adsabs/AstroCLIMB huggingface dataset:
Paper: Using a Quench Level Approximation to Estimate the Effect of Metallicity on the Abundances of N-bearing Species in H2-dominated Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The color bar shows the mole fraction of quenched HCN in the log10 scale as a function of pressure and temperature. The different panels represent the different values of g surface (5, 15, 45 m s−2) and K  zz  (108, 1010, 1012 cm2 s−1), which are labeled in the panel.
Paper: Spectra of V1405 Cas at the Very Beginning Indicate a Low-mass ONeMg White Dwarf Progenitor
Authors: Kenta Taguchi, Keiichi Maeda, Hiroyuki Maehara, Akito Tajitsu, Masayuki Yamanaka, Akira Arai, Keisuke Isogai, Masaaki Shibata, Yusuke Tampo, Naoto Kojiguchi, Daisaku Nogami, Taichi Kato
Figure caption: Enlarged views of the HDS spectrum on t = +53.53 hr. (a) 4580–4700 Å (Section 3.3.1). (b) 5660–5740 Å (Section 3.3.2). (c) 6180–6400 Å (Section 3.3.3).
Paper: Spectra of V1405 Cas at the Very Beginning Indicate a Low-mass ONeMg White Dwarf Progenitor
Authors: Kenta Taguchi, Keiichi Maeda, Hiroyuki Maehara, Akito Tajitsu, Masayuki Yamanaka, Akira Arai, Keisuke Isogai, Masaaki Shibata, Yusuke Tampo, Naoto Kojiguchi, Daisaku Nogami, Taichi Kato
Figure caption: The light curves of V1405 Cas. (a) V and I magnitudes provided by AAVSO are shown by the green-filled circles and magenta-filled diamonds, respectively. The black open pentagons show the pre-discovery magnitude by the NMW survey and the discovery magnitude by Nakamura. (b) An enlarged view of the initial phase (2,459,291 < JD < 2,459,296, the shaded region in the panel a. The dashed lines show the epochs of spectroscopic observations listed in Table 1, with the same color coordinate used to show our spectra in Figures 2 and 4.
Paper: Using a Quench Level Approximation to Estimate the Effect of Metallicity on the Abundances of N-bearing Species in H2-dominated Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: Same as Figure B1, but for NH3.
Paper: Using a Quench Level Approximation to Estimate the Effect of Metallicity on the Abundances of N-bearing Species in H2-dominated Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: Same as Figure B1, but for 10× solar metallicity.
Paper: Using a Quench Level Approximation to Estimate the Effect of Metallicity on the Abundances of N-bearing Species in H2-dominated Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: Same as Figure B1, but for 0.1× solar metallicity.
Paper: Deciphering the Pre–solar-storm Features of the 2017 September Storm From Global and Local Dynamics
Authors: Breno Raphaldini, Mausumi Dikpati, Aimee A. Norton, Andre S. W. Teruya, Scott W. McIntosh, Christopher B. Prior, David MacTaggart
Figure caption: Evolution of the magnetic toroid pattern during CR 2193 (2017 July 20–August 16), CR 2194 (2017 August 16–September 12), and CR 2195 (2017 September 12–October 10), i.e., from one CR before through the storm to one CR after, during which AR 12673, located at 120° longitude in the south (yellow circled region), produced the two biggest flares (X-9.3 and X-8.2) of cycle 24, during the late declining phase near solar minimum.
Paper: Deciphering the Pre–solar-storm Features of the 2017 September Storm From Global and Local Dynamics
Authors: Breno Raphaldini, Mausumi Dikpati, Aimee A. Norton, Andre S. W. Teruya, Scott W. McIntosh, Christopher B. Prior, David MacTaggart
Figure caption: Accumulation of magnetic helicity (top) and magnetic winding (bottom) for AR 12673. Purple and beige backgrounds indicate first and second major emergences, respectively. Here, the start time is 2017 August 28, 09:00.
