adsabs/AstroCLIMB huggingface dataset:
Paper: The POKEMON Speckle Survey of Nearby M Dwarfs. III. The Stellar Multiplicity Rate of M Dwarfs within 15 pc
Authors: Catherine A. Clark, Gerard T. van Belle, Elliott P. Horch, David R. Ciardi, Kaspar von Braun, Brian A. Skiff, Jennifer G. Winters, Michael B. Lund, Mark E. Everett, Zachary D. Hartman, Joe Llama
Figure caption: Projected separation distributions for various populations of M-dwarf multiples. The histogram shows the distribution of projected separations for the targets in the 15 pc POKEMON sample that are known to be multiple, separated by planet-hosting (orange) and non–planet-hosting (white) status. The dotted, black line is a Gaussian fit to the projected separations of the non–planet-hosting POKEMON multiples, with a peak at 5.57 au (﹩{\sigma }_{\mathrm{log}a}=1.3﹩, ﹩{\mathrm{SE}}_{\mathrm{log}a}=0.11﹩). The dashed, orange line is a Gaussian fit to the projected separations of the planet-hosting POKEMON multiples, with a peak at 198 au (﹩{\sigma }_{\mathrm{log}a}=0.77﹩, ﹩{\mathrm{SE}}_{\mathrm{log}a}=0.32﹩). The solid, yellow line is a Gaussian fit to the projected separations of the M-dwarf TOIs from Clark et al. (2022a), with a peak at 735 au (﹩{\sigma }_{\mathrm{log}a}=0.83﹩, ﹩{\mathrm{SE}}_{\mathrm{log}a}=0.25﹩). We note that we use Gaussian fits to compare our distribution of projected separations with other studies of multiplicity (e.g., Raghavan et al. 2010; Winters et al. 2019a); we do not use this to indicate that the distribution of stellar multiples is Gaussian, but rather to show that the peaks of the distributions are shifted. The two planet-hosting distributions have peaks at relatively consistent values, whereas the peaks of the planet-hosting and non–planet-hosting distributions differ by more than an order of magnitude. This result indicates that the presence of a stellar companion impacts the formation and long-term stability of any planets in the system.
Paper: The POKEMON Speckle Survey of Nearby M Dwarfs. III. The Stellar Multiplicity Rate of M Dwarfs within 15 pc
Authors: Catherine A. Clark, Gerard T. van Belle, Elliott P. Horch, David R. Ciardi, Kaspar von Braun, Brian A. Skiff, Jennifer G. Winters, Michael B. Lund, Mark E. Everett, Zachary D. Hartman, Joe Llama
Figure caption: Cumulative stellar multiplicity rate as a function of distance, binned by 1 pc. The 95% Poisson confidence interval is shown. We also show the overall stellar multiplicity rate (and uncertainties) for comparison. No corrections have been applied for undetected companions. Although the cumulative multiplicity rate is higher at smaller distances due to a smaller number of stars in those bins, we do find that the cumulative multiplicity rate stays roughly flat from 11 pc outwards; the drop-off from 11 to 15 pc is 0.6%, which we consider negligible. Since the cumulative multiplicity rate remains roughly flat in these bins, this indicates that we are not missing multiples at these distances.
Paper: The POKEMON Speckle Survey of Nearby M Dwarfs. III. The Stellar Multiplicity Rate of M Dwarfs within 15 pc
Authors: Catherine A. Clark, Gerard T. van Belle, Elliott P. Horch, David R. Ciardi, Kaspar von Braun, Brian A. Skiff, Jennifer G. Winters, Michael B. Lund, Mark E. Everett, Zachary D. Hartman, Joe Llama
Figure caption: Percentage of stellar companions detectable within our speckle images vs. distance. Circles color coded by G magnitude represent the detectability of simulated companions at all separations. Open black circles represent the detectability of simulated companions specifically within 100 au. We find that the majority of potential stellar companions would be detectable, particularly for the nearby targets, with a median value of 78.1%. Specifically within 100 au, we find that 75.5% of simulated companions are recovered.
