adsabs/AstroCLIMB huggingface dataset:
Paper: Detection of Atmospheric Escape from Four Young Mini-Neptunes
Authors: Michael Zhang, Heather A. Knutson, Fei Dai, Lile Wang, George R. Ricker, Richard P. Schwarz, Christopher Mann, Karen Collins
Figure caption: Background-subtracted X-ray count rate as measured by XMM-Newton’s EPIC cameras. Left: TOI 1430; right: TOI 1683.
Paper: Detection of Atmospheric Escape from Four Young Mini-Neptunes
Authors: Michael Zhang, Heather A. Knutson, Fei Dai, Lile Wang, George R. Ricker, Richard P. Schwarz, Christopher Mann, Karen Collins
Figure caption: Phase-folded TESS light curves for TOI 1430.01 (left) and TOI 1683.01 (right).
Paper: The On-orbit Performance of the Colorado Ultraviolet Transit Experiment Mission
Authors: Arika Egan, Nicholas Nell, Ambily Suresh, Kevin France, Brian Fleming, Aickara Gopinathan Sreejith, Julian Lambert, Nicholas DeCicco
Figure caption: Two 2200 × 515 CUTE frames of different telescope elevation angles, 3° and 12°, to demonstrate the scattered light feature present at low telescope elevation angles. The elevation of each exposure is marked in the left-side overscan region. The top and middle frames compare the 3° and 12° elevation angles with the same colorbar. The bottom frame shows the 12° frame with a colorbar scaled to the frame. Typical frame features are evident on the 12° frame: an increase in counts from the bottom to the top of the frame and hot pixel streaks due to the 32 s CCD readout time. The horizontal dark bars in the top image are missing data packets that were unsuccessfully downlinked.
Paper: The On-orbit Performance of the Colorado Ultraviolet Transit Experiment Mission
Authors: Arika Egan, Nicholas Nell, Ambily Suresh, Kevin France, Brian Fleming, Aickara Gopinathan Sreejith, Julian Lambert, Nicholas DeCicco
Figure caption: CUTE CCD dark frame background rates plotted against detector temperature and colored by the elevation of the Sun with respect to the telescope boresight. In general, higher CCD temperatures produce higher background count rates. Background rates are additionally influenced by the position of astronomical bodies like the Sun as exemplified here, as well as the moon and Earth. At the time of writing, we are still exploring sources of contribution to background rates.
Paper: The Colorado Ultraviolet Transit Experiment Mission Overview
Authors: Kevin France, Brian Fleming, Arika Egan, Jean-Michel Desert, Luca Fossati, Tommi T. Koskinen, Nicholas Nell, Pascal Petit, Aline A. Vidotto, Matthew Beasley, Nicholas DeCicco, Aickara Gopinathan Sreejith, Ambily Suresh, Jared Baumert, P. Wilson Cauley, Carolina Villarreal D'Angelo, Keri Hoadley, Robert Kane, Richard Kohnert, Julian Lambert, Stefan Ulrich
Figure caption: CUTE spectral observations of WASP-189 and KELT-20, A-type host stars of CUTE's first Early Release Science targets. The top plots shows a “TRIM2D” 2048 × 100 pixel two-dimensional data product (exposure time = 5 minutes). The bottom plots show the one-dimensional spectral collapse including wavelength and flux calibration. A 10 pixel boxcar smooth has been applied to the one-dimensional spectra for display purposes.
Paper: The Colorado Ultraviolet Transit Experiment Mission Overview
Authors: Kevin France, Brian Fleming, Arika Egan, Jean-Michel Desert, Luca Fossati, Tommi T. Koskinen, Nicholas Nell, Pascal Petit, Aline A. Vidotto, Matthew Beasley, Nicholas DeCicco, Aickara Gopinathan Sreejith, Ambily Suresh, Jared Baumert, P. Wilson Cauley, Carolina Villarreal D'Angelo, Keri Hoadley, Robert Kane, Richard Kohnert, Julian Lambert, Stefan Ulrich
Figure caption: The CUTE instrument development from concept (instrument schematic, top) to telescope characterization (CUTE flight telescope in the test facilities at the University of Colorado, middle), to predelivery in-band spectral resolution test data (bottom).
