adsabs/AstroCLIMB huggingface dataset:
Paper: Central Massive Black Holes Are Not Ubiquitous in Local Low-mass Galaxies
Authors: Fan Zou, Elena Gallo, Anil C. Seth, Edmund Hodges-Kluck, David Ohlson, Tommaso Treu, Vivienne F. Baldassare, W. N. Brandt, Jenny E. Greene, Piero Madau, Dieu D. Nguyen, Richard M. Plotkin, Amy E. Reines, Alberto Sesana, Jong-Hak Woo, Jianfeng Wu
Figure caption: Visual illustration of the chosen parameterization for focc (left; Equation (2)) and p(λ) (right; Equation (7)). Left: in this plot, ﹩{\mathrm{log}}\,{M}_{0}=9.5﹩. The black horizontal line represents the limiting focc as δ → 0 for any θ. The other black curves correspond to δ → +∞ at different θ values, reaching focc = 1 at ﹩{\mathrm{log}}\,{M}_{\star }={\mathrm{log}}\,{M}_{0}﹩. The colored curves show how focc evolves with δ when θ = 1. As δ increases, the curve becomes less flat and approaches the corresponding limiting black curve for θ = 1. Right: the plot illustrates p(λ) for different (μ, σ, ξ) values, as indicated in the legend. When ξ = 1, p(λ) is a normal distribution, shown by the black curve. The blue and orange curves have different ξ values, resulting in heavier tails: on the left when ξ > 1 and on the right when ξ < 1. The green curve, compared to the orange curve, demonstrates that σ controls the width of p(λ). The red curve shows that our p(λ) can mimic a power-law distribution over the plotted ﹩{\mathrm{log}}\,\lambda ﹩ range when both μ and ξ are small.
Paper: Central Massive Black Holes Are Not Ubiquitous in Local Low-mass Galaxies
Authors: Fan Zou, Elena Gallo, Anil C. Seth, Edmund Hodges-Kluck, David Ohlson, Tommaso Treu, Vivienne F. Baldassare, W. N. Brandt, Jenny E. Greene, Piero Madau, Dieu D. Nguyen, Richard M. Plotkin, Amy E. Reines, Alberto Sesana, Jong-Hak Woo, Jianfeng Wu
Figure caption: Sampling results. Contours represent 68% and 95% levels; grayscale pixels represent probabilities, and the rasterized points outside the 95% contours are individual sampling points. The first three parameters, ﹩({\mathrm{log}}\,{M}_{0},\delta ,\theta )﹩, represent the dependence of focc on M⋆ (Equation (2)), as illustrated in the left panel of Figure 3. α represents the typical ﹩{\mathrm{log}}\,\lambda ﹩ of galaxies with M⋆ = 1010 M⊙, and β is the slope of the mass dependence of the SARDF (Equation (9)). ξ and σ control the shape of p(λ) (Equation (7)), as shown in the right panel of Figure 3. The fitted β is consistent with zero, indicating that p(λ) has little dependence on M⋆. The fitted ξ is ≪1, suggesting that p(λ) is highly right-skewed compared to normal distributions.
Paper: Central Massive Black Holes Are Not Ubiquitous in Local Low-mass Galaxies
Authors: Fan Zou, Elena Gallo, Anil C. Seth, Edmund Hodges-Kluck, David Ohlson, Tommaso Treu, Vivienne F. Baldassare, W. N. Brandt, Jenny E. Greene, Piero Madau, Dieu D. Nguyen, Richard M. Plotkin, Amy E. Reines, Alberto Sesana, Jong-Hak Woo, Jianfeng Wu
Figure caption: Nuclear X-ray luminosity vs. M⋆. Blue points represent sources with compact X-ray nuclei, with increased color transparency reflecting an increasing likelihood of XRB contamination to the signal. Most of the blue points are not transparent because most sources have low PXRB. Downward orange triangles represent upper limits, which include both nondetections as well as (few) extended sources. The solid red and violet lines are nonparametric, Akritas–Theil–Sen (ATS) regression lines for massive galaxies (with M⋆ > 1010 M⊙) and all the galaxies, respectively. The solid black line represents the best-fit ﹩\mathrm{log}{L}_{{\rm{X}}}﹩ = ﹩{\mathrm{log}}\,{M}_{\star }+\,{\mathrm{log}}\,\lambda ﹩ = ﹩{\mathrm{log}}\,{M}_{\star }+\alpha +\beta ({\mathrm{log}}\,{M}_{\star }-10)﹩ relation (Equation (9)). The shaded region, dashed lines, and dotted lines represent the 1σ, 2σ, and 3σ uncertainties, respectively.
