adsabs/AstroCLIMB huggingface dataset:
Paper: Discerning Misclassified Flat-spectrum Radio Quasars from Low-frequency-peaked BL Lacertae Objects
Authors: S. Liang, W. G. Yang, Y. G. Zheng, S. J. Kang
Figure caption: Spectral fitting for the quasar OP 186 at redshift z = 1.1367. The black curve shows the observed dereddened spectrum. Yellow represents the continuum model (fpl + fpoly), cyan denotes the Fe II templates (fFe II), blue corresponds to the total emission-line fit, red represents broad-line components, and green represents narrow-line components. Insets highlight detailed fits for Mg II (χ2 = 0.85) and Hβ (χ2 = 5.36), demonstrating line decomposition accuracy.
Paper: Discerning Misclassified Flat-spectrum Radio Quasars from Low-frequency-peaked BL Lacertae Objects
Authors: S. Liang, W. G. Yang, Y. G. Zheng, S. J. Kang
Figure caption: Spectral fitting for the quasar GB6 J0941+2721 at redshift z = 0.6310. The black curve shows the observed dereddened spectrum. Yellow represents the continuum model (fpl + fpoly), cyan denotes the Fe II templates (fFe II), blue corresponds to the total emission -ine fit, red represents broad-line components, and green represents narrow-line components. Insets highlight detailed fits for Mg II (χ2 = 0.85) and Hβ (χ2 = 5.36), demonstrating line decomposition accuracy.
Paper: Discerning Misclassified Flat-spectrum Radio Quasars from Low-frequency-peaked BL Lacertae Objects
Authors: S. Liang, W. G. Yang, Y. G. Zheng, S. J. Kang
Figure caption: The relationship between ﹩\mathrm{log}{L}_{\gamma }﹩ and Γγ based on a support vector machine (SVM) classification model. Red points represent LBL, while blue points correspond to FSRQ. The dashed line indicates the SVM decision boundary, separating the two classes by Γγ = −0.147logLγ + 8.819.
Paper: Discerning Misclassified Flat-spectrum Radio Quasars from Low-frequency-peaked BL Lacertae Objects
Authors: S. Liang, W. G. Yang, Y. G. Zheng, S. J. Kang
Figure caption: The spectrum of TXS 1146+189. In this figure, all the wide emission lines’ EW < 5 Å.
Paper: Discerning Misclassified Flat-spectrum Radio Quasars from Low-frequency-peaked BL Lacertae Objects
Authors: S. Liang, W. G. Yang, Y. G. Zheng, S. J. Kang
Figure caption: Spectral fitting of quasar B3 1222+438 at redshift z = 0.9576, observed at coordinates (R.A., decl.) = (186.214590, 43.588695). The top panel shows the full dereddened spectrum with black representing the observed data. Yellow represents the continuum component, cyan denotes the Fe II emission, blue represents the total emission-line profiles, and red highlights specific line fits. Key emission lines such as C III, Mg II, Hβ, and O III are labeled. The lower panels provide zoomed-in views of individual line fits for C III (left), Mg II (center), and Hβ (right), with blue lines representing the model fits. The reduced chi-square (﹩{\chi }_{r}^{2}﹩) values for each line fitting are displayed, indicating the fit quality for each component.
Paper: Discerning Misclassified Flat-spectrum Radio Quasars from Low-frequency-peaked BL Lacertae Objects
Authors: S. Liang, W. G. Yang, Y. G. Zheng, S. J. Kang
Figure caption: The spectrum of GB6 J0934+3926. This image illustrates the spectral-fitting results for the celestial object GB6 J0934+3926, with coordinates of R.A. 143﹩\mathop{.}\limits^{\unicode{x000B0}}﹩527800 and decl. 39﹩\mathop{.}\limits^{\unicode{x000B0}}﹩442277, and a redshift value of z = 1.1691. The plot displays the continuum and emission lines of the spectrum, including C III and Mg II. The fitting process involves correction for Galactic extinction, redshift correction, PCA decomposition, modeling of the continuum and pseudocontinuum, and Gaussian fitting of emission lines. The curves and legends in the plot represent different steps and components of the fitting process, where f2 (10−17erg s−1 cm−2 A−1) denotes the flux density of the spectrum.
