adsabs/AstroCLIMB huggingface dataset:
Paper: Detecting Exoplanets Closer to Stars with Moderate Spectral Resolution Integral-field Spectroscopy
Authors: Shubh Agrawal, Jean-Baptiste Ruffio, Quinn M. Konopacky, Bruce Macintosh, Dimitri Mawet, Eric L. Nielsen, Kielan K. W. Hoch, Michael C. Liu, Travis S. Barman, William Thompson, Alexandra Z. Greenbaum, Christian Marois, Jenny Patience
Figure caption: Corner plot showing posteriors for T eff, ﹩\mathrm{log}g﹩, spin, and RV for detected M dwarf companion to HD 148352, from a single 30-second exposure. The best-fit parameters are T eff = 3200 ± 100 K, ﹩\mathrm{log}(g)\gt 4﹩, spin < 25 km s−1, and RV  =   − 8.6 ± 2.5 km s−1. The lower and upper limits are given for a 95% probability. We use an emcee samplers with 512 walkers, 1000 burn-in, and 1000 real samples. breadscan similarly characterize possible exoplanetary detections.
Paper: Detecting Exoplanets Closer to Stars with Moderate Spectral Resolution Integral-field Spectroscopy
Authors: Shubh Agrawal, Jean-Baptiste Ruffio, Quinn M. Konopacky, Bruce Macintosh, Dimitri Mawet, Eric L. Nielsen, Kielan K. W. Hoch, Michael C. Liu, Travis S. Barman, William Thompson, Alexandra Z. Greenbaum, Christian Marois, Jenny Patience
Figure caption: Detection of a binary companion around HD 148352. (a) The left-hand panel illustrates the point-spread function of the host star (red cross) from a median collapsed spectral cube of a 30 s single exposure reduced by the OSIRIS data reduction pipeline. (b) The right-hand panel shows the combined detection map from ≈30 minutes of OSIRIS-Kn5 observations. The signal of the host star has been modeled out and the signal of the companion is highlighted by the blue dot. The S/N ≈34 detection at Δy = Δx = − 0.″08 from the host star is likely to be a previously undetected M dwarf binary companion.
Paper: Detecting Exoplanets Closer to Stars with Moderate Spectral Resolution Integral-field Spectroscopy
Authors: Shubh Agrawal, Jean-Baptiste Ruffio, Quinn M. Konopacky, Bruce Macintosh, Dimitri Mawet, Eric L. Nielsen, Kielan K. W. Hoch, Michael C. Liu, Travis S. Barman, William Thompson, Alexandra Z. Greenbaum, Christian Marois, Jenny Patience
Figure caption: Radial Velocity Cross-Correlation Function for the detected binary, up to a constant scaling factor. We see a peak signal-to-noise at around RV ∼0 km s−1, which is expected for a real astrophysical signal. The supplementary peak at ∼3700 km s−1 corresponds to the wavelength shift between two CO band-heads at 2.294 and 2.323 μm (visible in the bottom right-hand panel of Figure 2).
Paper: Detecting Exoplanets Closer to Stars with Moderate Spectral Resolution Integral-field Spectroscopy
Authors: Shubh Agrawal, Jean-Baptiste Ruffio, Quinn M. Konopacky, Bruce Macintosh, Dimitri Mawet, Eric L. Nielsen, Kielan K. W. Hoch, Michael C. Liu, Travis S. Barman, William Thompson, Alexandra Z. Greenbaum, Christian Marois, Jenny Patience
Figure caption: Zoomed-in section of the combined detection map from Figure 1, which is constructed from ≈30 minutes of OSIRIS-Kn5 observation around HD 148352. The position with the highest S/N is Δx = Δy = 4 pix away from the star, with a 0.02“ plate scale.
Paper: Detecting Exoplanets Closer to Stars with Moderate Spectral Resolution Integral-field Spectroscopy
Authors: Shubh Agrawal, Jean-Baptiste Ruffio, Quinn M. Konopacky, Bruce Macintosh, Dimitri Mawet, Eric L. Nielsen, Kielan K. W. Hoch, Michael C. Liu, Travis S. Barman, William Thompson, Alexandra Z. Greenbaum, Christian Marois, Jenny Patience
Figure caption: Relative signal-to-noise ratio as a function of the true effective temperature of the simulated planets (colored curves) and the model temperature (x axis) used to recover it. Simulated planets are injected at a separation of 100 mas.
