adsabs/AstroCLIMB huggingface dataset:
Paper: Beyond Ultra-diffuse Galaxies. II. Environmental Quenching of Mass–Size Outliers among the Satellites of Milky Way Analogs
Authors: Jiaxuan Li, 嘉轩 李, Jenny E. Greene, Johnny Greco, Rachael Beaton, Shany Danieli, Andy Goulding, Song Huang, 崧 黄, Erin Kado-Fong
Figure caption: Radial distributions of UDGs (left) and UPGs (right). We show the radial distributions after subtracting the foreground and background contamination (shown in teal) and correcting for completeness in each radial distance bin (shown in red). After excluding R < 0.2R vir (shown in lighter colors), we fit projected NFW and Einasto profiles to the radial distributions and find good fits for both profiles. The radial distributions of UDGs and UPGs are similar in shape. The best-fit NFW concentration is consistent with an MW-mass halo, whereas the best-fit Einasto profiles have a smaller concentration than MW-mass halos.
Paper: Beyond Ultra-diffuse Galaxies. II. Environmental Quenching of Mass–Size Outliers among the Satellites of Milky Way Analogs
Authors: Jiaxuan Li, 嘉轩 李, Jenny E. Greene, Johnny Greco, Rachael Beaton, Shany Danieli, Andy Goulding, Song Huang, 崧 黄, Erin Kado-Fong
Figure caption: Distribution of UDGs (left) and UPGs (right) on the mass–size plane. We classify galaxies into quiescent and star-forming based on a mass-dependent color cut. The average mass–size relation and 1.5σ above it are shown in green. The solid lines are constant surface brightness cuts at ﹩{\overline{\mu }}_{\mathrm{eff}}(g)=25\ \mathrm{mag}\,{\mathrm{arcsec}}^{-2}﹩ for two different colors, g − i = 0.4 (blue) and 0.8 (red). The UDG sample includes a significant number of galaxies that are not mass–size outliers (falling below the 1.5σ line) that are red in color because the surface brightness cuts are different on the mass–size plane for blue and red galaxies.
Paper: Beyond Ultra-diffuse Galaxies. II. Environmental Quenching of Mass–Size Outliers among the Satellites of Milky Way Analogs
Authors: Jiaxuan Li, 嘉轩 李, Jenny E. Greene, Johnny Greco, Rachael Beaton, Shany Danieli, Andy Goulding, Song Huang, 崧 黄, Erin Kado-Fong
Figure caption: Same as Figure 4, but the samples are divided into subsets based on the projected distance to the host R/R vir (top panels) and host g − i color (bottom panels), shown as dashed red and blue lines. The quenched fraction is larger for those associated with redder hosts and those that are closer to the host.
Paper: Prospects for a Precise Equation of State Measurement from Advanced LIGO and Cosmic Explorer
Authors: Daniel Finstad, Laurel V. White, Duncan A. Brown
Figure caption: Cumulative combined R 1.4 measurements for our simulated population in the LIGO–Virgo network. Results are shown for the soft (blue), medium (orange), and stiff (green) equations of state that we consider. Shaded regions represent the 90% credible interval for each measurement, and the true value of R 1.4 for each equation of state is plotted as a horizontal dashed line in the appropriate color. Dotted lines show the fractional uncertainty in the measurement, calculated as the ratio of the credible interval width to the true value of R 1.4 for a given equation of state. Left: combined measurement when recovering signals with a Gaussian mass prior that matches the population distribution. Right: same as the left panel, except all signals are recovered with a uniform mass prior in the interval [1, 2] M ⊙. The ordering of signals is the same in both panels.
Paper: Prospects for a Precise Equation of State Measurement from Advanced LIGO and Cosmic Explorer
Authors: Daniel Finstad, Laurel V. White, Duncan A. Brown
Figure caption: Cumulative combined R 1.4 measurements for our Cosmic Explorer population. Results are shown for the soft (blue) and medium (orange) equations of state that we consider. Shaded regions represent the 90% credible interval for each measurement, and the true value of R 1.4 for each equation of state is plotted as a horizontal dashed line in the appropriate color. Dotted lines show the fractional uncertainty in the measurement, calculated as the ratio of the credible interval width to the true value of R 1.4 for a given equation of state. Left: combined measurement when recovering signals with a Gaussian mass prior that matches the population distribution. Right: same as the left panel, except all signals are recovered with a uniform mass prior in the interval [1, 2] M ⊙. The ordering of signals is the same in both panels.