Paper: Discerning Misclassified Flat-spectrum Radio Quasars from Low-frequency-peaked BL Lacertae Objects
Authors: S. Liang, W. G. Yang, Y. G. Zheng, S. J. Kang
Figure caption: The spectrum of S4 0707+47. Black lines represent the total dereddened spectra, yellow lines represent the continua (fpl + fpoly), cyan lines represent the Fe II templates (fFe II), blue lines represent the overall emission lines, red lines represent the broad-line components, and green lines represent the narrow-line components. For a spectrum that is successfully decomposed into a host-galaxy component and a pure quasar component, the purple line represents the host component, the gray line represents the pure quasar component, and the pink line represents the spectrum reconstructed from the PCA host and quasar components.
Paper: Discerning Misclassified Flat-spectrum Radio Quasars from Low-frequency-peaked BL Lacertae Objects
Authors: S. Liang, W. G. Yang, Y. G. Zheng, S. J. Kang
Figure caption: The spectrum of 7C 1032+4424. This image illustrates the spectral-fitting results for the celestial object 7C 1032+4424, with coordinates of R.A. 158﹩\mathop{.}\limits^{\unicode{x000B0}}﹩883860 and decl. 44﹩\mathop{.}\limits^{\unicode{x000B0}}﹩158730, and a redshift value of z = 0.4436. The plot displays the continuum and emission lines of the spectrum, including Mg II, Hβ, and Hα. The fitting process involves correction for Galactic extinction, redshift correction, PCA decomposition, modeling of the continuum and pseudocontinuum, and Gaussian fitting of emission lines.
Paper: Discerning Misclassified Flat-spectrum Radio Quasars from Low-frequency-peaked BL Lacertae Objects
Authors: S. Liang, W. G. Yang, Y. G. Zheng, S. J. Kang
Figure caption: The spectrum of MG1 J114208+1547. This image illustrates the spectral-fitting results for the celestial object MG1 J114208+1547, with coordinates of R.A. 175﹩\mathop{.}\limits^{\unicode{x000B0}}﹩532240 and decl. 15﹩\mathop{.}\limits^{\unicode{x000B0}}﹩798385, and a redshift value of z = 0.299. The plot displays the continuum and emission lines of the spectrum, including Mg II, Hβ, and Hα. The fitting process involves correction for Galactic extinction, redshift correction, PCA decomposition, modeling of the continuum and pseudocontinuum, and Gaussian fitting of emission lines.
Paper: Discerning Misclassified Flat-spectrum Radio Quasars from Low-frequency-peaked BL Lacertae Objects
Authors: S. Liang, W. G. Yang, Y. G. Zheng, S. J. Kang
Figure caption: Spectral fitting for the quasar PKS 1514+197 at redshift z = 1.070. The black curve represents the observed dereddened spectrum. Yellow denotes the continuum model (fpl + fpoly), cyan represents the Fe II templates (fFe II), blue corresponds to all fitted emission lines, red shows the broad-line components, and green shows the narrow-line components. Insets illustrate detailed fits for specific lines: C III, Mg II, and Hβ, with reduced chi-squared (﹩{\chi }_{r}^{2}﹩) values indicating goodness of fit.
Paper: Discerning Misclassified Flat-spectrum Radio Quasars from Low-frequency-peaked BL Lacertae Objects
Authors: S. Liang, W. G. Yang, Y. G. Zheng, S. J. Kang
Figure caption: Multiband data-processing fitting process in the ﹩\mathrm{log}\nu -\mathrm{log}\nu {f}_{\nu }﹩ space. The black points are the multiband data points downloaded from the SSDC and 4FGL-DR2. In the middle panel we take the arithmetic average of multiple data points at the same radiation frequency to get the purple points, which are the points obtained after taking the arithmetic average, and the gray points are the points that do not participate in the fitting after taking the arithmetic average. In the bottom panel, the distance between the blue data points and the dashed line reflects the goodness of fit for corresponding data points in the upper panels. A closer alignment of blue points with the dashed line indicates superior fitting performance.
Paper: Discerning Misclassified Flat-spectrum Radio Quasars from Low-frequency-peaked BL Lacertae Objects
Authors: S. Liang, W. G. Yang, Y. G. Zheng, S. J. Kang
Figure caption: Energy spectrum distribution of Fermi blazars in the logν−logνfν space. The black solid line is the fitting curve of the synchrotron radiation peak, and the black dashed line is the fitting line of the IC scattering peak. The black dots are multiband data points. The red data points are the seven energy bands of Fermi, the blue areas are the confidence ranges, and the small plot below shows how each data point deviates from the fitted curve.
