adsabs/AstroCLIMB huggingface dataset:
Paper: Searching for GEMS: Characterizing Six Giant Planets Around Cool Dwarfs
Authors: Shubham Kanodia, Arvind F. Gupta, Caleb I. Cañas, Lia Marta Bernabò, Varghese Reji, Te Han, Madison Brady, Andreas Seifahrt, William D. Cochran, Nidia Morrell, Ritvik Basant, Jacob Bean, Chad F. Bender, Zoë L. de Beurs, Allyson Bieryla, Alexina Birkholz, Nina Brown, Franklin Chapman, David R. Ciardi, Catherine A. Clark, Ethan G. Cotter, Scott A. Diddams, Samuel Halverson, Suzanne Hawley, Leslie Hebb, Rae Holcomb, Steve B. Howell, Henry A. Kobulnicky, Adam F. Kowalski, Alexander Larsen, Jessica Libby-Roberts, Andrea S. J. Lin, Michael B. Lund, Rafael Luque, Andrew Monson, Joe P. Ninan, Brock A. Parker, Nishka Patel, Michael Rodruck, Gabrielle Ross, Arpita Roy, Christian Schwab, Guđmundur Stefánsson, Aubrie Thoms, Andrew Vanderburg
Figure caption: (Top left) RV time series for TOI-5634A. (Top right) Phase-folded RVs. (Bottom) The phase-folded light curves. The plot styling and definitions are similar to Figure 1.
Paper: Searching for GEMS: Characterizing Six Giant Planets Around Cool Dwarfs
Authors: Shubham Kanodia, Arvind F. Gupta, Caleb I. Cañas, Lia Marta Bernabò, Varghese Reji, Te Han, Madison Brady, Andreas Seifahrt, William D. Cochran, Nidia Morrell, Ritvik Basant, Jacob Bean, Chad F. Bender, Zoë L. de Beurs, Allyson Bieryla, Alexina Birkholz, Nina Brown, Franklin Chapman, David R. Ciardi, Catherine A. Clark, Ethan G. Cotter, Scott A. Diddams, Samuel Halverson, Suzanne Hawley, Leslie Hebb, Rae Holcomb, Steve B. Howell, Henry A. Kobulnicky, Adam F. Kowalski, Alexander Larsen, Jessica Libby-Roberts, Andrea S. J. Lin, Michael B. Lund, Rafael Luque, Andrew Monson, Joe P. Ninan, Brock A. Parker, Nishka Patel, Michael Rodruck, Gabrielle Ross, Arpita Roy, Christian Schwab, Guđmundur Stefánsson, Aubrie Thoms, Andrew Vanderburg
Figure caption: (Top left) RV time series for TOI-5414. (Top right) Phase-folded RVs. (Bottom) The phase-folded light curves. The plot styling and definitions are similar to Figure 1.
Paper: Generating X-Ray Transit Profiles with Batman
Authors: George W. King, Lía R. Corrales, Peter J. Wheatley, Raven C. Cilley, Mark Hollands
Figure caption: Comparison of transits of HD 189733 b resulting from varying different key parameters. In the top panel, we compare transits with four different absorber sizes for the same underlying coronal model. In the middle panel, we compare transits for four different coronal temperatures, assuming the effective X-ray radius of the planet is equal to the optical radius. In the bottom panel, we compare transits with four different impact parameters, assuming the same absorber size and coronal model in case. Calculated transit characteristics associated with the models in all three panels are given in Table 2.
Paper: Generating X-Ray Transit Profiles with Batman
Authors: George W. King, Lía R. Corrales, Peter J. Wheatley, Raven C. Cilley, Mark Hollands
Figure caption: Change in the total flux blocked (χ, a proxy for transit detectability) while varying three different parameters. The top panels show the change in χ with increasing absorbing region radius at fixed values of the impact parameter and coronal temperature. The middle panels show the change in χ with increasing impact parameter at fixed values of the absorber radius and coronal temperature. The bottom panels show the change in χ with increasing coronal temperature at fixed values of the absorber radius and impact parameter. Each panel’s label shows the quantity that is fixed across all results in that panel. Each legend shows the values of the other fixed quantity on that row, where each line style and color combination on that row refers to a different fixed value of that parameter.
