adsabs/AstroCLIMB huggingface dataset:
Paper: Quantifying Uncertainties on the Tip of the Red Giant Branch Method
Authors: Barry F. Madore, Wendy L. Freedman, Kayla A. Owens, In Sung Jang
Figure caption: Six subpanels illustrating the effect of increasing the photometric noise, (from 0.00 to ±0.20 mag) at fixed smoothing (±0.01 mag) and moderately large populations of RGB stars (11,000). The lower portions of each of the six subpanels show the first-derivative edge-detector output in both its uncorrected (thin black lines) and its noise-weighted (thicker black line) forms. See text for a detailed discussion of the trends.
Paper: Quantifying Uncertainties on the Tip of the Red Giant Branch Method
Authors: Barry F. Madore, Wendy L. Freedman, Kayla A. Owens, In Sung Jang
Figure caption: Six subpanels illustrating the effect of increasing the photometric noise, (from 0.00 to ±0.20 mag) at fixed smoothing (±0.01 mag) and impoverished populations of RGB stars (124). The lower portions of each of the six subpanels show the first-derivative edge-detector output in both its uncorrected (thin black lines) and its noise-weighted (thicker black line) forms. See text for a detailed discussion of the trends.
Paper: Quantifying Uncertainties on the Tip of the Red Giant Branch Method
Authors: Barry F. Madore, Wendy L. Freedman, Kayla A. Owens, In Sung Jang
Figure caption: Six subpanels illustrating the effect of increasing the photometric noise, (from 0.00 to ±0.20 mag) at fixed smoothing (±0.01 mag) and small populations of RGB stars (1200). The lower portions of each of the six subpanels show the first-derivative edge-detector output in both its uncorrected (thin black lines) and its noise-weighted (thicker black line) forms. See text for a detailed discussion of the trends.
Paper: Quantifying Uncertainties on the Tip of the Red Giant Branch Method
Authors: Barry F. Madore, Wendy L. Freedman, Kayla A. Owens, In Sung Jang
Figure caption: Nine subpanels illustrating a random sampling of TRGB measurements for the same number of RGB stars (1340) the same smoothing (0.10 mag) at the tip (±0.15 mag) as in subpanel (e) in Figure 11. These independently selected examples demonstrate the random drift of the peak response of the Sobel filter around the input value shown by the solid vertical black line at 0.0 mag. One peak ((b), (h), and (i)). Read left to right and top to bottom, the peak in subpanel (i) is noticeably displaced to a brighter magnitude; the example in subpanel (e) is displaced to fainter magnitudes. Other deflections are all within the 1σ expected deviations shown by the vertical dashed lines; five ((a), (b), (d), (g), and (h)) fall to the left, and two ((c) and (f)) fall to the right, although the latter is flanked by two peaks that are apparently more significant than the one found closest to the known answer. We note that more (low-level) structure in the output response is at magnitudes fainter than the true tip. Some of this structure is close enough (subpanels (d) and (i)) that, if excessive smoothing were applied, that action would preferentially draw the measured tip magnitudes systematically toward fainter magnitudes.
Paper: Quantifying Uncertainties on the Tip of the Red Giant Branch Method
Authors: Barry F. Madore, Wendy L. Freedman, Kayla A. Owens, In Sung Jang
Figure caption: Same as Figure 16 except this simulation involves slightly over 2,000,000 RGB stars in the frame. Crowding is now quite apparent in the inset CCD image, and has resulted in an appreciable population of crowded stars falling in number from the tip to 0.75 mag brighter where the self-crowding of two stars at the tip would appear as one unresolved source. See text for additional details.
Paper: Quantifying Uncertainties on the Tip of the Red Giant Branch Method
Authors: Barry F. Madore, Wendy L. Freedman, Kayla A. Owens, In Sung Jang
Figure caption: Binomial coefficient and their first derivatives. Each of the panels shows the values of the binomial coefficients, numerically in square brackets and graphically as vertical lines in the upper half of each plot. The smooth curve is a Gaussian. In the lower half of the panel is the first derivative of the binomial kernel, again given numerically inside of square brackets, and graphically as vertical black lines bounded by the smooth black line, which is the first derivative of the Gaussian.
Paper: Quantifying Uncertainties on the Tip of the Red Giant Branch Method
Authors: Barry F. Madore, Wendy L. Freedman, Kayla A. Owens, In Sung Jang
Figure caption: First derivatives of the binomial coefficients in Pascal’s triangle, as given in Figure 23 above. The first derivative of a Gaussian (DoG) is a well-known edge-detector in image processing. Each of the entries in this figure are then also edge-detectors, progressively more precise approximation to the DoG. Examples of their application to the detection of a step function are shown in Figure 23 (below).
