adsabs/AstroCLIMB huggingface dataset:
Paper: Characterizing the Umbral Magnetic Knots of δ-Sunspots
Authors: Aimee A. Norton, Peter J. Levens, Kalman J. Knizhnik, Mark G. Linton, Yang Liu
Figure caption: NOAA AR 11560 is a δ-spot shown at different times in SDO/HMI continuum intensity (left) and radial magnetic field, B  r  (right). The third panel from the top is the time of maximum umbral flux, ﹩{\phi }_{{\delta }_{\max }}﹩, while the fourth panel from the top is the time of maximum flux in the δ-umbrae only, Doδ of 56%. The umbral regions participating in the δ-configuration are identified by contours on the continuum intensity image, with yellow (red) contours identifying the negative (positive) umbra and yellow (red) crosses identifying the centroid location for the negative (positive) umbrae in the δ. This is a northern hemispheric AR in which the umbrae participating in the δ-configuration present an anti-Hale tilt but a tilt calculated using all umbrae in the AR presents an anti-Joy tilt, since most northern ARs in Solar Cycle 24 have a positive trailing polarity (white) closer to the pole and this one is closer to the equator. The δ-configuration stays compact, and the magnetic knot rotates 70° clockwise. The region has a δ-configuration for 29% of the time observed. It is an SEEQ, and its presentation is similar to either the inverted kink configuration, shown in Figure 1(b), or the multisegment buoyancy “quadrupole” configuration, shown in Figure 1(d).
Paper: Characterizing the Umbral Magnetic Knots of δ-Sunspots
Authors: Aimee A. Norton, Peter J. Levens, Kalman J. Knizhnik, Mark G. Linton, Yang Liu
Figure caption: AR flux emergence rates determined from observations (blue and green) and simulations (red) show the trend that regions containing more flux emerge faster. The average values of AR maximum signed flux and average flux emergence rates in this study are the δ-spots and β-spots shown as blue crosses and triangles, respectively, with the median absolute deviation shown as error bars. We overlay fits using a dashed (solid) line reported by Otsuji et al. (2011; Norton et al. 2017) of a power-law relationship from Hinode (HMI) observations where maximum (average) flux emergence rates were dependent on maximum flux. A value reported for the maximum flux emergence rate by Toriumi et al. (2014) is plotted as a green square, and an average flux emergence rate reported by Norton et al. (2017) is plotted as a green triangle. Two simulations of AR flux emergence from Rempel & Cheung (2014) and Chen et al. (2017) are also shown using red symbols; see Sections 4 and 5 for more details and discussion.
Paper: Characterizing the Umbral Magnetic Knots of δ-Sunspots
Authors: Aimee A. Norton, Peter J. Levens, Kalman J. Knizhnik, Mark G. Linton, Yang Liu
Figure caption: Top row: small sample. Bottom row: large sample. The AR tilts are binned by whether they are in the range of expected values (meaning that they obey Hale’s law and Joy’s law), or whether they have anti-Hale or anti-Joy tilt angles. The pie charts from left to right in the top row represent the tilts of the small sample of 19 δ-spots and 11 β-spots for only the umbrae involved in the δ-configuration at the time of maximum Doδ, then all umbrae in the δ AR at the time of maximum umbral flux, and all umbrae for the β-spots at the time of maximum umbral flux. The tilts from the large sample of 120 δ-spots are shown in the bottom row. Plotted left to right are tilts determined for umbrae involved in the δ-configuration at the time of maximum Doδ, then all umbrae in that region at the time of maximum umbral flux. One can see that the small and large samples are equivalent in that their pie charts differ only by a few percent for the δ-only analysis. Movies for all regions are found online.
Paper: Characterizing the Umbral Magnetic Knots of δ-Sunspots
Authors: Aimee A. Norton, Peter J. Levens, Kalman J. Knizhnik, Mark G. Linton, Yang Liu
Figure caption: The maximum Doδ umbral flux, ϕ Doδ  (black symbols), and the maximum total umbral flux, ﹩{\phi }_{{\delta }_{\max }}﹩ (red symbols), vs. the single, maximum flare energy produced by that region is plotted in the top panel for the large sample of δ-spots. The same quantities, ϕ Doδ  and ﹩{\phi }_{{\delta }_{\max }}﹩, are plotted vs. total observed flare energy over time in the bottom panel. The best fits are given in the legend and discussed in Section 4. All fits provide a positive correlation, but the correlation between maximum umbral flux, ﹩{\phi }_{{\delta }_{\max }}﹩, and total X-ray flux, E FlareTot, has the highest r-value of 0.52.
