adsabs/AstroCLIMB huggingface dataset:
Paper: A Comparison of the Composition of Planets in Single-planet and Multiplanet Systems Orbiting M dwarfs
Authors: Romy Rodríguez Martínez, David V. Martin, B. Scott Gaudi, Joseph G. Schulze, Anusha Pai Asnodkar, Kiersten M. Boley, Sarah Ballard
Figure caption: Histogram showing the distribution of planet-hosting M dwarfs by the number of planets per star. There are currently 170 systems hosting a single (detected) planet and 75 systems with two or more planets. There are currently no known M dwarfs hosting six planets.
Paper: The ﹩\dot{M}﹩–M disk Relationship for Herbig Ae/Be Stars: A Lifetime Problem for Disks with Low Masses?
Authors: Sierra L. Grant, Lucas M. Stapper, Michiel R. Hogerheijde, Ewine F. van Dishoeck, Sean Brittain, Miguel Vioque
Figure caption: Left: ﹩\dot{M}﹩–M disk relationship for our sample of Herbig Ae/Be stars (black points) and the T Tauri stars from Testi et al. (2022; blue points). We have excluded the few sources in the Testi et al. (2022) sample that have M * > 1.5 M ⊙. The black line is the best fit for the Herbig Ae/Be sample, and the blue line is the best fit for the T Tauri sample. The thin black and blue lines are 200 samples of the posterior for the fits to the Herbig Ae/Be and T Tauri points, respectively. Upper limits on the dust mass are shown as leftward-facing triangles, and upper limits on the accretion rate are shown as downward-facing triangles. If both the accretion rate and dust mass measurements are upper limits, the triangle points to the lower left. The dotted gray lines show different disk lifetimes. The Herbig Ae/Be disks are outliers above the already large scatter seen for the lower-mass stars. Right: relationship between the accretion luminosity and the millimeter flux (normalized by the distance).
Paper: The ﹩\dot{M}﹩–M disk Relationship for Herbig Ae/Be Stars: A Lifetime Problem for Disks with Low Masses?
Authors: Sierra L. Grant, Lucas M. Stapper, Michiel R. Hogerheijde, Ewine F. van Dishoeck, Sean Brittain, Miguel Vioque
Figure caption: Left: t disk distribution for T Tauri disks from Testi et al. (2022; blue) and our Herbig Ae/Be sample (black). We have removed any targets from the Testi et al. (2022) sample that have M * > 1.5 M ⊙. Objects with upper limits on ﹩\dot{M}﹩ or M disk are not included. A two-sample Kolmogorov–Smirnov test returns a p-value of 2.7 × 10−7, indicating that the distributions are drawn from different populations. Right: t disk distribution for group I (red) and group II (blue) disks. A two-sample Kolmogorov–Smirnov test returns a p-value of 0.02, indicating that the distributions may be drawn from different populations.
Paper: JWST/NIRCam Coronagraphy of the Young Planet-hosting Debris Disk AU Microscopii
Authors: Kellen Lawson, Joshua E. Schlieder, Jarron M. Leisenring, Ell Bogat, Charles A. Beichman, Geoffrey Bryden, András Gáspár, Tyler D. Groff, Michael W. McElwain, Michael R. Meyer, Thomas Barclay, Per Calissendorff, Matthew De Furio, Marie Ygouf, Anthony Boccaletti, Thomas P. Greene, John Krist, Peter Plavchan, Marcia J. Rieke, Thomas L. Roellig, John Stansberry, John P. Wisniewski, Erick T. Young
Figure caption: A comparison of the surface brightness profiles for the northwestern (NW) and southeastern (SE) extents of the disk for the MCRDI reductions (blue) in magnitudes. In the upper panel, profiles for the convolved disk models (black), whose unconvolved images are perfectly symmetric, are included to highlight effects artificially induced by coronagraph misalignment and by the asymmetry of the PSF itself. In the lower panel, the artificial asymmetry has been corrected by subtracting the model asymmetry measurements of the upper panel from those of the MCRDI measurements. For context, the dashed–dotted purple line shows the expected asymmetry based on the exponential fits to HST/STIS surface brightness profiles for AU Mic’s disk from Schneider et al. (2014). In both panels, error bars are offset slightly in the x-axis direction to improve readability.