Paper: A Low-mass line-rich Core Found in Massive Star-forming Region IRAS 16351-4722
Authors: Meizhu Liu, Sheng-Li Qin, Tie Liu, Mengyao Tang, Sheng-Yuan Liu, Li Chen, ChuanShou Li, HongQiong Shi, Xiaohu Li, Tianwei Zhang, Ken'ichi Tatematsu, Fengwei Xu, Yuefang Wu
Figure caption: 870  μm continuum emission map of I16351 from the ALMA Band 7 observations in color scale and with black contours, overlaid with the 3 mm continuum in the white contours. The synthesized beam size is shown in the bottom left corner. The black contours start at a level of 8σ = 0.0104 Jy beam−1 and increase in the following power-law function, D = 4 × N p +8, where D is the dynamical range of the intensity map as follows: 0.0104, 0.0156, 0.0267, 0.0423, 0.0614, 0.0841, 0.1099, 0.1386, 0.1701, 0.2043, 0.2411, 0.2803, 0.3219, 0.3658, and 0.4119 Jy beam−1. The p of 1.6 is the power index, while N = 15 is the number of contours used. The white contour levels are [3%, 6%, 10%, 30%, 50%, 70%, 90%]× peak integrated intensities (F peak = 0.1193 Jy beam−1 km−1). The crosses show the peak positions of each core.
Paper: A Low-mass line-rich Core Found in Massive Star-forming Region IRAS 16351-4722
Authors: Meizhu Liu, Sheng-Li Qin, Tie Liu, Mengyao Tang, Sheng-Yuan Liu, Li Chen, ChuanShou Li, HongQiong Shi, Xiaohu Li, Tianwei Zhang, Ken'ichi Tatematsu, Fengwei Xu, Yuefang Wu
Figure caption: Sample spectra in spw31 and spw29 toward the hot core and the low-mass line-rich core. The segments of spw31 and spw29 cover the frequency range from 342 to 346 GHz. The frequency scale is in terms of the rest frequency. The black curves are the observed spectra and the red curves indicate the simulated LTE spectra.
Paper: A Low-mass line-rich Core Found in Massive Star-forming Region IRAS 16351-4722
Authors: Meizhu Liu, Sheng-Li Qin, Tie Liu, Mengyao Tang, Sheng-Yuan Liu, Li Chen, ChuanShou Li, HongQiong Shi, Xiaohu Li, Tianwei Zhang, Ken'ichi Tatematsu, Fengwei Xu, Yuefang Wu
Figure caption: Spatial distributions of O-, N-, and S-bearing molecules. The black contour levels are [1%, 2%, 3%, 10%, 20%, 30%, 40%, 50%, 60%, 70%, 80%, 90%]× peak integrated intensities(Fpeak). The color scale background shows the continuum emission at 0.87 mm. The synthetic beam for the continuum is indicated in the bottom left corner by the blue ellipse. The value of the upper-level energy E  u  for each species is shown in the bottom of each panel.
Paper: A Low-mass line-rich Core Found in Massive Star-forming Region IRAS 16351-4722
Authors: Meizhu Liu, Sheng-Li Qin, Tie Liu, Mengyao Tang, Sheng-Yuan Liu, Li Chen, ChuanShou Li, HongQiong Shi, Xiaohu Li, Tianwei Zhang, Ken'ichi Tatematsu, Fengwei Xu, Yuefang Wu
Figure caption: Fractional abundances of different molecules relative to H2 in I16351 and the other hot cores and hot corinos listed in Tables B1 and B2.
Paper: High-altitude Spider-type Prominence above the Magnetic Null Point
Authors: Boris Filippov
Figure caption: Fragment of the SDO/AIA image taken in the 211 Å channel on February 15 at 07:10 UT (a), SDO/HMI magnetogram of the same area (b), and the same image with superposed PILs at the height of 66 Mm (red lines). Green marks show the section of the PIL with the upward-directed curvature of field lines. (Courtesy of the SDO/AIA and SDO/HMI science teams).
Paper: High-altitude Spider-type Prominence above the Magnetic Null Point
Authors: Boris Filippov
Figure caption: Changes of the prominence visibility during the day on 2023 February 15 observed in the SDO/AIA 193 Å channel. Green arrows show the position of the prominence; blue arrows show long coronal loops related to the prominence.
Paper: High-altitude Spider-type Prominence above the Magnetic Null Point
Authors: Boris Filippov
Figure caption: The passage of the prominence through the solar disk from the east limb to the west limb observed in the SDO/AIA 193 Å channel. Green arrows show the position of the prominence at limbs and the corresponding filament on the disk.