Paper: The POKEMON Speckle Survey of Nearby M Dwarfs. III. The Stellar Multiplicity Rate of M Dwarfs within 15 pc
Authors: Catherine A. Clark, Gerard T. van Belle, Elliott P. Horch, David R. Ciardi, Kaspar von Braun, Brian A. Skiff, Jennifer G. Winters, Michael B. Lund, Mark E. Everett, Zachary D. Hartman, Joe Llama
Figure caption: Distance (left) and absolute G RP magnitude (right) distributions for the 455 targets in the 15 pc POKEMON sample. We use the mass–magnitude relation from Giovinazzi & Blake (2022) to estimate the masses of these targets.
Paper: The POKEMON Speckle Survey of Nearby M Dwarfs. III. The Stellar Multiplicity Rate of M Dwarfs within 15 pc
Authors: Catherine A. Clark, Gerard T. van Belle, Elliott P. Horch, David R. Ciardi, Kaspar von Braun, Brian A. Skiff, Jennifer G. Winters, Michael B. Lund, Mark E. Everett, Zachary D. Hartman, Joe Llama
Figure caption: The sky locations of the 455 targets in the volume-limited, 15 pc POKEMON sample. Targets with no known companions are marked with open black circles, while targets with known companions are marked with larger, orange stars.
Paper: The 50 Mpc Galaxy Catalog (50 MGC): Consistent and Homogeneous Masses, Distances, Colors, and Morphologies
Authors: David Ohlson, Anil C. Seth, Elena Gallo, Vivienne F. Baldassare, Jenny E. Greene
Figure caption: An example of how we transform the Taylor et al. (2011) (g − i)0–M/L  i  relation into (g − r)0–M/L  r . The y-axis is determined by taking masses calculated from the NSA data using the (g − i)0–M/L  i  relation, and then dividing by the NSA L  r  values. This is then plotted against NSA (g − r)0 values and fit using a robust outlier-rejection algorithm, RANSAC. Also shown is the somewhat steeper relation from Zibetti et al. (2009). Our translation of the Taylor et al. (2011) relation into other colors ensures consistency between masses calculated in different bands. We note that although this (g − r)0–M/L  r  relation is used for galaxies with SGA data, we fit this relation with NSA photometry alone to ensure a large sample of galaxies and to minimize photometric outliers. A similar process was used to also create the other color–M/L relations given in Section 4.
Paper: The 50 Mpc Galaxy Catalog (50 MGC): Consistent and Homogeneous Masses, Distances, Colors, and Morphologies
Authors: David Ohlson, Anil C. Seth, Elena Gallo, Vivienne F. Baldassare, Jenny E. Greene
Figure caption: Completeness of our catalog as a function of stellar mass. Top–Mass completeness of our catalog, using 0.2 dex bins. The Y-axes show the radius of the effective volume, left, and the completeness fraction, right. The black line compares all catalog galaxies against a <50 Mpc mock sample created using the Driver et al. (2022) galaxy stellar mass function. The colored lines show comparisons between color_type separated catalog galaxies against the color-separated mock sample created using the Baldry et al. (2012) galaxy stellar mass functions. Bottom–Percent of galaxies classified as red by our catalog and the Baldry et al. (2012) sample in each bin.
Paper: The 50 Mpc Galaxy Catalog (50 MGC): Consistent and Homogeneous Masses, Distances, Colors, and Morphologies
Authors: David Ohlson, Anil C. Seth, Elena Gallo, Vivienne F. Baldassare, Jenny E. Greene
Figure caption: Position offsets and their potential effects on active fraction as a function of galaxy mass and type. Left–Comparison between the X-ray active fractions calculated using different separation radii to crossmatch with Chandra observations. The solid line shows the active fraction using a matching radius of 1″, the dashed lines use a radius of 2 ″, and the dotted lines use a radius of 3″. The red and blue lines show early- and late-type galaxies, respectively. Right–Fraction of catalog galaxies with large position offsets between our catalog and NED as a function of mass and type. The solid line shows the fraction with an offset >1″, the dashed lines show the fraction with an offset >2″, and the dotted lines show the fraction with an offset >3″. Large offsets are seen much more commonly in late-type galaxies than in early-type galaxies, especially at lower masses.
