Final Results from the Hubble Space Telescope Key Project to Measure the Hubble Constant

B. F. Madore; B. K. Gibson; D. D. Kelson; G. D. Illingworth; H. C. Ford; J. A. Graham; J. P. Huchra; Jr.; J. R. Mould; L. Ferrarese

REVIEW

Final Results from the Hubble Space Telescope Key Project to Measure the Hubble Constant

W. L. Freedman, B. F. Madore, B. K. Gibson, L. Ferrarese, D. D. Kelson, S. Sakai, J. R. Mould, R. C. Kennicutt

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Jr., H. C. Ford, J. A. Graham, J. P. Huchra, S. M. G. Hughes, G. D. Illingworth, L. M. Macri, P. B. Stetson

Astrophysics · Submitted 18 Dec 2000 · 15 references

Pith's verdict: The canonical H0 = 72 ± 8 result, well supported and unusually candid about its systematics — but the Type Ia calibrator list in §6.1 contradicts Tables 1 and 2 and cannot be reproduced as written.

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arXiv IDastro-ph/0012376 (version 1)

Pith IDNL7DAN3N, Pith's permanent record of this paper and its review

CitationB. F. Madore, B. K. Gibson, D. D. Kelson, G. D. Illingworth, H. C. Ford, J. A. Graham, J. P. Huchra, Jr., J. R. Mould, L. Ferrarese, L. M. Macri, P. B. Stetson, R. C. Kennicutt, S. M. G. Hughes, S. Sakai, W. L. Freedman. "Final Results from the Hubble Space Telescope Key Project to Measure the Hubble Constant." arXiv:astro-ph/0012376 (2000). https://pith.science/paper/NL7DAN3N

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Editor's note

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This is the paper everyone cites for H0 = 72, and the number holds up. What is actually new is not the individual Cepheid distances but the re-fitting of all 31 galaxies onto a single zero point: OGLE PL slopes, the Stetson WFPC2 zero point, a −0.2 mag/dex metallicity term, and a short-period bias cut. The Udalski slope change is the interesting ingredient, because it is distance-dependent (their eq. 6) and therefore fixes two things at once. The Type Ia zero point moves into line with the other methods, and the Cepheid distance to NGC 4258 moves from 8.1 to 7.8 Mpc against a 7.2 Mpc maser distance. That comparison with an external geometric measurement is the strongest evidence in the paper, and it is the part I would point a student to first. Table 14 is a real systematic budget, seven terms combined in quadrature, and §8.1 quantifies the LMC sensitivity outright (18.3 mag would give H0 = 79). The classifier's note that no limitations are stated is simply wrong; §3.2 concedes the metallicity sign is uncertain and §8.5 concedes crowding is uncorrected. This is more candid than most papers of its generation. The soft spots, in order. First, §6.1 names IC 4182 among the Type Ia calibrators and omits NGC 4496A, while Table 1 footnote d and Table 2 footnote 2 say the opposite: SN 1937C excluded, SN 1960F included. Swapping a 4.5 Mpc host for a 14.5 Mpc host is not obviously small against the quoted ±2 random error. It does not threaten 72 ± 8, since four of the five methods cluster at 70–72, but the 71 ± 2 ± 6 entry in Table 12 cannot be reproduced from the paper alone. That deserves a query to the authors. Second, the five methods share one Cepheid zero point, so their agreement is not independent confirmation of it. §7 says so; I would have said it louder, because the abstract's 'good agreement' reads as though it were. Third, the fundamental plane value of 82 rests on three clusters, and the paper downweights it correctly. The in-press citations (Newman, Macri, Freedman, Sebo) and the unpublished Mould erratum support cross-checks rather than the headline. Read it if you need a defensible H0 with an error budget, or if you calibrate secondary indicators. It deserves referees.

Referee report

Significance

If the result holds, this paper closes a seventy-year dispute at the 10% level and establishes H0 = 72 +/- 8 as the reference local value against which CMB-derived and lensing-derived values are compared. The work is unusually transparent for its genre: Table 14 enumerates seven systematic sources with percentage contributions that combine in quadrature to the quoted 10%, §8.1 states the sensitivity of H0 to the adopted LMC modulus explicitly (18.3 mag would give 79 km/s/Mpc), and the NGC 4258 maser comparison in §8.1.1 provides an external, geometric check on the zero point that is independent of the Cepheid ladder. The public archival database described in §2.3 and the double-blind DoPHOT/ALLFRAME reduction described in §2.4 are durable community resources. The paper is also candid about what it cannot settle: §8.1.2 concedes that the LMC zero point is unlikely to be resolved without SIM or GAIA, and §8.5 concedes that blending remains an unquantified systematic with only a lower limit from artificial-star tests.

Major objections (4)

[§6.1 vs. Table 1 footnote d and Table 2 footnote 2] The Type Ia calibrator list in §6.1 is internally inconsistent with the paper's own tables. §6.1 states that the zero points come from 'NGC 4639, 4536, 3627, 3368, 5253, and IC 4182.' Table 1 footnote d instead lists the hosts of SN 1960F, 1972E, 1981B, 1989B, 1990N, and 1998bu, 'but excluding 1895B, 1937C, 1974G,' and Table 2 footnote 2 states explicitly that IC 4182 is 'not used in Gibson et al. (2000) nor this paper's SNIa calibration.' SN 1937C is in IC 4182 and SN 1960F is in NGC 4496A, so the two lists differ by exactly one member: §6.1 includes a 4.5 Mpc host and omits a 14.5 Mpc host. Because each calibrator sets the SN Ia absolute magnitude through m - mu, this substitution is not obviously small compared with the +/-2 random error quoted for this method in Table 12. The authors should state which six galaxies were actually used, reconcile §6.1 with Tables 1 and 2, and confirm that the 71 +/- 2r +/- 6s entry in Table 12 was computed with that set.
[§8.4 vs. Table 3, NGC 3627 row] §8.4 states that the period-cut bias corrections 'amount to only a few hundredths of a mag' and that 'in 2 cases (M81 and NGC 4414) they are as large as 0.08 and -0.08 mag (4% in distance), respectively.' Table 3 contradicts this: the NGC 3627 modulus moves from 29.71 (column 5) to 29.86 (column 7), a correction of +0.15 mag, or 7% in distance, and the number of Cepheids retained drops from 35 to 16. This is the largest correction in the table and it is not mentioned in the text. The point is load-bearing because NGC 3627 hosts SN 1989B and is one of the Type Ia calibrators listed in §6.1, so a 0.15 mag shift in its modulus propagates directly into the SN Ia zero point. The authors should correct the §8.4 statement, explain why NGC 3627 requires so much larger a cut than the rest of the sample, and verify that the SN Ia calibration in §6.1 uses the period-cut modulus rather than the uncorrected one.
[§7 and Table 12] The combination in §7 reports a frequentist median of H0 = 72 +/- 3 (random) and a Bayesian value of 72 +/- 2 (random), but no consistency statistic is given for the five input values, which span 70 to 82 km/s/Mpc with quoted random errors of 2 to 9. The combined random error of +/-3 is smaller than the random error of three of the five inputs, which is only legitimate if the inputs are consistent with a common value at the quoted errors. The authors should report a chi-square (or equivalent) for the five values against the combined mean, state the number of degrees of freedom, and indicate whether the quoted random error has been scaled by sqrt(chi2/nu). If the fundamental plane is excluded, the remaining four values are consistent, but that exclusion should be justified statistically rather than by the qualitative statement in §7 that the fundamental plane 'is an outlier.'
[§8.1, Table 13, Table 14] The dominant systematic in Table 14 is the +/-5% assigned to the LMC zero point, which is derived in §8.1 from the standard error of the mean of seven methods in Table 13 (rms dispersion 0.15 mag over seven techniques, giving +/-0.06 mag, inflated to the adopted +/-0.10 mag). The standard error of the mean is the right statistic only if the seven methods are independent and unbiased, and several are not obviously so: the Cepheid and TRGB entries both depend on the same HST photometric zero point, and the red clump and RR Lyrae entries both rest on similar Population II calibrations. The authors should either justify the independence assumption or state explicitly what range of H0 is implied by the full spread of Figure 5 (18.1 to 18.7 mag), so that the reader can see the difference between a 1-sigma error on the mean and a systematic bound. The sensitivity statement already in §8.1 (18.3 mag gives 79 km/s/Mpc) is helpful and should be paired with the corresponding statement for the upper end of the distribution.

