitting stellar photospheres to the observed optical and NIR photometry. The blue solid curves are isochrones from the PARSEC stellar model (A. Bressan et al. 2012), with corresponding ages labeled. The 14 newly discovered Peter Pan disks are marked with additional red plus signs. Right: same as the left panel, but the stellar luminosities and effective temperatures are obtained by fitting disked models to the full SEDs. Also displayed in the left panel are the Peter Pan disks (green filled stars) from J. Lee et al. (2020) and the 10 Myr isochrone (cyan dashed curve) from I. Baraffe et al. (2015).
Paper: LAMOST Reveals Long-lived Protoplanetary Disks
Authors: Xiao-Long Wang, Min Fang, Yao Liu, Miao-Miao Zhang, Wen-Yuan Cui
Figure caption: Accretion rates vs. stellar masses (left) and ages (right). In each panel, young and old accretors are shown as red and blue circles, respectively. Nonaccreting stars are shown as downward-pointing triangles, with purple for the young population and cyan for the old population. The green filled stars are Peter Pan disks tabulated in J. Lee et al. (2020). In the left panel, the solid line and gray shaded area show respectively the best linear fit and the corresponding 1σ scatter (0.75 dex) from L. Hartmann et al. (2016). In the right panel, the solid line and gray shaded area show respectively the best-fitted relation for stars with M⋆ = 0.7 M⊙ and the corresponding 1σ scatter (0.5 dex). The dashed line is the same relation corrected for stellar mass (M⋆ = 0.4 M⊙, the typical stellar mass of our sample) using the relation in the left panel. To perform the correction, the solid line is downward by ∼0.5 dex according to the difference in mass accretion rates of 0.4 and 0.7 M⊙ stars using the relation in the left panel.
Paper: LAMOST Reveals Long-lived Protoplanetary Disks
Authors: Xiao-Long Wang, Min Fang, Yao Liu, Miao-Miao Zhang, Wen-Yuan Cui
Figure caption: Left: E(KS − W3) vs. E(KS − W4) color excess plot for our targets. Full disks, transitional disks, evolved disks, and debris disks are shown as red circles, orange squares, cyan triangles, and blue diamonds, respectively. The newly discovered Peter Pan disks are highlighted with additional blue plus signs. The solid lines display the boundaries used to classify our targets into different categories (T. L. Esplin et al. 2014, 2018). Right: same as the left panel, but showing the E(KS − W2) vs. E(KS − W3) color excess plot.
Paper: LAMOST Reveals Long-lived Protoplanetary Disks
Authors: Xiao-Long Wang, Min Fang, Yao Liu, Miao-Miao Zhang, Wen-Yuan Cui
Figure caption: Infrared color–color plots used to select candidates displaying infrared excess emission. In each panel, the solid cyan curve denotes the intrinsic colors of 5–30 Myr old stars (M. J. Pecaut & E. E. Mamajek 2013). The dashed blue line displays the extinction direction (S. Wang & X. Chen 2019) and is used as the border line separating disked objects from diskless ones. The background gray image displays the distribution of the full catalog. The blue circles are candidates showing excess emission in the color–color plots, and the red plus signs mark our working sample comprising 855 genuine disked objects (see Section 3.1 for selecting genuine disked objects).
Paper: LAMOST Reveals Long-lived Protoplanetary Disks
Authors: Xiao-Long Wang, Min Fang, Yao Liu, Miao-Miao Zhang, Wen-Yuan Cui
Figure caption: Comparison of the spectral types derived in this work and those from the LAMOST archive. The solid line is the line of equality. The dashed and dashed–dotted lines show differences of three and five subtypes, respectively. In the lower right corner, we display the typical uncertainties of our spectral typing (∼1.0 subtypes).
Paper: LAMOST Reveals Long-lived Protoplanetary Disks
Authors: Xiao-Long Wang, Min Fang, Yao Liu, Miao-Miao Zhang, Wen-Yuan Cui
Figure caption: SEDs and WISE images of the 14 newly discovered Peter Pan disks. For each source, the main panel shows the SED of the target, with blue, orange, and red circles representing optical, NIR, and WISE photometry, respectively. The black dashed line represents the best-fitted stellar photosphere, and the red solid line is the best-fitted disked model. The source names and the best-fitted inclination angles are labeled. The top panels show the WISE images of the source, and only bands with reliable photometry are displayed.
Paper: LAMOST Reveals Long-lived Protoplanetary Disks
Authors: Xiao-Long Wang, Min Fang, Yao Liu, Miao-Miao Zhang, Wen-Yuan Cui
Figure caption: Histogram showing the distribution of the reduced χ2 of the light curves. The old and young populations are shown as blue hatched and red filled histograms, respectively. The black vertical dashed line marks the threshold distinguishing between variables and nonvariables (i.e., ﹩{\chi }_{{\rm{red}}}^{2}=5﹩).