Paper: Generating X-Ray Transit Profiles with Batman
Authors: George W. King, Lía R. Corrales, Peter J. Wheatley, Raven C. Cilley, Mark Hollands
Figure caption: Comparison of optical and X-ray transit models for HD 189733. The annotations mark key moments where the X-ray transit shape changes characteristics (blue) due to the relative position of the planetary disk and stellar photosphere, analogous to key moments in the optical transit (red). In the case of HD 189733 b, the impact parameter is high enough that optical transit light curve never goes flat, making it so the Φ2 and Φ3 points are not readily apparent. At both wavelengths, the transit midpoint (Φ C ) are the same. Calculated transit characteristics associated with these models are given in Table 2.
Paper: Generating X-Ray Transit Profiles with Batman
Authors: George W. King, Lía R. Corrales, Peter J. Wheatley, Raven C. Cilley, Mark Hollands
Figure caption: Examples of methods for mitigating the limitations of our model. In the top panel, we consider a possible mitigation of the isothermal nature of our coronal model by combining the model arrays of two separate models. Here, we use the same 0.34 keV and 1.0 keV models we used in Section 3.3. We combine their model fluxes with a factor 0.5 in the 1.0 keV to reflect a case where the count rate of photons from the plasma at that temperature is half that from the lower temperature plasma. In the bottom panel, we give examples of including a third light parameter in the model, in order to partly mitigate the symmetric nature of our model. The positive and negative third light reflect transit chords across latitudes that are dimmer and brighter, respectively, as compared to the rest of the corona.
Paper: Generating X-Ray Transit Profiles with Batman
Authors: George W. King, Lía R. Corrales, Peter J. Wheatley, Raven C. Cilley, Mark Hollands
Figure caption: The considered geometry of the coronal profile in the 0 < x < 1 coordinate system used by BATMAN. N scale is the number of emission scale heights the model is calculated out to, which is user defined. We use N scale = 6 throughout the examples shown in this work. The stellar radius in this coordinate system, ﹩R{{\prime} }_{* }﹩, is defined as 1-(N scale * ﹩H{{\prime} }_{{\rm{e}}}﹩).
Paper: Generating X-Ray Transit Profiles with Batman
Authors: George W. King, Lía R. Corrales, Peter J. Wheatley, Raven C. Cilley, Mark Hollands
Figure caption: The effect of changing the coronal scale height/temperature on the emission profile. In the top panel we show the relative 1D intensities as a function of distance from the center of the stellar disk associated with the H e = 0.127 and 0.375 R * (kT = 0.34 and 1.0 keV) models. In the bottom panel we show the 2D representations of the stellar X-ray emission profiles associated with the same models. The relative emissions are plotted on the same scale, which is I(x) renormalized to the maximum coronal emission intensity of the H e = 0.127 R * model. Transit profiles associated with these models are plotted in the middle panel of Figure 4.
Paper: Generating X-Ray Transit Profiles with Batman
Authors: George W. King, Lía R. Corrales, Peter J. Wheatley, Raven C. Cilley, Mark Hollands
Figure caption: The effect of changing the time resolution with the same underlying model. The “high-res sampling” model is the original 500 bin model, also plotted in e.g., Figure 3. The “correct low-res model” takes the original 500 bin model and averages across groups of ∼20 points to obtain a representative value of the model for the phase range each resulting point covers. The 25 phases between 0.9 and 1.1 that these points are plotted at were then ran through BATMAN to obtain an instantaneous value of the model at those phases for comparison—these are plotted as the “low-res sampling.” This demonstrates why the X-ray transit model we present should always be calculated at high resolution first, and then binned to the cadence of the data it is being compared to.
Paper: Generating X-Ray Transit Profiles with Batman
Authors: George W. King, Lía R. Corrales, Peter J. Wheatley, Raven C. Cilley, Mark Hollands
Figure caption: 1D (left panel) and 2D (right panel) schematic of the normalized emission intensities for HD 189733 for kT = 0.34 keV, H e = 0.127  R  *. In the 1D plot, the distance from the stellar disk center in is plotted in batman’s 0–1 coordinate system, with the edge of the stellar disk displayed with the gray dashed line.
