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Paper: JWST MIRI MRS Observations of T Cha: Discovery of a Spatially Resolved Disk Wind
Authors: Naman S. Bajaj, Ilaria Pascucci, Uma Gorti, Richard Alexander, Andrew Sellek, Jane Morrison, Andras Gaspar, Cathie Clarke, Chengyan Xie, Giulia Ballabio, Dingshan Deng
Figure caption: The left two panels compare the radial profiles of continuum and continuum-subtracted lines with the PSF (standard star HD 37962) in the horizontal and vertical directions. The two panels on the right show the PSF-subtracted images of the continuum at 12.81 and 7 μm and the [Ne II] and [Ar II] lines. The white contours in the PSF-subtracted images follow 5× the rms calculated in the source-emission-free regions in the PSF-subtracted images.
Paper: JWST MIRI MRS Observations of T Cha: Discovery of a Spatially Resolved Disk Wind
Authors: Naman S. Bajaj, Ilaria Pascucci, Uma Gorti, Richard Alexander, Andrew Sellek, Jane Morrison, Andras Gaspar, Cathie Clarke, Chengyan Xie, Giulia Ballabio, Dingshan Deng
Figure caption: Comparison of the 2D Gaussian size calculated from images of the continuum-subtracted line, T Cha continuum (represented as Cont), and standard star (represented as Std Star). The three are compared at the same wavelength for [Ar II], [Ne II], and [Ne III], respectively.
Paper: JWST MIRI MRS Observations of T Cha: Discovery of a Spatially Resolved Disk Wind
Authors: Naman S. Bajaj, Ilaria Pascucci, Uma Gorti, Richard Alexander, Andrew Sellek, Jane Morrison, Andras Gaspar, Cathie Clarke, Chengyan Xie, Giulia Ballabio, Dingshan Deng
Figure caption: The left two panels compare the radial profiles of continuum and continuum-subtracted lines with the PSF (standard star HD 167060) in the horizontal and vertical directions. The two panels on the right show the PSF-subtracted images of the continuum at 12.81 and 7 μm and the [Ne II] and [Ar II] lines. The white contours in the images follow 5σ emission.
Paper: JWST MIRI MRS Observations of T Cha: Discovery of a Spatially Resolved Disk Wind
Authors: Naman S. Bajaj, Ilaria Pascucci, Uma Gorti, Richard Alexander, Andrew Sellek, Jane Morrison, Andras Gaspar, Cathie Clarke, Chengyan Xie, Giulia Ballabio, Dingshan Deng
Figure caption: The upper panel is the JWST MIRI MRS spectrum of T Cha plotted between ∼5 and ∼28 μm with the PAH features and H2ν0-0 S(3) line marked in black and the forbidden noble gas emissions in green. The lower four panels further highlight the four forbidden line emissions, [Ar II], [Ar III], [Ne II], and [Ne III], which will be the focus of this study.(The data used to create this figure are available.)
Paper: JWST MIRI MRS Observations of T Cha: Discovery of a Spatially Resolved Disk Wind
Authors: Naman S. Bajaj, Ilaria Pascucci, Uma Gorti, Richard Alexander, Andrew Sellek, Jane Morrison, Andras Gaspar, Cathie Clarke, Chengyan Xie, Giulia Ballabio, Dingshan Deng
Figure caption: The figure shows JWST MIRI MRS spectral profiles for the lines listed in Table 1 in blue and the performed Gaussian fit in orange. The green dashed line indicates the rest wavelength of the transition. Each subplot has the same length of the wavelength range (∼0.055 μm) plotted on the x-axis with the lines peaking at the center.
Paper: JWST MIRI MRS Observations of T Cha: Discovery of a Spatially Resolved Disk Wind
Authors: Naman S. Bajaj, Ilaria Pascucci, Uma Gorti, Richard Alexander, Andrew Sellek, Jane Morrison, Andras Gaspar, Cathie Clarke, Chengyan Xie, Giulia Ballabio, Dingshan Deng
Figure caption: The two panels compare the radial profiles of continuum and continuum-subtracted PAH emission with the PSF/standard star in the horizontal and vertical directions.
