adsabs/AstroCLIMB huggingface dataset:
Paper: The TANDEM Project as a Pilot Case for Wide-field Telescope Arrays
Authors: A. Buzzoni, A. Carbognani, R. Di Luca, E. Diolaiti, R. Gualandi, A. Semola, G. M. Stirpe, F. Bonoli, I. Bruni, F. Cortecchia, I. Foppiani, S. Galleti, M. Lombini, L. Schreiber
Figure caption: The TANDEM photometric system includes a set of four BVRcIc filters. Effective wavelengths (dots and labels in the plot) fairly well reproduce the Johnson–Cousins system. As a common feature, note that the Ic band is in fact mainly constrained by the CMOS spectral transmission.
Paper: The TANDEM Project as a Pilot Case for Wide-field Telescope Arrays
Authors: A. Buzzoni, A. Carbognani, R. Di Luca, E. Diolaiti, R. Gualandi, A. Semola, G. M. Stirpe, F. Bonoli, I. Bruni, F. Cortecchia, I. Foppiani, S. Galleti, M. Lombini, L. Schreiber
Figure caption: The superposed TANDEM radial profile of vignetting, as directly assessed from each of the four telescope’s FOV. According to the adopted size of the secondary mirror we have that the central 1° × 1° region of the frame is virtually unvignetted while a residual effect of up to 0.15 mag appears at the 2° × 2° edge of the frame.
Paper: The TANDEM Project as a Pilot Case for Wide-field Telescope Arrays
Authors: A. Buzzoni, A. Carbognani, R. Di Luca, E. Diolaiti, R. Gualandi, A. Semola, G. M. Stirpe, F. Bonoli, I. Bruni, F. Cortecchia, I. Foppiani, S. Galleti, M. Lombini, L. Schreiber
Figure caption: The same pointing is compared before (left) and after (right) TANDEM optimization. Note in the right panel that the four telescopes are automatically reassigned to each field such as to obtain a converging pointing pattern that minimizes the cross section through the dome shutter.
Paper: Identifying Hierarchically Triple Star Systems with Gaia DR3 and LAMOST
Authors: Tongyu He, Jiao Li, Jiangdan Li, Jianping Xiong, Xiaobin Zhang, Mikhail Kovalev, Qiyuan Cheng, Sufen Guo, Mingkuan Yang, Xuefei Chen, Zhanwen Han
Figure caption: Distribution of the number of ΔVs between any two components in the triples. The three velocities, ordered from lowest to highest, are labeled as V1, V2, and V3. The upper panel shows the ΔV distribution between any two components of the triple-star sample from Section 3, while the lower panel shows the same for the 132 triple-star candidates from C. Li et al. (2021). The black dashed line denotes ΔV between V2 − V1 (ΔV2−1), the red dashed–dotted line shows ΔV between V3 − V2 (ΔV3−2), and the blue solid line indicates ΔV between V3 − V1 (ΔV3−1).
Paper: Identifying Hierarchically Triple Star Systems with Gaia DR3 and LAMOST
Authors: Tongyu He, Jiao Li, Jiangdan Li, Jianping Xiong, Xiaobin Zhang, Mikhail Kovalev, Qiyuan Cheng, Sufen Guo, Mingkuan Yang, Xuefei Chen, Zhanwen Han
Figure caption: Comparison of the CCF peak values for Gaia DR3 2077667962475652864 using different template spectra. In the upper part of the figure shows the normalized spectra. In the lower part of the figure, we present the generated CCF, A1 = 0.53, V1 = −131 km s−1, A2 = 0.48, V2 = 134 km s−1, and A3 = 0.41, V3 = 19 km s−1. The black solid line represents a template spectrum with a temperature of 7862 K, while the gray dashed line represents a CCF generated using a conventional solar spectrum template.
Paper: Identifying Hierarchically Triple Star Systems with Gaia DR3 and LAMOST
Authors: Tongyu He, Jiao Li, Jiangdan Li, Jianping Xiong, Xiaobin Zhang, Mikhail Kovalev, Qiyuan Cheng, Sufen Guo, Mingkuan Yang, Xuefei Chen, Zhanwen Han
Figure caption: RV fitting for the triple-star system Gaia DR3 249662295687401216. The black points and red stars represent the observed data after phase folding, and the red line indicates the fitted RV curve. The blue points show the velocity of the inner binary's center of mass, while the blue dashed line represents the fitted curve for the inner binary's center of mass velocity. The green points indicate the velocity of the tertiary star, and the green dashed line illustrates the fitted curve for the tertiary star's velocity. V1 and V2 denote the RVs of the primary and secondary stars in the inner binary, respectively, and V3 represents the RV curve of the tertiary star.
