adsabs/AstroCLIMB huggingface dataset:
Paper: Identification of Inertial Modes in the Solar Convection Zone
Authors: Santiago A. Triana, Gustavo Guerrero, Ankit Barik, Jérémy Rekier
Figure caption: Eigenfrequencies of equatorially antisymmetric vorticity modes as a function of the radial width δ of the convective zone for different azimuthal wavenumbers m. Color and symbol size indicates the eigenmodes’ damping decay factor σ with larger deep-red points representing lightly damped modes (more likely to be excited), and smaller green-turquoise points representing heavily damped modes (less likely to be excited). The vertical black dashed line marks the Sun’s actual convective zone width at δ = 0.29 R ⊙. Black circles mark the modes we identify as the observed HFR waves. The horizontal orange dashed lines in the m = 4 panel are the frequencies of the (l = 5, m = 4) and the (l = 7, m = 4) tesseral Rossby modes according to Equation (B3).
Paper: Identification of Inertial Modes in the Solar Convection Zone
Authors: Santiago A. Triana, Gustavo Guerrero, Ankit Barik, Jérémy Rekier
Figure caption: Comparison of two m = 8 modes, one on the main branch with ω/Ω⊙ = −0.641 (left column) and one on the secondary branch with ω/Ω⊙ = −0.456 (right column). The top panels show the radial profile of the kinetic energy associated with the radial, consoidal, and toroidal components of the velocity (averaged over θ and ϕ, modes are normalized to have unit kinetic energy). The bottom panels show the fractional energy content of each spherical harmonic component at r = 0.99 R ⊙ (fractions of the total kinetic energy at that radius). The convective zone width is δ = 0.29 R ⊙ and the Ekman number is E = 2.1 × 10−4. Note that the (l, m) spherical harmonic component of the radial vorticity is proportional to l(l + 1)T  lm (r)/r.
Paper: Identification of Inertial Modes in the Solar Convection Zone
Authors: Santiago A. Triana, Gustavo Guerrero, Ankit Barik, Jérémy Rekier
Figure caption: Meridional cross sections of the m = 8, ω/Ω⊙ = −0.641 eigenmode on the main branch (top row), and the m = 8, ω/Ω⊙ = −0.118 of the tesseral-like Rossby-mode family (bottom row). This latter mode is essentially the same as the one reported by Bekki et al. (2022), see their Figure 11(d). Note the absence of radial nodes of ﹩{ \mathcal P }﹩ or ﹩| \hat{{\boldsymbol{r}}}\cdot {{\boldsymbol{u}}}_{0}| ﹩ in the equatorial plane for the main branch mode. The Ekman number here is E = 2.1 × 10−4, and the convective zone width is δ = 0.29 R ⊙.
Paper: Identification of Inertial Modes in the Solar Convection Zone
Authors: Santiago A. Triana, Gustavo Guerrero, Ankit Barik, Jérémy Rekier
Figure caption: Reducing the Ekman number by an order of magnitude has only a weak influence on the eigenfrequencies ω but a strong one on the damping rates σ. The plot on the left is computed for E = 1.98 × 10−4 and the one on the right for E = 1.98 × 10−5, both for δ = 0.29 R ⊙, modes from m = 4 to m = 15 are included. Even at a reduced Ekman number, the HFR modes (orange dots) remain as the least-damped ones, along with some tesseral-like Rossby modes (green dots). Blue dots represent the remaining inertial modes.
Paper: Identification of Inertial Modes in the Solar Convection Zone
Authors: Santiago A. Triana, Gustavo Guerrero, Ankit Barik, Jérémy Rekier
Figure caption: On the top-left panel, we show the effect of changing the truncation level N on the eigenvalue of the m = 8, ω/Ω⊙ = −0.641 eigenmode depicted in Figure 4 as a representative example. The reference eigenvalue σ 0 − i ω 0 corresponds to the solution with N = 160. The angular truncation l max is linked to N so that ﹩{l}_{\max }\sim N﹩. The bottom-left panel shows the residual (defined in the text). The panels on the right show the maximum magnitude of the Chebyshev coefficients for a given l (top), and for a given k (bottom), associated with a particular solution with N = 128, l max = 135.