Paper: Measuring the Cosmic X-Ray Background in 3–20 KeV with Stray Light from NuSTAR
Authors: Steven Rossland, Daniel R. Wik, Brian Grefenstette, Nico Cappelluti, Francesca Civano, Fabio Gastaldello, Roberto Gilli, Fiona Harrison, Ann Hornschemeier, Ryan Hickox, Roman Krivonos, Kristin Madsen, Silvano Molendi, Andrew Ptak, Daniel Stern, Andreas Zoglauer
Figure caption: The energy spectrum of the CXB as measured in past studies and by CXB Measurement in this work, using the best-fit cutoff power-law model found from joint fits to FPMA (gray crosses) and FPMB (black crosses). Detector components a 0 through a 3 were tied together and limited to a maximum value based on the Earth-occulted NOSUN measurements, and detector a 3 on FPMA was excluded, adjusted for energy bandwidth and exposure time. Below 10 keV, the CXB Measurement measurements agree very well with those from the HEAO 1 A2/A4 analysis (partly obscuring their thin red crosses). Above 10 keV FPMA and FPMB still largely agree with HEAO 1, however the aCXB starts to become less dominant than other background components in CXB Measurement and become strongly influenced by strong emission lines found at these higher energies. (Past CXB measurements are taken from Frontera et al. 2007; Fukada et al. 1975; Georgantopoulos et al. 1993; Gendreau et al. 1995; Kinzer et al. 1997; Watanabe et al. 1997; Gruber et al. 1999; Vecchi et al. 1999; Kushino et al. 2002; Lumb et al. 2002; Revnivtsev et al. 2003; De Luca & Molendi 2004; Hickox & Markevitch 2006; Churazov et al. 2007; Ajello et al. 2008; Moretti et al. 2009; Türler et al. 2010; Cappelluti et al. 2017, as indicated in the plot.)
Paper: Measuring the Cosmic X-Ray Background in 3–20 KeV with Stray Light from NuSTAR
Authors: Steven Rossland, Daniel R. Wik, Brian Grefenstette, Nico Cappelluti, Francesca Civano, Fabio Gastaldello, Roberto Gilli, Fiona Harrison, Ann Hornschemeier, Ryan Hickox, Roman Krivonos, Kristin Madsen, Silvano Molendi, Andrew Ptak, Daniel Stern, Andreas Zoglauer
Figure caption: Stacked images from 3 to 8 keV of the Earth-occulted data for FPMA (left column) and FPMB (right column) during periods when CXB Measurement is illuminated by the Sun (top row) and when it is in Earth’s shadow (bottom row). A shadow pattern very similar to that produced by the CXB is apparent in the Sun-illuminated images but disappears when CXB Measurement is in Earth’s shadow.
Paper: Measuring the Cosmic X-Ray Background in 3–20 KeV with Stray Light from NuSTAR
Authors: Steven Rossland, Daniel R. Wik, Brian Grefenstette, Nico Cappelluti, Francesca Civano, Fabio Gastaldello, Roberto Gilli, Fiona Harrison, Ann Hornschemeier, Ryan Hickox, Roman Krivonos, Kristin Madsen, Silvano Molendi, Andrew Ptak, Daniel Stern, Andreas Zoglauer
Figure caption: Measurements of the aCXB component extracted from spatial fits in narrow energy bands for FPMA (black) and FPMB (red) of the Blank Sky list (top panel) and the Full Sky list (bottom panel), jointly fit with the cutoff power-law model. For each observation set, the upper panel shows the measurements and best-fit model, in units of counts s−1 keV−1 deg−2, and the lower panel gives the ratio of the data to the model.
Paper: Measuring the Cosmic X-Ray Background in 3–20 KeV with Stray Light from NuSTAR
Authors: Steven Rossland, Daniel R. Wik, Brian Grefenstette, Nico Cappelluti, Francesca Civano, Fabio Gastaldello, Roberto Gilli, Fiona Harrison, Ann Hornschemeier, Ryan Hickox, Roman Krivonos, Kristin Madsen, Silvano Molendi, Andrew Ptak, Daniel Stern, Andreas Zoglauer
Figure caption: Left: spectra extracted from stray-light observations of the Crab fit to a power-law model. The data points are derived from fits to narrow-band images performed in the same way as in the CXB analysis. Right: detector images for ObsID 10110005001 of FPMB in the 20–40 keV (top) and 3–20 keV (below) energy ranges. Above 20 keV the aperture stops start to become transparent, as evidenced by the additional half-circle stray-light patterns seen in the top image. More information can be found in Madsen et al. (2017a).
