adsabs/AstroCLIMB huggingface dataset:
Paper: Stable Fiber-illumination for Extremely Precise Radial Velocities with NEID
Authors: Shubham Kanodia, Andrea S. J. Lin, Emily Lubar, Samuel Halverson, Suvrath Mahadevan, Chad F. Bender, Sarah E. Logsdon, Lawrence W. Ramsey, Joe P. Ninan, Gumundur Stefánsson, Andrew Monson, Christian Schwab, Arpita Roy, Leonardo A. Paredes, Eli Golub, Jesus Higuera, Jessica Klusmeyer, William McBride, Cullen Blake, Scott A. Diddams, Fabien Grisé, Arvind F. Gupta, Fred Hearty, Michael W. McElwain, Jayadev Rajagopal, Paul Robertson, Ryan C. Terrien
Figure caption: Far-field scrambling: on-sky testing of far-field scrambling performance. Error bars reflect photon-noise estimates only. HD141004 was observed with NEID under “standard” (full) mirror illumination (red circles), with one half of the WIYN primary mirror vignetted (orange diamonds), and the the other half vignetted (green squares). To maintain relatively constant signal-to-noise in the stellar spectra the exposure lengths were increased by ∼2×  with half of the telescope pupil obscured. Within expected stellar jitter and photon errors, we do not measure a statistically significant offset between the three clusters of points.
Paper: Stable Fiber-illumination for Extremely Precise Radial Velocities with NEID
Authors: Shubham Kanodia, Andrea S. J. Lin, Emily Lubar, Samuel Halverson, Suvrath Mahadevan, Chad F. Bender, Sarah E. Logsdon, Lawrence W. Ramsey, Joe P. Ninan, Gumundur Stefánsson, Andrew Monson, Christian Schwab, Arpita Roy, Leonardo A. Paredes, Eli Golub, Jesus Higuera, Jessica Klusmeyer, William McBride, Cullen Blake, Scott A. Diddams, Fabien Grisé, Arvind F. Gupta, Fred Hearty, Michael W. McElwain, Jayadev Rajagopal, Paul Robertson, Ryan C. Terrien
Figure caption: Near-field scrambling: measured differential drift between the NEID Science (SCI) and Calibration (CAL) fibers during the near-field scrambling test using the telescope fiber port. The cartoon above shows the sequence of offsets applied to the port Calibration fiber (yellow) as the image is stepped across the Science fiber (blue). The NEID etalon calibration source was used to alternately illuminate both fibers during this test. Upon subtracting the intrinsic instrumental drift (measured using the Calibration fiber, red points), the residual Science fiber drifts (green points) are consistent with a near-field scrambling gain of over 10,000.
Paper: Stable Fiber-illumination for Extremely Precise Radial Velocities with NEID
Authors: Shubham Kanodia, Andrea S. J. Lin, Emily Lubar, Samuel Halverson, Suvrath Mahadevan, Chad F. Bender, Sarah E. Logsdon, Lawrence W. Ramsey, Joe P. Ninan, Gumundur Stefánsson, Andrew Monson, Christian Schwab, Arpita Roy, Leonardo A. Paredes, Eli Golub, Jesus Higuera, Jessica Klusmeyer, William McBride, Cullen Blake, Scott A. Diddams, Fabien Grisé, Arvind F. Gupta, Fred Hearty, Michael W. McElwain, Jayadev Rajagopal, Paul Robertson, Ryan C. Terrien
Figure caption: Block diagram showing the setup used to measure the (a) focal ratio degradation and (b) throughput for the test fiber. We use a point-source microscope to ensure that the test fiber face is normal to the principal axis of the input beam, where the input light (Thorlabs TED4015 with a 635 nm pig-tailed SMF fiber output with ∼10 nm bandwidth) is focused on the fiber at a deterministic f/# using a motorized iris. The beam is centered on the fiber face by translating the face using an XYZ stage. The throughput was performed as a differential measurement using a power meter.
