adsabs/AstroCLIMB huggingface dataset:
Paper: TOI 560: Two Transiting Planets Orbiting a K Dwarf Validated with iSHELL, PFS, and HIRES RVs
Authors: Mohammed El Mufti, Peter P. Plavchan, Howard Isaacson, Bryson L. Cale, Dax L. Feliz, Michael A. Reefe, Coel Hellier, Keivan Stassun, Jason Eastman, Alex Polanski, Ian J. M. Crossfield, Eric Gaidos, Veselin Kostov, Justin M. Wittrock, Joel Villaseñor, Joshua E. Schlieder, Luke G. Bouma, Kevin I. Collins, Farzaneh Zohrabi, Rena A. Lee, Ahmad Sohani, John Berberian, David Vermilion, Patrick Newman, Claire Geneser, Angelle Tanner, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Lea A. Hirsch, Rae Holcomb, Jack Lubin, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Christopher Stockdale, Karen Collins, Ryan Cloutier, Howard Relles, Thiam-Guan Tan, Nicholas J Scott, Zach Hartman, Elisabeth Matthews, David R. Ciardi, Erica Gonzales, Rachel A. Matson, Charles Beichman, Allyson Bieryla, E. Furlan, Crystal L. Gnilka, Steve B. Howell, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Markus Rabus, Marshall C. Johnson, Jessie Christiansen, Laura Kreidberg, David Anthony Berardo, Drake Deming, Varoujan Gorjian, Farisa Y. Morales, Björn Benneke, Diana Dragomir, Robert A. Wittenmyer, Sarah Ballard, Brendan P. Bowler, Jonathan Horner, John Kielkopf, Huigen Liu, Avi Shporer, C. G. Tinney, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura
Figure caption: The Spitzer light curve for TOI 560, with normalized flux plotted as a function of time since mid-transit. The Spitzer data points are binned for clarity, and overlaid with a transit model independently fit in blue.
Paper: Importance of Sample Selection in Exoplanet-atmosphere Population Studies
Authors: Natasha E. Batalha, Angie Wolfgang, Johanna Teske, Munazza K. Alam, Lili Alderson, Natalie M. Batalha, Mercedes López-Morales, Hannah R. Wakeford
Figure caption: The result of three metrics used to evaluate the success of the three hypothetical NIRSpec G395H surveys (QS, ESBE and 3Bin). The first metric (left panel) describes the accuracy and precision of the constrained atmospheric C/O ratio (shown for individual planets in Figure 3 for Trial 0). The second and third metrics (middle/right panel) describe the ability to constrain the population parameters precisely and accurately, respectively. For all three metrics, the lower the value, the “better” the survey performed (indicated by *). Horizontal lines indicate the mean across all 10 trials (for M atm the purple and pink lines are overlapping). Overall, the QS- and 3Bin- derived samples have the highest success in constraining atmospheric parameters, while the QS- and ESBE- have the highest success in constraining population parameters.
Paper: Importance of Sample Selection in Exoplanet-atmosphere Population Studies
Authors: Natasha E. Batalha, Angie Wolfgang, Johanna Teske, Munazza K. Alam, Lili Alderson, Natalie M. Batalha, Mercedes López-Morales, Hannah R. Wakeford
Figure caption: Differences between 3σ-credible intervals for the population parameter describing the radius relation, m  r , for the 3Bin sampling method vs. the QS and ESBE sampling methods, with two choices of prior. As shown in Figure 4, m  r  is the only parameter with Gaussian credible intervals, as opposed to upper or lower limits on the other parameters. The QS and ESBE sampling methods result in smaller credible intervals on m  r  for nearly all trials when compared to the 3Bin method.
Paper: Importance of Sample Selection in Exoplanet-atmosphere Population Studies
Authors: Natasha E. Batalha, Angie Wolfgang, Johanna Teske, Munazza K. Alam, Lili Alderson, Natalie M. Batalha, Mercedes López-Morales, Hannah R. Wakeford
Figure caption: The posterior probability distributions for the three population parameters (see Equation (3)) for one trial and two different assumptions for prior on the population-level parameters. True injected values are shown with black vertical lines.
