adsabs/AstroCLIMB huggingface dataset:
Paper: Inferring Exoplanet Disequilibria with Multivariate Information in Atmospheric Reaction Networks
Authors: Theresa Fisher, Hyunju Kim, Camerian Millsaps, Michael Line, Sara I. Walker
Figure caption: The abundance of H2O as a function of temperature and K zz, at 0.1, 1, 10, and 100 times solar metallicity. The x-axis is temperature, y-axis is K zz, and color corresponds to the abundance of H2O (see color bar for each individual plot for scale).
Paper: Inferring Exoplanet Disequilibria with Multivariate Information in Atmospheric Reaction Networks
Authors: Theresa Fisher, Hyunju Kim, Camerian Millsaps, Michael Line, Sara I. Walker
Figure caption: The abundance of NH3 as a function of temperature and K zz, at 0.1, 1, 10, and 100 times solar metallicity. The x-axis is temperature, y-axis is K zz, and color corresponds to the abundance of NH3 (see color bar for each individual plot for scale).
Paper: Inferring Exoplanet Disequilibria with Multivariate Information in Atmospheric Reaction Networks
Authors: Theresa Fisher, Hyunju Kim, Camerian Millsaps, Michael Line, Sara I. Walker
Figure caption: Mean degree as a function of temperature and K zz, at 0.1, 1, 10, and 100 times solar metallicity. The x-axis is temperature, y-axis is K zz, and color corresponds to the weighted mean degree (see color bar for each individual plot for scale).
Paper: Inferring Exoplanet Disequilibria with Multivariate Information in Atmospheric Reaction Networks
Authors: Theresa Fisher, Hyunju Kim, Camerian Millsaps, Michael Line, Sara I. Walker
Figure caption: Boosting up the predicting accuracy for the disequilibrium state of the atmospheric chemical reaction networks with multivariate information. Each panel of the plot shows the predicting accuracy of variables for atmospheric networks associated with K zz = 0, 106, 108, and 1010 at a given mean temperature between 500 and 1900 K with uncertainty ±500 K. The three variables with the highest predictive power at each mean temperature compared to other individual variables (in gray) are colored red (for detailed information about topological variables used in this plot, see Table 1 and Section 2.2). T*, A*, and N* represent multidimensional variable sets composed of the three top predictors, the abundance of the four chemical species shown in this plot, and the six network topological measures represented in Figure 9, respectively. The three different multivariable sets demonstrated higher predicting accuracy than individual variables even in the cases where the highest predictors are not included.
Paper: The Galactic Distribution of Phosphorus: A Survey of 163 Disk and Halo Stars 
Authors: Zachary G. Maas, Keith Hawkins, Natalie R. Hinkel, Phillip Cargile, Steven Janowiecki, Tyler Nelson
Figure caption: From left to right, panels show a comparison of this work to that of Bensby et al. (2014) as blue circles, to APOGEE DR16 (Jönsson et al. 2020) as black diamonds, to Casagrande et al. (2011) as magenta stars, and to the PASTEL catalog as brown triangles (Soubiran et al. 2016). The top panels show the differences in derived effective temperature, and the bottom panels show differences in log(g). Error bars are only shown for stars with errors above 1σ from the average uncertainty on the parameter difference for the Bensby et al. (2014) and APOGEE DR16 comparisons. We also include representative error bars as gray “x” symbols in the APOGEE DR16 and Bensby et al. (2014). Light green boxes highlight stars with highly uncertain (>0.2 mag) 2MASS photometry for two or more filters.
Paper: The Galactic Distribution of Phosphorus: A Survey of 163 Disk and Halo Stars 
Authors: Zachary G. Maas, Keith Hawkins, Natalie R. Hinkel, Phillip Cargile, Steven Janowiecki, Tyler Nelson
Figure caption: Three observations of relatively metal-poor stars with similar T eff and log(g) from HPF on the HET are plotted with three synthetic spectra. The observed spectrum of HIP 80837 is represented as black circles, that of HIP 100792 is shown as red crosses, and that of HIP 36849 is shown as blue circles. Model spectra for these stars are displayed as a black dotted–dashed line, a red solid line, and a blue dashed line, respectively.