Paper: Prospects for a Precise Equation of State Measurement from Advanced LIGO and Cosmic Explorer
Authors: Daniel Finstad, Laurel V. White, Duncan A. Brown
Figure caption: Distribution of number of events required to reach 2% precision for the soft (blue), medium (orange), and stiff (green) equations of state in our LIGO–Virgo analysis after 500 permutations of the combination order. Numbers of events are converted to years of observation at O4 sensitivity using the median estimate and upper/lower confidence limits of the binary neutron star merger rate from Abbott et al. (2021), shown in the top axes with labels ﹩{{ \mathcal R }}^{\mathrm{pess}}﹩ (lower limit), ﹩{{ \mathcal R }}^{\mathrm{med}}﹩ (median), and ﹩{{ \mathcal R }}^{\mathrm{opt}}﹩ (upper limit). Vertical dashed lines enclose the 90% credible interval for each equation of state.
Paper: Prospects for a Precise Equation of State Measurement from Advanced LIGO and Cosmic Explorer
Authors: Daniel Finstad, Laurel V. White, Duncan A. Brown
Figure caption: Match between gravitational waveforms for equal-mass binaries with and without tidal deformability included. The match is calculated as the noise-weighted overlap between the two waveforms in the frequency range 20–2048  Hz using the Advanced LIGO design sensitivity noise curve. Waveforms are generated using masses ranging from 1 to 2  M ⊙, and for the waveform including tidal deformability. The range of ﹩\tilde{{\rm{\Lambda }}}={{\rm{\Lambda }}}_{1}={{\rm{\Lambda }}}_{2}﹩ used in our analysis is bounded above by the stiffest equation of state in our analysis (green, upper curve) and bounded below by the softest equation of state (blue, lower curve).
Paper: Prospects for a Precise Equation of State Measurement from Advanced LIGO and Cosmic Explorer
Authors: Daniel Finstad, Laurel V. White, Duncan A. Brown
Figure caption: Mass–radius curves for the soft (blue), medium (orange), and stiff (green) equations of state we consider in our analysis. These equations of state were chosen to approximately span the range of currently allowed stiffness based on observational constraints. Also shown in gray is the full set of 2000 equations of state that we use as a prior distribution in the parameter estimation analysis of our simulated signals.
Paper: Prospects for a Precise Equation of State Measurement from Advanced LIGO and Cosmic Explorer
Authors: Daniel Finstad, Laurel V. White, Duncan A. Brown
Figure caption: Probability of seeing 10, 25, and 50 events with signal-to-noise ρ > 10 over time, assuming Advanced LIGO’s projected sensitivity for O4 and the median binary neutron star merger rate estimate from Abbott et al. (2021). The probabilities for 10, 25, and 50 events are shown as solid, dashed, and dotted lines, respectively.
Paper: High-resolution Chemical Abundances of the Nyx Stream
Authors: Shuyu Wang, 书玉 汪, Lina Necib, Alexander P. Ji, Xiaowei Ou, Mariangela Lisanti, Mithi A. C. de los Reyes, Allison L. Strom, Mimi Truong
Figure caption: Differential chemical abundances ([X/Fe] vs. [Fe/H]. The y-axis is [X/Fe], except when another ratio is indicated) of metal-rich Nyx dwarfs (dots) relative to HIP88622 (cyan dot), giants (stars, labeled “Nyx”) relative to Arcturus (cyan star), and metal-poor stars (squares) relative to HIP7162 (gold square), color-coded by effective temperature. For Na, Mg, and Ni, 18 Nyx stars selected by Zucker et al. (2021) from GALAH DR3 are plotted as blue crosses. The abundances of thick-disk stars (light gray dots) are from Bensby et al. (2014), except for the La abundances, which are from Battistini & Bensby (2016). The abundances of three Sgr dwarf galaxy stars from McWilliam et al. (2013) are indicated by the green triangles, while those of 12 Sgr stars from Sbordone et al. (2007) are indicated by the red plusses. A dashed line at [X/Fe]  =  0.0 is shown as a reference. The black error bar in the Ni, Zn, and La abundance panel indicates the zeropoint uncertainty. In general, the chemical abundances of the metal-rich Nyx component are consistent with the thick disk and distinct from the Sgr dwarf galaxy.
