adsabs/AstroCLIMB huggingface dataset:
Paper: A Catalog of Distance Determinations for 5 Million Stars in LAMOST DR10
Authors: Chengqun Yang, Xiang-Xiang Xue, Chao Liu, Hao Tian, Ling Zhu, Lan Zhang
Figure caption: The cumulative probability density function (cpdf) of the absolute magnitude in the 2MASS K band (left) and Gaia G band (right) for a LAMOST DR10 star with observation ID 116242. The atmospheric parameters and their uncertainties are provided in the caption of Figure 4, and the pdf is derived from the total likelihood shown in the bottom right panel of Figure 4. The best estimate of the absolute magnitude in the K band is M50,K = 4.540 mag (50th percentile), with a lower limit of M16,K = 4.432 mag (16th percentile) and an upper limit of M84,K = 4.655 mag (84th percentile). For the G band, the best estimate is M50,G = 6.989 mag, with a lower limit of M16,G = 6.805 mag and an upper limit of M84,G = 7.181 mag.
Paper: A Catalog of Distance Determinations for 5 Million Stars in LAMOST DR10
Authors: Chengqun Yang, Xiang-Xiang Xue, Chao Liu, Hao Tian, Ling Zhu, Lan Zhang
Figure caption: Distribution of relative distance uncertainties as a function of distance for LAMOST DR10 low-resolution spectra. Distances are derived from absolute magnitudes and extinction-corrected photometric magnitudes in the corresponding band, with the 2MASS K band shown on the left and the Gaia G band on the right. The distances d16, d50, and d84 are derived from the absolute magnitudes M84, M50, and M16, respectively. Contour lines illustrate the density distribution of these uncertainties, while histograms at the top and right of each panel show the frequency distributions of distances and relative uncertainties. The distance errors are primarily influenced by uncertainties in stellar atmospheric parameters.
Paper: A Catalog of Distance Determinations for 5 Million Stars in LAMOST DR10
Authors: Chengqun Yang, Xiang-Xiang Xue, Chao Liu, Hao Tian, Ling Zhu, Lan Zhang
Figure caption: The 1σ residual distributions of absolute magnitudes (M50 − Mtrue) for different combinations of uncertainties in atmospheric parameters as presented in Table 1, with absolute magnitudes in the K band shown on the top and in the G band on the bottom. The atmospheric parameters and true values of absolute magnitudes were derived from mock data generated using MIST isochrones. The values M50 correspond to the 50th percentile of the cumulative pdf (cpdf) of absolute magnitudes. The results indicate that uncertainties in [Fe/H] for LAMOST stars have relatively higher accuracy and contribute the least to absolute magnitude estimation, while uncertainties in ﹩\mathrm{log}(g)﹩ have the largest impact.
Paper: A Catalog of Distance Determinations for 5 Million Stars in LAMOST DR10
Authors: Chengqun Yang, Xiang-Xiang Xue, Chao Liu, Hao Tian, Ling Zhu, Lan Zhang
Figure caption: The stellar halo density and metallicity distributions in the R–z plane using distances derived from the K band (left panels) and G band (right panels). The selection effects have been corrected using the method in C. Liu et al. (2017). The top panels show the logarithmic number density of halo stars (﹩{\mathrm{log}}_{10}(N\,{\mathrm{kpc}}^{-3})﹩) with contours indicating density levels. The bottom panels show the median metallicity ([Fe/H]) distribution of halo stars. The stellar halo is more oblate and metal-rich in the inner regions, transitioning to a nearly spherical shape and being metal-poor in the outer regions.
Paper: A Catalog of Distance Determinations for 5 Million Stars in LAMOST DR10
Authors: Chengqun Yang, Xiang-Xiang Xue, Chao Liu, Hao Tian, Ling Zhu, Lan Zhang
Figure caption: Gaia parallaxes (ϖ) as a function of the reciprocal of distance (1/d50) derived from the K band (top panels) and G band (bottom panels). The black dashed lines represent the 1:1 ratio, while the red dashed lines show the fitted line using linear regression. For almost the entire data set (left panels), there is good consistency between our results and Gaia parallaxes. For parallaxes less than 1 mas (middle panels), distances derived from the K and G bands are underestimated by approximately 5% and 10%, respectively. For parallaxes less than 0.25 mas (right panels), distances derived from the K and G bands are overestimated by around 9% and 7%, respectively.