Paper: The Galactic Distribution of Phosphorus: A Survey of 163 Disk and Halo Stars 
Authors: Zachary G. Maas, Keith Hawkins, Natalie R. Hinkel, Phillip Cargile, Steven Janowiecki, Tyler Nelson
Figure caption: A(P) abundances from this study compared to those from APOGEE DR 16 (black stars), from Maas et al. (2017; red diamonds), from Maas et al. (2019; orange circle), and from Caffau et al. (2011; blue squares).
Paper: The Galactic Distribution of Phosphorus: A Survey of 163 Disk and Halo Stars 
Authors: Zachary G. Maas, Keith Hawkins, Natalie R. Hinkel, Phillip Cargile, Steven Janowiecki, Tyler Nelson
Figure caption: Comparison of [P/Fe] to T eff from this work. Black stars are targets selected from Bensby et al. (2014), and red stars are those chosen from APOGEE DR16. The gray “x” in the upper right corner is a representative error bar for T eff.
Paper: The Galactic Distribution of Phosphorus: A Survey of 163 Disk and Halo Stars 
Authors: Zachary G. Maas, Keith Hawkins, Natalie R. Hinkel, Phillip Cargile, Steven Janowiecki, Tyler Nelson
Figure caption: Comparison of literature [Fe/H] abundance measurements to results from this paper. The symbols here have the same meanings as those in Figure 2.
Paper: pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry
Authors: Rachel B. Fernandes, Gijs D. Mulders, Ilaria Pascucci, Galen J. Bergsten, Tommi T. Koskinen, Kevin K. Hardegree-Ullman, Kyle A. Pearson, Steven Giacalone, Jon Zink, David R. Ciardi, Patrick O'Brien
Figure caption: Overall detection efficiency of pterodactyls while taking into account flux contamination. The confirmed planets are depicted using blue stars, except for TOI 1726b, whose recovery required changing pterodactyls. Darker bins represent regions of higher detection efficiency. n ⋆ is the total number of stars in our sample, while n is the total number of injections done. Black box denotes the bin over which the intrinsic occurrence rates were calculated, i.e., sub-Neptunes and Neptunes (0.017–0.055 ﹩\tfrac{{R}_{{\rm{p}}}}{{R}_{\star }}﹩ or 1.8–6 R ⊕, assuming a solar radius) within 12.5 days (about half a TESS sector).
Paper: pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry
Authors: Rachel B. Fernandes, Gijs D. Mulders, Ilaria Pascucci, Galen J. Bergsten, Tommi T. Koskinen, Kevin K. Hardegree-Ullman, Kyle A. Pearson, Steven Giacalone, Jon Zink, David R. Ciardi, Patrick O'Brien
Figure caption: Left: Progression of the DS Tuc A light curve through pterodactyls. Upper panel: PSF flux (in dark gray) and penalized spline trend (in blue). Lower panel: Detrended light curve (PSF flux divided by the trend). The multi-transit signature (in red) can be clearly seen. Right: Upper panel shows phase-folded light curve of DS Tuc A b (gray data points) along with the best-fit model using EXOTIC (in red). Lower panel shows the residuals in parts per million.
Paper: pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry
Authors: Rachel B. Fernandes, Gijs D. Mulders, Ilaria Pascucci, Galen J. Bergsten, Tommi T. Koskinen, Kevin K. Hardegree-Ullman, Kyle A. Pearson, Steven Giacalone, Jon Zink, David R. Ciardi, Patrick O'Brien
Figure caption: Left: Comparison of planetary radii recovered using pterodactyls (fitted with EXOTIC) vs. known planet radii for the eight recovered known planets. As can be seen, despite being recovered from 30-minute cadence data, the radii are often consistent with those published. In two cases, TOI 1726c and TOI 451 c, we slightly underestimate the planet’s radius. We also overestimate the radius of the planet for HIP 6752b. Right: Comparison of orbital periods recovered using pterodactyls vs. known orbital periods for the eight recovered planets, to depict consistency between the results of our work and those from the discovery papers. Note: Orbital period errors are extremely small and hence cannot be seen in the plot.
