adsabs/AstroCLIMB huggingface dataset:
Paper: Broadband Multiwavelength Study of LHAASO-detected Active Galactic Nuclei
Authors: Ze-Rui Wang, Rui Xue, Dingrong Xiong, Hai-Qin Wang, Lu-Ming Sun, Fang-Kun Peng, Jirong Mao
Figure caption: Multiwavelength light curves (LCs) of LHAASO sources. Panels from top to bottom in these six figures: LCs of WISE, ZTF, Swift-UVOT, Swift-XRT, Fermi-LAT, and TS of GeV detection. There is no Swift-UVOT figure for NGC 4278. The meaning of symbols is given in the legend of Mrk 421. Note that the y-axis of some panels does not start from zero.
Paper: Broadband Multiwavelength Study of LHAASO-detected Active Galactic Nuclei
Authors: Ze-Rui Wang, Rui Xue, Dingrong Xiong, Hai-Qin Wang, Lu-Ming Sun, Fang-Kun Peng, Jirong Mao
Figure caption: The ratio of L jet/L Edd in the Γ − B diagram for the one-zone proton-synchrotron model. The upper six panels show the results that applying proton-synchrotron emission to explain the entire high-energy component, and the lower six panels show the results that applying proton-synchrotron emission to explain the high-energy tail of LHAASO spectra. The black curves with arrows represent the parameter space that satisfied the Hillas condition. The vertical blue curves with arrows show the lower limit of Γ that allows the escape of maximum energy γ-ray photons. The vertical and horizontal purple curves show the space that B ≲ 10 G and Γ ≲ 30. The white dashed contours denote specific values of log (L jet/L Edd) associated with the color bar.
Paper: Broadband Multiwavelength Study of LHAASO-detected Active Galactic Nuclei
Authors: Ze-Rui Wang, Rui Xue, Dingrong Xiong, Hai-Qin Wang, Lu-Ming Sun, Fang-Kun Peng, Jirong Mao
Figure caption: The fitting results of the Swift-XRT spectra.
Paper: Broadband Multiwavelength Study of LHAASO-detected Active Galactic Nuclei
Authors: Ze-Rui Wang, Rui Xue, Dingrong Xiong, Hai-Qin Wang, Lu-Ming Sun, Fang-Kun Peng, Jirong Mao
Figure caption: Two-zone proton-synchrotron Modeling. The meanings of symbols and line styles are given in the legend.
Paper: Broadband Multiwavelength Study of LHAASO-detected Active Galactic Nuclei
Authors: Ze-Rui Wang, Rui Xue, Dingrong Xiong, Hai-Qin Wang, Lu-Ming Sun, Fang-Kun Peng, Jirong Mao
Figure caption: The first fitting strategy of the spine-layer model. The multiwavelength data are explained by the emission from one component. The meanings of symbols and line styles are given in the legend of Mrk 421.
Paper: Broadband Multiwavelength Study of LHAASO-detected Active Galactic Nuclei
Authors: Ze-Rui Wang, Rui Xue, Dingrong Xiong, Hai-Qin Wang, Lu-Ming Sun, Fang-Kun Peng, Jirong Mao
Figure caption: One-zone SSC+pp modeling. The meanings of symbols and line styles are given in the legend of Mrk 421.
Paper: Detection of Solar-like Oscillations in Subgiant and Red Giant Stars Using 2 minute Cadence TESS Data
Authors: Jianzhao Zhou, Shaolan Bi, Jie Yu, Yaguang Li, Xianfei Zhang, Tanda Li, Liu Long, Mengjie Li, Tiancheng Sun, Lifei Ye
Figure caption: The distribution of detected solar-like oscillators across the celestial sphere. The color bar corresponds to the observation duration, denoted by the number of sectors. Some stars (green dots) are observed for two to three sectors near the ecliptic, because TESS focused on a specific segment of the ecliptic from Sector 42 to 46 coinciding with the portion of the K2 observation zones. The northern ecliptic hemisphere contains gaps to avoid excessive contamination from stray Earth- and moonlight, and the corresponding region appears at low latitudes close to the ecliptic. The black dashed circles represent the CVZs.
