adsabs/AstroCLIMB huggingface dataset:
Paper: UPdec-Webb: A Data Set for Coaddition of JWST NIRCam Images
Authors: Lei Wang, Huanyuan Shan, Lin Nie, Cheng Cheng, Fang-Ting Yuan, Qifan Cui, Guoliang Li, Yushan Xie, Dezi Liu, Yao Liu, Min Fang, Nan Li, Peng Jia, Ran Li, Fengshan Liu, Yiping Shu, Chang Jiang, Cheng-Liang Wei, Han Qu, Wen-Wen Zheng, Li-Yan Zhu, Xi Kang
Figure caption: Zoomed-in objects near the center of SMACSJ0723. The UPDC processing reveals clearer globular clusters in the Sparkler Galaxy, as shown in Tag-A. Tag-B and Tag-C display reconstructed spatial details and additional substructures in galaxies processed with UPDC software. Additionally, the gravitational lensing of a galaxy cluster results in a stretched galaxy forming a giant arc, which becomes slimmer after UPDC processing, as depicted in Tag-D.
Paper: UPdec-Webb: A Data Set for Coaddition of JWST NIRCam Images
Authors: Lei Wang, Huanyuan Shan, Lin Nie, Cheng Cheng, Fang-Ting Yuan, Qifan Cui, Guoliang Li, Yushan Xie, Dezi Liu, Yao Liu, Min Fang, Nan Li, Peng Jia, Ran Li, Fengshan Liu, Yiping Shu, Chang Jiang, Cheng-Liang Wei, Han Qu, Wen-Wen Zheng, Li-Yan Zhu, Xi Kang
Figure caption: Enhancement for spiral galaxies and a strong gravitational lens system. The UPDC reconstructed images reveal richer structural details of two spiral galaxies—red and blue (Tag-A). The peripheral structure of the red galaxy, hidden by its spikes, is now visible in the output images (Tag-B). The UPDC also helped detect a candidate for a strong gravitational lens system (L. Deng et al. 2025, in preparation) by reconstructing the background galaxies that were originally obscured by the spikes of the foreground high-brightness lens galaxy (Tag-C).
Paper: UPdec-Webb: A Data Set for Coaddition of JWST NIRCam Images
Authors: Lei Wang, Huanyuan Shan, Lin Nie, Cheng Cheng, Fang-Ting Yuan, Qifan Cui, Guoliang Li, Yushan Xie, Dezi Liu, Yao Liu, Min Fang, Nan Li, Peng Jia, Ran Li, Fengshan Liu, Yiping Shu, Chang Jiang, Cheng-Liang Wei, Han Qu, Wen-Wen Zheng, Li-Yan Zhu, Xi Kang
Figure caption: Enhancement for the details of galaxies in the SMACSJ0723 field. As shown in Tag-A, the dust at the edge of the spiral galaxy, which is originally obscured by PSF blurring in the left panel, has become discernible in the right one (the yellow belt traversing the galaxy). Two spiral arms of the spiral galaxy, which are originally blurred in the upper left, have also become very distinguishable in the right panel generated by UPDC, as indicated in Tag-B.
Paper: UPdec-Webb: A Data Set for Coaddition of JWST NIRCam Images
Authors: Lei Wang, Huanyuan Shan, Lin Nie, Cheng Cheng, Fang-Ting Yuan, Qifan Cui, Guoliang Li, Yushan Xie, Dezi Liu, Yao Liu, Min Fang, Nan Li, Peng Jia, Ran Li, Fengshan Liu, Yiping Shu, Chang Jiang, Cheng-Liang Wei, Han Qu, Wen-Wen Zheng, Li-Yan Zhu, Xi Kang
Figure caption: The photometry of crossmatched sources in the parallel field of SMACSJ0723 is compared between UPDC-iter0 and UPDC-iter5. Three panels are for three LW bands: F277W, F356W, and F444W.
Paper: UPdec-Webb: A Data Set for Coaddition of JWST NIRCam Images
Authors: Lei Wang, Huanyuan Shan, Lin Nie, Cheng Cheng, Fang-Ting Yuan, Qifan Cui, Guoliang Li, Yushan Xie, Dezi Liu, Yao Liu, Min Fang, Nan Li, Peng Jia, Ran Li, Fengshan Liu, Yiping Shu, Chang Jiang, Cheng-Liang Wei, Han Qu, Wen-Wen Zheng, Li-Yan Zhu, Xi Kang
Figure caption: The dependency of detection upon UPDC iterations. The left panel displays total detection numbers for three LW bands while the right panel shows corresponding detection growth rates, normalized to the Drizzle image's detection number (UPDC-iter0).