Paper: The Colorado Ultraviolet Transit Experiment Mission Overview
Authors: Kevin France, Brian Fleming, Arika Egan, Jean-Michel Desert, Luca Fossati, Tommi T. Koskinen, Nicholas Nell, Pascal Petit, Aline A. Vidotto, Matthew Beasley, Nicholas DeCicco, Aickara Gopinathan Sreejith, Ambily Suresh, Jared Baumert, P. Wilson Cauley, Carolina Villarreal D'Angelo, Keri Hoadley, Robert Kane, Richard Kohnert, Julian Lambert, Stefan Ulrich
Figure caption: CUTE calibration observations of the O4 supergiant ζ Puppis. The top plot shows the full-frame (2048 × 515 pixel) calibration image and the bottom plot shows the extracted one-dimensional spectrum (flux calibrated against archival HST and IUE spectra). ζ Puppis was selected as a calibration target because of the wealth of archival NUV spectra and the high photospheric temperature ensures that iron and magnesium lines in the spectrum are narrow, interstellar features.
Paper: The On-orbit Performance of the Colorado Ultraviolet Transit Experiment Mission
Authors: Arika Egan, Nicholas Nell, Ambily Suresh, Kevin France, Brian Fleming, Aickara Gopinathan Sreejith, Julian Lambert, Nicholas DeCicco
Figure caption: Jitter histogram for 254 × 300 s science exposures from the WASP-189b campaign. The pointing sample rate is 5 s for each 300 s observation. Histogram bin widths are 0.″5 for jitter < 10″ and 1″ for jitter > 10″. A vertical dashed line indicates the cutoff used to eliminate low signal-to-noise observations from light curve analysis.
Paper: The On-orbit Performance of the Colorado Ultraviolet Transit Experiment Mission
Authors: Arika Egan, Nicholas Nell, Ambily Suresh, Kevin France, Brian Fleming, Aickara Gopinathan Sreejith, Julian Lambert, Nicholas DeCicco
Figure caption: A typical CCD temperature profile over several CUTE orbits.
Paper: The Colorado Ultraviolet Transit Experiment Mission Overview
Authors: Kevin France, Brian Fleming, Arika Egan, Jean-Michel Desert, Luca Fossati, Tommi T. Koskinen, Nicholas Nell, Pascal Petit, Aline A. Vidotto, Matthew Beasley, Nicholas DeCicco, Aickara Gopinathan Sreejith, Ambily Suresh, Jared Baumert, P. Wilson Cauley, Carolina Villarreal D'Angelo, Keri Hoadley, Robert Kane, Richard Kohnert, Julian Lambert, Stefan Ulrich
Figure caption: Schematic description of CUTE science and calibration observations.
Paper: Three Ultra-short-period Contact Eclipsing Binary Systems Mined from Massive Astronomical Surveys
Authors: Athanasios Papageorgiou, Panagiota-Eleftheria Christopoulou, C. E. Ferreira Lopes, Eleni Lalounta, Márcio Catelan, Andrew J. Drake
Figure caption: Phase-folded LCs for OGLE104 (panel (a)) and OGLE012 (panel (b)) in different bandpasses with error bars as shown by green squares (V), red dots (I), and purple triangles (K  s ). Panels (c) and (d): phase-folded gri and BVRI LCs for CRTSJ172718, respectively, as shown by blue stars (B), green squares (g, V), purple crosses (r, R), and red dots (i, I). In panel (d), the LCs are shifted vertically for clarity by the following amounts: B − 0.7, V − 0.2, R + 0.2, I + 0.5. The synthetic models (black or white dashed lines) from MCMC analysis are overplotted to the observed data. The bottom plots of panels (a)–(d) show the residuals between synthetic and photometric data. Panel (e): time series CSS data of CRTSJ172718 (2005–2016).
Paper: Three Ultra-short-period Contact Eclipsing Binary Systems Mined from Massive Astronomical Surveys
Authors: Athanasios Papageorgiou, Panagiota-Eleftheria Christopoulou, C. E. Ferreira Lopes, Eleni Lalounta, Márcio Catelan, Andrew J. Drake
Figure caption: Probability distributions (Foreman-Mackey et al. 2014) of q, i, Ω, and T  r  determined by the MCMC modeling (a) of CRTSJ172718 from gri ZTF data, (b) and our BVRI data, (c) OGLE104, and (d) and OGLE012.