Minor objections (9)

[Abstract vs. Table 12] The abstract quotes the Tully-Fisher result as 71 +/- 2 +/- 7, whereas Table 12 gives 71 +/- 3r +/- 7s. The two should agree.
[Figure 3 caption vs. §7] The Figure 3 caption gives the cumulative distribution midpoint as 'H0 = 72 (71) +/- 4 +/- 7,' while §7 gives the frequentist median as 72 +/- 3r. The random error and the parenthetical value should be made consistent between text and caption.
[§2.2 and §11] §2.2 states that 'Cepheid distances were obtained for 17 galaxies chosen to provide a calibration for secondary methods,' while the same paragraph and §11 refer to 18 galaxies surveyed and analyzed. The count should be reconciled.
[§10, Eq. (7)] The Friedmann equation is written with a curvature term -k/r^2, where the standard form uses the scale factor, -k/a^2 (or -k/R^2). The symbol should be corrected to avoid confusion with the radial coordinate.
[§3.2 and Table 14] The adopted metallicity slope is -0.2 +/- 0.2 mag/dex, and §3.2 notes that Caputo, Marconi & Musella (2000) find +0.27 mag/dex with the opposite sign. Table 14 assigns a symmetric +/-4% to metallicity. Given that the sign is not established, the authors should state whether the +/-4% covers the full range of published slopes, including the positive ones, or only the range around the adopted negative value.
[References] Several citations do not match the reference list: the text cites Han & Mould (1990) but the list gives Han & Mould 1992; the text cites Kelson et al. 1994 in §3.4 but the list gives Kelson et al. 1996; the text cites 'Schmidt, Kirshner, & Eastman (1994)' while the list gives 'Schmidt, B.P., Eastman, R.G., & Kirshner, R. 1994'; and the Eastman, Schmidt & Kirshner entry reads 'ApJ, 466 9 11,' which appears to be a mangled page range.
[§9.2 heading] The heading reads 'Time Delays for Gravitional Lenses'; 'Gravitational' is meant.
[§8.1, footnote 20] The footnote reads 'In two recent Key Project papers, we adopted a distance modulus to the LMC of +/-0.13 mag,' which omits the central value and reads as a fragment. It should state the modulus and its error explicitly.
[Table 12, Type II row] Table 12 lists the Type II sample as '4 Type II supernovae' over '1,900 < cz < 14,200 km/sec,' whereas §6.5 describes the same sample as having velocities 'in the range ~2000 < vCMB < 14,000.' The two ranges should be made identical.

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The paper

The paper claims

The Hubble Space Telescope Key Project concludes that the universe expands at about 72 km/s/Mpc, with a total uncertainty of roughly 8 km/s/Mpc, after recalibrating Cepheid distances and five secondary distance indicators.

The reading

The paper's aim is to pin down the Hubble constant, the present-day expansion rate that sets the age and size of the universe, by using HST-discovered Cepheid variables to calibrate five independent methods that reach far beyond the Cepheids. The authors re-derive Cepheid distances to 31 galaxies with a new LMC period-luminosity relation, a revised WFPC2 photometric zero point, a metallicity correction, and a correction for short-period incompleteness bias, then apply those distances to Type Ia and Type II supernovae, the Tully-Fisher relation, surface brightness fluctuations, and the fundamental plane. They conclude that the methods agree and give $H_0 = 72 pm 3$ (random) $pm 7$ (systematic) km/s/Mpc, or $72 pm 8$ with errors added in quadrature. If correct, the long-standing disagreement over $H_0$ is reduced to a 10% error budget, and the result favors a universe about 13 Gyr old with a cosmological constant. The authors themselves flag the LMC distance zero point as one of the largest remaining systematics.

What carries the argument

The load-bearing device is the Cepheid period-luminosity relation used as an absolute calibrator: the LMC sets the zero point, the Udalski et al. slopes set the period dependence, and a reddening-free Wesenheit combination $W = V - R(V-I)$ turns $V$ and $I$ photometry into a true distance modulus. The authors then correct that modulus for metallicity and for magnitude-limited bias at short periods, and tie the HST WFPC2 photometry to a revised zero point. Each secondary method is calibrated with a subset of these Cepheid distances, so the same zero-point error propagates coherently through all five $H_0$ values; that coherence is why method-to-method agreement cannot by itself validate the absolute scale.

Extended reading notes

Core claim

The central claim is that a single, internally consistent Cepheid calibration yields $H_0 = 72 pm 8$ km/s/Mpc across five secondary distance indicators. The individual values are $71 pm 2 pm 6$ for Type Ia supernovae, $71 pm 3 pm 7$ for Tully-Fisher, $70 pm 5 pm 6$ for surface brightness fluctuations, $72 pm 9 pm 7$ for Type II supernovae, and $82 pm 6 pm 9$ for the fundamental plane. Four methods cluster at 70-72 km/s/Mpc; the fundamental plane is the outlier but carries low weight because it is calibrated by only three clusters. Combining the five with frequentist, Bayesian, and Monte Carlo weighting gives $72 pm 3$ random $pm 7$ systematic, and the revised calibration also brings the Cepheid distance to NGC 4258 closer to its maser distance.

Load-bearing premise

The whole ladder rests on the adopted Large Magellanic Cloud distance modulus of $18.50 pm 0.10$ mag, an external zero point that multiplies every Cepheid distance and every secondary-method $H_0$; the paper notes that 18.3 mag would raise $H_0$ to about 79 km/s/Mpc.

Editorial extensions

If this is right

For a flat universe with $\Omega_m = 0.3$ and $\Omega_\Lambda = 0.7$, $H_0 = 72$ gives an expansion age near 13 Gyr, consistent with revised globular-cluster ages and favoring a cosmological constant.
The Einstein-de Sitter case ($\Omega_m = 1$, $\Omega_\Lambda = 0$) would give only about 9 Gyr at this $H_0$, in tension with the oldest stars.
The long-standing spread among $H_0$ measurements is reduced to a 10% error budget, with the remaining spread dominated by shared systematics rather than by the secondary methods.
The Cepheid-calibrated distances provide a common zero point for Type Ia supernovae, Tully-Fisher, surface brightness fluctuations, and the fundamental plane, so future distance indicators can be placed on the same scale.
The revised Cepheid distance to NGC 4258 agrees with its maser distance within about $1.2\sigma$, an external check on the ladder.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

Because all five methods inherit the same LMC zero point, a future geometric LMC distance that shifts the modulus by 0.1 mag would move every $H_0$ value coherently; the observed method-to-method scatter therefore cannot reveal that error.
The fundamental plane's 82 km/s/Mpc value is the one place where the calibration sample is thin, at three clusters; a larger Cepheid-calibrated cluster sample would test whether that outlier is a real astrophysical difference or a small-number calibration error.
Unresolved blending is assigned a $+5/-0$% uncertainty rather than a correction; if blending is stronger in the most distant Cepheid hosts, the ladder could be biased toward low $H_0$ at exactly the distances where the secondary methods are calibrated.
An independent geometric distance to a galaxy hosting both Cepheids and a Type Ia supernova would break the degeneracy between the LMC zero point and the supernova absolute magnitude, which is the tightest current route to a percent-level $H_0$.

Original abstract

We present here the final results of the Hubble Space Telescope Key Project to measure the Hubble constant. We summarize our method, the results and the uncertainties, tabulate our revised distances, and give the implications of these results for cosmology. The analysis presented here benefits from a number of recent improvements and refinements, including (1) a larger LMC Cepheid sample to define the fiducial period-luminosity (PL) relations, (2) a more recent HST Wide Field and Planetary Camera 2 (WFPC2) photometric calibration, (3) a correction for Cepheid metallicity, and (4) a correction for incompleteness bias in the observed Cepheid PL samples. New, revised distances are given for the 18 spiral galaxies for which Cepheids have been discovered as part of the Key Project, as well as for 13 additional galaxies with published Cepheid data. The new calibration results in a Cepheid distance to NGC 4258 in better agreement with the maser distance to this galaxy. Based on these revised Cepheid distances, we find values (in km/sec/Mpc) of H0 = 71 +/- 2 (random) +/- 6 (systematic) (type Ia supernovae), 71 +/- 2 +/- 7 (Tully-Fisher relation), 70 +/- 5 +/- 6 (surface brightness fluctuations), 72 +/- 9 +/- 7 (type II supernovae), and 82 +/- 6 +/- 9 (fundamental plane). We combine these results for the different methods with 3 different weighting schemes, and find good agreement and consistency with H0 = 72 +/- 8. Finally, we compare these results with other, global methods for measuring the Hubble constant.

