adsabs/AstroCLIMB huggingface dataset:
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: Spectral windows belonging to the Dumusque et al. (2012) α Cen B data set. The ringing in the Lomb–Scargle spectral window (light blue) means each periodic signal yields multiple peaks in ﹩{\hat{S}}_{{xx}}(f)﹩. The Welch’s spectral window (dark blue), which has a much cleaner main lobe, will translate each periodic signal into a single power spectrum peak. While this plot zooms in on low frequencies, all spectral windows have nonzero power throughout the frequency domain.
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: Hα indices of Kapteyn’s star measured by Robertson et al. (2015) from the spectra of Anglada-Escude et al. (2014). Top right: Lomb–Scargle periodogram of ﹩{I}_{{{\rm{H}}}_{\alpha }}﹩ with 5% and 1% FALs (purple and green, respectively). The FALs give the unrealistic impression that the periodogram has ≥ 10 significant peaks. Bottom: Spectral window W(f) of the Kapteyn’s star ﹩{I}_{{{\rm{H}}}_{\alpha }}﹩ time series. The broadness of the main lobe and the large number of spurious spikes suggest that peaks in the Lomb–Scargle periodogram are window function artifacts.
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: Welch’s power spectrum estimate of the GJ 581 ﹩{I}_{{{\rm{H}}}_{\alpha }}﹩ time series reported by Robertson et al. (2014), with Lomb–Scargle periodogram plotted for comparison. Bottom: Welch’s power spectrum estimate and Lomb–Scargle periodogram of the HARPS GJ 581 RVs reported by Forveille et al. (2011). Dotted horizontal lines show 0.1%, 1%, and 5% bootstrap FALs for the Welch’s power spectra (Lomb–Scargle FALs are not shown), while vertical black dashed–dotted lines show the rotation frequency and its first two harmonics. The resolution of the Welch’s estimator is indicated by the gray shading.
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: Spectral windows of the generalized Lomb–Scargle periodogram (light blue) and the Welch’s power spectrum estimate (dark blue) calculated from the Forveille et al. (2011) observations of GJ 581. The Welch’s power spectrum estimate was created using three 50%-overlapping segments with minimum four-term Blackman–Harris tapers.
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: Magnitude-squared coherence estimate from HARPS spectra, with RV measured by Forveille et al. (2011) and Hα index measured by Robertson et al. (2014). Solid horizontal lines show false-alarm levels from Equation (27), while dotted lines in the same color scheme show bootstrap false-alarm levels. The stellar signals originally identified as planets d and g are shown by yellow shaded regions of width ﹩2{ \mathcal B }﹩. Gray shaded regions of width ﹩2{ \mathcal B }﹩ surround the orbital frequencies of planets b and c. Vertical dotted black lines show rotation harmonics at which z(f) exceeds the 1% FAL.
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: Welch’s power spectra of the Dumusque et al. (2012) α Cen B data set: FWHM (top left), BIS (top right), ﹩\mathrm{log}{R}_{\mathrm{HK}}^{{\prime} }﹩ (bottom left), and RV (bottom right). Lomb–Scargle periodograms are shown in light blue for comparison. Dotted horizontal lines show 0.1%, 1%, and 5% bootstrap false-alarm thresholds for the Welch’s power spectrum (Lomb–Scargle false-alarm thresholds are not shown). The black dashed–dotted line denotes the star rotation period, while the gray shaded region shows the resolution limit of the Welch’s power spectrum estimate. Vertical dashed–dotted yellow lines show shared oscillations identified via magnitude-squared coherence.
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: Scatter plots yt versus xt for all four α Cen B observables. While there is no obvious straight-line relationship between RV and any activity indicator, the indicators are tightly correlated among themselves, suggesting that they trace the same physical processes.
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: Hyperbolic arctangent-ransformed activity indicator coherences from the Dumusque et al. (2012) α Cen B data. Top: z(f) given ﹩{x}_{t}=\mathrm{log}{R}_{\mathrm{HK}}^{{\prime} },{y}_{t}﹩ = FWHM; middle: z(f) given ﹩{x}_{t}=\mathrm{log}{R}_{\mathrm{HK}}^{{\prime} },{y}_{t}﹩ = BIS; bottom: z(f) given xt = FWHM, yt = BIS. The black dashed–dotted line shows the shared rotation signal, while the gray shaded area represents the resolution limit ﹩{ \mathcal B }﹩. Yellow dashed–dotted lines show signals that exceed the 1% false-alarm threshold in at least two of the three panels.