Paper: Characterizing the Umbral Magnetic Knots of δ-Sunspots
Authors: Aimee A. Norton, Peter J. Levens, Kalman J. Knizhnik, Mark G. Linton, Yang Liu
Figure caption: Snapshots of NOAA AR 11302 (HARP 892), NOAA AR 11429 (HARP 1449), NOAA AR 12158 (HARP 4536), and NOAA AR 12673 (HARP 7115) are shown from top to bottom in continuum intensity (left) and radial magnetic field, B  r  (right). The umbral regions participating in the δ-configuration are identified by yellow (red) contours on the continuum intensity image outlining the negative (positive) umbra. The corresponding Doδ at each time is written in the continuum intensity image.
Paper: Characterizing the Umbral Magnetic Knots of δ-Sunspots
Authors: Aimee A. Norton, Peter J. Levens, Kalman J. Knizhnik, Mark G. Linton, Yang Liu
Figure caption: The δ-regions listed in Tables 5–14 are shown on a butterfly diagram where ARs are plotted as a function of time and sine latitude. δ-regions are shown in yellow and are not colored for polarity or anti-Hale orientation. All non-δ regions observed during this cycle are also plotted, with the leading spot polarity shown in red (blue) and with total flux indicated by symbol marker size. Anti-Hale regions are obvious as the nondominant color in each hemisphere. The data used to generate this figure are the HMI SHARPS data summarized in the Solar Photospheric Ephemeral and Active Region (SPEAR) catalog (Norton 2021), which is an easy-to-read tabulated text file, SPEAR-CR.txt, available at http://Sun.stanford.edu/~norton/SPEAR/. The catalog currently contains information on nearly 4000 magnetic regions at their nearest central meridian crossing time for Carrington Rotations 2096–2239. For reference, the northern hemispheric sunspot number peaked in late 2011 and the southern hemispheric sunspot number peaked in early 2014, information available from multiple sources and found at http://users.telenet.be/j.janssens/SC24web.
Paper: Characterizing the Umbral Magnetic Knots of δ-Sunspots
Authors: Aimee A. Norton, Peter J. Levens, Kalman J. Knizhnik, Mark G. Linton, Yang Liu
Figure caption: NOAA AR 12715 snapshots are shown because its configuration and behavior are somewhat anomalous for a δ-spot. The region is not AH or AJ. It is an SEEB with very little rotation whose opposite polarities emerge with some separation but remain close, converging somewhat over time. We speculate that this could be the signature of flux emerging as an Ω-loop initially, but the legs of the region have reconnected beneath in an O-ring and hence the polarities converge, or the region is confined by strong subsurface flows. Neither mechanism is considered to be a formation mechanism for δ-spots. NOAA AR 11465 is another AR consistent with an O-ring.
Paper: Characterizing the Umbral Magnetic Knots of δ-Sunspots
Authors: Aimee A. Norton, Peter J. Levens, Kalman J. Knizhnik, Mark G. Linton, Yang Liu
Figure caption: The sign of current helicity for the δ-regions is shown as a function of time and latitude. A total of 64% of all the δ-regions follow the HR in which the northern (southern) hemispheric ARs have a preference for − (+) current helicity. The northern hemisphere has 71% obeying the HR, whereas the southern hemisphere has 57%. We found that 74% of anti-Hale δ-regions exhibit the preference (83% in N and 63% in S), as do 60% of the anti-Joy regions (65% in N and 55% in S).
