adsabs/AstroCLIMB huggingface dataset:
Paper: DELVE-ing into the Jet: A Thin Stellar Stream on a Retrograde Orbit at 30 kpc
Authors: P. S. Ferguson, N. Shipp, A. Drlica-Wagner, T. S. Li, W. Cerny, K. Tavangar, A. B. Pace, J. L. Marshall, A. H. Riley, M. Adamów, J. L. Carlin, Y. Choi, D. Erkal, D. J. James, Sergey E. Koposov, N. Kuropatkin, C. E. Martínez-Vázquez, S. Mau, B. Mutlu-Pakdil, K. A. G. Olsen, J. D. Sakowska, G. S. Stringfellow, B. Yanny
Figure caption: Modeling the track, width, and intensity of the Jet stream from DELVE DR1 photometric data. Top: density of stars that pass the optimized matched-filter selection that takes into account the observed distance gradient in the region of the Jet stream. Middle: maximum a posteriori model of the data shown in the top panel containing both stream and background components. Bottom: residual density map showing the observed density minus the model.
Paper: DELVE-ing into the Jet: A Thin Stellar Stream on a Retrograde Orbit at 30 kpc
Authors: P. S. Ferguson, N. Shipp, A. Drlica-Wagner, T. S. Li, W. Cerny, K. Tavangar, A. B. Pace, J. L. Marshall, A. H. Riley, M. Adamów, J. L. Carlin, Y. Choi, D. Erkal, D. J. James, Sergey E. Koposov, N. Kuropatkin, C. E. Martínez-Vázquez, S. Mau, B. Mutlu-Pakdil, K. A. G. Olsen, J. D. Sakowska, G. S. Stringfellow, B. Yanny
Figure caption: Measurement of Jet stream parameters as a function of position along the stream (ϕ 1) as derived from modeling the DELVE DR1 stellar density maps. From top to bottom are stream surface brightness, stream track, stream width, and linear density. The shaded area shows the 68% containment peak interval, and the black line shows the best-fit estimate of each parameter.
Paper: DELVE-ing into the Jet: A Thin Stellar Stream on a Retrograde Orbit at 30 kpc
Authors: P. S. Ferguson, N. Shipp, A. Drlica-Wagner, T. S. Li, W. Cerny, K. Tavangar, A. B. Pace, J. L. Marshall, A. H. Riley, M. Adamów, J. L. Carlin, Y. Choi, D. Erkal, D. J. James, Sergey E. Koposov, N. Kuropatkin, C. E. Martínez-Vázquez, S. Mau, B. Mutlu-Pakdil, K. A. G. Olsen, J. D. Sakowska, G. S. Stringfellow, B. Yanny
Figure caption: Selection of stars used to measure the proper motion of the Jet stream. Left: color–magnitude diagram demonstrating the selection applied to the data. The orange lines show the empirical M92 horizontal branch and Dotter isochrone ([Fe/H] = −1.57) used to select data. The blue dashed lines show our selection range in distance, and the red dashed lines our selection range in color. Center: color–color plot showing our selection range in blue around an empirical stellar locus of dereddened DES photometry in orange. Right: proper motion in stream coordinates of the sample of stars passing all selection cuts. The signal from the Jet stream is easily seen at ﹩({\mu }_{{\phi }_{1}}^{\star },{\mu }_{{\phi }_{2}})\sim (-1,0)﹩ mas yr−1 (circled in red).
Paper: DELVE-ing into the Jet: A Thin Stellar Stream on a Retrograde Orbit at 30 kpc
Authors: P. S. Ferguson, N. Shipp, A. Drlica-Wagner, T. S. Li, W. Cerny, K. Tavangar, A. B. Pace, J. L. Marshall, A. H. Riley, M. Adamów, J. L. Carlin, Y. Choi, D. Erkal, D. J. James, Sergey E. Koposov, N. Kuropatkin, C. E. Martínez-Vázquez, S. Mau, B. Mutlu-Pakdil, K. A. G. Olsen, J. D. Sakowska, G. S. Stringfellow, B. Yanny
Figure caption: Proper motion of high-probability member RGB (red) and BHB (blue) stars (p mem > 0.8). Additionally the line of best-fit proper motion is shown as a black dashed line. All the BHB stars used to measure the distance gradient are also high-probability members.