Paper: Identifying Hierarchically Triple Star Systems with Gaia DR3 and LAMOST
Authors: Tongyu He, Jiao Li, Jiangdan Li, Jianping Xiong, Xiaobin Zhang, Mikhail Kovalev, Qiyuan Cheng, Sufen Guo, Mingkuan Yang, Xuefei Chen, Zhanwen Han
Figure caption: Light curve fitting for the triple-star system Gaia DR3 249662295687401216. The blue dots indicate phase-folded observations, and the solid yellow line indicates the results of the fit. The horizontal axis indicates the phase, and the fitting residuals are shown at the bottom of the plot.
Paper: Identifying Hierarchically Triple Star Systems with Gaia DR3 and LAMOST
Authors: Tongyu He, Jiao Li, Jiangdan Li, Jianping Xiong, Xiaobin Zhang, Mikhail Kovalev, Qiyuan Cheng, Sufen Guo, Mingkuan Yang, Xuefei Chen, Zhanwen Han
Figure caption: The color–magnitude graph of 23 triple-star systems (red stars) determined from Gaia DR3 and LAMOST (blue dots). The x-axis shows the color difference between GBP and GRP, and the y-axis displays the absolute magnitudes MG. All photometric data are from Gaia DR3.
Paper: Identifying Hierarchically Triple Star Systems with Gaia DR3 and LAMOST
Authors: Tongyu He, Jiao Li, Jiangdan Li, Jianping Xiong, Xiaobin Zhang, Mikhail Kovalev, Qiyuan Cheng, Sufen Guo, Mingkuan Yang, Xuefei Chen, Zhanwen Han
Figure caption: RV fitting of inner binaries for the triple-star system j03 Gaia DR3 669133613876714. The green circles show the velocity of the primary star, while blue squares represent the velocity of the secondary star. V1 and V2 denote the RV curves of the primary and secondary stars in the inner binary.
Paper: Identifying Hierarchically Triple Star Systems with Gaia DR3 and LAMOST
Authors: Tongyu He, Jiao Li, Jiangdan Li, Jianping Xiong, Xiaobin Zhang, Mikhail Kovalev, Qiyuan Cheng, Sufen Guo, Mingkuan Yang, Xuefei Chen, Zhanwen Han
Figure caption: RV variations of the triple-star system Gaia DR3 249662295687401216 over time. Red circles indicate spectra where CCF analysis detected only one RV. Blue circles and stars represent spectra with two detected RVs, and green circles, stars, and triangles denote spectra with three different RVs.
Paper: Resolved Stellar Mass Estimation of Nearby Late-type Galaxies for the SPHEREx Era: Dependence on Stellar Population Synthesis Models
Authors: Jeong Hwan Lee, Minjin Kim, Taehyun Kim, Hyunjin Shim, Luis C. Ho, Ho Seong Hwang, Hyunmi Song, Dohyeong Kim, Yujin Yang, Woong-Seob Jeong
Figure caption: Example SEDs of rebinned spaxels in the central regions of the four PHANGS-MUSE galaxies. The left-hand panels display the observed spectra (orange) and best-fit templates from pPXF (blue) over the full wavelength range of the SPS model (λ ∼ 0.2−5.0 μm), along with the photometric data points from 2MASS JHKs (orange diamonds) and Spitzer/IRAC 3.6, 4.5 μm (red star symbols). The zoomed-in panels on the right-hand side show the SEDs within the pPXF fitting range of λ = 0.485−0.7 μm. The observed spectra and best-fit templates are depicted in the left-hand panels, with the residual SEDs represented by green curves. Gray-shaded regions indicate the masked wavelength ranges. The stellar population parameters derived from the best-fit pPXF results are displayed at the top of each zoomed-in panel. These results were obtained using the E-MILES models.