Paper: Central Massive Black Holes Are Not Ubiquitous in Local Low-mass Galaxies
Authors: Fan Zou, Elena Gallo, Anil C. Seth, Edmund Hodges-Kluck, David Ohlson, Tommaso Treu, Vivienne F. Baldassare, W. N. Brandt, Jenny E. Greene, Piero Madau, Dieu D. Nguyen, Richard M. Plotkin, Amy E. Reines, Alberto Sesana, Jong-Hak Woo, Jianfeng Wu
Figure caption: The BHMF, plotted as ϕ(MBH) and MBHϕ(MBH) in the left and right panels, respectively. The right panel highlights the contributions from MBHs at different masses to the total MBH budget. The black curve represents the BHMF based on the occupation fraction derived in this study, with the gray shaded regions indicating the 1σ, 2σ, and 3σ uncertainty ranges, accounting solely for uncertainties in focc. The cyan shaded area illustrates the possible BHMF range derived from F. Shankar et al. (2020b), which is extensive due to the uncertainties in the MBH–M⋆ scaling relation. The effect of a declining focc is to flatten ϕ(MBH) for M⋆ ≲ 106 M⊙.
Paper: Central Massive Black Holes Are Not Ubiquitous in Local Low-mass Galaxies
Authors: Fan Zou, Elena Gallo, Anil C. Seth, Edmund Hodges-Kluck, David Ohlson, Tommaso Treu, Vivienne F. Baldassare, W. N. Brandt, Jenny E. Greene, Piero Madau, Dieu D. Nguyen, Richard M. Plotkin, Amy E. Reines, Alberto Sesana, Jong-Hak Woo, Jianfeng Wu
Figure caption: Example comparison among the likelihood ignoring measurement uncertainties (blue), the likelihood accurately accounting for measurement uncertainties (red), and our adopted approximation (black). All likelihoods are normalized to a maximum value of one. Here, β is varied while all other parameters are fixed at their median posterior values. The near-complete overlap of the black and red curves indicates that our adopted likelihood closely approximates the fully accurate likelihood.
Paper: Central Massive Black Holes Are Not Ubiquitous in Local Low-mass Galaxies
Authors: Fan Zou, Elena Gallo, Anil C. Seth, Edmund Hodges-Kluck, David Ohlson, Tommaso Treu, Vivienne F. Baldassare, W. N. Brandt, Jenny E. Greene, Piero Madau, Dieu D. Nguyen, Richard M. Plotkin, Amy E. Reines, Alberto Sesana, Jong-Hak Woo, Jianfeng Wu
Figure caption: Sampled focc (left) and p(λ) (right) for different types of galaxies separately. In the top panels, the red and blue solid curves represent the median of the posterior distributions for early-type and late-type galaxies, respectively, while in the bottom panels, they represent quiescent and star-forming galaxies, respectively. The black dotted curves correspond to all galaxies, referenced from Figures 6 and 7. The shaded regions indicate the 2σ uncertainty levels.
Paper: Central Massive Black Holes Are Not Ubiquitous in Local Low-mass Galaxies
Authors: Fan Zou, Elena Gallo, Anil C. Seth, Edmund Hodges-Kluck, David Ohlson, Tommaso Treu, Vivienne F. Baldassare, W. N. Brandt, Jenny E. Greene, Piero Madau, Dieu D. Nguyen, Richard M. Plotkin, Amy E. Reines, Alberto Sesana, Jong-Hak Woo, Jianfeng Wu
Figure caption: Local black hole occupation fraction constraints from Chandra ACIS imaging observations of 1606 galaxies within 50 Mpc. The black solid curve is the median of our sampling results; the dashed, dashed–dotted, dotted curves, and their corresponding shaded regions enclose the 1σ, 2σ, and 3σ ranges, respectively. The 1σ measurements in M15 and B25 are also shown for comparison. Our focc quickly drops down when M⋆ decreases below 1010 M⊙ and is below unity at a statistically significant level for low-mass galaxies.
