adsabs/AstroCLIMB huggingface dataset:
Paper: Accurate Modeling of Grazing Transits Using Umbrella Sampling
Authors: Gregory J. Gilbert
Figure caption: Distribution of the grazing coordinate, γ, for posterior MCMC samples obtained under the transition umbrella, ψT, for three simulated transits of a warm Jupiter orbiting a Sun-like star at various impact parameters. Simulated parameter values are collected in Table 1, and corresponding simulated light curves are shown in Figure 5. Unsurprisingly, the fraction of posterior samples consistent with a nongrazing geometry is highest for the simulated nongrazing transit (top), and vice versa for a grazing geometry (bottom). The near-grazing transit (middle) reflects an intermediate state. In all three cases, at least some fraction of the posteriors is consistent with both a grazing and a nongrazing trajectory, indicating the transit geometry is ambiguous and the application of umbrella sampling is warranted.
Paper: Accurate Modeling of Grazing Transits Using Umbrella Sampling
Authors: Gregory J. Gilbert
Figure caption: Posterior distributions of r, b, and T for a simulated near-grazing transit of a Jupiter-sized planet on a 13 day orbit around a Sun-like star (simulation J-85). See Table 1 for simulated model parameters and Figure 5 for the simulated photometry. Each thin line represents a 2000 sample chain from a single independent Monte Carlo run, while the thick lines give the combined results of 20 such runs. Vertical dashed lines represent ground-truth parameter values. Both methods produce posterior distributions consistent with the true value, but only umbrella sampling is able to fully explore the high-b, high-r tail of the distribution.
Paper: Accurate Modeling of Grazing Transits Using Umbrella Sampling
Authors: Gregory J. Gilbert
Figure caption: Posterior distributions of r, b, and T for a simulated nongrazing transit of a Jupiter-sized planet on a 3.6 day orbit around a Sun-like star (simulation J-22). See Table 1 for simulated model parameters and Figure 5 for the simulated photometry. Each thin line represents a 2000 sample chain from a single independent Monte Carlo run, while the thick lines give the combined results of 100 such runs. Vertical dashed lines represent ground-truth parameter values. Both methods produce comparable results; however, only umbrella sampling is able to smoothly explore deep into the grazing regime. This augmented exploration allows us to confidently rule out a grazing geometry by placing reliable upper limits on r and b.
Paper: Accurate Modeling of Grazing Transits Using Umbrella Sampling
Authors: Gregory J. Gilbert
Figure caption: Posterior distributions of r, b, and T for a simulated grazing transit of a Jupiter-sized planet on a 45 day orbit around a Sun-like star (simulation J-100). See Table 1 for simulated model parameters and Figure 5 for the simulated photometry. Each thin line represents a 2000 sample chain from a single independent Monte Carlo run, while the thick lines give the combined results of 100 such runs. Vertical dashed lines represent ground-truth parameter values. In this case, both methods produce comparable results.
Paper: Accurate Modeling of Grazing Transits Using Umbrella Sampling
Authors: Gregory J. Gilbert
Figure caption: Top panel: simulated photometry for a mini-Neptune (model MN) orbiting a K-dwarf star on a barely grazing orbit. Bottom panel: simulated photometry for a super-Earth (model SE) orbiting the same star on a nongrazing orbit. Ground-truth simulation parameters are collected in Table 1. See Section 5.2 for discussion.
Paper: Accurate Modeling of Grazing Transits Using Umbrella Sampling
Authors: Gregory J. Gilbert
Figure caption: Posterior distributions of r, b, and T for a simulated nongrazing transit of a super-Earth orbiting a K-dwarf star (simulation SE). See Table 1 for simulated model parameters and Figure 15 for the simulated photometry. Each thin line represents a 2000 sample chain from a single independent Monte Carlo run, while the thick lines give the combined results of 20 such runs. Vertical dashed lines represent ground-truth parameter values. The transit trajectory is far from grazing (b = 0.7, r = 0.012), and the two methods produce comparable results, as expected.
