adsabs/AstroCLIMB huggingface dataset:
Paper: Comparing Apples with Apples: Robust Detection Limits for Exoplanet High-contrast Imaging in the Presence of Non-Gaussian Noise
Authors: Markus J. Bonse, Emily O. Garvin, Timothy D. Gebhard, Felix A. Dannert, Faustine Cantalloube, Gabriele Cugno, Olivier Absil, Jean Hayoz, Julien Milli, Markus Kasper, Sascha P. Quanz
Figure caption: Violations of the independence assumption in the presence of speckle noise. The top two images illustrate the two cases described in the text. Pixels A and B are separated by 1 FWHM. We use the unsaturated PSF of the NACO data set to display the speckle. The plots below give 1D profiles of the two cases, cut along the white dashed lines. The shaded areas highlight the information contributing to the aperture averages ﹩A^{\prime} ﹩ and ﹩B^{\prime} ﹩.
Paper: Comparing Apples with Apples: Robust Detection Limits for Exoplanet High-contrast Imaging in the Presence of Non-Gaussian Noise
Authors: Markus J. Bonse, Emily O. Garvin, Timothy D. Gebhard, Felix A. Dannert, Faustine Cantalloube, Gabriele Cugno, Olivier Absil, Jean Hayoz, Julien Milli, Markus Kasper, Sascha P. Quanz
Figure caption: Relationship between the value of the test statistic T obs and the detection uncertainty specified as ﹩5{\sigma }_{{ \mathcal N }}=2.87\times {10}^{-7}\quad \mathrm{FPF}﹩ and ﹩3{\sigma }_{{ \mathcal N }}=1.35\times {10}^{-3}\quad \mathrm{FPF}﹩. The t-distribution shown in blue converges toward a Gaussian for large separations (black dashed line) while the Laplacian parametric bootstrap remains heavier-tailed.
Paper: Comparing Apples with Apples: Robust Detection Limits for Exoplanet High-contrast Imaging in the Presence of Non-Gaussian Noise
Authors: Markus J. Bonse, Emily O. Garvin, Timothy D. Gebhard, Felix A. Dannert, Faustine Cantalloube, Gabriele Cugno, Olivier Absil, Jean Hayoz, Julien Milli, Markus Kasper, Sascha P. Quanz
Figure caption: The top two panels show example residuals for the β Pictoris data set with and without fake planets. The bottom left image gives their difference. The bottom right image shows the result of the same experiment but for a fake planet closer to the star and with 50 PCA components. For 20 PCA components the presence of the planet only affects the values of the residual image in the direct neighborhood of the signal. For 50 PCA components the whole image changes. This is potentially problematic as discussed in the text.
Paper: Comparing Apples with Apples: Robust Detection Limits for Exoplanet High-contrast Imaging in the Presence of Non-Gaussian Noise
Authors: Markus J. Bonse, Emily O. Garvin, Timothy D. Gebhard, Felix A. Dannert, Faustine Cantalloube, Gabriele Cugno, Olivier Absil, Jean Hayoz, Julien Milli, Markus Kasper, Sascha P. Quanz
Figure caption: Comparison of the analytical contrast curve (based on the approximation that the throughput is only a function of separation) with the complete contrast grid presented in the main paper (Section 6.2). The orange line gives the contrast grid thresholded at ﹩5{\sigma }_{{ \mathcal N }}﹩. The results are based on the assumption of Gaussian noise.
Paper: Comparing Apples with Apples: Robust Detection Limits for Exoplanet High-contrast Imaging in the Presence of Non-Gaussian Noise
Authors: Markus J. Bonse, Emily O. Garvin, Timothy D. Gebhard, Felix A. Dannert, Faustine Cantalloube, Gabriele Cugno, Olivier Absil, Jean Hayoz, Julien Milli, Markus Kasper, Sascha P. Quanz
Figure caption: Detection limits for the β Pictoris data set under the assumption of Gaussian noise. The results under the assumption of Laplacian noise are presented later. The contrast grid (top panel) gives the detection uncertainty (FPF) as a function of separation and contrast. Each value in the grid is based on six fake planet residuals. Below three example residuals are shown, which were used to compute the contrast grid at the positions marked in orange and yellow. The FPFmedian given for each residual is the median FPF over different noise sample positions (see the details in Section 6.1). The mean of all six FPFmedian values gives the final FPF value of the contrast grid. An interactive version of the plot is available on the documentation page of applefy: https://applefy.readthedocs.io/.