Paper: Discerning Misclassified Flat-spectrum Radio Quasars from Low-frequency-peaked BL Lacertae Objects
Authors: S. Liang, W. G. Yang, Y. G. Zheng, S. J. Kang
Figure caption: The relationship between ﹩\mathrm{log}{L}_{\gamma }﹩ (y-axis) and ﹩\mathrm{log}{L}_{R}﹩ (x-axis). The scatter plot shows the relationship between ﹩\mathrm{log}{L}_{\gamma }﹩ and ﹩\mathrm{log}{L}_{R}﹩ on a logarithmic scale. Blue points represent LBL sources, while red points represent FSRQ sources. A positive correlation is observed between ﹩\mathrm{log}{L}_{\gamma }﹩ and ﹩\mathrm{log}{L}_{R}﹩ for both types, with FSRQ sources generally exhibiting higher values in both luminosities compared to LBL sources.
Paper: Discerning Misclassified Flat-spectrum Radio Quasars from Low-frequency-peaked BL Lacertae Objects
Authors: S. Liang, W. G. Yang, Y. G. Zheng, S. J. Kang
Figure caption: This figure illustrates the distribution of Gγ. The x-axis represents the logarithmic values of gamma-ray loudness, with the red curve representing the log-gamma-ray loudness distribution for LBLs and the blue curve representing the log-gamma-ray loudness distribution for FSRQs. From the figure, it can be observed that the distribution ranges for both types of sources largely overlap, indicating their similarity in gamma-ray loudness.
Paper: Monitoring AGNs with Hβ Asymmetry. V. Long-term Variation and Evolution of the Broad Hβ Emission-line Profiles
Authors: Feng-Na Fang, Pu Du, Michael S. Brotherton, Jacob N. McLane, T. E. Zastrocky, Kianna A. Olson, Dong-Wei Bao, Shuo Zhai, Hua-Rui Bai, Yi-Xin Fu, Bi-Xuan Zhao, Yong-Jie Chen, Yue-Chang Peng, Yu-Yang Songsheng, Yan-Rong Li, Chen Hu, Ming Xiao, Bo-Wei Jiang, Yi-Lin Wang, Hao Zhang, Yu Zhao, Jia-Qi Feng, Yi-Peng Zhao, David H. Kasper, William T. Chick, My L. Nguyen, Jaya Maithil, H. A. Kobulnicky, D. A. Dale, Derek Hand, C. Adelman, Z. Carter, G. M. Murphree, M. Oeur, S. Schonsberg, T. Roth, Hartmut Winkler, Paola Marziani, Mauro D'Onofrio, Keith Horne, Luis C. Ho, Jin-Ming Bai, Jian-Min Wang
Figure caption: Correlations between Hβ flux, the FWHM, σline, FWHM/σline, and Δv. The orange lines and regions represent the linear regressions and their uncertainties. The FHβ is in units of 10−15 erg s−1 cm−2. The FWHM and σline are in units of ​​​​​kilometers per second, and Δv is in units of thousands of kilometers per second. In each panel, r and p are the Pearson’s correlation coefficients and the null probabilities, and β2 represents the slope.
Paper: Monitoring AGNs with Hβ Asymmetry. V. Long-term Variation and Evolution of the Broad Hβ Emission-line Profiles
Authors: Feng-Na Fang, Pu Du, Michael S. Brotherton, Jacob N. McLane, T. E. Zastrocky, Kianna A. Olson, Dong-Wei Bao, Shuo Zhai, Hua-Rui Bai, Yi-Xin Fu, Bi-Xuan Zhao, Yong-Jie Chen, Yue-Chang Peng, Yu-Yang Songsheng, Yan-Rong Li, Chen Hu, Ming Xiao, Bo-Wei Jiang, Yi-Lin Wang, Hao Zhang, Yu Zhao, Jia-Qi Feng, Yi-Peng Zhao, David H. Kasper, William T. Chick, My L. Nguyen, Jaya Maithil, H. A. Kobulnicky, D. A. Dale, Derek Hand, C. Adelman, Z. Carter, G. M. Murphree, M. Oeur, S. Schonsberg, T. Roth, Hartmut Winkler, Paola Marziani, Mauro D'Onofrio, Keith Horne, Luis C. Ho, Jin-Ming Bai, Jian-Min Wang
Figure caption: Correlations between Hβ flux and asymmetry A. The orange lines and regions represent the linear regressions and their uncertainties. The FHβ is in units of 10−15 erg s−1 cm−2. In each panel, r and p are the Pearson’s correlation coefficients and the corresponding null probabilities, and β1 represents the slope.