Paper: LAMOST Reveals Long-lived Protoplanetary Disks
Authors: Xiao-Long Wang, Min Fang, Yao Liu, Miao-Miao Zhang, Wen-Yuan Cui
Figure caption: Equivalent width of Hα emission line as a function of spectral type. The young population is displayed as red pluses and the old population as blue circles. The solid curve is the dividing line separating strong accretors from weak ones (M. Fang et al. 2009).
Paper: The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
Authors: Judah Van Zandt, Erik A. Petigura, Jack Lubin, Lauren M. Weiss, Emma V. Turtelboom, Tara Fetherolf, Joseph M. Akana Murphy, Ian J. M. Crossfield, Gregory J. Gilbert, Teo Močnik, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Isabel Angelo, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Steve B. Howell, Andrew W. Mayo, Daria Pidhorodetska, Alex S. Polanski, James Rogers, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Dakotah Tyler, Samuel W. Yee, Jon Zink
Figure caption: Side-by-side comparison of injection/recovery results and calculated completeness to resolved orbits (left) and trends (right). We tracked whether our automated search algorithm recovered injected RV signals successfully (blue/green points for resolved orbits/trends) or unsuccessfully (red points). From this collection of recoveries, we calculated a sensitivity map, with the contour lines marking completeness deciles and the black contour denoting the 50% completeness boundary. We injected 2000 signals for each system. Top row: completeness for a typical system in our survey (TOI-1173: 3.9 yr baseline, 27 observations). Bottom row: average completeness of the 47 targets in our survey, with the blue boxes indicating our nominal definition of a DG. Our average sensitivity in this interval is 30% for resolved orbits and 35% for trends. The orange and purple dashed boxes indicate the giant-planet definitions used by L. J. Rosenthal et al. (2022) and M. L. Bryan et al. (2019), respectively. Our survey had 32% (27%) sensitivity to resolved orbits (trends) using the L. J. Rosenthal et al. (2022) definition and 30% (43%) sensitivity using that of M. L. Bryan et al. (2019). Note that we treated resolved orbits and trends as distinct detection classes, meaning that an orbit recovered as a trend was considered an unsuccessful recovery in the resolved recovery map and vice versa.
Paper: The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
Authors: Judah Van Zandt, Erik A. Petigura, Jack Lubin, Lauren M. Weiss, Emma V. Turtelboom, Tara Fetherolf, Joseph M. Akana Murphy, Ian J. M. Crossfield, Gregory J. Gilbert, Teo Močnik, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Isabel Angelo, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Steve B. Howell, Andrew W. Mayo, Daria Pidhorodetska, Alex S. Polanski, James Rogers, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Dakotah Tyler, Samuel W. Yee, Jon Zink
Figure caption: Left: our orbital fit to the TOI-1174 system using radvel. (a) The full RV time series and errors with black circles, with our preferred model as a blue line. (b) The residuals to the planetary model, isolating the fitted trend/curvature. (c) The RV time series phase-folded to the period of the inner planet in this system. The red points give binned RV values. We did not recover the inner-transiting-planet signal in the RVs. Right: our ethraid posterior surface derived using the measured trend. The green regions show models consistent with the RV trend, and the red regions show models consistent with both the RVs and the direct imaging for this system, revealing no luminous companions. The dark (light) regions indicate 68% (95%) confidence intervals. The gray line approximates the contrast limits imposed by imaging for a circular, face-on companion. The gray panels at low mass and short separations show companion parameters incompatible with the observed trend due to our observing baseline.
Paper: The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
Authors: Judah Van Zandt, Erik A. Petigura, Jack Lubin, Lauren M. Weiss, Emma V. Turtelboom, Tara Fetherolf, Joseph M. Akana Murphy, Ian J. M. Crossfield, Gregory J. Gilbert, Teo Močnik, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Isabel Angelo, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Steve B. Howell, Andrew W. Mayo, Daria Pidhorodetska, Alex S. Polanski, James Rogers, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Dakotah Tyler, Samuel W. Yee, Jon Zink
Figure caption: Mass–separation prior informed by the L. J. Rosenthal et al. (2021) and D. Raghavan et al. (2010) surveys. Left: minimum masses and orbital separations of the CLS (L. J. Rosenthal et al. 2021) sample of planets (blue points) and brown dwarfs (orange points). We also show the survey-averaged completeness map (red contours), emphasizing the 50% contour with a black line. We compute the companion occurrence in the cells defined by the red dashed lines. The hatch marks show cells containing fewer than three objects, giving rise to highly uncertain occurrence rates. However, inspection of the RV constraints in Appendix A shows negligible overlap with these regions, so they do not affect our overall results. Right: the domain of M and a we explore in our companion search. Each M–a subdomain is colored with the number of objects per star and serves as our joint M–a prior described in Section 5.2. The highest-mass bins are based on the D. Raghavan et al. (2010) rates.