Paper: The 50 Mpc Galaxy Catalog (50 MGC): Consistent and Homogeneous Masses, Distances, Colors, and Morphologies
Authors: David Ohlson, Anil C. Seth, Elena Gallo, Vivienne F. Baldassare, Jenny E. Greene
Figure caption: Comparison of our mass estimates (logmass_best) against those from S4G (blue; Sheth et al. 2010; Eskew et al. 2012) and ATLAS3D dynamical stellar mass estimates (red; Cappellari et al. 2011). The S4G masses are corrected for a Salpeter to Chabrier IMF by subtracting 0.24 dex for a consistent comparison to our catalog. The solid line shows the one-to-one relation, and the dashed lines indicate an 0.5 dex offset.
Paper: The 50 Mpc Galaxy Catalog (50 MGC): Consistent and Homogeneous Masses, Distances, Colors, and Morphologies
Authors: David Ohlson, Anil C. Seth, Elena Gallo, Vivienne F. Baldassare, Jenny E. Greene
Figure caption: Examples of SDSS imaging of NSA contaminant objects that are removed from our catalog. (a) Imaging shows a bright, star-forming region of a galaxy (NSAID: 177945). (b) A foreground star centered on a distant galaxy that causes incorrect redshift values for the galaxy (NSAID: 401970). (c) An imaging artifact treated as a galaxy by NSA (NSAID: 460798). (d) An artifact from a bright star in the top left corner surrounds a nearby star in the center, which causes both the classification as a galaxy and provides the redshift of the star (NSAID: 460798).
Paper: The 50 Mpc Galaxy Catalog (50 MGC): Consistent and Homogeneous Masses, Distances, Colors, and Morphologies
Authors: David Ohlson, Anil C. Seth, Elena Gallo, Vivienne F. Baldassare, Jenny E. Greene
Figure caption: Difference between HyperLeda galaxies with overlapping total ((B − V) t,0) and effective ((B − V) e,0) colors vs. their (B − V) e,0 value. The red line shows the linear correction applied to (B − V) e,0 values to correct for the slight color-dependent offset to allow a combination of colors into a single field. Correction coefficients are based on a linear fit from 0.2 ≤ (B − V) e,0 ≤ 1.0.
Paper: The 50 Mpc Galaxy Catalog (50 MGC): Consistent and Homogeneous Masses, Distances, Colors, and Morphologies
Authors: David Ohlson, Anil C. Seth, Elena Gallo, Vivienne F. Baldassare, Jenny E. Greene
Figure caption: The distribution of the B-band luminosities ﹩\mathrm{log}({L}_{B})﹩ for the entire catalog (shaded histogram), along with the subset that has available masses (dark gray line). The colored lines indicate the source of photometry used in estimating the galaxy masses (see Section 4.)
Paper: The 50 Mpc Galaxy Catalog (50 MGC): Consistent and Homogeneous Masses, Distances, Colors, and Morphologies
Authors: David Ohlson, Anil C. Seth, Elena Gallo, Vivienne F. Baldassare, Jenny E. Greene
Figure caption: Distribution of log(M ⋆/M ⊙) estimates for the entire catalog (shaded histogram). The colored lines indicate which colors are used to estimate the stellar mass using color-mass-to-light ratio relations and precedence as described in Section 4.
Paper: The 50 Mpc Galaxy Catalog (50 MGC): Consistent and Homogeneous Masses, Distances, Colors, and Morphologies
Authors: David Ohlson, Anil C. Seth, Elena Gallo, Vivienne F. Baldassare, Jenny E. Greene
Figure caption: Distribution of our chosen best distances for the entire catalog (shaded histogram). The colored lines indicate the source (bestdist_source) used for the final distance compilation (see Section 3).
Paper: The 50 Mpc Galaxy Catalog (50 MGC): Consistent and Homogeneous Masses, Distances, Colors, and Morphologies
Authors: David Ohlson, Anil C. Seth, Elena Gallo, Vivienne F. Baldassare, Jenny E. Greene
Figure caption: X-ray active fraction of catalog galaxies as a function of galaxy mass and type, using a 1″ matching radius. Top row—The log(M ⋆/M ⊙) distribution of catalog galaxies with Chandra data. The solid line shows galaxies with Chandra observations, and the filled histogram shows galaxies with Chandra detections with log(L X)> 38.3 for (a) early types and (b) late types. Panel (c)–X-ray detection fraction as a function of log(M ⋆/M ⊙) and separated by best_type, a combination of morphological and color-based types (see Section 5). Panel (d)–X-ray detection fraction as a function of log(M ⋆/M ⊙) and separated using color_type. The shaded areas in the bottom panels show Agresti-Coull binomial confidence intervals.