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: Transformed magnitude-squared coherence for xt = FWHM, yt = RV (top); xt = BIS, yt = RV (middle); and ﹩{x}_{t}=\mathrm{log}{R}_{\mathrm{HK}}^{{\prime} }﹩, yt = RV (bottom). The color scheme follows Figure 16. Yellow dashed–dotted lines mark shared oscillations that rise above the 1% FAL.
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: Welch’s (dark blue) and generalized Lomb–Scargle (light blue) periodograms of the GJ 3998 spectroscopic data of Affer et al. (2016). The color scheme is the same as in Figure 11.
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: Transformed magnitude-squared coherences between S-index and RV from the HADES GJ 3998 observations of Affer et al. (2016). Top left: xt = TERRA S-index, yt = TERRA RV. Top right: xt = TERRA S-index, yt = CCF RV. Bottom left: xt = H96 S-index, yt = TERRA RV. Bottom right: xt = H96 S-index, yt = CCF RV. All panels show a signal at the frequency of planet c. In addition, all z(f) estimates show high coherence at the fifth rotation harmonic (f = 6frot), while z(f) estimates with yt = CCF RV have high coherence at the third harmonic (f = 4frot). Rotation harmonics are marked by dotted black lines.
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: Transformed magnitude-squared coherences between ﹩{I}_{{{\rm{H}}}_{\alpha }}﹩ and RV from the HADES GJ 3998 observations of Affer et al. (2016). Top left: xt = TERRA ﹩{I}_{{{\rm{H}}}_{\alpha }}﹩, yt = TERRA RV. Top right: xt = TERRA ﹩{I}_{{{\rm{H}}}_{\alpha }}﹩, yt = CCF RV. Bottom left: xt = R13 ﹩{I}_{{{\rm{H}}}_{\alpha }}﹩, yt = TERRA RV. Bottom right: xt = R13 ﹩{I}_{{{\rm{H}}}_{\alpha }}﹩, yt = CCF RV. All panels show a stellar signal at the frequency of planet b, with FAP ≪ 1% for yt = CCF RV.
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: NWelch single-segment power spectrum estimate (dark blue, solid line) and astropy Lomb–Scargle periodogram (light blue, dashed line) of the α Cen B RVs measured by Dumusque et al. (2012). 5% and 1% false-alarm thresholds are shown in purple and green, respectively, with the solid horizontal lines showing astropy false-alarm thresholds and the dotted horizontal lines showing NWelch false-alarm thresholds. The two power spectrum estimates and their bootstrap false-alarm thresholds are nearly identical.
Paper: A Second Planet Transiting LTT 1445A and a Determination of the Masses of Both Worlds
Authors: Jennifer G. Winters, Ryan Cloutier, Amber A. Medina, Jonathan M. Irwin, David Charbonneau, Nicola Astudillo-Defru, Xavier Bonfils, Andrew W. Howard, Howard Isaacson, Jacob L. Bean, Andreas Seifahrt, Johanna K. Teske, Jason D. Eastman, Joseph D. Twicken, Karen A. Collins, Eric L. N. Jensen, Samuel N. Quinn, Matthew J. Payne, Martti H. Kristiansen, Alton Spencer, Andrew Vanderburg, Mathias Zechmeister, Lauren M. Weiss, Sharon Xuesong Wang, Gavin Wang, Stéphane Udry, Ivan A. Terentev, Julian Stürmer, Gudmundur Stefánsson, Avi Shporer, Stephen Shectman, Ramotholo Sefako, Hans Martin Schwengeler, Richard P. Schwarz, Nicholas Scarsdale, Ryan A. Rubenzahl, Arpita Roy, Lee J. Rosenthal, Paul Robertson, Erik A. Petigura, Francesco Pepe, Mark Omohundro, Joseph M. Akana Murphy, Felipe Murgas, Teo Močnik, Benjamin T. Montet, Ronald Mennickent, Andrew W. Mayo, Bob Massey, Jack Lubin, Christophe Lovis, Pablo Lewin, David Kasper, Stephen R. Kane, Jon M. Jenkins, Daniel Huber, Keith Horne, Michelle L. Hill, Paula Gorrini, Steven Giacalone, Benjamin Fulton, Thierry Forveille, Pedro Figueira, Tara Fetherolf, Courtney Dressing, Rodrigo F. Díaz, Xavier Delfosse, Paul A. Dalba, Fei Dai, C. C. Cortés, Ian J. M. Crossfield, Jeffrey D. Crane, Dennis M. Conti, Kevin I. Collins, Ashley Chontos, R. Paul Butler, Peyton Brown, Madison Brady, Aida Behmard, Corey Beard, Natalie M. Batalha, and Jose-Manuel Almenara
Figure caption: Periodograms and window functions of TESS and MEarth data of LTT 1445. The TESS data (top two panels), which include all three stellar components, exhibit a 1.4 day period. This signal is also seen in the periodogram of the MEarth data for LTT 1445BC (fourth panel), confirming that either the B or C component is the origin of the 1.4 day signal in the TESS data. The peak at 3.5 days represents an alias of the 1.4 day period. The cluster of peaks between 50 and 100 days likely indicates the rotation period of A (middle two panels), but more data are needed for a robust detection of the expected period of 85 ± 22 days. A marginal 6.7 day signal is also seen in both the TESS data and the MEarth data of LTT 1445BC, which we discuss further in Section 4.5.
