adsabs/AstroCLIMB huggingface dataset:
Paper: The TESS Grand Unified Hot Jupiter Survey. II. Twenty New Giant Planets 
Authors: Samuel W. Yee, Joshua N. Winn, Joel D. Hartman, Luke G. Bouma, George Zhou, Samuel N. Quinn, David W. Latham, Allyson Bieryla, Joseph E. Rodriguez, Karen A. Collins, Owen Alfaro, Khalid Barkaoui, Corey Beard, Alexander A. Belinski, Zouhair Benkhaldoun, Paul Benni, Krzysztof Bernacki, Andrew W. Boyle, R. Paul Butler, Douglas A. Caldwell, Ashley Chontos, Jessie L. Christiansen, David R. Ciardi, Kevin I. Collins, Dennis M. Conti, Jeffrey D. Crane, Tansu Daylan, Courtney D. Dressing, Jason D. Eastman, Zahra Essack, Phil Evans, Mark E. Everett, Sergio Fajardo-Acosta, Raquel Forés-Toribio, Elise Furlan, Mourad Ghachoui, Michaël Gillon, Coel Hellier, Ian Helm, Andrew W. Howard, Steve B. Howell, Howard Isaacson, Emmanuel Jehin, Jon M. Jenkins, Eric L. N. Jensen, John F. Kielkopf, Didier Laloum, Naunet Leonhardes-Barboza, Pablo Lewin, Sarah E. Logsdon, Jack Lubin, Michael B. Lund, Mason G. MacDougall, Andrew W. Mann, Natalia A. Maslennikova, Bob Massey, Kim K. McLeod, Jose A. Muñoz, Patrick Newman, Valeri Orlov, Peter Plavchan, Adam Popowicz, Francisco J. Pozuelos, Tyler A. Pritchard, Don J. Radford, Michael Reefe, George R. Ricker, Alexander Rudat, Boris S. Safonov, Richard P. Schwarz, Heidi Schweiker, Nicholas J. Scott, S. Seager, Stephen A. Shectman, Chris Stockdale, Thiam-Guan Tan, Johanna K. Teske, Neil B. Thomas, Mathilde Timmermans, Roland Vanderspek, David Vermilion, David Watanabe, Lauren M. Weiss, Richard G. West, Judah Van Zandt, Michal Zejmo, Carl Ziegler
Figure caption: Distribution of planet radius as a function of planet equilibrium temperature, computed at the planets’ semimajor axis and assuming no albedo and perfect heat redistribution. TOI-1937A b is anomalously small for its orbit and is labeled in the plot.
Paper: The Complex Structure of the Bulge of M31
Authors: Denis Leahy, Traian Craiciu, Joseph Postma
Figure caption: Central part of F148W image (a) and residual images for a series of models (b)−(i). Each image is 125″ × 125″ (475 pc × 475 pc) centered on the nucleus. The gray scale for each image scale is linear from the image mean −0.5 standard deviations to the image mean +5 standard deviations. Panel (a) shows the nuclear region excluded (green rectangle) for the bulge-only fits (b), (c), and (d). Panels (b), (c), and (d) show the residual images for the best one-, two-, and three-component fits for the bulge with nuclear region excluded. These are the one-, two-, and three-Sérsic models with Sérsic index free and that have χ 2 and parameters given in Tables 4 and 5. Panels (e)−(i) show the residual images for the best four-, five-, six-, seven-, and eight-component fits for the bulge including the nuclear region. These models are given in Table 7. The residual images are given in order of decreasing χ 2 for each set ((b)−(d) fits with nuclear region omitted, and (e)−(i) fits to the entire image).
Paper: The Complex Structure of the Bulge of M31
Authors: Denis Leahy, Traian Craiciu, Joseph Postma
Figure caption: (a) Full (417″ × 417″) image of the eight-component bulge model (listed in Table 7). (b) Large (800″ × 800″) region showing the ellipses with semimajor axis R  e  for the three Sérsic components of the bulge model. (c) Central (40″ × 40″) region showing the ellipses with semimajor axis FWHM/2 for Gaussians or R  e  for the five components of the nuclear region model. Panels (b) and (c) have different scales than panel (a) in order to show the components with their greatly different sizes.