Paper: High-altitude Spider-type Prominence above the Magnetic Null Point
Authors: Boris Filippov
Figure caption: PILs of the potential magnetic field at different heights. Green marks show the sections of PILs with the upward-directed curvature of field lines.
Paper: High-altitude Spider-type Prominence above the Magnetic Null Point
Authors: Boris Filippov
Figure caption: Hα images of the prominence at the eastern limb (a), close to the central meridian (b), and at the western limb (c). (Courtesy of the Cerro Tololo Inter-American Observatory, Chile).
Paper: ΣSFR–M ∗ Diagram: A Valuable Galaxy Evolution Diagnostic to Complement (s)SFR–M ∗ Diagrams
Authors: Samir Salim, Sandro Tacchella, Chandler Osborne, S. M. Faber, Janice C. Lee, Sara L. Ellison
Figure caption: The placement of galaxies separated into star-forming, transitional, and quenched (quiescent) categories on various diagrams with stellar mass on the x-axis. Panels from left to right demonstrate the successive improvements in the ability to separate these categories afforded by moving from optical to UV–optical color and then to sSFR. Specific SFRs provide a good separation between these categories, but the use of ΣSFR (based on which these categories have been defined) goes an additional step by eliminating the effect of age on the main sequence (its tilt).
Paper: ΣSFR–M ∗ Diagram: A Valuable Galaxy Evolution Diagnostic to Complement (s)SFR–M ∗ Diagrams
Authors: Samir Salim, Sandro Tacchella, Chandler Osborne, S. M. Faber, Janice C. Lee, Sara L. Ellison
Figure caption: Diagrams of the sSFR vs. stellar mass based on three measures of the SFR. All panels include the same, main-sequence galaxies. The left panel uses integrated sSFRs from the SED fitting (nominal values in this work). The running average is shown as a red line. The middle panel uses sSFRs from the Balmer-decrement-corrected Hα emission. The right panel uses SFRs from the MPA/JHU catalog. In the middle and right panels the running average is shown as an orange line, and the running average from the left panel is repeated for reference.
Paper: ΣSFR–M ∗ Diagram: A Valuable Galaxy Evolution Diagnostic to Complement (s)SFR–M ∗ Diagrams
Authors: Samir Salim, Sandro Tacchella, Chandler Osborne, S. M. Faber, Janice C. Lee, Sara L. Ellison
Figure caption: Differences in inferences regarding a galaxy’s SF based on whether the sSFR or ΣSFR is considered. The left panels correspond to LEDA 1793, whereas the right panels show UGC 5965. The upper panels present optical images from SDSS and the lower panels are UV images from GALEX. UGC 5965 has a red center, but its central SFR surface density is as high as that of LEDA 1793, which is blue and has a high central sSFR. Quantities are based on dust-corrected Hα and correspond to the 3″ SDSS fiber, shown as a circle. The SDSS images are taken from SkyServer, whereas the GALEX images (FUV plus NUV composites) are from the Legacy Survey Sky Browser.
Paper: Resolved Star Formation in TNG100 Central and Satellite Galaxies
Authors: Bryanne McDonough, Olivia Curtis, Tereasa G. Brainerd
Figure caption: Left: global star-forming main sequence for resolved TNG100 galaxies, where global star formation rate is plotted against stellar mass (measured as the sum of all stellar particles bound to the subhalo). Galaxies that have not experienced any new star formation in the last 100 Myr are assigned a fixed value of sSFR = 10−12 yr−1 with some scatter. Point color is determined by ΔSFR, the mean logarithmic distance to the global main sequence (magenta line). Shaded areas indicate the classification of galaxies in that region (starburst—purple, main sequence—blue, green valley—green, and quenched—white). Right: distribution of ΔSFR values. Colored regions indicate where galaxies are classified as starburst (purple), main sequence (blue), green valley (green), and quenched (red).