The compiled record

The paper's own sentences, arranged, kept beside the review and separate from it. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 6,621 input tokens.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.65 · human participants 0.02 · controlled comparison 0.10 · randomized assignment 0.01 · states quantitative result 0.99 · compares with prior results 0.96 · mentions code or data availability 0.03.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; show every role.

We present here the final results of the Hubble Space Telescope Key Project to measure the Hubble constant. We summarize our method, the results and the uncertainties, tabulate our revised distances, and give the implications of these results for cosmology. The analysis presented here benefits from a number of recent improvements and refinements, including (1) a larger LMC Cepheid sample to define the fiducial period-luminosity (PL) relations, (2) a more recent HST Wide Field and Planetary Camera 2 (WFPC2) photometric calibration, (3) a correction for Cepheid metallicity, and (4) a correction for incompleteness bias in the observed Cepheid PL samples. New, revised distances are given for the 18 spiral galaxies for which Cepheids have been discovered as part of the Key Project, as well as for 13 additional galaxies with published Cepheid data. The new calibration results in a Cepheid distance to NGC 4258 in better agreement with the maser distance to this galaxy. Based on these revised Cepheid distances, we find values (in km/sec/Mpc) of H0 = 71 +/- 2 (random) +/- 6 (systematic) (type Ia supernovae), 71 +/- 2 +/- 7 (Tully-Fisher relation), 70 +/- 5 +/- 6 (surface brightness fluctuations), 72 +/- 9 +/- 7 (type II supernovae), and 82 +/- 6 +/- 9 (fundamental plane). We combine these results for the different methods with 3 different weighting schemes, and find good agreement and consistency with H0 = 72 +/- 8. Finally, we compare these results with other, global methods for measuring the Hubble constant.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
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s0	We present here the final results of the Hubble Space Telescope Key Project to measure the Hubble constant.	contribution 1.00	0.87	0.07	asserted 0.93
s1	We summarize our method, the results and the uncertainties, tabulate our revised distances, and give the implications of these results for cosmology.	contribution 0.98	0.92	0.05	asserted 0.94
s2	The analysis presented here benefits from a number of recent improvements and refinements, including (1) a larger LMC Cepheid sample to define the fiducial period-luminosity (PL) relations, (2) a more recent HST Wide Field and Planetary Camera 2 (WFPC2) photometric calibration, (3) a correction for Cepheid metallicity, and (4) a correction for incompleteness bias in the observed Cepheid PL samples.	method 0.94	0.39	0.03	asserted 0.99
s3	New, revised distances are given for the 18 spiral galaxies for which Cepheids have been discovered as part of the Key Project, as well as for 13 additional galaxies with published Cepheid data.	contribution 0.68	0.86	0.03	asserted 1.00
s4	The new calibration results in a Cepheid distance to NGC 4258 in better agreement with the maser distance to this galaxy.	result 0.92	0.87	0.04	asserted 0.97
s5	Based on these revised Cepheid distances, we find values (in km/sec/Mpc) of H0 = 71 +/- 2 (random) +/- 6 (systematic) (type Ia supernovae), 71 +/- 2 +/- 7 (Tully-Fisher relation), 70 +/- 5 +/- 6 (surface brightness fluctuations), 72 +/- 9 +/- 7 (type II supernovae), and 82 +/- 6 +/- 9 (fundamental plane).	result 1.00	0.97	0.57	asserted 1.00
s6	We combine these results for the different methods with 3 different weighting schemes, and find good agreement and consistency with H0 = 72 +/- 8.	result 0.97	0.97	0.66	asserted 0.98
s7	Finally, we compare these results with other, global methods for measuring the Hubble constant.	contribution 0.66	0.80	0.03	unclear 0.66

What kind of paper the classifier reports this is: empirical study 1.00 · evidence from observation or experiment 0.56.

What was examined, and what was not

sources read

arXiv listing abstract v1

not examined

full text
figures and tables
references and citing sentences
relations to other papers

levels run

P abstract

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T body sentences
C citations
R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

Figures

**Figure 1.** — Velocity versus distance for galaxies with Cepheid

**Figure 2.** — Three sets of Hubble relations constructed from the

**Figure 3.** — Values of H0 and their uncertainties for type Ia supernovae, the Tully-Fisher relation, the fundamental plane, surface brightness fluctuations, and type II supernovae, all calibrated by Cepheid variables. Each value is represented by a Gaussian curve (joined solid dots) with unit area and a 1-σ scatter equal to the random uncertainty. The systematic uncertainties for each method are indicated by the horizontal bars near the peak of each Gaussian. The upper curve is obtained by summing the individual Gaussians. The cumulative (frequentist) distribution has a midpoint (median) value…

**Figure 4.** — [Top panel]: A Hubble diagram of distance versus vel

**Figure 5.** — The distribution of LMC distance moduli as compiled

**Figure 7.** — Values of the Hubble constant determined using the S

**Figure 8.** This Hubble diagram covers over 3 orders of magnitu

**Figure 9.** — H0t0 versus Ω for H0 = 72 km s−1 Mpc−1 , t0 = 12.5 Gyr, and uncertainties of ±10% adopted for both quantities. The dark line indicates the case of a flat Universe with ΩΛ + Ωm = 1. The abscissa in this case corresponds to ΩΛ. The lighter curve represents a Universe with ΩΛ = 0. In this case, the abcissa should be read as Ωm. The dashed and dot-dashed lines indicate 1-σ and 2-σ limits, respectively for values of H0 = 72 and t0 = 12.5 Gyr in the case where both quantities are assumed to be known to ±10% (1-σ). The large open circle denotes values of H0t0 = 2/3 and Ωm = 1 (i.e.,…

Showing 8 of the paper's 9 figures. See all figures in the PDF ↗ Figures reproduced from arXiv:astro-ph/0012376 by the authors.

References

Works cited (15)

[1]

Aaronson, M., Mould, J. R. & Huchra, J. 1979, ApJ, 229, 1 Aaronson, M., et al. 1982, ApJS, 50, 241 Aaronson, M., & Mould, J. R. 1986, ApJ, 303, 1 Aaronson, M., Bothun, G.D., Mould, J.R., Huchra, J., Schomm er, R.A., & Cornell, M.E. 1986, ApJ, 302, 536 Alibert, Y., Baraﬀe, I., Hauschildt, P. and Allard, F. 1999, A&A, 344, 551 Bahcall, N.A., & Fan, X. 1998,...

View on Pith Pith review arXiv 2000
[2]

List of Cepheid Galaxies / Calibrators Galaxy Secondary Methods Calibrated by a Given Galaxy NGC 224 TF, SBF NGC 300 . . . NGC 598 TF NGC 925 TF NGC 1326A FP-Fornax 1 NGC 1365 TF, FP-Fornax NGC 1425 TF, FP-Fornax NGC 2090 TF NGC 2403 TF NGC 2541 TF NGC 3031 TF, SBF NGC 3198 TF NGC 3319 TF NGC 3351 TF, FP-Leo 1 NGC 3368 TF, FP-Leo, SBF, SNIa (1998bu) NGC 3...

View on Pith 2000
[3]

Numbers of Cepheid Calibrators for Secondary Metho ds Secondary Method σ N (pre–HST) σmean N (post–HST) σmean % % % Tully-Fisher relation ±20% a 5 b ±10% 21 ±5% Type Ia supernovae ±8% c 0 n/a 6 d ±4% Surface brightness ﬂuctuations ±9% e 1 ±9% 6 ±4% Fundamental plane ±14% 0 n/a 3 f ±10% Type II supernovae ±12% g 1 ±12% 4 ±6% a Giovanelli et al. (1997) b M3...

View on Pith 1997
[5]

Local Velocity Flow Galaxy VHelio VLG VCM B VV irgo VGA VShapley VT onry NGC 0300 144 125 -57 114 92 133 -140 NGC 0925 553 781 398 778 561 664 374 NGC 1326A 1836 1749 1787 1698 1742 1794 1164 NGC 1365 1636 1544 1597 1503 1544 1594 1157 NGC 1425 1512 1440 1477 1403 1417 1473 1465 NGC 2403 131 300 216 343 222 278 193 NGC 2541 559 646 736 744 674 714 936 NGC...