Paper: pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry
Authors: Rachel B. Fernandes, Gijs D. Mulders, Ilaria Pascucci, Galen J. Bergsten, Tommi T. Koskinen, Kevin K. Hardegree-Ullman, Kyle A. Pearson, Steven Giacalone, Jon Zink, David R. Ciardi, Patrick O'Brien
Figure caption: A comparison of extreme detection efficiencies, to highlight the effect of flux contamination. Top: Detection efficiency of Pisces–Eridani, a moving group with members that are spread out such that flux contamination is minimal. Middle: Detection efficiency of IC 2602, a crowded cluster, while taking into account flux contamination while injecting planets. Bottom: Detection efficiency of IC 2602 while assuming no flux contamination while injecting planets.
Paper: pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry
Authors: Rachel B. Fernandes, Gijs D. Mulders, Ilaria Pascucci, Galen J. Bergsten, Tommi T. Koskinen, Kevin K. Hardegree-Ullman, Kyle A. Pearson, Steven Giacalone, Jon Zink, David R. Ciardi, Patrick O'Brien
Figure caption: Left: Recovery of TOI 1726b. Upper panel: PSF flux (in dark gray) and penalized spline trend (in blue). Lower panel: Detrended light curve (PSF flux divided by the trend). The multi-transit signature (in red) can be clearly seen. Right: Upper panel shows phase-folded light curve of TOI 1726b (gray data points) along with the best-fit model using EXOTIC (in red). Lower panel shows the residuals in parts per million.
Paper: pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry
Authors: Rachel B. Fernandes, Gijs D. Mulders, Ilaria Pascucci, Galen J. Bergsten, Tommi T. Koskinen, Kevin K. Hardegree-Ullman, Kyle A. Pearson, Steven Giacalone, Jon Zink, David R. Ciardi, Patrick O'Brien
Figure caption: Left: Recovery of TOI 1726c. Upper panel: PSF flux (in dark gray) and penalized spline trend (in blue). Lower panel: Detrended light curve (PSF flux divided by the trend). The multi-transit signature (in red) can be clearly seen. Right: Upper panel shows phase-folded light curve of TOI 1726c (gray data points) along with the best-fit model using EXOTIC (in red). Lower panel shows the residuals in parts per million.
Paper: pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry
Authors: Rachel B. Fernandes, Gijs D. Mulders, Ilaria Pascucci, Galen J. Bergsten, Tommi T. Koskinen, Kevin K. Hardegree-Ullman, Kyle A. Pearson, Steven Giacalone, Jon Zink, David R. Ciardi, Patrick O'Brien
Figure caption: A demonstration of how different splines detrend the light curve of HIP 67522. As can be seen by the low rms, the penalized spline does a superior job of matching the stellar variability trend and detrending the light curve.
Paper: pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry
Authors: Rachel B. Fernandes, Gijs D. Mulders, Ilaria Pascucci, Galen J. Bergsten, Tommi T. Koskinen, Kevin K. Hardegree-Ullman, Kyle A. Pearson, Steven Giacalone, Jon Zink, David R. Ciardi, Patrick O'Brien
Figure caption: Left: Recovery of TIC 460205581b. Upper panel: PSF flux (in dark gray) and penalized spline trend (in blue). Lower panel: Detrended light curve (PSF flux divided by the trend). The multi-transit signature (in red) can be clearly seen. Right: Upper panel shows phase-folded light curve of TIC 460205581 b (gray data points) along with the best-fit model using EXOTIC (in red). Lower panel shows the residuals in parts per million.
Paper: pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry
Authors: Rachel B. Fernandes, Gijs D. Mulders, Ilaria Pascucci, Galen J. Bergsten, Tommi T. Koskinen, Kevin K. Hardegree-Ullman, Kyle A. Pearson, Steven Giacalone, Jon Zink, David R. Ciardi, Patrick O'Brien
Figure caption: Left: Recovery of TOI 837 b. Upper panel: PSF flux (in dark gray) and penalized spline trend (in blue). Lower panel: Detrended light curve (PSF flux divided by the trend). The multi-transit signature (in red) can be clearly seen. Right: Upper panel shows phase-folded light curve of TOI 837 b (gray data points) along with the best-fit model using EXOTIC (in red). Lower panel shows the residuals in parts per million.