Paper: The 50 Mpc Galaxy Catalog (50 MGC): Consistent and Homogeneous Masses, Distances, Colors, and Morphologies
Authors: David Ohlson, Anil C. Seth, Elena Gallo, Vivienne F. Baldassare, Jenny E. Greene
Figure caption: Images of catalog galaxies with Chandra sources within 1″ of their centers that have log(L X) > 38.3 and have available SDSS imaging. The white circle is centered on the catalog’s galaxy coordinates and shows the 1″ radius used to match to Chandra detections, while the red dot marks the Chandra source position. Each image has a width of 20″. The galaxies are arranged in order of increasing log(M ⋆/M ⊙). The top three rows show the 18 galaxies with the lowest log(M ⋆/M ⊙) and represent 18/22 lowest-mass galaxies with X-ray sources. The bottom four rows show galaxies at higher masses sampled evenly in log(M ⋆/M ⊙). The image labels provide the catalog objname, logmass, and best_type (red are early types, and blue are late types).
Paper: The 50 Mpc Galaxy Catalog (50 MGC): Consistent and Homogeneous Masses, Distances, Colors, and Morphologies
Authors: David Ohlson, Anil C. Seth, Elena Gallo, Vivienne F. Baldassare, Jenny E. Greene
Figure caption: Mass distribution of galaxies as a function of their morphology. Left–Distribution of log(M ⋆/M ⊙) for the full catalog (shaded histogram), using best_type as described in Section 5.1 to separate into early (red) and late types (blue). Right–Comparison of numerical T-Type vs. log(M ⋆/M ⊙) for all catalog galaxies with an available t_type. The color gradient is included for visual representation of the galaxy type and coincides with the T-Type value.
Paper: The 50 Mpc Galaxy Catalog (50 MGC): Consistent and Homogeneous Masses, Distances, Colors, and Morphologies
Authors: David Ohlson, Anil C. Seth, Elena Gallo, Vivienne F. Baldassare, Jenny E. Greene
Figure caption: Morphological classifications of our galaxies in the color–mass plane. Left–A color–mass diagram of 6677 galaxies with g–i data from NSA and morphologies from HyperLeda and LVG. Right–The same color–mass distribution (early-type galaxies in red contours, and late-type galaxies in blue), with the black line showing our linear fit to most cleanly separate early- and late-type galaxies. This fit is extrapolated to higher and lower masses (gray line). The dotted line and the shaded blue regions show where we reclassify blue early-type galaxies as late-type galaxies based on visual inspection of these galaxies (see Section 5).
Paper: Kepler-discovered Multiple-planet Systems near Period Ratios Suggestive of Mean-motion Resonances Are Young
Authors: Jacob H. Hamer, Kevin C. Schlaufman
Figure caption: Indirect age indicators for our sample of Kepler multiple-planet system host stars. We plot as blue points systems with at least one plausibly resonant planet pair and as orange points systems that lack a plausibly resonant planet pair. Top left: from Berger et al. (2018), the equivalent width in mÅ of the 670.8 nm lithium feature as a function of G BP − G RP. Top right: from Berger et al. (2018), lithium abundance as a function of G BP − G RP. At constant G BP − G RP, large equivalent widths or lithium abundances should be observed in the spectra of stars younger than about 650 Myr. We see no significant equivalent width or abundance offsets between plausibly resonant/implausibly resonant systems, suggesting that these plausibly resonant systems are not young in an absolute sense. Bottom left: from Brewer & Fischer (2018), ﹩\mathrm{log}{R}_{\mathrm{HK}}^{{\prime} }﹩ as a function of G BP − G RP. Bottom right: from Brewer & Fischer (2018), S HK as a function of G BP − G RP. ﹩\mathrm{log}{R}_{\mathrm{HK}}^{{\prime} }﹩ and S HK are measures of the strength of emission in the core of the calcium H and K lines. At constant G BP − G RP, stronger emission should be observed in the spectra of younger stars. We see no significant ﹩\mathrm{log}{R}_{\mathrm{HK}}^{{\prime} }﹩ or S HK offsets between plausibly resonant/implausibly resonant systems, suggesting that these plausibly resonant systems are not young in an absolute sense.
