adsabs/AstroCLIMB huggingface dataset:
Paper: More Old Dogs, More New Tricks: Photographic Plates of the Globular Cluster M10 (NGC 6254) Digitized with a Commercial Scanner
Authors: T. J. Davidge
Figure caption: Plate-to-plate dispersion in the photometric measurements. The variance σ is in magnitudes measured from the 16 B emulsion plates. Instrumental magnitudes are shown along the lower axis, while approximate V magnitudes calculated from the relation in Figure 2 are shown along the upper axis. Sources within 37″ of the cluster center have not been included. Sources with a large dispersion that is driven by a single point or that have large uncertainties in the PSF fitting due to saturation have also been excluded (see text). The upturn in σ at the bright end is due to image saturation, the degree of which varies between plates. It can be seen that σ progressively increases near the faint end owing to the lowering of the S/N toward fainter magnitudes. Known variables are indicated in red, while new variables identified in this study are highlighted in green with their identification number. The W Virginis variable V2 and the new candidate variables 5533 and 3744 stand out from the other stars on the σ vs. magnitude plane.
Paper: More Old Dogs, More New Tricks: Photographic Plates of the Globular Cluster M10 (NGC 6254) Digitized with a Commercial Scanner
Authors: T. J. Davidge
Figure caption: Relation between instrumental and V magnitudes. The green line is a linear least-squares fit that does not include star 4255, which has the smallest bp − rp color of the sources in this figure. The scatter at the bright end is due to color effects, which become significant when bp − rp ≥ 1.7.
Paper: More Old Dogs, More New Tricks: Photographic Plates of the Globular Cluster M10 (NGC 6254) Digitized with a Commercial Scanner
Authors: T. J. Davidge
Figure caption: Examples of plate quality. Starting from the top left panel and moving clockwise: plates with (1) the B emulsion and excellent cosmetics (# 23253); (2) the E40 emulsion and excellent cosmetics (# 21514); (3) cosmetic defects that are likely due to problems with development, fixing, and/or handling (# 20673); and (4) scattered moon light (# 21569). Each plate covers 37′ × 37′, with east to the right and north at the bottom. (The FITS files of the unprocessed images shown in this figure, as well as those for the other nights, can be accessed in the online version of this paper).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: More Old Dogs, More New Tricks: Photographic Plates of the Globular Cluster M10 (NGC 6254) Digitized with a Commercial Scanner
Authors: T. J. Davidge
Figure caption: Difference between V and instrumental magnitudes (ΔV) as a function of bp − rp. Two linear trends are defined, and the green lines show linear least-squares fits to points with bp − rp < 1, 4 and bp − rp > 1.3. The relations meet at bp − rp = 1.38.
Paper: Predicting Exoplanet Occurrence Using Association Analysis
Authors: Vasundhara Gatne, Michael L. Wong, Anirudh Prabhu
Figure caption: Notable network visualizations highlighting key associations in the six data subsets outlined in Figure 4 and Table 6. In these graphs, blue boxes represent planet or stellar types, red circles denote association rules, and the intensity of a rule’s red color denotes the rule’s lift (see Section 3.3).
Paper: Predicting Exoplanet Occurrence Using Association Analysis
Authors: Vasundhara Gatne, Michael L. Wong, Anirudh Prabhu
Figure caption: Our scientific workflow. We begin by cleaning the data set and assigning missing stellar and planetary attributes, followed by assigning primary classifications to each exoplanet. Further planetary/stellar subtype classifications result in six main subsets of our data.
Paper: Predicting Exoplanet Occurrence Using Association Analysis
Authors: Vasundhara Gatne, Michael L. Wong, Anirudh Prabhu
Figure caption: Histogram of planets by orbital-period-based planetary subtype.
Paper: Predicting Exoplanet Occurrence Using Association Analysis
Authors: Vasundhara Gatne, Michael L. Wong, Anirudh Prabhu
Figure caption: Histogram of planets by temperature-based planetary subtype.