Paper: JWST/NIRCam Coronagraphy of the Young Planet-hosting Debris Disk AU Microscopii
Authors: Kellen Lawson, Joshua E. Schlieder, Jarron M. Leisenring, Ell Bogat, Charles A. Beichman, Geoffrey Bryden, András Gáspár, Tyler D. Groff, Michael W. McElwain, Michael R. Meyer, Thomas Barclay, Per Calissendorff, Matthew De Furio, Marie Ygouf, Anthony Boccaletti, Thomas P. Greene, John Krist, Peter Plavchan, Marcia J. Rieke, Thomas L. Roellig, John Stansberry, John P. Wisniewski, Erick T. Young
Figure caption: Surface brightness measurements along the spine of AU Mic’s disk in F356W (solid lines) and F444W (dashed lines) measured in circular apertures (r = 4 pixels = 0.″252) for images produced by three distinct starlight subtraction techniques: MCRDI (blue), RDI/KLIP (orange), and classical RDI (green). The x-axis indicates the stellocentric separation projected onto the assumed disk major axis, with negative values corresponding to the southeastern extent of the disk. The roll-averaged coronagraph transmission profile is displayed as a light gray line (measured at the same locations and using the same aperture size), with values given along the right y-axis. To improve readability, error bars are plotted for alternating surface brightness measurements.
Paper: JWST/NIRCam Coronagraphy of the Young Planet-hosting Debris Disk AU Microscopii
Authors: Kellen Lawson, Joshua E. Schlieder, Jarron M. Leisenring, Ell Bogat, Charles A. Beichman, Geoffrey Bryden, András Gáspár, Tyler D. Groff, Michael W. McElwain, Michael R. Meyer, Thomas Barclay, Per Calissendorff, Matthew De Furio, Marie Ygouf, Anthony Boccaletti, Thomas P. Greene, John Krist, Peter Plavchan, Marcia J. Rieke, Thomas L. Roellig, John Stansberry, John P. Wisniewski, Erick T. Young
Figure caption: Surface brightness profiles for the MCRDI reductions (F356W in blue and F444W in red) presented in a log-log scale and including separations to 6″. The roll-averaged coronagraph transmission profiles are displayed in light gray, with values given along the right y-axis. For both surface brightness and coronagraph transmission, the northwestern (NW) and southeastern (SE) profiles are indicated by solid and dashed lines (respectively). Error bars are excluded to improve readability.
Paper: JWST/NIRCam Coronagraphy of the Young Planet-hosting Debris Disk AU Microscopii
Authors: Kellen Lawson, Joshua E. Schlieder, Jarron M. Leisenring, Ell Bogat, Charles A. Beichman, Geoffrey Bryden, András Gáspár, Tyler D. Groff, Michael W. McElwain, Michael R. Meyer, Thomas Barclay, Per Calissendorff, Matthew De Furio, Marie Ygouf, Anthony Boccaletti, Thomas P. Greene, John Krist, Peter Plavchan, Marcia J. Rieke, Thomas L. Roellig, John Stansberry, John P. Wisniewski, Erick T. Young
Figure caption: Final F444W MCRDI products following the injection of two low-mass companions into observations of AU Mic (see Section 5.1). The images are oriented such that the disk major axis is aligned with the horizontal axis. Left: the final MCRDI image, which has been multiplied by the projected radial separation in units of arcsec to improve the visualization. Right: the SNRE map for the residuals between the MCRDI image and the MCRDI disk model. For both panels, the location of each injected companion is indicated by a white caret marker and annotation. Major and minor axis ticks delineate separation in increments of 1″ and 0.″5, respectively. A linear color stretch is used for both images.
Paper: JWST/NIRCam Coronagraphy of the Young Planet-hosting Debris Disk AU Microscopii
Authors: Kellen Lawson, Joshua E. Schlieder, Jarron M. Leisenring, Ell Bogat, Charles A. Beichman, Geoffrey Bryden, András Gáspár, Tyler D. Groff, Michael W. McElwain, Michael R. Meyer, Thomas Barclay, Per Calissendorff, Matthew De Furio, Marie Ygouf, Anthony Boccaletti, Thomas P. Greene, John Krist, Peter Plavchan, Marcia J. Rieke, Thomas L. Roellig, John Stansberry, John P. Wisniewski, Erick T. Young
Figure caption: Maps of orbit-averaged companion detection probabilities as a function of companion semimajor axis (au) and companion mass (Jupiter masses on the left axis and Earth masses on the right). For the F444W observations, the map indicates detection probabilities for analogs of Jupiter, Saturn, and Neptune (i.e., matching semimajor axis and mass) of 0.73, 0.76, and 0.70, respectively.