Paper: A Catalog of Habitable Zone Exoplanets
Authors: Michelle L. Hill, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, Stephen R. Kane, Ravi Kopparapu, Zhexing Li, Colby Ostberg
Figure caption: Depiction of both the conservative (light green) and optimistic (combined light and dark green) HZ regions, with boundary labels defined by Kopparapu et al. (2013).
Paper: Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N
Authors: Victoria DiTomasso, Chantanelle Nava, Mercedes López-Morales, Allyson Bieryla, Ryan Cloutier, Luca Malavolta, Annelies Mortier, Lars A. Buchhave, Keivan G. Stassun, Alessandro Sozzetti, Aldo Stefano Bonomo, David Charbonneau, Andrew Collier Cameron, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martínez Fiorenzano, Adriano Ghedina, Avet Harutyunyan, R. D. Haywood, David Latham, Emilio Molinari, Francesco A. Pepe, Matteo Pinamonti, Ennio Poretti, Ken Rice, Dimitar Sasselov, Manu Stalport, Stéphane Udry, Christopher Watson, Thomas G. Wilson
Figure caption: Zoomed-in periodogram of the HD 79211 white light HARPS-N RVs, highlighting the strongest peak in the periodogram at 24.41 days and the aliases that result in its interaction with the 365 and 1550.8 day peaks in the window function. The periodogram calculated from the best-fit Keplerian planet orbit, sampled with the observing cadence of the HARPS-N data, is plotted in light blue. There is variation between the periodograms of the model and the data, caused by the data’s uncertainties and the influence of stellar activity in the data, but much of the aliasing structure can be seen in both periodograms. The 24.76 day peak (above the 0.01% FAP line) can be explained as an alias.
Paper: Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N
Authors: Victoria DiTomasso, Chantanelle Nava, Mercedes López-Morales, Allyson Bieryla, Ryan Cloutier, Luca Malavolta, Annelies Mortier, Lars A. Buchhave, Keivan G. Stassun, Alessandro Sozzetti, Aldo Stefano Bonomo, David Charbonneau, Andrew Collier Cameron, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martínez Fiorenzano, Adriano Ghedina, Avet Harutyunyan, R. D. Haywood, David Latham, Emilio Molinari, Francesco A. Pepe, Matteo Pinamonti, Ennio Poretti, Ken Rice, Dimitar Sasselov, Manu Stalport, Stéphane Udry, Christopher Watson, Thomas G. Wilson
Figure caption: Radial velocities for HD 79210 measured from CARMENES (orange, top panel only), HARPS-N (blue, all panels), and HIRES (green, top panel only) spectra. For most data points, the uncertainty in the RV is smaller than the size of the point. We mark the binary trend, fit as a second-order polynomial, with a dashed line in the first and third panels. The bottom panel shows the HARPS-N radial velocities with the binary trend subtracted. We use the HARPS-N RVs with the binary trend removed in our periodograms and when calculating correlation with stellar activity indicators analysis (Figures B2, B3, B4).
Paper: Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N
Authors: Victoria DiTomasso, Chantanelle Nava, Mercedes López-Morales, Allyson Bieryla, Ryan Cloutier, Luca Malavolta, Annelies Mortier, Lars A. Buchhave, Keivan G. Stassun, Alessandro Sozzetti, Aldo Stefano Bonomo, David Charbonneau, Andrew Collier Cameron, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martínez Fiorenzano, Adriano Ghedina, Avet Harutyunyan, R. D. Haywood, David Latham, Emilio Molinari, Francesco A. Pepe, Matteo Pinamonti, Ennio Poretti, Ken Rice, Dimitar Sasselov, Manu Stalport, Stéphane Udry, Christopher Watson, Thomas G. Wilson
Figure caption: We fit the chromatic radial velocities using RadVel, fixing all of the parameters and hyperparameters except for K  b  to the best-fit values found from fitting the white light HARPS-N DRS RVs (the white light counterpart to the chromatic RVs), not the HARPS-TERRA RVs that we use in the rest of this work. Here, we plot the resulting K  b  versus the wavelength band used to calculate those radial velocities. The white light RV result from fitting the HARPS-N DRS RVs is noted by the black point. All of these values agree within their error bars, and they do not show the trend of increasing semiamplitude with decreasing wavelength that we would expect of a signal caused by stellar activity.
