adsabs/AstroCLIMB huggingface dataset:
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 of the HD 25463 TESS photometry and RVs where the APF-Levy RVs are measured using the default Doppler pipeline (Howard et al. 2010) as opposed to the iGrand reduction pipeline. This figure is only included for comparison with Figure 15 and the planet properties listed in the phase-folded panels should not be used. The figure description is the same as for Figure 6. The default APF-Levy RVs show unreasonably large scatter, which is a possible symptom of the star’s rapid rotation. Mass estimates for planets b and c are consistent with the results of our adopted model, which uses the iGrand APF-Levy velocities (Figure 15). The results of the photometry portion of this joint model (not shown here for brevity) are entirely consistent with those of the model shown on the left in Figure 15—because both the model here and in Figure 15 assume circular orbits for the planets, there is minimal information sharing between the photometry and RV components (for circular orbits, only the planet’s orbital period and time of inferior conjunction, both of which are largely determined by the transits, are shared between the photometry and RV models). As such, we would expect the photometric model results to be essentially the same regardless of which APF-Levy velocities are used. Since they are not listed in an associated table of properties, for use in conjunction with the “HD 25463 Default” RVs in Table 5, the instrumental offsets and jitter terms for this model are: γ APF = − 7.56 ± 1.95 m s−1, ﹩{\gamma }_{\mathrm{HIRES}}=-1.99\pm 0.81﹩ m s−1, σ APF = 19.97 ± 0.03 m s−1 (which would be larger if not for the joint model’s prior on instrumental RV jitter that enforces a maximum of 20 m s−1), and ﹩{\sigma }_{\mathrm{HIRES}}=7.31\pm 0.61﹩ m s−1.
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 HD 25463 RVs. Keck-HIRES RVs are shown as the black circles, the default pipeline’s APF-Levy RVs are shown as the green diamonds, and the iGrand pipeline’s APF-Levy RVs are shown as the orange diamonds. The default APF-Levy RVs show scatter that is seemingly inconsistent with the astrophysical jitter when compared to contemporaneous Keck-HIRES RVs. The iGrand reduction method seems to mitigate these systematics.
Paper: The Extreme Stellar-signals Project. III. Combining Solar Data from HARPS, HARPS-N, EXPRES, and NEID
Authors: Lily L. Zhao, Xavier Dumusque, Eric B. Ford, Joe Llama, Annelies Mortier, Megan Bedell, Khaled Al Moulla, Chad F. Bender, Cullen H. Blake, John M. Brewer, Andrew Collier Cameron, Rosario Cosentino, Pedro Figueira, Debra A. Fischer, Adriano Ghedina, Manuel Gonzalez, Samuel Halverson, Shubham Kanodia, David W. Latham, Andrea S. J. Lin, Gaspare Lo Curto, Marcello Lodi, Sarah E. Logsdon, Christophe Lovis, Suvrath Mahadevan, Andrew Monson, Joe P. Ninan, Francesco Pepe, Rachael M. Roettenbacher, Arpita Roy, Nuno C. Santos, Christian Schwab, Guđmundur Stefánsson, Andrew E. Szymkowiak, Ryan C. Terrien, Stephane Udry, Sam A. Weiss, François Wildi, Thibault Wildi, Jason T. Wright
Figure caption: Left: day-to-day offsets relative to other instruments. Each subplot shows the day-to-day offsets for the instrument specified in the y-axis label as calculated relative to the other three instruments. A point is shown for each day in which both instruments have at least one overlapping binned RV. Days for which there exist offsets measured against two or more instruments are shown as filled-in circular points; days for which there only exists one comparison are shown as outlines. It should be noted that the expected error due to binning for each point is shown as an error bar, but all error bars lie interior to each point, suggesting that binning error is not the dominant source of uncertainty. The total number of days for which an offset was calculated across all three comparisons as well as the rms of all offsets are written on the right of each subplot. Right: stacked, horizontal histograms of the relative day-to-day offsets calculated for each instrument. The resulting distribution of comparisons against each of the three instruments is stacked on top of each other. In other words, the height of a multicolored bar is the frequency of that bin’s values across the comparison with multiple instruments.