Paper: Stable Fiber-illumination for Extremely Precise Radial Velocities with NEID
Authors: Shubham Kanodia, Andrea S. J. Lin, Emily Lubar, Samuel Halverson, Suvrath Mahadevan, Chad F. Bender, Sarah E. Logsdon, Lawrence W. Ramsey, Joe P. Ninan, Gumundur Stefánsson, Andrew Monson, Christian Schwab, Arpita Roy, Leonardo A. Paredes, Eli Golub, Jesus Higuera, Jessica Klusmeyer, William McBride, Cullen Blake, Scott A. Diddams, Fabien Grisé, Arvind F. Gupta, Fred Hearty, Michael W. McElwain, Jayadev Rajagopal, Paul Robertson, Ryan C. Terrien
Figure caption: NEID fused-silica puck effectively functions as the NEID slit with three HR fibers (Calibration, Science, and Sky) and two HE fibers (Science and Sky). (a) SolidWorks rendering of the puck showing the five fibers, and (b) the NEID puck after potting the fibers and polishing to the final finish.
Paper: SPar: Estimating Stellar Parameters from Multiband Photometries with Empirical Stellar Libraries
Authors: Mingxu Sun, Bingqiu Chen, Helong Guo, He Zhao, Ming Yang, Wenyuan Cui
Figure caption: Comparison of T eff (left) and [Fe/H] (right) of this work with LAMOST (top), APOGEE (middle), and GALAH (bottom). For every panel, the top half shows the consistency of T eff or [Fe/H], and the bottom half shows the differences change with T eff or [Fe/H] of this work. The black and red line in the top and bottom half panel are the equal and zero lines.
Paper: SPar: Estimating Stellar Parameters from Multiband Photometries with Empirical Stellar Libraries
Authors: Mingxu Sun, Bingqiu Chen, Helong Guo, He Zhao, Ming Yang, Wenyuan Cui
Figure caption: Comparison of final parameters (T eff (top-left), [Fe/H] (top-right), M G (bottom-left), E(G BP − G RP) (bottom-middle), and distance (bottom-right)) of this work with parameters from 100 walkers and 1000 steps chains. The blue dashed line is the equal line.
Paper: SPar: Estimating Stellar Parameters from Multiband Photometries with Empirical Stellar Libraries
Authors: Mingxu Sun, Bingqiu Chen, Helong Guo, He Zhao, Ming Yang, Wenyuan Cui
Figure caption: Histograms of the differences between our predicted absolute magnitudes of stars and those from the PARSEC isochrones (Bressan et al. 2012). The mean and dispersion values of the differences are labeled in each panel.
Paper: SPar: Estimating Stellar Parameters from Multiband Photometries with Empirical Stellar Libraries
Authors: Mingxu Sun, Bingqiu Chen, Helong Guo, He Zhao, Ming Yang, Wenyuan Cui
Figure caption: Comparison of simulated magnitude and parallax based on the MCMC results with the observed data. N is the total source number, and μ e and σ e are the median and standard deviation of differences after 3σ elimination.
Paper: SPar: Estimating Stellar Parameters from Multiband Photometries with Empirical Stellar Libraries
Authors: Mingxu Sun, Bingqiu Chen, Helong Guo, He Zhao, Ming Yang, Wenyuan Cui
Figure caption: The changes of ΔT eff (left) and Δ[Fe/H] (right) with E(G BP − G RP) of LAMOST (top), APOGEE (middle), and GALAH (bottom) stars. The red point and error bar is the median and standard deviation in every 0.1  mag bin. The black line is the zero line.
Paper: SPar: Estimating Stellar Parameters from Multiband Photometries with Empirical Stellar Libraries
Authors: Mingxu Sun, Bingqiu Chen, Helong Guo, He Zhao, Ming Yang, Wenyuan Cui
Figure caption: The same as Figure 5, but for E(G BP − G RP) and distance. The black line is the equal line.
Paper: SPar: Estimating Stellar Parameters from Multiband Photometries with Empirical Stellar Libraries
Authors: Mingxu Sun, Bingqiu Chen, Helong Guo, He Zhao, Ming Yang, Wenyuan Cui
Figure caption: The same as Figure 5, but for M G of all samples (left), high-precision parallax samples (middle), and low-precision parallax samples (right). The black line is the equal line.
Paper: SPar: Estimating Stellar Parameters from Multiband Photometries with Empirical Stellar Libraries
Authors: Mingxu Sun, Bingqiu Chen, Helong Guo, He Zhao, Ming Yang, Wenyuan Cui
Figure caption: The distribution of χ 2. The black dashed line is χ 2 = 10 line.
