adsabs/AstroCLIMB huggingface dataset:
Paper: Density Fluctuation–Mach Number Scaling in Compressible, High Plasma Beta Turbulence: In Situ Space Observations and High-Reynolds Number Simulations
Authors: Riddhi Bandyopadhyay, James R. Beattie, Amitava Bhattacharjee
Figure caption: The corner plots for the two ﹩{\mathrm{log}}_{10}\delta \rho /{\rho }_{0}={\theta }_{0}{\mathrm{log}}_{10}{{ \mathcal M }}_{t}+{\mathrm{log}}_{10}{\theta }_{1}﹩ fits (shown in Equations (11) and (17)) to the MMS (a) and simulation data (b), showing that (1) within 1σ, ﹩\delta \rho /{\rho }_{0}={{ \mathcal M }}_{t}﹩, as predicted from weakly compressible turbulence theory (A. Bhattacharjee et al. 1998), and (2) that with 1σ both the MMS and simulation data agree with one another.
Paper: Mass-dependent Radial Distribution of Single and Binary Stars in the Pleiades and Their Dynamical Implications
Authors: Rongrong Liu, Zhengyi Shao, Lu Li
Figure caption: Distribution of main-sequence (MS) members in the Pleiades. Color represents the binary probability, and the symbol size denotes the stellar mass. The solid and dashed circles represent the half-mass–radius (rh) from our sample and the tidal radius (rt) from J. Alfonso & A. García-Varela (2023), respectively.
Paper: Mass-dependent Radial Distribution of Single and Binary Stars in the Pleiades and Their Dynamical Implications
Authors: Rongrong Liu, Zhengyi Shao, Lu Li
Figure caption: fb–R relation in different mass ranges within the tidal radius. Panel (a) shows the relation for all binaries. Panels (b) and (c) present the relations for low and high mass binaries separated by ﹩{{ \mathcal M }}_{{\rm{seg}}}﹩. The size and color of the symbols represent the average mass and average mass ratio in each R bin, respectively. The errors are estimated based on the Poisson fluctuation.
Paper: Mass-dependent Radial Distribution of Single and Binary Stars in the Pleiades and Their Dynamical Implications
Authors: Rongrong Liu, Zhengyi Shao, Lu Li
Figure caption: Color–magnitude diagram of stars in the Pleiades region for the Gaia magnitudes. The gray dots represent field stars. The circles are MS members of Pleiades, with color indicating the mass ratio. The red solid and dashed lines represent the empirical isochrones (derived from Table 3 of Paper I) for single and binary stars, respectively.
Paper: Mass-dependent Radial Distribution of Single and Binary Stars in the Pleiades and Their Dynamical Implications
Authors: Rongrong Liu, Zhengyi Shao, Lu Li
Figure caption: Mass function of MS members. The black, green, and orange histograms show the mass distribution of all objects, single stars, and binaries, respectively. The objects in the shaded region are incomplete. The black dashed line shows the best-fit mass function for the complete part with the format of ﹩{{ \mathcal M }}^{1-\alpha }﹩.
Paper: A New Approach to the Low-frequency Stochastic Gravitational-wave Background: Constraints from Quasars and the Astrometric Hellings–Downs Curve
Authors: Jeremy Darling
Figure caption: Generalized HD curves showing the predicted pairwise correlations of radial and angular motions produced by transverse traceless stochastic gravitational waves as a function of angular separation. The blue track shows the correlated angular motions along and perpendicular to the great circles connecting pairs of objects (Γ∥∥ and Γ⊥⊥, respectively). The orange track depicts the angular cross correlations, Γ⊥∥ and Γ∥⊥, which are expected to be null valued for all angular separations. The green line shows the canonical HD curve seen in pulsar timing that is caused by radial motions (Γzz).
Paper: A New Approach to the Low-frequency Stochastic Gravitational-wave Background: Constraints from Quasars and the Astrometric Hellings–Downs Curve
Authors: Jeremy Darling
Figure caption: Proper motion power in the four correlations (Equations (16)–(19)) vs. the angular separation of quasar pairs for a sample of 67,917 quasars. These were selected based on a proper motion amplitude uncertainty <150 μas yr−1 and show a systematic in the C∥∥ correlation (Equation (17)). The orange line shows the best fit of this systematic, described by Vμ(θ) in Equation (9), a modified version of the quasar proper motion uncertainty correlation found in Gaia eDR3 by L. Lindegren et al. (2021). The points are laterally offset a few degrees from the center of each angular separation bin for clarity. The lower histogram shows the distribution of quasar pairs, scaled by 108.