View on Pith 2024
[6]

Revised Cepheid Distances to Galaxies . . . Galaxy µ aold σ Nceph µ brevised σ µ cP cut σ Ncutceph Data Source NGC 224 d 24.41 0.08 37 24.38 0.05 24.38 0.05 37 Freedman & Madore (1990 ) NGC 300 d 26.62 0.10 16 26.53 0.07 26.53 0.07 14 Freedman et al. (1992) NGC 598 d 24.58 0.10 12 24.56 0.10 24.56 0.08 11 Freedman et al. (1991) NGC 925 29.94 0.04 73 29.80...

View on Pith 1992
[8]

NGC 4321 30.93 0.07 52 30.75 0.07 30.78 0.07 42 Ferrarese et al . (1996) NGC 4414 31.37 0.09 9 31.18 0.09 31.10 0.05 8 Turner et al. (199

View on Pith 1996
[9]

f IC 1613 24.29 0.14 10 24.24 0.14 24.19 0.15 9 Freedman (1988) f aAdopting Madore & Freedman (1991) PL slopes; LMC distance mo dulus 18.50; ALLFRAME intensity- weighted mean magnitudes or Stetson template ﬁts if availab le; Hill et al. (1998) calibration, except for M31 (NGC 224), M33 (NGC 598), IC 1613, NGC 300, NGC 2403, M81 (NGC 3 031), M101 (outer; NGC

View on Pith 1988
[12]

Uncertainties in H 0 for Secondary Methods Method H 0 Error (%) References 36 Type Ia supernovae 71 ±2r ±6s Hamuy et al. (1996), Riess et al. (1998), 4,000 < cz < 30,000 km/sec Jha et al. (1999), Gibson et al. (2000) 21 Tully–Fisher clusters 71 ±3r ±7s Giovanelli et al. (1997), Aaronson et al. (1982, 1986), 1,000 < cz < 9,000 km/sec Sakai et al. (2000) 11...

View on Pith 1996
[13]

LMC Distance Moduli for Diﬀerent Methods Method < µ 0 > (mag) a σ (mag) N < µ 0 >(mag) b σ (mag) N Cepheids 18.57 ±0.14 5 18.52 ±0.13 15 Eclipsing variables 18.33 ±0.05 3 . . . . . . . . . SN1987A 18.47 ±0.08 4 18.50 ±0.12 5 TRGB 18.64 ±0.05 2 18.42 ±0.15 1 Red Clump 18.27 ±0.11 10 . . . . . . . . . RR Lyrae variables 18.30 ±0.13 7 18.40 ±0.19 14 Mira var...

View on Pith 2000
[30]

86 14.86 8.77 NGC 4535 31.32 0.04 31.13 0.04 0.19 0.02 30.85 0.05 14.79 30.9 9 15.78 9.20 NGC 4536 31.24 0.04 31.06 0.04 0.18 0.02 30.80 0.04 14.45 30.8 7 14.93 8.85 NGC 4548 31.30 0.07 31.12 0.04 0.18 0.04 30.88 0.05 15.00 31.0 5 16.22 9.34 NGC 4639 31.96 0.09 31.84 0.07 0.12 0.04 31.61 0.08 20.99 31.7 1 21.98 9.00 NGC 4725 31.08 0.08 30.79 0.07 0.29 0.0...

View on Pith 1996
[31]

04 16.14 8.50 NGC 1365 31.69 0.05 31.49 0.04 0.20 0.02 31.18 0.05 17.22 31.2 7 17.95 8.96 NGC 1425 32.01 0.07 31.85 0.05 0.16 0.03 31.60 0.05 20.89 31.7 0 21.88 9.00 NGC 2090 30.71 0.05 30.54 0.04 0.17 0.02 30.29 0.04 11.43 30.3 5 11.75 8.80 NGC 2403 . . . . . . 27.75 0.10 0.2 c 0.1 27.48 0.10 3.13 27.54 3.22 8.80 NGC 2541 30.74 0.05 30.54 0.04 0.20 0.02 ...

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[998]

NGC 2403 e 27.59 0.24 10 27.48 0.24 27.48 0.24 10 Freedman & Madore (1988 ) NGC 2541 30.43 0.07 34 30.26 0.07 30.25 0.05 29 Ferrarese et al . (1998) NGC 3031 27.75 0.07 25 27.67 0.07 27.75 0.08 17 Freedman et al. (1994) NGC 3198 30.80 0.08 42 30.64 0.08 30.68 0.08 36 Kelson et al. (1

View on Pith 1998
[1990]

c Hamuy et al. (1996) d Using the distances to the host galaxies to SN 1960F, 1972E, 1 981B, 1989B, 1990N, 1998bu; but excluding 1895B, 1937C, 1974G e Tonry et al. (1997) f calibration based on Cepheid distances to Leo I group, Virgo and Fornax clusters gthis paper, Schmidt et al. (1994) distant clusters – 58 – Table

View on Pith 1996
[1999]

Type Ia supernova sa mples. Left Panel : The full sample of 50 supernovae, with peak magnitudes correcte d only for foreground Galactic reddening. All tabulated heliocentric velocities have bee n corrected to the cosmic microwave background reference frame using the velocity calculator a vailable in the NASA Extragalactic Database (NED). Middle Panel : Ou...

View on Pith 1989
[5457]

bAdopting Udalski et al. (1999) PL slopes; same Cepheid sampl e as for column 2; Stetson (1998) WFPC2 calibration, except for for M31, M33, IC 1613, NGC 300, NGC 24 03, M81. (To transform distance moduli from Hill et al. to Stetson, 0.07 mag is subtracted.) cSame calibration as for column 5, but applying a period cut at the short period end to minimize bi...

View on Pith 1999

Forward citations

Cited by 50 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

A kilonova as the electromagnetic counterpart to a gravitational-wave source
astro-ph.HE 2017-10 accept novelty 9.0 of 10

The transient AT2017gfo, spatially and temporally coincident with GW170817, faded and reddened as a low-mass, high-velocity, radioactively powered kilonova should, tying neutron-star mergers to r-process nucleosynthesis.
A Jet from a Nearly Dormant Black Hole
astro-ph.HE 2026-06 unverdicted novelty 8.0 of 10

Multi-frequency VLBI observations detect a two-sided jet with steep synchrotron spectrum from the nearly dormant SMBH in M60, with frequency-dependent core shift locating the engine ~10 Schwarzschild radii upstream of...
The Dancing Bonfire: An Unusual Persistent X-ray Source in M81 Exhibiting Recurrent Luminous Flares
astro-ph.HE 2026-10 accept novelty 7.0 of 10

M81F4是一个在M81中持续明亮的X射线源，其重复的数百秒耀斑与任何已知X射线双星均不匹配，暗示了一个通过盘-磁层不稳定性产生耀斑的磁化中子星。
The Effective Field Theory of Dark Energy
hep-th 2012-09 accept novelty 7.0 of 10

A single unitary-gauge action with time-dependent coefficients reproduces all single-field dark energy and modified gravity models, with only three functions fixed by the background expansion.
Recovering the Inflationary Potential and Primordial Power Spectrum With a Slow Roll Prior: Methodology and Application to WMAP 3 Year Data
astro-ph 2006-03 conditional novelty 7.0 of 10

A new Markov Chain Monte Carlo method that varies the Hubble slow roll parameters directly, using the inflationary flow equations, is applied to WMAP3 and SDSS data, yielding tight constraints on inflationary models a...