Paper: On the Probability of the Extremely Lensed z = 6.2 Earendel Source Being a Population III Star
Authors: Anna T. P. Schauer, Volker Bromm, Niv Drory, Michael Boylan-Kolchin
Figure caption: Probability of Earendel being a Pop II star (dashed lines) or a Pop III star (solid lines) as a function of stellar mass. The two Pop III cases are a Larson-type IMF with a characteristic mass of m char = 0.35 M ⊙ (blue) and a log-normal IMF (light blue). While the Larson-IMF model stays nearly constant at a Pop III probability of 1%–2%, the log-normal IMF case rises to 15%. If we include an exponential cutoff at the high-mass end of the Pop II IMF, the probability for a Pop III star exceeds the Pop II probability at 280 M ⊙ (log-normal IMF, green) or 330 M ⊙ (Larson IMF, dark green), respectively.
Paper: On the Probability of the Extremely Lensed z = 6.2 Earendel Source Being a Population III Star
Authors: Anna T. P. Schauer, Volker Bromm, Niv Drory, Michael Boylan-Kolchin
Figure caption: Weighted number density of stars in the Earendel host galaxy versus stellar mass. Blue and light blue lines: Pop III case for the Larson and log-normal IMF. Dotted and dashed pink lines: Pop II case with and without the empirical high-mass cutoff beyond 150 M ⊙. The white region indicates the allowed mass range for Earendel between 50 and 500 M ⊙.
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications for Oxygen-18 Isotope Anomalies in ﹩{{\rm{H}}}_{2}^{18}{\rm{O}}﹩ Infrared Emission and Meteorites
Authors: Jenny K. Calahan, Edwin A. Bergin, Arthur D. Bosman
Figure caption: The evolution of 18O in equilibrium chemistry in the ﹩{{\rm{H}}}_{2}^{18}{\rm{O}}﹩-enhanced region. Most of the oxygen comes from the dark cloud material originating from molecules like H2O, CO2, organics, and silicates. In this region photodissociation of C18O provides an elevated abundance of 18O that reacts with H and H2 to quickly form 18OH and ﹩{{\rm{H}}}_{2}^{18}{\rm{O}}﹩. Because C16O is shielded, very little extra 16O is included in this oxygen cycle, thus the relative increase in ﹩{{\rm{H}}}_{2}^{18}{\rm{O}}﹩ production.
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications for Oxygen-18 Isotope Anomalies in ﹩{{\rm{H}}}_{2}^{18}{\rm{O}}﹩ Infrared Emission and Meteorites
Authors: Jenny K. Calahan, Edwin A. Bergin, Arthur D. Bosman
Figure caption: The H2O, ﹩{{\rm{H}}}_{2}^{18}{\rm{O}}﹩, CO, and C18O abundance in units of (mol/cm−3)/n  gas  throughout the inner disk (left and center plots), and the ratio between H2O and ﹩{{\rm{H}}}_{2}^{18}{\rm{O}}﹩ (top right) and CO and C18O (bottom right). At z/r ≈ 0.2 a unique region exits where ﹩{{\rm{H}}}_{2}^{18}{\rm{O}}﹩ is enhanced and C18O is greatly depleted.
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications for Oxygen-18 Isotope Anomalies in ﹩{{\rm{H}}}_{2}^{18}{\rm{O}}﹩ Infrared Emission and Meteorites
Authors: Jenny K. Calahan, Edwin A. Bergin, Arthur D. Bosman
Figure caption: Top: the overlapping spectra from H2O and ﹩{{\rm{H}}}_{2}^{18}{\rm{O}}﹩ focusing on a narrow wavelength regions within the MIRI instrument on JWST, focused on the ﹩{{\rm{H}}}_{2}^{18}{\rm{O}}﹩ 27 μm line (left) and 22.77 μm (right) lines. Bottom: the 50% (yellow contour) and 90% (white contour) contribution regions for each line plotted over the H2O-to-﹩{{\rm{H}}}_{2}^{18}{\rm{O}}﹩ ratio.
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications for Oxygen-18 Isotope Anomalies in ﹩{{\rm{H}}}_{2}^{18}{\rm{O}}﹩ Infrared Emission and Meteorites
Authors: Jenny K. Calahan, Edwin A. Bergin, Arthur D. Bosman
Figure caption: The H2O and ﹩{{\rm{H}}}_{2}^{18}{\rm{O}}﹩ spectra as predicted from an AS 209 model including water UV-shielding and Lyα contributions with 0.1 km s−1 velocity bins. Blue lines correspond to H2O and dark purple with ﹩{{\rm{H}}}_{2}^{18}{\rm{O}}﹩. ﹩{{\rm{H}}}_{2}^{18}{\rm{O}}﹩ lines that are relatively bright and isolated from H2O lines are highlighted.