Paper: Quantifying Uncertainties on the Tip of the Red Giant Branch Method
Authors: Barry F. Madore, Wendy L. Freedman, Kayla A. Owens, In Sung Jang
Figure caption: Examples of the Pascal edge-detector response to a step function. These are the results of applying the third, fifth, and seventh (centrally peaked) filters given in Figure 22 (above), shown as red, blue, and black lines, respectively. They are scaled to equal areas, demonstrating the relatively stable width of the response-functions, independent of the smoothing width of the chosen edge-detector.
Paper: Quantifying Uncertainties on the Tip of the Red Giant Branch Method
Authors: Barry F. Madore, Wendy L. Freedman, Kayla A. Owens, In Sung Jang
Figure caption: The binomial coefficients of Pascal’s triangle. Each line represents a digital kernel, each of which is a progressively higher-fidelity approximation to a Gaussian. Applied to digital data, these kernels act as weighted smoothing functions.
Paper: Quantifying Uncertainties on the Tip of the Red Giant Branch Method
Authors: Barry F. Madore, Wendy L. Freedman, Kayla A. Owens, In Sung Jang
Figure caption: Same as Figure 16 except this simulation involves slightly over 1,370,000 RGB stars in the frame. Crowding is now quite apparent in the inset CCD image, and has resulted in an appreciable population of crowded stars falling in number from the tip to 0.75 mag brighter where the self-crowding of two stars at the tip would appear as one unresolved source. For clarity, only one star in 10 is plotted. See text for additional details.
Paper: Quantifying Uncertainties on the Tip of the Red Giant Branch Method
Authors: Barry F. Madore, Wendy L. Freedman, Kayla A. Owens, In Sung Jang
Figure caption: Same as Figure 16 except this simulation involves slightly over 700,000 RGB stars in the frame. Crowding is now quite apparent in the inset CCD image, and has resulted in an appreciable population of crowded stars falling in number from the tip to 0.75 mag brighter where the self-crowding of two stars at the tip would appear as one unresolved source. See text for additional details.
Paper: Quantifying Uncertainties on the Tip of the Red Giant Branch Method
Authors: Barry F. Madore, Wendy L. Freedman, Kayla A. Owens, In Sung Jang
Figure caption: Toy model of a rising AGB luminosity function + an exponential RGB luminosity function, Gaussian smoothed (upper subpanes) and convolved with a Sobel edge-detection response filter (lower subpanels).
Paper: A Wide View of the Galactic Globular Cluster NGC 2808: Red Giant and Horizontal Branch Star Spatial Distributions
Authors: Christian I. Johnson, Annalisa Calamida, Justin A. Kader, Ivan Ferraro, Catherine A. Pilachowski, Giuseppe Bono, Alessandra Mastrobuono-Battisti, Armin Rest, Alfredo Zenteno, Alice Zocchi
Figure caption: Demonstration of the technique used to divide NGC 2808 RGB stars into individual populations using photometry from DECam (top) and HST (bottom). The left panels show the g band (or equivalent F438W for HST) vs. C  ugi  CMDs. The orange line is the median fiducial ridge line, and orange circles indicate the magnitude bin centers, which are separated by 0.1 mag. The 4th and 96th quantiles in C  ugi  as a function of apparent magnitude are indicated with the blue and red curves, respectively. The magnitude at which we measure the RGB width is shown as a green line, which is 1 mag brighter than the faintest RGB star analyzed, which is indicated by the green open circle. The rms spread in C  ugi  colors and the mean photometric error of stars along the RGB are shown as black and blue horizontal error bars to the left, respectively. The middle panels show the rectified RGBs, where the deviation from median RGB color is shown for each star as a function of magnitude. We collapse the rectified RGBs in the magnitude direction to reveal the individual sequences in ΔC  ugi , shown in the right panels. The best-fitting GMMs are overlaid on the ΔC  ugi  histograms: individual components are colored blue, green, and red, and the sum is the black curve. The Gaussian kernel density estimation of the distribution is shown as an magenta curve.
