adsabs/AstroCLIMB huggingface dataset:
Paper: The EXPRES Stellar Signals Project II. State of the Field in Disentangling Photospheric Velocities
Authors: Lily L. Zhao, Debra A. Fischer, Eric B. Ford, Alex Wise, Michaël Cretignier, Suzanne Aigrain, Oscar Barragan, Megan Bedell, Lars A. Buchhave, João D. Camacho, Heather M. Cegla, Jessi Cisewski-Kehe, Andrew Collier Cameron, Zoe L. de Beurs, Sally Dodson-Robinson, Xavier Dumusque, João P. Faria, Christian Gilbertson, Charlotte Haley, Justin Harrell, David W. Hogg, Parker Holzer, Ancy Anna John, Baptiste Klein, Marina Lafarga, Florian Lienhard, Vinesh Maguire-Rajpaul, Annelies Mortier, Belinda Nicholson, Michael L. Palumbo, Victor Ramirez Delgado, Christopher J. Shallue, Andrew Vanderburg, Pedro T. P. Viana, Jinglin Zhao, Norbert Zicher, Samuel H. C. Cabot, Gregory W. Henry, Rachael M. Roettenbacher, John M. Brewer, Joe Llama, Ryan R. Petersburg, and Andrew E. Szymkowiak
Figure caption: (Left column) EXPRES radial velocities obtained in 2019 and 2020. (right column) Several years of APT ground-based differential photometry obtained for the four ESSP stars. Both RVs and photometry time series are plotted with the median value subtracted. The photometric smoothing model constructed using a 100 day window for each time series is overplotted as a red curve over the photometry (where the photometry is shown before any detrending). The time stamps of the EXPRES RVs are marked in the right column by gray, vertical lines. The RVs were not taken simultaneously with the photometry with most of the RVs taken after the last photometric observation for all targets but HD 101501. The GP interpolation/extrapolation of the photometric data to the RV time stamps are overplotted as green points.
Paper: The EXPRES Stellar Signals Project II. State of the Field in Disentangling Photospheric Velocities
Authors: Lily L. Zhao, Debra A. Fischer, Eric B. Ford, Alex Wise, Michaël Cretignier, Suzanne Aigrain, Oscar Barragan, Megan Bedell, Lars A. Buchhave, João D. Camacho, Heather M. Cegla, Jessi Cisewski-Kehe, Andrew Collier Cameron, Zoe L. de Beurs, Sally Dodson-Robinson, Xavier Dumusque, João P. Faria, Christian Gilbertson, Charlotte Haley, Justin Harrell, David W. Hogg, Parker Holzer, Ancy Anna John, Baptiste Klein, Marina Lafarga, Florian Lienhard, Vinesh Maguire-Rajpaul, Annelies Mortier, Belinda Nicholson, Michael L. Palumbo, Victor Ramirez Delgado, Christopher J. Shallue, Andrew Vanderburg, Pedro T. P. Viana, Jinglin Zhao, Norbert Zicher, Samuel H. C. Cabot, Gregory W. Henry, Rachael M. Roettenbacher, John M. Brewer, Joe Llama, Ryan R. Petersburg, and Andrew E. Szymkowiak
Figure caption: Final overall rms of the clean RVs submitted for each of the four targets. The height and x-position of each bar scales with the final rms. Bars are colored by the type of input data used. For each target, the rms of the original, uncorrected EXPRES CBC RVs is shown as a black bar with its height emphasized by a horizontal dashed line across the full plot. The average intranight scatter of the EXPRES CBC RVs is also marked with a horizontal dashed–dotted line. Methods returning similar rms values to each other are emphasized via green shading.