Paper: Comparing Apples with Apples: Robust Detection Limits for Exoplanet High-contrast Imaging in the Presence of Non-Gaussian Noise
Authors: Markus J. Bonse, Emily O. Garvin, Timothy D. Gebhard, Felix A. Dannert, Faustine Cantalloube, Gabriele Cugno, Olivier Absil, Jean Hayoz, Julien Milli, Markus Kasper, Sascha P. Quanz
Figure caption: Throughput of the β Pictoris data set for 30 PCA components. Every value in the plot is the average of six experiments with artificial planets inserted at six different azimuthal positions.
Paper: Comparing Apples with Apples: Robust Detection Limits for Exoplanet High-contrast Imaging in the Presence of Non-Gaussian Noise
Authors: Markus J. Bonse, Emily O. Garvin, Timothy D. Gebhard, Felix A. Dannert, Faustine Cantalloube, Gabriele Cugno, Olivier Absil, Jean Hayoz, Julien Milli, Markus Kasper, Sascha P. Quanz
Figure caption: The effect of the aperture placement on the detection uncertainty. The top two images show the residuals with the inserted fake planets at 2 and 3 FWHM. The white circles indicate the initial positions of the apertures used to extract the noise. Below we show the computed test statistic T obs (orange) and detection uncertainty (FPF; blue) for different rotations of the initial noise positions. The difference between the values of T obs and the FPF are due to the number of apertures changing by ±1 during the rotation.
Paper: Comparing Apples with Apples: Robust Detection Limits for Exoplanet High-contrast Imaging in the Presence of Non-Gaussian Noise
Authors: Markus J. Bonse, Emily O. Garvin, Timothy D. Gebhard, Felix A. Dannert, Faustine Cantalloube, Gabriele Cugno, Olivier Absil, Jean Hayoz, Julien Milli, Markus Kasper, Sascha P. Quanz
Figure caption: Sensitivity and false-positive rate (FPR) of the Shapiro–Wilk test as a function of separation from the star. For each separation, 105 samples are drawn, each containing as many values as independent resolution elements are available. We sample from a Gaussian distribution to measure the FPR (blue) and from a Laplacian distribution to measure the sensitivity (orange). The left and right plots show the results for two different thresholds of p < 0.01 and p < 0.2, respectively.
Paper: Comparing Apples with Apples: Robust Detection Limits for Exoplanet High-contrast Imaging in the Presence of Non-Gaussian Noise
Authors: Markus J. Bonse, Emily O. Garvin, Timothy D. Gebhard, Felix A. Dannert, Faustine Cantalloube, Gabriele Cugno, Olivier Absil, Jean Hayoz, Julien Milli, Markus Kasper, Sascha P. Quanz
Figure caption: Comparison of the detection limits for the β Pictoris data sets, once under the assumption of Gaussian (blue line) and once for Laplacian (orange line) residual noise. The solid line is the median contrast over 360 different placements of the noise values in the residuals. The shaded area gives the mean absolute deviation from the median. We used 30 PCA components for all separations.
Paper: Comparing Apples with Apples: Robust Detection Limits for Exoplanet High-contrast Imaging in the Presence of Non-Gaussian Noise
Authors: Markus J. Bonse, Emily O. Garvin, Timothy D. Gebhard, Felix A. Dannert, Faustine Cantalloube, Gabriele Cugno, Olivier Absil, Jean Hayoz, Julien Milli, Markus Kasper, Sascha P. Quanz
Figure caption: Effect of different noise distributions on the detection uncertainty. The plots give the relationship between the selected detection threshold and the actually observed FPF for the t-test and the parametric bootstrap tests presented in this paper. Any deviation from the diagonal corresponds to an over- or underestimation of the FPF. The results are based on a Monte Carlo simulation described in the text.