Paper: UPdec-Webb: A Data Set for Coaddition of JWST NIRCam Images
Authors: Lei Wang, Huanyuan Shan, Lin Nie, Cheng Cheng, Fang-Ting Yuan, Qifan Cui, Guoliang Li, Yushan Xie, Dezi Liu, Yao Liu, Min Fang, Nan Li, Peng Jia, Ran Li, Fengshan Liu, Yiping Shu, Chang Jiang, Cheng-Liang Wei, Han Qu, Wen-Wen Zheng, Li-Yan Zhu, Xi Kang
Figure caption: Normalized flux profile (left panel) and curve of growth (right panel) for a star at R.A. = 110﹩\mathop{.}\limits^{\circ }﹩865243, decl. = −73﹩\mathop{.}\limits^{\circ }﹩454731. The measurements are obtained from the coaddition of SMACSJ0723 exposures in the F200W band. On the left panel, all curves represent the flux normalized to the total flux within the circle of radius 1″ (≃67 pixels). There are several valleys in each curve, which corresponds to the minimums of the Airy pattern. Black (red) hexagons on the right panel indicate the nominal (the officially measured) encircled energy fraction at different radii. All curves on the right panel are normalized to the total flux measured on the Drizzled image within the circle of radius 120 pixels (≃1﹩\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}﹩8).
Paper: UPdec-Webb: A Data Set for Coaddition of JWST NIRCam Images
Authors: Lei Wang, Huanyuan Shan, Lin Nie, Cheng Cheng, Fang-Ting Yuan, Qifan Cui, Guoliang Li, Yushan Xie, Dezi Liu, Yao Liu, Min Fang, Nan Li, Peng Jia, Ran Li, Fengshan Liu, Yiping Shu, Chang Jiang, Cheng-Liang Wei, Han Qu, Wen-Wen Zheng, Li-Yan Zhu, Xi Kang
Figure caption: Error propagation of PSF convolution in simulation with Poisson noise. Panel (0) shows the underlying image (truth). For a Poisson distribution, the mean and variance are equal. To generate panel (1), we Poissonize the truth (panel (0)). Panel (2) represents the result of convolving the truth with a PSF (the ideal case). By taking the square root of panel (1) and convolving it with the same PSF, we obtain panel (3) (the convolved error). Squaring panel (3) gives us panel (4) (the variance). Convolution of the variance from panel (1) with the same PSF results in panel (6). Meanwhile, panels (5) and (7) represent the residuals for these two types of error propagation. This simulation indicates that calculating error propagation of PSF convolution through variance is more accurate than doing so through the error itself.
Paper: UPdec-Webb: A Data Set for Coaddition of JWST NIRCam Images
Authors: Lei Wang, Huanyuan Shan, Lin Nie, Cheng Cheng, Fang-Ting Yuan, Qifan Cui, Guoliang Li, Yushan Xie, Dezi Liu, Yao Liu, Min Fang, Nan Li, Peng Jia, Ran Li, Fengshan Liu, Yiping Shu, Chang Jiang, Cheng-Liang Wei, Han Qu, Wen-Wen Zheng, Li-Yan Zhu, Xi Kang
Figure caption: A closed binary is resolved by the UPDC in the SMACSJ0723 field. The binary is located at R.A. = 110﹩\mathop{.}\limits^{\circ }﹩845109, decl. = −73﹩\mathop{.}\limits^{\circ }﹩455443. The lower panels present a cross sectional view of the upper images along the dashed line. The binary in the left lower image is not fully resolved, but the one in the right lower image provides significant evidence.
Paper: Addressing Distribution Discrepancies in Pulsar Candidate Identification via Bayesian-neural-network-based Multimodal Incremental Learning
Authors: Yi Liu, Jing Jin, Hongyang Zhao, Zhenyi Wang, Yi Shen
Figure caption: Pulsar candidate diagnostic feature maps: profile, DM curve, subband plot, and subintegration plot.