Paper: The Extreme Stellar-signals Project. III. Combining Solar Data from HARPS, HARPS-N, EXPRES, and NEID
Authors: Lily L. Zhao, Xavier Dumusque, Eric B. Ford, Joe Llama, Annelies Mortier, Megan Bedell, Khaled Al Moulla, Chad F. Bender, Cullen H. Blake, John M. Brewer, Andrew Collier Cameron, Rosario Cosentino, Pedro Figueira, Debra A. Fischer, Adriano Ghedina, Manuel Gonzalez, Samuel Halverson, Shubham Kanodia, David W. Latham, Andrea S. J. Lin, Gaspare Lo Curto, Marcello Lodi, Sarah E. Logsdon, Christophe Lovis, Suvrath Mahadevan, Andrew Monson, Joe P. Ninan, Francesco Pepe, Rachael M. Roettenbacher, Arpita Roy, Nuno C. Santos, Christian Schwab, Guđmundur Stefánsson, Andrew E. Szymkowiak, Ryan C. Terrien, Stephane Udry, Sam A. Weiss, François Wildi, Thibault Wildi, Jason T. Wright
Figure caption: Top: histograms of the residuals between one instrument’s binned RVs against another instrument’s binned RVs. The title of each subplot details the two instruments being compared (where the binned RVs of the second instrument listed are subtracted from the binned RVs of the first instrument). The total number of overlapping binned RVs across the entire month of shared data is given at the top of each subplot, followed by the rms of the residuals. Bottom: Comparison of one instrument’s binned RVs (y-axis) against the binned RVs of the other three instruments (x-axis). A point is shown for each binned time stamp at which both instruments have a binned RV. The corresponding Pearson correlation coefficient, ρ, for each pairwise comparison is given in the top left corner. Values of ρ closer to 1 indicate more significantly positively correlated data.
Paper: The Extreme Stellar-signals Project. III. Combining Solar Data from HARPS, HARPS-N, EXPRES, and NEID
Authors: Lily L. Zhao, Xavier Dumusque, Eric B. Ford, Joe Llama, Annelies Mortier, Megan Bedell, Khaled Al Moulla, Chad F. Bender, Cullen H. Blake, John M. Brewer, Andrew Collier Cameron, Rosario Cosentino, Pedro Figueira, Debra A. Fischer, Adriano Ghedina, Manuel Gonzalez, Samuel Halverson, Shubham Kanodia, David W. Latham, Andrea S. J. Lin, Gaspare Lo Curto, Marcello Lodi, Sarah E. Logsdon, Christophe Lovis, Suvrath Mahadevan, Andrew Monson, Joe P. Ninan, Francesco Pepe, Rachael M. Roettenbacher, Arpita Roy, Nuno C. Santos, Christian Schwab, Guđmundur Stefánsson, Andrew E. Szymkowiak, Ryan C. Terrien, Stephane Udry, Sam A. Weiss, François Wildi, Thibault Wildi, Jason T. Wright
Figure caption: Top row: per-exposure solar S/N at the blaze peak of every échelle order for a representative observation from each instrument. Black vertical lines mark the wavelengths for which the average S/N is reported in Table 1. We note that NEID’s wavelength range extends further red beyond the edge of the plot. Bottom row: difference between the wavelength of an instrument’s blaze peak, λ peak, for each order. From left to right, HARPS-N, HARPS, and NEID are compared to the blaze peak wavelength of EXPRES. For HARPS-N and HARPS, the λ peak of each order falls on average within 2 Å of the EXPRES λ peak; between NEID and EXPRES, the λ peak is on average within 7 Å.
Paper: The Extreme Stellar-signals Project. III. Combining Solar Data from HARPS, HARPS-N, EXPRES, and NEID
Authors: Lily L. Zhao, Xavier Dumusque, Eric B. Ford, Joe Llama, Annelies Mortier, Megan Bedell, Khaled Al Moulla, Chad F. Bender, Cullen H. Blake, John M. Brewer, Andrew Collier Cameron, Rosario Cosentino, Pedro Figueira, Debra A. Fischer, Adriano Ghedina, Manuel Gonzalez, Samuel Halverson, Shubham Kanodia, David W. Latham, Andrea S. J. Lin, Gaspare Lo Curto, Marcello Lodi, Sarah E. Logsdon, Christophe Lovis, Suvrath Mahadevan, Andrew Monson, Joe P. Ninan, Francesco Pepe, Rachael M. Roettenbacher, Arpita Roy, Nuno C. Santos, Christian Schwab, Guđmundur Stefánsson, Andrew E. Szymkowiak, Ryan C. Terrien, Stephane Udry, Sam A. Weiss, François Wildi, Thibault Wildi, Jason T. Wright
Figure caption: Residuals between binned RVs across all 29 days phase-folded to UTC time of day. Each subplot shows the residuals between binned RVs of the instrument specified in the y-axis label and the other three instruments. A point is shown for each binned time stamp at which both instruments have a binned RV. Of particular interest are features traced by the residuals from multiple instruments, which lends confidence to the feature and helps diagnose its origin.