Paper: More Old Dogs, More New Tricks: Photographic Plates of the Globular Cluster M10 (NGC 6254) Digitized with a Commercial Scanner
Authors: T. J. Davidge
Figure caption: Phased light curves of the W Vir stars V2 and V3, the BL Her star V24, and the RR Lyrae star V22. The photometric measurements made from the plates are shown as black crosses, while the Stetson V CCD measurements are shown as green squares. Phases were computed using ephemerides from the GCVS version 5.1 (N. N. Samus et al. 2017). The relation shown in Figure 2 is used to compute V for the three stars brighter than V = 14 (V2, V3, and V24), while the relation in Figure 3 was used to calculate V for V22. The bright and faint limits of the DAO and Stetson V2 light curves are in excellent agreement. The ∼0.4 offset in phase between the DAO and Stetson light curves is consistent with the period of V2 changing over the past century. As for V3, there is a ∼0.3 mag offset between many of the DAO and Stetson measurements at some phases. The phase coverage of the DAO measurements is not sufficient to identify a difference in phasing. Still, the dispersion in the DAO measurements at a given phase is comparable to that in the Stetson photometry. The phase coverage of the V24 measurements is poor, although the bright and faint limits of the light curve in Figure 3 of A. A. Ferro et al. (2020), shown with the dashed green lines, are consistent with the majority of the DAO measurements. V22 is an RR Lyrae variable that has been associated with M10 (A. A. Ferro et al. 2020), and its light variations are consistent with the ±0.2 mag variations seen in the DAO light curve. There is also good agreement with the bright and faint limits in Figure 3 of A. A. Ferro et al. (2020).
Paper: More Old Dogs, More New Tricks: Photographic Plates of the Globular Cluster M10 (NGC 6254) Digitized with a Commercial Scanner
Authors: T. J. Davidge
Figure caption: Same as Figure 4, but for stars within 37″ of the cluster center that are in the 12 plates where the area near the cluster center is not completely saturated. The upper axis shows approximate V magnitudes calculated from the relation in Figure 3 for a fixed bp − rp = 2, which is the approximate color of bright giants in M10. As expected, the plate-to-plate consistency at a given magnitude is poorer than in Figure 4 owing to crowding. Still, internally consistent photometry for the brightest stars at the 10%–20% level can be obtained from the plates. The variables V1 and V30 stand out with respect to the other stars.
Paper: More Old Dogs, More New Tricks: Photographic Plates of the Globular Cluster M10 (NGC 6254) Digitized with a Commercial Scanner
Authors: T. J. Davidge
Figure caption: CMD of stars in M10 that are within 90″ of the cluster center, which corresponds roughly to the cluster half-light radius. The photometric measurements are from Gaia DR3. Additional constraints were placed on the parallax and proper-motion measurements to suppress contamination from noncluster stars. The open red squares are stars in Tables 3 and 4 that have parallaxes <0.5 mas. Stars that are outliers from the cluster sequence are labeled. Star 3744, which was identified as a variable star, falls well off of the M10 giant branch and has a Gp that is over 1 mag below the RGB tip as defined by the brightest giants near the cluster center. The location of star 3744 with respect to the M10 CMD is indicated in the inset.
Paper: More Old Dogs, More New Tricks: Photographic Plates of the Globular Cluster M10 (NGC 6254) Digitized with a Commercial Scanner
Authors: T. J. Davidge
Figure caption: Photometric observations of stars 6071, 2262, and 4003, which are listed as variable in the Gaia DR3. Evidence for variability with an amplitude of roughly 1 mag can be seen in the light curve of the foreground star 6071. There is evidence for long-term and possible short-term variations. Like star 6071, star 2262 has a parallax that is consistent with it being a foreground object. The dispersion during the same observing blocks suggests that variations may occur on timescales of a day or less. Star 4003 has a parallax that is consistent with that of M10. It is offset from the cluster HB on the CMD by roughly 1 mag, suggesting that it might be a supra-HB star. The dispersion may be due to long-term variations, although it falls close to the ridgeline along the σ axis in Figure 10.