Paper: Central Massive Black Holes Are Not Ubiquitous in Local Low-mass Galaxies
Authors: Fan Zou, Elena Gallo, Anil C. Seth, Edmund Hodges-Kluck, David Ohlson, Tommaso Treu, Vivienne F. Baldassare, W. N. Brandt, Jenny E. Greene, Piero Madau, Dieu D. Nguyen, Richard M. Plotkin, Amy E. Reines, Alberto Sesana, Jong-Hak Woo, Jianfeng Wu
Figure caption: M⋆ vs. distance for the target sample of 1606 galaxies. Blue and orange points represent X-ray-detected and undetected galaxies, respectively. There are points visually “piling up” at a distance of 16.5 Mpc because they are from the Virgo Cluster (see Section 3.3 in D. Ohlson et al. 2024).
Paper: JADES-GS-z14-1: A Compact, Faint Galaxy at z ≈ 14 with Weak Metal Lines from Extremely Deep JWST MIRI, NIRCam, and NIRSpec Observations
Authors: Zihao Wu, Daniel J. Eisenstein, Benjamin D. Johnson, Peter Jakobsen, Stacey Alberts, Santiago Arribas, William M. Baker, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Jacopo Chevallard, Mirko Curti, Emma Curtis-Lake, Francesco D'Eugenio, Kevin Hainline, Jakob M. Helton, Tiger Yu-Yang Hsiao, Xihan Ji, Zhiyuan Ji, Tobias J. Looser, George Rieke, Pierluigi Rinaldi, Brant Robertson, Jan Scholtz, Fengwu Sun, Sandro Tacchella, James A. A. Trussler, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok, Yongda Zhu
Figure caption: The data, model, and residual for JADES-GS-z14-1 and foreground galaxies across multiple NIRCam bands and the MIRI F770W band. Each panel shows a stack of 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 × 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 exposure cutouts centered on JADES-GS-z14-1. NIRCam images are shown using false-color stacking with filters assigned to each color channel as annotated on the right. The models are the best-fit Sérsic profiles convolved with the PSF in each band. Model parameters are inferred from ForcePho fitting and are the same across all bands. Images are oriented with north up and east to the left. A scale bar is shown in the lower right panel.
Paper: JADES-GS-z14-1: A Compact, Faint Galaxy at z ≈ 14 with Weak Metal Lines from Extremely Deep JWST MIRI, NIRCam, and NIRSpec Observations
Authors: Zihao Wu, Daniel J. Eisenstein, Benjamin D. Johnson, Peter Jakobsen, Stacey Alberts, Santiago Arribas, William M. Baker, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Jacopo Chevallard, Mirko Curti, Emma Curtis-Lake, Francesco D'Eugenio, Kevin Hainline, Jakob M. Helton, Tiger Yu-Yang Hsiao, Xihan Ji, Zhiyuan Ji, Tobias J. Looser, George Rieke, Pierluigi Rinaldi, Brant Robertson, Jan Scholtz, Fengwu Sun, Sandro Tacchella, James A. A. Trussler, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok, Yongda Zhu
Figure caption: NIRSpec prism spectra of JADES-GS-z14-1, with resolving power of 30 ≲ R ≲ 300. (a) Combined 1D spectrum from all observations under PID 1287 and PID 5997. The shaded area in light blue shows the 1σ uncertainty. Vertical dashed lines indicate the expected positions of major emission lines at redshift z = 13.86. No emission lines are detected above 3σ significance. A tentative signal of O III] λλ1661, 1666 is observed at 2.3σ for z = 13.80 and one of C III] λ1908 at 1.9σ for z = 13.75. (b) NIRCam false-color image with overlaid slit positions for PIDs 1287 and 5997. (c)–(e) Individual spectra from (c) PID 1287 first and third dithers, (d) PID 1287 second dither, and (e) PID 5997, after slit-loss correction based on NIRCam photometry. Each panel displays the 1D extracted spectrum at the top and the 2D map of the signal-to-noise ratio (SNR) at the bottom.
