adsabs/AstroCLIMB huggingface dataset:
Paper: Binding Energy Evaluation Platform: A Database of Quantum Chemical Binding Energy Distributions for the Astrochemical Community
Authors: Giulia M. Bovolenta, Stefan Vogt-Geisse, Stefano Bovino, Tommaso Grassi
Figure caption: Comparison between BE distributions obtained using metahybrid GGA geometries (orange histogram, Gaussian function represented with solid line) and HF-3 c geometries (blue, dashed line). Left panel: Group D; right panel: Group H. BE values are shown without ZPVE correction.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: The distribution of the correction factor, defined as the ratio between L X and the observed X-ray luminosities, for X-ray-detected sources. The vertical black line marks the median correction (0.1 dex).
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: The typical SEDs of sources satisfying different AGN-selection conditions, as indicated by the panel titles, where “SED” means refined SED AGN candidates, and MIR AGNs are those satisfying any criterion in Stern et al. (2005), Lacy et al. (2007), or Donley et al. (2012). The source SEDs are normalized by their total fluxes integrated from X-ray to FIR, and the black, cyan, and red solid lines are the median total SEDs, galaxy, and AGN components, respectively. The shaded regions indicate 16th–84th percentiles of the corresponding components. The red shaded regions become large in the optical because there are both type 1 and type 2 AGNs—the former have bright and blue optical emission, while the latter are usually much fainter. The red shaded region for MIR-only AGNs is large because its 16th percentile is zero across all wavelengths, indicating that MIR-only AGNs may be largely contaminated by star-forming galaxies. The AGN components of X-ray- or MIR-only AGNs are generally more obscured and less dominant, which also explains why they are not selected as refined SED AGN candidates.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: Venn diagrams comparing different AGN-selection results. The two panels differ for MIR AGNs, where the left panel contains MIR AGNs satisfying any criterion in Stern et al. (2005), Lacy et al. (2007), or Donley et al. (2012), while the right panel only contains MIR AGNs based on Donley et al. (2012) to increase the purity. 63% of X-ray AGNs, 41% of MIR AGN, and 91% of MIR AGNs based on Donley et al. (2012) are also selected as refined SED AGN candidates, i.e., with ΔBIC2(AGN) > 2. There are many more SED AGN candidates than X-ray or MIR AGNs because of both the contamination of normal galaxies and missed AGNs by X-ray and MIR. The total number of AGNs and refined SED AGN candidates is slightly different from the number of sources with “best” results from the AGN fitting in Table 1 because the best results of some refined SED AGN candidates are instead from the BQ-galaxy fitting (see Section 4.5).
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: The distributions of sources on the IR color–color diagram. Red points are sources satisfying the criterion in the panel title, and cyan ones are the others. The kernel density estimations of the red points are plotted as the red-to-blue contour profiles. The dashed and solid lines are the AGN-selection wedges in Lacy et al. (2007) and Donley et al. (2012), respectively. Among the four panels on the left, the upper left one shows galaxies that are not selected as raw SED AGN candidates; the upper right one shows sources that are selected as raw SED AGN candidates but fail to pass the refined candidate selection; the bottom two panels present the refined SED AGN candidates and divide them into two ΔBIC2(AGN) bins that roughly contain the same number of sources. As a comparison, the distribution of X-ray AGNs is plotted in the rightmost panel. The distribution of the red points gradually converges into the MIR AGN-selection wedges as ΔBIC increases.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: The HB flux upper-limit map with units of ergs per square centimeter per second. We derive flux upper limits for X-ray-undetected sources based on this map.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: The gzK color–color diagram for sources in W-CDF-S. Cyan and orange points are our selected nonstars and stars, respectively. Our selected stars form a clear stellar locus, justifying the overall reliability of the star selection. The branch lying roughly 1 mag above the stellar locus is early-type galaxies; see, e.g., Figure 1 in Lane et al. (2007) for an example.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: The stacked and smoothed X-ray FB net count-rate images covering 84″ × 84″. Each image is constructed from 1000 random sources satisfying the criterion in the corresponding panel title and at least 1′ away from all the X-ray sources. The stacked signal visually increases with ΔBIC(AGN).
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: The correction factor of the HB flux upper limit for undetected sources, C undet, as a function of z. We multiply the observed HB flux upper limits by this factor to obtain the intrinsic HB flux upper limits.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: Same as Figure 6, but for the AGN-selection wedge in Stern et al. (2005).