Paper: A Wide View of the Galactic Globular Cluster NGC 2808: Red Giant and Horizontal Branch Star Spatial Distributions
Authors: Christian I. Johnson, Annalisa Calamida, Justin A. Kader, Ivan Ferraro, Catherine A. Pilachowski, Giuseppe Bono, Alessandra Mastrobuono-Battisti, Armin Rest, Alfredo Zenteno, Alice Zocchi
Figure caption:  i vs. u − i, g − i, and r − i CMDs are shown for the full DECam FOV. The cluster RGB, at 12.0 mag ≲ i ≲ 16.0 mag and 1.4 mag ≲ g − i ≲ 2.5 mag, and blue HB, at 16.0 mag ≲ i ≲ 18.5 mag and g − i ≲ 0.5 mag, are clearly visible despite significant field star contamination. Error bars are shown.
Paper: A Wide View of the Galactic Globular Cluster NGC 2808: Red Giant and Horizontal Branch Star Spatial Distributions
Authors: Christian I. Johnson, Annalisa Calamida, Justin A. Kader, Ivan Ferraro, Catherine A. Pilachowski, Giuseppe Bono, Alessandra Mastrobuono-Battisti, Armin Rest, Alfredo Zenteno, Alice Zocchi
Figure caption: The left panel shows a source density map for all DECam data utilized in this project, with NGC 2808 at the center of the field. The middle and right panels show similar source density maps for the inner 40′ region around NGC 2808 that was used to separate nonmember (middle) and member (right) stars. The blue circle in each panel highlights the tidal radius of 21.′97 adopted from de Boer et al. (2019), and the red box illustrates the location of archival HST observations that were used to fill a coverage gap in the very crowded cluster core (r < 1.′5). Note that even though some stars observed near the cluster core with DECam were identified as nonmembers, most of these objects are inside the HST footprint for which we assumed 100% membership rates.
Paper: A Wide View of the Galactic Globular Cluster NGC 2808: Red Giant and Horizontal Branch Star Spatial Distributions
Authors: Christian I. Johnson, Annalisa Calamida, Justin A. Kader, Ivan Ferraro, Catherine A. Pilachowski, Giuseppe Bono, Alessandra Mastrobuono-Battisti, Armin Rest, Alfredo Zenteno, Alice Zocchi
Figure caption: The C  ugi,DECam CMD for NGC 2808 derived with DECam data is shown in the left panel, while a similar C  ugi,HST CMD derived with HST data is shown in the right panel. Both data sets support the existence of at least two to three distinct RGB subpopulations. Note that the DECam data only include stars outside 1.′5 from the cluster center, while the HST data trace stars inside ∼1.′5.
Paper: A Wide View of the Galactic Globular Cluster NGC 2808: Red Giant and Horizontal Branch Star Spatial Distributions
Authors: Christian I. Johnson, Annalisa Calamida, Justin A. Kader, Ivan Ferraro, Catherine A. Pilachowski, Giuseppe Bono, Alessandra Mastrobuono-Battisti, Armin Rest, Alfredo Zenteno, Alice Zocchi
Figure caption: Same CMDs as those shown in Figure 3, except only candidate cluster members are shown. The CMDs are compared against BASTI isochrones and ZAHB models for different abundances and the same age as labeled in the figure. A distance modulus of μ 0 = 15.05 and a reddening of E(B − V) = 0.18 mag were used. Error bars are shown. See text for more details.
Paper: A Wide View of the Galactic Globular Cluster NGC 2808: Red Giant and Horizontal Branch Star Spatial Distributions
Authors: Christian I. Johnson, Annalisa Calamida, Justin A. Kader, Ivan Ferraro, Catherine A. Pilachowski, Giuseppe Bono, Alessandra Mastrobuono-Battisti, Armin Rest, Alfredo Zenteno, Alice Zocchi
Figure caption: Reddening color density map as derived from Schlafly & Finkbeiner (2011) for stars toward the observed region across NGC 2808. Stars identified as cluster members from DECam photometric catalog are overplotted as red circles. The north and east directions are indicated with red arrows.
Paper: Quantifying Uncertainties on the Tip of the Red Giant Branch Method
Authors: Barry F. Madore, Wendy L. Freedman, Kayla A. Owens, In Sung Jang
Figure caption: Toy model of declining AGB luminosity + an exponential RGB luminosity function, Gaussian smoothed (upper subpanes) and convolved with a Sobel edge-detection response filter (lower subpanels).
Paper: Quantifying Uncertainties on the Tip of the Red Giant Branch Method
Authors: Barry F. Madore, Wendy L. Freedman, Kayla A. Owens, In Sung Jang
Figure caption: Toy model of a flat AGB luminosity function + an exponential RGB luminosity function, Gaussian smoothed (upper subpanes) and convolved with a Sobel edge-detection response filter (lower subpanels).