Paper: JADES-GS-z14-1: A Compact, Faint Galaxy at z ≈ 14 with Weak Metal Lines from Extremely Deep JWST MIRI, NIRCam, and NIRSpec Observations
Authors: Zihao Wu, Daniel J. Eisenstein, Benjamin D. Johnson, Peter Jakobsen, Stacey Alberts, Santiago Arribas, William M. Baker, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Jacopo Chevallard, Mirko Curti, Emma Curtis-Lake, Francesco D'Eugenio, Kevin Hainline, Jakob M. Helton, Tiger Yu-Yang Hsiao, Xihan Ji, Zhiyuan Ji, Tobias J. Looser, George Rieke, Pierluigi Rinaldi, Brant Robertson, Jan Scholtz, Fengwu Sun, Sandro Tacchella, James A. A. Trussler, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok, Yongda Zhu
Figure caption: Flux densities of JADES-GS-z14-1 from JWST/NIRCam imaging in 2022, 2023, and 2024, shown across 16 filters spanning observed wavelengths from 0.7 to 4.8 μm. Blue circles, red squares, and orange hexagons represent measurements from 2022, 2023, and 2024, respectively. Wide-band filters are shown with filled markers and medium-band filters with open markers. Flux values from exposures with total integration time below one hour are excluded. For visual clarity, 2023 and 2024 data points are shifted by +0.05 and +0.10 μm, respectively, along the wavelength axis. All observations were conducted between October and December of each year. Flux densities from the NIRCam A and B modules are averaged within each year.
Paper: JADES-GS-z14-1: A Compact, Faint Galaxy at z ≈ 14 with Weak Metal Lines from Extremely Deep JWST MIRI, NIRCam, and NIRSpec Observations
Authors: Zihao Wu, Daniel J. Eisenstein, Benjamin D. Johnson, Peter Jakobsen, Stacey Alberts, Santiago Arribas, William M. Baker, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Jacopo Chevallard, Mirko Curti, Emma Curtis-Lake, Francesco D'Eugenio, Kevin Hainline, Jakob M. Helton, Tiger Yu-Yang Hsiao, Xihan Ji, Zhiyuan Ji, Tobias J. Looser, George Rieke, Pierluigi Rinaldi, Brant Robertson, Jan Scholtz, Fengwu Sun, Sandro Tacchella, James A. A. Trussler, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok, Yongda Zhu
Figure caption: Integration time map of the JADES deep MIRI/F770W parallel field. The cross with circle marks the location of JADES-GS-z14-1, which lies in the overlapping region of two pointings and thus has an integrated on-source exposure time of 70.7 hr.
Paper: Selecting Clusters and Protoclusters via Stellar Mass Density. I. Method and Tests on Mock HSC-SSP Catalogs
Authors: Marcelo C. Vicentin, Pablo Araya-Araya, Laerte Sodré, Michael A. Strauss
Figure caption: From left to right: the first row of plots shows the estimated stellar mass (M⋆,phot) of galaxies, σNMAD (Equation (7)), Bias (Equation (8)), and fout (Equation (9)), respectively, as a function of the mock stellar mass (M⋆,true). Gray dots and lines represent all objects from the test sample. Orange (green) dots and lines stand for true mock BCGs with (without) W1 unWISE band information. Red lines stand for all true mock BCGs. Second row of plots shows the results for photometric redshift estimates (zphot) as a function of ztrue, analogous to the stellar mass estimates in the first row. Blue dots and lines denote all objects in the test sample. The purple line represents the results obtained by A. J. Nishizawa et al. (2020). The dashed line in the second plot (σNMAD vs. true) denotes the results obtained by W&H21. Third row of plots is analogous to the second row, now including only BCGs after preselecting galaxies above a given threshold in photometric stellar mass (as described in Section 5.1).