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: The 24–500 μm upper-limit maps in a ﹩10^{\prime} \times 10^{\prime} ﹩ region of the W-CDF-S, centered at J2000 R. A. = 53°, decl. = −28.°4. The map units are all mJy.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: Comparisons of our M ⋆ (top) and SFR (bottom) measurements in XMM-LSS with the HELP values (left), the Prospector- α values (middle; before corrections), and the Prospector- α values after applying the empirical corrections in Equations (E2) and (E3). The left and middle panels are similar to those in Figure 26, but for XMM-LSS, and the right panels correspond to Figure 27. The blue dashed–dotted line in the right panel is the resulting LOESS curve if we apply the W-CDF-S corrections (Equations (23) and (24)), which is generally consistent with the XMM-LSS corrections, as represented by the red solid line.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: Left: the distribution of our sources in the z − σ  z  plane, where only bins with at least 200 sources are shown. Middle: the map of the additional error from photo-z uncertainties for ﹩\mathrm{log}{M}_{\star }﹩. Right: the map of the additional error from photo-z uncertainties for logSFR.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: Venn diagrams comparing different AGN-selection results in ELAIS-S1. Left: comparison among X-ray AGNs, MIR AGNs, and the refined SED AGN candidates. Middle: the MIR AGNs are limited to those satisfying the criterion in Donley et al. (2012). Right: the SED AGNs are only limited to those satisfying the reliable-AGN criterion in W-CDF-S (see Section 3.2.4). The left and middle panels correspond to Figure 9, and the right panel corresponds to the right panel of Figure 14.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: The number of good bands vs. i mag. Each background point represents one source, and the large red points with error bars represent the median, 25th, and 75th percentiles of the number of good bands in each magnitude bin. The number of good bands drops significantly around i mag = 24.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: Comparisons of our M ⋆ (left) and SFR (right) measurements with the HELP values. They are the same as the left panels of Figure 26, but for ELAIS-S1.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: Comparisons between our SED-based and FIR-based SFRs in ELAIS-S1. This figure corresponds to Figure 28.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: Same as Figure D1, but for XMM-LSS, and the reliable-AGN criterion is Equation (E1).
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: Comparison between the SED-fitting results with or without FIR data for M ⋆ (left) and SFR (right). The results are consistent, indicating that the fitting without FIR data does not have significant biases.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: Comparisons between our SED-based and FIR-based SFRs in XMM-LSS. This figure corresponds to Figure 28.
Paper: A Multifluid Dust Module in Athena++: Algorithms and Numerical Tests
Authors: Pinghui Huang, Xue-Ning Bai
Figure caption: 1D (top six panels) and 1.5D (bottom six panels) dust diffusion tests without (“No Correction, NoCo”; dashed lines)/with (“Correction, Co”; solid lines) momentum corrections. The first and third rows show the gas density (ρ g) and velocities (v g,x, v g,y) at different times (t = 0.0, 1.0, 3.0, and 5.0). Note that the gas density and x-velocity in the first and third panels are identically one and zero in the “NoCo” cases, with these dashed lines embedded below the black solid line. The second and fourth rows show the dust concentration (ρ d/ρ g) and dust velocities (v d,x, v d,y) at different times. Similarly, the dust x-velocity in the “NoCo” case is zero, with the corresponding dashed lines embedded below the black solid line.
Paper: A Multifluid Dust Module in Athena++: Algorithms and Numerical Tests
Authors: Pinghui Huang, Xue-Ning Bai
Figure caption: The top eight panels are the velocities and energy of the gas and dust in collision Tests B and C, with the numerical time steps Δt = 0.005 and Δt = 0.05. The solutions obtained by different semi-implicit and fully implicit drag integrators are shown. The black dashed lines represent the analytic solutions. Note that the explicit methods are unstable for our choice of Δt > 1/∣λ 2∣ (see Table 1), and the results are not shown. The bottom three panels are the scaling of the total relative error ΔE total, with numerical time step Δt, for different drag integrators (see the legends) in the collision Tests A (left), B (middle), and C (right).
Paper: A Multifluid Dust Module in Athena++: Algorithms and Numerical Tests
Authors: Pinghui Huang, Xue-Ning Bai
Figure caption: 2D dust diffusion tests without correction (top eight panels), with only Π dif correction (middle eight panels), and with both Π dif and ∂(ρ d  v  d,dif)/∂t corrections (bottom eight panels). From left to right, the panels are at time t = 0.0, 1.0, 3.0, and 5.0. The first, third, and fifth rows are for the gas density (ρ g), while the second, fourth, and sixth rows are for the dust concentration (ρ d/ρ g). The black (white) lines represent the velocity streamlines of gas (dust).