Paper: Cross-scale Correlations in Imbalanced Solar Wind Turbulence: Parker Solar Probe Observations
Authors: G. Q. Zhao, R. Meyrand, H. Q. Feng, D. J. Wu, J. C. Kasper
Figure caption: Panels (a)–(c): distributions of cross helicity (σ  c ), proton temperature (T  p ), and speed (V  p ), where dotted lines in panels (b) and (c) correspond to all data while solid lines correspond to part data with σ  c  > 0 as shown in panel (a). Panels (d)–(f): plots of scale-dependent magnetic energy density (P  k ) during 2018 November 1–4, average values of local spectral index (〈α  k 〉), and average values of local magnetic helicity (〈σ  k 〉), where the bars indicate standard deviations.
Paper: Cross-scale Correlations in Imbalanced Solar Wind Turbulence: Parker Solar Probe Observations
Authors: G. Q. Zhao, R. Meyrand, H. Q. Feng, D. J. Wu, J. C. Kasper
Figure caption: Scatter plots of (PI , σ  c ; a, d), (PI , T  p ; b), (σ  c , T  p ; c), (PI , V  p ; e), (σ  c , V  p ; f). The color in panels (a) and (d) marks T  p  and V  p , respectively. The blue dashed lines indicate linear fitting of the data (in logarithmic space accordingly). CC is the correlation coefficient of the data in each panel.
Paper: Cross-scale Correlations in Imbalanced Solar Wind Turbulence: Parker Solar Probe Observations
Authors: G. Q. Zhao, R. Meyrand, H. Q. Feng, D. J. Wu, J. C. Kasper
Figure caption: Top panels: scatter plots of σ  c  with PI  and V  p . Middle and bottom panels: scatter plots of σ  m  with σ  c , PI , T  p , and V  p . All data in this figure are bound by the plasma beta β  p  < 0.6. The blue dashed lines are linear fitting of the data (in logarithmic space accordingly). CC is the correlation coefficient of the data in each panel.
Paper: Cross-scale Correlations in Imbalanced Solar Wind Turbulence: Parker Solar Probe Observations
Authors: G. Q. Zhao, R. Meyrand, H. Q. Feng, D. J. Wu, J. C. Kasper
Figure caption: Panels (a)–(f): case plot of the three components of the velocity and magnetic field in the RTN coordinate system. Panel (g): case plot of the normalized cross helicity (σ  c ), where 〈σ  c 〉 is the average over the time segment.
Paper: Cross-scale Correlations in Imbalanced Solar Wind Turbulence: Parker Solar Probe Observations
Authors: G. Q. Zhao, R. Meyrand, H. Q. Feng, D. J. Wu, J. C. Kasper
Figure caption: The format is the same as in Figure 3 but for the parameters ∣α∣ and σ  m .
Paper: Binding Energies of Interstellar Relevant S-bearing Species on Water Ice Mantles: A Quantum Mechanical Investigation
Authors: Jessica Perrero, Joan Enrique-Romero, Stefano Ferrero, Cecilia Ceccarelli, Linda Podio, Claudio Codella, Albert Rimola, Piero Ugliengo
Figure caption: Top panel: side view of the crystalline (010) water P-ice slab model (along the b lattice vector). Bottom panel: side view of the amorphous water ice slab model (along the b lattice vector). Numbers identify the different adsorption sites: those in blue represent dangling hydrogen atoms (dH), while those in red represent dangling oxygen atoms (dO).
Paper: Binding Energies of Interstellar Relevant S-bearing Species on Water Ice Mantles: A Quantum Mechanical Investigation
Authors: Jessica Perrero, Joan Enrique-Romero, Stefano Ferrero, Cecilia Ceccarelli, Linda Podio, Claudio Codella, Albert Rimola, Piero Ugliengo
Figure caption: (a) Best linear fit between the DFT//DFT and the ONIOM2-corrected BEs for the crystalline ice systems. (b) Best linear fit between the DFT//DFT BEs and the HF-3c//HF-3c (in blue) and the DFT//HF-3c (in orange) schemes, for the crystalline ice systems. BEs are in kelvin.
Paper: Binding Energies of Interstellar Relevant S-bearing Species on Water Ice Mantles: A Quantum Mechanical Investigation
Authors: Jessica Perrero, Joan Enrique-Romero, Stefano Ferrero, Cecilia Ceccarelli, Linda Podio, Claudio Codella, Albert Rimola, Piero Ugliengo
Figure caption: Set of 17 S-bearing species considered in this work. Dots represent unpaired electrons.
