adsabs/AstroCLIMB huggingface dataset:
Paper: TESS Giants Transiting Giants. I.: A Noninflated Hot Jupiter Orbiting a Massive Subgiant
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, Karen A. Collins, Eric L. N. Jensen, Andrew Vanderburg, Rafael Brahm, Andrés Jordán, Néstor Espinoza, Thomas Henning, Melissa J. Hobson, Samuel N. Quinn, George Zhou, R. Paul Butler, Lisa Crause, Rudi B. Kuhn, K. Moses Mogotsi, Coel Hellier, Ruth Angus, Soichiro Hattori, Ashley Chontos, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, David W. Latham, Sara Seager, Roland K. Vanderspek, Joshua N. Winn, Chris Stockdale, Ryan Cloutier
Figure caption: Hertzsprung–Russell diagram of confirmed exoplanet host stars from TESS. The position of TOI-2184 is marked by the red star. Gray circles show the positions of confirmed TESS planet host stars. We also mark the positions of similar or otherwise notable planet host stars. These values were downloaded from the NASA Exoplanet Archive.
Paper: TESS Giants Transiting Giants. I.: A Noninflated Hot Jupiter Orbiting a Massive Subgiant
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, Karen A. Collins, Eric L. N. Jensen, Andrew Vanderburg, Rafael Brahm, Andrés Jordán, Néstor Espinoza, Thomas Henning, Melissa J. Hobson, Samuel N. Quinn, George Zhou, R. Paul Butler, Lisa Crause, Rudi B. Kuhn, K. Moses Mogotsi, Coel Hellier, Ruth Angus, Soichiro Hattori, Ashley Chontos, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, David W. Latham, Sara Seager, Roland K. Vanderspek, Joshua N. Winn, Chris Stockdale, Ryan Cloutier
Figure caption: The contrast curve for TOI-2184 in two bands: 562 nm and 832 nm. These observations were taken on 2020 March 13 using the Gemini South telescope at CTIO. There are no significant spikes in the contrast curve above Δm > 4 in the 562 nm observation and Δm > 5 in the 832 nm observation, indicating that TOI-2184 has no close companions. The inset figure is a high-contrast speckle image centered on TOI-2184.
Paper: TESS Giants Transiting Giants. I.: A Noninflated Hot Jupiter Orbiting a Massive Subgiant
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, Karen A. Collins, Eric L. N. Jensen, Andrew Vanderburg, Rafael Brahm, Andrés Jordán, Néstor Espinoza, Thomas Henning, Melissa J. Hobson, Samuel N. Quinn, George Zhou, R. Paul Butler, Lisa Crause, Rudi B. Kuhn, K. Moses Mogotsi, Coel Hellier, Ruth Angus, Soichiro Hattori, Ashley Chontos, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, David W. Latham, Sara Seager, Roland K. Vanderspek, Joshua N. Winn, Chris Stockdale, Ryan Cloutier
Figure caption: A comparison between the even and odd transits of TOI-2184b for the first seven sectors (top) and the final four sectors (bottom). Faint points show the original phase-folded photometry and solid lines show the binned photometry.
Paper: TESS Giants Transiting Giants. I.: A Noninflated Hot Jupiter Orbiting a Massive Subgiant
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, Karen A. Collins, Eric L. N. Jensen, Andrew Vanderburg, Rafael Brahm, Andrés Jordán, Néstor Espinoza, Thomas Henning, Melissa J. Hobson, Samuel N. Quinn, George Zhou, R. Paul Butler, Lisa Crause, Rudi B. Kuhn, K. Moses Mogotsi, Coel Hellier, Ruth Angus, Soichiro Hattori, Ashley Chontos, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, David W. Latham, Sara Seager, Roland K. Vanderspek, Joshua N. Winn, Chris Stockdale, Ryan Cloutier
Figure caption: The light curve for TOI-2184b before (top panel) and after (bottom panel) applying our detrending method.