Paper: The Extreme Stellar-signals Project. III. Combining Solar Data from HARPS, HARPS-N, EXPRES, and NEID
Authors: Lily L. Zhao, Xavier Dumusque, Eric B. Ford, Joe Llama, Annelies Mortier, Megan Bedell, Khaled Al Moulla, Chad F. Bender, Cullen H. Blake, John M. Brewer, Andrew Collier Cameron, Rosario Cosentino, Pedro Figueira, Debra A. Fischer, Adriano Ghedina, Manuel Gonzalez, Samuel Halverson, Shubham Kanodia, David W. Latham, Andrea S. J. Lin, Gaspare Lo Curto, Marcello Lodi, Sarah E. Logsdon, Christophe Lovis, Suvrath Mahadevan, Andrew Monson, Joe P. Ninan, Francesco Pepe, Rachael M. Roettenbacher, Arpita Roy, Nuno C. Santos, Christian Schwab, Guđmundur Stefánsson, Andrew E. Szymkowiak, Ryan C. Terrien, Stephane Udry, Sam A. Weiss, François Wildi, Thibault Wildi, Jason T. Wright
Figure caption: The time stamps of observations from each instrument as a function of time of day. Top: airmass of the Sun in June as a function of UTC time of day as seen from each of the four instruments. The EXPRES and NEID curves largely overlap. The analysis presented here uses only data taken at an airmass lower than 2.2 (marked by the horizontal black line). Bottom: Time stamps of observations from each instrument for each day (y-axis, increasing top to bottom) and UTC time of day (x-axis). This layout highlights the cadence of each time series as well as the times at which observations from different instruments overlap or when there are gaps in the observations. To help interpret UTC time of day, the local time at each instrument’s location is given on separate axes below this plot. (Because EXPRES and NEID are located in the same time zone, they share a local time axis that is therefore colored yellow and orange.)
Paper: The Extreme Stellar-signals Project. III. Combining Solar Data from HARPS, HARPS-N, EXPRES, and NEID
Authors: Lily L. Zhao, Xavier Dumusque, Eric B. Ford, Joe Llama, Annelies Mortier, Megan Bedell, Khaled Al Moulla, Chad F. Bender, Cullen H. Blake, John M. Brewer, Andrew Collier Cameron, Rosario Cosentino, Pedro Figueira, Debra A. Fischer, Adriano Ghedina, Manuel Gonzalez, Samuel Halverson, Shubham Kanodia, David W. Latham, Andrea S. J. Lin, Gaspare Lo Curto, Marcello Lodi, Sarah E. Logsdon, Christophe Lovis, Suvrath Mahadevan, Andrew Monson, Joe P. Ninan, Francesco Pepe, Rachael M. Roettenbacher, Arpita Roy, Nuno C. Santos, Christian Schwab, Guđmundur Stefánsson, Andrew E. Szymkowiak, Ryan C. Terrien, Stephane Udry, Sam A. Weiss, François Wildi, Thibault Wildi, Jason T. Wright
Figure caption: Binned RVs as a function of UTC time of day. We show here the four days for which there were the greatest number of overlapping points between all instruments. Error bars for each binned RV are derived empirically, as described in Section 3. A different RV offset is applied for each instrument for each day; the offset is calculated as the median of the binned RVs for that instrument taken on the day in question. Features that are traced by more than one instrument are most likely solar in nature rather than due to instrument-specific systematics.