Paper: A Multifluid Dust Module in Athena++: Algorithms and Numerical Tests
Authors: Pinghui Huang, Xue-Ning Bai
Figure caption: Fitted averaging growth rates (normalized as s/Ω0), by measuring the mean kinetic energy E kinetic of the gas and dust in the Lin-A, Lin-B, and Lin-3 tests of the SI. The results are shown as a function of the number of grids per wavelength (N/λ). The analytic growth rates are marked with the blacked dotted lines. The different drag integrators are marked with different colors. The solid (dashed) lines represent the runs with PPM (PLM) spatial reconstruction.
Paper: A Multifluid Dust Module in Athena++: Algorithms and Numerical Tests
Authors: Pinghui Huang, Xue-Ning Bai
Figure caption: Flow chart of a single integration stage of the multifluid dust module in Athena++.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: Comparisons of our M ⋆ (top) and SFR (bottom) measurements with the HELP values (left), the Prospector- α values (middle), and those in Guo et al. (2020; right). The black solid lines are zero-difference relationships, and the black dashed lines represent 0.5 dex offsets. The red lines are LOESS curves for galaxies in the left and middle panels and all the sources in the right panel. The numerical comparison results are displayed in Table 7. Our measurements are generally consistent with others; though a small mass-dependent offset exists between ours and the Prospector- α values.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: The rest-frame ﹩{L}_{6\,\mu {\rm{m}}}^{\mathrm{AGN}}\mbox{--}{L}_{{\rm{X}},\mathrm{obs}}﹩ relation of AGNs and refined SED AGN candidates, where the L X,obs upper limits are adopted for sources undetected in X-ray. Only sources whose best-fit SEDs have nonzero AGN contributions are shown. The standard relation in Stern (2015) is also displayed as a comparison.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: Comparisons between our corrected M ⋆ and SFR (Equations (23) and (24)) and the Prospector- α values. Galaxies generally follow one-to-one relations well while there are still systematic offsets for AGNs, possibly because the Prospector- α fitting attributes some AGN emission to the galaxy component.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: Comparisons between our original SED-based SFRs and FIR-based SFRs, where the left and right panels show the original and corrected FIR-based SFRs, respectively. The original FIR-based SFRs suffer from the old-star heating bias and thus are overestimated for low-SFR galaxies. After correcting this issue, our FIR-based and SED-based SFRs are generally consistent for both galaxies and AGNs across a wide SFR range.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: The cyan points are all of our sources in the M ⋆–SFR plane, which pile up together and visually form linear cuts as the black lines. The black solid and dashed lines correspond to the maximum sSFR allowed (10−7.70 and 10−7.18 yr−1) for our normal-galaxy and BQ-galaxy SFHs, respectively. When only plotting the results from the normal-galaxy fits, all the points will be constrained to lie below the black solid line. The yellow and blue bands represent the 16th–84th and 2.5th–97.5th percentile ranges of sSFR for our star-forming galaxies, respectively. The red curves are the MS at z = 0, 1, and 6. All the bands and MS curves are far below the sSFR limits, and thus the apparent sSFR cut does not cause problems.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: Comparison of M ⋆ (left) and SFR (right) between the SED fitting with weighted and unweighted X-ray data for X-ray AGNs. The black dashed lines represent 0.5 dex offsets from the one-to-one relationships, and the red lines, which visually overlap with the one-to-one lines, are LOESS curves of the points. The inferences about host-galaxy properties are generally not affected by the weighting.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: Comparison between our M ⋆ and SFR results for star-forming galaxies and the MS in Popesso et al. (2022) in seven redshift bins. The SFRs at the lowest redshift are not shifted (i.e., const. = 0), and the subsequent SFRs at higher redshifts are progressively shifted upward by 1 dex for a better visualization. The solid lines are the MS at the median redshift of each redshift bin, as marked explicitly in the figure, and the transparent bands represent ≤0.5 dex offset from the MS. The points are the median M ⋆ and shifted SFR values in several M ⋆ bins of our star-forming galaxies and are generally consistent with the MS curves.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: Comparison of f AGN between the SED fitting with and without X-ray upper limits for all the X-ray-undetected sources. The black line is the one-to-one relationship. X-ray upper limits can help constrain the decomposed AGN power to a lower level.
Paper: Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties
Authors: Fan Zou, W. N. Brandt, Chien-Ting Chen, Joel Leja, Qingling Ni, Wei Yan, Guang Yang, Shifu Zhu, Bin Luo, Kristina Nyland, Fabio Vito, Yongquan Xue
Figure caption: The typical decomposed SED of quasars, constructed from 424 BL quasars in W-CDF-S. This SED is plotted in the same way as for Figure 10, where the cyan and red solid lines represent the galaxy and AGN components, respectively.