Paper: Revisiting KELT-19Ab, WASP-156b, and WASP-121b in the TESS Era
Authors: Fan Yang, Ranga-Ram Chary, Ji-Feng Liu
Figure caption: Fits to the TESS TPF transit light curves of KELT-19Ab (top), WASP-156b (middle), and WASP-121b (bottom). The blue points are observed, 2 minute data decontaminated using Gaia photometry. The green points are bins of 30 minute cadence data. The red dashed line represents the best-fit transit model to the 2 minute data. The yellow region shows the 1σ confidence region of the fits. The midpoint of the transit event is shifted to half the period, at the center of the x-axis. The free parameters in the fits are inclination, semimajor axis, and limb-darkening parameters as shown in Figure 4.
Paper: Revisiting KELT-19Ab, WASP-156b, and WASP-121b in the TESS Era
Authors: Fan Yang, Ranga-Ram Chary, Ji-Feng Liu
Figure caption: 14 × 14 pixel TESS images of KELT-19Ab, WASP-156b, WASP-121b, from top to bottom, respectively. The blue markers indicate the position of the exoplanet host star in the Gaia catalog. The red markers indicate the position of nearby sources in the Gaia catalog which contaminate the photometry of the host star, i.e., within 6 pixel separation. Each pixel in the image is 21″. The direction is north up, east to the left.
Paper: Revisiting KELT-19Ab, WASP-156b, and WASP-121b in the TESS Era
Authors: Fan Yang, Ranga-Ram Chary, Ji-Feng Liu
Figure caption: The normalized brightness profile of stars as seen by TESS used to estimate the amount of contamination of an exoplanet host stars’ photometry by background stars seen by Gaia. The scatter points are the observed data. The red line indicates the polynomial fit to the data.
Paper: Infrared Absolute Calibration. I. Comparison of Sirius with Fainter Calibration Stars
Authors: G. H. Rieke, Kate Su, G. C. Sloan, E. Schlawin
Figure caption: Overall approach to calibration of Sirius at K  S  and to transfer this calibration to fainter stars relative to Sirius. The first column shows fiducial magnitudes at K. The second column shows the starting points for the photometry, while the third and fourth columns identify the steps we have used to put the outputs of these starting points onto a common photometric system. Where we started from the photometry of the star to be calibrated, this is also registered in these columns. The fifth column shows the calibrated sources. Where additional calibration steps were taken among these sources, they are indicated within this column.
Paper: Infrared Absolute Calibration. I. Comparison of Sirius with Fainter Calibration Stars
Authors: G. H. Rieke, Kate Su, G. C. Sloan, E. Schlawin
Figure caption: Color–color plot showing K  S  − IRAC1 vs. V − K  S  for stars from Spitzer PID 70076 with K  S  measurements transformed from heritage K photometry (red squares; 89 stars) compared with stars with only 2MASS K  S  measurements (blue dots; 820 stars) over the range of V − K  S  represented by the former sample, −0.5 < V − K  S  < 2.5. The blue line is a fourth-order polynomial fitted to the blue dots.
Paper: A Machine Learning–based Direction-of-origin Filter for the Identification of Radio Frequency Interference in the Search for Technosignatures
Authors: Pavlo Pinchuk, Jean-Luc Margot
Figure caption: Example of a Siamese network tested in this work. The labels “A” and “B” represent input from two different scans. The “Network” in the middle was replaced with one of the architectures that was tested in this work (see Section 4.2). The output layers were joined in two different ways. (Top right) In standard Siamese networks, the output layers are subtracted. (Bottom right) In our generalized version, the output layers are concatenated and connected to another layer with N neurons. Equation (B1) gives the set of weights for this configuration that reproduce the standard layer subtraction procedure.
Paper: Infrared Absolute Calibration. I. Comparison of Sirius with Fainter Calibration Stars
Authors: G. H. Rieke, Kate Su, G. C. Sloan, E. Schlawin
Figure caption: Comparison of proposed color difference K  S  − W1 as a function of V − K  S  for main-sequence stars. The dashed line is from Mamajek (2018), the solid one from Jian et al. (2017) and Deng et al. (2020), and the dashed–dotted one from Davenport et al. (2014).