Paper: Resolved Stellar Mass Estimation of Nearby Late-type Galaxies for the SPHEREx Era: Dependence on Stellar Population Synthesis Models
Authors: Jeong Hwan Lee, Minjin Kim, Taehyun Kim, Hyunjin Shim, Luis C. Ho, Ho Seong Hwang, Hyunmi Song, Dohyeong Kim, Yujin Yang, Woong-Seob Jeong
Figure caption: Violin diagrams illustrating the distributions of mass-to-light ratios at IRAC 3.6 μm for each SPS model. The results are displayed in separate panels: E-MILES (top left-hand panel), BC03 (top right-hand panel), CB19 (bottom left-hand panel), and FSPS (bottom right-hand panel). Within each panel, the distributions are presented for all individual galaxies included in this study. These galaxies in the x-axis are ordered by their median stellar ages derived using E-MILES model. The median mass-to-light ratios for all galaxies are represented by gray horizontal lines, with the specific values indicated at the bottom of each panel.
Paper: Resolved Stellar Mass Estimation of Nearby Late-type Galaxies for the SPHEREx Era: Dependence on Stellar Population Synthesis Models
Authors: Jeong Hwan Lee, Minjin Kim, Taehyun Kim, Hyunjin Shim, Luis C. Ho, Ho Seong Hwang, Hyunmi Song, Dohyeong Kim, Yujin Yang, Woong-Seob Jeong
Figure caption: Contour plots showing the distribution of Spitzer/IRAC colors at 3.6 and 4.5 μm ([3.6] − [4.5]) as a function of stellar ages. In each panel, colored contours show the stellar-only IRAC color distributions derived from the best-fit spectra of the pPXF results, based on different SPS models: E-MILES (blue), BC03 (orange), CB19 (red), and FSPS (green). The contour levels represent the 50th, 70th, 80th, 85th, 90th, 95th, and 99th percentiles of the 2D distributions of spaxel counts.
Paper: Resolved Stellar Mass Estimation of Nearby Late-type Galaxies for the SPHEREx Era: Dependence on Stellar Population Synthesis Models
Authors: Jeong Hwan Lee, Minjin Kim, Taehyun Kim, Hyunjin Shim, Luis C. Ho, Ho Seong Hwang, Hyunmi Song, Dohyeong Kim, Yujin Yang, Woong-Seob Jeong
Figure caption: Comparison of stellar kinematics between this study and a previous PHANGS-MUSE study (E. Emsellem et al. 2022), both based on the E-MILES model. The two panels show the differences in radial velocities (left-hand panel) and velocity dispersions (right-hand panel), plotted as a function of galactocentric radius normalized by the effective radius of each galaxy. These differences are calculated by subtracting the luminosity-weighted mean kinematic parameters of Voronoi-binned spaxels (PHANGS-MUSE data release 1) from the values of SPHEREx-rebinned spaxels (this study). Blue diamonds with error bars represent the median differences within the radial bins, alongside the 16th and 84th percentiles of their distributions.
Paper: Resolved Stellar Mass Estimation of Nearby Late-type Galaxies for the SPHEREx Era: Dependence on Stellar Population Synthesis Models
Authors: Jeong Hwan Lee, Minjin Kim, Taehyun Kim, Hyunjin Shim, Luis C. Ho, Ho Seong Hwang, Hyunmi Song, Dohyeong Kim, Yujin Yang, Woong-Seob Jeong
Figure caption: Contour plots showing the distribution of output parameters, including age, metallicity, and V-band extinction magnitude (AV), derived from the best-fit pPXF results for all spaxels in 19 PHANGS-MUSE galaxies. In each panel, the contour levels represent the 50th, 70th, 80th, 85th, 90th, 95th, and 99th percentiles of the 2D distributions of spaxel counts. The top four panels show the distributions of age and metallicity, and the bottom panels show the distributions of age and AV. Results from the four SPS models are displayed in separate columns: E-MILES (first column), BC03 (second column), CB19 (third column), and FSPS (fourth column). Note that for BC03, the AV values are fixed to those derived from the CB19 model in this study.
Paper: Resolved Stellar Mass Estimation of Nearby Late-type Galaxies for the SPHEREx Era: Dependence on Stellar Population Synthesis Models
Authors: Jeong Hwan Lee, Minjin Kim, Taehyun Kim, Hyunjin Shim, Luis C. Ho, Ho Seong Hwang, Hyunmi Song, Dohyeong Kim, Yujin Yang, Woong-Seob Jeong
Figure caption: Comparison of stellar population parameters between this study and a previous PHANGS-MUSE study (I. Pessa et al. 2023). The two panels show the differences in stellar ages (left-hand panel) and metallicities (right-hand panel), with the same x-axis as in Figure 4. The data for ages and metallicities were digitized from Figures 2 and 7 in the work of I. Pessa et al. (2023), respectively. The symbols have the same meaning as in Figure 4.