Show 45 more citing papers

Gravitational clustering of relic neutrinos and implications for their detection
hep-ph 2004-08 accept novelty 7.0 of 10

Relic neutrinos cluster gravitationally onto dark matter halos and the Milky Way, reaching local overdensities of up to about 20 for a 0.6 eV neutrino, and the linear approximation systematically underestimates this c...
Pulsation periods reveal tension between theoretical and empirical radii for classical Cepheids in eclipsing binary systems
astro-ph.SR 2026-08 conditional novelty 6.0 of 10

Using pulsation period instead of radius as a constraint for Cepheid evolutionary models systematically lowers the predicted radius, exposing a tension that is partially explained by a nonlinear radius increase in ful...
JWST Reveals Large Reservoirs of Dust and Ongoing Circumstellar Interaction in SN Ibn/Icn 2023xgo over a Year Post-Explosion
astro-ph.HE 2026-05 unverdicted novelty 6.0 of 10

Late-time JWST spectra of SN 2023xgo detect cool silicate or carbonaceous dust masses of order 0.01-0.03 solar masses plus narrow He I emission indicating ongoing circumstellar interaction at +377 days.
Expanding Ejecta Method: I. Mapping Supernova Morphology with Intensity Interferometry
astro-ph.HE 2025-04 conditional novelty 6.0 of 10

The expanding ejecta method extracts supernova morphology and angular diameter distance from spectrally resolved intensity interferometry, forecasting ~2% distance precision for a magnitude-12 Type IIP supernova in 60 hours.
Rock 'n' Roll Solutions to the Hubble Tension
astro-ph.CO 2019-04 conditional novelty 6.0 of 10

A φ^4 scalar field thawing near matter-radiation equality fits CMB, BAO, and local H0 data better than ΛCDM, raising H0 to about 70 km/s/Mpc, while the coarse-grained fluid approximation used in earlier work misrepres...
Planck 2013 results. XVI. Cosmological parameters
astro-ph.CO 2013-03 conditional novelty 6.0 of 10

Planck's first CMB temperature and lensing spectra fit a flat six-parameter LambdaCDM model at high multipoles and yield H0 = 67.3 +/- 1.2 km/s/Mpc, Omega_m = 0.315 +/- 0.017, and no evidence for extra relativistic sp...
The 6dF Galaxy Survey: Baryon Acoustic Oscillations and the Local Hubble Constant
astro-ph.CO 2011-06 conditional novelty 6.0 of 10

A 2.4-sigma baryon acoustic oscillation detection in the 6dF Galaxy Survey yields an independent local Hubble constant of 67 plus or minus 3.2 km/s/Mpc.
Cosmography with the Einstein Telescope
astro-ph.CO 2009-06 conditional novelty 6.0 of 10

Simulated catalogues of 1,000 neutron-star mergers detected by the Einstein Telescope with optical counterparts give 1-sigma errors of about 4% on dark energy density, 18% on matter density, and 18% on the dark energy...
Local Void vs Dark Energy: Confrontation with WMAP and Type Ia Supernovae
astro-ph 2007-12 conditional novelty 6.0 of 10

A spherical void of radius 200-250 Mpc/h with central underdensity about 45% can fit supernova and WMAP three-year data without dark energy, at the cost of a low external Hubble constant and large spectral running.
Compact Stars as Dark Matter Probes
astro-ph 2007-09 conditional novelty 6.0 of 10

Captured dark matter annihilating inside white dwarfs in globular clusters and inside neutron stars can set constraints on the dark matter density and on the WIMP-nucleon cross section competitive with direct detection.
Inflationary Potential Reconstruction for a WMAP Running Power Spectrum
astro-ph 2006-03 conditional novelty 6.0 of 10

A running spectral index at the WMAP level, if real, forces a high inflation scale with a tensor-to-scalar ratio near 0.5 and a quartic-like reconstructed inflaton potential, with only 15 to 20 e-foldings of exponenti...
Constraining Cosmological Parameters Based on Relative Galaxy Ages
astro-ph 2001-06 conditional novelty 6.0 of 10

Age differences between passively evolving galaxies at nearby redshifts give dz/dt, hence H(z) and, through its second derivative, the dark energy equation of state, with far more sensitivity than luminosity distances.
Exploring the synergies of $[\mathrm{O\,II}]\lambda 3727$ with MUSE spectroscopy in PHANGS H II regions
astro-ph.GA 2026-07 unverdicted novelty 5.5 of 10

Combining [O II] doublet data with MUSE spectra creates a homogeneous H II region catalog and compares strong-line metallicity calibrations, showing low scatter in radial gradients and [S III]/[S II] as a robust ioniz...
DOWSING, Dust Observations With SCUBA-2 In Nearby Galaxies: I. Dust in M81
astro-ph.GA 2026-11 conditional novelty 5.0 of 10

New SCUBA-2 450/850 micron observations of M81 give dust masses of 1.77e7 Msun (single-temperature fit) and 2.65e7 Msun (multi-temperature PPMAP), plus an HI-based gas-to-dust ratio gradient of 0.065 dex/kpc.
Theoretical RR Lyrae Instability Strip from MESA-RSP Pulsation models and updated BaSTI Evolutionary Tracks
astro-ph.SR 2026-09 conditional novelty 5.0 of 10

Updated BaSTI tracks plus mesa-rsp linear pulsation models reproduce earlier RR Lyrae instability strips while showing the strip edges and period-luminosity relations depend jointly on mode, metallicity, and convectio...
No Evidence for Nearby Circumstellar Material in the Type Ia Supernova 2025rbs
astro-ph.HE 2026-08 conditional novelty 5.0 of 10

No time-variable sodium or calcium absorption is seen toward SN 2025rbs from -5 to +15 days, ruling out detectable circumstellar material near the progenitor.
Toward Unbiased Abundance Measurements in Inhomogeneous $\mathrm{H\,II}$ Regions
astro-ph.GA 2026-07 conditional novelty 5.0 of 10

Combining [N II] electron temperatures with [O II] auroral-to-nebular densities yields HII-region oxygen abundances less biased by density inhomogeneities, with the abundance discrepancy factor possibly larger in meta...
Toward Bayesian photometric cosmic chronometers: Application to VIPERS
astro-ph.GA 2026-06 unverdicted novelty 5.0 of 10

Bayesian photometric cosmic chronometer analysis on VIPERS PDR2 data yields H(z=0.65)=93.68±28.27(stat)±10.67(syst) km/s/Mpc, consistent with spectroscopic CC results and Planck ΛCDM, as a proof of concept for photome...
Combined analysis of Planck and SPTPol data favors the early dark energy models
astro-ph.CO 2020-04 conditional novelty 5.0 of 10

Truncating Planck temperature data below multipole 1000 and adding SPTPol polarization and lensing lowers S8 to 0.763 and raises H0 to 69.7, and an early dark energy component then removes the remaining Hubble tension...
New physics in light of the $H_0$ tension: an alternative view
astro-ph.CO 2019-07 conditional novelty 5.0 of 10

Fixing the dark energy equation of state near -1.3, or the relativistic species count near 3.95, makes the CMB plus BAO plus supernova estimate of the Hubble constant coincide with the local ladder value, at a steep B...
GW170817 Falsifies Dark Matter Emulators
astro-ph.HE 2017-10 conditional novelty 5.0 of 10

The near-simultaneous arrival of gravitational waves and gamma rays from GW170817 falsifies modified-gravity 'dark matter emulator' theories, which predicted a photon delay of roughly 400 days.
Cosmic Chronometers: Constraining the Equation of State of Dark Energy. I: H(z) Measurements
astro-ph.CO 2009-07 conditional novelty 5.0 of 10

New Keck spectra of red-envelope galaxies in 24 clusters yield direct expansion-rate measurements H(z) = 97 +/- 62 at z about 0.5 and 90 +/- 40 km/s/Mpc at z about 0.8, which modestly tighten dark-energy and neutrino ...
Confronting Lemaitre-Tolman-Bondi models with Observational Cosmology
astro-ph 2008-02 conditional novelty 5.0 of 10

A Gpc-scale local void in an otherwise Einstein-de Sitter universe fits current supernova, CMB and BAO data about as well as flat LCDM, but Bayesian model comparison still mildly favours LCDM.
Probing Inflation and Dark Energy with Current Cosmological Observations
astro-ph 2006-03 conditional novelty 5.0 of 10

Jointly fitting inflation parameters (spectral index, running, tensor ratio) and dark energy parameters (w0, w1) to WMAP1+SDSS+SNIa data broadens constraints and slightly increases preference for a running primordial ...
A Markov Chain Monte Carlo Analysis of the CMSSM
hep-ph 2006-02 conditional novelty 5.0 of 10

A Bayesian MCMC scan of the Constrained MSSM yields 68% intervals for m1/2, m0, A0 and tan beta, shows m0 is prior-dependent while the other parameters are robust, and maps correlations among rare B decays and dark ma...
Cosmological parameters from CMB and other data: a Monte-Carlo approach
astro-ph 2002-05 accept novelty 5.0 of 10