Paper: Detection of Solar-like Oscillations in Subgiant and Red Giant Stars Using 2 minute Cadence TESS Data
Authors: Jianzhao Zhou, Shaolan Bi, Jie Yu, Yaguang Li, Xianfei Zhang, Tanda Li, Liu Long, Mengjie Li, Tiancheng Sun, Lifei Ye
Figure caption:  R vs. T eff for 2 minute cadence targets and seismic targets. The T eff and radii are sourced from TICv8.2. The light gray dots show the 2 minute cadence targets, the blue dots show the seismic targets, and the red dashed line, in reference to Hon et al. (2019), shows the boundary used to distinguish early subgiant stars from those ascending the red giant branch.
Paper: Detection of Solar-like Oscillations in Subgiant and Red Giant Stars Using 2 minute Cadence TESS Data
Authors: Jianzhao Zhou, Shaolan Bi, Jie Yu, Yaguang Li, Xianfei Zhang, Tanda Li, Liu Long, Mengjie Li, Tiancheng Sun, Lifei Ye
Figure caption: An example of measuring Δν for TIC 38828538 (a) The échelle diagram—the red dashed line represents the value of ﹩{\nu }_{\max }﹩. (b) The residual power spectrum. (c) The ACF—the two red dashed lines represent the positions of Δν and twice Δν, from left to right. (d) The FTs of the ACF—the two red dashed lines represent the positions of half of Δν and Δν in period, from left to right, while the blue dashed line shows the noise.
Paper: Detection of Solar-like Oscillations in Subgiant and Red Giant Stars Using 2 minute Cadence TESS Data
Authors: Jianzhao Zhou, Shaolan Bi, Jie Yu, Yaguang Li, Xianfei Zhang, Tanda Li, Liu Long, Mengjie Li, Tiancheng Sun, Lifei Ye
Figure caption: Representative power spectra of the TESS 2 minute cadence light curves. In each panel, the gray line shows the real data and the black line shows the data smoothed by a boxcar filter of 3 μHz wide. The solid blue line shows the MCMC fitting result, with the red dashed line for the fitted Gaussian envelope, the green dashed curve for the three Harvey components, and the brown straight line for the white noise. The inset figure shows the power spectrum near ﹩{\nu }_{\max }﹩ divided by the background.
Paper: Detection of Solar-like Oscillations in Subgiant and Red Giant Stars Using 2 minute Cadence TESS Data
Authors: Jianzhao Zhou, Shaolan Bi, Jie Yu, Yaguang Li, Xianfei Zhang, Tanda Li, Liu Long, Mengjie Li, Tiancheng Sun, Lifei Ye
Figure caption: The relation of ﹩{\nu }_{\max }﹩ and Δν in logarithmic coordinates. The color bar shows the relative error of the measured Δν. The black dotted line follows an MCMC-fitted power-law relation: ﹩{\rm{\Delta }}\nu =\alpha \cdot {({\nu }_{\max })}^{\beta }﹩, where α = 0.236 ± 0.001 and β = 0.789 ± 0.001.
Paper: Detection of Solar-like Oscillations in Subgiant and Red Giant Stars Using 2 minute Cadence TESS Data
Authors: Jianzhao Zhou, Shaolan Bi, Jie Yu, Yaguang Li, Xianfei Zhang, Tanda Li, Liu Long, Mengjie Li, Tiancheng Sun, Lifei Ye
Figure caption: Histogram of relative uncertainties for ﹩{\nu }_{\max }﹩ and Δν. N sectors shows the number of sectors. The gray line represents the entire sample, while the purple, blue, yellow, and red lines represent stars observed for one to two sectors, three to four sectors, five to 13 sectors, and stars observed for more than 14 sectors, respectively.