Paper: Measuring the Cosmic X-Ray Background in 3–20 KeV with Stray Light from NuSTAR
Authors: Steven Rossland, Daniel R. Wik, Brian Grefenstette, Nico Cappelluti, Francesca Civano, Fabio Gastaldello, Roberto Gilli, Fiona Harrison, Ann Hornschemeier, Ryan Hickox, Roman Krivonos, Kristin Madsen, Silvano Molendi, Andrew Ptak, Daniel Stern, Andreas Zoglauer
Figure caption: Earth-occulted stacked image for FPMB made from the default 02 nupipeline filtering (left) and the same stacked image after applying an elevation limit of ELV < −3° with nuscreen (right). The bright blob in the middle of the left image is the integrated sum of point-source photons from target sources that were not completely obscured by the limb of the Earth due to the OCC data files starting to accept data before the limb is within the FOV.
Paper: Measuring the Cosmic X-Ray Background in 3–20 KeV with Stray Light from NuSTAR
Authors: Steven Rossland, Daniel R. Wik, Brian Grefenstette, Nico Cappelluti, Francesca Civano, Fabio Gastaldello, Roberto Gilli, Fiona Harrison, Ann Hornschemeier, Ryan Hickox, Roman Krivonos, Kristin Madsen, Silvano Molendi, Andrew Ptak, Daniel Stern, Andreas Zoglauer
Figure caption: Same as Figure 12 but for the full observational catalog with the full exposure time, ∼18 Ms per telescope. The increase in exposure time provides better agreement between FPMA and FPMB. The fluxes in Table 3 for FPMB are similar to those reported for FPMB in the NOSUN data sets.
Paper: Measuring the Cosmic X-Ray Background in 3–20 KeV with Stray Light from NuSTAR
Authors: Steven Rossland, Daniel R. Wik, Brian Grefenstette, Nico Cappelluti, Francesca Civano, Fabio Gastaldello, Roberto Gilli, Fiona Harrison, Ann Hornschemeier, Ryan Hickox, Roman Krivonos, Kristin Madsen, Silvano Molendi, Andrew Ptak, Daniel Stern, Andreas Zoglauer
Figure caption: Top: stacked data for the Blank Sky list in the energy band 3–8 keV with a total exposure of ∼7 Ms for each telescope. Bottom: model images created from the best-fit parameters of Equation (1) multiplied by the exposure maps. Slight offsets in the gradient pattern are due to differing instrumental a  i  contributions. FPMA and FPMB are shown in the left and right columns, respectively.
Paper: Measuring the Cosmic X-Ray Background in 3–20 KeV with Stray Light from NuSTAR
Authors: Steven Rossland, Daniel R. Wik, Brian Grefenstette, Nico Cappelluti, Francesca Civano, Fabio Gastaldello, Roberto Gilli, Fiona Harrison, Ann Hornschemeier, Ryan Hickox, Roman Krivonos, Kristin Madsen, Silvano Molendi, Andrew Ptak, Daniel Stern, Andreas Zoglauer
Figure caption: FPMA (top) and FPMB (bottom) measurements from all observations between Galactic latitudes 10° < ∣b∣ < 30° (stars) and ∣b∣ ≥ 30° (circles). In both spectra at lower b, an excess is present around the Fe complex, marked by the red arrows—a known feature of the GRXE but generally absent in CXB measurements, as evidenced by the ∣b∣ ≥ 30° spectra.
Paper: Measuring the Cosmic X-Ray Background in 3–20 KeV with Stray Light from NuSTAR
Authors: Steven Rossland, Daniel R. Wik, Brian Grefenstette, Nico Cappelluti, Francesca Civano, Fabio Gastaldello, Roberto Gilli, Fiona Harrison, Ann Hornschemeier, Ryan Hickox, Roman Krivonos, Kristin Madsen, Silvano Molendi, Andrew Ptak, Daniel Stern, Andreas Zoglauer
Figure caption: Spectra of stacked observations of Earth-occulted data from FPMB separated into periods when the observatory is illuminated by the Sun (black) or is in Earth’s shadow (red).