Paper: The First Fall is the Hardest: The Importance of Peculiar Galaxy Dynamics at Infall Time for Tidal Stripping Acting at the Centers of Groups and Clusters
Authors: Rory Smith, Paula Calderón-Castillo, Jihye Shin, Mojtaba Raouf, Jongwan Ko
Figure caption: Evolution of R peri with time for a point mass orbiting in a cluster-like fixed analytical potential for a typical orbit of a satellite in a cluster (left) and for a more extreme plunging orbit (right). The red line shows the R peri evolution for 1 Myr timesteps, while the red symbols show the R peri evolution with 100 Myr timesteps, similar to the cosmological simulation. Blue symbols show the minimum R peri values seen with the 100 Myr timesteps. The horizontal lines show the true R peri value. With 100 Myr timesteps, typically the recovered R peri measurement matches the true measurement to within 1%.
Paper: The First Fall is the Hardest: The Importance of Peculiar Galaxy Dynamics at Infall Time for Tidal Stripping Acting at the Centers of Groups and Clusters
Authors: Rory Smith, Paula Calderón-Castillo, Jihye Shin, Mojtaba Raouf, Jongwan Ko
Figure caption: Age of the universe in gigayears at the time of infall (t inf) vs. mass ratio grids, colored by the median R peri of all halos in a pixel (R peri,All). In the central panel, the total sample is shown (labeled “All”). In the left panels, we split the sample by host mass (labeled “Hi M host” and “Lo M host”). In the right panels, we split the sample by infaller mass (labeled “Lo ﹩{M}_{\inf }﹩” and “Hi ﹩{M}_{\inf }﹩”).
Paper: Probing Magnetic Fields in Protoplanetary Disk Atmospheres through Polarized Near-IR Light Scattered by Aligned Grains
Authors: Haifeng Yang, 海峰 杨, Zhi-Yun Li
Figure caption: The geometry of a simple setting in the grain frame. The photon propagating in the ﹩\hat{z}﹩ direction is scattered by the dust grain sitting at the origin O toward the ﹩{\hat{n}}_{s}﹩ direction in the xOz plane. The scattering angle is θ. The scattered light is decomposed into E 1 and E 2 directions. Note that it is often assumed that the scattered light is polarized along E 1 direction.
Paper: Probing Magnetic Fields in Protoplanetary Disk Atmospheres through Polarized Near-IR Light Scattered by Aligned Grains
Authors: Haifeng Yang, 海峰 杨, Zhi-Yun Li
Figure caption: The polarization pattern in our fiducial disk model (Model 1). The parameters adopted are listed in the left panel. See Figure 2 for their definitions. Left: the black unilength line segments represent the polarization orientation. The dotted lines connect the central star with each test scattering grain. The red line segments are perpendicular to the dotted lines and represent the often assumed azimuthal polarization patterns. Upper right: the difference in polarization orientation as a function of the azimuthal angle of the test scattering grain in the disk frame. The polarization is essentially “reversed” and is along the radial direction at an azimuthal angle of 330°. Lower right: the polarization fraction as a function of the azimuthal angle. The solid line represents the fiducial case, whereas the dashed line represents the small spherical grain case.
Paper: Probing Magnetic Fields in Protoplanetary Disk Atmospheres through Polarized Near-IR Light Scattered by Aligned Grains
Authors: Haifeng Yang, 海峰 杨, Zhi-Yun Li
Figure caption: The geometry of an oblate grain aligned by a pure toroidal magnetic field. By definition, the magnetic field  B  is perpendicular to the incoming light direction ﹩{\hat{n}}_{1}﹩. The incoming light excites two dipoles in the grain, denoted as  P  1 and  P  2. The scattered light direction ﹩{\hat{n}}_{2}﹩ makes an angle of ι with  P  2. Note that we have ∣ P  2∣ > ∣ P  1∣ under this configuration.