Paper: The EXPRES Stellar Signals Project II. State of the Field in Disentangling Photospheric Velocities
Authors: Lily L. Zhao, Debra A. Fischer, Eric B. Ford, Alex Wise, Michaël Cretignier, Suzanne Aigrain, Oscar Barragan, Megan Bedell, Lars A. Buchhave, João D. Camacho, Heather M. Cegla, Jessi Cisewski-Kehe, Andrew Collier Cameron, Zoe L. de Beurs, Sally Dodson-Robinson, Xavier Dumusque, João P. Faria, Christian Gilbertson, Charlotte Haley, Justin Harrell, David W. Hogg, Parker Holzer, Ancy Anna John, Baptiste Klein, Marina Lafarga, Florian Lienhard, Vinesh Maguire-Rajpaul, Annelies Mortier, Belinda Nicholson, Michael L. Palumbo, Victor Ramirez Delgado, Christopher J. Shallue, Andrew Vanderburg, Pedro T. P. Viana, Jinglin Zhao, Norbert Zicher, Samuel H. C. Cabot, Gregory W. Henry, Rachael M. Roettenbacher, John M. Brewer, Joe Llama, Ryan R. Petersburg, and Andrew E. Szymkowiak
Figure caption: Pairwise comparisons between the activity RVs of all submitted methods. Each marker represents a pairing; the color of the marker gives the PCC between the activity RVs of two methods. Methods that did not submit activity RVs (for which the difference between the original and clean RVs was used instead) are shown as marker outlines. Significant PCC values (i.e., PCC > 0.4) are shown as squares, while a PCC < 0.4 is depicted with a circle. The first column of each plot gives the PCCs of activity RVs with the provided CBC RVs. The following rows/columns have methods ordered from top to bottom and left to right by decreasing total rms, the same as how methods are ordered in Figure 4. At the top of each subplot in green is a scaled bar graph of the resultant rms for each method. As recreated from Figure 4, methods that returned similar final rms values are highlighted in shades of green along with their associated correlation coefficients.
Paper: The EXPRES Stellar Signals Project II. State of the Field in Disentangling Photospheric Velocities
Authors: Lily L. Zhao, Debra A. Fischer, Eric B. Ford, Alex Wise, Michaël Cretignier, Suzanne Aigrain, Oscar Barragan, Megan Bedell, Lars A. Buchhave, João D. Camacho, Heather M. Cegla, Jessi Cisewski-Kehe, Andrew Collier Cameron, Zoe L. de Beurs, Sally Dodson-Robinson, Xavier Dumusque, João P. Faria, Christian Gilbertson, Charlotte Haley, Justin Harrell, David W. Hogg, Parker Holzer, Ancy Anna John, Baptiste Klein, Marina Lafarga, Florian Lienhard, Vinesh Maguire-Rajpaul, Annelies Mortier, Belinda Nicholson, Michael L. Palumbo, Victor Ramirez Delgado, Christopher J. Shallue, Andrew Vanderburg, Pedro T. P. Viana, Jinglin Zhao, Norbert Zicher, Samuel H. C. Cabot, Gregory W. Henry, Rachael M. Roettenbacher, John M. Brewer, Joe Llama, Ryan R. Petersburg, and Andrew E. Szymkowiak
Figure caption: Periodograms of RVs for HD 26965. The leftmost two plots in the top row show the periodogram for the provided EXPRES CBC RVs (left) and over 30 years of RVs from the CLS on the right (Rosenthal et al. 2021). Periodograms of the clean (blue) and activity (orange) RVs are given for all 21 of the methods that submitted ESSP results for HD 26965. Horizontal dashed and solid black lines denote p-values of 0.1 and 0.01, respectively. The proposed period for HD 26965 b, 42.38 days, is marked by a vertical, dashed blue line while the range given for the stellar rotation rate, 39–44.5 days, is shaded orange (Ma et al. 2018). The maximum power in this shaded region for both the clean (C) and activity (A) RV periodogram is given in the top-left corner of each subplot along with the corresponding p-value of the peak. Methods are ordered left-to-right and top-to-bottom by the difference between the clean and activity periodogram peaks. Subplots for methods resulting in a stronger peak with their clean RVs have blue axes; orange axes indicate a stronger periodicity in the activity RVs. Methods with comparable peaks in their clean and activity RVs are shown with black axes.