Paper: The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
Authors: Judah Van Zandt, Erik A. Petigura, Jack Lubin, Lauren M. Weiss, Emma V. Turtelboom, Tara Fetherolf, Joseph M. Akana Murphy, Ian J. M. Crossfield, Gregory J. Gilbert, Teo Močnik, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Isabel Angelo, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Steve B. Howell, Andrew W. Mayo, Daria Pidhorodetska, Alex S. Polanski, James Rogers, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Dakotah Tyler, Samuel W. Yee, Jon Zink
Figure caption: Measurements of the field (blue) and conditional (orange) occurrence rates of DGs under different planet definitions. The black lines show distribution quartiles. The distributions to the left show occurrence rates for our nominal definitions: a = 1–10 au, ﹩{M}_{p}\sin i=﹩ 70–4000 M⊕ for DGs and a > 1 au, Rp = 1–4 R⊕ for CSs. The distributions in the center and right show occurrence rates for planet definitions matching those of L. J. Rosenthal et al. (2022) and M. L. Bryan et al. (2019), respectively. We annotate each distribution with the probability that the conditional rate is enhanced over the field rate.
Paper: The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
Authors: Judah Van Zandt, Erik A. Petigura, Jack Lubin, Lauren M. Weiss, Emma V. Turtelboom, Tara Fetherolf, Joseph M. Akana Murphy, Ian J. M. Crossfield, Gregory J. Gilbert, Teo Močnik, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Isabel Angelo, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Steve B. Howell, Andrew W. Mayo, Daria Pidhorodetska, Alex S. Polanski, James Rogers, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Dakotah Tyler, Samuel W. Yee, Jon Zink
Figure caption: Average sensitivity to companions as a function of minimum mass and separation for the CLS. The shaded regions show domains of constant detection probability, and the solid black contour shows the 50% detection probability boundary. We recalculated this map after adjusting for inclination effects to determine the CLS sensitivity to true mass (see Section 6.2). We show the 50% boundary of the adjusted map as a dashed black line. We use a blue rectangle to show our nominal definition of a DG (a = 1–10, M = 70–4000M⊕). The average CLS sensitivity to minimum/true masses within this domain is 59%/52%.
Paper: The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
Authors: Judah Van Zandt, Erik A. Petigura, Jack Lubin, Lauren M. Weiss, Emma V. Turtelboom, Tara Fetherolf, Joseph M. Akana Murphy, Ian J. M. Crossfield, Gregory J. Gilbert, Teo Močnik, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Isabel Angelo, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Steve B. Howell, Andrew W. Mayo, Daria Pidhorodetska, Alex S. Polanski, James Rogers, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Dakotah Tyler, Samuel W. Yee, Jon Zink
Figure caption: Distribution of eccentricity vs. orbital separation for confirmed exoplanets in the NEA with σe ≤ 0.13. The confirmed planets are shown as unfilled circles and the confirmed DGs (1–10 au and 70–4000 M⊕) as blue circles. For confirmed giants, the marker size is proportional to our survey-averaged completeness at the planet’s mass and separation. We show the giants in our survey in orange and indicate measurements with less than 3σ eccentricity precision with an arrow, placing the bottom of the arrow at the 1σ upper limit. The giant companions in our survey may have lower eccentricities than the average DG, but a larger sample is needed to draw a strong conclusion.
Paper: The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
Authors: Judah Van Zandt, Erik A. Petigura, Jack Lubin, Lauren M. Weiss, Emma V. Turtelboom, Tara Fetherolf, Joseph M. Akana Murphy, Ian J. M. Crossfield, Gregory J. Gilbert, Teo Močnik, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Isabel Angelo, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Steve B. Howell, Andrew W. Mayo, Daria Pidhorodetska, Alex S. Polanski, James Rogers, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Dakotah Tyler, Samuel W. Yee, Jon Zink
Figure caption: The same as Figure A1 but for HD 191939. We included the three transiting planets in our model, and our blind search algorithm detected the known 100 days super-Saturn as well as a spurious long-period planet. The blue posterior surface shows constraints imposed by the astrometric acceleration measured in this system. The trend and curvature in our truncated RV time series along with the astrometric acceleration yield a high planetary odds ratio.
Paper: The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
Authors: Judah Van Zandt, Erik A. Petigura, Jack Lubin, Lauren M. Weiss, Emma V. Turtelboom, Tara Fetherolf, Joseph M. Akana Murphy, Ian J. M. Crossfield, Gregory J. Gilbert, Teo Močnik, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Isabel Angelo, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Steve B. Howell, Andrew W. Mayo, Daria Pidhorodetska, Alex S. Polanski, James Rogers, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Dakotah Tyler, Samuel W. Yee, Jon Zink
Figure caption: The same as Figure A1 but for HD 219134. We chose RV measurements from an arbitrary 4 yr span of this system’s full data set. We recovered one of the nontransiting planets using a blind search but missed two others. We analyzed the measured trend and HGCA astrometry to calculate a probability near 1 of this signal originating from a planet. We also tested other 4 yr spans and verified that our choice did not strongly influence our final odds ratio.