Cepheid parallaxes and the Hubble constant

By F. V. Leeuwen, M. Feast, P. Whitelock, C. D. Laney. 2007

175 citations recorded by the source corpus.

Revised Hipparcos parallaxes for classical Cepheids are analysed together with 10 Hubble Space Telescope (HST)-based parallaxes. In a reddening-free V, I relation we find that the coefficient of log P is the same within the uncertainties in our Galaxy as in the Large Magellanic Cloud (LMC), contrary to some previous suggestions. Cepheids in the inner region of NGC 4258 with near solar metallicities confirm this result. We obtain a zero-point for the reddening-free relation and apply it to the Cepheids in galaxies used by Sandage et al. to calibrate the absolute magnitudes of Type Ia supernova (SNIa) and to derive the Hubble constant. We revise their result for H0 from 62 to 70 ± 5k m s −1 Mpc −1 . The Freedman et al. value is revised from 72 to 76 ± 8k m s −1 Mpc −1 . These results are insensitive to Cepheid metallicity corrections. The Cepheids in the inner region of NGC 4258 yield a modulus of 29.22 ± 0.03 (int.) compared with a maser-based modulus of 29.29 ± 0.15. Distance moduli for the LMC, uncorrected for any metallicity effects, are 18.52 ± 0.03 from a reddening-free relation in V, I; 18.47 ± 0.03 from a period‐luminosity relation at K; 18.45 ± 0.04 from a period‐luminosity‐ colour relation in J, K. Adopting a metallicity correction in V, I from Macri et al. leads to a true LMC modulus of 18.39 ± 0.05.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/8e5e3b4f2d21c5652ccf055fd2372271661e3865

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. A. Riess
2. F. V. D. Bosch
3. H. Mo
4. Xiaohu Yang
5. S. More
6. C. Conroy
7. L. Hernquist
8. Risa Wechsler