Paper: A Catalog of Distance Determinations for 5 Million Stars in LAMOST DR10
Authors: Chengqun Yang, Xiang-Xiang Xue, Chao Liu, Hao Tian, Ling Zhu, Lan Zhang
Figure caption: Distribution of derived distances and relative uncertainties for LAMOST DR10 low-resolution spectra in the K band (left panel) and G band (right panel). The gray histogram represents the number of spectra as a function of the best-estimated distance (d50), while the orange dots show the median relative distance uncertainty (d84 − d16)/(2d50) in each distance bin. The typical relative uncertainty is around 5% at ∼1 kpc, increasing to 17% at 20 kpc, then decreasing to 10%–15% for distances greater than 50 kpc.
Paper: FAST Drift Scan Survey for H I Intensity Mapping. II. Stacking-based Beam Construction of the 19-feed Array at 1.4 GHz
Authors: Xinyang Zhao, Yichao Li, Wenxiu Yang, Furen Deng, Yougang Wang, Fengquan Wu, Xin Wang, Xiaohui Sun, Xin Zhang, Xuelei Chen
Figure caption: Top panels: the constructed beam pattern with the first 23 orders of ZP modes. All the beam patterns are rotated to the 19FA frame. The δH- and δV-axes represent the separation angle in the H − V axes with respect to the beam center. Bottom panels: the corresponding ZP fitting coefficients shown as the function of Noll indices. The filled markers denote positive coefficients and the empty markers indicate negative coefficients. The colors mark different angular frequencies m. The horizontal dashed line indicates 1% of the maximum fitting coefficient.
Paper: FAST Drift Scan Survey for H I Intensity Mapping. II. Stacking-based Beam Construction of the 19-feed Array at 1.4 GHz
Authors: Xinyang Zhao, Yichao Li, Wenxiu Yang, Furen Deng, Yougang Wang, Fengquan Wu, Xin Wang, Xiaohui Sun, Xin Zhang, Xuelei Chen
Figure caption: The stacked beam patterns for four different beams (Beam01, Beam02, Beam08, and Beam19) were obtained from the data between 1375 and 1425 MHz. The three columns represent the data from three different sources: FATHOMER (first column), CRAFTS (second column), and a combination of both (third column). Each row corresponds to a unique beam, with each beam having a distinct distance from the central beam center.
Paper: FAST Drift Scan Survey for H I Intensity Mapping. II. Stacking-based Beam Construction of the 19-feed Array at 1.4 GHz
Authors: Xinyang Zhao, Yichao Li, Wenxiu Yang, Furen Deng, Yougang Wang, Fengquan Wu, Xin Wang, Xiaohui Sun, Xin Zhang, Xuelei Chen
Figure caption: The residual histogram distribution of all the beams in the same beam subset, i.e., the center beam, inner-circle beams, middle-circle beams, and outer-circle beams. The residuals for the ZP model are shown in green (left side of the violin plot) and residuals for the Gaussian model are shown in blue (right side of the violin plot). The left panel shows the residuals within the main beam size, i.e., ρ < θFWHM; while the right panel shows the residuals of the side lobe, i.e., θFWHM ≤ ρ < 2θFWHM.
Paper: FAST Drift Scan Survey for H I Intensity Mapping. II. Stacking-based Beam Construction of the 19-feed Array at 1.4 GHz
Authors: Xinyang Zhao, Yichao Li, Wenxiu Yang, Furen Deng, Yougang Wang, Fengquan Wu, Xin Wang, Xiaohui Sun, Xin Zhang, Xuelei Chen
Figure caption: The positions of the feeds in the frame of the FAST L-band 19FA. The circles are the FAST beams with the beam size ﹩2.^{\prime} 9﹩. The center, inner-circle, middle-circle, and outer-circle beams are shown in red, blue, green, and black, respectively. The cyan dashed line with an arrow indicates the drift scanning direction along R.A.