Paper: Monitoring AGNs with Hβ Asymmetry. V. Long-term Variation and Evolution of the Broad Hβ Emission-line Profiles
Authors: Feng-Na Fang, Pu Du, Michael S. Brotherton, Jacob N. McLane, T. E. Zastrocky, Kianna A. Olson, Dong-Wei Bao, Shuo Zhai, Hua-Rui Bai, Yi-Xin Fu, Bi-Xuan Zhao, Yong-Jie Chen, Yue-Chang Peng, Yu-Yang Songsheng, Yan-Rong Li, Chen Hu, Ming Xiao, Bo-Wei Jiang, Yi-Lin Wang, Hao Zhang, Yu Zhao, Jia-Qi Feng, Yi-Peng Zhao, David H. Kasper, William T. Chick, My L. Nguyen, Jaya Maithil, H. A. Kobulnicky, D. A. Dale, Derek Hand, C. Adelman, Z. Carter, G. M. Murphree, M. Oeur, S. Schonsberg, T. Roth, Hartmut Winkler, Paola Marziani, Mauro D'Onofrio, Keith Horne, Luis C. Ho, Jin-Ming Bai, Jian-Min Wang
Figure caption: The Hα light curves and their correlations with Hβ flux. The units of Hα and Hβ are both 10−15 erg s−1 cm−2. r and p are the Pearson’s correlation coefficients and the null probabilities, and β3 is the slope. The contribution from the narrow line in the FHβ here has been removed.
Paper: Monitoring AGNs with Hβ Asymmetry. V. Long-term Variation and Evolution of the Broad Hβ Emission-line Profiles
Authors: Feng-Na Fang, Pu Du, Michael S. Brotherton, Jacob N. McLane, T. E. Zastrocky, Kianna A. Olson, Dong-Wei Bao, Shuo Zhai, Hua-Rui Bai, Yi-Xin Fu, Bi-Xuan Zhao, Yong-Jie Chen, Yue-Chang Peng, Yu-Yang Songsheng, Yan-Rong Li, Chen Hu, Ming Xiao, Bo-Wei Jiang, Yi-Lin Wang, Hao Zhang, Yu Zhao, Jia-Qi Feng, Yi-Peng Zhao, David H. Kasper, William T. Chick, My L. Nguyen, Jaya Maithil, H. A. Kobulnicky, D. A. Dale, Derek Hand, C. Adelman, Z. Carter, G. M. Murphree, M. Oeur, S. Schonsberg, T. Roth, Hartmut Winkler, Paola Marziani, Mauro D'Onofrio, Keith Horne, Luis C. Ho, Jin-Ming Bai, Jian-Min Wang
Figure caption: Examples of asymmetry measurement and comparisons between the line profiles in bright (blue solid lines), faint (green solid lines), and mean spectra (orange solid lines). The units are 10−15 erg s−1 cm−2 Å−1. The horizontal colored dotted lines mark the 3/4 and 1/4 levels of the peak intensity. The black dotted lines represent the spectra before the narrow-line subtraction. The middle panels are the residuals and subtracting the mean spectra from the bright spectra, while the bottom panels are those from the faint spectra. The blue and red bars indicate the average flux in the corresponding ranges. The residuals were calculated after aligning the profiles according to their velocity shift Δv.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: The top section of the panels compares metallicity estimates for RRab stars between L20 and our photometric estimators, with results for the gri bands shown from left to right, respectively. Red dots in each panel represent sample stars excluded by the 3σ clipping, while black dots are those included in the final fitting. The solid purple line is the one-to-one line. The lower section of each panel shows Δ[Fe/H] differences (our work minus L20), with the mean and standard deviation displayed at the bottom left of each panel. Purple-dashed lines denote the 1σ boundaries, and the solid purple line indicates the mean residual level. The cyan dots and associated error bars represent the median Δ[Fe/H] values and their standard deviations for each [Fe/H]L20 bin.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: The PMZ relations for the ZTF_RRL_FIT_DIS1 sample, refined by absolute magnitude error constraints, are presented in two columns of panels, color coded by metallicity. The left and right columns correspond to RRab and RRc types, respectively, displaying the gri bands from top to bottom. The solid red line in each panel denotes the best fit, and the standard deviation of the residuals is provided in the top left corner of each panel.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: The PMZ relation, similar to Figure 4, but with an adjusted y-axis to display only absolute magnitude without the metallicity term, showing the sample distributed in the period–absolute magnitude space. The fitted PMZ relations are evaluated at [Fe/H] =  −2.0 and  −1.0, and depicted in two distinct colors. For comparison, the relations from this work (TW), S17, N22, at these fixed [Fe/H] values are represented by the solid dashed–dotted, and dashed lines, respectively. The slopes of the lines indicate the dependence on the period terms, while the vertical separation between two lines from the different [Fe/H] levels reflects the metallicity term’s influence.