Paper: More Old Dogs, More New Tricks: Photographic Plates of the Globular Cluster M10 (NGC 6254) Digitized with a Commercial Scanner
Authors: T. J. Davidge
Figure caption: Location on the σ vs. magnitude plane of variables in the Gaia DR3. The top panel includes sources that are at least 37″ from the cluster center, while the bottom panel shows sources within 37″ of the center. The Gaia variables and new candidate variables are marked with green squares. Only three of the stars flagged as variable in the Gaia database (6071, 4003, and 2262) fall along or close to the upper envelope along the dispersion axis and so are candidates for finding photometric variations. Star 4003 has a parallax that is consistent with that of M10.
Paper: More Old Dogs, More New Tricks: Photographic Plates of the Globular Cluster M10 (NGC 6254) Digitized with a Commercial Scanner
Authors: T. J. Davidge
Figure caption: Light variations of the stars 3744 and 5533, which were identified as variable based on their locations in Figure 4. The parallax of star 3744 differs from that of M10 at roughly the 1σ level. Its photometric properties are consistent with it being a highly evolved star, and its very red color places significant uncertainties on the estimated V magnitudes. While time coverage is spotty, the repeatability of the points is suggestive of a period near ∼80 days. Star 3744 then appears to be an LPV at roughly the same distance as M10. The parallax of star 5533 places it in the foreground, and its photometric properties suggest that it is likely a K giant.
Paper: More Old Dogs, More New Tricks: Photographic Plates of the Globular Cluster M10 (NGC 6254) Digitized with a Commercial Scanner
Authors: T. J. Davidge
Figure caption: Phased light curves of the SR variables V27 and V29. The green dashed lines are the approximate bright and faint limits of the light curves in Figure 3 of A. A. Ferro et al. (2020). The periods used to phase the data are from A. A. Ferro et al. (2020). We are not aware of a published epoch for V29, and the phasing used here assumes a baseline epoch of 1932 July 26, which is the date of the first observation taken with the “B” emulsion. The DAO measurements for V27 fall within the bright and faint limits defined by CCD light curves. As for V29, some of the DAO measurements fall within the limits defined by the CCD data, although there is a systematic downward trend with increasing phase, suggesting that the measurements discussed by A. A. Ferro et al. (2020) may not track the entire light cycle.
Paper: Additional JWST/NIRSpec Transits of the Rocky M Dwarf Exoplanet GJ 1132 b Reveal a Featureless Spectrum
Authors: Katherine A. Bennett, Ryan J. MacDonald, Sarah Peacock, Junellie Perez, E. M. May, Sarah E. Moran, Lili Alderson, Jacob Lustig-Yaeger, Hannah R. Wakeford, David K. Sing, Kevin B. Stevenson, Natasha E. Batalha, Mercedes López-Morales, Munazza K. Alam, Joshua D. Lothringer, Guangwei Fu, James Kirk, Jeff A. Valenti, L. C. Mayorga, Kristin S. Sotzen
Figure caption: Retrieval results for GJ 1132 b. Top panels: comparison between the retrieved transmission spectra for the FIREFLy reduction with all four visits (top-left panel) and for three visits with Visit 1 excluded (top-right panel). Three POSEIDON retrieval models are shown: (i) an atmosphere (gray), (ii) stellar contamination (orange), and (iii) a flat line (purple). The corresponding median retrieved spectra (solid lines) and 1σ and 2σ model confidence intervals (dark and light contours) are overlaid. Labels indicate H2O and CO2 absorption bands (neither are detected, but CO2 is allowed by FIREFLy). Bottom panels: atmosphere posterior histograms for the three data reductions: FIREFLy (gray), Eureka! (pink), and ExoTiC-JEDI (cyan). The four-visit combined analysis weakly favors a thin H2O-rich atmosphere (driven by a short-wavelength slope), but this solution is not favored when Visit 1 is excluded.