Paper: The TESS–Keck Survey. XIX. A Warm Transiting Sub-Saturn-mass Planet and a Nontransiting Saturn-mass Planet Orbiting a Solar Analog
Authors: Michelle L. Hill, Stephen R. Kane, Paul A. Dalba, Mason MacDougall, Tara Fetherolf, Zhexing Li, Daria Pidhorodetska, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Lea A. Hirsch, Rae Holcomb, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Judah Van Zandt, Allyson Bieryla, David R. Ciardi, Jason D. Eastman, Ben Falk, Katharine M. Hesse, David W. Latham, John Livingston, Rachel A. Matson, Elisabeth Matthews, George R. Ricker, Alexander Rudat, Joshua E. Schlieder, S. Seager, Joshua N. Winn
Figure caption: Top: TESS full light curve for Sectors 16, 17, 56, and 57. Sectors 16 and 17 have 30 minute cadence, processed from the fast-frame images and Sectors 56 and 57 have 2 minute cadence processed by the SPOC pipeline. TESS discovered three transits of TOI-1386 in (from top) Sectors 16, 17, and 56. The best-fit period for the transiting planet positions a transit in the data gap of Sector 57 and hence a fourth transit was not recovered. Bottom left: the three transits of TOI-1386 discovered by TESS in (from top) Sectors 16, 17, and 56. The red lines show the best-fit model to each individual transit found with EXOFASTv2. Bottom right: EXOFASTv2 combined these transits with the RV data to determine the best-fit model (red line). The residuals to the fit are shown below the transit model.
Paper: The TESS–Keck Survey. XIX. A Warm Transiting Sub-Saturn-mass Planet and a Nontransiting Saturn-mass Planet Orbiting a Solar Analog
Authors: Michelle L. Hill, Stephen R. Kane, Paul A. Dalba, Mason MacDougall, Tara Fetherolf, Zhexing Li, Daria Pidhorodetska, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Lea A. Hirsch, Rae Holcomb, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Judah Van Zandt, Allyson Bieryla, David R. Ciardi, Jason D. Eastman, Ben Falk, Katharine M. Hesse, David W. Latham, John Livingston, Rachel A. Matson, Elisabeth Matthews, George R. Ricker, Alexander Rudat, Joshua E. Schlieder, S. Seager, Joshua N. Winn
Figure caption: Left: the Gemini/NIRI contrast curve and AO image (inset). The curve shows the limiting magnitudes (Δmag) for the nondetection of a neighboring star. At 1″ of separation we achieve a Δmag > 7. Two visual neighbors can be seen in the AO image, one with a magnitude difference of ΔKmag = 1.25 ± 0.01 and separation of ∼10.″5. The other has a separation of ∼7″ and a ΔKmag = 7.23 ± 0.13 (shown with a different color scaling). Both of these neighboring stars have a parallax difference to TOI-1386 of ≥7 mas (Gaia Collaboration et al. 2021). Right: limiting magnitudes for the nondetection of a neighboring star based on the speckle imaging from the NESSI speckle imager on the WIYN telescope.
Paper: The TESS–Keck Survey. XIX. A Warm Transiting Sub-Saturn-mass Planet and a Nontransiting Saturn-mass Planet Orbiting a Solar Analog
Authors: Michelle L. Hill, Stephen R. Kane, Paul A. Dalba, Mason MacDougall, Tara Fetherolf, Zhexing Li, Daria Pidhorodetska, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Lea A. Hirsch, Rae Holcomb, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Judah Van Zandt, Allyson Bieryla, David R. Ciardi, Jason D. Eastman, Ben Falk, Katharine M. Hesse, David W. Latham, John Livingston, Rachel A. Matson, Elisabeth Matthews, George R. Ricker, Alexander Rudat, Joshua E. Schlieder, S. Seager, Joshua N. Winn
Figure caption: Top: the S-value and velocity correlation. We found a Pearson correlation coefficient of 0.62 between the S HK values and RVs. Bottom left: RV periodogram, with a maximum peak at 227 days. Note the secondary peak at 787 days was investigated and ruled out as the solution to the fit. Bottom right: the S-value periodogram, with a maximum peak at ∼1300 days and another peak at 234 days. We tested our model for the outer planet via the methods outlined in Section 4.2 and concluded that the RV signals were not caused by stellar activity.