Paper: A Near-infrared Survey of Candidate Haumea Family Members
Authors: Benjamin C. N. Proudfoot, Estela Fernández-Valenzuela, John A. Stansberry, Csaba Kiss, Darin Ragozzine, Wesley C. Fraser, Rosemary E. Pike, Noemi Pinilla-Alonso
Figure caption: F139M−F153M color as a function of absolute magnitude in the F606W filter (H 606, left panel) and F606W−F139M (right panel). In blue, we show the colors found by the observations presented in this work. In green, colors of HCs from the H/WTSOSS survey (W. C. Fraser & M. E. Brown 2012). The pink shaded region shows the extent of HC color. Six of our observed TNOs have colors consistent with the confirmed family members found in previous work, while one has colors consistent with other HCs.
Paper: A Near-infrared Survey of Candidate Haumea Family Members
Authors: Benjamin C. N. Proudfoot, Estela Fernández-Valenzuela, John A. Stansberry, Csaba Kiss, Darin Ragozzine, Wesley C. Fraser, Rosemary E. Pike, Noemi Pinilla-Alonso
Figure caption: F139M−F153M color as a function of family probability, using the color scheme of Figure 1. Points that have substantial increases in family probability when accounting for resonant diffusion are shown by two points connected by a gray line. To prevent overlapping lines, a small vertical offset has been added to two data points with the same F139M−F153M color. As most of the W. C. Fraser & M. E. Brown (2012) sample is not located near the Haumea family, p fam = 0 (for readability, we omit these points). All of the TNOs with colors consistent with family membership have high family probabilities but only after accounting for possible resonant diffusion, which we call maximum p fam.
Paper: A Radio Technosignature Search of TRAPPIST-1 with the Allen Telescope Array
Authors: Nick Tusay, Sofia Z. Sheikh, Evan L. Sneed, Wael Farah, Alexander W. Pollak, Luigi F. Cruz, Andrew Siemion, David R. DeBoer, Jason T. Wright
Figure caption: Distributions of the relevant signal parameters from all eight observations combined. The SNR is truncated at 1000 for readability, but the data extend out several orders of magnitude, up to a maximum of ∼1.15 × 107 for a few (∼1% of the data) powerful nearby signals. Most signals were detected at lower frequencies, where the major bands are known to be more crowded with RFI. The drift-rate distribution extends beyond the target maximum of 15 nHz due to bin doubling during the “frequency-scrunching” process, but is still strongly clustered around 0 nHz due to an abundance of terrestrial RFI.
Paper: A Radio Technosignature Search of TRAPPIST-1 with the Allen Telescope Array
Authors: Nick Tusay, Sofia Z. Sheikh, Evan L. Sneed, Wael Farah, Alexander W. Pollak, Luigi F. Cruz, Andrew Siemion, David R. DeBoer, Jason T. Wright
Figure caption: Results of Mars test observations showing the recovery of 37 Mars orbiter downlinks during the time of observation. Three signals were classified as RFI below the nominal cutoff, and one false positive showed an attenuated signal at a known transmitting frequency for STEREO-A, which was not in either beam at the time. Signals that are powerful enough to show up in both beams, overwhelming the DOT scoring algorithm and trending toward 1.0, are still attenuated in the off-beam and identified as potentially interesting for follow-up. Candidate signals localized to a distant source may show up only weakly in the target beam at the limits of the telescope’s sensitivity and are expected to appear in the top left of this kind of plot.
Paper: A Radio Technosignature Search of TRAPPIST-1 with the Allen Telescope Array
Authors: Nick Tusay, Sofia Z. Sheikh, Evan L. Sneed, Wael Farah, Alexander W. Pollak, Luigi F. Cruz, Andrew Siemion, David R. DeBoer, Jason T. Wright
Figure caption: The third injection recovery test using setigen to score a weak signal on top of stronger RFI. The added signal seen only in the target panel was injected on top of previously identified RFI, originally calculated by turboSETI as 78.88. The signal was given a width of 2 Hz, a drift rate of 0.07 Hz s−1, and an SNR equal to that of the RFI. turboSETI calculates SNR independently from the SNR input into setigen, but the reported SNR is relatively close to the original RFI. The RFI centered on 0 in these frames shows why this was removed by spatial filtering. The very high correlation score of 0.983 is unlikely to indicate an interesting signal for follow-up.