Paper: Addressing Distribution Discrepancies in Pulsar Candidate Identification via Bayesian-neural-network-based Multimodal Incremental Learning
Authors: Yi Liu, Jing Jin, Hongyang Zhao, Zhenyi Wang, Yi Shen
Figure caption: Comparative performance of BNNs and CNNs on incremental learning tasks.
Paper: Addressing Distribution Discrepancies in Pulsar Candidate Identification via Bayesian-neural-network-based Multimodal Incremental Learning
Authors: Yi Liu, Jing Jin, Hongyang Zhao, Zhenyi Wang, Yi Shen
Figure caption: Multimodal incremental learning model based on a BNN. Profile, DM curve, subband, and subint represent the corresponding pulsar candidate diagnostic feature maps. BBBConv1D, BBBConv2D, and BBBLinear are the three basic layer types used in the model, where “BBB” stands for “Bayes By Backprop.” Prior Update and Adaptive Replay involve how the model updates its prior knowledge and integrates new learning tasks through adaptive replay, enhancing the model's memory of historical data.
Paper: Addressing Distribution Discrepancies in Pulsar Candidate Identification via Bayesian-neural-network-based Multimodal Incremental Learning
Authors: Yi Liu, Jing Jin, Hongyang Zhao, Zhenyi Wang, Yi Shen
Figure caption: Impact of varying replay data volumes on F1-scores for Task 1 and Task 2 in incremental learning.
Paper: Addressing Distribution Discrepancies in Pulsar Candidate Identification via Bayesian-neural-network-based Multimodal Incremental Learning
Authors: Yi Liu, Jing Jin, Hongyang Zhao, Zhenyi Wang, Yi Shen
Figure caption: Overview of how BCNNs differ from traditional CNNs.
Paper: Addressing Distribution Discrepancies in Pulsar Candidate Identification via Bayesian-neural-network-based Multimodal Incremental Learning
Authors: Yi Liu, Jing Jin, Hongyang Zhao, Zhenyi Wang, Yi Shen
Figure caption: Calibration curve comparing model predictions (blue line) with perfect calibration (orange dashed line).
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: A floor–scale diagram for the R.A. scaled by the ﹩\cos \delta ﹩ factor: local decimation (left) and global decimation (right). The color corresponds to the rms of the fit. Only the sources with positional errors < 0.4 mas are considered.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: A floor–scale diagram for the decl.: local decimation (left) and global decimation (right). The color corresponds to the rms of the fit. Only the sources with positional errors < 0.4 mas are considered.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: A histogram of normalized source positional errors for R.A. scaled by the ﹩\cos \delta ﹩ factor (left) and decl. (right) derived from decimation solutions. The upper red curve corresponds to the local decimation solutions. The lower green curve corresponds to the global decimation solutions. Only sources with positional errors < 0.2 mas are considered. The central blue curve is a Gaussian function shown as a reference.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: Estimates of the scale s for decl. errors from the global decimation solution with the error floor fixed to zero as a function of the mean decl. error within a sliding window [σ  l , σ  u ]. There were 1000 decl. error estimates within each window. The blue line shows the result of smoothing with B-spline.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: Estimates of the error floor from the global decimation solutions as a function of decl. for R.A. (left) and decl. (right). The thin blue line approximates them with a smoothing spline.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: Time allocation for VLBI experiments for 10 days in 2020 March. Upper (blue): 1 hr IVS intensive experiments. Middle (green): 24 hr IVS geodetic experiments. Bottom (red): an astrometric experiment. Thin vertical lines correspond to epochs of B-spline knots.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: A histogram of the final normalized source positional errors for R.A. scaled by the ﹩\delta \cos ﹩ factor (left) and decl. (right) after applying error rescaling (green points). The smooth blue curve is a Gaussian function shown as a reference.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: The distributions of sources by the logarithm of the number of observations used in the solutions in geodetic observing sessions (left) and astrometric sessions (right).