Paper: The TESS–Keck Survey. XIX. A Warm Transiting Sub-Saturn-mass Planet and a Nontransiting Saturn-mass Planet Orbiting a Solar Analog
Authors: Michelle L. Hill, Stephen R. Kane, Paul A. Dalba, Mason MacDougall, Tara Fetherolf, Zhexing Li, Daria Pidhorodetska, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Lea A. Hirsch, Rae Holcomb, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Judah Van Zandt, Allyson Bieryla, David R. Ciardi, Jason D. Eastman, Ben Falk, Katharine M. Hesse, David W. Latham, John Livingston, Rachel A. Matson, Elisabeth Matthews, George R. Ricker, Alexander Rudat, Joshua E. Schlieder, S. Seager, Joshua N. Winn
Figure caption: The RV measurements of TOI-1386. (a) Our complete RV time series with our preferred model shown in red. (b) Residuals between the RVs and best-fit two-planet model. Panels (c) and (e) phase-folded RV time series for planets b and c, respectively. Panels (d) and (f) the residuals to each of the planet fits.
Paper: The TESS–Keck Survey. XIX. A Warm Transiting Sub-Saturn-mass Planet and a Nontransiting Saturn-mass Planet Orbiting a Solar Analog
Authors: Michelle L. Hill, Stephen R. Kane, Paul A. Dalba, Mason MacDougall, Tara Fetherolf, Zhexing Li, Daria Pidhorodetska, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Lea A. Hirsch, Rae Holcomb, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Judah Van Zandt, Allyson Bieryla, David R. Ciardi, Jason D. Eastman, Ben Falk, Katharine M. Hesse, David W. Latham, John Livingston, Rachel A. Matson, Elisabeth Matthews, George R. Ricker, Alexander Rudat, Joshua E. Schlieder, S. Seager, Joshua N. Winn
Figure caption: The attributes of planet TOI-1386 b (panels (A)–(D)) and star TOI-1386 (panels (E) and (F)) compared to the population of sub-Saturn planets. TOI-1386 b’s position is indicated by the cross. Planets with a measured mass between 6 and 60 M ⊕ are included in our sub-Saturn population. The color bar for each plot indicates the TSM value of the planet, with TOI-1386 b having a TSM of 42.5. Compared to the rest of the sub-Saturn population, TOI-1386 b is a massive, cool, moderately eccentric planet orbiting a metal-rich Sun-like star.
Paper: The TESS–Keck Survey. XIX. A Warm Transiting Sub-Saturn-mass Planet and a Nontransiting Saturn-mass Planet Orbiting a Solar Analog
Authors: Michelle L. Hill, Stephen R. Kane, Paul A. Dalba, Mason MacDougall, Tara Fetherolf, Zhexing Li, Daria Pidhorodetska, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Lea A. Hirsch, Rae Holcomb, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Judah Van Zandt, Allyson Bieryla, David R. Ciardi, Jason D. Eastman, Ben Falk, Katharine M. Hesse, David W. Latham, John Livingston, Rachel A. Matson, Elisabeth Matthews, George R. Ricker, Alexander Rudat, Joshua E. Schlieder, S. Seager, Joshua N. Winn
Figure caption: Heat map of the mass and radius distribution of exoplanets showing the position of TOI-1386 b (black X) compared to the full catalog of known exoplanets (gray). TOI-1386 b is positioned in the sub-Saturn valley between the cluster of Jupiter-sized planets and that of the super-Earths/Neptunes.
Paper: The TESS–Keck Survey. XIX. A Warm Transiting Sub-Saturn-mass Planet and a Nontransiting Saturn-mass Planet Orbiting a Solar Analog
Authors: Michelle L. Hill, Stephen R. Kane, Paul A. Dalba, Mason MacDougall, Tara Fetherolf, Zhexing Li, Daria Pidhorodetska, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Lea A. Hirsch, Rae Holcomb, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Judah Van Zandt, Allyson Bieryla, David R. Ciardi, Jason D. Eastman, Ben Falk, Katharine M. Hesse, David W. Latham, John Livingston, Rachel A. Matson, Elisabeth Matthews, George R. Ricker, Alexander Rudat, Joshua E. Schlieder, S. Seager, Joshua N. Winn
Figure caption: Eccentricity evolution of the TOI-1386 b and c planets. Shown here are the first 106 yr from the full 107 yr dynamical simulation, described in Section 4.4.