Paper: A New Approach to the Low-frequency Stochastic Gravitational-wave Background: Constraints from Quasars and the Astrometric Hellings–Downs Curve
Authors: Jeremy Darling
Figure caption: Proper motion power in parallel and perpendicular modes (blue) and mixed modes (orange) vs. the angular separation of quasar pairs for 64,879 quasars selected based on their proper motion amplitude <100 μas yr−1. The points are offset by ±1∘ from the center of each angular separation bin for clarity. The green line shows the best-fit (and nonsignificant amplitude) astrometric HD curve to the aligned correlations, (C⊥⊥ + C∥∥)/2, and the filled region shows the <95% confidence envelope. This envelope equates to 95% confidence limits on the characteristic strain hc ≤ 2.7 × 10−12 and the gravitational-wave energy density ﹩{h}_{70}^{2}{\Omega }_{\mathrm{GW}}\leqslant 0.0096﹩ at reference frequency fref = 1 yr−1. The mixed-mode measurements should be consistent with zero and provide a control on systematics. The lower histogram shows the distribution of quasar pairs, scaled by 108.
Paper: A New Approach to the Low-frequency Stochastic Gravitational-wave Background: Constraints from Quasars and the Astrometric Hellings–Downs Curve
Authors: Jeremy Darling
Figure caption: Angular correlations of quasar proper motions show significant excess power when the E- and B-mode dipoles are not removed. Top: aligned parallel and perpendicular modes (blue) and mixed modes (orange) vs. the angular separation of quasar pairs for 64,879 quasars selected for proper motion amplitude <100 μas yr−1. The points are laterally offset from the center of each angular separation bin for clarity. Middle: all four individual proper motion correlation combinations. Bottom: the distribution of quasar pairs, scaled by 108.
Paper: Fast Transients from Magnetic Disks around Nonspinning Collapsar Black Holes
Authors: Justin Bopp, Ore Gottlieb
Figure caption: Distributions for model α0ωσHR. Top panel: angular distribution of the isotropic equivalent energy of the gas at r > R⋆ shows that the polar outflows possess Eiso ≈ 1052 erg at t = 23.3 s. Middle panel: bound (orange) and unbound (blue) mass distributions show that the disk outflows unbind most of the star, leaving only a small fraction to supply for the BH mass growth. Bottom panel: histograms of the (unbound) mass (red) and energy (blue) as a function of ﹩\frac{v}{c}﹩ at t = 23.3 s reveal a large amount of energy that is uniformly distributed at β < 0.3.
Paper: The Red Supergiant Progenitor of the Type II Supernova 2024abfl
Authors: Jingxiao Luo, Lifu Zhang, Bing-Qiu Chen, Qiyuan Cheng, Boyang Guo, Jiao Li, Yanjun Guo, Jianping Xiong, Xiangcun Meng, Xuefei Chen, Zhengwei Liu, Zhanwen Han
Figure caption: The zoomed-in cutout of the SN 2024abfl location. The upper left image is from Legacy Sky Survey DR10. The lower left image is a color preview of HST data, which shows the spiral arm and dust lanes around SN 2024abfl. On the right is the F555W+F606W/F814W color composite image centered on the location of SN 2024abfl. The red and cyan dashed circles represent the location of SN 2024abfl reported by the Zwicky Transient Facility and the ATLAS team, respectively. The white dashed circle represents the location of SN 2018zd reported by GaiaAlerts. The radius of the dashed circles is 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩25. The FOV of this cutout is 15﹩\mathop{.}\limits^{\unicode{x02033}}﹩85 by 15﹩\mathop{.}\limits^{\unicode{x02033}}﹩85. F555W and F606W are colored in blue; F814W is colored in orange.
Paper: Fast Transients from Magnetic Disks around Nonspinning Collapsar Black Holes
Authors: Justin Bopp, Ore Gottlieb
Figure caption: Meridional (top) and equatorial (bottom) maps at the time of a flux eruption (﹩\hat{y}\gt 0﹩) in the innermost ∼2 × 107 cm. The logarithm of the mass density (panels (a) and (b)) and magnetization (panels (c) and (d)) maps show the buildup of magnetic flux and the low-density region associated with it in the disk (bottom panels), leading to vertical outflows (top). The white arrows in panel (a) represent velocity streamlines, while the white lines in panel (c) represent magnetic field lines. Panels (e) and (f) display the power of the outflows in the ﹩\hat{z}﹩ direction, demonstrating that the bulk of the flux originates from the eruption. We note that the high magnetization connected to the nonspinning BH in panel (c) contains no energy, and originates from the floor values in the code.