Paper: The Extreme Stellar-signals Project. III. Combining Solar Data from HARPS, HARPS-N, EXPRES, and NEID
Authors: Lily L. Zhao, Xavier Dumusque, Eric B. Ford, Joe Llama, Annelies Mortier, Megan Bedell, Khaled Al Moulla, Chad F. Bender, Cullen H. Blake, John M. Brewer, Andrew Collier Cameron, Rosario Cosentino, Pedro Figueira, Debra A. Fischer, Adriano Ghedina, Manuel Gonzalez, Samuel Halverson, Shubham Kanodia, David W. Latham, Andrea S. J. Lin, Gaspare Lo Curto, Marcello Lodi, Sarah E. Logsdon, Christophe Lovis, Suvrath Mahadevan, Andrew Monson, Joe P. Ninan, Francesco Pepe, Rachael M. Roettenbacher, Arpita Roy, Nuno C. Santos, Christian Schwab, Guđmundur Stefánsson, Andrew E. Szymkowiak, Ryan C. Terrien, Stephane Udry, Sam A. Weiss, François Wildi, Thibault Wildi, Jason T. Wright
Figure caption: Observed RVs from HARPS-N, HARPS, EXPRES, and NEID. DRP RVs (i.e., not binned RVs) are shown over two hours on 2021 May 31 from UTC 17:00 to UTC 19:15. A separate RV offset, calculated as the median of all RVs from that instrument taken on the day, has been applied to each instrument. The x-axis is given in minutes from UTC 17:00 with minor tick marks every 5 minutes (which is close to the ﹩{\nu }_{\max }﹩ for the Sun). All four instruments trace similar short-term RV variations.
Paper: The Extreme Stellar-signals Project. III. Combining Solar Data from HARPS, HARPS-N, EXPRES, and NEID
Authors: Lily L. Zhao, Xavier Dumusque, Eric B. Ford, Joe Llama, Annelies Mortier, Megan Bedell, Khaled Al Moulla, Chad F. Bender, Cullen H. Blake, John M. Brewer, Andrew Collier Cameron, Rosario Cosentino, Pedro Figueira, Debra A. Fischer, Adriano Ghedina, Manuel Gonzalez, Samuel Halverson, Shubham Kanodia, David W. Latham, Andrea S. J. Lin, Gaspare Lo Curto, Marcello Lodi, Sarah E. Logsdon, Christophe Lovis, Suvrath Mahadevan, Andrew Monson, Joe P. Ninan, Francesco Pepe, Rachael M. Roettenbacher, Arpita Roy, Nuno C. Santos, Christian Schwab, Guđmundur Stefánsson, Andrew E. Szymkowiak, Ryan C. Terrien, Stephane Udry, Sam A. Weiss, François Wildi, Thibault Wildi, Jason T. Wright
Figure caption: Solar RVs from HARPS-N, HARPS, EXPRES, and NEID. Observed RVs are shown as black points; colored points represent the RVs binned to shared time stamps with an interval of five minutes throughout a day. The color assigned to the data for each instrument is consistent throughout this work. The bottom most subplot overlays the binned RVs from all instruments (with a separate offset applied to each instrument). All instruments trace similar long-term RV variations.
Paper: The Extreme Stellar-signals Project. III. Combining Solar Data from HARPS, HARPS-N, EXPRES, and NEID
Authors: Lily L. Zhao, Xavier Dumusque, Eric B. Ford, Joe Llama, Annelies Mortier, Megan Bedell, Khaled Al Moulla, Chad F. Bender, Cullen H. Blake, John M. Brewer, Andrew Collier Cameron, Rosario Cosentino, Pedro Figueira, Debra A. Fischer, Adriano Ghedina, Manuel Gonzalez, Samuel Halverson, Shubham Kanodia, David W. Latham, Andrea S. J. Lin, Gaspare Lo Curto, Marcello Lodi, Sarah E. Logsdon, Christophe Lovis, Suvrath Mahadevan, Andrew Monson, Joe P. Ninan, Francesco Pepe, Rachael M. Roettenbacher, Arpita Roy, Nuno C. Santos, Christian Schwab, Guđmundur Stefánsson, Andrew E. Szymkowiak, Ryan C. Terrien, Stephane Udry, Sam A. Weiss, François Wildi, Thibault Wildi, Jason T. Wright
Figure caption: Resulting Binning rms from different binning methods as a function of bin width. The color of the point indicates whether the RVs in a bin were weighted by analytic error before being averaged (blue) or weighted by error and time from the center of the bin (orange). The saturation of the color indicates the time between each bin.