Paper: The Pantheon+ Analysis: The Full Data Set and Light-curve Release
Authors: Dan Scolnic, Dillon Brout, Anthony Carr, Adam G. Riess, Tamara M. Davis, Arianna Dwomoh, David O. Jones, Noor Ali, Pranav Charvu, Rebecca Chen, Erik R. Peterson, Brodie Popovic, Benjamin M. Rose, Charlotte M. Wood, Peter J. Brown, Ken Chambers, David A. Coulter, Kyle G. Dettman, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Charles D. Kilpatrick, Robert P. Kirshner, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Matthew R. Siebert, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Light curves of all SNe Ia used for the SN Ia–Cepheid calibration (second rung of the distance ladder). When an SN has been observed by multiple surveys, multiple light curves are shown for each filter. The SALT2 fit from each light curve is overplotted. Certain filters (e.g., I and sometimes R) are not included in the fit when the observed-frame filter is outside the used SALT2 wavelength range of 300–700 nm.
Paper: The Pantheon+ Analysis: The Full Data Set and Light-curve Release
Authors: Dan Scolnic, Dillon Brout, Anthony Carr, Adam G. Riess, Tamara M. Davis, Arianna Dwomoh, David O. Jones, Noor Ali, Pranav Charvu, Rebecca Chen, Erik R. Peterson, Brodie Popovic, Benjamin M. Rose, Charlotte M. Wood, Peter J. Brown, Ken Chambers, David A. Coulter, Kyle G. Dettman, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Charles D. Kilpatrick, Robert P. Kirshner, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Matthew R. Siebert, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Top: the redshift distribution of the Pantheon+ sample that passes all of the light-curve requirements, as well as the same for the JLA and Pantheon samples. The largest increase in the number of SNe for the Pantheon+ sample is at low redshift owing to the addition of the Foundation, LOSS1, LOSS2, SOUSA, and CNIa0.2 samples. The largest increase at higher redshift is due to the inclusion of the DES 3 yr sample. We do not use SNe from SNLS at z > 0.8 due to sensitivity to the U band in model training, so the Pantheon+ statistics between 0.8 < z < 1.0 are lower than that of Pantheon and JLA. Bottom: the Pantheon+ redshift diagram shown cumulatively by survey.
Paper: The Pantheon+ Analysis: The Full Data Set and Light-curve Release
Authors: Dan Scolnic, Dillon Brout, Anthony Carr, Adam G. Riess, Tamara M. Davis, Arianna Dwomoh, David O. Jones, Noor Ali, Pranav Charvu, Rebecca Chen, Erik R. Peterson, Brodie Popovic, Benjamin M. Rose, Charlotte M. Wood, Peter J. Brown, Ken Chambers, David A. Coulter, Kyle G. Dettman, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Charles D. Kilpatrick, Robert P. Kirshner, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Matthew R. Siebert, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Top: the median host-galaxy mass per redshift bin for the seven samples with the highest statistics. Bottom: same as above, but showing the distributions per subsample in histogram format.
Paper: The Pantheon+ Analysis: The Full Data Set and Light-curve Release
Authors: Dan Scolnic, Dillon Brout, Anthony Carr, Adam G. Riess, Tamara M. Davis, Arianna Dwomoh, David O. Jones, Noor Ali, Pranav Charvu, Rebecca Chen, Erik R. Peterson, Brodie Popovic, Benjamin M. Rose, Charlotte M. Wood, Peter J. Brown, Ken Chambers, David A. Coulter, Kyle G. Dettman, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Charles D. Kilpatrick, Robert P. Kirshner, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Matthew R. Siebert, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Display of what an .FITRES file looks like that has all of the information from the light-curve fit, as well as ancillary information. A value of −9 is given where information is unavailable. The full file will be included at pantheonplussh0es.github.io.