Paper: DELVE-ing into the Jet: A Thin Stellar Stream on a Retrograde Orbit at 30 kpc
Authors: P. S. Ferguson, N. Shipp, A. Drlica-Wagner, T. S. Li, W. Cerny, K. Tavangar, A. B. Pace, J. L. Marshall, A. H. Riley, M. Adamów, J. L. Carlin, Y. Choi, D. Erkal, D. J. James, Sergey E. Koposov, N. Kuropatkin, C. E. Martínez-Vázquez, S. Mau, B. Mutlu-Pakdil, K. A. G. Olsen, J. D. Sakowska, G. S. Stringfellow, B. Yanny
Figure caption: Best-fit stream model to the Jet stream. In each row the dark blue points show the best-fit stream model and the red points show the observations to which the model was fit. First row: on-sky distribution of the stream. Second row: distance modulus of the stream. Third and fourth rows: reflex-corrected proper motions of the stream in ϕ 1 and ϕ 2 respectively. Fifth row: predicted heliocentric velocities of the stream.
Paper: Mapping the Pressure-dependent Day–Night Temperature Contrast of a Strongly Irradiated Atmosphere with HST Spectroscopic Phase Curve
Authors: Ben W. P. Lew, Dániel Apai, Yifan Zhou, Mark Marley, L. C. Mayorga, Xianyu Tan, Vivien Parmentier, Sarah Casewell, Siyi Xu (许偲艺)
Figure caption: Left panel: the median spectra of the white dwarf–brown dwarf system. The blue line highlights the spectra from 1.1 to 1.67 μm. The two hydrogen absorption regions of white dwarfs are 1.09–1.11 μm and 1.27–1.32 μm. Right panel: the six-orbit 1.1–1.67 μm integrated broadband light curve. The two white dwarf eclipse events occur at the first and fifth HST orbits. The error bar at t = 9 hr shows the representative flux uncertainties of 1.4% for a single photometric point. The shaded blue regions indicate the expected eclipse events with a period of 121.72 minutes.
Paper: Mapping the Pressure-dependent Day–Night Temperature Contrast of a Strongly Irradiated Atmosphere with HST Spectroscopic Phase Curve
Authors: Ben W. P. Lew, Dániel Apai, Yifan Zhou, Mark Marley, L. C. Mayorga, Xianyu Tan, Vivien Parmentier, Sarah Casewell, Siyi Xu (许偲艺)
Figure caption: (a) The folded light curve with the fitted period of 2.02862 hr. The primary-eclipse part of the phase-folded light curve is plotted separately in panel (e). (b) The residuals of the model fit to the light curve. The residuals are normalized by the photometric uncertainty. (c) The histogram of all the residuals. The orange line shows a normal distribution with one standard deviation. (d) The best-fit model and the light curve plotted in units of time on the x-axis. (e) A zoom-in plot of the model fit to the light curve in the eclipse region.
Paper: Mapping the Pressure-dependent Day–Night Temperature Contrast of a Strongly Irradiated Atmosphere with HST Spectroscopic Phase Curve
Authors: Ben W. P. Lew, Dániel Apai, Yifan Zhou, Mark Marley, L. C. Mayorga, Xianyu Tan, Vivien Parmentier, Sarah Casewell, Siyi Xu (许偲艺)
Figure caption: An illustration of the white dwarf–brown dwarf system at different phases. We define Phase A (ϕ = 0) as the primary-eclipse phase and Phase C (ϕ = 0.5) as the secondary-eclipse phase. The white dwarf emission is completely blocked by the brown dwarf, so only the brown dwarf nightside (midnight) emission is observed during the primary eclipse. Because the brown dwarf radius is at least 3.5 times larger than that of the white dwarf, the brown dwarf’s emission is at best only partially obscured during the secondary eclipse.