Paper: On the Rigidly Precessing, Eccentric Gas Disk Orbiting the White Dwarf SDSS J1228+1040
Authors: Olcay Ates Goksu, Taylor Kutra, Yanqin Wu
Figure caption: Observed and modeled emission profiles as functions of the precession phase (vertical axis). The data plot is generated using epochs from 2007 April to 2015 May (Manser et al. 2016) and summing over the Ca II infrared triplet. While the overall resemblance is good, we highlight one notable exception. Near phase ϕ = π/2, the observed profile is less symmetric than the model and shows a sharper cutoff at the blue peak (yellow boxes).
Paper: On the Rigidly Precessing, Eccentric Gas Disk Orbiting the White Dwarf SDSS J1228+1040
Authors: Olcay Ates Goksu, Taylor Kutra, Yanqin Wu
Figure caption: Comparing the emission profiles between the model and data for three phases. At ϕ = π/2, we expect symmetry, but the data shows a deficit of emission in the blue wing.
Paper: On the Rigidly Precessing, Eccentric Gas Disk Orbiting the White Dwarf SDSS J1228+1040
Authors: Olcay Ates Goksu, Taylor Kutra, Yanqin Wu
Figure caption: Corner plot for the 1D and 2D marginalized posterior distributions for our model parameters, with the first 2000 steps discarded as burn-in. We see good overall convergence for our parameters.
Paper: On the Rigidly Precessing, Eccentric Gas Disk Orbiting the White Dwarf SDSS J1228+1040
Authors: Olcay Ates Goksu, Taylor Kutra, Yanqin Wu
Figure caption: An illustration of our disk model. We represent the disk using a discreet set of elliptical, aligned, Keplerian rings, with a surface density profile (left panel) that is composed of two broken power laws and an eccentricity profile (middle panel) that is linear in radius. The right panel is a bird's-eye view of the disk with the color indicating normalized emission. This figure is produced using our best-fit parameters. The phase angle ϕ takes the value of 0 if the disk's long axis lies on the plane of the sky.
Paper: On the Rigidly Precessing, Eccentric Gas Disk Orbiting the White Dwarf SDSS J1228+1040
Authors: Olcay Ates Goksu, Taylor Kutra, Yanqin Wu
Figure caption: Comparing our disk model to the linear eigenmode calculations, assuming an inclination of 90°. Solid curves in the left panel show the calculated precession period as a function of temperature at the inner edge for a few choices of γ (Equation (9)). The gray band corresponds to the precession period determined from the data, and the blue dotted line is that of the GR period at the disk's inner edge. The right panel shows the calculated eccentricity eigenfunctions in solid lines (they are too close to tell apart) corresponding to the three-starred positions on the left panel. Our best-fit eccentricity profile is plotted as the thick blue line. The theoretical modes are normalized to have the same eccentricity at the inner edge as the observed one.
Paper: Planet Hunters TESS. V. A Planetary System Around a Binary Star, Including a Mini-Neptune in the Habitable Zone
Authors: Nora L. Eisner, Samuel K. Grunblatt, Oscar Barragán, Thea H. Faridani, Chris Lintott, Suzanne Aigrain, Cole Johnston, Ian R. Mason, Keivan G. Stassun, Megan Bedell, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Guillaume Hebrard, David W. Hogg, Steve B. Howell, Baptiste Klein, Joe Llama, Joshua N. Winn, Lily L. Zhao, Joseph M. Akana Murphy, Corey Beard, Casey L. Brinkman, Ashley Chontos, Pia Cortes-Zuleta, Xavier Delfosse, Steven Giacalone, Emily A. Gilbert, Neda Heidari, Rae Holcomb, Jon M. Jenkins, Flavien Kiefer, Jack Lubin, Eder Martioli, Alex S. Polanski, Nicholas Saunders, Sara Seager, Avi Shporer, Dakotah Tyler, Judah Van Zandt, Safaa Alhassan, Daval J. Amratlal, Lais I. Antonel, Simon L. S. Bentzen, Milton K. D Bosch, David Bundy, Itayi Chitsiga, Jérôme F. Delaunay, Xavier Doisy, Richard Ferstenou, Mark Fynø, James M. Geary, Gerry Haynaly, Pete Hermes, Marc Huten, Sam Lee, Paul Metcalfe, Garry J. Pennell, Joanna Puszkarska, Thomas Schäfer, Lisa Stiller, Christopher Tanner, Allan Tarr, Andrew Wilkinson
Figure caption: Spectral energy distribution of TIC 307958020. Red symbols represent the observed photometric measurements, where the horizontal bars represent the effective width of the passband. Blue symbols are the model fluxes from the best-fit Kurucz atmosphere model (gray) for the combined light of the binary star system. Cyan and red curves represent the Kurucz atmosphere models corresponding to the warmer (larger) and cooler (smaller) stellar components of the system, respectively.