Paper: Kepler-discovered Multiple-planet Systems near Period Ratios Suggestive of Mean-motion Resonances Are Young
Authors: Jacob H. Hamer, Kevin C. Schlaufman
Figure caption: Distributions of Galactic velocity dispersion based on bootstrap resampling for systems with (blue) or without (orange) a plausibly second-order resonant planet pair according to the ﹩{\delta }_{\mathrm{res}}﹩-based definition. We indicate median values as solid vertical lines, 1σ ranges between vertical dashed lines, and 2σ ranges between vertical dotted–dashed lines. The top panels include systems in which the innermost planet is likely affected by tidal evolution, while the bottom panels include systems in which the innermost planet is unlikely to be affected by tidal dissipation. Left: tidal and nontidal samples separated at τ  e  = 20 Myr. The probability that offsets this large could occur by chance is about 1 in 210 (equivalent to about 2.6σ) for the systems likely to be affected by tides and about 1 in 76,000 (equivalent to about 4.2σ) for systems unlikely to be affected by tides. Right: tidal and nontidal samples separated by the median circularization time τ  e  = 400 Myr. The probability that offsets this large could occur by chance is about 1 in 280 (equivalent to about 2.7σ) for the systems likely to be affected by tides and about 1 in 76,000 (equivalent to about 4.2σ) for systems unlikely to be affected by tides. Regardless of the importance of tidal dissipation inside the innermost planets, the Galactic velocity dispersion of the sample of Kepler-discovered multiple small planet systems with a plausibly second-order resonant planet pair is colder than the Galactic velocity dispersion of systems that lack such a pair. The implication is that tidal dissipation is not the process responsible for moving systems initially in second-order mean-motion resonance out of resonance.
Paper: Kepler-discovered Multiple-planet Systems near Period Ratios Suggestive of Mean-motion Resonances Are Young
Authors: Jacob H. Hamer, Kevin C. Schlaufman
Figure caption: Distributions of Galactic velocity dispersions for the indicated populations. We indicate median values as solid vertical lines, 1σ ranges between vertical dashed lines, and 2σ ranges between vertical dotted–dashed lines. First panel: the populations of plausibly first-order (blue) and second-order (orange) resonant multiple-planet systems. Second panel: the population of implausibly resonant multiple-planet systems. Third panel: the population of all multiple-planet systems. Fourth panel: the populations of confirmed (orange) and candidate (blue) single-transiting systems. The plausibly second-order resonant system population has a significantly colder Galactic velocity dispersion than the single-transiting system population. The population of single-transiting systems has a Galactic velocity dispersion consistent with the populations of implausibly resonant multiple-planet systems and all multiple-planet systems.
Paper: Kepler-discovered Multiple-planet Systems near Period Ratios Suggestive of Mean-motion Resonances Are Young
Authors: Jacob H. Hamer, Kevin C. Schlaufman
Figure caption: Distribution of Galactic velocity dispersion based on bootstrap resampling for systems with (blue) or without (orange) a plausibly second-order resonant planet pair according to the ﹩{\delta }_{\mathrm{res}}﹩-based definition. We indicate median values as solid vertical lines, 1σ ranges between vertical dashed lines, and 2σ ranges between vertical dotted–dashed lines. The Galactic velocity dispersion of the sample of Kepler-discovered multiple small planet systems with a plausibly second-order resonant planet pair is significantly colder than the Galactic velocity dispersion of systems that lack such a pair. The probability that an offset this large could occur by chance is less than 1 in 100,000 or, equivalently, about 4.6σ. This observation implies that systems initially in second-order resonance are driven out of resonance over Gyr timescales.