Paper: Mapping the Pressure-dependent Day–Night Temperature Contrast of a Strongly Irradiated Atmosphere with HST Spectroscopic Phase Curve
Authors: Ben W. P. Lew, Dániel Apai, Yifan Zhou, Mark Marley, L. C. Mayorga, Xianyu Tan, Vivien Parmentier, Sarah Casewell, Siyi Xu (许偲艺)
Figure caption: The calculated centroids with partial light curves with phase coverage around the secondary eclipse (ϕ = 0.5). The centroid of a light curve that peaks after secondary eclipse has a value above 0.5 and vice versa. The derived centroids depend on the phase coverage of the partial light curves, so we find no convincing evidence of phase offset based on our data set.
Paper: Mapping the Pressure-dependent Day–Night Temperature Contrast of a Strongly Irradiated Atmosphere with HST Spectroscopic Phase Curve
Authors: Ben W. P. Lew, Dániel Apai, Yifan Zhou, Mark Marley, L. C. Mayorga, Xianyu Tan, Vivien Parmentier, Sarah Casewell, Siyi Xu (许偲艺)
Figure caption: The comparison of marginalized brown dwarf radius posterior distribution based on the MCMC eclipse light-curve fitting results and that with the additional constraint from white dwarf evolutionary models, radial velocity semiamplitudes, and white dwarf near-infrared spectral fitting.
Paper: Mapping the Pressure-dependent Day–Night Temperature Contrast of a Strongly Irradiated Atmosphere with HST Spectroscopic Phase Curve
Authors: Ben W. P. Lew, Dániel Apai, Yifan Zhou, Mark Marley, L. C. Mayorga, Xianyu Tan, Vivien Parmentier, Sarah Casewell, Siyi Xu (许偲艺)
Figure caption: The binned averaged nightside spectra (black line), which are observed just before or after the primary eclipse, show less scatters between spectral points and is similar to the SDSS1411-B spectrum during eclipse (orange line). The gray lines show the potential bias of the averaged nightside spectrum due to uncertainty of white dwarf temperature, gravity, and wavelength calibration sampled by the Monte Carlo method.
Paper: Mapping the Pressure-dependent Day–Night Temperature Contrast of a Strongly Irradiated Atmosphere with HST Spectroscopic Phase Curve
Authors: Ben W. P. Lew, Dániel Apai, Yifan Zhou, Mark Marley, L. C. Mayorga, Xianyu Tan, Vivien Parmentier, Sarah Casewell, Siyi Xu (许偲艺)
Figure caption: The blue line shows the cleaned white dwarf spectrum after removal of the brown dwarf eclipse spectrum. The orange line shows the binned white dwarf model spectrum. The gray shaded regions highlight the absorption lines in the white dwarf spectrum.
Paper: Mapping the Pressure-dependent Day–Night Temperature Contrast of a Strongly Irradiated Atmosphere with HST Spectroscopic Phase Curve
Authors: Ben W. P. Lew, Dániel Apai, Yifan Zhou, Mark Marley, L. C. Mayorga, Xianyu Tan, Vivien Parmentier, Sarah Casewell, Siyi Xu (许偲艺)
Figure caption: Top panel: the binned spectra at morning, noon, evening, and night orbital phases. The gray line represents the nightside spectrum. Bottom panel: comparison of the evening and morning spectra shows similar spectral features across 1.1–1.67 μm. The scaled day–night spectral difference (dashed line) also matches well to the evening and morning spectra, showing that the evening and morning spectra can be reproduced by a linear combination of the dayside and nightside spectra.
Paper: Mapping the Pressure-dependent Day–Night Temperature Contrast of a Strongly Irradiated Atmosphere with HST Spectroscopic Phase Curve
Authors: Ben W. P. Lew, Dániel Apai, Yifan Zhou, Mark Marley, L. C. Mayorga, Xianyu Tan, Vivien Parmentier, Sarah Casewell, Siyi Xu (许偲艺)
Figure caption: Top panel: the binned dayside and nightside spectra of SDSS1411-B. The water-band flux of the dayside spectrum is almost two times higher than that of nightside spectrum. Bottom panel: the relative spectral variation between the dayside and nightside spectra. The spectral variation is almost 10 times larger in the water band than in the ﹩J^{\prime} ﹩ band. To show order-of-magnitude variations with uncertainty ranges that include negative values, we use the “symlog” y-axis scale, which is in linear scale below unity and in log scale above unity.