Paper: A Radio Technosignature Search of TRAPPIST-1 with the Allen Telescope Array
Authors: Nick Tusay, Sofia Z. Sheikh, Evan L. Sneed, Wael Farah, Alexander W. Pollak, Luigi F. Cruz, Andrew Siemion, David R. DeBoer, Jason T. Wright
Figure caption: Three representative signals in the on- and off-beams resulting from test observations of Martian probes that were subsequently filtered through the NbeamAnalysis pipeline. The detected frequencies of these signals were cross-referenced with known transmission frequencies for various Martian probes to identify their source. The top panel shows a signal from the Emirates Hope orbiter. The middle panel shows a signal from the Mars Odyssey orbiter. The bottom panel shows the “false-positive” signal noted in Figure 6 from STEREO-A, a heliocentric satellite. The color bar indicates the amount of power in each beam, normalized to the peak of the target beam signal and displayed in a logarithmic scale.
Paper: A Radio Technosignature Search of TRAPPIST-1 with the Allen Telescope Array
Authors: Nick Tusay, Sofia Z. Sheikh, Evan L. Sneed, Wael Farah, Alexander W. Pollak, Luigi F. Cruz, Andrew Siemion, David R. DeBoer, Jason T. Wright
Figure caption: The second injection recovery test using setigen to score a strong signal on top of weaker RFI. The added signal seen only in the target panel was injected on top of previously identified RFI, originally calculated by turboSETI as 42.25. The signal was given a width of 2 Hz, a drift rate of 0.07 Hz s−1, and an SNR of 1000 times that of the RFI. turboSETI calculates SNR independently from the SNR input into setigen, but nevertheless indicates a relatively strong signal, as intended. The RFI offset from 0 in these frames shows why this was not removed by spatial filtering. The somewhat low correlation score of 0.276 could indicate an interesting signal for follow-up, depending on the user-defined cutoff value.
Paper: A Radio Technosignature Search of TRAPPIST-1 with the Allen Telescope Array
Authors: Nick Tusay, Sofia Z. Sheikh, Evan L. Sneed, Wael Farah, Alexander W. Pollak, Luigi F. Cruz, Andrew Siemion, David R. DeBoer, Jason T. Wright
Figure caption: A cartoon illustrating that PPO events, in this work, can occur in scenarios broader than strict occultation. Specifically, PPO events occur where the opening angle of the transmitted beam, ϕ/2, is greater than the angle θ between the line of the planets and the ﹩-\hat{z}﹩ direction, toward Earth. The top panel shows the projected xy-plane view. The bottom panel shows a bird’s-eye, xz-plane view of the same scenario, where a transmitter on the surface of planet b is sending a radio signal toward planet c. This sketch is not to scale, but it provides a visual reference for the geometry considered in calculating a PPO event.
Paper: A Radio Technosignature Search of TRAPPIST-1 with the Allen Telescope Array
Authors: Nick Tusay, Sofia Z. Sheikh, Evan L. Sneed, Wael Farah, Alexander W. Pollak, Luigi F. Cruz, Andrew Siemion, David R. DeBoer, Jason T. Wright
Figure caption: An injection recovery test using setigen used to score an isolated signal with the DOT algorithm. The isolated linearly drifting signal seen in the target panel was injected in a region of frequency space known to contain only noise. The signal was given a width of 2 Hz, a drift rate of 0.07 Hz s−1, and an SNR of 42,000. turboSETI calculates SNR independently from the SNR input into setigen, but nevertheless indicates a relatively strong signal, as intended. The low correlation score of 0.019 indicates that the signal detected in the target panel is distinct from the pure noise in the off panel.
Paper: A Radio Technosignature Search of TRAPPIST-1 with the Allen Telescope Array
Authors: Nick Tusay, Sofia Z. Sheikh, Evan L. Sneed, Wael Farah, Alexander W. Pollak, Luigi F. Cruz, Andrew Siemion, David R. DeBoer, Jason T. Wright
Figure caption: Sketch of the geometry of a PPO event where the effects on our observations due to the uncertainties in the semimajor axis and inclination would be maximized. When the opening angle of the transmitted beam, ϕ/2, is greater than the angle θ between the line of the planets and the ﹩-\hat{z}﹩ direction, spillover emission from a PPO event could be detected.
