adsabs/AstroCLIMB huggingface dataset:
Paper: The Si K Edge Gas and Dust Optical Depths Toward the Galactic Bulge
Authors: Jun Yang, Norbert S. Schulz, Daniele Rogantini, Claude R. Canizares, Lia Corrales, Ioanna Psaradaki
Figure caption: Unfolded spectra (black) with the final model fits (red) for all survey sources. The data are unbinned, and one HEG resolution element (0.011 Å) has four data bins.
Paper: WISE/NEOWISE Multiepoch Imaging of the Potentially Geminid-related Asteroids: (3200) Phaethon, 2005 UD, and 1999 YC
Authors: Toshihiro Kasuga, Joseph R. Masiero
Figure caption: WISE observation of Phaethon on UT 2010 January 7 (MJD 55203.2564). The measured flux densities at W1 (3.4 μm), W2 (4.6 μm), W3 (12 μm), and W4 (22 μm) are shown as points. The 2σ upper limit is represented with downward arrows. The reflected sunlight model (blue dashed line), thermal model (red dashed line), and combined signal (black solid line) are overplotted.
Paper: DELIGHT: Deep Learning Identification of Galaxy Hosts of Transients using Multiresolution Images
Authors: Francisco Förster, Alejandra M. Muñoz Arancibia, Ignacio Reyes-Jainaga, Alexander Gagliano, Dylan Britt, Sara Cuellar-Carrillo, Felipe Figueroa-Tapia, Ava Polzin, Yara Yousef, Javier Arredondo, Diego Rodríguez-Mancini, Javier Correa-Orellana, Amelia Bayo, Franz E. Bauer, Márcio Catelan, Guillermo Cabrera-Vives, Raya Dastidar, Pablo A. Estévez, Giuliano Pignata, Lorena Hernández-García, Pablo Huijse, Esteban Reyes, Paula Sánchez-Sáez, Mauricio Ramírez, Daniela Grandón, Jonathan Pineda-García, Francisca Chabour-Barra, Javier Silva-Farfán
Figure caption: Training set preparation process: (A) initial PanSTARRS r-band 480 × 480 pixels (0.″25 pixel−1) image centered around the position of the transient candidate (white star, in this example SN2004eh), where the output of the model should be the two-dimensional vector connecting the transient and the host-galaxy center (white arrow); (B) the images are sky-subtracted, and sources are detected using SExtractor, masking out all pixels that are not within four elliptical dimensionless radii of any source; (C) the image is resampled into five images of 30 × 30 pixels, all centered around the transient position, but with different fields of view, going from larger to smaller scales as shown in frames (D)–(H). Note that the final multiresolution image requires 3.5% of the memory space used by the original image and about 60 ms per source to generate.
Paper: DELIGHT: Deep Learning Identification of Galaxy Hosts of Transients using Multiresolution Images
Authors: Francisco Förster, Alejandra M. Muñoz Arancibia, Ignacio Reyes-Jainaga, Alexander Gagliano, Dylan Britt, Sara Cuellar-Carrillo, Felipe Figueroa-Tapia, Ava Polzin, Yara Yousef, Javier Arredondo, Diego Rodríguez-Mancini, Javier Correa-Orellana, Amelia Bayo, Franz E. Bauer, Márcio Catelan, Guillermo Cabrera-Vives, Raya Dastidar, Pablo A. Estévez, Giuliano Pignata, Lorena Hernández-García, Pablo Huijse, Esteban Reyes, Paula Sánchez-Sáez, Mauricio Ramírez, Daniela Grandón, Jonathan Pineda-García, Francisca Chabour-Barra, Javier Silva-Farfán
Figure caption: Angular semimajor axis of transient host galaxies (A) and transient to host angular separation (B) distributions of the input samples. Note that the isophotal semimajor axis is approximately 3 times the reported semimajor axis (Bertin & Arnouts 1996). The ALeRCE sample is significantly larger than the nearby sample (14,111  vs. 2680  galaxies, respectively), but it is dominated by smaller and more distant galaxies. Combining both samples helps to reduce the imbalance in host-galaxy size (see discussion in Section 2).