Paper: Iron-rich Metal-poor Stars and the Astrophysics of Thermonuclear Events Observationally Classified as Type Ia Supernovae. I. Establishing the Connection
Authors: Henrique Reggiani, Kevin C. Schlaufman, Andrew R. Casey
Figure caption: Predicted stable nucleosynthetic yields for thermonuclear explosions that produce M Fe ≥ 0.1 M ⊙ with varying progenitor systems and explosion mechanisms. Each rectangle represents the full range of predicted elemental abundances after marginalizing over the parameters that define each progenitor system and explosion mechanism. Top: predicted stable elemental abundances produced by delayed detonations. Middle: predicted stable elemental abundances produced by double detonations. Bottom: predicted stable elemental abundances produced by deflagrations and direct collisions. Regardless of the progenitor system or explosion mechanism, relative to iron the elemental abundances of carbon, nitrogen, oxygen, fluorine, neon, sodium, magnesium, aluminum, chlorine, potassium, cobalt, copper, and zinc are always subsolar. From this list, we use in our IRMP star selection sodium, magnesium, and cobalt because those abundances are usually straightforward to infer in the photospheres of metal-poor giants.
Paper: EMU Detection of a Large and Low Surface Brightness Galactic SNR G288.8–6.3
Authors: Miroslav D. Filipović, Shi Dai, Bojan Arbutina, Natasha Hurley-Walker, Robert Brose, Werner Becker, Hidetoshi Sano, Dejan Urošević, T. H. Jarrett, Andrew M. Hopkins, Rami Z. E. Alsaberi, R. Alsulami, Cristobal Bordiu, Brianna Ball, Filomena Bufano, Christopher Burger-Scheidlin, Evan Crawford, Jayanne English, Frank Haberl, Adriano Ingallinera, Anna D. Kapinska, Patrick J. Kavanagh, Bärbel S. Koribalski, Roland Kothes, Sanja Lazarević, Jonathan Mackey, Gavin Rowell, Denis Leahy, Sara Loru, Peter J. Macgregor, Luciano Nicastro, Ray P. Norris, Simone Riggi, Manami Sasaki, Milorad Stupar, Corrado Trigilio, Grazia Umana, Tessa Vernstrom, Branislav Vukotić
Figure caption: ASKAP image of the Galactic SNR G288.8–6.3 at 943 MHz. (a) The publicly released image with a synthesized beam of 15″ × 15″. (b) An extended and reprocessed image that is convolved to the resolution of 30″ × 30″. (c) To enhance the diffuse emission, we show panel (b) scaled with a 90″ box using the multiresolution filtering method of Rudnick (2002). The magenta ellipse marks the position of gamma-ray source 4FGL J1028.7–6431c (68% containment), while the cyan plus sign marks the position of nearby radio pulsar J1036–6559. The yellow rectangular box marks the area covered in Figure 5. The grayscale (in Jy beam−1) is displayed on the right side, with panels (a) and (b) using a logarithmic scale and panel (c) using a linear scale.
Paper: EMU Detection of a Large and Low Surface Brightness Galactic SNR G288.8–6.3
Authors: Miroslav D. Filipović, Shi Dai, Bojan Arbutina, Natasha Hurley-Walker, Robert Brose, Werner Becker, Hidetoshi Sano, Dejan Urošević, T. H. Jarrett, Andrew M. Hopkins, Rami Z. E. Alsaberi, R. Alsulami, Cristobal Bordiu, Brianna Ball, Filomena Bufano, Christopher Burger-Scheidlin, Evan Crawford, Jayanne English, Frank Haberl, Adriano Ingallinera, Anna D. Kapinska, Patrick J. Kavanagh, Bärbel S. Koribalski, Roland Kothes, Sanja Lazarević, Jonathan Mackey, Gavin Rowell, Denis Leahy, Sara Loru, Peter J. Macgregor, Luciano Nicastro, Ray P. Norris, Simone Riggi, Manami Sasaki, Milorad Stupar, Corrado Trigilio, Grazia Umana, Tessa Vernstrom, Branislav Vukotić
Figure caption: Radio surface brightness−diameter diagram for SNRs at a frequency of 1 GHz (black triangles), obtained from numerical simulations (Pavlović et al. 2018, their Figure 3). Our newly detected SNR G288.8–6.3 is marked with a red star in the lower right corner, while Cassiopeia A is shown with an open triangle. The open circle represents the youngest Galactic SNR, G1.9+0.3 (Luken et al. 2020). Numbers represent the following SNRs: (1) CTB 37A, (2) Kes 97, (3) CTB 37B, and (4) G65.1+0.6.