Paper: Fast Transients from Magnetic Disks around Nonspinning Collapsar Black Holes
Authors: Justin Bopp, Ore Gottlieb
Figure caption: Top: the bolometric luminosity (blue) and temperature (orange) as functions of observed time (bottom horizontal axis) and emitting shell velocity (top horizontal axis). Bottom: absolute (left vertical axis) and apparent (right vertical axis) AB magnitudes at 200 Mpc in various UV/optical bands. The dashed lines indicate the approximate 5σ point source limiting magnitudes for the Rubin Observatory bands: u (8.4 × 1014 Hz), r (4.9 × 1014 Hz), y (3.0 × 1014 Hz), and ULTRASAT/UVEX NUV (1.2 × 1015 Hz) band.
Paper: The Red Supergiant Progenitor of the Type II Supernova 2024abfl
Authors: Jingxiao Luo, Lifu Zhang, Bing-Qiu Chen, Qiyuan Cheng, Boyang Guo, Jiao Li, Yanjun Guo, Jianping Xiong, Xiangcun Meng, Xuefei Chen, Zhengwei Liu, Zhanwen Han
Figure caption: Progenitor of SN 2024abfl on the CMD. The background dots are nearby stars in its host galaxy. The position of the progenitor is shown as the blue dot with error bars. If shifted back along the direction of extinction vector AF814W,host ∼ 0.1 indicated by the NaID absorption, then the progenitor would be at the green dot. The red dashed line represents the center line of the RSG branch in the host galaxy. The orange dots are stars used to calculate the position of RSG branch. The blue dashed line shows the direction of movement if one tries to shift the progenitor back to the RSG branch along the antidirection of the extinction vector.
Paper: Fast Transients from Magnetic Disks around Nonspinning Collapsar Black Holes
Authors: Justin Bopp, Ore Gottlieb
Figure caption: 3D rendering of the logarithm of the magnetization in model a0ωσHR at t = 23.3 s. Massive outflows moving at v ≈ 0.15c (red) unbind faster, lighter ejecta traveling at v ≲ 0.4c, forming a double-lobed structure (blue). The star’s original radius is outlined by the white dotted sphere.
Paper: The Red Supergiant Progenitor of the Type II Supernova 2024abfl
Authors: Jingxiao Luo, Lifu Zhang, Bing-Qiu Chen, Qiyuan Cheng, Boyang Guo, Jiao Li, Yanjun Guo, Jianping Xiong, Xiangcun Meng, Xuefei Chen, Zhengwei Liu, Zhanwen Han
Figure caption: Light curve of SN 2024abfl progenitor candidate.
Paper: The Red Supergiant Progenitor of the Type II Supernova 2024abfl
Authors: Jingxiao Luo, Lifu Zhang, Bing-Qiu Chen, Qiyuan Cheng, Boyang Guo, Jiao Li, Yanjun Guo, Jianping Xiong, Xiangcun Meng, Xuefei Chen, Zhengwei Liu, Zhanwen Han
Figure caption: 3﹩\mathop{.}\limits^{\unicode{x02033}}﹩2 by 3﹩\mathop{.}\limits^{\unicode{x02033}}﹩2 cutouts centered on the SN 2024abfl location. The cutouts in the upper row are from the F814W observations. The cutouts in the lower row are from the F555W and F606W observations.