Paper: Planet Hunters TESS. V. A Planetary System Around a Binary Star, Including a Mini-Neptune in the Habitable Zone
Authors: Nora L. Eisner, Samuel K. Grunblatt, Oscar Barragán, Thea H. Faridani, Chris Lintott, Suzanne Aigrain, Cole Johnston, Ian R. Mason, Keivan G. Stassun, Megan Bedell, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Guillaume Hebrard, David W. Hogg, Steve B. Howell, Baptiste Klein, Joe Llama, Joshua N. Winn, Lily L. Zhao, Joseph M. Akana Murphy, Corey Beard, Casey L. Brinkman, Ashley Chontos, Pia Cortes-Zuleta, Xavier Delfosse, Steven Giacalone, Emily A. Gilbert, Neda Heidari, Rae Holcomb, Jon M. Jenkins, Flavien Kiefer, Jack Lubin, Eder Martioli, Alex S. Polanski, Nicholas Saunders, Sara Seager, Avi Shporer, Dakotah Tyler, Judah Van Zandt, Safaa Alhassan, Daval J. Amratlal, Lais I. Antonel, Simon L. S. Bentzen, Milton K. D Bosch, David Bundy, Itayi Chitsiga, Jérôme F. Delaunay, Xavier Doisy, Richard Ferstenou, Mark Fynø, James M. Geary, Gerry Haynaly, Pete Hermes, Marc Huten, Sam Lee, Paul Metcalfe, Garry J. Pennell, Joanna Puszkarska, Thomas Schäfer, Lisa Stiller, Christopher Tanner, Allan Tarr, Andrew Wilkinson
Figure caption: Contrast curves showing the 5σ detection sensitivity and speckle auto-correlation functions obtained using Gemini North/‘Alopeke (left) and Keck II/NIRC2 (right).
Paper: Planet Hunters TESS. V. A Planetary System Around a Binary Star, Including a Mini-Neptune in the Habitable Zone
Authors: Nora L. Eisner, Samuel K. Grunblatt, Oscar Barragán, Thea H. Faridani, Chris Lintott, Suzanne Aigrain, Cole Johnston, Ian R. Mason, Keivan G. Stassun, Megan Bedell, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Guillaume Hebrard, David W. Hogg, Steve B. Howell, Baptiste Klein, Joe Llama, Joshua N. Winn, Lily L. Zhao, Joseph M. Akana Murphy, Corey Beard, Casey L. Brinkman, Ashley Chontos, Pia Cortes-Zuleta, Xavier Delfosse, Steven Giacalone, Emily A. Gilbert, Neda Heidari, Rae Holcomb, Jon M. Jenkins, Flavien Kiefer, Jack Lubin, Eder Martioli, Alex S. Polanski, Nicholas Saunders, Sara Seager, Avi Shporer, Dakotah Tyler, Judah Van Zandt, Safaa Alhassan, Daval J. Amratlal, Lais I. Antonel, Simon L. S. Bentzen, Milton K. D Bosch, David Bundy, Itayi Chitsiga, Jérôme F. Delaunay, Xavier Doisy, Richard Ferstenou, Mark Fynø, James M. Geary, Gerry Haynaly, Pete Hermes, Marc Huten, Sam Lee, Paul Metcalfe, Garry J. Pennell, Joanna Puszkarska, Thomas Schäfer, Lisa Stiller, Christopher Tanner, Allan Tarr, Andrew Wilkinson
Figure caption: Generalized Lomb-Scargle Periodogram of the HIRES and SOPHIE RV data (navy and maroon bold panels, respectively). The non-bold panels show periodograms of various activity indicators for each instrument, while the vertical gray line indicates a period of 34 days. The horizontal dotted orange and dashed gray lines represent the 10% and 30% FAPs, respectively.