Paper: Additional JWST/NIRSpec Transits of the Rocky M Dwarf Exoplanet GJ 1132 b Reveal a Featureless Spectrum
Authors: Katherine A. Bennett, Ryan J. MacDonald, Sarah Peacock, Junellie Perez, E. M. May, Sarah E. Moran, Lili Alderson, Jacob Lustig-Yaeger, Hannah R. Wakeford, David K. Sing, Kevin B. Stevenson, Natasha E. Batalha, Mercedes López-Morales, Munazza K. Alam, Joshua D. Lothringer, Guangwei Fu, James Kirk, Jeff A. Valenti, L. C. Mayorga, Kristin S. Sotzen
Figure caption: Mean molecular weight constraints for GJ 1132 b’s atmosphere. Top panels: constraints from all four visits combined, comparing the prior distribution (blue) with the posteriors from FIREFLy (gray; left), Eureka! (pink; middle), and ExoTiC-JEDI (cyan; right). Bottom panels: constraints from three visits with Visit 1 excluded. The peaks in the prior at ∼100% abundances of each considered molecule (annotated) arise from the use of the centered log-ratio prior (e.g., B. Benneke & S. Seager 2012), which formally encodes that all gases are equally likely to be the background gas. Higher relative prior amplitudes arise from multiple molecules overlapping in a given mean molecular weight bin (e.g., N2 and CO both have μ = 28). The four-visit results favor an H2O-dominated composition for all three reductions, but without Visit 1, this solution is disfavored relative to higher mean molecular weights (e.g., CO2-dominated atmospheres). H2-dominated atmospheres are excluded in all cases.
Paper: Additional JWST/NIRSpec Transits of the Rocky M Dwarf Exoplanet GJ 1132 b Reveal a Featureless Spectrum
Authors: Katherine A. Bennett, Ryan J. MacDonald, Sarah Peacock, Junellie Perez, E. M. May, Sarah E. Moran, Lili Alderson, Jacob Lustig-Yaeger, Hannah R. Wakeford, David K. Sing, Kevin B. Stevenson, Natasha E. Batalha, Mercedes López-Morales, Munazza K. Alam, Joshua D. Lothringer, Guangwei Fu, James Kirk, Jeff A. Valenti, L. C. Mayorga, Kristin S. Sotzen
Figure caption: Top: the weighted mean of all four visits is shown for all three reductions, with the mean transit depth for FIREFLy shown as a horizontal dashed black line. No offsets have been applied to any data set. Bottom: the σ difference between reductions is shown, with the 1σ difference region highlighted in gray. Reductions show exquisite agreement to within 1σ for most channels.
Paper: Additional JWST/NIRSpec Transits of the Rocky M Dwarf Exoplanet GJ 1132 b Reveal a Featureless Spectrum
Authors: Katherine A. Bennett, Ryan J. MacDonald, Sarah Peacock, Junellie Perez, E. M. May, Sarah E. Moran, Lili Alderson, Jacob Lustig-Yaeger, Hannah R. Wakeford, David K. Sing, Kevin B. Stevenson, Natasha E. Batalha, Mercedes López-Morales, Munazza K. Alam, Joshua D. Lothringer, Guangwei Fu, James Kirk, Jeff A. Valenti, L. C. Mayorga, Kristin S. Sotzen
Figure caption: Retrieved stellar properties from GJ 1132 b’s FIREFLy transmission spectra from Visit 1 (NIRSpec G395H) and Visit 3 (NIRSpec G395M). These stellar contamination retrievals assume all spectral features arise from unocculted heterogeneities (i.e., no planetary absorption). The slope seen in Visit 1 can be explained with a moderate starspot covering fraction (fhet ∼ 10%), but the relatively flat Visit 3 spectrum does not require unocculted starspots (fhet → 0).
Paper: Additional JWST/NIRSpec Transits of the Rocky M Dwarf Exoplanet GJ 1132 b Reveal a Featureless Spectrum
Authors: Katherine A. Bennett, Ryan J. MacDonald, Sarah Peacock, Junellie Perez, E. M. May, Sarah E. Moran, Lili Alderson, Jacob Lustig-Yaeger, Hannah R. Wakeford, David K. Sing, Kevin B. Stevenson, Natasha E. Batalha, Mercedes López-Morales, Munazza K. Alam, Joshua D. Lothringer, Guangwei Fu, James Kirk, Jeff A. Valenti, L. C. Mayorga, Kristin S. Sotzen
Figure caption: Best-fit multicomponent stellar models for each visit. Each of the four main panels corresponds to one visit, and contains three subpanels. In every subpanel, all models with Δχ2 ≤ 6 from the best-fit are shown (25 models for Visit 1, 46 for Visit 2, 9 for Visit 3, and 10 for Visit 4). The models are nearly indistinguishable due to their close agreement. The observed spectra, smoothed to the resolution of G395M, are overplotted in black. The residuals (in units of σ) are shown in each bottom subpanel, with dotted lines indicating the ±1σ range.