Paper: Spectral Diversity of DiSCo’s TNOs Revealed by JWST: Early Sculpting and Late Irradiation
Authors: R. Brunetto, E. Hénault, S. Cryan, N. Pinilla-Alonso, J. P. Emery, A. Guilbert-Lepoutre, B. J. Holler, L. T. McClure, T. G. Müller, Y. Pendleton, A. C. de Souza-Feliciano, J. Stansberry, W. Grundy, N. Peixinho, G. Strazzulla, M. T. Bannister, D. Cruikshank, B. Harvison, J. Licandro, V. Lorenzi, M. N. de Prá, C. Schambeau
Figure caption: (a) The collection of DiSCo Cliff-type spectra, compared to Huya, Double-Dip Varda, and Bowl 2012 DR30, normalized at 2.6 μm and offset by 0.5 for clarity. In all figures, the TNOs are labeled by their ObsID (Table A1). The spectrum of ID49 2001 QY297 was impacted by a NIRSpec electrical short and is unexploitable beyond 2.7 μm, but the NIR spectral slopes classify it as a Cliff2-TNO (Figure 3(b)). (b) Three example Cliff1, Cliff2-Eccentric, and Cliff2-ColdCl objects compared to the spectrum of a tholin rich in C–H and N–H groups (D. Nna-Mvondo et al. 2013), a Hapke model of a mixture of methanol and amorphous carbon, a laboratory transmission spectrum of pure methanol, a mixture of H2O:CH3OH:CO2 = 0.9:1.4:1 at 67K reported by P. Ehrenfreund et al. (1999), a lab spectrum of ion-irradiated methanol (dose of 50 ± 10 eV/CH3OH molecule), and a model of a stratified surface with a decreasing fraction of irradiated methanol from the surface down to 1.5 mm; see Section 4. We saturated the optical depth of the lab measurements to highlight the different molecular absorptions. The ratio of the average Cliff1/Cliff2 is also shown (excluding 2004 PG115), offset by −0.2. All other spectra are offset by 0.5 for clarity. (c) Expansion of the short wavelength range. Vertical lines in panels (b) and (c) guide the eye at some features of interest.
Paper: Spectral Diversity of DiSCo’s TNOs Revealed by JWST: Early Sculpting and Late Irradiation
Authors: R. Brunetto, E. Hénault, S. Cryan, N. Pinilla-Alonso, J. P. Emery, A. Guilbert-Lepoutre, B. J. Holler, L. T. McClure, T. G. Müller, Y. Pendleton, A. C. de Souza-Feliciano, J. Stansberry, W. Grundy, N. Peixinho, G. Strazzulla, M. T. Bannister, D. Cruikshank, B. Harvison, J. Licandro, V. Lorenzi, M. N. de Prá, C. Schambeau
Figure caption: The areas of (a) the 2.7 μm band (CO2), (b) the large 3 μm band (O–H, N–H), (c) the large 3.4 μm band (C–H), and (d) the 2.5 μm band for Double-Dip and Cliff-TNOs, as a function of the 2.27 μm band area (CH3OH and other organics). (e) The 3 μm band area as a function of the 2.7 μm band area. (f) The 2 μm band area against its peak position, with vertical gray areas showing the peak position of pure amorphous and crystalline water ice (from R. M. Mastrapa et al. 2008) and water produced after irradiation of methanol (from R. Brunetto et al. 2006 and this work). TNOs are labeled by their ObsID (Table A1). TNO ID49 2001 QY297 is not included because its spectrum was too noisy to perform reliable calculations of band areas. ID3 Huya and ID20 2004 PG115 are represented by gray data points. Note that all panels except panel (c) can significantly discriminate between Cliff1 and Cliff2. Panels (a), (d), and (e) can also marginally discriminate Cliff2-Eccentric from Cliff2-ColdCl (see also Figure 4). Panel (f) also includes the Bowl-TNOs to show that the position of Cliff1 is blueshifted.
Paper: Subclustering and Star Formation Efficiency in Three Protoclusters in the Central Molecular Zone
Authors: Suinan Zhang, 遂楠 张, Xing Lu, 行 吕, Adam Ginsburg, Nazar Budaiev, Yu Cheng, Hauyu Baobab Liu, Tie Liu, Qizhou Zhang, Keping Qiu, Siyi Feng, Thushara Pillai, Xindi Tang, Elisabeth A. C. Mills, Qiuyi Luo, Shanghuo Li, Namitha Issac, Xunchuan Liu, Fengwei Xu, Jennifer Wallace, Xiaofeng Mai, Yan-Kun Zhang, Cara Battersby, Steven N. Longmore, Zhiqiang Shen
Figure caption: Brightness temperature images overlaid with white contours outlining the Submillimeter Array (SMA) 1.3 mm continuum from X. Lu et al. (2019b) at the level of 3﹩{\sigma }_{\mathrm{SMA}}^{1.3\,\mathrm{mm}}﹩, where ﹩{\sigma }_{\mathrm{SMA}}^{1.3\,\mathrm{mm}}=3﹩ mJy beam−1. Values lower than 10σ are shown in a linear grayscale, while those higher than 10σ are highlighted in a logarithmic colorscale. The locations of H2O masers, Class II CH3OH masers, and H II regions are marked in cyan, green, and red (X. Lu et al. 2019a, 2019b). The black dotted circles indicate 20% of the primary-beam response for 20 km s−1 C1 and C4 and 50% for Sgr C C4. The right panels are the zoomed-in views of subregions outlined by the black squares in the left panels. The squares are labeled from “A” to “F,” with a size of ∼3″ for A, B, C, and D and ∼5″ for E and F. The crosses mark the locations of the fragments in the “robust” catalog. The synthesized beams of the SMA 1.3 mm continuum and the ALMA 1.3 mm continuum are shown in the bottom left corners of the left and right panels, respectively.