Paper: A Machine Learning–based Direction-of-origin Filter for the Identification of Radio Frequency Interference in the Search for Technosignatures
Authors: Pavlo Pinchuk, Jean-Luc Margot
Figure caption: Example time–frequency diagrams of signals with a P bottom/P top ratio of 0.2 or lower. The horizontal blue line delimits the top and bottom halves. No signals with a prominence value greater than 3σ are present in the bottom halves. All of these signals represent valid negative samples.
Paper: A Machine Learning–based Direction-of-origin Filter for the Identification of Radio Frequency Interference in the Search for Technosignatures
Authors: Pavlo Pinchuk, Jean-Luc Margot
Figure caption: Example dynamic spectra of signals with a top-half S/N < 6 (exact values shown above each panel). The horizontal blue line delimits the top and bottom halves. Note that these signals (located in the center of the image starting at 0 Hz offset at time t = 0) are faint in the top half of the image and difficult to detect visually.
Paper: A Machine Learning–based Direction-of-origin Filter for the Identification of Radio Frequency Interference in the Search for Technosignatures
Authors: Pavlo Pinchuk, Jean-Luc Margot
Figure caption: Example dynamic spectra of signals with a top-half S/N ≥ 6 (exact values shown above each panel). The horizontal blue line delimits the top and bottom halves. Note that all of these signals (starting at 0 Hz offset at time t = 0) are visually detectable in the top half of each sample.
Paper: Spectroscopy of Candidate Members of the Sco-Cen Complex 
Authors: K. L. Luhman, T. L. Esplin
Figure caption: IR spectra from Whelan et al. (2018) and Riaz & Bally (2021) for three candidate protostellar brown dwarfs in Ophiuchus, each of which is compared to (1) a young early-M star that has been artificially veiled to match the strengths of the Ca and CO features (Covey et al. 2010) and (2) a young late-M object (Allers & Liu 2013).
Paper: Spectroscopy of Candidate Members of the Sco-Cen Complex 
Authors: K. L. Luhman, T. L. Esplin
Figure caption: Equivalent widths of Li and Na vs. spectral type for candidate members of Sco-Cen for which we have obtained optical spectra (Table 2). The left diagram contains detections of Li and useful upper limits. In the right diagram, we show Na measurements from all optical spectra, including those that lack constraints on Li. For comparison, we include the upper envelopes for Li data in IC 2602 (30 Myr) and the Pleiades (125 Myr; upper and lower solid lines; Neuhäuser et al. 1997) in the left diagram and Na measurements for a sample of field dwarfs in the right diagram.
Paper: Polarization-based Speckle Nulling Using a Spatial Light Modulator to Generate a Wide-field Dark Hole
Authors: Naoshi Murakami, Kenta Yoneta, Kenya Kawai, Hajime Kawahara, Takayuki Kotani, Motohide Tamura, Naoshi Baba
Figure caption: Numerical simulation to evaluate the chromaticity of speckle-nulling wave-front control using an SLM. Left: two simulated images after speckle nulling at assumed wavelengths of 500 and 700 nm. Right: acquired contrast before and after speckle nulling. It is assumed that the phase error is caused only by optical surface irregularity in the entrance pupil plane and corrected by an SLM of arbitrarily assumed refractive indices. The dotted vertical line indicates the optimized wavelength λ opt = 633 nm.
Paper: Spectroscopy of Candidate Members of the Sco-Cen Complex 
Authors: K. L. Luhman, T. L. Esplin
Figure caption: Our reduction of an IR spectrum from Lodieu et al. (2021) for a candidate late-type member of Upper Sco, UGCS J161110.14−214516.8, which has been binned to a resolution of R = 150. For comparison, we have included the young standard spectra from Luhman et al. (2017) for M9, L0, and L2. Reddening has been applied to the M9 and L0 spectra to match the slope of the Upper Sco candidate.
Paper: Spectroscopy of Candidate Members of the Sco-Cen Complex 
Authors: K. L. Luhman, T. L. Esplin
Figure caption: Examples of near-IR spectra of candidate members of Sco-Cen, which are displayed at a resolution of R = 150. The data used to create this figure are available.(The data used to create this figure are available.)