Paper: The EXPRES Stellar Signals Project II. State of the Field in Disentangling Photospheric Velocities
Authors: Lily L. Zhao, Debra A. Fischer, Eric B. Ford, Alex Wise, Michaël Cretignier, Suzanne Aigrain, Oscar Barragan, Megan Bedell, Lars A. Buchhave, João D. Camacho, Heather M. Cegla, Jessi Cisewski-Kehe, Andrew Collier Cameron, Zoe L. de Beurs, Sally Dodson-Robinson, Xavier Dumusque, João P. Faria, Christian Gilbertson, Charlotte Haley, Justin Harrell, David W. Hogg, Parker Holzer, Ancy Anna John, Baptiste Klein, Marina Lafarga, Florian Lienhard, Vinesh Maguire-Rajpaul, Annelies Mortier, Belinda Nicholson, Michael L. Palumbo, Victor Ramirez Delgado, Christopher J. Shallue, Andrew Vanderburg, Pedro T. P. Viana, Jinglin Zhao, Norbert Zicher, Samuel H. C. Cabot, Gregory W. Henry, Rachael M. Roettenbacher, John M. Brewer, Joe Llama, Ryan R. Petersburg, and Andrew E. Szymkowiak
Figure caption: Submitted results for HD 101501. For each periodogram, p-values of 0.01 and 0.01 are shown as horizontal solid and dashed black lines, respectively.
Paper: The EXPRES Stellar Signals Project II. State of the Field in Disentangling Photospheric Velocities
Authors: Lily L. Zhao, Debra A. Fischer, Eric B. Ford, Alex Wise, Michaël Cretignier, Suzanne Aigrain, Oscar Barragan, Megan Bedell, Lars A. Buchhave, João D. Camacho, Heather M. Cegla, Jessi Cisewski-Kehe, Andrew Collier Cameron, Zoe L. de Beurs, Sally Dodson-Robinson, Xavier Dumusque, João P. Faria, Christian Gilbertson, Charlotte Haley, Justin Harrell, David W. Hogg, Parker Holzer, Ancy Anna John, Baptiste Klein, Marina Lafarga, Florian Lienhard, Vinesh Maguire-Rajpaul, Annelies Mortier, Belinda Nicholson, Michael L. Palumbo, Victor Ramirez Delgado, Christopher J. Shallue, Andrew Vanderburg, Pedro T. P. Viana, Jinglin Zhao, Norbert Zicher, Samuel H. C. Cabot, Gregory W. Henry, Rachael M. Roettenbacher, John M. Brewer, Joe Llama, Ryan R. Petersburg, and Andrew E. Szymkowiak
Figure caption: Submitted results for HD 26965. Otherwise the same as Figure 7.
Paper: The EXPRES Stellar Signals Project II. State of the Field in Disentangling Photospheric Velocities
Authors: Lily L. Zhao, Debra A. Fischer, Eric B. Ford, Alex Wise, Michaël Cretignier, Suzanne Aigrain, Oscar Barragan, Megan Bedell, Lars A. Buchhave, João D. Camacho, Heather M. Cegla, Jessi Cisewski-Kehe, Andrew Collier Cameron, Zoe L. de Beurs, Sally Dodson-Robinson, Xavier Dumusque, João P. Faria, Christian Gilbertson, Charlotte Haley, Justin Harrell, David W. Hogg, Parker Holzer, Ancy Anna John, Baptiste Klein, Marina Lafarga, Florian Lienhard, Vinesh Maguire-Rajpaul, Annelies Mortier, Belinda Nicholson, Michael L. Palumbo, Victor Ramirez Delgado, Christopher J. Shallue, Andrew Vanderburg, Pedro T. P. Viana, Jinglin Zhao, Norbert Zicher, Samuel H. C. Cabot, Gregory W. Henry, Rachael M. Roettenbacher, John M. Brewer, Joe Llama, Ryan R. Petersburg, and Andrew E. Szymkowiak
Figure caption: Submitted results for HD 10700. Otherwise the same as Figure 7.