Paper: The Complex Structure of the Bulge of M31
Authors: Denis Leahy, Traian Craiciu, Joseph Postma
Figure caption: UVIT 1001 × 1001 pixel (417″ × 417″) images of the M31 bulge in (a) F148W filter, (b) F169M filter, (c) F172M filter, (d) N219M filter, (e) N279N filter, and (f) F148W filter with dust mask. The dust mask used to omit the dust cloud features is marked in blue in the F148W image. The pixel size is 0.″4168. 1″ at M31's distance is 3.81 pc.
Paper: The Complex Structure of the Bulge of M31
Authors: Denis Leahy, Traian Craiciu, Joseph Postma
Figure caption: Flowchart for finding best-fit set of functions to the image of the M31 bulge (Sections 2.2.1 and 3.2.2).
Paper: The Complex Structure of the Bulge of M31
Authors: Denis Leahy, Traian Craiciu, Joseph Postma
Figure caption: The nuclear spiral dust lane features: negative contours for the UVIT residual images (after subtraction of the best-fit bulge model) are shown in the first five panels: (a) F148W, (b) F169M, (c) F172M, (d) N219M, and (e) N279N; the extinction map from Dong et al. (2016) in gray scale is shown in panel (f). The ellipse in panel (f) marks a foreground dust cloud.
Paper: The Complex Structure of the Bulge of M31
Authors: Denis Leahy, Traian Craiciu, Joseph Postma
Figure caption: Overlays of nuclear spiral dust lane features from UVIT on the grayscale extinction map of Dong et al. (2016): N279N residual image negative contours (left panel) and F148W residual image negative contours (right panel).
Paper: The Complex Structure of the Bulge of M31
Authors: Denis Leahy, Traian Craiciu, Joseph Postma
Figure caption: Contour lines for the UVIT images of the bulge of M31 in the (a) F148W, (b) F169M, (c) F172M, (d) N219M, and (e) N279N filters. On the same scale, the contours from Beaton et al. (2007) are shown for comparison in panel (f). The boxy nature of the contours is evident at all wave bands.
Paper: Offsets between X-Ray and Radio Components in X-Ray Jets: The AtlasX
Authors: Karthik Reddy, Markos Georganopoulos, Eileen T. Meyer, Mary Keenan, Kassidy E. Kollmann
Figure caption: Stacked histograms for the deprojected offsets (in kiloparsecs), plotted on a log scale, for the knots in the FR II–type sources. (a) Histograms for the Xf-type and Co-s-type offsets for all the FR II–type sources. The Co-s-type knots are plotted by assuming a 0.″15 offset, and are distributed like the Xf types. The histograms roughly describe a unimodal profile peaking at ≈4 kpc, suggesting similar knot sizes and formation mechanisms. (b) Only the Xf-type offsets, grouped into their respective subclasses; the CDQs and LDQs peak at higher values than the FR IIs, which may suggest an intrinsic difference between the knots in quasars and those in FR IIs. Alternatively, we can interpret this difference as a result of the knots moving, where their relativistic motion increases the observed offset by a factor of δ. (c) and (d) The δ-corrected counterparts of the top panels, where we assume Γ = 1.25 to estimate δ. The corrected offsets are distributed more uniformly across classes and peak at ≈2 kpc, which is a better lower limit on the sizes of the knots (see Section 4.3 for discussion).
Paper: Offsets between X-Ray and Radio Components in X-Ray Jets: The AtlasX
Authors: Karthik Reddy, Markos Georganopoulos, Eileen T. Meyer, Mary Keenan, Kassidy E. Kollmann
Figure caption: Demonstrating how similar offsets imply similar linear sizes using Centaurus A. With the smoothed Chandra X-ray image in the background, the VLA 8.4 GHz A- and B-config contours are overlaid on the left and right panels, respectively. The beam size is shown to the bottom left of each image, and the dashed red arrow points into the core. The A-config image resolves the radio knot A2A, while the B-config image produces a point-like knot, with its peak located near the weighted centroid of the resolved knot (indicated with a red “X”), measured using the dashed black ellipse, producing an X-ray/radio peak-to-peak offset. This means that when a knot like A2A—with extended radio and compact X-ray-emitting regions—becomes unresolved, it produces an offset, which is a lower limit on the knot’s size. Hence, similar offsets imply similar structures.