Paper: Additional JWST/NIRSpec Transits of the Rocky M Dwarf Exoplanet GJ 1132 b Reveal a Featureless Spectrum
Authors: Katherine A. Bennett, Ryan J. MacDonald, Sarah Peacock, Junellie Perez, E. M. May, Sarah E. Moran, Lili Alderson, Jacob Lustig-Yaeger, Hannah R. Wakeford, David K. Sing, Kevin B. Stevenson, Natasha E. Batalha, Mercedes López-Morales, Munazza K. Alam, Joshua D. Lothringer, Guangwei Fu, James Kirk, Jeff A. Valenti, L. C. Mayorga, Kristin S. Sotzen
Figure caption: Surface pressure vs. mean molecular weight constraints for GJ 1132 b. Top panels: posterior probability density (colored contours) from four NIRSpec G395H/M transits combined from FIREFLy (gray; left), Eureka! (pink; middle), and ExoTiC-JEDI (cyan; right). Bottom panels: the same as the top panels, but excluding Visit 1. The 1σ, 2σ, and 3σ credible regions have solid line boundaries, while the 0.5σ, 1.5σ, and 2.5σ credible regions have dashed boundaries. Pressure upper limits from emission spectroscopy of GJ 1132 b (2σ limits from Q. Xue et al. 2024) are annotated for 100% H2O (blue arrow), an Earth-like composition (brown arrow), and 100% CO2 (green arrow). Three exoplanets with detected atmospheres and well-constrained mean molecular weights heavier than pure H2+He (TOI-270d; B. Benneke et al. 2024; GJ 9827d; C. Piaulet-Ghorayeb et al. 2024; and K2-18b; S. P. Schmidt et al. 2025) are annotated (circles with arrows, located at the 2σ lower limit on the surface / cloud pressure), alongside terrestrial atmospheres in the solar system. GJ 1132 b’s transmission spectrum favors a thin ∼10−4 bar H2O-dominated atmosphere when using all four visits, but the exclusion of Visit 1 allows for a wider range of heavier and/or thin atmospheres (or no atmosphere) as viable ways to produce a featureless three-visit transmission spectrum (see Figure 7).
Paper: Additional JWST/NIRSpec Transits of the Rocky M Dwarf Exoplanet GJ 1132 b Reveal a Featureless Spectrum
Authors: Katherine A. Bennett, Ryan J. MacDonald, Sarah Peacock, Junellie Perez, E. M. May, Sarah E. Moran, Lili Alderson, Jacob Lustig-Yaeger, Hannah R. Wakeford, David K. Sing, Kevin B. Stevenson, Natasha E. Batalha, Mercedes López-Morales, Munazza K. Alam, Joshua D. Lothringer, Guangwei Fu, James Kirk, Jeff A. Valenti, L. C. Mayorga, Kristin S. Sotzen
Figure caption: Red noise diagnostic plot (depicting the rms of the residuals as a function of bin size in time) for the residuals from the four FIREFLy visits (top panel) and each observing mode with residuals from visits concatenated (bottom panel). rms as a function of bin size is shown, with the dotted lines representing the expected decrease in noise with the square root of bin size (﹩\sqrt{N}﹩). Bin size is in seconds, not number of integrations, in order to appropriately compare G395H and G395M. There is no apparent difference in correlated noise between the G395H (Visits 1 and 2) and G395M (Visits 3 and 4) observations, nor is there an indication that an instrumental noise floor is being reached.