Paper: A Second Planet Transiting LTT 1445A and a Determination of the Masses of Both Worlds
Authors: Jennifer G. Winters, Ryan Cloutier, Amber A. Medina, Jonathan M. Irwin, David Charbonneau, Nicola Astudillo-Defru, Xavier Bonfils, Andrew W. Howard, Howard Isaacson, Jacob L. Bean, Andreas Seifahrt, Johanna K. Teske, Jason D. Eastman, Joseph D. Twicken, Karen A. Collins, Eric L. N. Jensen, Samuel N. Quinn, Matthew J. Payne, Martti H. Kristiansen, Alton Spencer, Andrew Vanderburg, Mathias Zechmeister, Lauren M. Weiss, Sharon Xuesong Wang, Gavin Wang, Stéphane Udry, Ivan A. Terentev, Julian Stürmer, Gudmundur Stefánsson, Avi Shporer, Stephen Shectman, Ramotholo Sefako, Hans Martin Schwengeler, Richard P. Schwarz, Nicholas Scarsdale, Ryan A. Rubenzahl, Arpita Roy, Lee J. Rosenthal, Paul Robertson, Erik A. Petigura, Francesco Pepe, Mark Omohundro, Joseph M. Akana Murphy, Felipe Murgas, Teo Močnik, Benjamin T. Montet, Ronald Mennickent, Andrew W. Mayo, Bob Massey, Jack Lubin, Christophe Lovis, Pablo Lewin, David Kasper, Stephen R. Kane, Jon M. Jenkins, Daniel Huber, Keith Horne, Michelle L. Hill, Paula Gorrini, Steven Giacalone, Benjamin Fulton, Thierry Forveille, Pedro Figueira, Tara Fetherolf, Courtney Dressing, Rodrigo F. Díaz, Xavier Delfosse, Paul A. Dalba, Fei Dai, C. C. Cortés, Ian J. M. Crossfield, Jeffrey D. Crane, Dennis M. Conti, Kevin I. Collins, Ashley Chontos, R. Paul Butler, Peyton Brown, Madison Brady, Aida Behmard, Corey Beard, Natalie M. Batalha, and Jose-Manuel Almenara
Figure caption: MEarth light curves of LTT 1445A (top) and BC (bottom), phase-folded to the 1.4 day stellar rotation period. The data have been corrected for precipitable water vapor, and outliers have been rejected. The gray points and error bars indicate the individual measurements, while the black points indicate the binned data. The red curve in the bottom panel illustrates the 1.4 day rotation period model for LTT 1445BC. The top panel illustrates that we do not yet have enough data for a robust rotation period detection of LTT 1445A.(The data used to create this figure are available.)