Paper: Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N
Authors: Victoria DiTomasso, Chantanelle Nava, Mercedes López-Morales, Allyson Bieryla, Ryan Cloutier, Luca Malavolta, Annelies Mortier, Lars A. Buchhave, Keivan G. Stassun, Alessandro Sozzetti, Aldo Stefano Bonomo, David Charbonneau, Andrew Collier Cameron, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martínez Fiorenzano, Adriano Ghedina, Avet Harutyunyan, R. D. Haywood, David Latham, Emilio Molinari, Francesco A. Pepe, Matteo Pinamonti, Ennio Poretti, Ken Rice, Dimitar Sasselov, Manu Stalport, Stéphane Udry, Christopher Watson, Thomas G. Wilson
Figure caption: Periodograms of the three chromatic HARPS-N RV sets and the window function. The top panel shows chrom1 RVs (calculated using the bluest portion of the spectrum), followed by chrom2, and chrom3 in the lowest RV panel (calculated using the reddest portion of the spectrum). The window function is shown in the bottom panel. The same significant peaks that are marked in the white light RV periodogram (Figure 6) are marked here with vertical dashed lines. Both signals are present in these chromatic periodograms, with increasing significance as we look to the redder RVs. Because this signal is not larger in the bluer wavelengths, as we would expect if the signal were caused by stellar activity, we do not take this as evidence that the 24.41 day signal is caused by stellar activity.
Paper: Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N
Authors: Victoria DiTomasso, Chantanelle Nava, Mercedes López-Morales, Allyson Bieryla, Ryan Cloutier, Luca Malavolta, Annelies Mortier, Lars A. Buchhave, Keivan G. Stassun, Alessandro Sozzetti, Aldo Stefano Bonomo, David Charbonneau, Andrew Collier Cameron, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martínez Fiorenzano, Adriano Ghedina, Avet Harutyunyan, R. D. Haywood, David Latham, Emilio Molinari, Francesco A. Pepe, Matteo Pinamonti, Ennio Poretti, Ken Rice, Dimitar Sasselov, Manu Stalport, Stéphane Udry, Christopher Watson, Thomas G. Wilson
Figure caption: Stacked Bayesian Generalized Lomb–Scargle periodograms (SBGLS) for the HD 79211 HARPS-N white light radial velocities, with the binary trend removed. The horizontal axis is the frequency of the signal, the color is the power, and the vertical axis shows how the periodogram changes as observations are added to the calculation. This periodogram is oversampled by a factor of 5. The same peaks are highlighted from the 2D periodogram; Figure 6. The strongest peak at 24.41 days gets stronger as more observations are added, as we would expect for a planet signal.
Paper: Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N
Authors: Victoria DiTomasso, Chantanelle Nava, Mercedes López-Morales, Allyson Bieryla, Ryan Cloutier, Luca Malavolta, Annelies Mortier, Lars A. Buchhave, Keivan G. Stassun, Alessandro Sozzetti, Aldo Stefano Bonomo, David Charbonneau, Andrew Collier Cameron, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martínez Fiorenzano, Adriano Ghedina, Avet Harutyunyan, R. D. Haywood, David Latham, Emilio Molinari, Francesco A. Pepe, Matteo Pinamonti, Ennio Poretti, Ken Rice, Dimitar Sasselov, Manu Stalport, Stéphane Udry, Christopher Watson, Thomas G. Wilson
Figure caption: Periodograms of HARPS-N radial velocities of HD 79210, without the binary trend removed (top) and with the binary trend removed (bottom). Signals with frequencies from 0 to 0.33 day−1 are plotted. Before the binary trend is removed, there are many significant low-frequency signals (blue shaded region), as we would expect from the long-period binary. Once the binary trend is removed, there are no signals with less than 0.01% FAP.