Paper: Accurate Modeling of Grazing Transits Using Umbrella Sampling
Authors: Gregory J. Gilbert
Figure caption: Posterior distributions of r, b, and T for a simulated barely grazing transit of a mini-Neptune orbiting a K-dwarf star (simulation MN). See Table 1 for simulated model parameters and Figure 15 for the simulated photometry. Each thin line represents a 2000 sample chain from a single independent Monte Carlo run, while the thick lines give the combined results of 20 such runs. Vertical dashed lines represent ground-truth parameter values. In this case, umbrella sampling produces obviously improved results, as direct sampling struggles to smoothly explore the grazing regime.
Paper: Accurate Modeling of Grazing Transits Using Umbrella Sampling
Authors: Gregory J. Gilbert
Figure caption: Simulated photometry for a Mercury-radius planet orbiting in the habitable zone of an M-dwarf host star (model MHZ). Ground-truth simulation parameters are collected in Table 1. See Section 5.3 for discussion.
Paper: Accurate Modeling of Grazing Transits Using Umbrella Sampling
Authors: Gregory J. Gilbert
Figure caption: Posterior distributions of r, b, and T for a simulated barely grazing transit of a Mercury-sized planet orbiting in the habitable zone of an M-dwarf star (simulation MHZ). See Table 1 for simulated model parameters and Figure 18 for the simulated photometry. Each thin line represents a 2000 sample chain from a single independent Monte Carlo run, while the thick lines give the combined results of 100 such runs. Vertical dashed lines represent ground-truth parameter values. For this test case, both direct sampling and umbrella sampling perform equally well.
Paper: Accurate Modeling of Grazing Transits Using Umbrella Sampling
Authors: Gregory J. Gilbert
Figure caption: Phase-folded transits of KOI-2068 with a posterior model from umbrella sampling are overplotted in red. The pink shaded region shows the 1σ credible interval. The V-shape of the transit is apparent, which is suggestive of a grazing transit. The posterior corner plot for r and b is shown on the right.
Paper: Accurate Modeling of Grazing Transits Using Umbrella Sampling
Authors: Gregory J. Gilbert
Figure caption: Posterior transit models for the two candidate planets orbiting K01-2050. Shaded regions (just barely visible on the plots) show 1σ credible intervals.
Paper: Accurate Modeling of Grazing Transits Using Umbrella Sampling
Authors: Gregory J. Gilbert
Figure caption: Posterior transit model for K01-1426.03. The 1σ credible interval is so narrow that it is not even visible on the plot.
Paper: Accurate Modeling of Grazing Transits Using Umbrella Sampling
Authors: Gregory J. Gilbert
Figure caption: Samples of γ obtained under the transition umbrella, ψT, for the three planets in the KOI-1426 system. Neither of the two confirmed objects (top two panels, blue) have any posterior samples γ < 1, indicating that both planets are almost certainly on nongrazing trajectories. For these two objects, we can comfortably ignore the grazing umbrella, ψG, and perform a two-window analysis. The candidate object (bottom panel, orange) has 97% of samples with γ < 1, indicating that this planet is probably on a grazing trajectory. For this object, we might choose to ignore the nongrazing umbrella, ψN, but the more conservative approach would be to perform a three-window analysis as usual. The distributions seen here for KOI-1426 are typical of Kepler targets, in that samples of γ from the transition umbrella can often be used to rule out/in certain transit geometries.
Paper: Modeling the Spectral Diversity of Quasars in the Sixteenth Data Release from the Sloan Digital Sky Survey
Authors: Allyson Brodzeller, and Kyle Dawson
Figure caption: The black data points correspond to the absolute i-band magnitude of a 10% random sampling of all quasars in DR16Q as a function of redshift. Only quasars detected at 1σ in the i band are displayed. The quasars selected for the training sample are shown in red. The quasars selected for the standard test sample are shown in blue. The vertical lines indicate the redshift bins of the training sample.