Paper: Spectral Analysis of GRB 220426A: Another Case of a Thermally Dominated Burst
Authors: Li-Tao Deng, Da-Bin Lin, Li Zhou, Kai Wang, Xing Yang, Shu-Jin Hou, Jing Li, Xiang-Gao Wang, Rui-Jing Lu, En-Wei Liang
Figure caption: Left panel: modeling the radiation spectrum of photospheric emission with CPL-mBB (red dashed line), where the solid line is the numerical result (e.g., Deng & Zhang 2014). Right panel: fitting the radiation spectrum of GRB 090902B with CPL-mBB and the power-law spectral model.
Paper: Spectral Analysis of GRB 220426A: Another Case of a Thermally Dominated Burst
Authors: Li-Tao Deng, Da-Bin Lin, Li Zhou, Kai Wang, Xing Yang, Shu-Jin Hou, Jing Li, Xiang-Gao Wang, Rui-Jing Lu, En-Wei Liang
Figure caption: Light curves of GRB 220426A in different energy ranges.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: HST observations of Cepheids in 37 hosts of 42 “ideal” SNe Ia and NGC 4258, collected over 20 yr with four cameras and >1000 orbits of HST time. In most cases, 60 to 90 day campaigns in F555W and F814W or in F350LP were used to identify Cepheids from their light curves with occasional observations years later to identify longer-period Cepheids. NIR follow-up observations in F160W are used to reduce the effects of host-galaxy extinction, sensitivity to metallicity, and breaks in the P–L relation. Data sources: (1) HST Key Project, Freedman et al. (2001); (2) HST SN Ia Luminosity Calibration Program, Sandage et al. (2006); (3) Riess et al. (2005); (4) Macri et al. (2006); (5) Mager et al. (2013); (6) Yuan et al. (2022).
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Sources of data for the distance ladder. The red block shows data from this work.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Pseudocolor images of all Cepheid-bearing galaxies analyzed in this work. From top left, 37 hosts of 42 SNe Ia presented in the same order as Table 1. The last row includes our three anchors (NGC 4258, MW, and LMC) and two supporting galaxies (SMC and M31). Galaxies are presented at arbitrary plate scales, though in most cases the panels encompass the entire ACS or WFC3/UVIS field of view. Credits: SN hosts and NGC 4258—ESA Hubble site; MW, LMC, and SMC—ESA Gaia site; M31—STScI.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Images of 18 newly observed hosts of 23 SNe Ia and NGC 4258. Each image is of the Cepheid host indicated. The magenta outline shows the 2.′7 × 2.′7 field of the WFC3/NIR observations. Red dots indicate the positions of the Cepheids. Compass indicates north (long axis) and east (short axis). The NGC 4258 image shows Cepheids from Macri et al. (2006) in white and new ones from Yuan et al. (2022) in red.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Complete distance ladder. The simultaneous agreement of distance pairs: geometric and Cepheid-based (lower left), Cepheid- and SN-based (middle), and SN- and redshift-based (top right) provides the measurement of H 0. For each step, geometric or calibrated distances on the abscissa serve to calibrate a relative distance indicator on the ordinate through the determination of M  B  or H 0. Results shown are an approximation to the global fit as discussed in the text. Red SN points are at 0.0233 < z < 0.15, with the lower-redshift bound producing the appearance of asymmetric residuals when plotted against distance.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Distance-ladder covariance matrix. Graphical representation of the covariance matrix of measurements with values applicable to different sources indicated. The covariance matrix contains past sources of systematic error that propagate here as error in the fit. Among Cepheid hosts, square blocks along the diagonal indicate the background covariance within a host (Equation (8)) while the covariance pattern between hosts farther off the diagonals comes from the covariance of the metallicity scale (Equation (9)). The SN–SN covariance is characterized in the Pantheon+ analysis (Brout et al. 2021; Scolnic et al. 2021).