Paper: Three Ultra-short-period Contact Eclipsing Binary Systems Mined from Massive Astronomical Surveys
Authors: Athanasios Papageorgiou, Panagiota-Eleftheria Christopoulou, C. E. Ferreira Lopes, Eleni Lalounta, Márcio Catelan, Andrew J. Drake
Figure caption: The mass ratios (top) and orbital angular momenta J orb (bottom) of CRTSJ172718, OGLE104, and OGLE012 (filled stars) and USPCBs from Table 5 (open circles) are plotted as a function of the period (in days) and compared with the various evolutionary models (1a–d and 2a–b; colored lines) described in the text. Contact phases correspond to the solid lines and precontact phases to the dashed lines.
Paper: Three Ultra-short-period Contact Eclipsing Binary Systems Mined from Massive Astronomical Surveys
Authors: Athanasios Papageorgiou, Panagiota-Eleftheria Christopoulou, C. E. Ferreira Lopes, Eleni Lalounta, Márcio Catelan, Andrew J. Drake
Figure caption: Primary and secondary components (filled circles and squares, respectively) of CRTSJ172718, OGLE104, and OGLE012 compared with primary and secondary components (open circles and squares, respectively) of USPCBs from Table 5, plotted on the ﹩\mathrm{log}M\mbox{--}\mathrm{log}R﹩ diagram. The ZAMS (solid) and TAMS (dotted) lines for solar metallicity, as obtained using the BSE code (Hurley et al. 2002), are overplotted.
Paper: V907 Sco Switched to the Eclipsing Mode Again
Authors: Petr Zasche, David Vokrouhlický, Brad N. Barlow, Martin Mašek
Figure caption: Inclination i 1 (label 1) and i 2 (label 2) of the inner- (binary) and the outer-component orbits of V907 Sco over the past century and extending toward the next decade (the abscissa in calendar years). The red symbols are data with their uncertainties determined in Section 2 (Table 2). The right panel provides a zoom on the modern, most accurate data (depicted using the rectangle on the right panels) and shows only the i 1 values. The best-fitting model from Figure 7 (blue star) having m 2 = 1.062 M ⊙, P  ν  = 63.5 yr and J = 26.°2. The gray horizontal line at inclination 73.°3 delimit the zone of i 1 values for which the inner binary is eclipsing, the one at 90° shows just the configuration maximizing eclipses depth. The black dashed horizontal line at inclination 71° shows the inclination of the total angular momentum of the system, about which the inner and outer orbital planes precess. The gray line is the approximate best-fit solution from the secular model from Section 3.1 only. The full solution (solid line and Section 3.2) contains also the long-periodic signal with periodicity P 2, required to match the data from 2022.
Paper: V907 Sco Switched to the Eclipsing Mode Again
Authors: Petr Zasche, David Vokrouhlický, Brad N. Barlow, Martin Mašek
Figure caption: Left: distribution of solutions for which ﹩{\chi }^{2}\leqslant {\chi }_{\star }^{2}\simeq 13.13﹩ projected onto the plane of mass m 2 (abscissa) and precession period P  ν  (ordinate). The solution density is indicated in gray scale, white corresponds to possible solution, black denotes the largest number of solutions. The dashed lines delimit the zone of acceptable solutions. The blue star at m 2 = 1.062 M ⊙ and P  ν  = 63.5 yr shows the location of the best-fitting solution with ﹩{\chi }_{\min }^{2}=3.89﹩. Right: the minimum χ 2 (abscissa) for a given P  ν  value (ordinate). The dashed vertical line is the limit for accepted solutions ﹩{\chi }^{2}={\chi }_{\star }^{2}﹩; the solid vertical line is the best achieved value ﹩{\chi }_{\ \min }^{2}\simeq 3.89﹩.