Paper: FAST Drift Scan Survey for H I Intensity Mapping. II. Stacking-based Beam Construction of the 19-feed Array at 1.4 GHz
Authors: Xinyang Zhao, Yichao Li, Wenxiu Yang, Furen Deng, Yougang Wang, Fengquan Wu, Xin Wang, Xiaohui Sun, Xin Zhang, Xuelei Chen
Figure caption: The residuals of the measured beam pattern and the fitting models. These residuals are divided by the main lobe peak value of fitting models. The top panels show the residuals for the Gaussian model while the bottom panels show the residuals for the ZP model. From the left to the right columns, there are the residuals for Beam01, Beam02, Beam19, and Beam08, which are examples of the subset of the center beam, inner-circle beams, middle-circle beams, and outer-circle beams.
Paper: FAST Drift Scan Survey for H I Intensity Mapping. II. Stacking-based Beam Construction of the 19-feed Array at 1.4 GHz
Authors: Xinyang Zhao, Yichao Li, Wenxiu Yang, Furen Deng, Yougang Wang, Fengquan Wu, Xin Wang, Xiaohui Sun, Xin Zhang, Xuelei Chen
Figure caption: The stacked beam patterns for four different beams (Beam01, Beam02, Beam08, and Beam19) were obtained from the data between 1375 and 1425 MHz. The three columns represent the polarization results for XX (vertical), YY (horizontal), and Stokes I (total intensity), respectively. Each row corresponds to a unique beam, with each beam having a distinct distance from the central beam center.
Paper: FAST Drift Scan Survey for H I Intensity Mapping. II. Stacking-based Beam Construction of the 19-feed Array at 1.4 GHz
Authors: Xinyang Zhao, Yichao Li, Wenxiu Yang, Furen Deng, Yougang Wang, Fengquan Wu, Xin Wang, Xiaohui Sun, Xin Zhang, Xuelei Chen
Figure caption: The beam pattern constructed with ZP mode of different angular frequency m, i.e., the beam pattern constructed with ZP modes of m = 0, m = ±1, and m = ±2 are shown in the top, middle, and bottom rows, respectively.
Paper: FAST Drift Scan Survey for H I Intensity Mapping. II. Stacking-based Beam Construction of the 19-feed Array at 1.4 GHz
Authors: Xinyang Zhao, Yichao Li, Wenxiu Yang, Furen Deng, Yougang Wang, Fengquan Wu, Xin Wang, Xiaohui Sun, Xin Zhang, Xuelei Chen
Figure caption: The histogram distribution of source number counts for the two source isolating methods. The straightforward isolating method result is shown in blue and the flux-weighted isolating method result is in orange. The left panel shows the results of the FATHOMER data set and the right panel shows the results of the CRAFTS data set, respectively.
Paper: FAST Drift Scan Survey for H I Intensity Mapping. II. Stacking-based Beam Construction of the 19-feed Array at 1.4 GHz
Authors: Xinyang Zhao, Yichao Li, Wenxiu Yang, Furen Deng, Yougang Wang, Fengquan Wu, Xin Wang, Xiaohui Sun, Xin Zhang, Xuelei Chen
Figure caption: The noise-filtered beam pattern of all the 19 beams of the FAST L-band feed array. The beam patterns are rotated to align with the 19FA frame. The positions of the beams correspond to their projected pointing direction in the sky. The yellow, green, and blue contours represent the 50%, 10%, and 1% of maximum response value at the beam center.
Paper: FAST Drift Scan Survey for H I Intensity Mapping. II. Stacking-based Beam Construction of the 19-feed Array at 1.4 GHz
Authors: Xinyang Zhao, Yichao Li, Wenxiu Yang, Furen Deng, Yougang Wang, Fengquan Wu, Xin Wang, Xiaohui Sun, Xin Zhang, Xuelei Chen
Figure caption: The stacked beam profiles along the radial (top panel) and tangential (bottom panel) directions of the 19FA frame. δR and δT axes indicate the separation angle with respect to the beam center along the radial and tangential directions, respectively. The beam profiles for different beam subsets are shown in different colors. The central beam profile is constructed by circular averaging of the center beam pattern and it is the same for the radial and tangential profile. The Gaussian profile is assumed to have θFWHM is ﹩2.^{\prime} 9﹩, the prior angular resolution of FAST at 1400 MHz.