Paper: Data-constrained Magnetohydrodynamic Simulation of an Intermediate Solar Filament Eruption
Authors: Yang Guo, Jinhan Guo, Yiwei Ni, M. D. Ding, P. F. Chen, Chun Xia, Rony Keppens, Kai E. Yang
Figure caption: Kinematics of the erupting filament in observation and flux rope in MHD simulation. (a) The purple line overplotted on the SDO/AIA 171 Å image at 03:00 UT indicates the slice that we choose to measure the time–distance profile of the erupting filament. Red dots are one example of measurements of the filament positions from 03:00 to 03:44 UT. (b) The purple line overplotted on the MHD simulation at 03:24 UT indicates the slice that we choose to measure the velocity of the erupting magnetic flux rope. Yellow dots are one example of measurements of the flux rope positions from 03:00 to 03:44 UT. (c) Red dots and vertical line segments represent the positions and errors measured from the observation of SDO/AIA 171 Å wave band. Yellow dots and vertical line segments represent the positions and errors measured from the MHD simulation. The blue and cyan lines are linear fittings to the time–distance profile of the filament and flux rope at the fast erupting stage, which lead to speeds of 521.8 km s−1 and 200.6 km s−1, respectively.
Paper: Data-constrained Magnetohydrodynamic Simulation of an Intermediate Solar Filament Eruption
Authors: Yang Guo, Jinhan Guo, Yiwei Ni, M. D. Ding, P. F. Chen, Chun Xia, Rony Keppens, Kai E. Yang
Figure caption: Path of the filament. (a) Filament in the SDO/AIA 304 Å image at 03:00 UT. Green diamonds represent the projected path of the filament body on the solar surface. (b) Projected path overlaid on SDO/HMI magnetic field at 03:00 UT. Green and yellow filled circles represent the two footpoints of the filament. Red and blue lines depict the projected path of the filament on the solar surface.
Paper: Data-constrained Magnetohydrodynamic Simulation of an Intermediate Solar Filament Eruption
Authors: Yang Guo, Jinhan Guo, Yiwei Ni, M. D. Ding, P. F. Chen, Chun Xia, Rony Keppens, Kai E. Yang
Figure caption: Heliocentric coordinate system and the local coordinate system of the filament. Point O is located at the center of the Sun, the x-axis points to the central meridian on the Sun’s back side and on the equator, the y-axis points to the east solar limb and on the equator, and the z-axis constitutes a right-hand system together with the x- and y-axes. ﹩O^{\prime} ﹩ is located at the middle point of the two footpoints (indicated by the two blue dots F1 and F2) of the filament on the photosphere, the X-axis is perpendicular to both ﹩{OO}^{\prime} ﹩ and the line joining the two footpoints, the Y-axis is parallel to the line joining the two footpoints, and the Z-axis constitutes a right-hand system together with the X- and Y-axes and pointing radially outward.
Paper: Data-constrained Magnetohydrodynamic Simulation of an Intermediate Solar Filament Eruption
Authors: Yang Guo, Jinhan Guo, Yiwei Ni, M. D. Ding, P. F. Chen, Chun Xia, Rony Keppens, Kai E. Yang
Figure caption: MHD model overlaid on SDO/AIA 193 Å observations. (a), (c), and (e) Background images show the 193 Å observations at 03:00, 03:35, and 03:42 UT from top to bottom panels. Colored lines represent the magnetic field lines in the MHD model. (b), (d), and (f) SDO/AIA 193 Å images highlighting the erupting filament indicated by the cyan arrows at 03:00, 03:35, and 03:42 UT from top to bottom panels.
Paper: Coherent Cherenkov Radiation by Bunches in Fast Radio Bursts
Authors: Ze-Nan Liu, Jin-Jun Geng, Yuan-Pei Yang, Wei-Yang Wang, Zi-Gao Dai
Figure caption: The normalized radiated power spectrum of an individual electron for CR and ChR. The solid red line denotes the CR (ρ = 107cm, γ  e  = 100), and the blue lines denote the ChR. The solid blue line, blue dashed line, and blue dotted line indicate radiation radii R = 107 cm, γ  e /γ  p  = 50, R = 2 × 107 cm, γ  e /γ  p  = 50, and R = 107 cm, γ  e /γ  p  = 10, respectively. We adopt the below physical parameters: ξ = 100, B  s  = 1015 G, and P = 1 s.
Paper: Coherent Cherenkov Radiation by Bunches in Fast Radio Bursts
Authors: Ze-Nan Liu, Jin-Jun Geng, Yuan-Pei Yang, Wei-Yang Wang, Zi-Gao Dai
Figure caption: The coherence factor as a function of frequency for ChR. The upper, middle, and bottom panels denote ω  c  < ω  l , ω  c  ≃ ω  l , and ω  c  > ω  l , respectively.