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Distribution of the Fourier parameters (Atot, ϕ21, R21, ϕ31), as a function of the period in the g band, for 73,796 ZTF_RRL_ALL sample stars (52,572 type RRab and 21,224 type RRc stars). In each panel, type RRab stars and their relatively low-quality sample stars are indicated in red and dark green, and type RRc stars and their relatively low-quality sample stars are indicated in cyan and dark purple. Figures for the r and I bands are presented in Figures A1 and A2, respectively, in Appendix A.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Similar to Figure 2, but for RRc stars.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: The PWZ relations for the ZTF_RRL_FIT_DIS2 sample, refined by absolute magnitude error constraints, are presented in two columns of panels, color coded by metallicity. The left and right columns correspond to RRab and RRc stars, respectively, displaying the gr-, gi-, and ri-band pairs from top to bottom. The solid red line in each panel denotes the best fit, and the standard deviation of the residuals is shown in the top left corner of each panel.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: The PWZ relations, similar to Figure 6, but with an adjusted y-axis to display only the absolute magnitude without the metallicity term, showing the sample distributed in the period–absolute magnitude space. The fitted PWZ relations are evaluated at [Fe/H] =  −2.0 and  −0.5(−1) for RRab and RRc stars, and depicted in two distinct colors. For comparison, relations from this work (TW) and N22 at the fixed [Fe/H] values are represented by solid and dashed lines, respectively. The slopes of the lines indicate the dependence on period terms, while the vertical separation between two lines from the different [Fe/H] levels reflects the metallicity term’s influence.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Comparison of distance estimates calculated from our PMZ and PWZ relations for RRab stars (left panel) and RRc stars (right panel). The solid red line is the one-to-one line. The lower section of each panel displays the relative difference between dPMZ and dPWZ, along with the mean and standard deviation of the relative difference indicated at the upper right of each panel. The red-dashed line is the zero residual level.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Upper section of the panel: comparison of photometric metallicity estimates from this work and metallicity from the high-resolution spectroscopic sample. The red solid line is the one-to-one line. Lower section of the panel: Δ[Fe/H] differences (our work minus high-resolution spectroscopic results), with the mean and standard deviation displayed in the lower left. The red-dashed line is the zero residual level.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Our estimated metallicity (y-axis) compared with two reference works (x-axis), with black dots representing H10 and gray dots representing the GOTHAM survey. Circles denote RRab stars, and triangles denote RRc stars. The solid red line is the one-to-one line. The mean and scatter of the residuals are shown in the lower panel. The red-dashed line is the zero residual level.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Distribution of relative distance errors for the GCs. Left panel: using weighted average distances calculated with the newly calibrated PWZ relations. Right panel: using the PMZ relations. The median relative errors of distance are indicated with blue-dashed and yellow-dashed lines for RRab and RRc stars, respectively.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: The uncertainty distributions of our metallicity estimates for each GC are shown for RRab (blue) and RRc (yellow) member stars, respectively. The typical accuracies in median values are indicated with blue-dashed and yellow-dashed lines for RRab and RRc stars, respectively.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: The heliocentric distance distribution for our final RRL sample. The prominent structures are marked by dashed lines in different colors. The y-axis represents the frequency on a logarithmic scale.
Paper: Photometric Metallicity and Distance Estimates for ∼70,000 RR Lyrae Stars from the Zwicky Transient Facility
Authors: Shun-Xuan He, Yang Huang, Xin-Yi Li, Hua-Wei Zhang, Gao-Chao Liu, Timothy C. Beers, Hong Wu, Zhou Fan
Figure caption: Sky distribution in Galactic coordinates of our final sample are shown in gray, with the sample stars with newly obtained photometric metallicity estimates colored red, and those with newly obtained distance estimates colored cyan.