Paper: TESS Spots a Super-puff: The Remarkably Low Density of TOI-1420b
Authors: Stephanie Yoshida, Shreyas Vissapragada, David W. Latham, Allyson Bieryla, Daniel P. Thorngren, Jason D. Eastman, Mercedes López-Morales, Khalid Barkaoui, Charles Beichman, Perry Berlind, Lars A. Buchave, Michael L. Calkins, David R. Ciardi, Karen A. Collins, Rosario Cosentino, Ian J. M. Crossfield, Fei Dai, Victoria DiTomasso, Nicholas Dowling, Gilbert A. Esquerdo, Raquel Forés-Toribio, Adriano Ghedina, Maria V. Goliguzova, Eli Golub, Erica J. Gonzales, Ferran Grau Horta, Jesus Higuera, Nora Hoch, Keith Horne, Steve B. Howell, Jon M. Jenkins, Jessica Klusmeyer, Didier Laloum, Jack J. Lissauer, Sarah E. Logsdon, Luca Malavolta, Rachel A. Matson, Elisabeth C. Matthews, Kim K. McLeod, Jennifer V. Medina, Jose A. Muñoz, Hugh P. Osborn, Boris Safonov, Joshua Schlieder, Michael Schmidt, Heidi Schweiker, Sara Seager, Alessandro Sozzetti, Gregor Srdoc, Guđmundur Stefánsson, Ivan A. Strakhov, Stephanie Striegel, Joel Villaseñor, Joshua N. Winn
Figure caption: Sensitivities of our SAI 2.5 m I  c -band speckle image (left) and Gemini/NIRI Brγ AO image (right). The insets are the high-resolution images of TOI-1420. The star appears single, and no visual companions are observed anywhere in either field of view, which extend to 5.″1 × 10.″6 for the SAI image and 26″ × 26″ for the Gemini/NIRI image (we only show the central few arcseconds in the contrast curves and inset images for visual clarity).
Paper: TESS Spots a Super-puff: The Remarkably Low Density of TOI-1420b
Authors: Stephanie Yoshida, Shreyas Vissapragada, David W. Latham, Allyson Bieryla, Daniel P. Thorngren, Jason D. Eastman, Mercedes López-Morales, Khalid Barkaoui, Charles Beichman, Perry Berlind, Lars A. Buchave, Michael L. Calkins, David R. Ciardi, Karen A. Collins, Rosario Cosentino, Ian J. M. Crossfield, Fei Dai, Victoria DiTomasso, Nicholas Dowling, Gilbert A. Esquerdo, Raquel Forés-Toribio, Adriano Ghedina, Maria V. Goliguzova, Eli Golub, Erica J. Gonzales, Ferran Grau Horta, Jesus Higuera, Nora Hoch, Keith Horne, Steve B. Howell, Jon M. Jenkins, Jessica Klusmeyer, Didier Laloum, Jack J. Lissauer, Sarah E. Logsdon, Luca Malavolta, Rachel A. Matson, Elisabeth C. Matthews, Kim K. McLeod, Jennifer V. Medina, Jose A. Muñoz, Hugh P. Osborn, Boris Safonov, Joshua Schlieder, Michael Schmidt, Heidi Schweiker, Sara Seager, Alessandro Sozzetti, Gregor Srdoc, Guđmundur Stefánsson, Ivan A. Strakhov, Stephanie Striegel, Joel Villaseñor, Joshua N. Winn
Figure caption: TESS PDCSAP light curves for TOI-1420 phased to the planetary ephemeris and binned to 0.1 days cadence. The transits are masked and occur at a phase of 0 day.
Paper: TESS Spots a Super-puff: The Remarkably Low Density of TOI-1420b
Authors: Stephanie Yoshida, Shreyas Vissapragada, David W. Latham, Allyson Bieryla, Daniel P. Thorngren, Jason D. Eastman, Mercedes López-Morales, Khalid Barkaoui, Charles Beichman, Perry Berlind, Lars A. Buchave, Michael L. Calkins, David R. Ciardi, Karen A. Collins, Rosario Cosentino, Ian J. M. Crossfield, Fei Dai, Victoria DiTomasso, Nicholas Dowling, Gilbert A. Esquerdo, Raquel Forés-Toribio, Adriano Ghedina, Maria V. Goliguzova, Eli Golub, Erica J. Gonzales, Ferran Grau Horta, Jesus Higuera, Nora Hoch, Keith Horne, Steve B. Howell, Jon M. Jenkins, Jessica Klusmeyer, Didier Laloum, Jack J. Lissauer, Sarah E. Logsdon, Luca Malavolta, Rachel A. Matson, Elisabeth C. Matthews, Kim K. McLeod, Jennifer V. Medina, Jose A. Muñoz, Hugh P. Osborn, Boris Safonov, Joshua Schlieder, Michael Schmidt, Heidi Schweiker, Sara Seager, Alessandro Sozzetti, Gregor Srdoc, Guđmundur Stefánsson, Ivan A. Strakhov, Stephanie Striegel, Joel Villaseñor, Joshua N. Winn
Figure caption: Mass–radius diagram of transiting planets from the NASA Exoplanet Archive with 0⊕ < M p < 100M ⊕ and better than 30% precision on the mass. The blue, orange, and green curves indicate 0.1 g cm−3, 0.5 g cm−3, and 1.0 g cm−3, respectively. TOI-1420 (the red point) is extremely low-density and falls along the 0.1 g cm−3 line.