Paper: Detection of Pairwise Kinetic Sunyaev–Zel’dovich Effect with DESI Galaxy Groups and Planck in Fourier Space
Authors: Shaohong Li, Yi Zheng, Ziyang Chen, Haojie Xu, Xiaohu Yang
Figure caption: Left: the ﹩\bar{\tau }﹩ profiles of group samples with different lower mass thresholds. N in the legend represents the size of the sample. For a clear presentation of the error bars, data points are shifted horizontally from their real θ APs. Right: corresponding S/Ns of the measurements.
Paper: CatNorth: An Improved Gaia DR3 Quasar Candidate Catalog with Pan-STARRS1 and CatWISE
Authors: Yuming Fu, Xue-Bing Wu, Yifan Li, Yuxuan Pang, Ravi Joshi, Shuo Zhang, Qiyue Wang, Jing Yang, FanLam Ng, Xingjian Liu, Yu Qiu, Rui Zhu, Huimei Wang, Christian Wolf, Yanxia Zhang, Zhi-Ying Huo, Y. L. Ai, Qinchun Ma, Xiaotong Feng, R. J. Bouwens
Figure caption: Top row: ensemble photometric redshift (z ph) against SDSS/Milliquas spectral redshift of the validation set with 90,796 quasars (a), RegNet redshift (z xp_nn) against SDSS/Milliquas spectral redshift of the validation set with 7599 quasars (b), and z ph vs. z xp_nn (c). Middle row: comparisons of redshift values between SDSS and Gaia (d), CatNorth z ph and Gaia (e), and CatNorth z xp_nn and Gaia (f). Bottom row: comparisons of redshift values between SDSS and Quaia (g), CatNorth z ph and Quaia (h), and CatNorth z xp_nn and Quaia (i). The plots are color coded with two-dimensional densities (number counts in the pixels) of the samples, the values of which are indicated in the color bars.
Paper: CatNorth: An Improved Gaia DR3 Quasar Candidate Catalog with Pan-STARRS1 and CatWISE
Authors: Yuming Fu, Xue-Bing Wu, Yifan Li, Yuxuan Pang, Ravi Joshi, Shuo Zhang, Qiyue Wang, Jing Yang, FanLam Ng, Xingjian Liu, Yu Qiu, Rui Zhu, Huimei Wang, Christian Wolf, Yanxia Zhang, Zhi-Ying Huo, Y. L. Ai, Qinchun Ma, Xiaotong Feng, R. J. Bouwens
Figure caption: H-R diagrams of the LVAC_PLUS stellar sample (left) and the GDR3_PLUS stellar sample (right). The effective temperatures are from column teff_gspphot of the Gaia DR3 source table, which are estimated with the General Stellar Parametrizer from the photometry module (GSP-Phot; Bailer-Jones 2011; Andrae et al. 2023; Creevey et al. 2023). The absolute G-band magnitude is calculated as ﹩{M}_{G}=G-5\mathrm{log}(1000/\varpi )+5﹩, where ϖ is the Gaia DR3 parallax in units of mas. The H-R diagrams are color coded with source number counts in the pixels, the values of which are indicated in the color bars.
Paper: CatNorth: An Improved Gaia DR3 Quasar Candidate Catalog with Pan-STARRS1 and CatWISE
Authors: Yuming Fu, Xue-Bing Wu, Yifan Li, Yuxuan Pang, Ravi Joshi, Shuo Zhang, Qiyue Wang, Jing Yang, FanLam Ng, Xingjian Liu, Yu Qiu, Rui Zhu, Huimei Wang, Christian Wolf, Yanxia Zhang, Zhi-Ying Huo, Y. L. Ai, Qinchun Ma, Xiaotong Feng, R. J. Bouwens
Figure caption: Color–color diagrams of 200,000 quasars (blue contours), 200,000 galaxies (green contours), and 400,000 stars (red-shaded density plots) using photometric data from PS1, CatWISE, and Gaia DR3. The quasar and galaxy samples are random subsets of the quasar and galaxy samples described in Sections 2.3.1 and 2.3.2. The star sample is randomly selected from the union of LVAC_PLUS and GDR3_PLUS. The density plots of stars are color coded with density, with higher density being darker, and lower density being lighter. All magnitudes are in the AB system.