Paper: High-resolution Chemical Abundances of the Nyx Stream
Authors: Shuyu Wang, 书玉 汪, Lina Necib, Alexander P. Ji, Xiaowei Ou, Mariangela Lisanti, Mithi A. C. de los Reyes, Allison L. Strom, Mimi Truong
Figure caption: Orbital parameters including eccentricities e, maximum vertical distances from the Galactic plane z max, apocenters, and v  ϕ  vs. metallicities [Fe/H] of the Nyx stars, as well as a kinematics plot v  r  − v  ϕ  in galactocentric spherical coordinates, and a Toomre plot of the Nyx stars. The Bensby thick-disk stars are denoted by the light gray circles in the background. The rest of the unobserved sample of Nyx stars is shown in cyan (see Figure 4 for details of the selection of the Nyx stars). These stars are not shown in the orbital parameter panels because we do not have matching metallicity measurements.
Paper: High-resolution Chemical Abundances of the Nyx Stream
Authors: Shuyu Wang, 书玉 汪, Lina Necib, Alexander P. Ji, Xiaowei Ou, Mariangela Lisanti, Mithi A. C. de los Reyes, Allison L. Strom, Mimi Truong
Figure caption: Spatial distributions of Nyx stars observed with high-resolution spectroscopy in this paper. The velocities are shown as arrows, where the length of the arrow is proportional to the speed of the stars in that projection (e.g., in the first panel, the length of the arrow is proportional to ﹩\sqrt{{v}_{x}^{2}+{v}_{y}^{2}}﹩). The observed stars in this paper are shown in peach, and the metal-poor stars are plotted in purple. Overlaid in light turquoise are the rest of the Nyx stars, selected as having probabilities >0.75 of belonging to the Nyx velocity Gaussian distribution (Necib et al. 2020b; see Section 2 for more details of the selection of the stars). These stars have been subsampled by a factor of five for clarity of the figure. The metal-poor stars (purple) are coherent with the rest of the sample.
Paper: High-resolution Chemical Abundances of the Nyx Stream
Authors: Shuyu Wang, 书玉 汪, Lina Necib, Alexander P. Ji, Xiaowei Ou, Mariangela Lisanti, Mithi A. C. de los Reyes, Allison L. Strom, Mimi Truong
Figure caption: Kiel diagram (left) and color-magnitude diagram (right) of the observed Nyx stars. Nyx stars are color-coded by model metallicity. MIST isochrones with age 10 Gyr and [M/H]  ∈  [ −2.0, −0.5] (Choi et al. 2016) are plotted for comparison. The reference stars HIP7162, HIP88622, and Arcturus used in Section 3.2 are indicated by the gold square, the cyan dot, and the star, respectively. The plot demonstrates that the Nyx sample is composed of slightly metal-poor dwarf and giant stars, with five Nyx stars having distinctly lower model metallicity.
Paper: Decomposing the Spectrum of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Shogo B. Kobayashi, Hirofumi Noda, Teruaki Enoto, Tomohisa Kawashima, Akihiro Inoue, Ken Ohsuga
Figure caption: Schematic pictures of the possible accretion geometry (top) and spectral variability (bottom) of NGC 300 ULX-1.
Paper: Decomposing the Spectrum of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Shogo B. Kobayashi, Hirofumi Noda, Teruaki Enoto, Tomohisa Kawashima, Akihiro Inoue, Ken Ohsuga
Figure caption: Same as Figure 6, but the data points indicate the count rate of NuSTAR FPM-B.
Paper: High-resolution Chemical Abundances of the Nyx Stream
Authors: Shuyu Wang, 书玉 汪, Lina Necib, Alexander P. Ji, Xiaowei Ou, Mariangela Lisanti, Mithi A. C. de los Reyes, Allison L. Strom, Mimi Truong
Figure caption: Spectra of the selected Nyx stars observed with HIRES (blue) or MIKE (orange) around the Mg I line at 5711 Å (dashed vertical lines). The stars are selected and sorted based on star type and metallicity. From top to bottom, the star in each subplot is a metal-rich dwarf, a metal-rich giant, or a metal-poor star.