Paper: Offsets between X-Ray and Radio Components in X-Ray Jets: The AtlasX
Authors: Karthik Reddy, Markos Georganopoulos, Eileen T. Meyer, Mary Keenan, Kassidy E. Kollmann
Figure caption: Categorical parallel coordinates plot for the offsets of the knots in FR II–type and FR I–type sources. Each stripe represents a group of knots with identical values at each coordinate, and is colored according to the offset type. Starting from the left, the coordinates are source type, subclassification, parsec-scale jet speed, redshift range, and type of offset.
Paper: Offsets between X-Ray and Radio Components in X-Ray Jets: The AtlasX
Authors: Karthik Reddy, Markos Georganopoulos, Eileen T. Meyer, Mary Keenan, Kassidy E. Kollmann
Figure caption: Histograms of the sky-projected offsets in knots and hotspots. The left panels show histograms of the offsets in knots for the FR I and FR II types, while the right panels show histograms of the offsets in hotspots. The units of the offsets are arcseconds and kiloparsecs in the top and bottom panels, respectively.
Paper: Offsets between X-Ray and Radio Components in X-Ray Jets: The AtlasX
Authors: Karthik Reddy, Markos Georganopoulos, Eileen T. Meyer, Mary Keenan, Kassidy E. Kollmann
Figure caption: Histogram of the standard deviations of the knot regions on deconvolved images for Xf (green) and Co-s-type (gray) knots. The two blue dashed lines locate the half and single ACIS-S pixel sizes, while the red dashed line indicates the median of the distribution.
Paper: Neural Stellar Population Synthesis Emulator for the DESI PROVABGS
Authors: K. J. Kwon, ChangHoon Hahn, Justin Alsing
Figure caption: Fractional error of the PROVABGS emulator based on the 100,000 test SEDs. The fractional errors are calculated with respect to the model SEDs calculated using PROVABGS-FSPS. Each panel represents a separate wavelength bin with a unique emulator. The fractional errors for 68%, 95%, 99%, and 99.9% of the test SEDs are shown with different shades. The dashed lines represent ±1% errors. The emulator can reconstruct SEDs to subpercent accuracy for 95% of the test SEDs over the full wavelength range, and for 99.9% of the test SEDs over λ > 3000 Å. Although there is a relatively large error on λ < 3000 Å, we find that this does not impact the accuracy of the posteriors of the properties of forward-modeled BGS-like spectra, because BGS spectra generally have low S/N at these wavelengths.
Paper: Neural Stellar Population Synthesis Emulator for the DESI PROVABGS
Authors: K. J. Kwon, ChangHoon Hahn, Justin Alsing
Figure caption: The distribution of the physical properties of 93 LGAL-simulated galaxies that we use for our emulator vs. PROVABGS-FSPS posterior comparison (red). We focus on the total stellar mass, average star formation rate over 1 Gyr, mass-weighted metallicity, and mass-weighted stellar age. The black contours mark the 68th and 95th percentiles of each property for the entire LGAL samples. The selected LGAL galaxies are a representative sample of the full LGAL sample. We infer the posteriors of galaxy properties using both our emulator and the PROVABGS-FSPS from realistic BGS-like spectra constructed from these simulated galaxies.
Paper: Neural Stellar Population Synthesis Emulator for the DESI PROVABGS
Authors: K. J. Kwon, ChangHoon Hahn, Justin Alsing
Figure caption: Cumulative distribution of the absolute fractional error of the PROVABGS emulator, averaged over the wavelength 2400 < λ < 10000 Å. Each shaded region marks the percentiles of the emulator reconstruction errors (68%, 95%, 99%, 99.9%, from darkest to lightest). The emulator produces the mean absolute fractional error ≪1% on 99.9% test SEDs.