Paper: Calibrating VLBI Polarization Data Using GPCAL. I. Frequency-dependent Calibration
Authors: Jongho Park, Keiichi Asada, Do-Young Byun
Figure caption: Comparison of the ground-truth D-term components (real and imaginary parts) assumed in the synthetic data sets shown on the x-axis with the reconstructed D-term components derived by the method shown on the y-axis for each frequency channel. Each station’s result is presented using distinct colors. For each antenna, the correlation between the actual and estimated D-term components is shown in units of percentage. The norm L 1 ≡ ∣D Truth − D Recon∣ is averaged over the real and imaginary components of the D-terms for RCP and LCP for all antennas, and is denoted in each panel.
Paper: Coherent Cherenkov Radiation by Bunches in Fast Radio Bursts
Authors: Ze-Nan Liu, Jin-Jun Geng, Yuan-Pei Yang, Wei-Yang Wang, Zi-Gao Dai
Figure caption: A geometric sketch of the FRBs produced by coherent ChR. Some relativistic particles are emitted from the polar cap of a magnetar and move along the field lines through a charge-separated magnetic plasma, emitting coherent ChR along the way. The relativistic particles lie on the top of the cone, and the black arrows denote the radiation direction. The electric vector lies in the plane formed by the particle velocity and radiation direction, perpendicular to the radiation direction.
Paper: Local Star-forming Galaxies Build Up Central Mass Concentration Most Actively near M ∗ = 1010 M ⊙ 
Authors: Zhizheng Pan, Xianzhong Zheng, Xu Kong
Figure caption: Left: the luminosity-weighted age gradient as a function of M * for SFGs. The mean age gradient is marked by the blue dashed line. Large symbols show the median ∇age values of each stellar mass bin, with a bin size of ΔM * = 0.2  dex. The shaded region indicates the 16–84 percentile region. Right: violin plot showing the distribution of F positive at each stellar mass bin.
Paper: Local Star-forming Galaxies Build Up Central Mass Concentration Most Actively near M ∗ = 1010 M ⊙ 
Authors: Zhizheng Pan, Xianzhong Zheng, Xu Kong
Figure caption: Left: the R e−M * relation, color-coded by the luminosity-weighted stellar age gradient (with LOESS smoothing). Large symbols show the median R e values of each stellar mass bin, with a bin size of ΔM * = 0.2 dex. The two dashed lines indicate the 16–84 percentile region. Right: Sérsic index n as a function of M *, with LOESS smoothing. Symbols are color-coded by luminosity-weighted stellar age gradient.
Paper: Local Star-forming Galaxies Build Up Central Mass Concentration Most Actively near M ∗ = 1010 M ⊙ 
Authors: Zhizheng Pan, Xianzhong Zheng, Xu Kong
Figure caption: Left: the logSFR−logM * plane. Symbols are color-coded by the luminosity-weighted stellar age gradient. The dashed line indicates log sSFR = 10−11 yr−1, and SFGs are selected as those with SFRs above the line. Right: a LOESS-smoothed version of the left panel.
Paper:  r-process Abundance Patterns in the Globular Cluster M92
Authors: Evan N. Kirby, Alexander P. Ji, Mikhail Kovalev
Figure caption: Correlations between the neutron-capture elements Y, Ba, La, and Eu. The top two rows show M92 by itself. The linear Pearson correlation coefficient, r measured, is given in the upper left of each panel. Each panel also includes r(0), an estimate of the correlation coefficient if the scatter in the points was due entirely to their individual covariances, represented by the ellipses. Another test of correlation is θ LEO−Py, the slope of the best-fit line taking covariance into account. The bottom two rows show M92 with measurements of M15 from the literature (Sobeck et al. 2011; Worley et al. 2013). The dashed lines show the solar r-process pattern (Simmerer et al. 2004). The symbols (evolutionary state) and colors (T eff) have the same meaning as in Figure 1. M92 stars in the sample of Cohen (2011) are outlined in black in the top two rows.