Paper: FAST Drift Scan Survey for H I Intensity Mapping. II. Stacking-based Beam Construction of the 19-feed Array at 1.4 GHz
Authors: Xinyang Zhao, Yichao Li, Wenxiu Yang, Furen Deng, Yougang Wang, Fengquan Wu, Xin Wang, Xiaohui Sun, Xin Zhang, Xuelei Chen
Figure caption: The main beam efficiency of 19 beams. The x-axis represents the distance to the feed array center normalized with the radius of the inner circle. The main beam efficiency of the center beam, inner-circle beams, middle-circle beams, and the outer-circle beams are shown with x = 0, 1, ﹩\sqrt{3}﹩, and 2, respectively. The red error bars indicate the mean and standard deviation of the main beam efficiency across the beams in the same subset.
Paper: FAST Drift Scan Survey for H I Intensity Mapping. II. Stacking-based Beam Construction of the 19-feed Array at 1.4 GHz
Authors: Xinyang Zhao, Yichao Li, Wenxiu Yang, Furen Deng, Yougang Wang, Fengquan Wu, Xin Wang, Xiaohui Sun, Xin Zhang, Xuelei Chen
Figure caption: The beam pattern stacked with the beam in the subset of inner-circle (left panel), middle-circle (middle panel), and outer-circle (right panel) beams. The horizontal and vertical black dashed lines indicate the radial and tangential direction of the 19FA frame, respectively.
Paper: Erratum: “Candidate RR Lyrae Associated with the Ultrafaint Dwarf Galaxy Aquarius III” (2025, AJ, 169, 156)
Authors: Chow-Choong Ngeow, Anupam Bhardwaj
Figure caption: Corrected Figure 2 of C.-C. Ngeow & A. Bhardwaj (2025). The cyan contours represent {1, 2, 3, 4} × rh, where rh is the half-light radius of Aquarius III.
Paper: [PK2008] HalphaJ115927 and IGR J14091-6108: Two New Intermediate Polars Above the Period Gap
Authors: Arti Joshi
Figure caption: TESS power spectrum of H115927, with the inset panel representing a zoomed-in plot of the lower-frequency region. The significant frequencies observed in the power spectrum are marked.
Paper: [PK2008] HalphaJ115927 and IGR J14091-6108: Two New Intermediate Polars Above the Period Gap
Authors: Arti Joshi
Figure caption: TESS light curve of H115927.
Paper: [PK2008] HalphaJ115927 and IGR J14091-6108: Two New Intermediate Polars Above the Period Gap
Authors: Arti Joshi
Figure caption: Orbital-and-spin phase-folded light curves of IGRJ14091 with a phase bin of 0.05.
Paper: [PK2008] HalphaJ115927 and IGR J14091-6108: Two New Intermediate Polars Above the Period Gap
Authors: Arti Joshi
Figure caption: Time-resolved power spectra of H115927 computed using a 1 day wide moving window across the entire data set of the TESS observations near Ω, ω − Ω, and ω frequency regions.
Paper: [PK2008] HalphaJ115927 and IGR J14091-6108: Two New Intermediate Polars Above the Period Gap
Authors: Arti Joshi
Figure caption: Spin-and-orbital period distribution of the confirmed IPs compiled by Mukai’s catalog. Light green symbols denote propeller systems, golden circles represent low-luminosity IPs. The symbol star represents H115927 and IGRJ14091 from the present study.
Paper: [PK2008] HalphaJ115927 and IGR J14091-6108: Two New Intermediate Polars Above the Period Gap
Authors: Arti Joshi
Figure caption: TESS power spectrum of IGRJ14091 obtained from 120 s cadence TESS data, with inset panels representing zoomed-in plots of the ω and Ω frequency regions. The significant frequencies observed in the power spectrum are marked.