Paper: A Second Planet Transiting LTT 1445A and a Determination of the Masses of Both Worlds
Authors: Jennifer G. Winters, Ryan Cloutier, Amber A. Medina, Jonathan M. Irwin, David Charbonneau, Nicola Astudillo-Defru, Xavier Bonfils, Andrew W. Howard, Howard Isaacson, Jacob L. Bean, Andreas Seifahrt, Johanna K. Teske, Jason D. Eastman, Joseph D. Twicken, Karen A. Collins, Eric L. N. Jensen, Samuel N. Quinn, Matthew J. Payne, Martti H. Kristiansen, Alton Spencer, Andrew Vanderburg, Mathias Zechmeister, Lauren M. Weiss, Sharon Xuesong Wang, Gavin Wang, Stéphane Udry, Ivan A. Terentev, Julian Stürmer, Gudmundur Stefánsson, Avi Shporer, Stephen Shectman, Ramotholo Sefako, Hans Martin Schwengeler, Richard P. Schwarz, Nicholas Scarsdale, Ryan A. Rubenzahl, Arpita Roy, Lee J. Rosenthal, Paul Robertson, Erik A. Petigura, Francesco Pepe, Mark Omohundro, Joseph M. Akana Murphy, Felipe Murgas, Teo Močnik, Benjamin T. Montet, Ronald Mennickent, Andrew W. Mayo, Bob Massey, Jack Lubin, Christophe Lovis, Pablo Lewin, David Kasper, Stephen R. Kane, Jon M. Jenkins, Daniel Huber, Keith Horne, Michelle L. Hill, Paula Gorrini, Steven Giacalone, Benjamin Fulton, Thierry Forveille, Pedro Figueira, Tara Fetherolf, Courtney Dressing, Rodrigo F. Díaz, Xavier Delfosse, Paul A. Dalba, Fei Dai, C. C. Cortés, Ian J. M. Crossfield, Jeffrey D. Crane, Dennis M. Conti, Kevin I. Collins, Ashley Chontos, R. Paul Butler, Peyton Brown, Madison Brady, Aida Behmard, Corey Beard, Natalie M. Batalha, and Jose-Manuel Almenara
Figure caption: Transits of LTT 1445Ab measured from ground-based data. The top panel shows the transit of LTT 1445Ab as observed by MEarth-South on UT 2019 September 2 using seven telescopes. The bottom panel shows two transits of LTT 1445Ab as observed by LCOGT.
Paper: A Second Planet Transiting LTT 1445A and a Determination of the Masses of Both Worlds
Authors: Jennifer G. Winters, Ryan Cloutier, Amber A. Medina, Jonathan M. Irwin, David Charbonneau, Nicola Astudillo-Defru, Xavier Bonfils, Andrew W. Howard, Howard Isaacson, Jacob L. Bean, Andreas Seifahrt, Johanna K. Teske, Jason D. Eastman, Joseph D. Twicken, Karen A. Collins, Eric L. N. Jensen, Samuel N. Quinn, Matthew J. Payne, Martti H. Kristiansen, Alton Spencer, Andrew Vanderburg, Mathias Zechmeister, Lauren M. Weiss, Sharon Xuesong Wang, Gavin Wang, Stéphane Udry, Ivan A. Terentev, Julian Stürmer, Gudmundur Stefánsson, Avi Shporer, Stephen Shectman, Ramotholo Sefako, Hans Martin Schwengeler, Richard P. Schwarz, Nicholas Scarsdale, Ryan A. Rubenzahl, Arpita Roy, Lee J. Rosenthal, Paul Robertson, Erik A. Petigura, Francesco Pepe, Mark Omohundro, Joseph M. Akana Murphy, Felipe Murgas, Teo Močnik, Benjamin T. Montet, Ronald Mennickent, Andrew W. Mayo, Bob Massey, Jack Lubin, Christophe Lovis, Pablo Lewin, David Kasper, Stephen R. Kane, Jon M. Jenkins, Daniel Huber, Keith Horne, Michelle L. Hill, Paula Gorrini, Steven Giacalone, Benjamin Fulton, Thierry Forveille, Pedro Figueira, Tara Fetherolf, Courtney Dressing, Rodrigo F. Díaz, Xavier Delfosse, Paul A. Dalba, Fei Dai, C. C. Cortés, Ian J. M. Crossfield, Jeffrey D. Crane, Dennis M. Conti, Kevin I. Collins, Ashley Chontos, R. Paul Butler, Peyton Brown, Madison Brady, Aida Behmard, Corey Beard, Natalie M. Batalha, and Jose-Manuel Almenara
Figure caption: The TESS PDCSAP light curves from sector 4 (top 3 panels) and 31 (bottom 3 panels) data. The top panels of each plot are the nondetrended light curves from each sector of data, which show evidence of flares and rotational modulation due to stellar spots on either the B or C component. The purple lines indicates the fits to the modulations. The middle panels of each plot show the residual data after the removal of the stellar variability with GP regression; the planetary transit models for the 5.36 day planet (purple line) and 3.12 day planet (orange line) are overplotted. The dotted lines indicate transits that occurred during a data download, and which were not observed. The bottom panels of each plot illustrate the light curves with planetary transits and stellar variability removed.