Paper: Probing Magnetic Fields in Protoplanetary Disk Atmospheres through Polarized Near-IR Light Scattered by Aligned Grains
Authors: Haifeng Yang, 海峰 杨, Zhi-Yun Li
Figure caption: The critical curve for polarization reversal. The s in the x-axis is the aspect ratio of dust grains. The ι is the angle between the scattered light propagating direction ﹩{\hat{n}}_{2}﹩ and the second dipole direction  P  2 (see, Figure 3). In the gray parameter space, the polarization is potentially reversed, i.e., the light is polarized along that radial, rather than the canonical azimuthal direction.
Paper: Probing Magnetic Fields in Protoplanetary Disk Atmospheres through Polarized Near-IR Light Scattered by Aligned Grains
Authors: Haifeng Yang, 海峰 杨, Zhi-Yun Li
Figure caption: The maximum angle difference for different configurations of magnetic fields, assuming an inclination angle of 60°, H/R of 0.2, and a dust aspect ratio of s = 1.5. The color map represents the maximum angle difference Δη. Also plotted are contours of constant angle difference Δη = 70° for different inclination angles. The inclination angle i is labeled next to each line.
Paper: Probing Magnetic Fields in Protoplanetary Disk Atmospheres through Polarized Near-IR Light Scattered by Aligned Grains
Authors: Haifeng Yang, 海峰 杨, Zhi-Yun Li
Figure caption: The geometry of our setup in the disk frame. The black dot represents the central star. The red dot represents the scattering dust grain. Hence ﹩{\hat{n}}_{1}﹩ connecting these two dots is the incoming light direction. The scattered light propagates along ﹩{\hat{n}}_{2}﹩, making an angle of i with the z-axis. The local magnetic field direction is prescribed by the angles θ  B  and ϕ  B . See text for more details.
Paper: Probing Magnetic Fields in Protoplanetary Disk Atmospheres through Polarized Near-IR Light Scattered by Aligned Grains
Authors: Haifeng Yang, 海峰 杨, Zhi-Yun Li
Figure caption: The τ = 1 surface. Top: the solid line represents the height of τ = 1 surface as a function of radius, whereas the dashed line shows the H/R of this surface. Bottom: the solid line shows the height of τ = 1 surface in terms of local gas scale height. The dashed line represents the critical grain size as a function of radius defined by setting the Stokes number equal to the viscous parameter α.
Paper: Probing Magnetic Fields in Protoplanetary Disk Atmospheres through Polarized Near-IR Light Scattered by Aligned Grains
Authors: Haifeng Yang, 海峰 杨, Zhi-Yun Li
Figure caption: The same as Figure 5, but for Model 2. This represents a less inclined disk model with a moderate magnetic field configuration. There is no polarization reversal. The maximum angle difference is only 11° but still detectable at the 3σ level if S/N > 7.8 for the Stokes parameters.
Paper: Probing Magnetic Fields in Protoplanetary Disk Atmospheres through Polarized Near-IR Light Scattered by Aligned Grains
Authors: Haifeng Yang, 海峰 杨, Zhi-Yun Li
Figure caption: The same as Figure 6 but for i = 45°, H/R = 0.2, s = 1.5, and without the constant angle difference Δη = 70° contours. Note the difference in the color map.
Paper: Probing Magnetic Fields in Protoplanetary Disk Atmospheres through Polarized Near-IR Light Scattered by Aligned Grains
Authors: Haifeng Yang, 海峰 杨, Zhi-Yun Li
Figure caption: Maximum angle difference as a function of inclination angle i, for H/R = 0.2 and three different dust aspect ratios s = 1.1, 1.5, and 2.0.