Paper: V907 Sco Switched to the Eclipsing Mode Again
Authors: Petr Zasche, David Vokrouhlický, Brad N. Barlow, Martin Mašek
Figure caption: TESS photometry of V907 Sco from Sectors 39 (lower plot) and 13 (upper plot), each spanning about 27 days and folded on the 3.7762049 day period of the eclipsing binary. The ordinate is the differential magnitude, which has been shifted by 0.01 mag for the Sector 13 data for better visualization. The red lines are the respective best fits obtained using the PHOEBE code (Table 1). In the Sector 13 data, only a very subtle dip is noticed at the zero phase of the primary eclipse, implying the stellar configuration seen by the observer was nearly grazing.
Paper: V907 Sco Switched to the Eclipsing Mode Again
Authors: Petr Zasche, David Vokrouhlický, Brad N. Barlow, Martin Mašek
Figure caption: Upper part: disentangled radial velocities at the period P 2 for the center of mass of the inner binary. The individual data points are shown with black symbols. The red line is the Keplerian best fit with the parameters listed in Table 3; the gray horizontal line is at ﹩K\,{e}_{2}\cos {\omega }_{2}\simeq -6﹩ km s−1, a center to which semi-amplitude K is referred to. The abscissa is the Julian date with 2450000 subtracted. Bottom part: residuals of the radial velocities after the motion of the inner and outer orbits has been subtracted from the data.
Paper: V907 Sco Switched to the Eclipsing Mode Again
Authors: Petr Zasche, David Vokrouhlický, Brad N. Barlow, Martin Mašek
Figure caption: Disentangled radial velocities at the period P 1 for the components in the eclipsing binary using CHIRON spectra from 2022. The black symbols are the individual data, and the red/blue lines are the Keplerian best fits for the primary/secondary components with the parameters listed in Table 1. The abscissa is the phase of the binary cycle (with a zero value at the epoch of the primary eclipse). The gray horizontal line is the systemic velocity of v  γ  ≃ −17.3 km s−1.
Paper: V907 Sco Switched to the Eclipsing Mode Again
Authors: Petr Zasche, David Vokrouhlický, Brad N. Barlow, Martin Mašek
Figure caption: Sample light curves from different epochs: symbols are data, solid line is the best-fit model (the corresponding inclination values i 1 are listed in Table 2). The abscissa is the phase of P 1 cycle, and the ordinate is the differential magnitude, with a shift for sake of visibility. Top data are from modern instrumentation (FRAM observations in August 2022), bottom three examples are from various archival sources.
Paper: V907 Sco Switched to the Eclipsing Mode Again
Authors: Petr Zasche, David Vokrouhlický, Brad N. Barlow, Martin Mašek
Figure caption: Example of two spectra taken at different phases ϕ of the inner binary motion (vertically shifted for visibility) obtained by CHIRON spectrograph. Labels 1a and 1b identify the stellar components in the binary. A narrow window in the red part of the spectrum around the SiII lines (634.7 and 637.1 nm) is shown.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: Gaia CMDs with (left panel) rotational velocity and (right panel) Li abundance information. Gaia-selected likely binary members are shown with small black points, and photometrically selected single-star members in red. Approximate G magnitudes of the DS And components are shown with green lines, and BD +37 410 is shown with a blue line.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: Example broadening functions for the binaries. Primary star fits are in red, secondary star fits in blue, and tertiary star fits in cyan. Top panel: DS And broadening function from an HET HRS spectrum for HJD 2,455,811.801, with fits of rotational broadening functions with ﹩{v}_{\mathrm{rot}}\sin i=106.6,59.7﹩ km s−1. Bottom panel: BD +37 410 broadening function from a WIYN Hydra spectrum for HJD 2,452,140.878, with Gaussian fits with σ = 14.1, 12.4, and 7.3 km s−1.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: Top panel: synthetic spectrum for T eff = 6750 K from Coelho et al. (2005). Bottom panel: disentangled average spectrum of DS And A from NOT FIES observations in the region of the 6707.8 Å Li I line, with other strong lines identified. The rotationally broadened synthetic spectrum (using ﹩{v}_{\mathrm{rot}}\sin i=105﹩ km s−1) is shown in red for comparison.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: Top: SED for DS And B (red points) and a fitted ATLAS9 model for T eff = 6100 K (solid line, and green points for integrations over filter response curves). Horizontal error bars represent the effective width of the filter. Bottom: fractional difference between the stellar fluxes and the best-fit fluxes for the ATLAS9 (green) model.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: Mass–luminosity plot for measured members of BD +37 410 and DS And, with 2σ uncertainties indicated by the red error ellipses. Models use Z = 0.0152, 0.0149, 0.0142, and 0.0162, respectively, for PARSEC (Bressan et al. 2012), BaSTI-IAC (Hidalgo et al. 2018), MIST (Choi et al. 2016; Dotter 2016), and YaPSI (Spada et al. 2017) isochrones.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: Phased photometry for DS And compared with the best-fit binary models. B, V, R  C , and TESS light curves are zero-pointed to the magnitude at eclipse ingress/egress phases. W1 and W2 photometry is in calibrated magnitudes. The U curve is in instrumental magnitudes.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: Top panel: radial velocities of the stars in BD +37 410, phased to the orbital period, along with best-fit models. Empty symbols show measurements not used in the orbit fitting. Bottom panels: (O − C) residuals for the radial velocities.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: Phased TESS photometry for BD +37 410 compared with the best-fit binary models at the eclipse and noneclipsing conjunction. The first TESS eclipse is shown with magenta points and the second with blue.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: Top panel: radial velocities of the stars of DS And, phased to the orbital period, along with best-fit models. Bottom panels: (O − C) residuals for the radial velocities.