Paper: Neural Stellar Population Synthesis Emulator for the DESI PROVABGS
Authors: K. J. Kwon, ChangHoon Hahn, Justin Alsing
Figure caption: Posterior distributions of galaxy properties derived from a synthetic BGS-like spectrum inferred using the emulator (red) and PROVABGS-FSPS (black). For a typical BGS-like spectrum, see Hahn et al. (2022b). The contours mark the 68th, 95th, and 99.7th percentiles and the vertical dashed lines in the histograms denote the median of 1D marginalized posteriors. The posteriors inferred using the emulator and PROVABGS-FSPS are in excellent agreement.
Paper: Light-curve Recovery with the Vera Rubin Observatory’s LSST. I. Pulsating Stars in Local Group Dwarf Galaxies
Authors: M. Di Criscienzo, S. Leccia, V. Braga, I. Musella, G. Bono, M. Dall'Ora, G. Fiorentino, M. Marconi, R. Molinaro, V. Ripepi, K. Carrell, Y. Choi, S. Savarese, L. Schreiber
Figure caption: Template’s light curves (orange) and simulated observations (colored points, crossed are used for saturated magnitudes) in ugrizy of selected RRab (a), RRc (b), short-period CCs CEP1 (c), long-period CCs CEP2 (d), and LPVs (e) at the position and distance of the Sagittarius dwarf galaxy (R.A. = 283.76292, decl. = −30.47833, dist = 0.02). The survey cadence is simulated by baselinev2.010 yrs.db, and only the observations expected in the first survey’s year were taken into consideration. Photometric errors (<0.001 mag) derived from Opsim and used in the simulation (see text) are too small to be shown.
Paper: Light-curve Recovery with the Vera Rubin Observatory’s LSST. I. Pulsating Stars in Local Group Dwarf Galaxies
Authors: M. Di Criscienzo, S. Leccia, V. Braga, I. Musella, G. Bono, M. Dall'Ora, G. Fiorentino, M. Marconi, R. Molinaro, V. Ripepi, K. Carrell, Y. Choi, S. Savarese, L. Schreiber
Figure caption: Simulated observations for an RRc in Sagittarius after 1 yr of observations in different magnitude–phase planes (colored filled points). For those photometric bands where Lcfitting converges (using three harmonics), we have also added the fitting result (black curve). In the z band, our choice of the number of harmonics is clearly too high due to the presence of a large gap in phase.
Paper: Light-curve Recovery with the Vera Rubin Observatory’s LSST. I. Pulsating Stars in Local Group Dwarf Galaxies
Authors: M. Di Criscienzo, S. Leccia, V. Braga, I. Musella, G. Bono, M. Dall'Ora, G. Fiorentino, M. Marconi, R. Molinaro, V. Ripepi, K. Carrell, Y. Choi, S. Savarese, L. Schreiber
Figure caption:                         Left: simulated ugriz                      y observations of a typical RRab in Sagittarius as in Figure 2. Right: single periodogram in each band (up) vs. multiband periodogram computed with a shared-phase (Nbase, Nband) = (1, 0) multiband (down). The last approach fits a single model to the full data and clearly recovers the true period (P = 0.38354 days).
Paper: Light-curve Recovery with the Vera Rubin Observatory’s LSST. I. Pulsating Stars in Local Group Dwarf Galaxies
Authors: M. Di Criscienzo, S. Leccia, V. Braga, I. Musella, G. Bono, M. Dall'Ora, G. Fiorentino, M. Marconi, R. Molinaro, V. Ripepi, K. Carrell, Y. Choi, S. Savarese, L. Schreiber
Figure caption: Simulated ugrizy light curves of RRab(a) and CEP2(b) in Leo I after 10 yr of observations. The orange curve in (a) is the starting template, while the black line in (b) is the result of the fit performed by PulsatingStarRecovery using seven harmonics.