Paper: Decomposing the Spectrum of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Shogo B. Kobayashi, Hirofumi Noda, Teruaki Enoto, Tomohisa Kawashima, Akihiro Inoue, Ken Ohsuga
Figure caption: Estimated mass accretion rate and the magnetic field of ULX-1. Dashed lines are the best estimates, which are derived from Equations (10) and (5) and the best-fit values of the spectral analysis. Solid lines indicate the width of 90% confidence level. The best estimate region is highlighted as the red-hatched region.
Paper: Probing the Conditions for the H I-to-H2 Transition in the Interstellar Medium
Authors: Gyueun Park, Min-Young Lee, Shmuel Bialy, Blakesley Burkhart, J. R. Dawson, Carl Heiles, Di Li, Claire Murray, Hiep Nguyen, Anita Hafner, Daniel R. Rybarczyk, Snežana Stanimirović
Figure caption: Fraction of each gas phase with respect to the total hydrogen. (Top) Optically thick and thin H I in solid blue and dashed tan. (Bottom) CO-dark and CO-bright H2 in solid blue and dashed tan. The leftward arrow indicates that the derived fractions for CO-bright H2 are upper limits.
Paper: Probing the Conditions for the H I-to-H2 Transition in the Interstellar Medium
Authors: Gyueun Park, Min-Young Lee, Shmuel Bialy, Blakesley Burkhart, J. R. Dawson, Carl Heiles, Di Li, Claire Murray, Hiep Nguyen, Anita Hafner, Daniel R. Rybarczyk, Snežana Stanimirović
Figure caption: GNOMES LOSs at b < − 5° overlaid on the Planck A  V  image (Section 4.1; 1, 3, and 5 mag are shown as white contours). Among the total 58 LOSs, the 19 LOSs where CO(1–0) emission is clearly detected are shown as tan crosses. The remaining 39 LOSs without CO detection are indicated as blue crosses. The green boxes represent the approximate extents of local molecular clouds (top to bottom: California, Taurus, and Perseus; Lee et al. 2018).
Paper: Probing the Conditions for the H I-to-H2 Transition in the Interstellar Medium
Authors: Gyueun Park, Min-Young Lee, Shmuel Bialy, Blakesley Burkhart, J. R. Dawson, Carl Heiles, Di Li, Claire Murray, Hiep Nguyen, Anita Hafner, Daniel R. Rybarczyk, Snežana Stanimirović
Figure caption: Illustration of LOSs with different gas phases. (Top) H I-only LOSs. (Middle) LOSs with H I and CO-dark H2 gas. (Bottom) LOSs with H I, CO-dark H2, and CO-bright H2 gas.
Paper: Rapidly Evolving Transients in Archival ZTF Public Alerts
Authors: Wenxiong Li, 文雄 李, Iair Arcavi, Ehud Nakar, Alexei V. Filippenko, Thomas G. Brink, WeiKang Zheng, Yi Yang, 轶 杨, Marco C. Lam, Ido Keinan, Seán J. Brennan, Noi Shitrit
Figure caption: PSF subtraction of the source at the position of AT 2019lbw in g (upper panels) and r (lower panels) imaging, produced with AUTOPHOT. The main panels show a cutout of the target position before (left) and after (right) PSF subtraction, while projections along the x- and y-axes are also shown for each panel. The pixel scale is 0.″136 pixel−1.
Paper: Probing the Conditions for the H I-to-H2 Transition in the Interstellar Medium
Authors: Gyueun Park, Min-Young Lee, Shmuel Bialy, Blakesley Burkhart, J. R. Dawson, Carl Heiles, Di Li, Claire Murray, Hiep Nguyen, Anita Hafner, Daniel R. Rybarczyk, Snežana Stanimirović
Figure caption: Histogram of the CO-dark H2 column density for the 39 CO non-detected LOSs.
Paper: Rapidly Evolving Transients in Archival ZTF Public Alerts
Authors: Wenxiong Li, 文雄 李, Iair Arcavi, Ehud Nakar, Alexei V. Filippenko, Thomas G. Brink, WeiKang Zheng, Yi Yang, 轶 杨, Marco C. Lam, Ido Keinan, Seán J. Brennan, Noi Shitrit
Figure caption: The distribution of ∣b gal∣ for undetermined events (blue), Galactic objects (red), RETs (green), and an extragalactic nova (yellow). Significant Galactic contamination extends out to ∣b gal∣ = 40°.