Paper: Modeling the Spectral Diversity of Quasars in the Sixteenth Data Release from the Sloan Digital Sky Survey
Authors: Allyson Brodzeller, and Kyle Dawson
Figure caption: An example of the NAL filter applied to a quasar spectrum. Top: the measured flux density is shown in black, with the estimated spectrum from the Gaussian smoothing filter overlaid in orange. The ID code corresponds to the unique PLATE-MJD-FIBERID of every SDSS spectrum. Bottom: the ratio of measured flux to smoothed flux is shown in black. Pixels at which the ratio deviates negatively by greater than three standard deviations are marked in purple. These flux decrements likely originate from CGM absorption and are masked in our clustering analysis.
Paper: Modeling the Spectral Diversity of Quasars in the Sixteenth Data Release from the Sloan Digital Sky Survey
Authors: Allyson Brodzeller, and Kyle Dawson
Figure caption: The error-weighted mean spectrum of each redshift bin is shown in black. The pixels that exhibit spectral diversity in the 68th percentile or higher are shown in red. Pixels at wavelengths <1216 Å are excluded from the percentile cut owing to the presence of the Lyα forest. The rest-frame wavelengths of Lyα, C IV, C III], and Mg II emission are indicated by vertical lines.
Paper: Modeling the Spectral Diversity of Quasars in the Sixteenth Data Release from the Sloan Digital Sky Survey
Authors: Allyson Brodzeller, and Kyle Dawson
Figure caption: Example spectra from each redshift bin that belong to one of the three primary outlier classes: spectra with unmasked NALs imprinted by CGM, spectra with strong intrinsic absorption, and spectra with peculiar shapes or features such as the flux calibration error seen in the peculiar spectrum of the highest-redshift bin. The spectra have been shifted to the rest-frame wavelength solution according to the Z_PCA redshift estimate. Quasar spectra with strong intrinsic absorption often also have an incorrect redshift estimate.
Paper: Modeling the Spectral Diversity of Quasars in the Sixteenth Data Release from the Sloan Digital Sky Survey
Authors: Allyson Brodzeller, and Kyle Dawson
Figure caption: Top: a region of the observer-frame spectrum of an outlier quasar at z = 2.028 featuring a candidate absorption system at z ≈ 1.507. Bottom: imaging data from DR9 of the DESI Legacy Imaging Survey centered on the quasar. Sources in DR9 are indicated with circles. There is a source to the northwest of the quasar that may be associated with the absorption seen in the spectrum.
Paper: Modeling the Spectral Diversity of Quasars in the Sixteenth Data Release from the Sloan Digital Sky Survey
Authors: Allyson Brodzeller, and Kyle Dawson
Figure caption: The six quasar spectra shown in black clustered together in redshift bin 1.57 < z < 1.8. The first panel shows the archetype spectrum. The resulting composite spectrum for the cluster is shown in red in the bottom panel.
Paper: Modeling the Spectral Diversity of Quasars in the Sixteenth Data Release from the Sloan Digital Sky Survey
Authors: Allyson Brodzeller, and Kyle Dawson
Figure caption: Three randomly selected composite quasar spectra from each redshift bin are shown in red. The number of quasars in the cluster is noted as N. Overlaid in black is the fit from the six-vector model described in Section 4.2 and its extrapolation (Section 4.5) beyond the observed wavelength range.
Paper: Modeling the Spectral Diversity of Quasars in the Sixteenth Data Release from the Sloan Digital Sky Survey
Authors: Allyson Brodzeller, and Kyle Dawson
Figure caption: The mean quasar spectrum and the first nine eigenspectra derived in this work are shown in black. The B12 eigenspectra are shown in red and are offset by two flux units for illustrative purposes.