Paper: Spectroscopy of Candidate Members of the Sco-Cen Complex 
Authors: K. L. Luhman, T. L. Esplin
Figure caption: Examples of optical spectra of candidate members of Sco-Cen, which are displayed at a resolution of 13 Å. The data used to create this figure are available.(The data used to create this figure are available.)
Paper: Orbital Dynamics and the Evolution of Planetary Habitability in the AU Mic System
Authors: Stephen R. Kane, Bradford J. Foley, Michelle L. Hill, Cayman T. Unterborn, Thomas Barclay, Bryson Cale, Emily A. Gilbert, Peter Plavchan, Justin M. Wittrock
Figure caption: Planet age when the atmosphere is completely lost as a function of an imposed, constant atmospheric loss rate for varying mantle reference viscosity, μ ref (A), initial heat production rate, Q 0 (B), mantle carbon budget, C tot (C), and initial mantle temperature, T init (D). All models assume ﹩{F}_{\mathrm{sfw}}^{* }=5\times {10}^{11}﹩ mol yr−1, E sfw = 75 kJ mol−1, and β = 0.5. Unless otherwise specified, models also assume μ ref = 1021 Pa s, Q 0 = 100 TW, C tot = 1022 mol, and T init = 2000 K. Model results are color coded based on the legends in each panel. Circles connected by solid lines are used for models started with a CO2-rich initial atmosphere, and diamonds connected by dashed lines denote models with an initially CO2-poor atmosphere. In many models sets there is little difference between the two initial conditions, so symbols lie on top of each other. Dotted lines show the age when interior degassing stops, color coded based on the legend for each panel. Models are run for 10 Gyr, so models where an atmosphere is retained after 10 Gyr are considered to have not lost their atmospheres.
Paper: Orbital Dynamics and the Evolution of Planetary Habitability in the AU Mic System
Authors: Stephen R. Kane, Bradford J. Foley, Michelle L. Hill, Cayman T. Unterborn, Thomas Barclay, Bryson Cale, Emily A. Gilbert, Peter Plavchan, Justin M. Wittrock
Figure caption: Planet age, measured after system formation, when an initially hot, CO2-rich climate state and an initially cold, CO2-poor climate state converge due to the negative feedback of the carbonate−silicate cycle. Convergence age is shown as a function of mantle reference viscosity (A), initial radiogenic heat production rate in the mantle (B), initial mantle potential temperature (C), total carbon budget of the mantle and surface reservoirs (D), reference seafloor weathering rate (E), activation energy for seafloor weathering (F), and dependence parameter of seafloor weathering on extrusive volcanism rate (G). Each symbol plotted represents one pair of model runs. Symbols are colored either by mantle reference viscosity or initial heat production rate, as denoted by the color bars.
Paper: Orbital Dynamics and the Evolution of Planetary Habitability in the AU Mic System
Authors: Stephen R. Kane, Bradford J. Foley, Michelle L. Hill, Cayman T. Unterborn, Thomas Barclay, Bryson Cale, Emily A. Gilbert, Peter Plavchan, Justin M. Wittrock
Figure caption: Same as in Figure 3, except climate convergence is measured as the time elapsed after volcanism and degassing has begun.
Paper: Orbital Dynamics and the Evolution of Planetary Habitability in the AU Mic System
Authors: Stephen R. Kane, Bradford J. Foley, Michelle L. Hill, Cayman T. Unterborn, Thomas Barclay, Bryson Cale, Emily A. Gilbert, Peter Plavchan, Justin M. Wittrock
Figure caption: Plot of the dynamical simulation results for an Earth-mass planet injected in the semimajor axis range 0.15–0.70 au. As in Figure 1, the light green and dark green areas represent the CHZ and OHZ regions at the present epoch, respectively. The vertical dashed lines represent the boundaries of the OHZ at a stellar age of 200 Myr. The solid line shows the survival of the Earth-mass planet in terms of the percentage of the simulations in which it remains in the system.