Paper: Resolved Stellar Mass Estimation of Nearby Late-type Galaxies for the SPHEREx Era: Dependence on Stellar Population Synthesis Models
Authors: Jeong Hwan Lee, Minjin Kim, Taehyun Kim, Hyunjin Shim, Luis C. Ho, Ho Seong Hwang, Hyunmi Song, Dohyeong Kim, Yujin Yang, Woong-Seob Jeong
Figure caption: Stellar mass-to-light ratios as a function of age, derived from the spectral templates from the four SPS models: E-MILES (first column), BC03 (second column), CB19 (third column), and FSPS (fourth column). The upper set of four panels displays the mass-to-light ratios calculated in the SDSS r band, while the lower set shows those obtained in Spitzer/IRAC channel 1 (3.6 μm). Each panel is color-coded according to the metallicity bin from the SPS models.
Paper: Resolved Stellar Mass Estimation of Nearby Late-type Galaxies for the SPHEREx Era: Dependence on Stellar Population Synthesis Models
Authors: Jeong Hwan Lee, Minjin Kim, Taehyun Kim, Hyunjin Shim, Luis C. Ho, Ho Seong Hwang, Hyunmi Song, Dohyeong Kim, Yujin Yang, Woong-Seob Jeong
Figure caption: SEDs in the wavelengths of 0.45−5.0 μm from SSP templates, assuming a stellar age of ﹩{\rm{log}}\,{\rm{Age}}\,{\rm{(yr)}}=8.9﹩ and solar metallicity ([Z/Z⊙] = 0.0), approximately corresponding to the median values of stellar parameters in Table 1. Each panel compared the SEDs of BC03 (left-hand panel), CB19 (middle panel), and FSPS (right-hand panel) with those from E-MILES, highlighing the differences among the models in the NIR regime.
Paper: Resolved Stellar Mass Estimation of Nearby Late-type Galaxies for the SPHEREx Era: Dependence on Stellar Population Synthesis Models
Authors: Jeong Hwan Lee, Minjin Kim, Taehyun Kim, Hyunjin Shim, Luis C. Ho, Ho Seong Hwang, Hyunmi Song, Dohyeong Kim, Yujin Yang, Woong-Seob Jeong
Figure caption: Example white light maps (left-hand column), resolved stellar mass maps (middle column), and 3.6 μm mass-to-light ratio maps (right-hand column) for two PHANGS-MUSE galaxies. The white light maps are generated from the original PHANGS-MUSE data cubes by summing the flux across all wavelengths, providing a comparison with the SPHEREx-binned maps. The resolved stellar mass maps and mass-to-light ratio maps are based on the SPHEREx-binned images, which were used to determine the fiducial stellar masses in this study.
Paper: Resolved Stellar Mass Estimation of Nearby Late-type Galaxies for the SPHEREx Era: Dependence on Stellar Population Synthesis Models
Authors: Jeong Hwan Lee, Minjin Kim, Taehyun Kim, Hyunjin Shim, Luis C. Ho, Ho Seong Hwang, Hyunmi Song, Dohyeong Kim, Yujin Yang, Woong-Seob Jeong
Figure caption: Dependence of the stellar mass-to-light ratio at IRAC 3.6 μm on stellar age, derived using the pPXF method. Each column displays results from the four SPS models: E-MILES, BC03, CB19, and FSPS (left- to right-hand panels). Each row represents the age dependence for spaxels grouped by metallicity: low metallicity ([Z/Z⊙] < Q1/3), medium metallicity (Q1/3 ≤ [Z/Z⊙] < Q2/3), and high metallicity ([Z/Z⊙] ≥ Q2/3) from top to bottom. Here, Q1/3 and Q2/3 correspond to the 33rd and 67th percentiles of the metallicity distribution from each SPS model. In each panel, the black solid line indicates the best-fit linear models, with the Spearman’s rank correlation coefficients (rS), slope, and scatter (standard deviation of the residuals) specified in the bottom right-hand corner. The gray dashed line represents the best-fit linear model for all spaxels across all metallicity bins, providing a reference to show deviations caused by metallicity grouping in each panel.