Paper: Multiplicity Boost of Transit Signal Classifiers: Validation of 69 New Exoplanets using the Multiplicity Boost of ExoMiner
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Douglas A. Caldwell, Joseph D. Twicken, Stephen T. Bryson
Figure caption: The mapping between ExoMiner scores and the boosted scores using the logistic regression classifier. Each colored curve represents the mapping for a different multiplicity scenario ﹩\left[{N}_{\mathrm{FPs}}(x),\,{N}_{\mathrm{CPs}}(x),\,{N}_{\mathrm{UNKs}}(x)\right]﹩. Scenarios are only plotted if they have more than 10 counts in the Kepler Q1-Q17 DR25 KOI catalog. The larger the number of existing CPs (N CPs(x)), the more the logistic regression classifier favors classification as an exoplanet.
Paper: Multiplicity Boost of Transit Signal Classifiers: Validation of 69 New Exoplanets using the Multiplicity Boost of ExoMiner
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Douglas A. Caldwell, Joseph D. Twicken, Stephen T. Bryson
Figure caption: The newly validated exoplanets are shown using black circles. The mapping lines between ExoMiner scores and the boosted scores for each tuple ﹩\left[{N}_{\mathrm{FPs}}(x),\,{N}_{\mathrm{CPs}}(x),\,{N}_{\mathrm{UNKs}}(x)\right]﹩ setting are displayed using solid lines. Lines are only plotted for tuples that are represented in the unknown KOIs.
Paper: Multiplicity Boost of Transit Signal Classifiers: Validation of 69 New Exoplanets using the Multiplicity Boost of ExoMiner
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Douglas A. Caldwell, Joseph D. Twicken, Stephen T. Bryson
Figure caption: The machine learning model to boost the performance of a given classifier using multiplicity information.
Paper: Multiplicity Boost of Transit Signal Classifiers: Validation of 69 New Exoplanets using the Multiplicity Boost of ExoMiner
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Douglas A. Caldwell, Joseph D. Twicken, Stephen T. Bryson
Figure caption: An adapted version of the classifier in Valizadegan et al. (2022). The red-dotted rectangles show the differences between ExoMiner and ExoMiner V1.2.
Paper: Multiplicity Boost of Transit Signal Classifiers: Validation of 69 New Exoplanets using the Multiplicity Boost of ExoMiner
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Douglas A. Caldwell, Joseph D. Twicken, Stephen T. Bryson
Figure caption: Planet radius vs. orbital period for confirmed transiting planets and validated planets in this paper. The CPs are indicated by the discovery source with Kepler indicated by “+,” K2 by a diamond “⋄,” and TESS by “*.” ExoMiner V1.2-boosted validated planets are indicated by a magenta square. For reference, Earth is indicated by a black circle.
Paper: Multiplicity Boost of Transit Signal Classifiers: Validation of 69 New Exoplanets using the Multiplicity Boost of ExoMiner
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Douglas A. Caldwell, Joseph D. Twicken, Stephen T. Bryson
Figure caption: The score mapping of the existing exoplanets and FPs in the training data. We only show lines for tuples ﹩\left[{N}_{\mathrm{FPs}}(x),\,{N}_{\mathrm{CPs}}(x),\,{N}_{\mathrm{UNKs}}(x)\right]﹩ with more than 10 points in the known KOI data for clarity. The lines for tuples with less than ten points exhibit similar patterns.
Paper: Multiplicity Boost of Transit Signal Classifiers: Validation of 69 New Exoplanets using the Multiplicity Boost of ExoMiner
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Douglas A. Caldwell, Joseph D. Twicken, Stephen T. Bryson
Figure caption: Two machine learning models to use multiplicity boost information.
Paper: Multiplicity Boost of Transit Signal Classifiers: Validation of 69 New Exoplanets using the Multiplicity Boost of ExoMiner
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Douglas A. Caldwell, Joseph D. Twicken, Stephen T. Bryson
Figure caption: Planet radius vs. energy received by planet for confirmed transiting planets and the validated planets in this paper. The symbols are the same as in Figure 7.