Paper: Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N
Authors: Victoria DiTomasso, Chantanelle Nava, Mercedes López-Morales, Allyson Bieryla, Ryan Cloutier, Luca Malavolta, Annelies Mortier, Lars A. Buchhave, Keivan G. Stassun, Alessandro Sozzetti, Aldo Stefano Bonomo, David Charbonneau, Andrew Collier Cameron, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martínez Fiorenzano, Adriano Ghedina, Avet Harutyunyan, R. D. Haywood, David Latham, Emilio Molinari, Francesco A. Pepe, Matteo Pinamonti, Ennio Poretti, Ken Rice, Dimitar Sasselov, Manu Stalport, Stéphane Udry, Christopher Watson, Thomas G. Wilson
Figure caption: Phase-folded, best-fit Keplerian orbital model, after the Gaussian processes and binary star trend have been removed, as well as their residuals. The top row shows the best-fit model to the HARPS-N data alone, the middle row shows the combined HARPS-N + CARMENES data set, and the bottom row shows the HARPS-N + CARMENES + HIRES data set. The left-hand column shows the circular fits to these data sets and the right-hand column shows the corresponding eccentric fits. The blue line is the best-fit model with the orbital parameters printed in the legend and listed in Table 2. Red circles are the same velocities binned in 0.1 units of orbital phase. The middle right-hand panel, marked with a bold border, shows our final, adopted parameters for the planet candidate.
Paper: Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N
Authors: Victoria DiTomasso, Chantanelle Nava, Mercedes López-Morales, Allyson Bieryla, Ryan Cloutier, Luca Malavolta, Annelies Mortier, Lars A. Buchhave, Keivan G. Stassun, Alessandro Sozzetti, Aldo Stefano Bonomo, David Charbonneau, Andrew Collier Cameron, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martínez Fiorenzano, Adriano Ghedina, Avet Harutyunyan, R. D. Haywood, David Latham, Emilio Molinari, Francesco A. Pepe, Matteo Pinamonti, Ennio Poretti, Ken Rice, Dimitar Sasselov, Manu Stalport, Stéphane Udry, Christopher Watson, Thomas G. Wilson
Figure caption: Various HARPS-N stellar activity indicators versus HD 79210's radial velocities after the stellar binary trend has been subtracted. The r-values are Pearson correlation coefficients. FWHM is moderately correlated, with an r-value of 0.39.
Paper: Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N
Authors: Victoria DiTomasso, Chantanelle Nava, Mercedes López-Morales, Allyson Bieryla, Ryan Cloutier, Luca Malavolta, Annelies Mortier, Lars A. Buchhave, Keivan G. Stassun, Alessandro Sozzetti, Aldo Stefano Bonomo, David Charbonneau, Andrew Collier Cameron, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martínez Fiorenzano, Adriano Ghedina, Avet Harutyunyan, R. D. Haywood, David Latham, Emilio Molinari, Francesco A. Pepe, Matteo Pinamonti, Ennio Poretti, Ken Rice, Dimitar Sasselov, Manu Stalport, Stéphane Udry, Christopher Watson, Thomas G. Wilson
Figure caption: Posterior distributions of the combined HARPS-N and CARMENES data set for HD 79211b’s parameters derived from fitting an eccentric orbit.
Paper: Radio-loud Exoplanet-exomoon Survey: GMRT Search for Electron Cyclotron Maser Emission
Authors: Mayank Narang, Apurva V. Oza, Kaustubh Hakim, P. Manoj, Ravinder K. Banyal, Daniel P. Thorngren
Figure caption: The GMRT image (magenta contours) of the HAT-P 12 field at (a) 150 MHz and (b) 325 MHz overlaid on PANSTARR g band image. The red cross marks the position of the HAT-P 12. The contours plotted are 5, 10, 30, and 50 ×  σ. The beam is shown as a red ellipse at the bottom-left corner.