Joint MCMC analysis of CMB, galaxy survey, supernova, Hubble and nucleosynthesis data yields tight cosmological parameter constraints, including neutrino mass below 0.3 eV and a dark energy equation of state consisten...
An all-sky catalogue of Be transition stars from WISE and Gaia
astro-ph.SR 2026-11 conditional novelty 4.0 of 10

A Gaia and WISE based search finds 3,300 stars transitioning between B-type and Be phases, with median disk build-up and decay times of 459 and 478 days.
Hubble tension: a short review of theoretical explanations
astro-ph.CO 2026-07 accept novelty 4.0 of 10

A comprehensive review finds no theoretical Hubble-tension solution yet passes all consistency tests; new early-dark-energy chains reach high H0 only when the SH0ES calibration is added.
Redshift Duality with Pantheon+SH0ES in a Planck-anchored Flat $\Lambda$CDM Framework: Implications for Hubble Tension and Observational Inference
astro-ph.CO 2026-06 unverdicted novelty 4.0 of 10

Hybrid redshift model with postulated quantum correction fits Pantheon+SH0ES data to recover Planck-consistent expansion H_Λ and eliminates apparent drift in inferred Hubble parameter across bins.
Effect of Peak Absolute Magnitude of Type Ia Supernovae and Sound Horizon Values on Hubble Tension using DESI results
astro-ph.CO 2024-12 conditional novelty 4.0 of 10

Using DESI DR1, Pantheon+ and cosmic chronometer data, the authors show that changing the Type Ia supernova absolute magnitude and sound-horizon priors moves the inferred H0 from about 73 to 68 km/s/Mpc, reducing the ...
Hubble tension or a transition of the Cepheid SnIa calibrator parameters?
astro-ph.CO 2021-09 conditional novelty 4.0 of 10

Allowing the Cepheid Wesenheit color parameter to take two values split at about 16 Mpc lowers the inferred Hubble constant from about 73 to about 68, consistent with Planck.
Reconstruction of $f(T)$ gravity: Rip cosmology, finite-time future singularities and thermodynamics
gr-qc 2012-02 conditional novelty 4.0 of 10

Finite-time cosmic singularities arise in f(T) torsion gravity and a T-squared correction term removes them, closely mirroring known behavior in f(R) gravity.
Constraints on massive sterile neutrino species from current and future cosmological data
astro-ph.CO 2011-02 conditional novelty 4.0 of 10

Current CMB, galaxy clustering and supernova data allow two sub-eV sterile neutrinos alongside three sub-eV active ones, though thermal sterile abundances conflict with Big Bang Nucleosynthesis.
Observables sensitive to absolute neutrino masses. II
hep-ph 2008-05 conditional novelty 4.0 of 10

Updated oscillation and cosmological data tighten neutrino mass-mixing parameters and leave the Heidelberg-Moscow neutrinoless double beta claim compatible with cosmology only if Lyman-alpha data are excluded.
CMB constraints on the fine structure constant
astro-ph 2006-02 conditional novelty 4.0 of 10

WMAP first-year CMB data place the fine structure constant during recombination within about 4 percent of its present value, and no variation is detected even when the electron mass is allowed to vary alongside it.
$\Lambda$CDM Tensions: Localising Missing Physics through Consistency Checks
astro-ph.CO 2024-02 conditional novelty 3.0 of 10

Fitting flat Lambda-CDM separately in redshift bins and finding that H0 falls and Omega_m rises with effective redshift would mean the background model is broken, and several independent compilations reportedly show e...
Strong gravitational lensing of explosive transients
astro-ph.CO 2019-07 accept novelty 3.0 of 10

Strong lensing of explosive transients, with their fast light curves and compact sizes, enables precise time-delay cosmography, small-scale dark matter probes, and wave-optics tests that lensed quasars cannot deliver.
Beyond the Cosmological Standard Model
astro-ph.CO 2014-06 accept novelty 3.0 of 10

Modified gravity models can be organized by their screening mechanism, and this review maps the three classes and the experiments that can test them.
The Hubble Tension and Early Dark Energy
astro-ph.CO 2022-11 unverdicted novelty 2.0 of 10

The Hubble tension between local and early-universe expansion-rate measurements may be resolved by early dark energy that speeds up expansion before recombination while satisfying existing constraints.
Dark energy cosmology: the equivalent description via different theoretical models and cosmography tests
gr-qc 2012-05 conditional novelty 2.0 of 10

The paper reviews how many dark energy and modified-gravity models can be recast as equivalent fluid or scalar-field descriptions and can be tuned to fit current cosmological data.
Quintom Cosmology: Theoretical implications and observations
hep-th 2009-09 accept novelty 2.0 of 10

Quintom dark energy, in which the equation of state crosses w = -1, is reviewed as an observationally motivated but theoretically challenging extension of standard cosmology.
Dark matter, and its darkness
astro-ph 2006-03 conditional novelty 2.0 of 10

Flat lambda-CDM cosmology with a stellar-age constraint implies Ωm between 0.22 and 0.35, far above the standard-model value of 0.05, and the essay identifies a spin-half field with (CPT)^2=-1 as the dark matter candidate.
Massive neutrinos and cosmology
astro-ph 2006-03 accept novelty 1.0 of 10

A detailed review of how cosmological observations bound the sum of neutrino masses through the free-streaming suppression of small-scale structure, and of future sensitivity forecasts.
Cosmology with strong gravitational lenses
astro-ph.CO 2026-10 accept

Strong gravitational lensing provides a purely gravitational probe that measures H0 at 3% precision from 11 lensed quasars and hints at dark matter self-interaction from dense subhalos.
Stable Massive Particles at Colliders
hep-ph 2006-11 accept

The paper is a comprehensive review of collider searches for stable massive particles, their theoretical motivations, detector signatures, and the resulting mass and cross-section limits.

How later papers used it

288 later papers cite it

Evidence: substantial. 273 of the citing papers share no author with it, and 151 of those carry a confident label from Pith's citation classifier.

Pith read 40 of the 384 citing sentences, choosing only those whose citation markers point at this paper alone, and wrote the paraphrases from them. The summary, the counts, the evidence level, the links and the quotes come from code; the summary counts the papers listed below. A later paper is listed under a label when Pith's citation classifier gives one of its sentences that label at probability 0.8 or more (0.95 for support), Pith's reading finds that the citing paper itself did it, and a second check confirms the paraphrase against the sentence. This section lists uses only. It does not list criticism or disagreement, so their absence here says nothing about how the paper has been received. Papers that share an author with this one are listed apart, under "By the same authors". A quote is the citing authors' own sentence, shown when their paper's licence is CC BY, CC BY-SA or CC0. JSON

23 later papers by other authors are listed below: 23 used its data or values.

Uses its data or values 23 of 146 papers with this label

Used a prior on the Hubble parameter H0 = 0.72 ± 0.08 derived from Hubble Space Telescope measurements from this paper.

Cosmological constraints on the Hu-Sawicki modified gravity scenario (2009) · 1.00 · paraphrased: the licence does not allow quoting
Used only this paper's result from the Hubble Space Telescope Key Project team papers, adopting its metallicity-corrected distance values.

An independent determination of the local Hubble constant (2017) · 1.00 · paraphrased: the licence does not allow quoting
Used the Hubble constant measurement from the Hubble Space Telescope Key Project of this paper as data.

Challenges to the DGP Model from Horizon-Scale Growth and Geometry (2008) · 1.00 · paraphrased: the licence does not allow quoting
Imposed the Gaussian Hubble Space Telescope prior h = 0.72 ± 0.08 from this paper.

Anisotropies in the Cosmic Neutrino Background after WMAP 5-year Data (2008) · 1.00 · paraphrased: the licence does not allow quoting
Included the Hubble Space Telescope Key Project measurement of H0 from this paper.

Are cosmological neutrinos free-streaming? (2008) · 1.00 · paraphrased: the licence does not allow quoting
Adopted the Cepheid distance of 3.15 Mpc from this paper for NGC 5253.

Thirty Years of Radio Observations of Type Ia SN 1972E and SN 1895B: Constraints on Circumstellar Shells (2020) · 1.00 · paraphrased: the licence does not allow quoting
Assumed a distance to M31 of d = 752 ± 17 kpc from this paper.

AT 2016dah and AT 2017fyp: the first classical novae discovered within a tidal stream (2020) · 1.00 · paraphrased: the licence does not allow quoting
Assumed the distance to the LMC is 50.1 kpc from this paper.