Paper: A Wide View of the Galactic Globular Cluster NGC 2808: Red Giant and Horizontal Branch Star Spatial Distributions
Authors: Christian I. Johnson, Annalisa Calamida, Justin A. Kader, Ivan Ferraro, Catherine A. Pilachowski, Giuseppe Bono, Alessandra Mastrobuono-Battisti, Armin Rest, Alfredo Zenteno, Alice Zocchi
Figure caption: [Na/Fe] vs. [O/Fe] abundance for RGB stars in common with the spectroscopic study of Carretta (2015) divided into our identified three subpopulation groups, P1 (Ns = 21; blue filled circles), P2 (Ns = 13; green diamonds), and P3 (Ns = 25; red squares). HB stars in common with the study of Gratton et al. (2011) are also overplotted and divided into RHBs (Ns = 32; magenta downward-pointing triangles) and EBT1 stars (Ns = 5; cyan leftward-pointing triangles).
Paper: V1507 CYGNI (HD187399): A Highly Evolved, Enigmatic Interacting Binary System with an Eccentric Orbit
Authors: T. J. Davidge
Figure caption: Phase-binned spectra of V1507 Cyg in two wavelength intervals. The centroids of the phase bins are listed along the right axis. The spectrum plotted in green is the median of the binned spectra after shifting them into the rest frame. The shapes of the Si II and He I lines change with orbital phase in a similar manner. The centers of the Si II, Fe II, and He I lines have a skewed appearance near phase 0.0, and in the text this behavior is attributed to tidal effects during periastron. The depression in the spectrum at wavelengths shortward of He I does not track the He I line in the spectrum of the brighter star, and in Section 4 it is argued that this trough is part of a P Cygni profile that originates in an envelope around the heavily obscured companion.
Paper: V1507 CYGNI (HD187399): A Highly Evolved, Enigmatic Interacting Binary System with an Eccentric Orbit
Authors: T. J. Davidge
Figure caption: (Left-hand panel:) Radial velocities. Velocities of the brighter star are shown as black crosses, while those obtained from the envelope spectra are shown as blue (He I) and red (Si II emission lines) crosses. (Right-hand panel:) Velocities from the left-hand panel phased using the ephemeris found by Hutchings & Redman (1973). The green squares are the means of the velocities for He I and metal lines listed in Table 1 of Merrill (1949) with phases computed from the Hutchings & Redman (1973) ephemeris. The velocities for the bright star measured from the DAO spectra agree with the Merrill measurements, indicating that the orbital properties of the system have then been stable to within ±10−3% over the time span of a century. That the amplitude of the radial-velocity curve of the bright star is larger than the range in radial velocities obtained from the envelope spectra indicates that the brighter star is less massive than the companion.
Paper: V1507 CYGNI (HD187399): A Highly Evolved, Enigmatic Interacting Binary System with an Eccentric Orbit
Authors: T. J. Davidge
Figure caption: Binned spectra with light from the brighter star removed. Orbital phases are listed below each spectrum. The central absorption in the Si II emission lines at some phases is due to an imperfect match with the Rigel spectrum. The overall strengths of the Si II emission lines vary with orbital phase. Absorption blueward of Si II emission at 6347 Å is seen at some phases, suggesting a P Cygni profile. Wavelengths near He I are shown in the right-hand panel. The broad He I feature changes character with orbital phase, and the movement with wavelength is consistent with motions in the direction expected for the companion star. Broad emission redward of the He I absorption component is also seen at most phases, except near periastron. The behavior of the emission lines suggests that the envelope around the companion is not symmetric.
Paper: V1507 CYGNI (HD187399): A Highly Evolved, Enigmatic Interacting Binary System with an Eccentric Orbit
Authors: T. J. Davidge
Figure caption: Extracting the spectrum of the brighter star. The template spectrum of the brighter star that was constructed by combining the V1507 Cyg spectra is shown at the top in green. Immediately below this is (1) the spectrum of the B8 I spectroscopic standard β Ori, (2) the β Ori spectrum scaled by a factor of 0.6, (3) the result of subtracting this scaled spectrum from the template spectrum (“Δ,”), and (4) the spectrum found by combining spectra that have had the β Ori spectrum subtracted individually and then aligning the results. The bottom spectrum contains broad Si II emission, while He I 6678 appears as a broad blueshifted line. There is also weak emission at the rest wavelength of the He I line, and a broad, shallow redshifted component.