Paper: Radio-loud Exoplanet-exomoon Survey: GMRT Search for Electron Cyclotron Maser Emission
Authors: Mayank Narang, Apurva V. Oza, Kaustubh Hakim, P. Manoj, Ravinder K. Banyal, Daniel P. Thorngren
Figure caption: The GMRT image (magenta contours) of the HD 189733 field at 325 MHz images overlaid on the PANSTARR g band image. The red cross marks the position of the HD 189733. The contours plotted are 5, 10, 30, and 50 × σ. The beam is shown as a red ellipse at the bottom-left corner.
Paper: Radio-loud Exoplanet-exomoon Survey: GMRT Search for Electron Cyclotron Maser Emission
Authors: Mayank Narang, Apurva V. Oza, Kaustubh Hakim, P. Manoj, Ravinder K. Banyal, Daniel P. Thorngren
Figure caption: The uGMRT image (magenta contours) of the WASP-49 field at 400 MHz for each of the individual nights of observation overlaid on the PANSTARR g band image. The red cross marks the position of the WASP-49. The contours plotted are 5, 10, 30, and 50 ×  σ. The beam is shown as a red ellipse at the bottom-left corner.
Paper: Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N
Authors: Victoria DiTomasso, Chantanelle Nava, Mercedes López-Morales, Allyson Bieryla, Ryan Cloutier, Luca Malavolta, Annelies Mortier, Lars A. Buchhave, Keivan G. Stassun, Alessandro Sozzetti, Aldo Stefano Bonomo, David Charbonneau, Andrew Collier Cameron, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martínez Fiorenzano, Adriano Ghedina, Avet Harutyunyan, R. D. Haywood, David Latham, Emilio Molinari, Francesco A. Pepe, Matteo Pinamonti, Ennio Poretti, Ken Rice, Dimitar Sasselov, Manu Stalport, Stéphane Udry, Christopher Watson, Thomas G. Wilson
Figure caption: Lomb–Scargle periodogram of the nightly averaged relative fluxes for HD 79210 using a separate comparison star (top), HD 79211 using a separate comparison star (middle) and HD 79211 using HD 79210 as a comparison star (bottom). The vertical, gray dashes note the shared peaks between the two stars’ periodograms, which are likely caused by systematics in the images. The statistically significant (<0.1% FAP) peak in the bottom periodogram is marked with the dotted green line, and the shaded region marks one standard deviation around the peak (P = 17.34 days, freq = 0.057 ± 0.003 day−1). This peak corresponds to the one peak in HD 79211's periodogram that is not present in that of HD 79210, marked with the blue dotted line in the middle panel, at 17.74 days (freq = 0.056 ± 0.003 day−1). Although the 17.74 days peak is not statistically significant, this suggests that this photometric variability originates in HD 79211, and we attribute it to this star’s rotation period.
Paper: Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N
Authors: Victoria DiTomasso, Chantanelle Nava, Mercedes López-Morales, Allyson Bieryla, Ryan Cloutier, Luca Malavolta, Annelies Mortier, Lars A. Buchhave, Keivan G. Stassun, Alessandro Sozzetti, Aldo Stefano Bonomo, David Charbonneau, Andrew Collier Cameron, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martínez Fiorenzano, Adriano Ghedina, Avet Harutyunyan, R. D. Haywood, David Latham, Emilio Molinari, Francesco A. Pepe, Matteo Pinamonti, Ennio Poretti, Ken Rice, Dimitar Sasselov, Manu Stalport, Stéphane Udry, Christopher Watson, Thomas G. Wilson
Figure caption: Relative photometry for HD 79210 using a comparison star (orange), relative photometry for HD 79211 using a comparison star (blue), and relative photometry for HD 79211 using HD 79210 as a comparison star (green), plus an offset, as taken with KeplerCam. Note the different y-axis scale between the two separate light curves in the upper panel and the combined light curve in the lower panel. The faint, round points represent the relative flux measurement from each individual image. The darker, star-shaped points represent the nightly averaged relative flux. These average nightly fluxes are what we used when calculating the periodograms (Figure 3). These two separate light curves are highly affected by systematics, which we discuss in detail in Section 4.