Paper: A Second Planet Transiting LTT 1445A and a Determination of the Masses of Both Worlds
Authors: Jennifer G. Winters, Ryan Cloutier, Amber A. Medina, Jonathan M. Irwin, David Charbonneau, Nicola Astudillo-Defru, Xavier Bonfils, Andrew W. Howard, Howard Isaacson, Jacob L. Bean, Andreas Seifahrt, Johanna K. Teske, Jason D. Eastman, Joseph D. Twicken, Karen A. Collins, Eric L. N. Jensen, Samuel N. Quinn, Matthew J. Payne, Martti H. Kristiansen, Alton Spencer, Andrew Vanderburg, Mathias Zechmeister, Lauren M. Weiss, Sharon Xuesong Wang, Gavin Wang, Stéphane Udry, Ivan A. Terentev, Julian Stürmer, Gudmundur Stefánsson, Avi Shporer, Stephen Shectman, Ramotholo Sefako, Hans Martin Schwengeler, Richard P. Schwarz, Nicholas Scarsdale, Ryan A. Rubenzahl, Arpita Roy, Lee J. Rosenthal, Paul Robertson, Erik A. Petigura, Francesco Pepe, Mark Omohundro, Joseph M. Akana Murphy, Felipe Murgas, Teo Močnik, Benjamin T. Montet, Ronald Mennickent, Andrew W. Mayo, Bob Massey, Jack Lubin, Christophe Lovis, Pablo Lewin, David Kasper, Stephen R. Kane, Jon M. Jenkins, Daniel Huber, Keith Horne, Michelle L. Hill, Paula Gorrini, Steven Giacalone, Benjamin Fulton, Thierry Forveille, Pedro Figueira, Tara Fetherolf, Courtney Dressing, Rodrigo F. Díaz, Xavier Delfosse, Paul A. Dalba, Fei Dai, C. C. Cortés, Ian J. M. Crossfield, Jeffrey D. Crane, Dennis M. Conti, Kevin I. Collins, Ashley Chontos, R. Paul Butler, Peyton Brown, Madison Brady, Aida Behmard, Corey Beard, Natalie M. Batalha, and Jose-Manuel Almenara
Figure caption: Lomb–Scargle periodogram of the residuals from the 5.36 day planet fit to the RV data of LTT 1445A. False alarm probabilities of 10%, 1% and 1 × 10−5% are noted (black dashed lines), as are the orbital periods for the 3.12 and 5.36 day period planets (dotted and solid orange and purple lines, respectively). A highly significant peak at 3.12 days is evident, which confirms that the 3.12 day planet also orbits LTT 1445A.
Paper: A Second Planet Transiting LTT 1445A and a Determination of the Masses of Both Worlds
Authors: Jennifer G. Winters, Ryan Cloutier, Amber A. Medina, Jonathan M. Irwin, David Charbonneau, Nicola Astudillo-Defru, Xavier Bonfils, Andrew W. Howard, Howard Isaacson, Jacob L. Bean, Andreas Seifahrt, Johanna K. Teske, Jason D. Eastman, Joseph D. Twicken, Karen A. Collins, Eric L. N. Jensen, Samuel N. Quinn, Matthew J. Payne, Martti H. Kristiansen, Alton Spencer, Andrew Vanderburg, Mathias Zechmeister, Lauren M. Weiss, Sharon Xuesong Wang, Gavin Wang, Stéphane Udry, Ivan A. Terentev, Julian Stürmer, Gudmundur Stefánsson, Avi Shporer, Stephen Shectman, Ramotholo Sefako, Hans Martin Schwengeler, Richard P. Schwarz, Nicholas Scarsdale, Ryan A. Rubenzahl, Arpita Roy, Lee J. Rosenthal, Paul Robertson, Erik A. Petigura, Francesco Pepe, Mark Omohundro, Joseph M. Akana Murphy, Felipe Murgas, Teo Močnik, Benjamin T. Montet, Ronald Mennickent, Andrew W. Mayo, Bob Massey, Jack Lubin, Christophe Lovis, Pablo Lewin, David Kasper, Stephen R. Kane, Jon M. Jenkins, Daniel Huber, Keith Horne, Michelle L. Hill, Paula Gorrini, Steven Giacalone, Benjamin Fulton, Thierry Forveille, Pedro Figueira, Tara Fetherolf, Courtney Dressing, Rodrigo F. Díaz, Xavier Delfosse, Paul A. Dalba, Fei Dai, C. C. Cortés, Ian J. M. Crossfield, Jeffrey D. Crane, Dennis M. Conti, Kevin I. Collins, Ashley Chontos, R. Paul Butler, Peyton Brown, Madison Brady, Aida Behmard, Corey Beard, Natalie M. Batalha, and Jose-Manuel Almenara
Figure caption: Transits of LTT 1445Ac (top) and LTT 1445Ab (bottom) observed with TESS. The data have been deblended to remove any signal from the stellar BC components and are shown in gray, while the orange and purple lines indicate the models for LTT 1445Ac and LTT 1445Ab.