Paper: JWST/NIRCam Coronagraphy of the Young Planet-hosting Debris Disk AU Microscopii
Authors: Kellen Lawson, Joshua E. Schlieder, Jarron M. Leisenring, Ell Bogat, Charles A. Beichman, Geoffrey Bryden, András Gáspár, Tyler D. Groff, Michael W. McElwain, Michael R. Meyer, Thomas Barclay, Per Calissendorff, Matthew De Furio, Marie Ygouf, Anthony Boccaletti, Thomas P. Greene, John Krist, Peter Plavchan, Marcia J. Rieke, Thomas L. Roellig, John Stansberry, John P. Wisniewski, Erick T. Young
Figure caption: Measurements of AU Mic’s disk color as described in Section 6. Measurements for the MCRDI disk model (black) are included for both the convolved (solid) and unconvolved (dotted) model images, to provide a qualitative estimate of the effect of the differing PSFs on the measured color. To improve readability, (a) error bars are plotted for every other measurement and (b) points for the three data reductions are offset slightly from one another in the x-axis direction.
Paper: JWST/NIRCam Coronagraphy of the Young Planet-hosting Debris Disk AU Microscopii
Authors: Kellen Lawson, Joshua E. Schlieder, Jarron M. Leisenring, Ell Bogat, Charles A. Beichman, Geoffrey Bryden, András Gáspár, Tyler D. Groff, Michael W. McElwain, Michael R. Meyer, Thomas Barclay, Per Calissendorff, Matthew De Furio, Marie Ygouf, Anthony Boccaletti, Thomas P. Greene, John Krist, Peter Plavchan, Marcia J. Rieke, Thomas L. Roellig, John Stansberry, John P. Wisniewski, Erick T. Young
Figure caption: As Figure 10, but for measurements of differing disk models and with color now encoding the filter (F356W in blue and F444W in red). Solid lines correspond to measurements of the convolved MCRDI model (as the black lines in Figure 10), the dashed–dotted lines are for the same model but assuming the star and coronagraph are perfectly aligned for convolution, and the dotted lines are for the model before convolution.
Paper: JWST/NIRCam Coronagraphy of the Young Planet-hosting Debris Disk AU Microscopii
Authors: Kellen Lawson, Joshua E. Schlieder, Jarron M. Leisenring, Ell Bogat, Charles A. Beichman, Geoffrey Bryden, András Gáspár, Tyler D. Groff, Michael W. McElwain, Michael R. Meyer, Thomas Barclay, Per Calissendorff, Matthew De Furio, Marie Ygouf, Anthony Boccaletti, Thomas P. Greene, John Krist, Peter Plavchan, Marcia J. Rieke, Thomas L. Roellig, John Stansberry, John P. Wisniewski, Erick T. Young
Figure caption: For both rolls of the F356W AU Mic observations: a map showing the vicinity of the star (gold star marker) with each oversampled pixel colored according to the coronagraphic image sample (colored round markers) with which it is paired for model convolution. Solid vertical and horizontal lines denote the boundaries of detector-sampled pixels, while dotted lines delineate the oversampled pixel boundaries. It should be noted that not all of the WebbPSF_ext samples in the grid are ultimately matched to any pixels.