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: A histogram of the number of detected sources per band. The dual-band box shows the number of sources that have been detected in both bands simultaneously. A detected source has at least three observations that have passed the outlier detection tests.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: The distributions of the normalized arc lengths between RFC and Gaia position estimates. A Rayleigh distribution with σ = 1.0 is shown with a black thick line for reference. Left: all matching sources. Right: the data set was split into three subsets according to χ 2/ndf. Gaia variable: the green line: χ 2/ndf < 1.1, the blue line: 1.1 < χ 2/ndf < 2.0, and the red line: χ 2/ndf > 2.0. The last bin collects all the normalized arc lengths ≥ 4.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: The smoothed differences in decl. from three solutions using subsets of data as a function of decl. Left: the differences in K-band solutions. Right: the differences in dual-band solutions.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: The distributions of the normalized arc lengths between Gaia and RFC position estimates from a subset of matching sources with differently rescaled errors. A Rayleigh distribution with σ = 1.0 is shown with a black thick line for reference. The green line shows the distribution without rescaling. The blue line shows the distribution with a rescaling factor of 1.2. The red line shows the distribution with a rescaling factor of 1.4.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: The normalized distributions of position angles of the differences in source coordinates from Gaia with respect to RFC counted from the north celestial pole (green circles) for four subsets. Each subset corresponded to sources that had a certain range of the number of observations used in a solution. The green line: 3–40; the blue line: 40–80; the red line: 81–120; and the black line >120 The thin dashed red line shows a uniform distribution.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: The differences in decl. from K-band solutions when the ionospheric contribution is applied with respect to solutions when it is not applied. Left: station positions are estimated. Right: station positions are not estimated.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: The differences in source position estimates from the X-band solution with respect to the dual-band solution. Only sources with positional errors < 0.5 mas are shown. Left: the differences in R.A. scaled by ﹩\cos \delta ﹩. Right: the differences in decl.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: The differences in source position estimates from the C-band solution with respect to the dual-band solution. Only sources with positional errors < 1 mas are shown. Left: the differences in R.A. scaled by ﹩\cos \delta ﹩. Right: the differences in decl.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: The differences in source position estimates from the S-band solution with respect to the dual-band solution. Only sources with positional errors < 3 mas are shown. Left: the differences in R.A. scaled by ﹩\cos \delta ﹩. Right: the differences in decl.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: The differences in decl. from the K-band solution with respect to the dual-band solution. The thick blue line shows smoother differences. The dash black line shows 0.0.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: The distribution of the share of sources with position differences between the RFC and ICRF3 catalogs significant at a given N σ level. The upper green line corresponds to ﹩\sigma =\min ({\sigma }_{\mathrm{rfc}},{\sigma }_{\mathrm{icrf}3})﹩. The middle blue line corresponds to σ = σ rfc. The lower red line corresponds to ﹩\sigma =\max ({\sigma }_{\mathrm{rfc}},{\sigma }_{\mathrm{icrf}3})﹩.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: Example of a source that is affected by scattering in the interstellar medium. The first plot from the left: scattered image at 2.3 GHz. The second plot: image of the same source at 15.4 GHz where scattering is negligible. The third and the fourth plots show the calibrated visibility amplitude as a function of the projected baseline length. See details in T. A. Koryukova et al. (2023).
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: The distribution of RFC sources over the celestial sphere in the equatorial coordinate system. The circle size corresponds to flux density at 8 GHz (or at lower frequencies if a source was not detected at 8 GHz). The circle color corresponds to the semimajor axis of the positional error ellipse. The red line shows the Galactic plane.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: Example of an image and a plot of the correlated flux density with respect to the baseline projection length. The image presented in the left plot is the result of a convolution of the CLEAN component model and the clean beam that is represented by an elliptical Gaussian with the FWHM size shown in the left bottom corner. The first contour in the image plot is shown at the 5 times the image rms level. The correlated flux density data points presented in the right plot are calculated as an average per baseline, frequency, and scan, and the error bars account for thermal noise only.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: Left: the dependence of the median semimajor positional error ellipse on the median flux density at baselines shorter than 1000 km. Right: the dependence of the median semimajor positional error ellipse on the median flux density at baselines longer than 1000 km.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: Left: the dependence of the median source positional error on the number of scans. Right: the dependence of the median source positional error on the number of observations. The gray area denotes the range of positional errors dominated by the contribution of systematic errors. Two vertical bars denote the range of the number of scans or the number of observations in a transition zone from random error dominated to the systematic error dominated.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: Example of S-band images of sources with large differences between the RFC and ICRF3 catalogs. Left: RFC J1120−2508. Right: RFC J1308+6544.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: Left: the cumulative distribution of the number of scans per source. Right: the cumulative distribution of the number of observations per source.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: The cumulative error distributions. The upper green line: semiminor positional error ellipse axes. The lower blue line: semimajor positional error ellipse axes. Right: zoom of the area that is marked with a gray color in the left panel.