Paper: CatNorth: An Improved Gaia DR3 Quasar Candidate Catalog with Pan-STARRS1 and CatWISE
Authors: Yuming Fu, Xue-Bing Wu, Yifan Li, Yuxuan Pang, Ravi Joshi, Shuo Zhang, Qiyue Wang, Jing Yang, FanLam Ng, Xingjian Liu, Yu Qiu, Rui Zhu, Huimei Wang, Christian Wolf, Yanxia Zhang, Zhi-Ying Huo, Y. L. Ai, Qinchun Ma, Xiaotong Feng, R. J. Bouwens
Figure caption: Histograms of the logarithmic redshift errors, ﹩{\rm{\Delta }}Z\,=\mathrm{log}(1+z)-\mathrm{log}(1+{z}_{\mathrm{SDSS}})﹩ of z Gaia (blue), z Quaia (green), and CatNorth z ph (red), for 286,107 sources contained in the SDSS DR16Q catalog. A bin width of 0.0026 is used for all curves. Several prominent peaks due to emission line misidentifications are indicated with vertical dashed lines and text.
Paper: CatNorth: An Improved Gaia DR3 Quasar Candidate Catalog with Pan-STARRS1 and CatWISE
Authors: Yuming Fu, Xue-Bing Wu, Yifan Li, Yuxuan Pang, Ravi Joshi, Shuo Zhang, Qiyue Wang, Jing Yang, FanLam Ng, Xingjian Liu, Yu Qiu, Rui Zhu, Huimei Wang, Christian Wolf, Yanxia Zhang, Zhi-Ying Huo, Y. L. Ai, Qinchun Ma, Xiaotong Feng, R. J. Bouwens
Figure caption: Schematic diagram of the CNN-based RegNet architecture, which is designed to extract redshifts from Gaia DR3 BP/RP spectra. This diagram shows the process of a single spectrum with 300 points passing through the network and yielding the redshift value. For simplicity, only a small fraction of the input and hidden neurons are plotted.
Paper: CatNorth: An Improved Gaia DR3 Quasar Candidate Catalog with Pan-STARRS1 and CatWISE
Authors: Yuming Fu, Xue-Bing Wu, Yifan Li, Yuxuan Pang, Ravi Joshi, Shuo Zhang, Qiyue Wang, Jing Yang, FanLam Ng, Xingjian Liu, Yu Qiu, Rui Zhu, Huimei Wang, Christian Wolf, Yanxia Zhang, Zhi-Ying Huo, Y. L. Ai, Qinchun Ma, Xiaotong Feng, R. J. Bouwens
Figure caption: Histograms of ﹩\mathrm{log}({f}_{\mathrm{PM}0})﹩ of the master stellar samples LVAC_PLUS (blue) and GDR3_PLUS (yellow), quasars from SDSS DR16Q (green), and galaxies from SDSS DR17 (white). Because f PM0 is the probability density that can be greater than 1 (the integral of the probability density function over the entire space is equal to 1), ﹩\mathrm{log}({f}_{\mathrm{PM}0})﹩ can have positive values.
Paper: CatNorth: An Improved Gaia DR3 Quasar Candidate Catalog with Pan-STARRS1 and CatWISE
Authors: Yuming Fu, Xue-Bing Wu, Yifan Li, Yuxuan Pang, Ravi Joshi, Shuo Zhang, Qiyue Wang, Jing Yang, FanLam Ng, Xingjian Liu, Yu Qiu, Rui Zhu, Huimei Wang, Christian Wolf, Yanxia Zhang, Zhi-Ying Huo, Y. L. Ai, Qinchun Ma, Xiaotong Feng, R. J. Bouwens
Figure caption: The MNSE losses in 1000 epochs of our RegNet model on the training sample (blue curve) and validation sample (red curve). As the model is trained iteratively, the training loss steadily decreases, signifying the network’s ability to fit the training set. Meanwhile, the validation loss from an independent validation set demonstrates the performance of the generalization of the model.