Paper: Rapidly Evolving Transients in Archival ZTF Public Alerts
Authors: Wenxiong Li, 文雄 李, Iair Arcavi, Ehud Nakar, Alexei V. Filippenko, Thomas G. Brink, WeiKang Zheng, Yi Yang, 轶 杨, Marco C. Lam, Ido Keinan, Seán J. Brennan, Noi Shitrit
Figure caption: Same as Figure A1 but for AT 2020oor.
Paper: Rapidly Evolving Transients in Archival ZTF Public Alerts
Authors: Wenxiong Li, 文雄 李, Iair Arcavi, Ehud Nakar, Alexei V. Filippenko, Thomas G. Brink, WeiKang Zheng, Yi Yang, 轶 杨, Marco C. Lam, Ido Keinan, Seán J. Brennan, Noi Shitrit
Figure caption: Same as Figure A1 but for AT 2020ddu.
Paper: Investigating Cosmological Models and the Hubble Tension Using Localized Fast Radio Bursts
Authors: Jun-Jie Wei, Fulvio Melia
Figure caption: DM–redshift correlation for FRBs. Data points are estimations of the IGM portion DMIGM vs. redshift for 24 localized FRBs. The DMIGM values are derived from the observed DMobs after removing the contributions from our Galaxy and the host galaxy. The ﹩{\mathrm{DM}}_{\mathrm{ISM}}^{\mathrm{MW}}﹩ term is estimated from the Galactic ISM model, and ﹩{\mathrm{DM}}_{\mathrm{halo}}^{\mathrm{MW}}﹩ and DMhost are assumed to be 50 pc cm−3 and 50(1 + z)−1 pc cm−3, respectively. The dotted–dashed line represents the DMIGM result deduced from the IllustrisTNG simulation, and the gray shaded region encloses the 95% confidence region (Zhang et al. 2021). The other two lines correspond to the predictions of different cosmological models: (solid) flat ΛCDM, with H 0 = 95.8 km s−1 Mpc−1 and Ωm = 0.66; (dashed) the R h = ct cosmology, with H 0 = 94.2 km s−1 Mpc−1.
Paper: Investigating Cosmological Models and the Hubble Tension Using Localized Fast Radio Bursts
Authors: Jun-Jie Wei, Fulvio Melia
Figure caption: 1D marginalized posterior distributions and 2D 1–2σ contour regions representing the cosmological parameters H 0 and/or Ωm, constrained by 24 localized FRBs. The colors represent: flat ΛCDM (red contours) and R h = ct (blue line).
Paper: Polarization Signature of Companion-fed Supernovae Arising from BH–NS/BH Progenitor Systems
Authors: Xudong Wen, He Gao, Shunke Ai, Liang-Duan Liu, Jin-Ping Zhu, Wei-Hua Lei
Figure caption: The continuum polarization degree observed at 39 days after the SN explosion in oblate elliptic geometry at different θ los. The blue and yellow lines indicate the polarization degree in the case A and case B cases, respectively. The red line is the polarization degree produced by the nonspherical ejecta geometry powered by the decay of radioactive elements only. The green line is the polarization degree from the BP mechanism only.
Paper: Polarization Signature of Companion-fed Supernovae Arising from BH–NS/BH Progenitor Systems
Authors: Xudong Wen, He Gao, Shunke Ai, Liang-Duan Liu, Jin-Ping Zhu, Wei-Hua Lei
Figure caption: The continuum polarization degree observed on day 39 after the SN explosion in case B at different viewing angles θ los, where the color of the curve represents the continuum polarization degree for different θ BP of region I. The Stokes vector U is 0 owing to symmetry.
Paper: Polarization Signature of Companion-fed Supernovae Arising from BH–NS/BH Progenitor Systems
Authors: Xudong Wen, He Gao, Shunke Ai, Liang-Duan Liu, Jin-Ping Zhu, Wei-Hua Lei
Figure caption: Same as Figure 10, but for prolate elliptic geometry.
Paper: Polarization Signature of Companion-fed Supernovae Arising from BH–NS/BH Progenitor Systems
Authors: Xudong Wen, He Gao, Shunke Ai, Liang-Duan Liu, Jin-Ping Zhu, Wei-Hua Lei
Figure caption: The evolution of polarization degree with time after the SN explosion in case A, where the color of the curve represents the continuum polarization degree for the different θ BP at θ los = 90°.