Paper: Selecting Clusters and Protoclusters via Stellar Mass Density. I. Method and Tests on Mock HSC-SSP Catalogs
Authors: Marcelo C. Vicentin, Pablo Araya-Araya, Laerte Sodré, Michael A. Strauss
Figure caption: Number density of structures as a function of redshift in the PCcones mocks. Red (blue) line denotes the median number density of galaxy clusters (protoclusters), while the shaded area is limited by the 16th and 84th percentiles, considering 10 different lightcones with 36 deg2 each. We are defining galaxy clusters as structures with halo mass Mhalo ≥ 1014M⊙ and galaxy protoclusters as structures with halo mass below this threshold, which will surpass this value at some point in their future at z > 0. The large error bars at low redshifts for clusters are primarily due to cosmic variance. At low redshift, the survey volume per unit redshift is smaller, which enhances the impact of large-scale structure fluctuations on the measured cluster number densities.
Paper: Selecting Clusters and Protoclusters via Stellar Mass Density. I. Method and Tests on Mock HSC-SSP Catalogs
Authors: Marcelo C. Vicentin, Pablo Araya-Araya, Laerte Sodré, Michael A. Strauss
Figure caption: BCG i-band magnitude, r − i observed frame color, and stellar mass as function of redshift. For the mocks, we utilized perturbed magnitudes and photometric stellar masses and redshifts (Sections 3.1 and 4.2) for true mock BCGs. Points denote the median properties within a given redshift bin, and the bars are the dispersions bounded by the 16th and 84th percentiles. BCGs from CAMIRA (M. Oguri 2014), W&H21 (Z. L. Wen & J. L. Han 2021), and redMaPPer (E. S. Rykoff et al. 2014) catalogs are represented in the plots by blue, green, and orange colors, respectively, while mock BCGs are denoted by red color. Also, redMaPPer galaxies were cross-matched with the HSC-SSP Wide Survey to compare the measurements in the same photometric system. A slight horizontal shift was applied to the different markers to improve visualization.
Paper: Selecting Clusters and Protoclusters via Stellar Mass Density. I. Method and Tests on Mock HSC-SSP Catalogs
Authors: Marcelo C. Vicentin, Pablo Araya-Araya, Laerte Sodré, Michael A. Strauss
Figure caption: Red (blue) curve denotes mock (RedMaPPer) cumulative statistics for true mock galaxy clusters selected within the same magnitude limit (imag < 21) and at the same observed redshift interval (z < 0.8) as in the RedMaPPer sample from E. S. Rykoff et al. (2014), used here for comparison. Upper plot: Distribution of true mock galaxy clusters as a function of the velocity dispersion, calculated following A. Ferragamo et al. (2020). Bottom plot: Cumulative radial profile of the true mock clusters relative to their BCGs. Shaded area encompasses the 16th and 84th percentiles. In both cases we are using the BCG 3D coordinates (R.A., decl., and redshift) as the center and the distance to the other galaxies is calculated as the angular diameter transverse distance.
Paper: Selecting Clusters and Protoclusters via Stellar Mass Density. I. Method and Tests on Mock HSC-SSP Catalogs
Authors: Marcelo C. Vicentin, Pablo Araya-Araya, Laerte Sodré, Michael A. Strauss
Figure caption: Sample fraction with measured W1 values as a function of the true redshift (left panel) and true stellar mass (right). Blue dots denote all mock objects while red stars represent BCGs.
Paper: Selecting Clusters and Protoclusters via Stellar Mass Density. I. Method and Tests on Mock HSC-SSP Catalogs
Authors: Marcelo C. Vicentin, Pablo Araya-Araya, Laerte Sodré, Michael A. Strauss
Figure caption: Top: Structure’s halo mass functions for different redshift intervals depicted in the legend. The solid line is simply connecting the points, while the dotted lines are modified normal distributions fits. Bottom: Halo mass as a function of the redshift. Each point denotes the halo mass where the modified normal distributions reach their peak. The line denotes a power-law fit with 3 free parameters to these data. The function with the fitted parameters is showed in the upper right of this panel.
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: Fits to C273α emission. The solid red line indicates (the sum of) the fitted components, and the dotted red line indicates the residuals, the data subtracted by the fit.
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: The top row shows 12CO spectra and the bottom row shows 13CO spectra for the corresponding aperture regions. The aperture ID and the number of Gaussian components fit to the spectra are listed in the upper right corner of each plot.