Paper: A Transiting Super-Earth in the Radius Valley and an Outer Planet Candidate Around HD 307842
Authors: Xinyan Hua, Sharon Xuesong Wang, Johanna K. Teske, Tianjun Gan, Avi Shporer, George Zhou, Keivan G. Stassun, Markus Rabus, Steve B. Howell, Carl Ziegler, Jack J. Lissauer, Joshua N. Winn, Jon M. Jenkins, Eric B. Ting, Karen A. Collins, Andrew W. Mann, Wei Zhu, Su Wang, R. Paul Butler, Jeffrey D. Crane, Stephen A. Shectman, Luke G. Bouma, César Briceño, Diana Dragomir, William Fong, Nicholas Law, Jennifer V. Medina, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Chris Stockdale, Roland Vanderspek, Joel Villaseñor
Figure caption: The ln(MAP) values of an MAP grid search in the (P  c , K  c ) space using RadVel. Grids placed in a log-uniform distribution were applied along the P  c  and K  c  axes. The region framed by the gray dashed lines was also mapped with another uniformly distributed grid with a smaller interval. As informed in the upper-left legend, different ranges of the ln(MAP) values are marked by different colors. We treat the periods whose ln(MAP) values differ by five from the highest ln(MAP) value to be “the most possible solutions” of the planet candidate. The cyan region is the least favored solution with ln(MAP) differences larger than 30. We also explored the K  c  space between 30 and 60 m s−1 but did not find any plausible solutions, hence it is not plotted here.
Paper: A Transiting Super-Earth in the Radius Valley and an Outer Planet Candidate Around HD 307842
Authors: Xinyan Hua, Sharon Xuesong Wang, Johanna K. Teske, Tianjun Gan, Avi Shporer, George Zhou, Keivan G. Stassun, Markus Rabus, Steve B. Howell, Carl Ziegler, Jack J. Lissauer, Joshua N. Winn, Jon M. Jenkins, Eric B. Ting, Karen A. Collins, Andrew W. Mann, Wei Zhu, Su Wang, R. Paul Butler, Jeffrey D. Crane, Stephen A. Shectman, Luke G. Bouma, César Briceño, Diana Dragomir, William Fong, Nicholas Law, Jennifer V. Medina, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Chris Stockdale, Roland Vanderspek, Joel Villaseñor
Figure caption: Top: corner plot of the posteriors of partial variable parameters in the two-planet fit using Juliet at n live = 5000. Bottom: an enlarged version of the P  c −K  c  posterior space. The histogram of P  c  is plotted on a log scale.
Paper: A Transiting Super-Earth in the Radius Valley and an Outer Planet Candidate Around HD 307842
Authors: Xinyan Hua, Sharon Xuesong Wang, Johanna K. Teske, Tianjun Gan, Avi Shporer, George Zhou, Keivan G. Stassun, Markus Rabus, Steve B. Howell, Carl Ziegler, Jack J. Lissauer, Joshua N. Winn, Jon M. Jenkins, Eric B. Ting, Karen A. Collins, Andrew W. Mann, Wei Zhu, Su Wang, R. Paul Butler, Jeffrey D. Crane, Stephen A. Shectman, Luke G. Bouma, César Briceño, Diana Dragomir, William Fong, Nicholas Law, Jennifer V. Medina, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Chris Stockdale, Roland Vanderspek, Joel Villaseñor
Figure caption: The one-planet RV fit with two independent trends in the model. The orange and purple dots represent the first and second year PFS data, respectively. The best-fit model is shown by the thin blue line. (b) The linear residuals after subtracting the signal from TOI-784 b. (c) The phase-folded RV plot of TOI-784 b. Red circles are the same velocities binned in 0.08 units of the orbital phase.
Paper: A Transiting Super-Earth in the Radius Valley and an Outer Planet Candidate Around HD 307842
Authors: Xinyan Hua, Sharon Xuesong Wang, Johanna K. Teske, Tianjun Gan, Avi Shporer, George Zhou, Keivan G. Stassun, Markus Rabus, Steve B. Howell, Carl Ziegler, Jack J. Lissauer, Joshua N. Winn, Jon M. Jenkins, Eric B. Ting, Karen A. Collins, Andrew W. Mann, Wei Zhu, Su Wang, R. Paul Butler, Jeffrey D. Crane, Stephen A. Shectman, Luke G. Bouma, César Briceño, Diana Dragomir, William Fong, Nicholas Law, Jennifer V. Medina, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Chris Stockdale, Roland Vanderspek, Joel Villaseñor
Figure caption: Relation of planet insolation flux and radius. Forward blue points are exoplanets with data taken from the NASA exoplanet archive and background contours indicate their number density. The dashed line illustrates theoretical predictions under gas-poor formation scenarios (Lopez & Rice 2018), while the black dotted line is derived by Martinez et al. (2019) using the CKS sample with the shaded green region representing the 1σ error.