The recent LMC-SMC collision: Timing and impact parameter constraints from comparison of Gaia LMC disk kinematics and N-body simulations (2022) · 1.00 · paraphrased: the licence does not allow quoting
Drew random values for LMC and SMC distances from this paper.

The Proper Motion Field of the Small Magellanic Cloud: Kinematic Evidence for its Tidal Disruption (2018) · 1.00 · paraphrased: the licence does not allow quoting
Used the Hubble Space Telescope measurement of the Hubble parameter from this paper via a Gaussian likelihood centered on h = 0.72 with standard deviation 0.08.

Constraints on Models with a Break in the Primordial Power Spectrum (2009) · 1.00 · paraphrased: the licence does not allow quoting
Fixed the dimensionless Hubble constant to h = 0.72 from this paper.

Late universe dynamics with scale-independent linear couplings in the dark sector (2008) · 1.00 · paraphrased: the licence does not allow quoting
Used h = 0.72 ± 0.08 given by the Hubble Space Telescope Key Project of this paper.

Observational constraint on generalized Chaplygin gas model (2010) · 1.00 · paraphrased: the licence does not allow quoting
Used the Hubble Space Telescope prior on the reduced Hubble constant h = 0.72 ± 0.07 from this paper.

Observables sensitive to absolute neutrino masses. II (2008) · 1.00 · paraphrased: the licence does not allow quoting
Used the Hubble Space Telescope measurement of H0 from this paper to complete its H(z) data set.

From model dynamics to oscillating dark energy parameterisation (2008) · 1.00 · paraphrased: the licence does not allow quoting
Cited this paper for the distances to M100 and M101 in its table of observed sources.

Hydrogen Radio Recombination Line Emission from M51 and NGC628 (2018) · 1.00 · paraphrased: the licence does not allow quoting
Adopting a distance modulus for M31, $μ_o(M31) = 24.38±0.05$ [ref] , along with an absolute $K$-band magnitude for the sun of $M_K,⊙=3.27$ [ref] , yields an integrated $K$-band luminosity for M31 of $L_K(M31) = 1.2×10^11 L_⊙,K$.

The Rate and Spatial Distribution of Novae in M31 as Determined by a Twenty-Year Survey (2022) · The Luminosity-Specific Nova Rate · 1.00
We adopted a Galactic neutral hydrogen column density $NH_MW = 6.14 ×10^20 cm^-2$ [ref] in the direction of SN 2014C and a distance of 14.7 Mpc [ref] .

Six years of luminous X-ray emission from the strongly interacting type-Ib SN 2014C captured by Chandra and NuSTAR (2020) · Observations and Analysis · 1.00
Included a prior on the Hubble constant H0 from the HST Key Project of this paper.

Falsifying Paradigms for Cosmic Acceleration (2008) · 0.97 · paraphrased: the licence does not allow quoting
Took the central value of its Hubble constant prior from this paper, with a hypothetical error.

The Hubble constant and dark energy from cosmological distance measures (2007) · 1.00 · paraphrased: the licence does not allow quoting
Used this paper as a dominant source of distance information, rescaled slightly for consistency with other distances.

Cosmicflows-4: The Baryonic Tully-Fisher Relation Providing ~10,000 Distances (2022) · 0.94 · paraphrased: the licence does not allow quoting
Identified its calculated value with the measured value of the Hubble constant from this paper.

Equilibrium boundary conditions, dynamic vacuum energy, and the Big Bang (2008) · 0.99 · paraphrased: the licence does not allow quoting
Used Cepheid distances of NGC 3319 and NGC 3198 updated from this paper.

A measurement of the Hubble constant from Type II supernovae (2020) · 0.95 · paraphrased: the licence does not allow quoting
Used this paper's Key Project distances among the CPLR sample of 76 galaxies.

Cosmicflows-4 (2022) · 0.98 · paraphrased: the licence does not allow quoting

How the literature uses it

115 arXiv papers cite this in 144 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers whose main result relates to this one's

Found among the papers closest to this one by title and main claim. Pith's classifier compared each pair's main results and a second model family confirmed the relation; checked against two further families, shown conflicts agreed 118 times in 120 and shown same results 218 times in 239. The quoted sentence is the other paper's main claim.

States the same result 1 paper

The result was H_0 = 72 +/- 8 km/sec/Mpc and put an end to galaxy distances uncertain by a factor of two.

Measuring the Hubble Constant with the Hubble Space Telescope · 1.00

Papers citing it · 48 sentences without a confident label

Uses its method or tool 1 paper

We define the virial radius $R_vir$ as being the radius within which the average density is bigger than the average cosmological density by a factor $Δ$, called virial overdensity, for which we have adopted here the fitting form of Bryan and Norman [ref] [equation] leading to the relationship [equation] where we have assumed a Hubble constant of 72 km s$^-1$Mpc$^-1$ [ref] , and $Ω_m=0.3$.

Compact Stars as Dark Matter Probes · White dwarfs in globular clusters · 0.81

Uses its data or values 71 papers

In this section, we constrain the parameters in the axion model with the assumption of a flat Universe by using the latest observational data including the Type 1a Supernovae Union2 compilation [ref] , the Baryon Acoustic Oscillation [ref] measurement from the SDSS [ref] , the Cosmic Microwave background measurement given by WMAP [ref] observations and the H(z) data from HST key Project [ref] .

Observational Constraints on Axions as Quintessence in String Theory · Observational Constraint On Model Parameters · 1.00
We used the superovae data from Kowalski et al. [ref] to obtain the observational trend of $d_L(z)$ and we considered $H(z)$ values obtained by Simon, Verde and Jimenez [ref] and a prior on the Hubble parameter $H_0=0.72±0.08$ derived from measurements from the Hubble Space Telescope (HST, [ref] ), Finally, we used the value of $A$ from Eisenstein et al. [ref] .

Cosmological constraints on the Hu-Sawicki modified gravity scenario · Method · 1.00
Again, by utilizing Cepheid variables and SNe Ia from the Hubble Space Telescope (HST) project, the present day value of expansion rate stood at $74.03 ±1.42$km/s/Mpc [ref] .

Analysing Hubble Tension and Gravitational Waves for $f(Q,T)$ Gravity Theories · Introduction · 0.99

Compares with it 5 papers

[ref], [ref] and [ref] for the observable Hubble constant are all consistent with the low redshift measurements of the expansion rate that should specifically probe the observable Hubble constant; the value $H_0 = 66 kms^-1Mpc^-1$ sits firmly within the limits of the final results from the Hubble Key Project: $H_0 = 72 ±8 kms^-1Mpc^-1$ [ref] or $H_0 = 62.3 ±5.2 kms^-1Mpc^-1$ [ref] .

Dark energy as a mirage · The Hubble Key Project · 0.96
This value is consistent with that obtained from Cepheid measurements by Huterer et al. [ref] , but $9±13$% larger than the more commonly cited value of Freedman et al. [ref] , (see [ref] for a fuller discussion).

Radio Imaging of SN 1993J: The Story Continues · Introduction · 0.98
This result is consistent with the 3 year WMAP dataset result $H_0=73±3 km s^-1 Mpc^-1$ [ref] and with the Hubble Space Telescope key project result $H_0=73±8 km s^-1 Mpc^-1$ [ref] .

Cosmological constraints combining H(z), CMB shift and SNIa observational data · Hubble parameter observations · 0.87

Cites it as background 6 papers

The distance ladder approach [ref] in cosmology is a methodical technique used to determine cosmological distances across the universe, spanning from nearby stars to distant galaxies.

Hubble Tension or Distance Ladder Crisis? · Distance Ladder Approaches · 0.88
On the other hand, if one includes a cosmological constant [ref] , even the small one which is seemingly present in our universe [ref] , the presence of a cosmological horizon changes the late-time decay to one which is exponentially damped [ref] , replacing the branch cut with a discrete set of non-oscillatory, purely damped modes.

Pseudospectrum of de Sitter black holes · Introduction · 0.89
However, Type Ia SNe require independent calibration to anchor the distance ladder, relying on geometry [ref] and extensions to larger distances with empirical relations in Cepheid variables [ref] and the tip of the red giant branch [ref] , or with other methods [ref] .