In Instrumentation

1. F. V. D. Bosch
2. H. Mo
3. Xiaohu Yang
4. S. More
5. A. Riess
6. M. Cacciato
7. C. Conroy
8. Risa Wechsler

Citations in the corpus

• A New Calibration Of Galactic Cepheid Period-Luminosity Relations From B To K Bands, And A Comparison To LMC Relations (2007, methodology): “We use two sources of trigonometric parallaxes: HST parallaxes, published by Benedict et al. (2002) and Benedict et al. (2007), and the revised Hipparcos parallaxes of Cepheids, from van Leeuwen et al. (2007).”
• H 0 revisited (2013, methodology): “I use the sample of 13 MW Cepheids with parallax measurements and photometry as listed in van Leeuwen et al. (2007) (eliminating Polaris).”
• Observational probes of cosmic acceleration (2012, methodology): “…this analysis is a shift to Cepheid calibration based on the maser distances to NGC 4258 (Herrnstein et al., 1999; Humphreys et al., 2008, 2013) and on parallaxes to Galactic Cepheids measured with Hipparcos (van Leeuwen et al., 2007) and with the HST fine-guidance sensors (Benedict et al., 2007).”
• A 3% SOLUTION: DETERMINATION OF THE HUBBLE CONSTANT WITH THE HUBBLE SPACE TELESCOPE AND WIDE FIELD CAMERA 3 (2011, methodology): “…in precision beyond the first rung in the previous section suggests greater value in their use to enhance the calibration of the first rung. van Leeuwen et al. (2007) reanalyzed Hipparcos observations and determined independent parallax measurements for the same 10 Cepheids (albeit with half…”
• A REDETERMINATION OF THE HUBBLE CONSTANT WITH THE HUBBLE SPACE TELESCOPE FROM A DIFFERENTIAL DISTANCE LADDER (2009, methodology): “…Cepheids based on the Baade-Wesselink method or stellar associations as they are much more uncertain than well-measured parallaxes, and the former appear to be under refinement due to uncertainties in their projection factors, as discussed by Fouqué et al. (2007) and van Leeuwen et al. (2007).”
• Clustering of luminous red galaxies – IV. Baryon acoustic peak in the line-of-sight direction and a direct measurement of H(z) (2008, methodology): “In Fig.20 we compare our estimates with H0 = 70±5 km/s/Mpc from HST van Leeuwen et al. (2007) at z ≃ 0.03 and with the H(z) inferred from WMAP5 modeling with H0 = 71.9±2.6 km/s/Mpc and Ωm = 0.258±0.030 for a flat universe LCDM (w=-1) Komatsu et al. (2008).”
• THE SOLAR NEIGHBORHOOD. XXXVII. THE MASS–LUMINOSITY RELATION FOR MAIN-SEQUENCE M DWARFS (2016, methodology): “…the orbital motions of the binaries, are usually marked improvements — typically by factors of 5–10 over available parallaxes in the Yale Parallax Catalog (van Altena, Lee & Hoffleit 1995, hereafter YPC) and Hipparcos (van Leeuwen et al. 2007) — and are key in deriving the high-accuracy masses.”
• New Parallaxes of Galactic Cepheids from Spatially Scanning the Hubble Space Telescope: Implications for the Hubble Constant (2018, methodology): “This is a factor of 45 better than the ESA astrometric mission Hipparcos mean for all P>10 day MW Cepheids (σ= 1.4 mas; van Leeuwen et al. 2007), and an order of magnitude better than typically possible with the FGS on HST or from staring mode observations with WFC3.”
• DIRECT DETECTION OF THE CLOSE COMPANION OF POLARIS WITH THE HUBBLE SPACE TELESCOPE (2005, methodology): “Using the recently revised Hipparcos parallax of 7.72 ± 0.12 mas (van Leeuwen et al. 2007), we computed the total mass of the binary through Kepler’s Third Law for all of the solutions found in the Monte Carlo search.”
• Milky Way Cepheid Standards for Measuring Cosmic Distances and Application to Gaia DR2: Implications for the Hubble Constant (2018, methodology): “There are compilations of ground-based Cepheid photometry that could augment the HST sample by an additional ∼150–250 Cepheids, for example from van Leeuwen et al. (2007).”
• Hubble Space Telescope Trigonometric Parallax of Polaris B, Companion of the Nearest Cepheid (2017, background): “Because it is so nearby, Polaris can potentially serve as one of the anchor points near the shortperiod end for zero-point calibration of the Leavitt period– luminosity relation (e.g., Feast & Catchpole 1997; van Leeuwen et al. 2007).”
• Clarifying the Hubble constant tension with a Bayesian hierarchical model of the local distance ladder (2017, methodology): “…analysis: the absolute distance to NGC 4258 inferred from MASER measurements by Humphreys et al. (2013); parallaxes of 15 Milky Way Cepheids (van Leeuwen et al. 2007; Riess et al. 2014; Casertano et al. 2016); and the absolute distance to the LMC, derived from detached eclipsing binary…”
• EVOLUTION, NUCLEOSYNTHESIS, AND YIELDS OF LOW-MASS ASYMPTOTIC GIANT BRANCH STARS AT DIFFERENT METALLICITIES (2009, methodology): “Firstly, thanks to the use of Hipparcos parallaxes recently revised (van Leeuwen et al. 2007) and of IR data from the ISO and MSX missions or, secondly, from the period-Luminosity relation for Mira C-rich sources published in Whitelock et al. (2006) (see Guandalini et al. 2006 and Guandalini &…”
• A 2.4% DETERMINATION OF THE LOCAL VALUE OF THE HUBBLE CONSTANT (2016, methodology): “As in R11, we use the compilation from van Leeuwen et al. (2007), who combined 10 Cepheid parallax measurements with HST/FGS from Benedict et al. (2007) with those measured at lower precision with Hipparcos, plus another three measured only with significance by Hipparcos.”
• AGB variables and the Mira period–luminosity relation (2008, methodology): “The distance modulus of the LMC is taken to be (m − M)LMC = 18.39 ± 0.05 (van Leeuwen et al. 2007) Table 2 lists the values of the slope and zero-point found by least squares fitting separately to the O-rich stars and to the C-rich stars as well as to both groups together; σ is the standard…”
• Inclination- and dust-corrected galaxy parameters: bulge-to-disc ratios and size–luminosity relations (2008, result): “This Hubble constant is also the value reported in (Blakeslee et al. 2002) and is the halfway point between the two values reported in van Leeuwen et al. (2007).”