Paper: Fast Derivation of Contact Binary Parameters for Large Photometric Surveys
Authors: Xu Ding, KaiFan Ji, XuZhi Li, JianPing Xiong, QiYuan Cheng, JinLiang Wang, Hui Liu
Figure caption: The blue curve is the density of the distribution without the influence of third light. The red curve is the density of the distribution with the influence of third light.
Paper: Fast Derivation of Contact Binary Parameters for Large Photometric Surveys
Authors: Xu Ding, KaiFan Ji, XuZhi Li, JianPing Xiong, QiYuan Cheng, JinLiang Wang, Hui Liu
Figure caption: The figure shows the two structures without and with the influence of third light. The numbers in the figure represent the number of input and output nodes of each layer. The structure with the influence of third light has one more input parameter (l 3) than the structure without the influence of third light.
Paper: Asteroseismology of a Double-mode High-amplitude δ Scuti Star TIC 448892817
Authors: Chenglong Lv, Ali Esamdin, J. Pascual-Granado, A. García Hernández, A. Hasanzadeh
Figure caption: The left panel shows the procedure to find Δν. The black line represents the Fourier transform (FT) of the frequencies, the blue line is the autocorrelation function (AC), and the gray lines plot a histogram of frequency differences (HFD), following the methodology of García Hernández et al. (2009, 2013) and Ramón-Ballesta et al. (2021). The red dotted–dashed line indicates the identified value of Δν = 3.8 day−1 (44 μHz), corresponding to the most prominent peak in the AC and HFD (see details in the text). The right panel shows an échelle diagram of the frequencies depicted with a normalized amplitude of 1 in purple. The value of 3.8 day−1 (44 μHz) is used for the plot. The organization of the frequencies is clearly visible.
Paper: Asteroseismology of a Double-mode High-amplitude δ Scuti Star TIC 448892817
Authors: Chenglong Lv, Ali Esamdin, J. Pascual-Granado, A. García Hernández, A. Hasanzadeh
Figure caption: Evolutionary tracks from the zero-age MS to the post-MS for the 5 candidate models except for the low metallicity models, as listed in Table 3. The plus sign mark the minimum χ 2 for each specific model by fitting the calculated f 1 and f 2 with the observed values. The two vertical dotted lines mark T eff at 7000 K and 8500 K, respectively.
Paper: Asteroseismology of a Double-mode High-amplitude δ Scuti Star TIC 448892817
Authors: Chenglong Lv, Ali Esamdin, J. Pascual-Granado, A. García Hernández, A. Hasanzadeh
Figure caption: Fourier amplitude spectra for the light curve of TIC 448892817. The top panel shows the independent frequencies F0 and F1 of 2 minutes cadence. The bottom panel shows the residual spectrum after the extraction of all significant frequencies. No peak is statistically significant in the residual.
Paper: Asteroseismology of a Double-mode High-amplitude δ Scuti Star TIC 448892817
Authors: Chenglong Lv, Ali Esamdin, J. Pascual-Granado, A. García Hernández, A. Hasanzadeh
Figure caption: A portion of the rectified light curve of TIC 448892817 covering 2.9 days for the 2 minutes cadence. The amplitude of the light curve is about 0.32 mag.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These panels present the PV diagrams in the lines of H I β, [Ne III] λ3869, He I λ4471, and [O III] λ4959, lines that sample the majority of the mass of the nebula (all of it for H I), all from the CD2 wavelength interval. Compared to the lines in Figure 46, there is clearly less emission from the receding side of the main shell for lines of sight close to the central star.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These panels present the PV diagrams of the lines of highest ionization: C IV λλ5801,5811, [Ne IV] λ4724, and [Ar V] λ7006. Note that there is also C IV emission from the central star. In general, the receding side of the main shell and its outer edge (at top) are the brightest features. The approaching side of the main shell is fainter, but a feature half-way to the outer edge is visible in all three PV diagrams. Although it is discontinuous, the velocity ellipse has a semicircular shape in these PV diagrams.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These panels present the PV diagrams for the lines of [O II] λ3726, [N II] λ6583, and [S II] λ6716, and the sum of [Cl II] λλ8578,9123. In all of these lines, the emission from the main shell is much weaker than in the previous figures, while the only bright emission comes from the filament outside the main shell. Even so, the main shell is brighter in the [O II] λ3726 line than in the other lines, which is the result of collisional excitation (Section 3.3).