Paper: The EXPRES Stellar Signals Project II. State of the Field in Disentangling Photospheric Velocities
Authors: Lily L. Zhao, Debra A. Fischer, Eric B. Ford, Alex Wise, Michaël Cretignier, Suzanne Aigrain, Oscar Barragan, Megan Bedell, Lars A. Buchhave, João D. Camacho, Heather M. Cegla, Jessi Cisewski-Kehe, Andrew Collier Cameron, Zoe L. de Beurs, Sally Dodson-Robinson, Xavier Dumusque, João P. Faria, Christian Gilbertson, Charlotte Haley, Justin Harrell, David W. Hogg, Parker Holzer, Ancy Anna John, Baptiste Klein, Marina Lafarga, Florian Lienhard, Vinesh Maguire-Rajpaul, Annelies Mortier, Belinda Nicholson, Michael L. Palumbo, Victor Ramirez Delgado, Christopher J. Shallue, Andrew Vanderburg, Pedro T. P. Viana, Jinglin Zhao, Norbert Zicher, Samuel H. C. Cabot, Gregory W. Henry, Rachael M. Roettenbacher, John M. Brewer, Joe Llama, Ryan R. Petersburg, and Andrew E. Szymkowiak
Figure caption: Submitted results for HD 34411. Otherwise the same as Figure 7.
Paper: A Weighted Analysis to Improve the X-Ray Polarization Sensitivity of the Imaging X-ray Polarimetry Explorer
Authors: Alessandro Di Marco, Enrico Costa, Fabio Muleri, Paolo Soffitta, Sergio Fabiani, Fabio La Monaca, John Rankin, Fei Xie, Matteo Bachetti, Luca Baldini, Wayne Baumgartner, Ronaldo Bellazzini, Alessandro Brez, Simone Castellano, Ettore Del Monte, Niccolò Di Lalla, Riccardo Ferrazzoli, Luca Latronico, Simone Maldera, Alberto Manfreda, Stephen L. O'Dell, Matteo Perri, Melissa Pesce-Rollins, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Carmelo Sgrò, Gloria Spandre, Allyn F. Tennant, Antonino Tobia, Alessio Trois, and Martin C. Weisskopf
Figure caption: Example of ionization track resulting from the absorption of a 5.9 keV X-ray in the GPD. The reconstructed photoelectron direction and impact point are shown (Sgrò 2017).
Paper: A Weighted Analysis to Improve the X-Ray Polarization Sensitivity of the Imaging X-ray Polarimetry Explorer
Authors: Alessandro Di Marco, Enrico Costa, Fabio Muleri, Paolo Soffitta, Sergio Fabiani, Fabio La Monaca, John Rankin, Fei Xie, Matteo Bachetti, Luca Baldini, Wayne Baumgartner, Ronaldo Bellazzini, Alessandro Brez, Simone Castellano, Ettore Del Monte, Niccolò Di Lalla, Riccardo Ferrazzoli, Luca Latronico, Simone Maldera, Alberto Manfreda, Stephen L. O'Dell, Matteo Perri, Melissa Pesce-Rollins, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Carmelo Sgrò, Gloria Spandre, Allyn F. Tennant, Antonino Tobia, Alessio Trois, and Martin C. Weisskopf
Figure caption: Two examples of simulated tracks at about 4 keV from a GPD. Left: a circular track with α ≃ 0.01; right: a quasilinear track with α ≃ 0.7. In these plots, the green line represents the Monte Carlo true direction; the dotted-blue line, the first-step reconstructed direction; and the dotted-black line, the final reconstructed direction after Bragg removal (see text).
Paper: A Weighted Analysis to Improve the X-Ray Polarization Sensitivity of the Imaging X-ray Polarimetry Explorer
Authors: Alessandro Di Marco, Enrico Costa, Fabio Muleri, Paolo Soffitta, Sergio Fabiani, Fabio La Monaca, John Rankin, Fei Xie, Matteo Bachetti, Luca Baldini, Wayne Baumgartner, Ronaldo Bellazzini, Alessandro Brez, Simone Castellano, Ettore Del Monte, Niccolò Di Lalla, Riccardo Ferrazzoli, Luca Latronico, Simone Maldera, Alberto Manfreda, Stephen L. O'Dell, Matteo Perri, Melissa Pesce-Rollins, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Carmelo Sgrò, Gloria Spandre, Allyn F. Tennant, Antonino Tobia, Alessio Trois, and Martin C. Weisskopf
Figure caption: Distribution of event’s TL, TW, TS, TE, ellipticity, and skewness absolute value for simulated data (left) and modulation factor as a function of the considered parameter (right).