Paper: Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N
Authors: Victoria DiTomasso, Chantanelle Nava, Mercedes López-Morales, Allyson Bieryla, Ryan Cloutier, Luca Malavolta, Annelies Mortier, Lars A. Buchhave, Keivan G. Stassun, Alessandro Sozzetti, Aldo Stefano Bonomo, David Charbonneau, Andrew Collier Cameron, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martínez Fiorenzano, Adriano Ghedina, Avet Harutyunyan, R. D. Haywood, David Latham, Emilio Molinari, Francesco A. Pepe, Matteo Pinamonti, Ennio Poretti, Ken Rice, Dimitar Sasselov, Manu Stalport, Stéphane Udry, Christopher Watson, Thomas G. Wilson
Figure caption: Periodograms of HARPS-N radial velocities of HD 79211, without the binary trend removed (top) and with the binary trend removed (bottom). Signals with frequencies from 0 to 0.33 day−1 are plotted. Signals with False Alarm Probabilities of less than 0.1% are marked. Before the binary trend is removed, there are many significant low-frequency signals (blue shaded region), as we would expect from the long-period binary. Two signals with FAPs of less than 0.01% are marked for HD 79211 once the binary trend is removed, at 24.41, and 24.76 days. The signal at 24.41 days is attributed to the planet candidate and has the highest power of the present peaks.
Paper: Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N
Authors: Victoria DiTomasso, Chantanelle Nava, Mercedes López-Morales, Allyson Bieryla, Ryan Cloutier, Luca Malavolta, Annelies Mortier, Lars A. Buchhave, Keivan G. Stassun, Alessandro Sozzetti, Aldo Stefano Bonomo, David Charbonneau, Andrew Collier Cameron, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martínez Fiorenzano, Adriano Ghedina, Avet Harutyunyan, R. D. Haywood, David Latham, Emilio Molinari, Francesco A. Pepe, Matteo Pinamonti, Ennio Poretti, Ken Rice, Dimitar Sasselov, Manu Stalport, Stéphane Udry, Christopher Watson, Thomas G. Wilson
Figure caption: Radial velocities for HD 79211 measured from CARMENES (orange, top panel only), HARPS-N (blue, all panels), and HIRES (green, top panel only) spectra. For most data points, the uncertainty in the RV is smaller than the size of the point. We mark the binary trend, fit as a second-order polynomial, with a dashed line in the top and middle panels. The bottom panel shows the HARPS-N radial velocities with the binary trend subtracted. We use the HARPS-N RVs with the binary trend removed when calculating the correlation between RV and activity indicators (Figure 4), and when calculating periodograms (Figures 5, 6, 7, 8).
Paper: Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N
Authors: Victoria DiTomasso, Chantanelle Nava, Mercedes López-Morales, Allyson Bieryla, Ryan Cloutier, Luca Malavolta, Annelies Mortier, Lars A. Buchhave, Keivan G. Stassun, Alessandro Sozzetti, Aldo Stefano Bonomo, David Charbonneau, Andrew Collier Cameron, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martínez Fiorenzano, Adriano Ghedina, Avet Harutyunyan, R. D. Haywood, David Latham, Emilio Molinari, Francesco A. Pepe, Matteo Pinamonti, Ennio Poretti, Ken Rice, Dimitar Sasselov, Manu Stalport, Stéphane Udry, Christopher Watson, Thomas G. Wilson
Figure caption: Periodograms of HD 79211's white light HARPS-N radial velocities with the binary trend removed, activity indicators, and the window function. All of significant peaks (<0.01% FAP) are marked with dashed vertical lines. The most significant peak is at 24.41 days, which we attribute to the planet candidate. We attribute the other significant peak, at 24.76 days, to aliases of the planet candidate signal (see Figure 7).