Paper: Resolved Stellar Mass Estimation of Nearby Late-type Galaxies for the SPHEREx Era: Dependence on Stellar Population Synthesis Models
Authors: Jeong Hwan Lee, Minjin Kim, Taehyun Kim, Hyunjin Shim, Luis C. Ho, Ho Seong Hwang, Hyunmi Song, Dohyeong Kim, Yujin Yang, Woong-Seob Jeong
Figure caption: Comparisons of stellar masses obtained from pPXF (x-axis) and values predicted by the best-fit models of a linear relation with specific luminosity (y-axis). The gray dashed lines represent the one-to-one lines. In each panel, the slopes, intercepts, and their respective scatters (standard deviation of the residuals in dex) are noted in the lower right-hand corner.
Paper: Resolved Stellar Mass Estimation of Nearby Late-type Galaxies for the SPHEREx Era: Dependence on Stellar Population Synthesis Models
Authors: Jeong Hwan Lee, Minjin Kim, Taehyun Kim, Hyunjin Shim, Luis C. Ho, Ho Seong Hwang, Hyunmi Song, Dohyeong Kim, Yujin Yang, Woong-Seob Jeong
Figure caption: Comparisons of stellar masses obtained from pPXF (y-axis) with the values predicted by the best-fit models with linear combinations of specific luminosity, SDSS g − r color, and SPHEREx color between the 1.14 and 1.17 μm bands (x-axis). The panels are organized similarly to those in Figure 11. The scatters and best-fit coefficients of models, including the slopes of specific luminosity (﹩{C}_{{\rm{log}}{L}_{\lambda }}﹩), SDSS g − r color (Cg−r), and the SPHEREx color (CS), are presented on the bottom right-hand corner of each panel.
Paper: Resolved Stellar Mass Estimation of Nearby Late-type Galaxies for the SPHEREx Era: Dependence on Stellar Population Synthesis Models
Authors: Jeong Hwan Lee, Minjin Kim, Taehyun Kim, Hyunjin Shim, Luis C. Ho, Ho Seong Hwang, Hyunmi Song, Dohyeong Kim, Yujin Yang, Woong-Seob Jeong
Figure caption: Scatter (standard deviation of the residuals in dex) of the best-fit linear model for the stellar mass (﹩{\rm{log}}\,{M}_{* }﹩) vs. luminosity relationship at specific wavelengths (﹩{\rm{log}}\,{L}_{\lambda }﹩), depending on the central wavelength of photometric bands. Gray triangles represent the scatters from the relation using observed luminosities from 2MASS JHKs and IRAC 3.6, 4.5 μm. Error bars indicate the full range of scatters for stellar masses derived from the four SPS models. The results using luminosities of 96 SPHEREx channels computed by the four SPS models are presented as blue (E-MILES), orange (BC03), brown (CB19), and red (FSPS) curves. The vertical dashed line indicates the central wavelength of the SPHEREx channel with the minimum mean scatter for the SPS models, which is 1.63 μm.
Paper: Resolved Stellar Mass Estimation of Nearby Late-type Galaxies for the SPHEREx Era: Dependence on Stellar Population Synthesis Models
Authors: Jeong Hwan Lee, Minjin Kim, Taehyun Kim, Hyunjin Shim, Luis C. Ho, Ho Seong Hwang, Hyunmi Song, Dohyeong Kim, Yujin Yang, Woong-Seob Jeong
Figure caption: Logarithmic stellar mass differences between our pPXF results and the S4G survey, as a function of age. The panels in this figure are divided by SPS models (vertically) and dust fractions from the S4G survey (fd(S4G); horizontally). The four panels (from top to bottom) show the mass differences for E-MILES, BC03, CB19, and FSPS. Each vertical column represents a distinct bin of fd(S4G): fd(S4G) < 0.1, 0.1 ≤ fd(S4G) < 0.3, 0.3 ≤ fd(S4G) < 0.5, and fd(S4G) ≥ 0.5. In each panel, median values for age bins are indicated by diamonds.