Paper: A Weighted Analysis to Improve the X-Ray Polarization Sensitivity of the Imaging X-ray Polarimetry Explorer
Authors: Alessandro Di Marco, Enrico Costa, Fabio Muleri, Paolo Soffitta, Sergio Fabiani, Fabio La Monaca, John Rankin, Fei Xie, Matteo Bachetti, Luca Baldini, Wayne Baumgartner, Ronaldo Bellazzini, Alessandro Brez, Simone Castellano, Ettore Del Monte, Niccolò Di Lalla, Riccardo Ferrazzoli, Luca Latronico, Simone Maldera, Alberto Manfreda, Stephen L. O'Dell, Matteo Perri, Melissa Pesce-Rollins, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Carmelo Sgrò, Gloria Spandre, Allyn F. Tennant, Antonino Tobia, Alessio Trois, and Martin C. Weisskopf
Figure caption: Distribution of Ellipticity, α, at 2 keV (blue line), 4 keV (orange line), 6 keV (green line).
Paper: A Weighted Analysis to Improve the X-Ray Polarization Sensitivity of the Imaging X-ray Polarimetry Explorer
Authors: Alessandro Di Marco, Enrico Costa, Fabio Muleri, Paolo Soffitta, Sergio Fabiani, Fabio La Monaca, John Rankin, Fei Xie, Matteo Bachetti, Luca Baldini, Wayne Baumgartner, Ronaldo Bellazzini, Alessandro Brez, Simone Castellano, Ettore Del Monte, Niccolò Di Lalla, Riccardo Ferrazzoli, Luca Latronico, Simone Maldera, Alberto Manfreda, Stephen L. O'Dell, Matteo Perri, Melissa Pesce-Rollins, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Carmelo Sgrò, Gloria Spandre, Allyn F. Tennant, Antonino Tobia, Alessio Trois, and Martin C. Weisskopf
Figure caption:  ﹩{N}_{\mathrm{eff}}/{ \mathcal I }﹩ (left) and modulation factor (right) as a function of the energy at different λ values, as obtained by Monte Carlo simulations. See the text.
Paper: A Weighted Analysis to Improve the X-Ray Polarization Sensitivity of the Imaging X-ray Polarimetry Explorer
Authors: Alessandro Di Marco, Enrico Costa, Fabio Muleri, Paolo Soffitta, Sergio Fabiani, Fabio La Monaca, John Rankin, Fei Xie, Matteo Bachetti, Luca Baldini, Wayne Baumgartner, Ronaldo Bellazzini, Alessandro Brez, Simone Castellano, Ettore Del Monte, Niccolò Di Lalla, Riccardo Ferrazzoli, Luca Latronico, Simone Maldera, Alberto Manfreda, Stephen L. O'Dell, Matteo Perri, Melissa Pesce-Rollins, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Carmelo Sgrò, Gloria Spandre, Allyn F. Tennant, Antonino Tobia, Alessio Trois, and Martin C. Weisskopf
Figure caption: MDP99 values as a function of λ for 10 different Monte Carlo simulations. All these distributions have a minimum around λ = 0.75.
Paper: A Weighted Analysis to Improve the X-Ray Polarization Sensitivity of the Imaging X-ray Polarimetry Explorer
Authors: Alessandro Di Marco, Enrico Costa, Fabio Muleri, Paolo Soffitta, Sergio Fabiani, Fabio La Monaca, John Rankin, Fei Xie, Matteo Bachetti, Luca Baldini, Wayne Baumgartner, Ronaldo Bellazzini, Alessandro Brez, Simone Castellano, Ettore Del Monte, Niccolò Di Lalla, Riccardo Ferrazzoli, Luca Latronico, Simone Maldera, Alberto Manfreda, Stephen L. O'Dell, Matteo Perri, Melissa Pesce-Rollins, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Carmelo Sgrò, Gloria Spandre, Allyn F. Tennant, Antonino Tobia, Alessio Trois, and Martin C. Weisskopf
Figure caption: Comparison as a function of energy for three different analyses (unweighted, weighted, and “standard cuts”) displaying: (a) measured spurious modulation; (b) measured modulation factor; (c) relative quality factor. Although values are shown for the representative case of IXPE DU-FM2, similar behaviors are obtained for the other DUs aboard IXPE.