Paper: BSN. II. The First Light Curve Study of Eight Total Eclipsing Contact Binary Stars with Shallow Fillout Factors
Authors: Atila Poro, Kai Li, Raul Michel, Li-Heng Wang, Fahri Alicavus, Morgan Rhai Nájera, Priscila Santillán-Ortega, Francisco Javier Tamayo, Hector Aceves
Figure caption: The colored dots represent the observed light curves of the systems in different filters, and the synthetic light curves, generated using the light curve solutions, are also shown.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: BSN. II. The First Light Curve Study of Eight Total Eclipsing Contact Binary Stars with Shallow Fillout Factors
Authors: Atila Poro, Kai Li, Raul Michel, Li-Heng Wang, Fahri Alicavus, Morgan Rhai Nájera, Priscila Santillán-Ortega, Francisco Javier Tamayo, Hector Aceves
Figure caption: Position of both stars in six target system on the M–R and M–L diagrams.
Paper: BSN. II. The First Light Curve Study of Eight Total Eclipsing Contact Binary Stars with Shallow Fillout Factors
Authors: Atila Poro, Kai Li, Raul Michel, Li-Heng Wang, Fahri Alicavus, Morgan Rhai Nájera, Priscila Santillán-Ortega, Francisco Javier Tamayo, Hector Aceves
Figure caption: The O–C diagrams of the eight targets.
Paper: BSN. II. The First Light Curve Study of Eight Total Eclipsing Contact Binary Stars with Shallow Fillout Factors
Authors: Atila Poro, Kai Li, Raul Michel, Li-Heng Wang, Fahri Alicavus, Morgan Rhai Nájera, Priscila Santillán-Ortega, Francisco Javier Tamayo, Hector Aceves
Figure caption: Three-dimensional views of the stars in the target binary systems at orbital phases 0, 0.25, 0.5 and 0.75, respectively. The colors represent variations in surface temperature based on model simulations, with darker tones indicating cooler regions and lighter areas corresponding to higher temperatures.
Paper: BSN. II. The First Light Curve Study of Eight Total Eclipsing Contact Binary Stars with Shallow Fillout Factors
Authors: Atila Poro, Kai Li, Raul Michel, Li-Heng Wang, Fahri Alicavus, Morgan Rhai Nájera, Priscila Santillán-Ortega, Francisco Javier Tamayo, Hector Aceves
Figure caption: The sum of squared residuals as a function of mass ratio.
Paper: Formation Process of the Young Stellar Population in Messier 16 from a Kinematic Perspective
Authors: Beomdu Lim, Hyeong-Sik Yun, Hyun-Jeong Kim, Yuna Lee, Jae-Rim Koo, Jongsuk Hong, Heeyoung Oh
Figure caption: Spatial distribution of members and gas. The background images were taken from the Digitized Sky Survey available at MAST (STScI 2006). The positions of stars with good astrometric parameters (RUWE < 1.4 and duplicate flag = 0) are shown by red dots, while the blue dots represent stars with poor astrometric parameters. The size of dots is proportional to the brightness of individual stars. The cyan contours show the distribution of molecular gas traced by the 13CO J = 1–0 line. The contour levels are integrated intensities of 5, 10, 15, and 20 K km s−1. The coordinates of stars and gas are relative to R.A. = ﹩1{8}^{{\rm{h}}}\,1{8}^{{\rm{m}}}\,48\mathop{{\rm{.}}}\limits^{{\rm{s}}}00﹩, decl. ﹩=-13^\circ \,48^{\prime} \,24\mathop{.}\limits{^{\prime\prime} }0﹩ (J2000). The right panel displays the spatial distribution of members in the ﹩10^{\prime} \times 10^{\prime} ﹩ region around NGC 6611. The cross and the solid and dashed orange circles represent the center of NGC 6611, rh, and rcl, respectively.
Paper: Formation Process of the Young Stellar Population in Messier 16 from a Kinematic Perspective
Authors: Beomdu Lim, Hyeong-Sik Yun, Hyun-Jeong Kim, Yuna Lee, Jae-Rim Koo, Jongsuk Hong, Heeyoung Oh
Figure caption: IGRINS slit positions over one of the southern pillars. The grayscale images represent the NIRCam images obtained with the James Webb Space Telescope in F187N channel (M. J. Rieke et al. 2023). This image is made with publicly available data via the Mikulski Archive for Space Telescopes (MAST: DOI: 10.17909/r5ne-bs21). A total of 28 slits were used in our spectroscopic observations. The zoomed-in view shows the arrangement of the slits.