Paper: The Pantheon+ Analysis: The Full Data Set and Light-curve Release
Authors: Dan Scolnic, Dillon Brout, Anthony Carr, Adam G. Riess, Tamara M. Davis, Arianna Dwomoh, David O. Jones, Noor Ali, Pranav Charvu, Rebecca Chen, Erik R. Peterson, Brodie Popovic, Benjamin M. Rose, Charlotte M. Wood, Peter J. Brown, Ken Chambers, David A. Coulter, Kyle G. Dettman, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Charles D. Kilpatrick, Robert P. Kirshner, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Matthew R. Siebert, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Display of what an SNANA light-curve file looks like for SN 2021pit. The full file is included at https://pantheonplussh0es.github.io/.
Paper: The Pantheon+ Analysis: Cosmological Constraints
Authors: Dillon Brout, Dan Scolnic, Brodie Popovic, Adam G. Riess, Anthony Carr, Joe Zuntz, Rick Kessler, Tamara M. Davis, Samuel Hinton, David Jones, W. D'Arcy Kenworthy, Erik R. Peterson, Khaled Said, Georgie Taylor, Noor Ali, Patrick Armstrong, Pranav Charvu, Arianna Dwomoh, Cole Meldorf, Antonella Palmese, Helen Qu, Benjamin M. Rose, Bruno Sanchez, Christopher W. Stubbs, Maria Vincenzi, Charlotte M. Wood, Peter J. Brown, Rebecca Chen, Ken Chambers, David A. Coulter, Mi Dai, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Lisa Kelsey, Robert P. Kirshner, Anais Möller, Jessie Muir, Seshadri Nadathur, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Masao Sako, Matthew R. Siebert, Mat Smith, Benjamin E. Stahl, Phil Wiseman
Figure caption: Analysis roadmap of this work and supporting/complementary Pantheon+ and SH0ES papers. Components of the analysis here are shown in blue. The companion paper (Riess et al. 2022, hereafter R22), which provides a constraint on H 0, requires the Hubble diagram and covariance computed in this work. Likewise, measurements of H 0 in this work require the R22 Cepheid distance and covariance. Supporting papers are shown in gray boxes.
Paper: The Pantheon+ Analysis: Cosmological Constraints
Authors: Dillon Brout, Dan Scolnic, Brodie Popovic, Adam G. Riess, Anthony Carr, Joe Zuntz, Rick Kessler, Tamara M. Davis, Samuel Hinton, David Jones, W. D'Arcy Kenworthy, Erik R. Peterson, Khaled Said, Georgie Taylor, Noor Ali, Patrick Armstrong, Pranav Charvu, Arianna Dwomoh, Cole Meldorf, Antonella Palmese, Helen Qu, Benjamin M. Rose, Bruno Sanchez, Christopher W. Stubbs, Maria Vincenzi, Charlotte M. Wood, Peter J. Brown, Rebecca Chen, Ken Chambers, David A. Coulter, Mi Dai, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Lisa Kelsey, Robert P. Kirshner, Anais Möller, Jessie Muir, Seshadri Nadathur, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Masao Sako, Matthew R. Siebert, Mat Smith, Benjamin E. Stahl, Phil Wiseman
Figure caption: Pantheon+ distance-modulus uncertainties (shown as the dashed lines with mean σ  μ  and split on host mass) in comparison to the observed rms of the distance-modulus residuals (shown as solid lines as rms μ split on host mass), as a function of color. This shows that the distance errors are adequately modeled (Equation (4)) as a function of SN color and host stellar mass. In previous analyses, the uncertainties were roughly flat as a function of color.
Paper: The Pantheon+ Analysis: The Full Data Set and Light-curve Release
Authors: Dan Scolnic, Dillon Brout, Anthony Carr, Adam G. Riess, Tamara M. Davis, Arianna Dwomoh, David O. Jones, Noor Ali, Pranav Charvu, Rebecca Chen, Erik R. Peterson, Brodie Popovic, Benjamin M. Rose, Charlotte M. Wood, Peter J. Brown, Ken Chambers, David A. Coulter, Kyle G. Dettman, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Charles D. Kilpatrick, Robert P. Kirshner, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Matthew R. Siebert, Benjamin E. Stahl, WeiKang Zheng
Figure caption: A comparison of the fit parameters of duplicate SNe. Here we compare pairs for SALT2 parameters c, x 1, m  B , and μ. The strong level of agreement is given in the text, and any noticeable outliers are due to sparse light-curve quality.