Paper: Analyzing the Onset of Cometary Activity by the Jupiter-family Comet 2023 RN3 
Authors: Matthew M. Dobson, Megan E. Schwamb, Alan Fitzsimmons, Michael S. P. Kelley, Carrie E. Holt, Joseph Murtagh, Henry H. Hsieh, Larry Denneau, Nicolas Erasmus, A. N. Heinze, Luke J. Shingles, Robert J. Siverd, Ken W. Smith, John L. Tonry, Henry Weiland, David. R. Young, Tim Lister, Edward Gomez, Joey Chatelain, Sarah Greenstreet
Figure caption: Lightcurve of 2023 RN3 plotting apparent magnitude (top) and reduced magnitude (bottom) across time. All magnitudes are corrected to the ATLAS o filter wavelength. Filled markers indicate magnitude measurements of SNR ≥3; open markers indicate 3σ upper limits.
Paper: Analyzing the Onset of Cometary Activity by the Jupiter-family Comet 2023 RN3 
Authors: Matthew M. Dobson, Megan E. Schwamb, Alan Fitzsimmons, Michael S. P. Kelley, Carrie E. Holt, Joseph Murtagh, Henry H. Hsieh, Larry Denneau, Nicolas Erasmus, A. N. Heinze, Luke J. Shingles, Robert J. Siverd, Ken W. Smith, John L. Tonry, Henry Weiland, David. R. Young, Tim Lister, Edward Gomez, Joey Chatelain, Sarah Greenstreet
Figure caption: Lightcurve of 2023 RN3 (apparent magnitude across time) in each filter. Filled circles indicate magnitude measurements; open triangles indicate 3σ upper limits.
Paper: Analyzing the Onset of Cometary Activity by the Jupiter-family Comet 2023 RN3 
Authors: Matthew M. Dobson, Megan E. Schwamb, Alan Fitzsimmons, Michael S. P. Kelley, Carrie E. Holt, Joseph Murtagh, Henry H. Hsieh, Larry Denneau, Nicolas Erasmus, A. N. Heinze, Luke J. Shingles, Robert J. Siverd, Ken W. Smith, John L. Tonry, Henry Weiland, David. R. Young, Tim Lister, Edward Gomez, Joey Chatelain, Sarah Greenstreet
Figure caption: ATLAS c − o (upper), ZTF g − r (center), and LOOK g − r (lower) color index values calculated from binning observations by epoch plotted across time.
Paper: Simulating Self-lensing and Eclipsing Signals due to Detached Compact Objects in the TESS Light Curves
Authors: Sedighe Sajadian, Niayesh Afshordi
Figure caption: Maps of ﹩{\mathrm{log}}_{10}[{\rm{\Delta }}{F}_{{\rm{L}}}]﹩ in detached and edge-on binary systems over the 2D space of ﹩{\mathrm{log}}_{10}[{M}_{{\rm{c}}}({M}_{\odot })]-{\mathrm{log}}_{10}[a({R}_{\odot })]﹩. We consider four different source stars in binary systems: (i) a red dwarf with M ⋆ = 0.3M ⊙ and R ⋆ = 0.35R ⊙, (ii) a Sun-like star, (iii) a B-type star with M ⋆ = 2M ⊙ and R ⋆ = 1.8R ⊙, and (iv) a subgiant star with M ⋆ = 2M ⊙ and R ⋆ = 3.6R ☉. The contours display ﹩{\mathrm{log}}_{10}[T(\mathrm{days})]﹩. The interacting binaries with D RL < R ⋆ (see Equation (10)) are excluded and covered with white on maps.
Paper: Simulating Self-lensing and Eclipsing Signals due to Detached Compact Objects in the TESS Light Curves
Authors: Sedighe Sajadian, Niayesh Afshordi
Figure caption: The HC efficiencies for detecting signals due to compact objects in stellar light curves (in the logarithmic scale ﹩{\mathrm{log}}_{10}[{\varepsilon }_{\mathrm{HC}}( \% )]﹩) vs. nine parameters, which are D l (kpc), ﹩{\mathrm{log}}_{10}[\mathrm{Periority}]﹩, ﹩{\mathrm{log}}_{10}[a/{R}_{\star }]﹩, M ⋆(M ⊙), ﹩{\mathrm{log}}_{10}[{\rho }_{\star }]﹩, i {°}, ﹩{\mathrm{log}}_{10}[b/{R}_{\star }]﹩, M NS(M ⊙), and M BH(M ⊙) as shown in different panels. Three efficiency curves with different line styles are due to three values for T obs as mentioned in the first panel.