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: The panels in the left column present the PV diagrams in the lines of lowest ionization potential, [O I] λ6300 and [C I] λ9850. In [O I] λ6300, emission from the main shell is now nearly absent. In the right column, the panels contrast the PV diagrams of the O I λ7771 and O I λ8446 lines. The different morphologies likely arise due to different physical processes contributing to the two lines. The black streak is a cosmic ray.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These panels present the PV diagrams for the lines of C III λ4647, [K IV] λ6101, N III λ4379 (O III λ4379.6 is the second/redder line), [Cl IV] λ8045, and [Ar IV] λ4740. The velocity ellipse in these PV diagrams has returned to a rounder shape than in Figure 45, largely because of the greater velocity splitting.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: Left column: these panels present the PV diagrams in the lines of Si II λ6371 and Si I λ6486. Right column: these panels present the PV diagrams in the lines of [Ar IV] λ4740 (nebular line) and [Ar IV] λ7262 (auroral line). The vertical stripes of low counts (white) to the blue and red of the [Ar IV] λ7262 line profile are due to atmospheric absorption, which affects the measurement of the velocity splitting (Table 8; Figure 5).
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: We present the PV diagrams of the observed Hβ line (top panel), predictions of the Hβ emission from the normal nebular plasma based upon the [O III] λ4959 line assuming (a) the kinematic temperature of 8000 K (second panel) and (b) the [O III] temperature map (third panel), and the residual Hβ emission attributable to the additional plasma component assuming a temperature of 8000 K (fourth panel) and the [O III] temperature map (bottom panel). The contours in the bottom two panels are of the model of the Hβ emission based upon the O II λ4649 line broadened for a temperature of 2000 K (used in Figure 42). All panels share a common color scale. The residual emission amounts to 15.3% (fourth panel) and 41.7% (bottom panel) of the total Hβ emission, i.e., the bottom two panels correspond closely to the contributions supposed in the bottom two panels of Figure 42.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These panels present the PV diagrams for [Ar III] λ7135, [O III] λ5007, [Cl III] λ5517, and [S III] λ6312. Compared to [O III] λ5007, the other three lines have even less emission from the receding side of the main shell along lines of sight near the central star, but more emission from the filament beyond the receding side of the main shell (Figure 4). The difference between [O III] λ5007 and [O III] λ4959 (Figure 47) is due to the longer slit for lines redder than 5000 Å and a slight shift in the position of the slit perpendicular to its length.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These panels present lines of high ionization: He II λ3203, He II λ4686, O III λ3707 (recombination), O III λ5592 (charge exchange), O III λ3444 (Bowen fluorescence), and N III λ4634 (Bowen fluorescence). In terms of shape, these PV diagrams are more square than those in Figure 44 and extend to a larger distance from the central star.
Paper: Reduced Variations in Earth’s and Mars’ Orbital Inclination and Earth’s Obliquity from 58 to 48 Myr ago due to Solar System Chaos
Authors: Richard E. Zeebe
Figure caption: Inertial (fixed) coordinate system (x, y, z; blue) and coordinate system moving with the orbit plane (x *, y *, z *; red), with z * parallel to the orbit normal  n  and x * along the ascending node.  s  represents the spin axis (unit vector), and the obliquity (axial tilt) ϵ is the angle between  s  and  n  (﹩\cos \epsilon ={\boldsymbol{n}}\cdot {\boldsymbol{s}}﹩). Ω is the longitude of the ascending node, I is the orbital inclination (angle between z * and z), and ϕ * measures the precession angle in the orbit plane (see text).
Paper: Reduced Variations in Earth’s and Mars’ Orbital Inclination and Earth’s Obliquity from 58 to 48 Myr ago due to Solar System Chaos
Authors: Richard E. Zeebe
Figure caption: Earth’s and Mars’ orbital eccentricity and inclination in the invariable frame from ZB18a. Note the large change in the variation of Mars’ inclination around 48 Ma in (d).