Paper: Modeling the Spectral Diversity of Quasars in the Sixteenth Data Release from the Sloan Digital Sky Survey
Authors: Allyson Brodzeller, and Kyle Dawson
Figure caption: The average and range of the 16th to 84th percentiles of velocity offset for each redshift bin. The velocity offsets of the B12, six-vector, and PCA redshifts from Z_MGII are shown. The difference between the B12 model and PCA offsets is primarily a result of masking the Lyα forest.
Paper: Modeling the Spectral Diversity of Quasars in the Sixteenth Data Release from the Sloan Digital Sky Survey
Authors: Allyson Brodzeller, and Kyle Dawson
Figure caption: Top: the distributions of reduced χ2 for the best fits to the spectra of the standard test sample and BAL test sample using the B12 (upper left) and six-vector (lower left) models, and the corresponding distributions of reduced Δχ2 for the B12 (upper right) and six-vector (lower right) models. In all panels, the BAL test sample is split into two subsamples at an average S/N per pixel of 10. The vertical lines are the median value of each distribution. Bottom: the reduced χ2 of the best fits from the B12 (blue) and six-vector (red) models in the region of the Mg II emission line and C IV emission line in the standard test sample as a function of redshift. The uncertainties on the average reduced χ2 are on the 1% level and omitted for clarity.
Paper: Modeling the Spectral Diversity of Quasars in the Sixteenth Data Release from the Sloan Digital Sky Survey
Authors: Allyson Brodzeller, and Kyle Dawson
Figure caption: Each column shows the observer-frame spectrum of a randomly selected BAL quasar in gray. The fits from the B12 (top) and six-vector (bottom) models are overlaid on the observed spectrum in black. The red and blue shaded regions indicate the masked C IV and Si IV BAL troughs, respectively, as recorded in the BAL Quasar Catalog. The spectra have a BAL_PROB of at least 0.9.
Paper: Modeling the Spectral Diversity of Quasars in the Sixteenth Data Release from the Sloan Digital Sky Survey
Authors: Allyson Brodzeller, and Kyle Dawson
Figure caption: Each column shows the observer-frame spectrum of a randomly selected cluster outlier in gray. The fits from the B12 (top) and six-vector (bottom) models are overlaid on the observed spectrum in black.
Paper: Hydrogen and Helium Shock Phenomena during Rising Light in RR Lyrae Fundamental Mode Pulsators
Authors: George W. Preston, Christopher Sneden, and Merieme Chadid
Figure caption: Variations of Hα, He I 5875.62 Å, and He I 6678.15 Å, in the rising-light shock phases of RV Oct. Dotted lines indicate the rest wavelengths of these lines as defined by the metallic lines. The phases are written in the middle panel.
Paper: Hydrogen and Helium Shock Phenomena during Rising Light in RR Lyrae Fundamental Mode Pulsators
Authors: George W. Preston, Christopher Sneden, and Merieme Chadid
Figure caption: Mean line profiles of Hα, four He I lines and an He II line at the phase of maximum He emission in program stars RV Oct and X Ari.
Paper: Hydrogen and Helium Shock Phenomena during Rising Light in RR Lyrae Fundamental Mode Pulsators
Authors: George W. Preston, Christopher Sneden, and Merieme Chadid
Figure caption: A partial Grotrian diagram for He I. Transitions detected by Preston (2009) are in red, with the wavelengths labeled. No permitted dipole transitions connect the triplet and the ground states.
Paper: Hydrogen and Helium Shock Phenomena during Rising Light in RR Lyrae Fundamental Mode Pulsators
Authors: George W. Preston, Christopher Sneden, and Merieme Chadid
Figure caption: Two representative Hα lines near emission maximum. Top panel: the Hα profile in X Ari at phase ϕ = 0.909 in one of its pulsational cycles (black line). A Gaussian profile is fitted to the violet wing of the observed emission (blue curve) ignoring the broad violet and red wings present in most stars near emission maximum. A second fit to the broad wings is plotted as a red curve. Bottom panel: the same Gaussian fit (blue curve) is made to the observed Hα profile for the more typical case at a later phase, ϕ = 0.928, when there is no red emission component to constrain the Gaussian velocity center. Because of the general absence of this constraint, we adopted the photospheric velocity defined by metal lines to locate the centroids of all Gaussian fits.