Paper: Polarization Signature of Companion-fed Supernovae Arising from BH–NS/BH Progenitor Systems
Authors: Xudong Wen, He Gao, Shunke Ai, Liang-Duan Liu, Jin-Ping Zhu, Wei-Hua Lei
Figure caption: The polarization spectrum with a torus clump distributed in the equatorial direction outside the photosphere. The LOS is chosen to be 60° from the pole. The dashed blue line is the result predicted by Tanaka et al. (2017), and the red circles are the results from our MCPSC.
Paper: Polarization Signature of Companion-fed Supernovae Arising from BH–NS/BH Progenitor Systems
Authors: Xudong Wen, He Gao, Shunke Ai, Liang-Duan Liu, Jin-Ping Zhu, Wei-Hua Lei
Figure caption: The distribution of P along the equatorial direction obtained from 500 simulations. The yellow and green dashed lines represent the 1σ and 2σ  uncertainty ranges, respectively.
Paper: Constraining Cosmological Parameters Using the Cluster Mass–Richness Relation
Authors: Mohamed H. Abdullah, Gillian Wilson, Anatoly Klypin, Tomoaki Ishiyama
Figure caption: Left: distribution of clusters from the GalWCat19 catalog in the mass–richness plane. Gray points show all 1800 clusters (with a mass of ﹩\mathrm{log}{M}_{200}\,\geqslant 13.5﹩                      h −1 M ⊙ and at a redshift z ≤ 0.2 (see Section 2.3). Black points show the complete fiducial subsample (﹩{{ \mathcal S }}_{\mathrm{fid}}﹩) of 756 clusters to which the redshift selection function has been applied (﹩\mathrm{log}{M}_{200}\geqslant 13.9﹩                      h −1 M ⊙ and 0.045 ≤ z ≤ 0.125; see Section 2.2). The mean cluster mass as a function of richness in ﹩{{ \mathcal S }}_{\mathrm{fid}}﹩ is shown by the solid red circles, with the error bars indicating 1σ Poisson uncertainties. The blue solid line shows the Hinge function for ﹩{{ \mathcal S }}_{\mathrm{fid}}﹩ (see Section 2.5), with the dotted blue lines indicating 1σ uncertainties. The vertical blue dashed line shows the richness threshold at which the slope of the distribution changes (see Section 2.4 and Equation (4)). Right: red circles and uncertainties are as on the left. Also shown are the mean masses of clusters from two simulations (see 2.4). Black points show clusters from mini-Uchuu with a subhalo peak velocity threshold of v peak = 130 km s−1 and blue points show clusters from TNG with a galaxy stellar mass threshold of M  s  ≥ 5 × 109 h −1 M ⊙. As can be seen clearly from both panels, a flattening (tail) of the MRR occurs at low richness (﹩\mathrm{log}N\lesssim 1.23﹩). The short tail in the simulations is not intrinsic. It is partially due to the threshold of simulations as well as Poisson scattering (see Appendix B).
Paper: Constraining Cosmological Parameters Using the Cluster Mass–Richness Relation
Authors: Mohamed H. Abdullah, Gillian Wilson, Anatoly Klypin, Tomoaki Ishiyama
Figure caption: Comparison of constraints obtained on Ωm and σ 8 in this work with those obtained from previous MRR analyses using different cluster catalogs and richness thresholds. Left: 68% CLs derived within R 200 for all members with N th = 17 (yellow, ﹩{ \mathcal S }{\mathrm{all}}_{17}﹩) and red members with N th = 13 (gray, ﹩{ \mathcal S }{\mathrm{all}}_{13}﹩). Right: uncertainties on Ωm and σ 8 estimated from the previous studies of Rozo et al. (2010), Costanzi et al. (2019), Kirby et al. (2019), and Lesci et al. (2022; purple, brown, cyan, respectively), which use the cluster abundance technique and cluster mass estimates from the mass–richness relation (CMFMRR). Also shown is the study by Abdullah et al. (2020b; pink), which uses the cluster abundance technique and cluster mass estimates from the dynamics of member galaxies (CMFdyn), and the study by Aghanim et al. (2020; blue), which uses the CMB technique (see Table 1 for the abbreviation).