Paper: JWST/NIRCam Coronagraphy of the Young Planet-hosting Debris Disk AU Microscopii
Authors: Kellen Lawson, Joshua E. Schlieder, Jarron M. Leisenring, Ell Bogat, Charles A. Beichman, Geoffrey Bryden, András Gáspár, Tyler D. Groff, Michael W. McElwain, Michael R. Meyer, Thomas Barclay, Per Calissendorff, Matthew De Furio, Marie Ygouf, Anthony Boccaletti, Thomas P. Greene, John Krist, Peter Plavchan, Marcia J. Rieke, Thomas L. Roellig, John Stansberry, John P. Wisniewski, Erick T. Young
Figure caption: Normalized vertical brightness profiles for the F356W images described in Section 7. The profiles are normalized to have the same peak value and are offset along the y-axis according to the major axis position of the slice. Shaded gray regions indicate the 1σ uncertainties on the measurements for the MCRDI profiles. The top panel shows the locations and widths of the six slices in the context of the MCRDI image (which has been multiplied by the projected radial separation for this visualization only).
Paper: The TESS-Keck Survey. XVI. Mass Measurements for 12 Planets in Eight Systems
Authors: Joseph M. Akana Murphy, Natalie M. Batalha, Nicholas Scarsdale, Howard Isaacson, David R. Ciardi, Erica J. Gonzales, Steven Giacalone, Joseph D. Twicken, Anne Dattilo, Tara Fetherolf, Ryan A. Rubenzahl, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Corey Beard, Ashley Chontos, Fei Dai, Malena Rice, Judah Van Zandt, Jack Lubin, Sarah Blunt, Alex S. Polanski, Aida Behmard, Paul A. Dalba, Michelle L. Hill, Lee J. Rosenthal, Casey L. Brinkman, Andrew W. Mayo, Emma V. Turtelboom, Isabel Angelo, Teo Močnik, Mason G. MacDougall, Daria Pidhorodetska, Dakotah Tyler, Molly R. Kosiarek, Rae Holcomb, Emma M. Louden, Lea A. Hirsch, Emily A. Gilbert, Jay Anderson, Jeff A. Valenti
Figure caption: Our joint modeling results for HIP 8152. Left: the photometric model. The top panel shows the PDCSAP light curve as the black points, with the GP used to flatten the light curve plotted as the green line. Triangles mark transits for planets b (blue) and c (orange). The middle panel shows the flattened light curve in black and the best-fitting transit models for planets b and c in blue and orange, respectively. Residuals are shown below. Phase-folded light curves and residuals are shown in the bottom panels for planets b (left) and c (right), with data in 30 minute bins shown in red. The phase-folded best-fitting transit models for each planet are shown as the slightly thicker blue and orange lines, with 25 random posterior draws overplotted as the thinner lines. Right: the RV model. The top panel shows the RV time series with Keck-HIRES data in black and the RV model in blue. Residuals are shown below. Phase-folded RV curves for planets b and c are shown in the bottom panels. Red points are data binned in 0.125 units of orbital phase. The phase-folded best-fitting RV models for each planet are shown as the slightly thicker blue and orange lines, with 25 random posterior draws overplotted as the thinner lines.
Paper: The TESS-Keck Survey. XVI. Mass Measurements for 12 Planets in Eight Systems
Authors: Joseph M. Akana Murphy, Natalie M. Batalha, Nicholas Scarsdale, Howard Isaacson, David R. Ciardi, Erica J. Gonzales, Steven Giacalone, Joseph D. Twicken, Anne Dattilo, Tara Fetherolf, Ryan A. Rubenzahl, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Corey Beard, Ashley Chontos, Fei Dai, Malena Rice, Judah Van Zandt, Jack Lubin, Sarah Blunt, Alex S. Polanski, Aida Behmard, Paul A. Dalba, Michelle L. Hill, Lee J. Rosenthal, Casey L. Brinkman, Andrew W. Mayo, Emma V. Turtelboom, Isabel Angelo, Teo Močnik, Mason G. MacDougall, Daria Pidhorodetska, Dakotah Tyler, Molly R. Kosiarek, Rae Holcomb, Emma M. Louden, Lea A. Hirsch, Emily A. Gilbert, Jay Anderson, Jeff A. Valenti
Figure caption: HD 42813 (left) and HD 6061 (right) are the only two systems where the p-value of either the Spearman or Pearson test (and in their cases, both) was <0.05 for the Keck-HIRES RV residuals and S HK values. In each panel, the Keck-HIRES RVs are shown in blue and a linear least-squares fit to the data is plotted in orange. We note that for HD 42813, we removed the one observation with S HK >0.19 and refit the data, but still find p Spearman and p Pearson are both <0.05. The correlation between the RV residuals and the S HK values suggests that stellar activity might be manifesting itself in the RVs, but we emphasize that p-value testing can be unreliable (e.g., Colquhoun 2014). This test is just one point of reference in our broader investigation into stellar activity contamination in the RVs.