Paper: [PK2008] HalphaJ115927 and IGR J14091-6108: Two New Intermediate Polars Above the Period Gap
Authors: Arti Joshi
Figure caption: Top-to-bottom panels exhibit the phase-folded light curve variations at the longest signal (5.66 days), followed by the beat, spin, and orbital periods of H115927 with a phase bin of 0.05.
Paper: [PK2008] HalphaJ115927 and IGR J14091-6108: Two New Intermediate Polars Above the Period Gap
Authors: Arti Joshi
Figure caption: Spin-pulse profiles of H115927 obtained from one-day TESS observations, shown for both nonnormalized (top) and normalized (bottom) data, with a phase bin of 0.05.
Paper: [PK2008] HalphaJ115927 and IGR J14091-6108: Two New Intermediate Polars Above the Period Gap
Authors: Arti Joshi
Figure caption: Time-resolved power spectra of IGRJ14091 computed using a 1 day wide moving window across the entire data set of the TESS observations near 2Ω and ω frequency regions.
Paper: [PK2008] HalphaJ115927 and IGR J14091-6108: Two New Intermediate Polars Above the Period Gap
Authors: Arti Joshi
Figure caption: Orbital-pulse profiles of IGRJ14091 obtained from one-day TESS observations, shown for both nonnormalized (top) and normalized (bottom) data, with a phase bin of 0.05.
Paper: [PK2008] HalphaJ115927 and IGR J14091-6108: Two New Intermediate Polars Above the Period Gap
Authors: Arti Joshi
Figure caption: TESS light curve of IGRJ14091.
Paper: The Local Ultraviolet to Infrared Treasury. II. Refining Star Formation Histories of 10 Metal-poor Dwarf Galaxies with Simultaneous UV-optical Two-CMD Fitting
Authors: Yumi Choi, Karoline M. Gilbert, Benjamin F. Williams, Daniel R. Weisz, Evan D. Skillman, Julianne J. Dalcanton, Kristen B. W. McQuinn, Andrew E. Dolphin, Giada Pastorelli, Martha L. Boyer, Karl D. Gordon, Léo Girardi, Maude Gull
Figure caption: SagDIG as an example to illustrate our photometric quality cuts. The left column panels, from top to bottom, display the spatial distribution and optical CMD of sources that pass the default GST cuts in optical filters, and the UV CMD for sources that pass the GST cuts in UV filters. The dashed lines on the spatial maps indicate the overlapping area between optical and UV images, where SFHs are derived. The middle column shows the same data with an additional cut to remove diffraction spike artifacts (DGST cuts), which are position-based and applied across all filters. The right column shows the spatial distribution of sources excluded by DGST cuts, highlighting the location of diffraction spike artifacts in the optical and UV CMDs, respectively. Key evolutionary phases are annotated in the DGST cut-applied optical and UV CMDs. MW contaminants are noticeable in SagDIG due to its proximity to the Galactic Plane (b = −16﹩\mathop{.}\limits^{\unicode{x000B0}}﹩2879), whereas the other nine galaxies, located at higher Galactic latitudes, exhibit little to no MW contamination in their CMDs.
Paper: The Local Ultraviolet to Infrared Treasury. II. Refining Star Formation Histories of 10 Metal-poor Dwarf Galaxies with Simultaneous UV-optical Two-CMD Fitting
Authors: Yumi Choi, Karoline M. Gilbert, Benjamin F. Williams, Daniel R. Weisz, Evan D. Skillman, Julianne J. Dalcanton, Kristen B. W. McQuinn, Andrew E. Dolphin, Giada Pastorelli, Martha L. Boyer, Karl D. Gordon, Léo Girardi, Maude Gull
Figure caption: SFRs and distances for the full LUVIT sample, color-coded by their oxygen abundances. The quoted SFRs are calculated from extinction-corrected FUV measurements (I. D. Karachentsev et al. 2013), except for UGC 8508, which lacks GALEX FUV data and instead uses an Hα-based SFR as calculated by I. D. Karachentsev et al. (2013). This study focuses on the 10 galaxies observed with WFC/ACS (F475W, F814W) and WFC3/UVIS (F275W, F336W). These 10 galaxies are depicted as stars and labeled with their corresponding names. For more details on the LUVIT sample, including basic properties and references, see Table 1 in Paper I.