Paper: Hydrogen and Helium Shock Phenomena during Rising Light in RR Lyrae Fundamental Mode Pulsators
Authors: George W. Preston, Christopher Sneden, and Merieme Chadid
Figure caption: The correlation of Hα emission equivalent widths measured by direct integration and a Gaussian model approximation, as defined in the text. Data between dotted lines show that Gaussian model EWs exceed measured values by a factor of two.
Paper: Hydrogen and Helium Shock Phenomena during Rising Light in RR Lyrae Fundamental Mode Pulsators
Authors: George W. Preston, Christopher Sneden, and Merieme Chadid
Figure caption: Top panel: Hα emission EWs measured via direct integration plotted vs. phases. For each star ϕ = 0.00 was set to be the phase of minimum radial velocity. The red points for RR Cet and the green points for RV Oct have been connected with solid lines of their colors. Bottom panel: the emission EWs scaled to a common flux maximum and shifted to a common emission peak phase; see text for descriptions of these Hα emission manipulations. Here, the blue line represents the mean trend of scaled emission vs. shifted phase. The symbols and colors of points are identified in this panel’s legend and are consistent with those of Figure 5.
Paper: Hydrogen and Helium Shock Phenomena during Rising Light in RR Lyrae Fundamental Mode Pulsators
Authors: George W. Preston, Christopher Sneden, and Merieme Chadid
Figure caption: Measured EWs (top panels) and scaled emission EWs shifted to phase ϕ = 0.92 (bottom panels) for He I 5876 and 6678 Å in the manner employed for Hα in Figure 6. The symbols and colors of points are identified in panel (d) and are consistent with those of Figure 5.
Paper: Hydrogen and Helium Shock Phenomena during Rising Light in RR Lyrae Fundamental Mode Pulsators
Authors: George W. Preston, Christopher Sneden, and Merieme Chadid
Figure caption: Phases that produce alignment of emission maxima for He I 5876 Å are plotted vs. those for Hα. The two shifts are strongly correlated.
Paper: Hydrogen and Helium Shock Phenomena during Rising Light in RR Lyrae Fundamental Mode Pulsators
Authors: George W. Preston, Christopher Sneden, and Merieme Chadid
Figure caption: Spectra of the He II 4686 Å region of eight RRab stars arranged bottom to top in order of increasing [Fe/H]. The relative flux values for RV Oct are correct, and the spectra for the other stars are shifted vertically for display purposes. The average spectrum shown in blue at the top of the plot was formed by a straight mean of the individual spectra. Dotted vertical lines are located at the rest wavelengths of the He II line and the photospheric Mg I line.
Paper: Hydrogen and Helium Shock Phenomena during Rising Light in RR Lyrae Fundamental Mode Pulsators
Authors: George W. Preston, Christopher Sneden, and Merieme Chadid
Figure caption: The variations of Hα pulsation velocity dR/dt (km s−1), equivalent width EW (mÅ), and Maxwell line-of-sight velocity dispersion ﹩{\sigma }_{\mathrm{Max}}﹩ (km s−1) with phase during rising light for six RRab stars. Red and blue symbols are measures of lines produced by infalling and outflowing atmospheric layers, respectively.
Paper: Hydrogen and Helium Shock Phenomena during Rising Light in RR Lyrae Fundamental Mode Pulsators
Authors: George W. Preston, Christopher Sneden, and Merieme Chadid
Figure caption: The variations of He I pulsation velocity dR/dt (km s−1; left), equivalent width EW (mÅ; middle), and velocity dispersion ﹩{\sigma }_{\mathrm{Max}}﹩ (km s−1; right) with phase during rising light for the same six RRab stars shown in Figure 10. Red and blue symbols are measures of lines produced by infalling and outflowing atmospheric layers, respectively. Unfilled dark green symbols denote emission features.