Paper: Orbital Dynamics and the Evolution of Planetary Habitability in the AU Mic System
Authors: Stephen R. Kane, Bradford J. Foley, Michelle L. Hill, Cayman T. Unterborn, Thomas Barclay, Bryson Cale, Emily A. Gilbert, Peter Plavchan, Justin M. Wittrock
Figure caption: Climate convergence age as a function of an imposed, constant atmospheric loss rate for varying mantle reference viscosity, μ ref (A), initial heat production rate, Q 0 (B), mantle carbon budget, C tot (C), and initial mantle temperature, T init (D). Other model parameters are the same as listed in the caption to Figure 6. Climate convergence age drops to zero when atmospheric loss is rapid enough to prevent any appreciable atmosphere from forming.
Paper: Orbital Dynamics and the Evolution of Planetary Habitability in the AU Mic System
Authors: Stephen R. Kane, Bradford J. Foley, Michelle L. Hill, Cayman T. Unterborn, Thomas Barclay, Bryson Cale, Emily A. Gilbert, Peter Plavchan, Justin M. Wittrock
Figure caption: Histograms of model parameters for all models that produce climate convergence ages of less the 20 Myr, approximately the age of the AU Mic system. Shown are distributions of mantle reference viscosity (A), initial heat production rate (B), initial mantle temperature (C), total carbon budget (D), reference seafloor weathering rate (E), activation energy for seafloor weathering (F), and dependence parameter of seafloor weathering on extrusive volcanism rate (G).
Paper: Orbital Dynamics and the Evolution of Planetary Habitability in the AU Mic System
Authors: Stephen R. Kane, Bradford J. Foley, Michelle L. Hill, Cayman T. Unterborn, Thomas Barclay, Bryson Cale, Emily A. Gilbert, Peter Plavchan, Justin M. Wittrock
Figure caption: Eccentricity as a function of time for the known planets (solid and dotted lines) and a hypothetical terrestrial planet d with a semimajor axis of 0.23 au (dashed line).
Paper: Orbital Dynamics and the Evolution of Planetary Habitability in the AU Mic System
Authors: Stephen R. Kane, Bradford J. Foley, Michelle L. Hill, Cayman T. Unterborn, Thomas Barclay, Bryson Cale, Emily A. Gilbert, Peter Plavchan, Justin M. Wittrock
Figure caption: Orbital eccentricity as a function of time for the known planets, where planet b and planet c are shown as solid and dotted lines, respectively. The planets are long-term stable but exchange significant angular momentum through oscillating eccentricities with a period of ∼520 yr.
Paper: A Mid-infrared Study of Directly Imaged Planetary-mass Companions Using Archival Spitzer/IRAC Images
Authors: Raquel A. Martinez, Adam L. Kraus
Figure caption: Color–magnitude diagram for our sample detected in both channel 1 (3.6 μm) and channel 4 (8.0 μm). For comparison, we include young >M7 brown dwarf members of the Taurus (triangles; Esplin & Luhman 2017) and Upper Scorpius (squares; Luhman & Esplin 2020) star-forming regions. Orange symbols represent disk-free members, while red symbols denote disk-bearing members. We also include field brown dwarfs from Dupuy & Liu (2012), indicated by asterisks. The M [3.6] was determined from Gaia EDR3 parallactic measurements (Bailer-Jones et al. 2021) of each system primary. The primary components are indicated as filled stars, while substellar companions are indicated as filled circles. Also displayed are the intrinsic photospheric [3.6]–[8.0] colors from BT-Settl models of Allard et al. (2012) at 1, 10, 100, and 500 Myr (dashed lines). Not shown are the companions to GJ 504 and 1RXS J1609, which were not detected in either channel 1 or channel 4. Object ROXs 42B b was not detected in channel 1 by our pipeline but is shown here as an ﹩{L}^{{\prime} }﹩-band detection from Kraus et al. (2014a). The companions of our sample appear to be significantly redder than the BT-Settl isochrones, in line with previous comparisons between young and old free-floating brown dwarfs (Dupuy & Liu 2012; Liu et al. 2016). The mid-infrared colors of the companions are similar to the disk-bearing free-floating brown dwarfs in young star-forming regions.