Paper:  r-process Abundance Patterns in the Globular Cluster M92
Authors: Evan N. Kirby, Alexander P. Ji, Mikhail Kovalev
Figure caption: Light-element abundance anticorrelations for giant stars in M92. The ellipses represent the 1σ uncertainties, including covariance. The dashed lines in the indicate the division between first- and second-generation stars (1G and 2G).
Paper:  r-process Abundance Patterns in the Globular Cluster M92
Authors: Evan N. Kirby, Alexander P. Ji, Mikhail Kovalev
Figure caption: Same as Figure 11 but for other lanthanides (Nd, Sm, Eu, and Dy).
Paper:  r-process Abundance Patterns in the Globular Cluster M92
Authors: Evan N. Kirby, Alexander P. Ji, Mikhail Kovalev
Figure caption: First-peak neutron-capture abundances (Sr, Y, and Zr) vs. light-element abundances (Na and Mg). The dashed lines indicate the division between 1G and 2G. Stars included in Cohen (2011) sample are outlined in black, but the abundance measurements are ours.
Paper:  r-process Abundance Patterns in the Globular Cluster M92
Authors: Evan N. Kirby, Alexander P. Ji, Mikhail Kovalev
Figure caption: Trends of abundance with luminosity (bottom axis) or surface gravity (top axis). The red lines show fits to the trend, as described in Section 4.6. For the remainder of this work, the abundances are detrended such that the correction at M  G,0 = 0 (dotted gray line) is zero. Elements without red trend lines were not corrected. The dashed blue lines show the median abundances before the luminosity correction. The polynomial terms of the trend are shown in parentheses.
Paper:  r-process Abundance Patterns in the Globular Cluster M92
Authors: Evan N. Kirby, Alexander P. Ji, Mikhail Kovalev
Figure caption: Keck/HIRES archival spectra of giant stars in M92. The spectra in each row are grouped by T eff. The stars have T eff within 25 K of 4400 K (top), 4550 K (middle), and 4670 K (bottom). AGB stars are indicated with asterisks in their names. Abundances of Fe, Ba, and Eu are given. The absorption lines Eu II λ4130, Eu II λ4205, and Ba II λ5854 are particularly variable.
Paper:  r-process Abundance Patterns in the Globular Cluster M92
Authors: Evan N. Kirby, Alexander P. Ji, Mikhail Kovalev
Figure caption: The evolution of Li, C, and O abundances in M92 with stellar luminosity. The Li abundances in M92 are compared to those in NGC 6397 (Lind et al. 2009).
Paper:  r-process Abundance Patterns in the Globular Cluster M92
Authors: Evan N. Kirby, Alexander P. Ji, Mikhail Kovalev
Figure caption: Potassium vs. sodium (left) and magnesium (right) abundances in M92. The dashed lines indicate the division between 1G and 2G stars.
Paper:  r-process Abundance Patterns in the Globular Cluster M92
Authors: Evan N. Kirby, Alexander P. Ji, Mikhail Kovalev
Figure caption: Same as Figure 10 but for barium and some of the lanthanides (Ba, La, and Ce).
Paper: Identification of Superclusters and Their Properties in the Sloan Digital Sky Survey Using the WHL Cluster Catalog
Authors: Shishir Sankhyayan, Joydeep Bagchi, Elmo Tempel, Surhud More, Maret Einasto, Pratik Dabhade, Somak Raychaudhury, Ramana Athreya, Pekka Heinämäki
Figure caption: (a) Distribution of the superclusters’ mass and size. (b) Distribution of the superclusters’ mass and redshift. (c) Density contrast of the superclusters as a function of size. The blue dots represent the superclusters, the solid black line is a linear fit to the data points on the log–log plot, and the shaded black region denotes the associated errors in the fit. The slope of the fitted line is given at the top right corner of the plot.
Paper: Identification of Superclusters and Their Properties in the Sloan Digital Sky Survey Using the WHL Cluster Catalog
Authors: Shishir Sankhyayan, Joydeep Bagchi, Elmo Tempel, Surhud More, Maret Einasto, Pratik Dabhade, Somak Raychaudhury, Ramana Athreya, Pekka Heinämäki
Figure caption: Sky distribution of the WHL clusters and HR4 halos within 0.05 ≤ z ≤ 0.366. The WHL clusters and HR4 halos are the observed and mock samples, respectively.