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Comparison of SN and Cepheid distance measures on the second rung of the distance ladder, and residuals (middle). Because the residual panel includes SN measures on both axes, residuals are convolved by the SN error arrow as indicated. An alternate plot with Cepheids on the abscissa is shown in Figure 12. SNe that share a common host are identified with various colors. We find no significant trend (<1.5σ) in this space. Results shown are an approximation to the global fit as discussed in the text. The lower panel replaces the NIR-based Cepheid magnitudes with the optical only from Fit 60.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Distributions of recovered artificial stars in each host. For each real Cepheid, 100 artificial stars of the expected Cepheid magnitude (based on its period and the P–L relation) are added to the host images within an annulus with an outer radius of 2.″4 and measured following the same procedures as for the Cepheids to produce a distribution in magnitudes (log flux). The distributions for each host are combined after subtracting their mean and dividing by their standard deviation. They compare well to a Gaussian with a difference in median and mean (dashed and dotted lines) of ∼0.03σ.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Independent determinations of the slope of the P–L relation in each host plotted in order of precision. Black (red) points are after (before) outlier rejection. We find that the slopes are consistent with a single value of −3.27 to −3.30 as indicated by the blue line. The most metal poor (SMC) and metal rich (MW) also have consistent slopes. Error bars are for the fit error only and do not include uneven period sampling or background covariance. The large change in slope for Mrk 1337 was due to the relatively small sample size and rejection of a few Cepheids far from its center.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Comparison of Cepheids measured in a dense (inner) field (in red) and sparse (outer) field (in blue) of NGC 4258. Because these Cepheids are at the same distance, the comparison shows the accuracy of the background estimates, which differ in the mean over the same sampled range, ﹩0.7\lt \mathrm{log}(P/\mathrm{day})\lt 1.2﹩, by 0.45 mag (relative to the Cepheids) yet yield a consistent intercept with σ ≈ 0.05 mag. The difference in metallicity between the samples, Δ[O/H] = 0.08 dex, corresponds to a difference of 0.02 mag, smaller than the precision of this comparison.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Composite visual (F555W) or white-light (F350LP) Cepheid light curves binned by period (upper) and compared with individual MW Cepheids near the middle period of the bin. The “Hertzsprung progression” (relation between light-curve shape and period) is apparent, including subtle features like the progression in phase of a resonance “bump” between the second overtone and fundamental pulsation for P < 20 days. The red line is a cubic spline constrained by the averages of bins in phase.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: HST NIR Wesenheit Cepheid P–L relations. The Cepheid magnitudes are shown for 37 SN Ia hosts, M31, and 2 of the 3 possible distance-scale anchors (LMC and NGC 4258). The uniformity of the photometry and metallicity reduces systematic errors along the distance ladder. A single slope is shown and used for the baseline, but we also allow for a break (two slopes) as well as limited period ranges in some analysis variants.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Composite visual (F555W) or white-light (F350LP) Cepheid light curves. Each HST Cepheid light curve with 10 < P < 80 days is plotted after subtracting the mean magnitude and determining the phase of the observation.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Reddening ratios and impact on H 0. The upper-left panel shows various reddening laws and their free parameter R  V  used to estimate the appropriate ratio R  H  for dereddening the Cepheids and the range over which this is applicable. The upper-right panel shows the empirical determination of R  H  using the MW Cepheids from R21 and individual estimates parameterized by host, type, mass, and SFR from SDSS galaxies in Hahn et al. (2022). The lower panel shows the color excess, E(V − I), for Cepheid samples. The net change to H 0 due to differential Cepheid reddening on the ladder is 0.08 R  H  (0.03) mag, with realistic differences in R  H  producing changes <0.01 mag or <0.5%.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: The metallicity term and consistency of the geometric anchors. The mean slope of four hosts with geometric distances is plotted against the intercept of the Wesenheit magnitude P–L relation. The DEB distance difference between the SMC and LMC from Graczyk et al. (2020) as discussed is independent of the calibration uncertainties of the DEB method, making this link, the dashed line, robust and independent of the other anchors (a linear fit to the four points is very good, though not unexpectedly so with P = 10% to be better). The gray constraint on the MW comes from the breadth of metallicities and individual Gaia EDR3 parallaxes. The metallicities of the Cepheids in SN hosts span the range of the anchors, making the value of H 0 insensitive to the value of the metallicity dependence, with a change in H 0 of 0.2 units for a change in Z  W  of 0.1 mag dex−1.