Paper: Planet Hunters TESS. V. A Planetary System Around a Binary Star, Including a Mini-Neptune in the Habitable Zone
Authors: Nora L. Eisner, Samuel K. Grunblatt, Oscar Barragán, Thea H. Faridani, Chris Lintott, Suzanne Aigrain, Cole Johnston, Ian R. Mason, Keivan G. Stassun, Megan Bedell, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Guillaume Hebrard, David W. Hogg, Steve B. Howell, Baptiste Klein, Joe Llama, Joshua N. Winn, Lily L. Zhao, Joseph M. Akana Murphy, Corey Beard, Casey L. Brinkman, Ashley Chontos, Pia Cortes-Zuleta, Xavier Delfosse, Steven Giacalone, Emily A. Gilbert, Neda Heidari, Rae Holcomb, Jon M. Jenkins, Flavien Kiefer, Jack Lubin, Eder Martioli, Alex S. Polanski, Nicholas Saunders, Sara Seager, Avi Shporer, Dakotah Tyler, Judah Van Zandt, Safaa Alhassan, Daval J. Amratlal, Lais I. Antonel, Simon L. S. Bentzen, Milton K. D Bosch, David Bundy, Itayi Chitsiga, Jérôme F. Delaunay, Xavier Doisy, Richard Ferstenou, Mark Fynø, James M. Geary, Gerry Haynaly, Pete Hermes, Marc Huten, Sam Lee, Paul Metcalfe, Garry J. Pennell, Joanna Puszkarska, Thomas Schäfer, Lisa Stiller, Christopher Tanner, Allan Tarr, Andrew Wilkinson
Figure caption: Normalized light curve (left), Generalized Lomb-Scargle periodogram (middle), and light curve phase folded at the period of planet candidate b (P  b  = 34.15 ± 0.15 days) for the 2 minutes cadence TESS data (top) and the V-band ASAS-SN data. The vertical blue line in the middle panel indicates the period of planet candidate b, while the horizontal dotted orange and dashed gray lines represent the 10% and 30% FAPs, respectively.
Paper: Planet Hunters TESS. V. A Planetary System Around a Binary Star, Including a Mini-Neptune in the Habitable Zone
Authors: Nora L. Eisner, Samuel K. Grunblatt, Oscar Barragán, Thea H. Faridani, Chris Lintott, Suzanne Aigrain, Cole Johnston, Ian R. Mason, Keivan G. Stassun, Megan Bedell, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Guillaume Hebrard, David W. Hogg, Steve B. Howell, Baptiste Klein, Joe Llama, Joshua N. Winn, Lily L. Zhao, Joseph M. Akana Murphy, Corey Beard, Casey L. Brinkman, Ashley Chontos, Pia Cortes-Zuleta, Xavier Delfosse, Steven Giacalone, Emily A. Gilbert, Neda Heidari, Rae Holcomb, Jon M. Jenkins, Flavien Kiefer, Jack Lubin, Eder Martioli, Alex S. Polanski, Nicholas Saunders, Sara Seager, Avi Shporer, Dakotah Tyler, Judah Van Zandt, Safaa Alhassan, Daval J. Amratlal, Lais I. Antonel, Simon L. S. Bentzen, Milton K. D Bosch, David Bundy, Itayi Chitsiga, Jérôme F. Delaunay, Xavier Doisy, Richard Ferstenou, Mark Fynø, James M. Geary, Gerry Haynaly, Pete Hermes, Marc Huten, Sam Lee, Paul Metcalfe, Garry J. Pennell, Joanna Puszkarska, Thomas Schäfer, Lisa Stiller, Christopher Tanner, Allan Tarr, Andrew Wilkinson
Figure caption: Normalized photometric data from TESS sectors 20–22 to illustrate the stellar variability of the light curve. The first of the three transit events observed by TESS to date is highlighted by the vertical gray column. The normalized 2 minutes cadence flux binned to 10 minutes and unbinned are shown in maroon and gray, respectively.