Paper: Mapping the Pressure-dependent Day–Night Temperature Contrast of a Strongly Irradiated Atmosphere with HST Spectroscopic Phase Curve
Authors: Ben W. P. Lew, Dániel Apai, Yifan Zhou, Mark Marley, L. C. Mayorga, Xianyu Tan, Vivien Parmentier, Sarah Casewell, Siyi Xu (许偲艺)
Figure caption: The brightness temperatures of the dayside and nightside spectra. The brightness temperatures are binned with a bin size of 0.014 μm. The brightness temperatures are higher in the ﹩J^{\prime} ﹩ band than in the water bands.
Paper: Mapping the Pressure-dependent Day–Night Temperature Contrast of a Strongly Irradiated Atmosphere with HST Spectroscopic Phase Curve
Authors: Ben W. P. Lew, Dániel Apai, Yifan Zhou, Mark Marley, L. C. Mayorga, Xianyu Tan, Vivien Parmentier, Sarah Casewell, Siyi Xu (许偲艺)
Figure caption: Left panel: the T–P profiles of nightside (solid blue line) and dayside (solid red line) models. The purple, green, and red dashed lines show the condensation curves of MgSiO3, Mg2SiO4, and Fe, respectively, from Visscher et al. (2010). The RCBs of nightside and dayside models are at around 30–60  bars. Right panel: the day–night temperature difference.
Paper: Mapping the Pressure-dependent Day–Night Temperature Contrast of a Strongly Irradiated Atmosphere with HST Spectroscopic Phase Curve
Authors: Ben W. P. Lew, Dániel Apai, Yifan Zhou, Mark Marley, L. C. Mayorga, Xianyu Tan, Vivien Parmentier, Sarah Casewell, Siyi Xu (许偲艺)
Figure caption: Top panel: the nightside (purple line) and dayside (red line) model spectra qualitatively reproduce the spectral shape of the observed nightside (dark-green line) and dayside spectra (light-green line). We plot the ground-based H- and K  s -band photometry from Casewell et al. (2018) as black squares at 1.66 and 2.16 μm, respectively. The modeled dayside H-band flux (red square) is consistent with observed values, while the modeled K  s -band flux (red square) is higher than the observed value. See text for the discussion of the difference between modeled and observed spectra. Bottom panel: the modeled day–night spectral variation shows that the flux variation is about an order of magnitude higher in the water-band region than that in the J-band region, matching the observed wavelength dependence in day–night spectral variation.
Paper: Mapping the Pressure-dependent Day–Night Temperature Contrast of a Strongly Irradiated Atmosphere with HST Spectroscopic Phase Curve
Authors: Ben W. P. Lew, Dániel Apai, Yifan Zhou, Mark Marley, L. C. Mayorga, Xianyu Tan, Vivien Parmentier, Sarah Casewell, Siyi Xu (许偲艺)
Figure caption: Left panel: the contribution function of the nightside model. The colors represent the relative contribution per pressure layer to the emission. Right panel: the peak of the J-band and water-band contribution function of the nightside spectrum is at ∼20–80 bars and 2–20 bars, respectively.
Paper: Mapping the Pressure-dependent Day–Night Temperature Contrast of a Strongly Irradiated Atmosphere with HST Spectroscopic Phase Curve
Authors: Ben W. P. Lew, Dániel Apai, Yifan Zhou, Mark Marley, L. C. Mayorga, Xianyu Tan, Vivien Parmentier, Sarah Casewell, Siyi Xu (许偲艺)
Figure caption: Left panel: the nightside and dayside brightness temperatures are less different at higher nightside brightness temperatures. The orange y = x line portrays equal dayside and nightside temperatures. Right panel: the measured day–night brightness temperature contrast as a function of nightside pressures suggests that day–night temperature contrast increases with lower pressure.