Paper: V1507 CYGNI (HD187399): A Highly Evolved, Enigmatic Interacting Binary System with an Eccentric Orbit
Authors: T. J. Davidge
Figure caption: Spectrum of V1507 Cyg that was recorded on 2022 May 10. The Si II and He I lines originate mainly in the spectrum of the brighter star, while the Hα emission originates in circumstellar and intrasystem material. The weak emission lines are cosmic rays that were not suppressed during processing. The slight shift in wavelength between the expected and observed locations of the Si II and He I lines is due to the orbital motion of the brighter star.
Paper: Evidence That the Occurrence Rate of Hot Jupiters around Sun-like Stars Decreases with Stellar Age
Authors: Shota Miyazaki, Kento Masuda
Figure caption: Left: the panels show the marginalized posterior PDFs for [Fe/H], mass, and age (top to bottom). The solid lines and translucent regions represent the medians and 90% credible intervals (CIs) in each bin. Right: the inferred NPPS are functions of age for hot Jupiters and cold Jupiters, adopting the exponential model (left panel) and the sigmoid model (right panel). This is Equation (5) evaluated at the solar mass and metallicity. In each panel, solid lines present median values of the posterior predictions at ages and dark- and light-shaded regions show 68% and 90% credible intervals of the posterior predictions, respectively.
Paper: Evidence That the Occurrence Rate of Hot Jupiters around Sun-like Stars Decreases with Stellar Age
Authors: Shota Miyazaki, Kento Masuda
Figure caption: The NPPS function ﹩{\bar{n}}_{p}({\boldsymbol{z}})﹩ inferred for the Sun-like sample using the histogram model in Section 4.1. Left: the posterior PDFs of the NPPS for HJs (orange) and for CJs (blue). These are the numbers of planets per star in the searched sample, computed taking into account the stellar parameter dependence of the occurrence rate as well as the distribution of the stellar parameters in the sample; see Equation (6). Right: the posterior PDFs for the NPPS of HJs (top) and CJs (bottom) as functions of [Fe/H], mass, and age are shown as violin plots, whose widths represent the probability densities. The error bars represent their peaks (modes) and 68% highest density intervals (HDIs). This is essentially the NPPS as a function of  z  as given in Equation (5), but it has been marginalized for the stellar parameters that are not shown in the horizontal axis as in Equation (6); (see also the main text and Equation (23)).
Paper: Evidence That the Occurrence Rate of Hot Jupiters around Sun-like Stars Decreases with Stellar Age
Authors: Shota Miyazaki, Kento Masuda
Figure caption: The stellar parameter distribution p ⋆( z ) inferred for the Sun-like sample using the histogram model in Section 4.1. Left: the 3D view of the posterior in the parameter space of ([Fe/H], M ⋆, t ⋆), where the circles represent the mean values of p ⋆( z ) at the center of each grid. Right: the panels show the marginalized posterior PDFs for [Fe/H], mass, and age (top to bottom). The solid lines and translucent regions represent the medians and 90% equal-tail credible intervals (CIs) in each bin.
Paper: Evidence That the Occurrence Rate of Hot Jupiters around Sun-like Stars Decreases with Stellar Age
Authors: Shota Miyazaki, Kento Masuda
Figure caption: The posterior PDFs for the NPPS as a function of age derived using the histogram model in Section 4.1. Unlike in the right panels of Figure 7, here we show the NPPS evaluated at given stellar masses shown at the top of each column, after marginalizing over the metallicity distribution.
Paper: Evidence That the Occurrence Rate of Hot Jupiters around Sun-like Stars Decreases with Stellar Age
Authors: Shota Miyazaki, Kento Masuda
Figure caption: Corner plots for the posterior distributions of the parameters in the exponential NPPS model. The left panel is for HJs and the right panel is for CJs. The figure was created using corner.py (Foreman-Mackey 2016).
Paper: Evidence That the Occurrence Rate of Hot Jupiters around Sun-like Stars Decreases with Stellar Age
Authors: Shota Miyazaki, Kento Masuda
Figure caption: Cumulative distribution functions of the ages for the HJ hosts (red), CJ hosts (blue), and all the stars (gray) in the Sun-like sample, respectively. Here, the “age” for each star is evaluated as the median of the marginalized posterior distribution.
Paper: Evidence That the Occurrence Rate of Hot Jupiters around Sun-like Stars Decreases with Stellar Age
Authors: Shota Miyazaki, Kento Masuda
Figure caption: Same as Figure 10 but for the sigmoid model.