Paper: Hydrogen and Helium Shock Phenomena during Rising Light in RR Lyrae Fundamental Mode Pulsators
Authors: George W. Preston, Christopher Sneden, and Merieme Chadid
Figure caption: Hα and He I pulsation velocities from the left-hand windows of Figures 10 and 11 combined in one panel each for the six stars. The symbol colors are labeled in the panel for RR Cet. Squares are used for the Hα data; open squares denote those measurements made with IRAF fxcor, and filled squares for those made with IRAF splot. Data points for He 5876 Å in this figure represent more data than do those in Figures 10 and 11 because of coaddition.
Paper: Hydrogen and Helium Shock Phenomena during Rising Light in RR Lyrae Fundamental Mode Pulsators
Authors: George W. Preston, Christopher Sneden, and Merieme Chadid
Figure caption: The distance D traversed by the primary shock from the metallic line forming region just above the photosphere to the layer that produces outflowing Hα absorption. In the left panel D is expressed in units of km, and in the right panel D is shown in units of stellar radii. Data for six stars are taken from Table 13. Black lines show the mean trend of the data from a linear regression. Red lines show radii for Oo I and II groups taken from Table 1 of Marconi et al. (2005).
Paper: Hydrogen and Helium Shock Phenomena during Rising Light in RR Lyrae Fundamental Mode Pulsators
Authors: George W. Preston, Christopher Sneden, and Merieme Chadid
Figure caption: Line profiles of He I 5876 Å and Hα for six metal-poor RRab at four pulsation phases.
Paper: Hydrogen and Helium Shock Phenomena during Rising Light in RR Lyrae Fundamental Mode Pulsators
Authors: George W. Preston, Christopher Sneden, and Merieme Chadid
Figure caption: Line profiles of He I 5876 Å and Hα for six metal-rich RRab at four pulsation phases.
Paper: Challenging the Disk Instability Model. I. The Case of YZ LMi
Authors: Raymundo Baptista, and Wagner Schlindwein
Figure caption: Fractional amount of stream overflow (dashed lines) and of stream penetration (solid lines) as a function of the ratio of scale heights, Hs/Hd, and ratio of midplane densities, ρs0/ρd0 (labeled in each curve).
Paper: Challenging the Disk Instability Model. I. The Case of YZ LMi
Authors: Raymundo Baptista, and Wagner Schlindwein
Figure caption: Azimuthally averaged radial brightness temperature distributions of the YZ LMi quiescent accretion disk without (filled circles) and with (open squares) subtraction of a half-visible 22,500 K WD contribution, for radial bins of width 0.03 RL1 and d = 815 ± 138 pc. Dashed black curves show the 1σ limits on the distribution without WD subtraction. Asterisks depict temperatures along the ballistic stream trajectory. Red lines show Teff(R) curves of steady-state MTIM disk models including tidal dissipation for ﹩\mathrm{log}\dot{M}({\rm{g}}\,{{\rm{s}}}^{-1})=15.45﹩ (solid), 15.1 and 15.8 (dashed). Blue lines show Teff(R) curves of DIM disk models for Σmed (solid), Σ+ and Σ− (dashed); corresponding Teff(R) curves for DIM models including tidal dissipation are shown as blue dotted lines.
Paper: Challenging the Disk Instability Model. I. The Case of YZ LMi
Authors: Raymundo Baptista, and Wagner Schlindwein
Figure caption: Comparison of the vertical scale heights of the disk and the gas stream for YZ LMi. Radial runs of the disk scale height are shown for the DIM (blue) and MTIM (red) disk models; dashed lines show the corresponding 1σ limits. The vertical scale height of the gas stream is shown for T2 = 1900 K (solid line), 1000 K, and 3700 K (dashed lines). Vertical dotted lines depict the outer-disk radii Rd = 0.48 RL1 (C11) and Rd = 0.65 RL1 (SB18).