Paper: Mapping the Pressure-dependent Day–Night Temperature Contrast of a Strongly Irradiated Atmosphere with HST Spectroscopic Phase Curve
Authors: Ben W. P. Lew, Dániel Apai, Yifan Zhou, Mark Marley, L. C. Mayorga, Xianyu Tan, Vivien Parmentier, Sarah Casewell, Siyi Xu (许偲艺)
Figure caption: Left panel: the observed nightside brightness temperatures at different inferred pressures, which are derived from the contribution function of the nightside model, are plotted as blue points. The solid blue and orange lines show the modeled dayside and nightside temperature–pressure profile. The blue dashed line shows an adiabat profile that shares the same interior temperature at 30 bars with the model. Right panel: observed dayside brightness temperatures over different inferred pressures, which are derived from the contribution function of the dayside model, are plotted in orange points. The solid and dashed lines are the same as those in the left panel.
Paper: Mapping the Pressure-dependent Day–Night Temperature Contrast of a Strongly Irradiated Atmosphere with HST Spectroscopic Phase Curve
Authors: Ben W. P. Lew, Dániel Apai, Yifan Zhou, Mark Marley, L. C. Mayorga, Xianyu Tan, Vivien Parmentier, Sarah Casewell, Siyi Xu (许偲艺)
Figure caption: Comparison of the binned dayside (dotted red line) and nightside (solid blue line) SDSS1411-B spectra with field T dwarfs and WASP-43 b spectra. The SDSS1411-B nightside spectrum (thick light-blue line) shows a similar water-band absorption depth to the field T5 dwarf (solid purple line) and the lack of a strong methane absorption feature at 1.65 μm, which is prevalent among T dwarf spectra. The higher gravity and the steeper temperature gradient of SDSS1411-B cause the deeper water-band absorption compared to that of the nightside spectrum of hot Jupiter WASP-43 b (solid orange line). We also plot the spectra of field T1 and T7 dwarfs in solid green and maroon lines, respectively, for reference.
Paper: Mapping the Pressure-dependent Day–Night Temperature Contrast of a Strongly Irradiated Atmosphere with HST Spectroscopic Phase Curve
Authors: Ben W. P. Lew, Dániel Apai, Yifan Zhou, Mark Marley, L. C. Mayorga, Xianyu Tan, Vivien Parmentier, Sarah Casewell, Siyi Xu (许偲艺)
Figure caption: The isolated brown dwarfs, plotted as colored circles, manifest weak color variations in rotational modulations (Lew et al. 2020b); SDSS1411-B, plotted as black stars, shows significant change in J − H colors as the irradiation varies across the night (faintest M  J ), morning, evening, and noon (brightest M  J ) orbital phases. The colored solid lines are the fitted straight lines to the color–magnitude variations of each objects. The dashed–dotted lines show the semimajor axis of the fitted ellipses to the color–magnitude variations of two T dwarfs, GU Piscium b and 2MASS J22282889–431026. The gray circles show the J − H colors and J-band magnitudes of field L and T dwarfs based on the catalog managed by Dupuy & Liu (2012). The gray curve shows the evolution from L (upper right) to T spectral type (lower left).
Paper: Mapping the Pressure-dependent Day–Night Temperature Contrast of a Strongly Irradiated Atmosphere with HST Spectroscopic Phase Curve
Authors: Ben W. P. Lew, Dániel Apai, Yifan Zhou, Mark Marley, L. C. Mayorga, Xianyu Tan, Vivien Parmentier, Sarah Casewell, Siyi Xu (许偲艺)
Figure caption: The analytical estimate of day–night temperature contrast ratio with rotational periods of 2 hr (dashed brown line) and 3.5 days (solid brown line) with a fixed drag timescale of 109 s. The temperature contrast ratio of SDSS1411-B, shown as a filled black circle, is lower than the analytical estimate with a period of 2 hr. The analytical temperature contrast ratio with the 109 s drag timescale is a lower limit because the temperature contrast ratio increases with shorter drag timescale. The colored points show the observed day–night temperature contrast ratio of hot Jupiters listed in Table 2 in Komacek & Showman (2016), including HD 189733b (Knutson et al.2009, 2012), WASP-43b (Stevenson et al. 2014), HD 209458b (Crossfield et al. 2012; Zellem et al. 2014), HD 149026b (Knutson et al. 2009), WASP-14b (Wong et al. 2015), WASP-19b (Wong et al. 2016), HAT-P-7b (Wong et al. 2016), WASP-18b (Arcangeli et al. 2019), and WASP-12 b (Cowan et al. 2012). The temperature contrast ratios of hot Jupiters observed at different wavelengths are plotted in different colors and markers. The observed temperature contrast ratio of WD-0137-BD (Lothringer & Casewell 2020), which is another irradiated brown dwarf, is plotted as a black square.