Paper: The TESS-Keck Survey. XVI. Mass Measurements for 12 Planets in Eight Systems
Authors: Joseph M. Akana Murphy, Natalie M. Batalha, Nicholas Scarsdale, Howard Isaacson, David R. Ciardi, Erica J. Gonzales, Steven Giacalone, Joseph D. Twicken, Anne Dattilo, Tara Fetherolf, Ryan A. Rubenzahl, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Corey Beard, Ashley Chontos, Fei Dai, Malena Rice, Judah Van Zandt, Jack Lubin, Sarah Blunt, Alex S. Polanski, Aida Behmard, Paul A. Dalba, Michelle L. Hill, Lee J. Rosenthal, Casey L. Brinkman, Andrew W. Mayo, Emma V. Turtelboom, Isabel Angelo, Teo Močnik, Mason G. MacDougall, Daria Pidhorodetska, Dakotah Tyler, Molly R. Kosiarek, Rae Holcomb, Emma M. Louden, Lea A. Hirsch, Emily A. Gilbert, Jay Anderson, Jeff A. Valenti
Figure caption: AO imaging results for HIP 8152, HD 25463, HD 135694, HD 6061, and TOI-1736 from our observations with Palomar-PHARO and Keck-NIRC2. Contrast curves are shown in black with 1σ error envelopes in purple. The images themselves are shown as the postage stamp insets. HIP 8152, HD 25463, HD 135694, and TOI-1736 all appear single. Keck-NIRC2 observations of HD 6061 were taken in both Br-γ and J-cont, but only the former is shown here. In the image of HD 6061, TIC 600433892 can be seen in the lower-right corner at a separation of ≈3″. TIC 600433892 is fainter than HD 6061 by 6.2 mag in the TESS bandpass, meaning that its dilution of HD 6061 b’s transits is about a 0.1% effect (i.e., much less than the uncertainty on the stellar radius). HD 6061 and TIC 600433892 have consistent distances and proper motions according to Gaia DR3, meaning that the two stars are almost certainly gravitationally bound. At a distance of 67 pc, their on-sky separation of 3″ translates to a sky-projected separation of about 200 au.
Paper: The TESS-Keck Survey. XVI. Mass Measurements for 12 Planets in Eight Systems
Authors: Joseph M. Akana Murphy, Natalie M. Batalha, Nicholas Scarsdale, Howard Isaacson, David R. Ciardi, Erica J. Gonzales, Steven Giacalone, Joseph D. Twicken, Anne Dattilo, Tara Fetherolf, Ryan A. Rubenzahl, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Corey Beard, Ashley Chontos, Fei Dai, Malena Rice, Judah Van Zandt, Jack Lubin, Sarah Blunt, Alex S. Polanski, Aida Behmard, Paul A. Dalba, Michelle L. Hill, Lee J. Rosenthal, Casey L. Brinkman, Andrew W. Mayo, Emma V. Turtelboom, Isabel Angelo, Teo Močnik, Mason G. MacDougall, Daria Pidhorodetska, Dakotah Tyler, Molly R. Kosiarek, Rae Holcomb, Emma M. Louden, Lea A. Hirsch, Emily A. Gilbert, Jay Anderson, Jeff A. Valenti
Figure caption: An example of our simultaneous transit and GP fitting for the second transit of HD 42813 b in Sector 6. The PDCSAP data are shown in black, and data in 30 minute bins are shown in red. The GP prediction across the transit (plus a small global offset fit to the data) is shown as the green dashed line, and the best-fitting transit model is shown as the blue line. We visually inspected each transit across all systems to ensure that the GP prediction did not absorb any of the transit signal.