Paper: Resolved Stellar Mass Estimation of Nearby Late-type Galaxies for the SPHEREx Era: Dependence on Stellar Population Synthesis Models
Authors: Jeong Hwan Lee, Minjin Kim, Taehyun Kim, Hyunjin Shim, Luis C. Ho, Ho Seong Hwang, Hyunmi Song, Dohyeong Kim, Yujin Yang, Woong-Seob Jeong
Figure caption: Comparison of stellar masses from this study (pPXF) with those derived from the WISE scaling relations (J23). Each vertical column corresponds to a different SPS model: E-MILES (first column), BC03 (second column), CB19 (third column), and FSPS (fourth column). The gray dashed line marks where the stellar masses from pPXF and J23 coincide. Median mass differences, represented by gray solid lines, are shown across all color ranges, with circle and square symbols for each WISE color bin. The median offsets and scatter (standard deviation of the residuals) are indicated in the bottom right-hand corner of each panel.
Paper: Resolved Stellar Mass Estimation of Nearby Late-type Galaxies for the SPHEREx Era: Dependence on Stellar Population Synthesis Models
Authors: Jeong Hwan Lee, Minjin Kim, Taehyun Kim, Hyunjin Shim, Luis C. Ho, Ho Seong Hwang, Hyunmi Song, Dohyeong Kim, Yujin Yang, Woong-Seob Jeong
Figure caption: Comparisons of stellar masses obtained from the pPXF (x-axis) with the values predicted by the best-fit models with linear combinations of specific luminosity and SDSS g − r color (y-axis). The panels are organized similarly to those in Figure 11. The texts at the lower right-hand corner of each panel indicate the scatters of models and best-fit coefficients, including the slopes of specific luminosity (﹩{C}_{{\rm{log}}{L}_{\lambda }}﹩) and SDSS g − r color (Cg−r).
Paper: Resolved Stellar Mass Estimation of Nearby Late-type Galaxies for the SPHEREx Era: Dependence on Stellar Population Synthesis Models
Authors: Jeong Hwan Lee, Minjin Kim, Taehyun Kim, Hyunjin Shim, Luis C. Ho, Ho Seong Hwang, Hyunmi Song, Dohyeong Kim, Yujin Yang, Woong-Seob Jeong
Figure caption: Same as Figure A1, albeit for the difference in luminosity at IRAC 3.6 μm.
Paper: Statistical Reevaluation of the Ultra-short-period Planet Classification Boundary: Smaller Planets within 1 Day, Larger Period Ratios below 2 Days
Authors: Armaan V. Goyal, Songhu Wang
Figure caption: Orbital architectures of the 49 USP systems considered in this work. Marker sizes correspond to planetary radius, filled markers represent objects listed as confirmed within the NEA (R. L. Akeson et al. 2013), and hollow markers are associated with Kepler candidates from J. J. Lissauer et al. (2024), TESS candidates from from the revised TESS Input Catalog (K. G. Stassun et al. 2019), or the NEA’s K2 Planets and Candidates Table (R. L. Akeson et al. 2013). We observe, in accord with the literature (e.g., S. Rappaport et al. 2013; J. H. Steffen & W. M. Farr 2013), that USPs (red) are almost exclusively smaller than 2R⊕ and often exhibit wide orbital separations with respect to their non-USP companion planets (black).
Paper: Statistical Reevaluation of the Ultra-short-period Planet Classification Boundary: Smaller Planets within 1 Day, Larger Period Ratios below 2 Days
Authors: Armaan V. Goyal, Songhu Wang
Figure caption: Compared to non-USPs (black/gray), USPs (red) are smaller in size and more architecturally detached from their neighbors in a statistically significant manner. Left: The distribution of 49 USP radii exhibits a relative overdensity at very small sizes (∼1R⊕) and lacks extension beyond Rp ≈ 2R⊕ in a manner inconsistent with the 327 non-USP radii and likely representative of refractory mass loss (see Section 6.1). We generate 1000 CDFs each for the USP and non-USP population where all individual planetary radii are uniformly resampled within their associated 1σ uncertainties. Subjecting each of these bootstrapped distributions to a permutation-based implementation of the AD test (see Section 3), we find across the 1000 bootstrapping trials a median probability of pR = 0.0040 that the USP and non-USP samples are drawn from the same underlying size distribution. Right: USPs are often architecturally isolated from their companions while non-USPs almost exclusively reside in compact systems (Pi+1/Pi < 6; e.g., X.-Y. Wang et al. 2022). From the AD test, we obtain a probability ﹩{p}_{{ \mathcal P }}\lt 1{0}^{-4}﹩ that the two distributions correspond to the same population.