Paper: TESS Spots a Super-puff: The Remarkably Low Density of TOI-1420b
Authors: Stephanie Yoshida, Shreyas Vissapragada, David W. Latham, Allyson Bieryla, Daniel P. Thorngren, Jason D. Eastman, Mercedes López-Morales, Khalid Barkaoui, Charles Beichman, Perry Berlind, Lars A. Buchave, Michael L. Calkins, David R. Ciardi, Karen A. Collins, Rosario Cosentino, Ian J. M. Crossfield, Fei Dai, Victoria DiTomasso, Nicholas Dowling, Gilbert A. Esquerdo, Raquel Forés-Toribio, Adriano Ghedina, Maria V. Goliguzova, Eli Golub, Erica J. Gonzales, Ferran Grau Horta, Jesus Higuera, Nora Hoch, Keith Horne, Steve B. Howell, Jon M. Jenkins, Jessica Klusmeyer, Didier Laloum, Jack J. Lissauer, Sarah E. Logsdon, Luca Malavolta, Rachel A. Matson, Elisabeth C. Matthews, Kim K. McLeod, Jennifer V. Medina, Jose A. Muñoz, Hugh P. Osborn, Boris Safonov, Joshua Schlieder, Michael Schmidt, Heidi Schweiker, Sara Seager, Alessandro Sozzetti, Gregor Srdoc, Guđmundur Stefánsson, Ivan A. Strakhov, Stephanie Striegel, Joel Villaseñor, Joshua N. Winn
Figure caption: Periodograms of TOI-1420's HARPS-N RVs, activity indicators, and window function. The False Alarm Probabilities (FAPs) are calculated via 100,000 bootstrap simulations. The only significant peak (<0.1% FAP) in the RV periodogram is at 6.94 days, which we attribute to the planet candidate. This periodic signal is not present in any of the activity indicators.
Paper: TESS Spots a Super-puff: The Remarkably Low Density of TOI-1420b
Authors: Stephanie Yoshida, Shreyas Vissapragada, David W. Latham, Allyson Bieryla, Daniel P. Thorngren, Jason D. Eastman, Mercedes López-Morales, Khalid Barkaoui, Charles Beichman, Perry Berlind, Lars A. Buchave, Michael L. Calkins, David R. Ciardi, Karen A. Collins, Rosario Cosentino, Ian J. M. Crossfield, Fei Dai, Victoria DiTomasso, Nicholas Dowling, Gilbert A. Esquerdo, Raquel Forés-Toribio, Adriano Ghedina, Maria V. Goliguzova, Eli Golub, Erica J. Gonzales, Ferran Grau Horta, Jesus Higuera, Nora Hoch, Keith Horne, Steve B. Howell, Jon M. Jenkins, Jessica Klusmeyer, Didier Laloum, Jack J. Lissauer, Sarah E. Logsdon, Luca Malavolta, Rachel A. Matson, Elisabeth C. Matthews, Kim K. McLeod, Jennifer V. Medina, Jose A. Muñoz, Hugh P. Osborn, Boris Safonov, Joshua Schlieder, Michael Schmidt, Heidi Schweiker, Sara Seager, Alessandro Sozzetti, Gregor Srdoc, Guđmundur Stefánsson, Ivan A. Strakhov, Stephanie Striegel, Joel Villaseñor, Joshua N. Winn
Figure caption: Transit light curves of TOI-1420b with TESS and ground-based observatories. The red curves indicate the best-fit EXOFASTv2 model.