Paper: A Transiting Super-Earth in the Radius Valley and an Outer Planet Candidate Around HD 307842
Authors: Xinyan Hua, Sharon Xuesong Wang, Johanna K. Teske, Tianjun Gan, Avi Shporer, George Zhou, Keivan G. Stassun, Markus Rabus, Steve B. Howell, Carl Ziegler, Jack J. Lissauer, Joshua N. Winn, Jon M. Jenkins, Eric B. Ting, Karen A. Collins, Andrew W. Mann, Wei Zhu, Su Wang, R. Paul Butler, Jeffrey D. Crane, Stephen A. Shectman, Luke G. Bouma, César Briceño, Diana Dragomir, William Fong, Nicholas Law, Jennifer V. Medina, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Chris Stockdale, Roland Vanderspek, Joel Villaseñor
Figure caption: The M–R relation. The background gray dots are planets from the TEPCAT database. Solid and dashed curves indicate different planet compositions. TOI-784 b (the red point) is between the green and orange lines representing a MgSiO3 core and Earth composition, respectively, which implies that TOI-784 b is a rocky planet, i.e., the same conclusion found in our analyses. Considering the uncertainty of the planet size, TOI-784 b could be pure rocky or have a small amount of atmosphere consisting of heavy elements (e.g., H2O, CO2, etc.).
Paper: A Transiting Super-Earth in the Radius Valley and an Outer Planet Candidate Around HD 307842
Authors: Xinyan Hua, Sharon Xuesong Wang, Johanna K. Teske, Tianjun Gan, Avi Shporer, George Zhou, Keivan G. Stassun, Markus Rabus, Steve B. Howell, Carl Ziegler, Jack J. Lissauer, Joshua N. Winn, Jon M. Jenkins, Eric B. Ting, Karen A. Collins, Andrew W. Mann, Wei Zhu, Su Wang, R. Paul Butler, Jeffrey D. Crane, Stephen A. Shectman, Luke G. Bouma, César Briceño, Diana Dragomir, William Fong, Nicholas Law, Jennifer V. Medina, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Chris Stockdale, Roland Vanderspek, Joel Villaseñor
Figure caption: The result of the transit injection-and-recovery test for the planet candidate. Blue to light green represents an increasing detection possibility of its transit signal (assuming it transits). The solid blue histogram in the top panel illustrates the average number of transits within the TESS time baseline. The foreground yellow solid lines mark the six possible orbital solutions of the planet candidate found in Juliet.
Paper: A Transiting Super-Earth in the Radius Valley and an Outer Planet Candidate Around HD 307842
Authors: Xinyan Hua, Sharon Xuesong Wang, Johanna K. Teske, Tianjun Gan, Avi Shporer, George Zhou, Keivan G. Stassun, Markus Rabus, Steve B. Howell, Carl Ziegler, Jack J. Lissauer, Joshua N. Winn, Jon M. Jenkins, Eric B. Ting, Karen A. Collins, Andrew W. Mann, Wei Zhu, Su Wang, R. Paul Butler, Jeffrey D. Crane, Stephen A. Shectman, Luke G. Bouma, César Briceño, Diana Dragomir, William Fong, Nicholas Law, Jennifer V. Medina, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Chris Stockdale, Roland Vanderspek, Joel Villaseñor
Figure caption: Detection probability as a function of the planet radius. Different colors correspond to the six possible periods of the planet candidate estimated from Juliet, as shown in the legend. The results here incorporate the phase information from the RV data, and thus they are different from Figure 12, which used a random phase.
Paper: A Transiting Super-Earth in the Radius Valley and an Outer Planet Candidate Around HD 307842
Authors: Xinyan Hua, Sharon Xuesong Wang, Johanna K. Teske, Tianjun Gan, Avi Shporer, George Zhou, Keivan G. Stassun, Markus Rabus, Steve B. Howell, Carl Ziegler, Jack J. Lissauer, Joshua N. Winn, Jon M. Jenkins, Eric B. Ting, Karen A. Collins, Andrew W. Mann, Wei Zhu, Su Wang, R. Paul Butler, Jeffrey D. Crane, Stephen A. Shectman, Luke G. Bouma, César Briceño, Diana Dragomir, William Fong, Nicholas Law, Jennifer V. Medina, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Chris Stockdale, Roland Vanderspek, Joel Villaseñor
Figure caption: Phase-folded RV plots of the planet candidate with the most probable six periods from the two-planet fit in Juliet. We assumed a circular orbit for the planet candidate in all cases. PFS RVs are shown in magenta, with the big red dots representing the binned data points.