Paper: A Second Planet Transiting LTT 1445A and a Determination of the Masses of Both Worlds
Authors: Jennifer G. Winters, Ryan Cloutier, Amber A. Medina, Jonathan M. Irwin, David Charbonneau, Nicola Astudillo-Defru, Xavier Bonfils, Andrew W. Howard, Howard Isaacson, Jacob L. Bean, Andreas Seifahrt, Johanna K. Teske, Jason D. Eastman, Joseph D. Twicken, Karen A. Collins, Eric L. N. Jensen, Samuel N. Quinn, Matthew J. Payne, Martti H. Kristiansen, Alton Spencer, Andrew Vanderburg, Mathias Zechmeister, Lauren M. Weiss, Sharon Xuesong Wang, Gavin Wang, Stéphane Udry, Ivan A. Terentev, Julian Stürmer, Gudmundur Stefánsson, Avi Shporer, Stephen Shectman, Ramotholo Sefako, Hans Martin Schwengeler, Richard P. Schwarz, Nicholas Scarsdale, Ryan A. Rubenzahl, Arpita Roy, Lee J. Rosenthal, Paul Robertson, Erik A. Petigura, Francesco Pepe, Mark Omohundro, Joseph M. Akana Murphy, Felipe Murgas, Teo Močnik, Benjamin T. Montet, Ronald Mennickent, Andrew W. Mayo, Bob Massey, Jack Lubin, Christophe Lovis, Pablo Lewin, David Kasper, Stephen R. Kane, Jon M. Jenkins, Daniel Huber, Keith Horne, Michelle L. Hill, Paula Gorrini, Steven Giacalone, Benjamin Fulton, Thierry Forveille, Pedro Figueira, Tara Fetherolf, Courtney Dressing, Rodrigo F. Díaz, Xavier Delfosse, Paul A. Dalba, Fei Dai, C. C. Cortés, Ian J. M. Crossfield, Jeffrey D. Crane, Dennis M. Conti, Kevin I. Collins, Ashley Chontos, R. Paul Butler, Peyton Brown, Madison Brady, Aida Behmard, Corey Beard, Natalie M. Batalha, and Jose-Manuel Almenara
Figure caption: RV orbital plots and residuals from the global ExoFASTv2 two-planet fit. In the top panel, we show the RV data folded at the 3.12 day period (and corrected for the 5.36 day planet, and the slope), with the model for the 3.12 day planet overplotted in gray; residuals to the fit of both planets are shown underneath, phase-folded to the 3.12 day planet period. Similarly, in the third panel, we show the RV data folded at the 5.36 day period (and corrected for the 3.12 day planet, and the slope), with the model for the 5.36 day overplotted in gray; residuals to the fit of both planets are shown underneath, phase-folded to the 5.36 day planet period. The data from ESPRESSO are plotted as orange squares, HARPS as blue circles, HIRES as pale red stars, MAROON-X as purple diamonds, and PFS as green triangles. The bottom panel illustrates the unphased RV data, where the gray curve indicates the combination of the 3.12 day and 5.36 day planet models and the linear slope due to the orbit of LTT 1445A about BC.