Paper: Selecting Clusters and Protoclusters via Stellar Mass Density. I. Method and Tests on Mock HSC-SSP Catalogs
Authors: Marcelo C. Vicentin, Pablo Araya-Araya, Laerte Sodré, Michael A. Strauss
Figure caption: The top (bottom) panel displays the halo (photometric stellar) mass of selected galaxies as a function of redshift. Red stars, orange triangles, and green inverted triangles denote median values for BCGs, protoBCGs, and field galaxies that were selected with the highest probabilities based on the expected number of BCGs in a given redshift bin. Blue points represent true BCGs that were not selected. A slight horizontal shift was applied to the different markers to improve visualization.
Paper: Selecting Clusters and Protoclusters via Stellar Mass Density. I. Method and Tests on Mock HSC-SSP Catalogs
Authors: Marcelo C. Vicentin, Pablo Araya-Araya, Laerte Sodré, Michael A. Strauss
Figure caption: Recovery fraction as function of redshift when applying the preselection criteria where a given galaxy should be the most massive galaxy in a given cylindrical volume of height Δz (Equation (1)) and transverse radius equal 1, 1.5, or 2 Mpc. The four panels depict the results for BCGs, protoBCGs, cluster members, and the field, respectively. The blue, salmon, and green curves (shaded regions) represent the median (in between 16th and 84th percentiles) for the ten lightcones results when using a radius of 1, 1.5, and 2 Mpc, to delimit the cylindrical volume, respectively. The larger error bars at low redshift are due to cosmic variance, while those for BCGs reflect their relative rarity compared to other populations.
Paper: Selecting Clusters and Protoclusters via Stellar Mass Density. I. Method and Tests on Mock HSC-SSP Catalogs
Authors: Marcelo C. Vicentin, Pablo Araya-Araya, Laerte Sodré, Michael A. Strauss
Figure caption: Each panel in this figure represents a redshift interval, as indicated above each plot. The blue histogram depicts the distribution of density contrast for all preselected dominant galaxy candidates, while the red histogram represents the distribution only for galaxies classified as BCG or protoBCG, i.e., true dominant galaxies according to our criteria. The histograms have been normalized to unit integral. Black circles with error bars denote the probabilities (y-axis on the right) as a function of density contrast calculated according to Equation (10). The circles represent medians, and the error bars are calculated as the 16 and 84th percentiles from the measurements of the ten mocks. The lime curve represents a fit of a sigmoid function with four free parameters (Equation (11)) using median values, while the shaded area delineates fits based on the 16 and 84th percentiles.
Paper: Selecting Clusters and Protoclusters via Stellar Mass Density. I. Method and Tests on Mock HSC-SSP Catalogs
Authors: Marcelo C. Vicentin, Pablo Araya-Araya, Laerte Sodré, Michael A. Strauss
Figure caption: Fraction of candidate BCGs selected for each true galaxy type when using the expected number of BCGs in each redshift interval with the highest probabilities as a function of redshift. The red stars, orange triangles, blue circles, and green inverted triangles refer to BCGs, protoBCGs, Cluster Members, and Field galaxies, respectively. The false positive rate is the sum of the blue and green curves.
Paper: Selecting Clusters and Protoclusters via Stellar Mass Density. I. Method and Tests on Mock HSC-SSP Catalogs
Authors: Marcelo C. Vicentin, Pablo Araya-Araya, Laerte Sodré, Michael A. Strauss
Figure caption: Completeness and purity of (proto)cluster detection as a function of various quantities. Top-left panel: Completeness as a function of halo mass for two selection thresholds of dominant galaxy probability, Pdominant ≥ 0.5 (solid red) and Pdominant ≥ 0.8 (dashed blue). Top-right panel: Completeness as a function of photometric redshift, considering three different minimum halo mass thresholds: Mhalo ≥ 1014.0M⊙ (solid red), Mhalo ≥ 1014.15M⊙ (dashed green), and Mhalo ≥ 1014.3M⊙ (dashed–dotted blue). Bottom-left panel: Purity as a function of the probability threshold for dominant galaxy selection. Bottom-right panel: Purity as a function of photometric redshift for two probability thresholds, Pdominant ≥ 0.5 (solid red) and Pdominant ≥ 0.8 (dashed blue).