Paper: A Weighted Analysis to Improve the X-Ray Polarization Sensitivity of the Imaging X-ray Polarimetry Explorer
Authors: Alessandro Di Marco, Enrico Costa, Fabio Muleri, Paolo Soffitta, Sergio Fabiani, Fabio La Monaca, John Rankin, Fei Xie, Matteo Bachetti, Luca Baldini, Wayne Baumgartner, Ronaldo Bellazzini, Alessandro Brez, Simone Castellano, Ettore Del Monte, Niccolò Di Lalla, Riccardo Ferrazzoli, Luca Latronico, Simone Maldera, Alberto Manfreda, Stephen L. O'Dell, Matteo Perri, Melissa Pesce-Rollins, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Carmelo Sgrò, Gloria Spandre, Allyn F. Tennant, Antonino Tobia, Alessio Trois, and Martin C. Weisskopf
Figure caption: Distribution of MDP99 values for 200 IXPE simulated observations of a point-like source with energy spectrum described by a power law with number index −2, a flux 10−11 erg cm−2 s−1 in the energy range 2–8 keV, and 10 days of integration time. MDP99 values are estimated for weighted (left) and unweighted (right) analysis. See text.
Paper: Magnitude-squared Coherence: A Powerful Tool for Disentangling Doppler Planet Discoveries from Stellar Activity
Authors: Sarah E. Dodson-Robinson, Victor Ramirez Delgado, Justin Harrell, and Charlotte L. Haley
Figure caption: Top: Synthetic time series xt (Equation (3)), which represents an activity indicator, and yt (Equation (4)), which represents radial velocity. Star rotation manifests in both xt and yt, and yt also records planet-induced oscillations. Middle: A plot of yt as a function of xt fails to reveal a straight-line relationship between the two observables. This is because (1) the rotation signal in yt lags the rotation signal in xt by 90◦, and (2) both time series are plagued with Gaussian white noise. Bottom: The cross correlation ﹩{\hat{\gamma }}_{{xy}}(\tau )﹩ shows an oscillation at the rotation period.
Paper: Magnitude-squared Coherence: A Powerful Tool for Disentangling Doppler Planet Discoveries from Stellar Activity
Authors: Sarah E. Dodson-Robinson, Victor Ramirez Delgado, Justin Harrell, and Charlotte L. Haley
Figure caption: Top: The cross-spectrum estimate ﹩{\hat{S}}_{{xy}}(f)﹩ of synthetic signals xt and yt (Equation (6)). Spikes at ± frot appear in ﹩{\hat{q}}_{{xy}}(f)﹩ because the rotation signal in yt lags the signal in xt. Middle: Estimated magnitude-squared coherence between xt and yt (Equation (8)). From bottom to top, the red horizontal lines show the 1%, 0.1%, and 0.01% false alarm levels. The shared rotation signal generates a strong peak in ﹩{\hat{C}}_{{xy}}^{2}(f)﹩, but the planet signal present only in yt does not show up in ﹩{\hat{C}}_{{xy}}^{2}(f)﹩. Bottom: Estimated phase spectrum ﹩{\hat{\phi }}_{{xy}}(f)﹩. The dotted line shows the estimated phase at all frequencies. The solid line shows the part of the phase estimate at frequencies near frot, where the coherence is statistically significant. As expected from Equations (3) and (4), ﹩{\hat{\phi }}_{{xy}}({f}_{\mathrm{rot}})=270^\circ ﹩.