Paper: KMT-2022-BLG-2397: Brown Dwarf at the Upper Shore of the Einstein Desert
Authors: Andrew Gould, Yoon-Hyun Ryu, Jennifer C. Yee, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge
Figure caption: Relative sensitivity to FSPL events of the Roman and KMT surveys as a function of Einstein radius θ E. The asymptotic ratio of 11 at the right reflects the fact that 11 times more events take place in the KMT purview, while essentially all FSPL events with θ E ∼ 100 μas are detected in either survey. For smaller θ E, Roman continues to detect almost all events down to almost θ E ∼ 0.1 μas, whereas KMT sensitivity continuously declines over this range, dropping to zero near θ E ∼ 1 μas. This points to 0.1 ≲ θ E/μas ≲ 1 as a key “discovery space” for Roman, a region that could contain a vast population of FFPs.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. II. The First Catalog from a New Narrowband Survey for Emission-line Objects
Authors: Jennifer Sieben, David J. Carr, John J. Salzer, Alec S. Hirschauer
Figure caption: An example diagnostic plot for the SFF01 field. On the left, we plot Δm against the continuum magnitude. On the right, we plot the Δm against the ratio. The horizontal line represents our Δm cutoff of −0.4; the vertical line represents our ratio cutoff of 5.0. Inside the blue box in the left panel are the stars used to refine the Δm offsets. All objects within the lower-right section of the right plot are considered possible candidates, subject to further analysis. These objects are shown in red in both plots.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. II. The First Catalog from a New Narrowband Survey for Emission-line Objects
Authors: Jennifer Sieben, David J. Carr, John J. Salzer, Alec S. Hirschauer
Figure caption: Three Hα-detected SFACT objects. Each row shows three 50″ × 50″ image cutouts of the continuum image (left), the NB image (middle), and the difference image (right). The Hα redshift windows detect objects in the range 0.0 < z < 0.15 and include all of our extended galaxies. Top: SFF01-NB2-B19198 was detected in the NB2 filter and is a low-luminosity dwarf galaxy with z = 0.0034. Middle: SFF15-NB1-A2606 was detected in the NB1 filter via its many H II regions (z = 0.0643). Bottom: SFF01-NB3-D2175 was detected in the NB3 filter and has z = 0.1374.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. II. The First Catalog from a New Narrowband Survey for Emission-line Objects
Authors: Jennifer Sieben, David J. Carr, John J. Salzer, Alec S. Hirschauer
Figure caption: SFF10-NB2-C21205. Shown are three 50″ × 50″ image cutouts of the continuum image (left), the NB image (middle), and the difference image (right). This object was detected due its strong C III] line at 1908 Å falling in the NB2 filter. Follow-up spectra reveal it to be a quasar at z = 2.464.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. II. The First Catalog from a New Narrowband Survey for Emission-line Objects
Authors: Jennifer Sieben, David J. Carr, John J. Salzer, Alec S. Hirschauer
Figure caption: Three [O II]-detected objects. Each row shows three 50″ × 50″ image cutouts of the continuum image (left), the NB image (middle), and the difference image (right). The [O II] redshift windows detect objects in the range 0.78 < z < 1.0 and are typically small dots like these. Top: SFF10-NB2-A8098 was detected in the NB2 filter (z = 0.7670). Middle: SFF10-NB1-C19716 was detected in the NB1 filter and has z = 0.8694. Bottom: SFF01-NB3-B5847 was found in the NB3 filter (z = 1.0023).