Paper: EMU Detection of a Large and Low Surface Brightness Galactic SNR G288.8–6.3
Authors: Miroslav D. Filipović, Shi Dai, Bojan Arbutina, Natasha Hurley-Walker, Robert Brose, Werner Becker, Hidetoshi Sano, Dejan Urošević, T. H. Jarrett, Andrew M. Hopkins, Rami Z. E. Alsaberi, R. Alsulami, Cristobal Bordiu, Brianna Ball, Filomena Bufano, Christopher Burger-Scheidlin, Evan Crawford, Jayanne English, Frank Haberl, Adriano Ingallinera, Anna D. Kapinska, Patrick J. Kavanagh, Bärbel S. Koribalski, Roland Kothes, Sanja Lazarević, Jonathan Mackey, Gavin Rowell, Denis Leahy, Sara Loru, Peter J. Macgregor, Luciano Nicastro, Ray P. Norris, Simone Riggi, Manami Sasaki, Milorad Stupar, Corrado Trigilio, Grazia Umana, Tessa Vernstrom, Branislav Vukotić
Figure caption: 2.°5 × 2.°5 region surrounding G288.8–6.3 at (a) MWA 200 MHz, (b) CHIPASS 1400 MHz, and (c) S-PASS 2300 MHz after source and background subtraction as described in Section 4.1. The contours in panel (c) show the total linear polarization measured in S-PASS, in steps of 4× the local rms noise, 38 μJy beam−1. The FWHM of the point-spread function is shown as a solid black ellipse in the lower left corner of each panel.
Paper: EMU Detection of a Large and Low Surface Brightness Galactic SNR G288.8–6.3
Authors: Miroslav D. Filipović, Shi Dai, Bojan Arbutina, Natasha Hurley-Walker, Robert Brose, Werner Becker, Hidetoshi Sano, Dejan Urošević, T. H. Jarrett, Andrew M. Hopkins, Rami Z. E. Alsaberi, R. Alsulami, Cristobal Bordiu, Brianna Ball, Filomena Bufano, Christopher Burger-Scheidlin, Evan Crawford, Jayanne English, Frank Haberl, Adriano Ingallinera, Anna D. Kapinska, Patrick J. Kavanagh, Bärbel S. Koribalski, Roland Kothes, Sanja Lazarević, Jonathan Mackey, Gavin Rowell, Denis Leahy, Sara Loru, Peter J. Macgregor, Luciano Nicastro, Ray P. Norris, Simone Riggi, Manami Sasaki, Milorad Stupar, Corrado Trigilio, Grazia Umana, Tessa Vernstrom, Branislav Vukotić
Figure caption: Radio flux densities as a function of frequency. A power-law fit based on flux density measurements (blue points) from MWA, CHIPASS, and S-PASS surveys with S 1 GHz = 10.92 ± 0.06 Jy and α = − 0.41 ± 0.12 is shown with a green line. Two orange points are flux density measurements from ASKAP and PMN surveys, and they are not included in the spectral index estimate.
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 HD 6061. The figure description is the same as for Figure 7. The period of the GP used to model stellar activity in the RVs is marked with the red vertical line, and its first harmonic is marked with the light-red line.
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 HD 6061. The figure description is the same as for Figure 6, save for the RV model (right), which also shows the GP model of stellar activity. The combined Keplerian plus GP predictions for Keck-HIRES and APF-Levy are shown in blue, with 1σ error envelopes in gray and green, respectively.
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 TOI-1736. The figure description is the same as for Figure 6. The dashed gray line in the top panel of the RV figure represents the linear RV trend detected in the system.
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 HD 135694. The figure description is the same as for Figure 7.
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 9618. The figure description is the same as for Figure 7.
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 TOI-1736. The figure description is the same as for Figure 7. The dashed vertical line for planet c indicates that it is nontransiting.
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 9618. The figure description is the same as for Figure 6.
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 TOI-669. The figure description is the same as for Figure 7.
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 HD 135694. The figure description is the same as for Figure 6.