Paper: Magnitude-squared Coherence: A Powerful Tool for Disentangling Doppler Planet Discoveries from Stellar Activity
Authors: Sarah E. Dodson-Robinson, Victor Ramirez Delgado, Justin Harrell, and Charlotte L. Haley
Figure caption: z(f), the Fisher variance-stabilizing ﹩\mathrm{atanh}﹩ transformation of ﹩{\hat{C}}_{{xy}}^{2}(f)﹩. 1%, 0.1%, and 0.01% false alarm levels are shown in red.
Paper: Magnitude-squared Coherence: A Powerful Tool for Disentangling Doppler Planet Discoveries from Stellar Activity
Authors: Sarah E. Dodson-Robinson, Victor Ramirez Delgado, Justin Harrell, and Charlotte L. Haley
Figure caption: Nonoverlapping segmenting scheme for the α Cen B spectroscopic data set from Dumusque et al. (2012).
Paper: Magnitude-squared Coherence: A Powerful Tool for Disentangling Doppler Planet Discoveries from Stellar Activity
Authors: Sarah E. Dodson-Robinson, Victor Ramirez Delgado, Justin Harrell, and Charlotte L. Haley
Figure caption: Left: Cartoon showing the allocation of data points in xt among segments 0…K − 1 in Welch’s method. Series xt has 40 data points, which are broken into seven overlapping segments ﹩{x}_{j}^{(0)},\ldots ,{x}_{j}^{(6)}﹩ that each have 10 data points. Note that 10 data points per segment are far too few to compute any kind of periodogram, let alone a minimally biased one; this figure uses small N(k) simply for the sake of readability. Right: Tapers ﹩{w}_{j}^{(k)}﹩ applied to each segment shown in the left panel.
Paper: Magnitude-squared Coherence: A Powerful Tool for Disentangling Doppler Planet Discoveries from Stellar Activity
Authors: Sarah E. Dodson-Robinson, Victor Ramirez Delgado, Justin Harrell, and Charlotte L. Haley
Figure caption: Top left: Synthetic data set with N = 128, ti = 0…10 days, and ﹩{y}_{t}=\cos (2\pi {{tf}}_{1})+0.017\sin (2\pi {{tf}}_{2})﹩, where f1 = 1.7 days−1 and f2 = 1.2 days−1. Bottom left: wtyt, the product of yt with a minimum 4–term Blackman–Harris window (gray curve). Right: Estimated power spectra of yt (blue dashed–dotted line) and wtyt (solid red line). Vertical lines mark f1 and f2. Without tapering, leakage from planet 1's strong signal masks the weaker signal from planet 2. When the taper is applied, leakage from planet 1 is confined to frequencies near f1 and the weak signal at f2 is uncovered.
Paper: Magnitude-squared Coherence: A Powerful Tool for Disentangling Doppler Planet Discoveries from Stellar Activity
Authors: Sarah E. Dodson-Robinson, Victor Ramirez Delgado, Justin Harrell, and Charlotte L. Haley
Figure caption: GJ 3998 RV time series (black) divided into two 50%-overlapping segments shown by blue and orange shading. The dark pink area is where the two segments overlap. The minimum four-term Blackman–Harris tapers applied to each segment are shown at the top of the plot shifted vertically by +10 for visibility, with blue stars indicating Taper 1 and red triangles indicating Taper 2. RV data come from the HADES survey, which uses the HARPS-N instrument, and were extracted with the TERRA pipeline (Affer et al. 2016).
Paper: Magnitude-squared Coherence: A Powerful Tool for Disentangling Doppler Planet Discoveries from Stellar Activity
Authors: Sarah E. Dodson-Robinson, Victor Ramirez Delgado, Justin Harrell, and Charlotte L. Haley
Figure caption: Top left: 51 Peg RV time series measured by Butler et al. (2006), labeled yt in our notation. Bottom left: wtyt, the 51 Peg RV time series after applying a minimum four-term Blackman–Harris taper. Top right: ﹩{\hat{S}}_{{yy}}(f)﹩, the estimated power spectrum of yt, shows the strong planet signal at f = 1/4.2308 days−1 (dotted black line). Bottom right: ﹩{\hat{S}}_{y}^{w}(f)﹩, the estimated power spectrum of wtyt, shows only noise.