Paper: Simulating Self-lensing and Eclipsing Signals due to Detached Compact Objects in the TESS Light Curves
Authors: Sedighe Sajadian, Niayesh Afshordi
Figure caption: Simulated self-lensing signals vs. time (normalized to the orbital period) by considering different values for M c(M ⊙), ϵ, i, R ⋆(R ⊙), θ, and Γ. For each panel, several parameters are fixed and reported at the top of that panel. The vertical axis is the flux of the source star normalized to its baseline value.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South. II. WASP-121 b has Superstellar C/O and Refractory-to-volatile Ratios
Authors: Peter C. B. Smith, Jorge A. Sanchez, Michael R. Line, Emily Rauscher, Megan Weiner Mansfield, Eliza M.-R. Kempton, Arjun Savel, Joost P. Wardenier, Lorenzo Pino, Jacob L. Bean, Hayley Beltz, Vatsal Panwar, Matteo Brogi, Isaac Malsky, Jonathan Fortney, Jean-Michel Désert, Stefan Pelletier, Vivien Parmentier, Sai Krishna Teja Kanumalla, Luis Welbanks, Michael Meyer, John Monnier
Figure caption: Our measurements for WASP-121 b’s atmospheric oxygen- and carbon-to-refractory ratios and overall refractory enrichment using the model described in Section 5.2, compared to Y. Chachan et al. (2023)'s predictions for these values, depending on initial formation location. Some of these curves have been horizontally offset by up to 0.1 dex for visual clarity. The black contours are the 1σ, 2σ, and 3σ quantiles for these 2D posterior distributions.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South. II. WASP-121 b has Superstellar C/O and Refractory-to-volatile Ratios
Authors: Peter C. B. Smith, Jorge A. Sanchez, Michael R. Line, Emily Rauscher, Megan Weiner Mansfield, Eliza M.-R. Kempton, Arjun Savel, Joost P. Wardenier, Lorenzo Pino, Jacob L. Bean, Hayley Beltz, Vatsal Panwar, Matteo Brogi, Isaac Malsky, Jonathan Fortney, Jean-Michel Désert, Stefan Pelletier, Vivien Parmentier, Sai Krishna Teja Kanumalla, Luis Welbanks, Michael Meyer, John Monnier
Figure caption: Cross-correlation detection maps calculated by cross-correlating with the data a solar composition model spectrum with only each individual gas included, rather than the residual method as described in Section 3. Compare to Figure 4.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South. II. WASP-121 b has Superstellar C/O and Refractory-to-volatile Ratios
Authors: Peter C. B. Smith, Jorge A. Sanchez, Michael R. Line, Emily Rauscher, Megan Weiner Mansfield, Eliza M.-R. Kempton, Arjun Savel, Joost P. Wardenier, Lorenzo Pino, Jacob L. Bean, Hayley Beltz, Vatsal Panwar, Matteo Brogi, Isaac Malsky, Jonathan Fortney, Jean-Michel Désert, Stefan Pelletier, Vivien Parmentier, Sai Krishna Teja Kanumalla, Luis Welbanks, Michael Meyer, John Monnier
Figure caption: Similar to Figure 13, but showing log-likelihood detection maps calculated using model spectra including the opacity of only each individual gas. Compare to Figure 5.
Paper: Simulating Self-lensing and Eclipsing Signals due to Detached Compact Objects in the TESS Light Curves
Authors: Sedighe Sajadian, Niayesh Afshordi
Figure caption: Six examples of simulated stellar light curves due to detached and edge-on binary WDMS, NSMS, and BHMS systems. The synthetic data points are hypothetically taken by the TESS telescope. We fix the observational time to 27.4 days with a one-day gap in middle. The parameters used to make light curves are mentioned at the tops of panels. By applying HC detectability criteria, for three of these light curves the impacts of compact objects are realizable, as mentioned in their legends.