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. II. The First Catalog from a New Narrowband Survey for Emission-line Objects
Authors: Jennifer Sieben, David J. Carr, John J. Salzer, Alec S. Hirschauer
Figure caption: Distributions of r-band magnitude and NB flux broken down by field. The left-hand plots show the r-band magnitude distributions for each of the pilot-study fields, while the right shows the NB flux distributions. From top to bottom is SFF01, SFF10, then SFF15. The vertical dashed lines mark the median of each distribution. The distributions are seen to be very similar from field to field.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. II. The First Catalog from a New Narrowband Survey for Emission-line Objects
Authors: Jennifer Sieben, David J. Carr, John J. Salzer, Alec S. Hirschauer
Figure caption: Three [O III]-detected objects. Each row shows three 50″ × 50″ image cutouts of the continuum image (left), the NB image (middle), and the difference image (right). The [O III] redshift windows detect objects in the range 0.31 < z < 0.50, and the [O III]-detected objects are typically compact sources like these. Top: SFF15-NB2-C20849 was detected in the NB2 filter; it is a Seyfert 2 galaxy at z = 0.3228. Middle: SFF01-NB1-D4500 was detected in the NB1 filter and is a star-forming galaxy at z = 0.3906. Bottom: SFF10-NB3-D13569 was detected in the NB3 filter at z = 0.4829.
Paper: A Unified Treatment of Kepler Occurrence to Trace Planet Evolution. I. Methodology
Authors: Anne Dattilo, Natalie M. Batalha, Steve Bryson
Figure caption: FGK occurrence rate estimates. The number of planets per 100 stars (shown) is comparable to a percentage. Gray cells are either those with no planet detections or below the low occurrence boundary (see Section 3.1), with only the upper limit shown.
Paper: A Unified Treatment of Kepler Occurrence to Trace Planet Evolution. I. Methodology
Authors: Anne Dattilo, Natalie M. Batalha, Steve Bryson
Figure caption: Left: FGK completeness function. Completeness degrades quickly along orbital period. White contours mark the 10-, 1-, 1e-2-, and 1e-4% completeness levels. Right: the completeness contour for specific radii. There is a discontinuity in occurrence at 400 days caused by discontinuities in the detection efficiency model.
Paper: A Unified Treatment of Kepler Occurrence to Trace Planet Evolution. I. Methodology
Authors: Anne Dattilo, Natalie M. Batalha, Steve Bryson
Figure caption: KDE maps of the observed FGK planet population (left) and the completeness-corrected intrinsic occurrence (right).
Paper: A Unified Treatment of Kepler Occurrence to Trace Planet Evolution. I. Methodology
Authors: Anne Dattilo, Natalie M. Batalha, Steve Bryson
Figure caption: Same as Figure 7, calculated only for F-type stars.
Paper: The Radial Distribution and Excitation of H2 around Young Stars in the HST-ULLYSES Survey
Authors: Kevin France, Nicole Arulanantham, Erin Maloney, P. Wilson Cauley, P. Ábrahám, Juan M. Alcalá, Justyn Campbell-White, Eleonora Fiorellino, Gregory J. Herczeg, Brunella Nisini, Miguel Vioque
Figure caption: A comparison of the C IV luminosity with the average H2 emitting radius for four of the progressions studied in this work (color coded as indicated in the legend). As has been shown in previous work, the majority of H2 emission in CTTS systems arises between 0.1 and 3 au. The best-fit power-law relationship between L (C IV) and 〈R H2〉 for the [1, 4] progression is shown overplotted in purple and the Spearman rank coefficient (ρ) and probability coefficient for null correlation (n) are shown at the upper right. Assuming that C IV serves as a proxy for the accretion luminosity, the H2 radial distribution demonstrates a weak dependence on the strength of the high-energy emission, possibly suggesting increased molecular dissociation in the innermost region of rapidly accreting systems.
Paper: The Radial Distribution and Excitation of H2 around Young Stars in the HST-ULLYSES Survey
Authors: Kevin France, Nicole Arulanantham, Erin Maloney, P. Wilson Cauley, P. Ábrahám, Juan M. Alcalá, Justyn Campbell-White, Eleonora Fiorellino, Gregory J. Herczeg, Brunella Nisini, Miguel Vioque
Figure caption: The FUV continuum luminosity increases with pre-main-sequence stellar mass. The stars in the ULLYSES sample with good measurements of the average H2 emitting radius are shown with a black “x”, and those with literature A  V  < 1 are overlaid with pink circles (see Sections 3.3 and 4.1). A fit to the A  V  < 1 points is overplotted in purple. The Spearman rank coefficient (ρ) and probability coefficient for null correlation (n) of the A  V  < 1 points are shown at the upper left.