Paper: Subclustering and Star Formation Efficiency in Three Protoclusters in the Central Molecular Zone
Authors: Suinan Zhang, 遂楠 张, Xing Lu, 行 吕, Adam Ginsburg, Nazar Budaiev, Yu Cheng, Hauyu Baobab Liu, Tie Liu, Qizhou Zhang, Keping Qiu, Siyi Feng, Thushara Pillai, Xindi Tang, Elisabeth A. C. Mills, Qiuyi Luo, Shanghuo Li, Namitha Issac, Xunchuan Liu, Fengwei Xu, Jennifer Wallace, Xiaofeng Mai, Yan-Kun Zhang, Cara Battersby, Steven N. Longmore, Zhiqiang Shen
Figure caption: (a) Distribution of physical properties. The main plot shows the radii vs. masses of the fragments. The marginal plots show the histograms of radii and masses on the top and right panels, respectively. The fragments in different clumps are color-coded. The vertical dotted lines mark masses corresponding to 5σ. The horizontal dotted lines show effective radii of the synthesized beams. The black solid lines show constant column densities of 1024 and 1025 cm−2. The gray solid lines show constant number densities of 108 and 109 cm−3. (b)–(d) Distribution of deprojected separations of the three clumps. Each panel shows deprojected separations in red sticks along with the corresponding histogram and the kernel density estimate. The vertical lines represent the thermal Jeans length.
Paper: Subclustering and Star Formation Efficiency in Three Protoclusters in the Central Molecular Zone
Authors: Suinan Zhang, 遂楠 张, Xing Lu, 行 吕, Adam Ginsburg, Nazar Budaiev, Yu Cheng, Hauyu Baobab Liu, Tie Liu, Qizhou Zhang, Keping Qiu, Siyi Feng, Thushara Pillai, Xindi Tang, Elisabeth A. C. Mills, Qiuyi Luo, Shanghuo Li, Namitha Issac, Xunchuan Liu, Fengwei Xu, Jennifer Wallace, Xiaofeng Mai, Yan-Kun Zhang, Cara Battersby, Steven N. Longmore, Zhiqiang Shen
Figure caption: Cumulative distributions of dust mass (left column) and “luminosity” (right column; given by flux[mJy] × distance2 [kpc2]) of the fragments in our sample and their counterparts of similar sizes in Sgr B2 M and N (N. Budaiev et al. 2024). The shaded areas indicate the ranges of errors. The upper panels show complete distributions while the bottom panels show the cropped distributions.
Paper: Calibration of Complementary Metal-oxide-semiconductor Sensor–based Photometry to a Few-millimagnitude Precision: The Case of the Mini-SiTian Array
Authors: Kai Xiao, Yang Huang, Haibo Yuan, Zhirui Li, Yongkang Sun, Timothy C. Beers, Min He, Jifeng Liu, Hong Wu, Yongna Mao, Bowen Huang, Mingyang Ma, Chuanjie Zheng, Hongrui Gu, Beichuan Wang, Lin Yang, Shuai Xu
Figure caption: Upper-left panel: the final fitting residuals against calibrated MST GMST magnitude from one observation on 2023 January 18. Additionally, the panel includes red solid and red dashed curves representing the dependence of the median value and standard deviation on the MST-calibrated magnitude, respectively. Upper-right panel: similar to the upper-left panel, but showing the dependence on Gaia color instead. Bottom-left panel: the variation in dispersion for 79 repeat observations of a common source on 2023 January 18, plotted against the calibrated magnitude GMST. The pink, blue, and green dotted–dashed curves represent scintillation noise, photon noise, and sky noise, respectively. Bottom-right panel: similar to the bottom-left panel, but includes over 3100 observations from more than 30 different nights. The red dashed line represents a precision of 4 mmag. The black dotted–dashed curves and gray curves in the bottom panels represent theoretically calculated magnitude errors, as a function of magnitude and median values, respectively.