Paper: HybPSF: Hybrid Point-spread Function Reconstruction for the Observed JWST NIRCam Image
Authors: Lin Nie, Huanyuan Shan, Guoliang Li, Lei Wang, Cheng Cheng, Charling Tao, Qifan Cui, Yushan Xie, Dezi Liu, Zekang Zhang
Figure caption: Distribution of the shape parameter residuals (δ R 2/R 2, δ e 1 and δ e 2) for the JWST NIRCam imaging data of short-wavelength channels used in this work. The blue and red histogram represent the results obtained from WebbPSF and HybPSF, respectively. Lighter color histograms represent the results from all samples.
Paper: HybPSF: Hybrid Point-spread Function Reconstruction for the Observed JWST NIRCam Image
Authors: Lin Nie, Huanyuan Shan, Guoliang Li, Lei Wang, Cheng Cheng, Charling Tao, Qifan Cui, Yushan Xie, Dezi Liu, Zekang Zhang
Figure caption: Examples of our selected star stamps. The upper panels represent the star image candidates without masking the neighboring sources, and the lower panels shows the corresponding images after masking.
Paper: HybPSF: Hybrid Point-spread Function Reconstruction for the Observed JWST NIRCam Image
Authors: Lin Nie, Huanyuan Shan, Guoliang Li, Lei Wang, Cheng Cheng, Charling Tao, Qifan Cui, Yushan Xie, Dezi Liu, Zekang Zhang
Figure caption: The distribution “FWHM” as a function of “magnitude” for all objects detected from “jw02736001001_02105_00009_nrcblong_cal. fits” by SExtractor. The “AB [Magnitude]” is estimated from: FLUX_AUTO measuring from SExtractor, and “FWHM [pixel]” corresponds to the value of “FWHM_IMAGE” from SExtractor. The blue stars at the bottom of image represent the PSF stars.
Paper: HybPSF: Hybrid Point-spread Function Reconstruction for the Observed JWST NIRCam Image
Authors: Lin Nie, Huanyuan Shan, Guoliang Li, Lei Wang, Cheng Cheng, Charling Tao, Qifan Cui, Yushan Xie, Dezi Liu, Zekang Zhang
Figure caption: Residual image samples of the star images after subtracting the WebbPSF PSF images.
Paper: HybPSF: Hybrid Point-spread Function Reconstruction for the Observed JWST NIRCam Image
Authors: Lin Nie, Huanyuan Shan, Guoliang Li, Lei Wang, Cheng Cheng, Charling Tao, Qifan Cui, Yushan Xie, Dezi Liu, Zekang Zhang
Figure caption: Statistical results of the shape parameter residuals (δ R 2/R 2, δ e 1 and δ e 2) for the channel “F200W” from EMPCA method.
Paper: HybPSF: Hybrid Point-spread Function Reconstruction for the Observed JWST NIRCam Image
Authors: Lin Nie, Huanyuan Shan, Guoliang Li, Lei Wang, Cheng Cheng, Charling Tao, Qifan Cui, Yushan Xie, Dezi Liu, Zekang Zhang
Figure caption: Ellipticity comparison between the data and the modeled PSFs in channel F277W. The whiskers mimic the ellipticity of the PSFs. The left, middle, and right panels correspond to the ellipticity of star image, model, and residual subtracting the model from data, respectively.
Paper: HybPSF: Hybrid Point-spread Function Reconstruction for the Observed JWST NIRCam Image
Authors: Lin Nie, Huanyuan Shan, Guoliang Li, Lei Wang, Cheng Cheng, Charling Tao, Qifan Cui, Yushan Xie, Dezi Liu, Zekang Zhang
Figure caption: Residual image samples of the star images after subtracting the HybPSF model images.
Paper: Variability in Protoplanetary Nebulae. X. Multiyear Periods as an Indicator of Potential Binaries
Authors: Bruce J. Hrivnak, Wenxian Lu, Gary Henson, Todd C. Hillwig
Figure caption: IRAS 20056+1834: (top) Phased V light curve, with the long-period variation removed. (bottom) Phased (V − R  C ) color curve, using the same epoch and period (102.9 days). The (V − R  C ) data were first seasonally normalized to remove a slight reddening trend in the more recent data.