Paper: The GAPS Programme at TNG XXXIX. Multiple Molecular Species in the Atmosphere of the Warm Giant Planet WASP-80 b Unveiled at High Resolution with GIANO-B 
Authors: Ilaria Carleo, Paolo Giacobbe, Gloria Guilluy, Patricio E. Cubillos, Aldo S. Bonomo, Alessandro Sozzetti, Matteo Brogi, Siddharth Gandhi, Luca Fossati, Diego Turrini, Katia Biazzo, Francesco Borsa, Antonino F. Lanza, Luca Malavolta, Antonio Maggio, Luigi Mancini, Giusi Micela, Lorenzo Pino, Ennio Poretti, Monica Rainer, Gaetano Scandariato, Eugenio Schisano, Gloria Andreuzzi, Andrea Bignamini, Rosario Cosentino, Aldo Fiorenzano, Avet Harutyunyan, Emilio Molinari, Marco Pedani, Seth Redfield, Hristo Stoev
Figure caption: Likelihood confidence intervals maps for each investigated molecule as a function of K P and v rest and at the best-fit scaling factor. The dashed lines represent the nominal planetary velocities. As for the CC significance maps, the CO2 likelihood map is displayed in the case of coadding only three nights (not including the third night). As regards C2H2, the likelihood intervals map does not significantly change by coadding three or four nights.
Paper: The GAPS Programme at TNG XXXIX. Multiple Molecular Species in the Atmosphere of the Warm Giant Planet WASP-80 b Unveiled at High Resolution with GIANO-B 
Authors: Ilaria Carleo, Paolo Giacobbe, Gloria Guilluy, Patricio E. Cubillos, Aldo S. Bonomo, Alessandro Sozzetti, Matteo Brogi, Siddharth Gandhi, Luca Fossati, Diego Turrini, Katia Biazzo, Francesco Borsa, Antonino F. Lanza, Luca Malavolta, Antonio Maggio, Luigi Mancini, Giusi Micela, Lorenzo Pino, Ennio Poretti, Monica Rainer, Gaetano Scandariato, Eugenio Schisano, Gloria Andreuzzi, Andrea Bignamini, Rosario Cosentino, Aldo Fiorenzano, Avet Harutyunyan, Emilio Molinari, Marco Pedani, Seth Redfield, Hristo Stoev
Figure caption: Sample atmospheric models for WASP-80 b in radiative and thermochemical equilibrium for a solar elemental composition. The top-left panel shows the equilibrium temperature profile shifted by ±200 K, to simulate a low-temperature case (thick solid red line) and a high-temperature case (thin dashed blue line). The shaded area denotes the pressure range probed by the GIANO-B transmission observations for these models. The top-right panel shows the equilibrium composition for the two temperature profiles at low (thick solid lines) and high temperature (thin dashed lines), color coded for each relevant species (see legend, with the asterisks indicating the firmly detected species). The bottom panel shows the transmission spectra over the GIANO-B wavelength range, for the low-temperature case (red) and high-temperature model (blue). The horizontal black lines denote the wavelength ranges where each of the labeled species are expected to significantly shape the transmission spectrum of WASP-80 b.
Paper: The GAPS Programme at TNG XXXIX. Multiple Molecular Species in the Atmosphere of the Warm Giant Planet WASP-80 b Unveiled at High Resolution with GIANO-B 
Authors: Ilaria Carleo, Paolo Giacobbe, Gloria Guilluy, Patricio E. Cubillos, Aldo S. Bonomo, Alessandro Sozzetti, Matteo Brogi, Siddharth Gandhi, Luca Fossati, Diego Turrini, Katia Biazzo, Francesco Borsa, Antonino F. Lanza, Luca Malavolta, Antonio Maggio, Luigi Mancini, Giusi Micela, Lorenzo Pino, Ennio Poretti, Monica Rainer, Gaetano Scandariato, Eugenio Schisano, Gloria Andreuzzi, Andrea Bignamini, Rosario Cosentino, Aldo Fiorenzano, Avet Harutyunyan, Emilio Molinari, Marco Pedani, Seth Redfield, Hristo Stoev
Figure caption: Significance maps of the cross correlation between the GIANO-B spectra and the isothermal atmospheric models, as a function of the planet's maximum radial velocity (K P) and the planet's rest-frame velocity (v rest). For a better visualization, the maps do not show any signal <2.5σ. The dashed white lines indicate the known velocity for WASP-80 b (K P = 122 km s−1, v rest = 0 km s−1). The CO2 map is also shown in the case of coadding only the three nights (not including the third night). See discussion in the text (Section 3) and Table 2.