Paper: A Mid-infrared Study of Directly Imaged Planetary-mass Companions Using Archival Spitzer/IRAC Images
Authors: Raquel A. Martinez, Adam L. Kraus
Figure caption:  M [3.6] through M [8.0] vs. spectral type for the ≤L2 wide-orbit PMC samples of this work and Paper I (purple upside-down triangles), in addition to the young Taurus and Upper Sco brown dwarfs (depicted as in Figure 4). Similar to ROXs 42B b, 1RXS J1609 b was not detected in channel 1 but is shown in the upper left panel as an ﹩{L}^{{\prime} }﹩-band detection from Kraus et al. (2014a). We also indicate the expected field polynomial sequence of Dupuy & Liu (2012; solid line, dark gray) and the young ultracool dwarf polynomial sequence from Faherty et al. (2016; dashed line, light gray). The young objects sit above the field sequence, but the dynamic range is not high enough in magnitude space to distinguish between disk-bearing and disk-free members.
Paper: A Mid-infrared Study of Directly Imaged Planetary-mass Companions Using Archival Spitzer/IRAC Images
Authors: Raquel A. Martinez, Adam L. Kraus
Figure caption: The SEDs of our sample. We fit system components with solar-metallicity BT-Settl model atmospheres (Allard et al. 2012) and fit E(B − V) individually as a free parameter. The SED-fitting results (T eff/E(B − V)) for each component of our wide companion systems are plotted near the reddened best-fit model. Literature photometry for the systems is plotted as blue squares, while Spitzer/IRAC photometry from this work is indicated by red stars. Synthetic photometry of the best-fit model is also plotted as blue circles for the literature filters used or red circles at the IRAC channels. Specific filters and photometry used in our SED fits for the entire sample are listed in Table 5. The SED-fitting results for the entire sample, including the ﹩{\chi }_{\nu }^{2}﹩ of each fit and ﹩{[8.0]}_{\mathrm{mod}}-{[8.0]}_{\mathrm{obs}}﹩ mag excess, are listed in Table 8.
Paper: A Mid-infrared Study of Directly Imaged Planetary-mass Companions Using Archival Spitzer/IRAC Images
Authors: Raquel A. Martinez, Adam L. Kraus
Figure caption: Stacked images of HD 203030 across all four IRAC channels (rows) after its first-epoch images have gone through the PSF-fitting pipeline. The images were generated in the same fashion as AB Pic in Figure 2. The first and second columns show the original IRAC data of HD 203030 and the median two-source PSF model, respectively, displayed with a logarithmic color scale (leftmost color bar). The third column shows the residuals left behind after only the primary PSF model is subtracted from the data. The fourth column shows the residuals left behind after the two-source PSF model is subtracted from the data. The standard deviation of the pixel values outside an ∼6″ radius from the primary centroid is displayed in the lower left corner of the fourth column in units of DN s–1. Both the third and fourth columns are displayed in a linear color scale (rightmost color bar) with the area within ∼6″ of the primary centroid masked and 3σ and 5σ contours overlaid with solid and dotted lines, respectively. After subtracting the primary star PSF, a statistically significant positive residual is seen at the expected position of HD 203030 b. This residual disappears after subtracting the best-fit system PSFs, and no significant structure is left behind at the location of the companion.
Paper: A Mid-infrared Study of Directly Imaged Planetary-mass Companions Using Archival Spitzer/IRAC Images
Authors: Raquel A. Martinez, Adam L. Kraus
Figure caption: Stacked images of DH Tau, CHXR 73, 1RXS J1609, and ROXs 42B, the other four systems besides AB Pic (shown in Figure 2) with companions that are newly resolved in this work. The first and second columns show the original IRAC data and the median two-source PSF model, respectively, displayed with a logarithmic color scale (leftmost color bar). The third column shows the residuals left behind after only the primary PSF model is subtracted from the data. The third column is displayed with a linear color scale (rightmost color bar) with 3σ and 5σ contours overlaid with solid and dotted lines, respectively. For each panel, north is up, and east is left.