Paper: Metallicity Dependence of Giant Planets around M Dwarfs
Authors: Tianjun Gan, Christopher A. Theissen, Sharon X. Wang, Adam J. Burgasser, Shude Mao
Figure caption: The normalized SpeX spectra of 22 M dwarfs with confirmed giant planets. The data are presented in the order of stellar types derived through spectrum match (see Section 4). Three vertical gray areas mark telluric absorption features, which we excluded during the analysis. All SpeX spectra we collected are available.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: The probability to find a phase calibrator as a function of the angular distance between target and calibrator for three bands: C, X, and K. Left: zone [–40°, +90°]. The upper red curve is for the C band, the middle green curve is for the X band, and the low purple curve is for the K band. Right: zone [–90°, –40°] for the X band.
Paper: Metallicity Dependence of Giant Planets around M Dwarfs
Authors: Tianjun Gan, Christopher A. Theissen, Sharon X. Wang, Adam J. Burgasser, Shude Mao
Figure caption: Left panel: the Gaia color–magnitude diagram of 746 field M dwarfs colored by their [Fe/H], and 22 M stars with confirmed giant planets marked as orange stars. Right panel: the refined stellar masses and effective temperatures of two samples (see Section 4 for details).
Paper: Metallicity Dependence of Giant Planets around M Dwarfs
Authors: Tianjun Gan, Christopher A. Theissen, Sharon X. Wang, Adam J. Burgasser, Shude Mao
Figure caption: An example plot of spectrum match in Section 4. The black solid line is the normalized SpeX near-infrared spectrum of the target star GJ 463 while the best-match comparison spectrum taken from the IRTF library (J. T. Rayner et al. 2009) is shown in magenta. Strong atomic and molecular features are marked. The residuals (blue) are presented below.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: The RFC source density as a function of 1° wide decl. stripe zones. The black line shows the source density smoothed using B-spline. Note that the zone area in the stripes depends on ﹩\cos \delta ﹩, which affects statistics close to the poles.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: The empirical fudge factors to the a priori estimate of the probability of false association between Gaia EDR3 and the RFC catalog.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: Example VLASS images of areas in the vicinity of RFC sources. The thin green lines in the image centers show the RFC position. Left: RFC J0328+5509. Right: RFC J2137−1432. The⊕ character denotes the AT20G position.
Paper: The Radio Fundamental Catalog. I. Astrometry
Authors: L. Y. Petrov, Y. Y. Kovalev
Figure caption: The evolution of the VLBI absolute astrometry catalogs. The green circles show releases of the RFC. The blue circles show the historical VLBI position catalogs (M. H. Cohen & D. B. Shaffer 1971) followed by C. Ma et al. (1986), the IERS series of source catalogs, then ICRF1, ICRF2, and ICRF3.
Paper: Metallicity Dependence of Giant Planets around M Dwarfs
Authors: Tianjun Gan, Christopher A. Theissen, Sharon X. Wang, Adam J. Burgasser, Shude Mao
Figure caption: Metallicity distribution of the field M stars (black) and M dwarfs with giant planets (orange), either hot Jupiters (red) with a/R*≤20 or warm Jupiters (blue) with a/R* > 20. The left and right panels are the results from H- and K-band measurements. The vertical gray line in each panel marks the median [Fe/H] of the field M dwarf sample, −0.07 and 0.07 dex. The cumulative functions are shown above. Most confirmed giant planets were orbiting metal-rich M stars. The tentative bimodal distribution of [Fe/H] is likely due to Poisson noise.
Paper: Metallicity Dependence of Giant Planets around M Dwarfs
Authors: Tianjun Gan, Christopher A. Theissen, Sharon X. Wang, Adam J. Burgasser, Shude Mao
Figure caption: The cumulative [Fe/H] (top) and [M/H] (bottom) distributions from two bands of M dwarfs hosting giant planets located in three different scaled semimajor axis bins: a/R* ≤ 20, 20 < a/R* ≤ 200, and a/R* > 200. The outer cold Jupiters with a/R* > 200 tend to show a weaker preference for metallicity compared with the inner hot Jupiters with a/R* ≤ 20. The numbers listed on the left of each panel are the p-values of the K-S and A-D tests between the HJ (red) and CJ (purple) populations.