Paper: The Local Ultraviolet to Infrared Treasury. II. Refining Star Formation Histories of 10 Metal-poor Dwarf Galaxies with Simultaneous UV-optical Two-CMD Fitting
Authors: Yumi Choi, Karoline M. Gilbert, Benjamin F. Williams, Daniel R. Weisz, Evan D. Skillman, Julianne J. Dalcanton, Kristen B. W. McQuinn, Andrew E. Dolphin, Giada Pastorelli, Martha L. Boyer, Karl D. Gordon, Léo Girardi, Maude Gull
Figure caption: Recovery fraction of our photometry as a function of color and magnitude in the UV (left panels) and optical (right panels) for the closest galaxy Leo A (top panels) and the farthest galaxy UGCA 292 (bottom panels) in our sample, respectively. Low completeness at the bright end in the optical CMDs indicates saturation due to the absence of short exposures.
Paper: The Local Ultraviolet to Infrared Treasury. II. Refining Star Formation Histories of 10 Metal-poor Dwarf Galaxies with Simultaneous UV-optical Two-CMD Fitting
Authors: Yumi Choi, Karoline M. Gilbert, Benjamin F. Williams, Daniel R. Weisz, Evan D. Skillman, Julianne J. Dalcanton, Kristen B. W. McQuinn, Andrew E. Dolphin, Giada Pastorelli, Martha L. Boyer, Karl D. Gordon, Léo Girardi, Maude Gull
Figure caption: Top panels: comparison between the observed CMDs, constructed from the stars passing the DGST cuts, and the PARSEC models for HeB stars in UGC 8508 as an example. The HeB star selection is performed in an (F275W, F475W) CMD space where upper main-sequence stars are more clearly separated from HeB stars (left column). The PARSEC isochrones span ages from log10(t/[yr]) = 6.0 to 9.0 in steps of 0.2, assuming [M/H] = −1 with AV,MW = 0.04 mag. The 10% solar metallicity is consistent with the reported oxygen abundance of the star-forming region in this galaxy (see Table 1). We plot only the HeB phase of the isochrones. The blue dashed line denotes the blue extrema of the HeB tracks, which is much redder than the observed BHeB sequence both in the optical (middle column) and UV (right column) CMDs. The error bars on the left side of each optical and UV CMD represent the average photometric uncertainties in each 0.5 mag-wide bin, as derived from ASTs. Bottom panels: same as the top panels, but overlaid with the most metal-poor PARSEC isochrones with [M/H] = −2.2, which, in fact, shows a great match to the observed blue extrema. However, this very low metallicity does not physically make sense for these young stellar populations.
Paper: The Local Ultraviolet to Infrared Treasury. II. Refining Star Formation Histories of 10 Metal-poor Dwarf Galaxies with Simultaneous UV-optical Two-CMD Fitting
Authors: Yumi Choi, Karoline M. Gilbert, Benjamin F. Williams, Daniel R. Weisz, Evan D. Skillman, Julianne J. Dalcanton, Kristen B. W. McQuinn, Andrew E. Dolphin, Giada Pastorelli, Martha L. Boyer, Karl D. Gordon, Léo Girardi, Maude Gull
Figure caption: Test results from the simulated CMD fitting. The top row presents the differences between the recovered and input SFHs for four distinct dust configurations. The recovered SFHs closely match the input SFH for ages older than 1 Gyr, so the plots are limited to a 1 Gyr lookback time. The bottom row displays the standard deviation of SFRs in each time bin, calculated from the 100 best-fit SFHs for each dust configuration. The gray line denotes the input SFH. Across all cases, the UVopt scenario consistently demonstrates reduced deviation from the input SFH on average and smaller uncertainties in the resulting SFHs compared to the Opt-only case, underscoring the enhanced precision gained by including UV data. As total dust content increases, both deviations and uncertainties also increase, though the UVopt case continues to recover the input SFH more accurately than the Opt-only case.