Paper: Mapping the Pressure-dependent Day–Night Temperature Contrast of a Strongly Irradiated Atmosphere with HST Spectroscopic Phase Curve
Authors: Ben W. P. Lew, Dániel Apai, Yifan Zhou, Mark Marley, L. C. Mayorga, Xianyu Tan, Vivien Parmentier, Sarah Casewell, Siyi Xu (许偲艺)
Figure caption: Comparison of median spectra with different spectral extraction methods illustrates that the three spectra extracted with different methods are consistent with each other within ∼3% levels for a wavelength range of 1.1–1.67 μm. The uniform and optimal extraction methods do not change the median spectra but do change the standard deviation of the light curve. The bottom panel shows the ratio of spectra extracted with the self-developed pipeline and with the standard aXe pipeline. Visual inspection of the images confirms that the three gray shaded regions of the spectra extracted with the aXe pipeline are affected by cosmic-ray or bad pixels.
Paper: Mapping the Pressure-dependent Day–Night Temperature Contrast of a Strongly Irradiated Atmosphere with HST Spectroscopic Phase Curve
Authors: Ben W. P. Lew, Dániel Apai, Yifan Zhou, Mark Marley, L. C. Mayorga, Xianyu Tan, Vivien Parmentier, Sarah Casewell, Siyi Xu (许偲艺)
Figure caption: The posterior distribution of the light-curve model parameters with the MCMC method.
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: Grid of 2D event circles with uniform distribution of the stars.
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: Distribution of distances of stars of the region  R . Binning: 30 pc.
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: Distribution of multiplicities of events from regions  R  1 (panel a) and  R  2 (panel b). Red curves represent Poisson distributions, where discrete values M ! are interpolated by gamma function Γ(M + 1).
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: Signature of binaries in region  R : distribution P(d ij, α ij) (panels a and b are linear and logarithmic scales, respectively), distribution P(α ij) for d ij ≤ 15 as (panel c), and distribution P(d ij) for α ij ≤ 15° (panel d). Units: d ij[as], α ij[deg]. Binning: 1.44 as × 1.°8, 0.36 as × 0.°4, 0.°36, 0.288 as.
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: Radial separations for pairs of the region  R  outside window defined by Equation (15) (panel a) and inside the window (panel b). Binning: 4 pc.
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: Comparison of distributions of relative errors: ΔL/L outside (panel a), inside (panel b) the window of binaries defined by Equation (15), and Δp/p (panel c) for sources inside the window. Data are from the region  R . Binning: 0.002.
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: Scaled separation ﹩\hat{\xi }﹩: the peak of binaries and random background (red curve). Region  R  1: equal normalization of data and background (panel a), data and renormalized background (panel b). Region  R  2: data and renormalized background (panel c).
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: Ratio n 2/N 2 of the number of binaries and the total number of pairs in different d × α windows in the regions  R  1 and  R  2 under different conditions. The result of this ratio ﹩\left(\beta \right)﹩ is in the second row of the respective window.
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: Scaled separation ﹩\hat{\xi }﹩: peak of binaries of magnitude G ≤ 15 and random background (red curve) in region  R .
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: Function β defines probability of true binary at different separations in  R  for α ≤ α  c . Panel (a): all events. Panel (b): enriched exposition. Panel (c): only stars of magnitude G ≤ 15. Panel (d): enriched exposition, event subsample ρ 2 = 36 as. Unit: d ij[as].