Paper: Light-curve Recovery with the Vera Rubin Observatory’s LSST. I. Pulsating Stars in Local Group Dwarf Galaxies
Authors: M. Di Criscienzo, S. Leccia, V. Braga, I. Musella, G. Bono, M. Dall'Ora, G. Fiorentino, M. Marconi, R. Molinaro, V. Ripepi, K. Carrell, Y. Choi, S. Savarese, L. Schreiber
Figure caption: Light curve in the g band of LPVs in Sex A after 10 (circle) and 2 (crosses) years. The dotted line represents the detection limit in g at the Sex A position in the sky.
Paper: Light-curve Recovery with the Vera Rubin Observatory’s LSST. I. Pulsating Stars in Local Group Dwarf Galaxies
Authors: M. Di Criscienzo, S. Leccia, V. Braga, I. Musella, G. Bono, M. Dall'Ora, G. Fiorentino, M. Marconi, R. Molinaro, V. Ripepi, K. Carrell, Y. Choi, S. Savarese, L. Schreiber
Figure caption: RRab template intensity-weighted mean magnitude at the 3D sky position of selected galaxies of our sample (see Table 4) vs. mean detection limit derived by Opsim at that sky position in different filters. Leo I is marked with a cross (see text).
Paper: Light-curve Recovery with the Vera Rubin Observatory’s LSST. I. Pulsating Stars in Local Group Dwarf Galaxies
Authors: M. Di Criscienzo, S. Leccia, V. Braga, I. Musella, G. Bono, M. Dall'Ora, G. Fiorentino, M. Marconi, R. Molinaro, V. Ripepi, K. Carrell, Y. Choi, S. Savarese, L. Schreiber
Figure caption: Selected dwarf galaxies in an Aitoff diagram (Galactic coordinates). The location of the Magellanic Clouds is also shown, which will be discussed in detail in Section 3. Leo I is labeled with a red cross (see text).
Paper: Light-curve Recovery with the Vera Rubin Observatory’s LSST. I. Pulsating Stars in Local Group Dwarf Galaxies
Authors: M. Di Criscienzo, S. Leccia, V. Braga, I. Musella, G. Bono, M. Dall'Ora, G. Fiorentino, M. Marconi, R. Molinaro, V. Ripepi, K. Carrell, Y. Choi, S. Savarese, L. Schreiber
Figure caption: Software scheme diagram. Output quantities are described in Section 2.4 and Table 2.
Paper: Offsets between X-Ray and Radio Components in X-Ray Jets: The AtlasX
Authors: Karthik Reddy, Markos Georganopoulos, Eileen T. Meyer, Mary Keenan, Kassidy E. Kollmann
Figure caption: Trends in flux ratios. (a) The flux ratio plotted against the normalized distance from the core. The components from each jet are assigned the same color and joined with a solid line. The dashed blue line shows the linear fit, which describes a general trend where the flux ratio decreases along the jet. The shaded region indicates the 68% confidence interval. (b) The histogram of the slopes for each line segment plotted in (a), with a peak near zero. Only the slopes of 16 of 34 segments lie below zero, indicating that the declining trend is only marginally significant.
Paper: Offsets between X-Ray and Radio Components in X-Ray Jets: The AtlasX
Authors: Karthik Reddy, Markos Georganopoulos, Eileen T. Meyer, Mary Keenan, Kassidy E. Kollmann
Figure caption: Histograms of knot ejection timescales derived using interknot distances for different bulk Lorentz factors. (a) The histogram of the timescales measured using the orientation scheme adopted in Section 4.2, where the mean is ≈105 yr for Γ = 1.18, while it is smaller by a factor of 3 for Γ = 1.5 and 3. (b) The same, but with all the angles of the quasars set to an unrealistic value of 5°. The distribution peaks above 105 yr for Γ = 1.18 and 1.5, while it remains roughly similar for Γ = 3, suggesting that the knots can be mildly relativistic, at most, if intermittent activity in the central engine is producing them.