Expanding Ejecta Method: I. Mapping Supernova Morphology with Intensity Interferometry · Introduction · 0.84

Discussion

Disagree with the review, or know something it missed? Leave a comment, highlight any passage above to comment on it, or challenge this review formally.

[1] [1]

Aaronson, M., Mould, J. R. & Huchra, J. 1979, ApJ, 229, 1 Aaronson, M., et al. 1982, ApJS, 50, 241 Aaronson, M., & Mould, J. R. 1986, ApJ, 303, 1 Aaronson, M., Bothun, G.D., Mould, J.R., Huchra, J., Schomm er, R.A., & Cornell, M.E. 1986, ApJ, 302, 536 Alibert, Y., Baraﬀe, I., Hauschildt, P. and Allard, F. 1999, A&A, 344, 551 Bahcall, N.A., & Fan, X. 1998,...

View on Pith Pith review arXiv 2000

[2] [2]

List of Cepheid Galaxies / Calibrators Galaxy Secondary Methods Calibrated by a Given Galaxy NGC 224 TF, SBF NGC 300 . . . NGC 598 TF NGC 925 TF NGC 1326A FP-Fornax 1 NGC 1365 TF, FP-Fornax NGC 1425 TF, FP-Fornax NGC 2090 TF NGC 2403 TF NGC 2541 TF NGC 3031 TF, SBF NGC 3198 TF NGC 3319 TF NGC 3351 TF, FP-Leo 1 NGC 3368 TF, FP-Leo, SBF, SNIa (1998bu) NGC 3...

View on Pith 2000

[3] [3]

Numbers of Cepheid Calibrators for Secondary Metho ds Secondary Method σ N (pre–HST) σmean N (post–HST) σmean % % % Tully-Fisher relation ±20% a 5 b ±10% 21 ±5% Type Ia supernovae ±8% c 0 n/a 6 d ±4% Surface brightness ﬂuctuations ±9% e 1 ±9% 6 ±4% Fundamental plane ±14% 0 n/a 3 f ±10% Type II supernovae ±12% g 1 ±12% 4 ±6% a Giovanelli et al. (1997) b M3...

View on Pith 1997

[4] [5]

Local Velocity Flow Galaxy VHelio VLG VCM B VV irgo VGA VShapley VT onry NGC 0300 144 125 -57 114 92 133 -140 NGC 0925 553 781 398 778 561 664 374 NGC 1326A 1836 1749 1787 1698 1742 1794 1164 NGC 1365 1636 1544 1597 1503 1544 1594 1157 NGC 1425 1512 1440 1477 1403 1417 1473 1465 NGC 2403 131 300 216 343 222 278 193 NGC 2541 559 646 736 744 674 714 936 NGC...

View on Pith 2024

[5] [6]

Revised Cepheid Distances to Galaxies . . . Galaxy µ aold σ Nceph µ brevised σ µ cP cut σ Ncutceph Data Source NGC 224 d 24.41 0.08 37 24.38 0.05 24.38 0.05 37 Freedman & Madore (1990 ) NGC 300 d 26.62 0.10 16 26.53 0.07 26.53 0.07 14 Freedman et al. (1992) NGC 598 d 24.58 0.10 12 24.56 0.10 24.56 0.08 11 Freedman et al. (1991) NGC 925 29.94 0.04 73 29.80...

View on Pith 1992

[6] [8]

NGC 4321 30.93 0.07 52 30.75 0.07 30.78 0.07 42 Ferrarese et al . (1996) NGC 4414 31.37 0.09 9 31.18 0.09 31.10 0.05 8 Turner et al. (199

View on Pith 1996

[7] [9]

f IC 1613 24.29 0.14 10 24.24 0.14 24.19 0.15 9 Freedman (1988) f aAdopting Madore & Freedman (1991) PL slopes; LMC distance mo dulus 18.50; ALLFRAME intensity- weighted mean magnitudes or Stetson template ﬁts if availab le; Hill et al. (1998) calibration, except for M31 (NGC 224), M33 (NGC 598), IC 1613, NGC 300, NGC 2403, M81 (NGC 3 031), M101 (outer; NGC

View on Pith 1988

[8] [12]

Uncertainties in H 0 for Secondary Methods Method H 0 Error (%) References 36 Type Ia supernovae 71 ±2r ±6s Hamuy et al. (1996), Riess et al. (1998), 4,000 < cz < 30,000 km/sec Jha et al. (1999), Gibson et al. (2000) 21 Tully–Fisher clusters 71 ±3r ±7s Giovanelli et al. (1997), Aaronson et al. (1982, 1986), 1,000 < cz < 9,000 km/sec Sakai et al. (2000) 11...

View on Pith 1996

[9] [13]

LMC Distance Moduli for Diﬀerent Methods Method < µ 0 > (mag) a σ (mag) N < µ 0 >(mag) b σ (mag) N Cepheids 18.57 ±0.14 5 18.52 ±0.13 15 Eclipsing variables 18.33 ±0.05 3 . . . . . . . . . SN1987A 18.47 ±0.08 4 18.50 ±0.12 5 TRGB 18.64 ±0.05 2 18.42 ±0.15 1 Red Clump 18.27 ±0.11 10 . . . . . . . . . RR Lyrae variables 18.30 ±0.13 7 18.40 ±0.19 14 Mira var...

View on Pith 2000

[10] [30]

86 14.86 8.77 NGC 4535 31.32 0.04 31.13 0.04 0.19 0.02 30.85 0.05 14.79 30.9 9 15.78 9.20 NGC 4536 31.24 0.04 31.06 0.04 0.18 0.02 30.80 0.04 14.45 30.8 7 14.93 8.85 NGC 4548 31.30 0.07 31.12 0.04 0.18 0.04 30.88 0.05 15.00 31.0 5 16.22 9.34 NGC 4639 31.96 0.09 31.84 0.07 0.12 0.04 31.61 0.08 20.99 31.7 1 21.98 9.00 NGC 4725 31.08 0.08 30.79 0.07 0.29 0.0...

View on Pith 1996

[11] [31]

04 16.14 8.50 NGC 1365 31.69 0.05 31.49 0.04 0.20 0.02 31.18 0.05 17.22 31.2 7 17.95 8.96 NGC 1425 32.01 0.07 31.85 0.05 0.16 0.03 31.60 0.05 20.89 31.7 0 21.88 9.00 NGC 2090 30.71 0.05 30.54 0.04 0.17 0.02 30.29 0.04 11.43 30.3 5 11.75 8.80 NGC 2403 . . . . . . 27.75 0.10 0.2 c 0.1 27.48 0.10 3.13 27.54 3.22 8.80 NGC 2541 30.74 0.05 30.54 0.04 0.20 0.02 ...

View on Pith

[12] [998]

NGC 2403 e 27.59 0.24 10 27.48 0.24 27.48 0.24 10 Freedman & Madore (1988 ) NGC 2541 30.43 0.07 34 30.26 0.07 30.25 0.05 29 Ferrarese et al . (1998) NGC 3031 27.75 0.07 25 27.67 0.07 27.75 0.08 17 Freedman et al. (1994) NGC 3198 30.80 0.08 42 30.64 0.08 30.68 0.08 36 Kelson et al. (1

View on Pith 1998

[13] [1990]

c Hamuy et al. (1996) d Using the distances to the host galaxies to SN 1960F, 1972E, 1 981B, 1989B, 1990N, 1998bu; but excluding 1895B, 1937C, 1974G e Tonry et al. (1997) f calibration based on Cepheid distances to Leo I group, Virgo and Fornax clusters gthis paper, Schmidt et al. (1994) distant clusters – 58 – Table

View on Pith 1996

[14] [1999]

Type Ia supernova sa mples. Left Panel : The full sample of 50 supernovae, with peak magnitudes correcte d only for foreground Galactic reddening. All tabulated heliocentric velocities have bee n corrected to the cosmic microwave background reference frame using the velocity calculator a vailable in the NASA Extragalactic Database (NED). Middle Panel : Ou...

View on Pith 1989

[15] [5457]

bAdopting Udalski et al. (1999) PL slopes; same Cepheid sampl e as for column 2; Stetson (1998) WFPC2 calibration, except for for M31, M33, IC 1613, NGC 300, NGC 24 03, M81. (To transform distance moduli from Hill et al. to Stetson, 0.07 mag is subtracted.) cSame calibration as for column 5, but applying a period cut at the short period end to minimize bi...

View on Pith 1999