Paper: Reduced Variations in Earth’s and Mars’ Orbital Inclination and Earth’s Obliquity from 58 to 48 Myr ago due to Solar System Chaos
Authors: Richard E. Zeebe
Figure caption: (a) Earth’s orbital inclination in the invariable frame from ZB18a. Horizontal lines indicate maximum values from 58 to 48 Ma and 48 to 0 Ma. (b) Earth’s obliquity, ϵ, calculated using our spin vector integration. ZB18a(1,1) (light blue) is the default solution with tidal dissipation and dynamical ellipticity parameters (ϑ = 1, η = 1). The change in the obliquity variation around 48 Ma (arrows) may be illustrated using the envelope (Hilbert transform, ﹩{ \mathcal H }(\epsilon )﹩; green). (c) ﹩2{ \mathcal H }(\epsilon -\overline{\epsilon })﹩ indicates a ∼50% increase at ∼48 Ma in the average amplitude around the mean obliquity value (﹩\overline{\epsilon }﹩).
Paper: ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Néstor Espinoza, Benjamin V. Rackham, Munazza K. Alam, Natalie Allen, Nikolay Nikolov, Ian C. Weaver, Kevin Ortiz Ceballos, David J. Osip, Dániel Apai, Andrés Jordán, Jonathan J. Fortney
Figure caption: The specific binned light curve used to construct the WLC in Figure 23. The left column shows the binned target light curves (blue) and the binned comparison light curves (purple). The target light curve is composed of the transit, systematics common to all bins and the comparisons, systematics common to all bins and just the target, and systematics unique to each bin. The LD coefficients used for each bin are printed below the light curves, and were determined with PyLDTk. The right column shows the “raw” (target/comparison) light curve in black dots. The larger-amplitude GP systematics (constant for each bin) are shown as a yellow dashed line, the smaller-amplitude polynomial systematics (unique per bin) are shown in red, and the combined GP and polynomial systematics are shown as green dashes. The residuals of the out-of-transit data from the green dashed line are printed in the bottom left corner (σ  w ).
Paper: ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Néstor Espinoza, Benjamin V. Rackham, Munazza K. Alam, Natalie Allen, Nikolay Nikolov, Ian C. Weaver, Kevin Ortiz Ceballos, David J. Osip, Dániel Apai, Andrés Jordán, Jonathan J. Fortney
Figure caption: Left: raw binned light curves (LC) of VLT/FORS2 transit UT170729 produced by dividing the comparison star LC (or the sum of the comparison star LC, in the case of the IMACS data) by the target’s. The wavelength range of each bin is printed in the bottom left corner. Middle: LC produced by dividing the raw LC by the CMC term shown in Figure 2 (final row). The number of sigma-clipped points is printed in the bottom left, and those points are marked with a black x. The theoretical photon noise precision is also printed as σ  w . The additional polynomial systematic correction specifically fit for each bin is shown as a magenta line. Right: the final CMC and polynomial corrected light curve, with the best-fit transit model in magenta and the residuals of the detrended data from the best-fit transit model on the bottom. The standard deviation (σ  r ) of the residuals in ppm is printed in the bottom left corner, and the ratio of σ  r  and σ  w  (β) is printed in the bottom right.
Paper: ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Néstor Espinoza, Benjamin V. Rackham, Munazza K. Alam, Natalie Allen, Nikolay Nikolov, Ian C. Weaver, Kevin Ortiz Ceballos, David J. Osip, Dániel Apai, Andrés Jordán, Jonathan J. Fortney
Figure caption: An example synthetic white-light curve (black dots) constructed by adding all 10 binned light curves in Figure 24. Given that all of the individual chromatic systematics are smaller relative to the white-light systematics and the transit, we do not see their effects in this light curve. This is exactly what we would see in a true light curve (e.g., see Figure 2). The red line represents the systematics produced by a random draw from a GP distribution created using the air mass, full width at half maximum (FWHM), and rotational angle as inputs. Here, σ  w  represents the residuals of the out-of-transit data from the GP systematic model, which would be zero if no white noise were added.