Paper: Offsets between X-Ray and Radio Components in X-Ray Jets: The AtlasX
Authors: Karthik Reddy, Markos Georganopoulos, Eileen T. Meyer, Mary Keenan, Kassidy E. Kollmann
Figure caption: Class-wise histograms for the (a) X-ray and (b) radio luminosity of knots in FR II–type sources. (c) The mean values of each class at each wavelength, where the radio luminosity values are nudged to the right by 0.4 units (multiplied by 1.26), for easier comparison. The similarity in the interclass distance between the distributions (measured using the AD test statistic) at the X-ray and radio wavelengths suggests that the bulk Lorentz factors for both the emitting plasmas are similar.
Paper: Offsets between X-Ray and Radio Components in X-Ray Jets: The AtlasX
Authors: Karthik Reddy, Markos Georganopoulos, Eileen T. Meyer, Mary Keenan, Kassidy E. Kollmann
Figure caption: Examples of sources excluded from the analysis. The top panels show examples of jets with no spatially correlated X-ray and radio features. (a) X-ray image (bin: 0.5) of AP Librae, overlaid with VLA 1.4 GHz radio contours, where both jets lie along the same PA, but do not show correlated features. (b) X-ray image of 4C +13.41, with VLA 8.4 GHz radio contours overlaid. The X-ray and radio jets are mostly spatially disjointed. (c) X-ray image of 3C 371, with the VLA 4.8 GHz radio contours overlaid. The small interknot spacing (separation <1″) prevents the accurate measuring of the centroids on the LIRA images.
Paper: Offsets between X-Ray and Radio Components in X-Ray Jets: The AtlasX
Authors: Karthik Reddy, Markos Georganopoulos, Eileen T. Meyer, Mary Keenan, Kassidy E. Kollmann
Figure caption:  δ versus Γ for different inclination angles. A jet decelerating in the red zone of each curve experiences reduced δ, while it rises in the green zone.
Paper: Offsets between X-Ray and Radio Components in X-Ray Jets: The AtlasX
Authors: Karthik Reddy, Markos Georganopoulos, Eileen T. Meyer, Mary Keenan, Kassidy E. Kollmann
Figure caption: Redshift distribution for X-ray jets. (a) A stacked histogram of the redshifts for all 199 X-ray jets compiled in this work; the sources that are included in and excluded from the offset analysis are colored blue and gray, respectively. (b) A class-wise stacked histogram of the redshifts of the sources considered for offset analysis; the FR I–type and FR II–type sources are colored orange and blue, respectively. (c) Stacked redshift distributions of the excluded FR II–type sources, divided into individual spectral classes.
Paper: Offsets between X-Ray and Radio Components in X-Ray Jets: The AtlasX
Authors: Karthik Reddy, Markos Georganopoulos, Eileen T. Meyer, Mary Keenan, Kassidy E. Kollmann
Figure caption: Histograms of log-scaled flux ratios of knots in CDQs and LDQ/FR II sources. A two-sample AD test between the two groups reveals no statistically significant difference, suggesting that the contribution of the IC/CMB to the X-ray emission may be minimal.
Paper: Offsets between X-Ray and Radio Components in X-Ray Jets: The AtlasX
Authors: Karthik Reddy, Markos Georganopoulos, Eileen T. Meyer, Mary Keenan, Kassidy E. Kollmann
Figure caption: Normalized offsets in knots and hotspots of FR II–type jets plotted against the normalized distance from the core, showing a loose trend of the offsets increasing with distance. The moving-knot model can produce this increase if a forward-moving shock determines the radio peak in the blob.
Paper: Offsets between X-Ray and Radio Components in X-Ray Jets: The AtlasX
Authors: Karthik Reddy, Markos Georganopoulos, Eileen T. Meyer, Mary Keenan, Kassidy E. Kollmann
Figure caption: Histograms of deprojected Xf-type offsets in hotspots, stacked with Co-s-type hotspots, assuming a 0.″15 angular offset. Unlike the offsets in knots, the Xf-type and Co-s-type hotspots may indicate different structures (see Section 4.7).