Paper: The Pantheon+ Analysis: Cosmological Constraints
Authors: Dillon Brout, Dan Scolnic, Brodie Popovic, Adam G. Riess, Anthony Carr, Joe Zuntz, Rick Kessler, Tamara M. Davis, Samuel Hinton, David Jones, W. D'Arcy Kenworthy, Erik R. Peterson, Khaled Said, Georgie Taylor, Noor Ali, Patrick Armstrong, Pranav Charvu, Arianna Dwomoh, Cole Meldorf, Antonella Palmese, Helen Qu, Benjamin M. Rose, Bruno Sanchez, Christopher W. Stubbs, Maria Vincenzi, Charlotte M. Wood, Peter J. Brown, Rebecca Chen, Ken Chambers, David A. Coulter, Mi Dai, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Lisa Kelsey, Robert P. Kirshner, Anais Möller, Jessie Muir, Seshadri Nadathur, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Masao Sako, Matthew R. Siebert, Mat Smith, Benjamin E. Stahl, Phil Wiseman
Figure caption: Comparison between observed data (black points) and simulations (blue lines) for the largest subsamples in this analysis: DES, HST, SDSS, SNLS, PS1, LOW-z, and Foundation (FOUND). We compare three key distributions: the SALT2 light-curve-fit parameters x 1 and c are shown as well as the measured redshift.
Paper: The Pantheon+ Analysis: The Full Data Set and Light-curve Release
Authors: Dan Scolnic, Dillon Brout, Anthony Carr, Adam G. Riess, Tamara M. Davis, Arianna Dwomoh, David O. Jones, Noor Ali, Pranav Charvu, Rebecca Chen, Erik R. Peterson, Brodie Popovic, Benjamin M. Rose, Charlotte M. Wood, Peter J. Brown, Ken Chambers, David A. Coulter, Kyle G. Dettman, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Charles D. Kilpatrick, Robert P. Kirshner, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Matthew R. Siebert, Benjamin E. Stahl, WeiKang Zheng
Figure caption: The evolution of fitted SALT2 x 1 and c parameters, as well as the host-galaxy mass with redshift. SNe are shown here if they pass the light-curve selection requirements discussed in Section 2.2. The error bars in red are given as the rms of values in that redshift bin, and the smaller error bars in black show the uncertainty in the mean.
Paper: The Pantheon+ Analysis: Cosmological Constraints
Authors: Dillon Brout, Dan Scolnic, Brodie Popovic, Adam G. Riess, Anthony Carr, Joe Zuntz, Rick Kessler, Tamara M. Davis, Samuel Hinton, David Jones, W. D'Arcy Kenworthy, Erik R. Peterson, Khaled Said, Georgie Taylor, Noor Ali, Patrick Armstrong, Pranav Charvu, Arianna Dwomoh, Cole Meldorf, Antonella Palmese, Helen Qu, Benjamin M. Rose, Bruno Sanchez, Christopher W. Stubbs, Maria Vincenzi, Charlotte M. Wood, Peter J. Brown, Rebecca Chen, Ken Chambers, David A. Coulter, Mi Dai, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Lisa Kelsey, Robert P. Kirshner, Anais Möller, Jessie Muir, Seshadri Nadathur, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Masao Sako, Matthew R. Siebert, Mat Smith, Benjamin E. Stahl, Phil Wiseman
Figure caption: Top panel: the Pantheon+ “Hubble diagram” showing the distance modulus μ vs. redshift z. The 18 different surveys are each given different colors. Bottom panel: the distance-modulus residuals relative to a best-fit cosmological model with binned data for reference (black points). Both the data errors and the binned data errors include only statistical uncertainties. At z < 0.01, the sensitivity of peculiar velocities is very large, and the uncertainties shown reflect this uncertainty. The dashed line is the predicted Hubble residual bias stemming from biased redshifts due to volumetric effects in the very nearby universe (assuming 250 km s−1 uncorrected velocity scatter).