Paper: Calibration of Complementary Metal-oxide-semiconductor Sensor–based Photometry to a Few-millimagnitude Precision: The Case of the Mini-SiTian Array
Authors: Kai Xiao, Yang Huang, Haibo Yuan, Zhirui Li, Yongkang Sun, Timothy C. Beers, Min He, Jifeng Liu, Hong Wu, Yongna Mao, Bowen Huang, Mingyang Ma, Chuanjie Zheng, Hongrui Gu, Beichuan Wang, Lin Yang, Shuai Xu
Figure caption: Taking 20230118 as an example, showing the process of correcting spatial-dependent systematic errors. Upper-left panel: distribution of the magnitude offsets after color-dependent systematic errors correction from the first observation. Upper-right panel: distribution of the residuals after applying a second-order two-dimensional polynomial fitting to the magnitude offsets, which were previously corrected for the color-dependent systematics, from the same observation. Bottom-left panel: distribution of the medium-scale flat-field structure from all the 79 observations. Bottom-right panel: same as the bottom-left panel, but after the correction for medium-scale flat-field structure. A color bar indicating the residuals is shown at the right.
Paper: Calibration of Complementary Metal-oxide-semiconductor Sensor–based Photometry to a Few-millimagnitude Precision: The Case of the Mini-SiTian Array
Authors: Kai Xiao, Yang Huang, Haibo Yuan, Zhirui Li, Yongkang Sun, Timothy C. Beers, Min He, Jifeng Liu, Hong Wu, Yongna Mao, Bowen Huang, Mingyang Ma, Chuanjie Zheng, Hongrui Gu, Beichuan Wang, Lin Yang, Shuai Xu
Figure caption: Synthetic transmission curves for the MST GMST (yellow region), RMST (cyan), gMST (dark blue), rMST (green), and iMST (red) filters. The atmospheric transmission curve (solid black curve), filter transmission curves (colored curves), and quantum efficiency (dashed black curve) are also shown, along with the filter passbands. The influence of the telescope’s optical system is not considered in this work. To clearly illustrate the shapes of the transmission curves across different passbands, the filter transmission curves have been divided into two panels.
Paper: Calibration of Complementary Metal-oxide-semiconductor Sensor–based Photometry to a Few-millimagnitude Precision: The Case of the Mini-SiTian Array
Authors: Kai Xiao, Yang Huang, Haibo Yuan, Zhirui Li, Yongkang Sun, Timothy C. Beers, Min He, Jifeng Liu, Hong Wu, Yongna Mao, Bowen Huang, Mingyang Ma, Chuanjie Zheng, Hongrui Gu, Beichuan Wang, Lin Yang, Shuai Xu
Figure caption: Light curves from randomly selected stars—both nonvariable (first row) and variable (other rows)—are presented based on over 3100 observations, illustrating varying brightness levels. Median values are plotted with black dashed–dotted lines. For nonvariable stars, the standard deviation of the magnitude is estimated using a Gaussian fitting approach and indicated in each panel. To analyze a variable source, we first obtain the median of the light curve, then linearly interpolate to derive model values for all points, and finally use Gaussian fitting to determine the standard deviation of the differences between model values and measured values. The standard deviation is labeled in the bottom-right corner of each panel.
Paper: Calibration of Complementary Metal-oxide-semiconductor Sensor–based Photometry to a Few-millimagnitude Precision: The Case of the Mini-SiTian Array
Authors: Kai Xiao, Yang Huang, Haibo Yuan, Zhirui Li, Yongkang Sun, Timothy C. Beers, Min He, Jifeng Liu, Hong Wu, Yongna Mao, Bowen Huang, Mingyang Ma, Chuanjie Zheng, Hongrui Gu, Beichuan Wang, Lin Yang, Shuai Xu
Figure caption: Left panel: two-dimensional second-order polynomial fitting (with six free parameters) of intrinsic color as functions of Teff and [Fe/H], for the SCR calibration sample. The black and gray curves represent results for [Fe/H] = 0 and −1, respectively, and the standard deviation of the fitting residuals are estimated with Gaussian fitting and labeled in the panel. Right panel: difference between the SCR zero-points and the MST zero-points. The zero level is denoted by the black dashed line, and the standard deviation of the residual is also provided.