Paper: CatNorth: An Improved Gaia DR3 Quasar Candidate Catalog with Pan-STARRS1 and CatWISE
Authors: Yuming Fu, Xue-Bing Wu, Yifan Li, Yuxuan Pang, Ravi Joshi, Shuo Zhang, Qiyue Wang, Jing Yang, FanLam Ng, Xingjian Liu, Yu Qiu, Rui Zhu, Huimei Wang, Christian Wolf, Yanxia Zhang, Zhi-Ying Huo, Y. L. Ai, Qinchun Ma, Xiaotong Feng, R. J. Bouwens
Figure caption: HEALPix (Górski et al. 2005) sky density maps of the LVAC_PLUS stellar sample (left) and the GDR3_PLUS stellar sample (right). The maps are plotted in Galactic coordinates, with the parameter N side = 64 and an area of 0.839 deg2 px−1.
Paper: CatNorth: An Improved Gaia DR3 Quasar Candidate Catalog with Pan-STARRS1 and CatWISE
Authors: Yuming Fu, Xue-Bing Wu, Yifan Li, Yuxuan Pang, Ravi Joshi, Shuo Zhang, Qiyue Wang, Jing Yang, FanLam Ng, Xingjian Liu, Yu Qiu, Rui Zhu, Huimei Wang, Christian Wolf, Yanxia Zhang, Zhi-Ying Huo, Y. L. Ai, Qinchun Ma, Xiaotong Feng, R. J. Bouwens
Figure caption: Corrected flux excess factor C* vs. G BP − G RP color for stars (red-shaded density plots), quasars (blue contours), and galaxies (green contours). An inset of zoom-in plot for stars and quasars is displayed on the upper-right corner.
Paper: Detection of Pairwise Kinetic Sunyaev–Zel’dovich Effect with DESI Galaxy Groups and Planck in Fourier Space
Authors: Shaohong Li, Yi Zheng, Ziyang Chen, Haojie Xu, Xiaohu Yang
Figure caption: Left: Markov Chain Monte Carlo (MCMC) fitting results of multipoles of power spectrum of our baseline sample with three free parameters. Different colors indicate results of different photo-z damping functions. Upper right: the ﹩{b}_{1}\mbox{--}\tilde{M}﹩ relationship, where b 1s are obtained by MCMC fittings (data points with error bars) or given by theoretical models (solid lines). Lower right: Measured ﹩\bar{\tau }\mbox{--}\tilde{M}﹩ relationships when different D pho-z s and b 1–M models are adopted. The black data points with error bars are results when we fit b 1, b 2, and, σ  z  simultaneously. The colored points are results when we first calculate b 1 from the corresponding b 1–M model and then fit b 2 and σ  z  from ﹩{\hat{P}}_{{\ell }}﹩ measurements. The adopted b 1–M models embedded in the colossus Python toolkit (Diemer 2018) are: jing98 (Jing 1998), sheth01 (Sheth et al. 2001), tinker10 (Tinker et al. 2010), and bhattacharya11 (Bhattacharya et al. 2011).
Paper: Detection of Pairwise Kinetic Sunyaev–Zel’dovich Effect with DESI Galaxy Groups and Planck in Fourier Space
Authors: Shaohong Li, Yi Zheng, Ziyang Chen, Haojie Xu, Xiaohu Yang
Figure caption: The measured ﹩\bar{\tau }\mbox{--}\tilde{M}﹩ relationship with ﹩{\theta }_{\mathrm{AP}}=4\buildrel{\,\prime}\over{.} 2﹩. The points with error bars are measurements from various samples with different M th, and the solid lines are the best-fitted Equation (48) with ﹩\beta =({0.98}_{-0.15}^{+0.15})\times {10}^{-4}﹩, and ﹩\gamma ={0.55}_{-0.10}^{+0.10}﹩. We caution that cross-correlations between different ﹩\bar{\tau }{\rm{s}}﹩ are ignored in this fitting, so the fitted error bars for β and γ are underestimated here.