Paper: ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Néstor Espinoza, Benjamin V. Rackham, Munazza K. Alam, Natalie Allen, Nikolay Nikolov, Ian C. Weaver, Kevin Ortiz Ceballos, David J. Osip, Dániel Apai, Andrés Jordán, Jonathan J. Fortney
Figure caption: The transmission spectra of VLT/FORS2 data. The black diamonds with uncertainties represent the analysis done by Nikolov et al. (2018), and the cyan dots with uncertainties represent our initial analysis of the VLT/FORS2 data with the same wavelength bins and using the GP detrending method. An offset is applied so their mean depths are equal to one another. Each spectrum is a weighted average of observations taken with the B filter (350–617.3 nm) on the night of UT170729 and the R filter (529.3–801.3 nm) on the night of UT170822. The average deviation of each point relative to their uncertainties is 0.28σ, suggesting that the spectral structures are the same.
Paper: ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Néstor Espinoza, Benjamin V. Rackham, Munazza K. Alam, Natalie Allen, Nikolay Nikolov, Ian C. Weaver, Kevin Ortiz Ceballos, David J. Osip, Dániel Apai, Andrés Jordán, Jonathan J. Fortney
Figure caption: Corner plot of the GP fit on the FORS2 600B blue grism (UT170729) white-light light curve. The white-light curve fit is used to create the final CMC term, and this posterior corresponds to the fit shown in the first column of Figure 2. This would also be the same detrending routine used to detrend the binned data, if the GP (PCA+GP for the IMACS data) routine was used rather than the CMC routine. The alphas are the GP inverse squared length scales on the external parameter regressors. Alphas 0–5 correspond to the target dispersion drift, cross-dispersion drift, variation of the FWHM, air mass, mean sky flux, and rotator angle.
Paper: ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Néstor Espinoza, Benjamin V. Rackham, Munazza K. Alam, Natalie Allen, Nikolay Nikolov, Ian C. Weaver, Kevin Ortiz Ceballos, David J. Osip, Dániel Apai, Andrés Jordán, Jonathan J. Fortney
Figure caption: Same as Figure 19, but for VLT/FORS2 transit UT170822. Though there are a few cases (the eighth, ninth, and twelfth bins) where β is slightly less than one. We do not interpret this as the light curve being overcorrected; instead, given that they are nearly equal to unity, we see this as evidence that we achieved photon noise precision for those bins.
Paper: ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Néstor Espinoza, Benjamin V. Rackham, Munazza K. Alam, Natalie Allen, Nikolay Nikolov, Ian C. Weaver, Kevin Ortiz Ceballos, David J. Osip, Dániel Apai, Andrés Jordán, Jonathan J. Fortney
Figure caption: Same as Figure 16, but for the second IMACS transit (UT171108). Here, Alphas 0–4 correspond to air mass, drift of the wavelength solution, FWHM, mean sky flux, and central trace.
Paper: ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Néstor Espinoza, Benjamin V. Rackham, Munazza K. Alam, Natalie Allen, Nikolay Nikolov, Ian C. Weaver, Kevin Ortiz Ceballos, David J. Osip, Dániel Apai, Andrés Jordán, Jonathan J. Fortney
Figure caption: Same as Figure 18, but for Magellan/IMACS transit UT170804.
Paper: ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Néstor Espinoza, Benjamin V. Rackham, Munazza K. Alam, Natalie Allen, Nikolay Nikolov, Ian C. Weaver, Kevin Ortiz Ceballos, David J. Osip, Dániel Apai, Andrés Jordán, Jonathan J. Fortney
Figure caption: Same as Figure 20, but for Magellan/IMACS transit UT171108.
Paper: Magnetic Drag and 3D Effects in Theoretical High-resolution Emission Spectra of Ultrahot Jupiters: the Case of WASP-76b
Authors: Hayley Beltz, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Grace Ochs, Mireya Arora, Arjun Savel
Figure caption: Abundance contours of water (left) and CO (right) as a function of temperature and pressure, used to generate emission spectra, with dayside (red) and nightside (blue) equatorial profiles overplotted. The strong temperature difference between the dayside and nightside profiles results in a large difference in water abundances. CO, on the other hand, varies less as a function of temperature, and thus the CO abundances for the dayside and the nightside are similar.