Paper: Unifying High- and Low-resolution Observations to Constrain the Dayside Atmosphere of KELT-20b/MASCARA-2b
Authors: David Kasper, Jacob L. Bean, Michael R. Line, Andreas Seifahrt, Madison T. Brady, Joshua Lothringer, Lorenzo Pino, Guangwei Fu, Stefan Pelletier, Julian Stürmer, Björn Benneke, Matteo Brogi, Jean-Michel Désert
Figure caption: Summary of the joint retrieval analysis. The left panel shows the model fits to the space-based data resulting from the retrieval on the MAROON-X, HST/WFC3, and Spitzer/IRAC data. The red curves represent the spectra produced via 100 random draws from the posterior (smoothed to an R = 100). The blue points are those same spectra binned to the WFC3 wavelengths. The smearing in the blue points illustrates the spread in the binned model spectra. The inset in the bottom right of the left panel shows a zoom in on the WFC3 data. The “Retrieved T–P” inset in the upper left shows reconstructed T–P profiles from 100 posterior draws from the combined MAROON-X, WFC3, and Spitzer (blue) observations. A 3× Solar 1D-RC model T–P profile from ScCHIMERA is shown in black for comparison. The right panel summarizes the retrieved abundance constraints in the context of a 3 × solar 1D-RC model. The solid horizontal bars give the retrieved 68% confidence intervals on the chemical species. The position of the bars on the y-axis (pressure axis) are at the approximate location probed by the wavelengths sensitive to those species (see Figure 9 in the Appendix). The predicted thermochemical mixing ratio profiles are shown as dashed lines and the temperature profile is shown as the thick red curve (governed by the top x-axis). The thinner red temperature profile is the same 3× solar scenario but with the opacity due to TiO/VO removed.
Paper: Unifying High- and Low-resolution Observations to Constrain the Dayside Atmosphere of KELT-20b/MASCARA-2b
Authors: David Kasper, Jacob L. Bean, Michael R. Line, Andreas Seifahrt, Madison T. Brady, Joshua Lothringer, Lorenzo Pino, Guangwei Fu, Stefan Pelletier, Julian Stürmer, Björn Benneke, Matteo Brogi, Jean-Michel Désert
Figure caption: Comparison of retrieved elemental abundance proxies to those predicted from a battery of 1D-RC models. In each panel the histogram (scale on the left y-axis) is derived via a Monte Carlo propagation of the retrieved samples for Fe,I, H2O, and CO into the quantity given under each x-axis (left: log(Fe I+H2O+CO); middle: log(CO/(H2O+CO)); right: log(Fe I/(H2O+CO))). The light shaded region is the 95% confidence interval for each proxy. The solid curves are the vertical abundance proxy profiles (pressure scale on the right y-axis of each panel) derived from the indicated 1D-RC models. In each panel, all elemental abundances are scaled uniformly by the indicated value relative to solar. The retrieved abundance proxy constraints are consistent with solar composition, under the 1D-RC assumption.