Paper: The Radial Distribution and Excitation of H2 around Young Stars in the HST-ULLYSES Survey
Authors: Kevin France, Nicole Arulanantham, Erin Maloney, P. Wilson Cauley, P. Ábrahám, Juan M. Alcalá, Justyn Campbell-White, Eleonora Fiorellino, Gregory J. Herczeg, Brunella Nisini, Miguel Vioque
Figure caption: Comparison of the C IV and Lyα luminosities of the ULLYSES stars (black diamonds) and previous HST/COS survey of CTTSs (France et al. 2012; orange circles). The plot demonstrates the correlation between Lyα (as derived in Section 3.1) and accretion-dominated emission from C IV. This is consistent with the broad, bright Lyα profiles of CTTSs (Schindhelm et al. 2012; Arulanantham et al. 2023) being powered by mass accretion (e.g., France et al. 2014b).
Paper: The Radial Distribution and Excitation of H2 around Young Stars in the HST-ULLYSES Survey
Authors: Kevin France, Nicole Arulanantham, Erin Maloney, P. Wilson Cauley, P. Ábrahám, Juan M. Alcalá, Justyn Campbell-White, Eleonora Fiorellino, Gregory J. Herczeg, Brunella Nisini, Miguel Vioque
Figure caption: A comparison between the WISE 12 and 22 μm color and the 1600 Å Bump luminosity. Targets are labeled for reference and the Spearman rank coefficient (ρ) and probability coefficient for null correlation (n) are shown at the upper left. The positive correlation indicates that as the inner disk opacity decreases, stellar+accretion-generated Lyα photons can penetrate farther into the disk where they dissociate H2O, creating the nonthermal H2 population that gives rise to the 1600 Å molecular dissociation continuum.
Paper: The Radial Distribution and Excitation of H2 around Young Stars in the HST-ULLYSES Survey
Authors: Kevin France, Nicole Arulanantham, Erin Maloney, P. Wilson Cauley, P. Ábrahám, Juan M. Alcalá, Justyn Campbell-White, Eleonora Fiorellino, Gregory J. Herczeg, Brunella Nisini, Miguel Vioque
Figure caption: A comparison of the WISE 12 – 22 μm color with the average H2 emitting radius for four of the progressions studied in this work (color coded as indicated in the legend). The distribution of emitting radii are clustered between W3 and W4 ≈ 2.0 and 2.5, respectively, with a small number of transition disks (Sz 111, DM Tau, and CS Cha) extending to large mid-IR flux ratios. The Spearman rank coefficient (ρ) and probability coefficient for null correlation (n) are shown at the upper left.
Paper: The Radial Distribution and Excitation of H2 around Young Stars in the HST-ULLYSES Survey
Authors: Kevin France, Nicole Arulanantham, Erin Maloney, P. Wilson Cauley, P. Ábrahám, Juan M. Alcalá, Justyn Campbell-White, Eleonora Fiorellino, Gregory J. Herczeg, Brunella Nisini, Miguel Vioque
Figure caption: Projected Lyα luminosities for all ULLYSES DR5 stars (black diamonds) as a function of total fluorescent H2 luminosity. We created a power-law fit to the 14 stars with high-quality, multiprogression H2 emission line data and Lyα reconstructions from France et al. (2012), shown as orange circles on the plot. This fit was used to predict the Lyα luminosity of the ULLYSES stars based on their observed F(H2).