Paper: The TESS-Keck Survey. XVI. Mass Measurements for 12 Planets in Eight Systems
Authors: Joseph M. Akana Murphy, Natalie M. Batalha, Nicholas Scarsdale, Howard Isaacson, David R. Ciardi, Erica J. Gonzales, Steven Giacalone, Joseph D. Twicken, Anne Dattilo, Tara Fetherolf, Ryan A. Rubenzahl, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Corey Beard, Ashley Chontos, Fei Dai, Malena Rice, Judah Van Zandt, Jack Lubin, Sarah Blunt, Alex S. Polanski, Aida Behmard, Paul A. Dalba, Michelle L. Hill, Lee J. Rosenthal, Casey L. Brinkman, Andrew W. Mayo, Emma V. Turtelboom, Isabel Angelo, Teo Močnik, Mason G. MacDougall, Daria Pidhorodetska, Dakotah Tyler, Molly R. Kosiarek, Rae Holcomb, Emma M. Louden, Lea A. Hirsch, Emily A. Gilbert, Jay Anderson, Jeff A. Valenti
Figure caption: GLS periodograms for HIP 8152 are shown in black. The vertical blue and orange lines mark the orbital periods of planets b and c, respectively. The dashed horizontal line indicates the 0.1% FAP threshold (Baluev 2008). We compute the GLS periodogram of the RV window function with a minimum period slightly longer than 1 day to avoid the strong nightly alias, which otherwise skews the y-axis scale.
Paper: The TESS-Keck Survey. XVI. Mass Measurements for 12 Planets in Eight Systems
Authors: Joseph M. Akana Murphy, Natalie M. Batalha, Nicholas Scarsdale, Howard Isaacson, David R. Ciardi, Erica J. Gonzales, Steven Giacalone, Joseph D. Twicken, Anne Dattilo, Tara Fetherolf, Ryan A. Rubenzahl, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Corey Beard, Ashley Chontos, Fei Dai, Malena Rice, Judah Van Zandt, Jack Lubin, Sarah Blunt, Alex S. Polanski, Aida Behmard, Paul A. Dalba, Michelle L. Hill, Lee J. Rosenthal, Casey L. Brinkman, Andrew W. Mayo, Emma V. Turtelboom, Isabel Angelo, Teo Močnik, Mason G. MacDougall, Daria Pidhorodetska, Dakotah Tyler, Molly R. Kosiarek, Rae Holcomb, Emma M. Louden, Lea A. Hirsch, Emily A. Gilbert, Jay Anderson, Jeff A. Valenti
Figure caption: A 2MASS JHK  s  color–color diagram. The dwarf branch, giant branch, and brown dwarf loci are shown with green, blue, and red hashes, respectively. Black dashed lines represent the direction of reddening induced by extinction (A  V ). HD 6061 and TIC 600433892 are overplotted as the black circles with 1σ error bars. TIC 600433892 is consistent with being an M4/5V dwarf. We find that HD 6061 is consistent with being a G0 dwarf, which agrees with the classification from Cannon & Pickering (1993).
Paper: The TESS-Keck Survey. XVI. Mass Measurements for 12 Planets in Eight Systems
Authors: Joseph M. Akana Murphy, Natalie M. Batalha, Nicholas Scarsdale, Howard Isaacson, David R. Ciardi, Erica J. Gonzales, Steven Giacalone, Joseph D. Twicken, Anne Dattilo, Tara Fetherolf, Ryan A. Rubenzahl, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Corey Beard, Ashley Chontos, Fei Dai, Malena Rice, Judah Van Zandt, Jack Lubin, Sarah Blunt, Alex S. Polanski, Aida Behmard, Paul A. Dalba, Michelle L. Hill, Lee J. Rosenthal, Casey L. Brinkman, Andrew W. Mayo, Emma V. Turtelboom, Isabel Angelo, Teo Močnik, Mason G. MacDougall, Daria Pidhorodetska, Dakotah Tyler, Molly R. Kosiarek, Rae Holcomb, Emma M. Louden, Lea A. Hirsch, Emily A. Gilbert, Jay Anderson, Jeff A. Valenti
Figure caption: The RV portion of a joint model for HIP 9618 that includes the CAFE, HARPS-N, and SOPHIE RVs from O23 in addition to the APF-Levy and Keck-HIRES data from this work. The figure description is the same as for Figure 6. This RV model also includes a curvature term in addition to the linear trend, in order to mimic the adopted solution from O23. The results of this model are consistent with our joint model of the APF-Levy and Keck-HIRES RVs alone.