Paper: The Radial Distribution and Excitation of H2 around Young Stars in the HST-ULLYSES Survey
Authors: Kevin France, Nicole Arulanantham, Erin Maloney, P. Wilson Cauley, P. Ábrahám, Juan M. Alcalá, Justyn Campbell-White, Eleonora Fiorellino, Gregory J. Herczeg, Brunella Nisini, Miguel Vioque
Figure caption: A comparison of the dust masses derived from millimeter-wave observations (see Manara et al. 2022 for a review) with the average H2 emitting radius for the [1, 4] progression (29 sources had both dust masses, disk inclinations > 15°, and good H2 FWHM observations). The Spearman rank coefficient (ρ) and probability coefficient for null correlation (n) are shown at the upper left. The behavior is consistent with a picture where more massive stars hosting more massive dust disks also photodissociate their inner few 0.1 au, leading to a correlation between disk mass and H2 emitting radii.
Paper: The Radial Distribution and Excitation of H2 around Young Stars in the HST-ULLYSES Survey
Authors: Kevin France, Nicole Arulanantham, Erin Maloney, P. Wilson Cauley, P. Ábrahám, Juan M. Alcalá, Justyn Campbell-White, Eleonora Fiorellino, Gregory J. Herczeg, Brunella Nisini, Miguel Vioque
Figure caption: The 1600 Å Bump luminosity is strongly correlated with Lyα luminosity. This correlation supports the hypothesis that the Bump is powered by Lyα-driven H2O dissociation. The Spearman rank coefficient (ρ) and probability coefficient for null correlation (n) are shown at the upper left.
Paper: Lensing in the Blue. II. Estimating the Sensitivity of Stratospheric Balloons to Weak Gravitational Lensing
Authors: Jacqueline E. McCleary, Spencer W. Everett, Mohamed M. Shaaban, Ajay S. Gill, Georgios N. Vassilakis, Eric M. Huff, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Paul Clark, Bradley Holder, Aurelien A. Fraisse, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Jürgen Schmoll, Ellen Sirks, Sut Ieng Tam
Figure caption: Background galaxy number density as a function of total integration time on clusters at z = 0.059 (top), z = 0.3 (middle), and z = 0.45 (bottom). Plotted values are the mean of 30 simulated observations of clusters with M = 4.1 × 1014 and the indicated redshift; error bars are the standard errors of the mean. The source densities reflect the selection criteria for clusters’ respective “lensing” samples.
Paper: Lensing in the Blue. II. Estimating the Sensitivity of Stratospheric Balloons to Weak Gravitational Lensing
Authors: Jacqueline E. McCleary, Spencer W. Everett, Mohamed M. Shaaban, Ajay S. Gill, Georgios N. Vassilakis, Eric M. Huff, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Paul Clark, Bradley Holder, Aurelien A. Fraisse, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Jürgen Schmoll, Ellen Sirks, Sut Ieng Tam
Figure caption: Galaxy number density as a function of integration time (measured in five-minute increments) in four SUPERBIT bandpasses. Points are the mean values across 30 simulated galaxy clusters with M = 4.1 × 1014 M ⊙ h −1, z = 0.059; error bars are standard errors of the mean. Beyond a requirement that galaxy S/N >5, no selections on galaxy redshifts or fit parameters are made.
Paper: Lensing in the Blue. II. Estimating the Sensitivity of Stratospheric Balloons to Weak Gravitational Lensing
Authors: Jacqueline E. McCleary, Spencer W. Everett, Mohamed M. Shaaban, Ajay S. Gill, Georgios N. Vassilakis, Eric M. Huff, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Paul Clark, Bradley Holder, Aurelien A. Fraisse, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Jürgen Schmoll, Ellen Sirks, Sut Ieng Tam
Figure caption: Examples of tangential (top panels) and cross-shear profiles (bottom panels) for single galaxy cluster realizations in lum. Left: Realization of a cluster with M 200c  = 4.1 × 1014 M ⊙ h −1 and z = 0.45. Right: Realization of a cluster with M 200c  = 4.1 × 1014 M ⊙ h −1 and z = 0.059. The selections described in Section 4.3.1 were applied, yielding 31.3 and 31.6 galaxies arcmin−2 for the z = 0.059 and z = 0.3 clusters, respectively.