Calibration of the distance scale from galactic Cepheids

Paturel, G.; Teerikorpi, P.; Theureau, G.; Fouqué, P.; Musella, I.; Terry, J. N.

doi:10.1051/0004-6361:20020492

Cited by 31 publications

(23 citation statements)

References 67 publications

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“…The importance of unbiased Cepheid samples has been pointed out by several authors (e.g. Sandage 1988;Paturel et al 2002). Small-amplitude (A B ≈ 0.…”

Section: Amplitude and The Position Within The Instability Stripmentioning

confidence: 93%

New period-luminosity and period-color relations of classical Cepheids

Sandage

Tammann²,

Reindl³

2004

A&A

154

268

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Abstract. Photometric data for 593 Cepheids in the LMC, measured by Udalski et al. in the OGLE survey, augmented by 97 longer period Cepheids from other sources, are analyzed for the period-color (P-C) and period-luminosity (P-L) relations, and for the variations of amplitude, light curve shape, and period across the instability strip at constant absolute magnitude. Both the P-C and P-L relations have different slopes for periods smaller and larger than 10 days. The break at 10 days is also seen in the period-amplitude relations, and the compound Fourier combinations of R 21 and Φ 21 introduced by Simon and Lee. The LMC Cepheids are bluer than Galactic Cepheids in the B, V, and I color bands, part of which is due to differential Fraunhofer line blanketing and part to real differences in the temperature boundaries of the instability strip. The LMC strip is hotter by between 80 K and 350 K depending on the period. Hence, both the slopes and (necessarily) the zero points of the P-L relations in B, V, and I must differ between LMC and the revised relations (also given here) for the Galaxy, and in fact they do. The LMC Cepheids are brighter by up to 0.5 mag at log P = 0.4 (2 days) and fainter by 0.2 mag at log P = 1.5 (32 days). These facts complicate the use of Cepheid as precision distance indicators until the reason is found (metallicity differences or other unknown differences) for the non-universality of the P-L and P-C relations. The very large data base permits mapping of various Cepheid properties at different positions within the instability strip, both at constant period and at constant absolute magnitude over the range of 2 < P < 40 days and −2 > M V > −5. Amplitude of the light curves are largest near the blue edge of the strip for periods between 2 and 7 days and longer than 15 days. The sense is reversed for periods between 7 and 15 days. The shape of the light curves varies systematically across the strip. Highly peaked curves (of large amplitude) that necessarily have large values of R 21 of about 0.5, occur near the blue edge of the strip. More symmetrical (small amplitude) light curves that have, thereby, small values of R 21 , generally occur near the red edge of the strip. Consequently, there is a strong correlation of R 21 with color within the strip at a given absolute magnitude. Strong correlations also exist between color and period, and color and amplitude at given absolute magnitudes, for the same reason that has long been known for RR Lyrae stars, based on the sloping lines of constant period in the CMD combined with the variation of amplitude, and now R 21 , with color. The highly peaked light-curve shapes and large amplitudes (indicating a non-linear regime that is overdriven out of the linear regime) near the blue edge of the strip, show that the energy driver for the pulsation (i.e. the negative dissipation) is strongest at the blue edge.

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“…The importance of unbiased Cepheid samples has been pointed out by several authors (e.g. Sandage 1988;Paturel et al 2002). Small-amplitude (A B ≈ 0.…”

Section: Amplitude and The Position Within The Instability Stripmentioning

confidence: 93%

New period-luminosity and period-color relations of classical Cepheids

Sandage

Tammann²,

Reindl³

2004

A&A

154

268

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“…Based on this premise, the analysis led several teams (including us) to almost concordant Cepheid distances (Freedman et al 2001;Saha et al 2001;Paturel et al 2002b). The Hubble constant finally derived by the HST Key Project was H 0 = 72 ± 8 km s −1 Mpc −1 .…”

Section: Introductionmentioning

confidence: 92%

“…We add to the HST sample the previous ground-based Cepheid observations (Paturel et al 2002b) (Fig. 6).…”

Section: Implications For the Local Hubble Constantmentioning

confidence: 99%

The extragalactic Cepheid bias: significant influence on the cosmic distance scale

Paturel

Teerikorpi

2005

A&A

Self Cite

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The unique measurements with the Hubble Space Telescope of Cepheid variable stars in nearby galaxies led to extragalactic distances that made the HST Key Project conclude that the Hubble constant is H 0 = 72 km s −1 Mpc −1 . The idea that H 0 is now known is widely spread among the astronomical community. Some time ago, we suggested that a strong selection effect may still exist in the Cepheid method, resulting in too short distances. Using a model similar to traditional bias corrections, we deduce here new estimates of distances from HST and previous ground-based observations which are both affected by this effect, showing the same trend which starts at different distances. The recent measurement of M 83 with the VLT is unbiased. Revisiting the calibration of HSTKP's with our new scale, makes long-range distance criteria more concordant and reduces the value of H 0 to ≈60 km s −1 Mpc −1 . Locally, the corrected Cepheid distances give H local = 56 km s −1 Mpc −1 and reduce the velocity dispersion in the Hubble flow. These numbers are indicative of the influence of the suggested Cepheid bias in the context of the HSTKP studies and are not final values.

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“…The host galaxy NGC 1367 was observed as part of the HST Cepheid Key Project, hence the most accurate and recent distance estimate is taken from Paturel et al (2002), μ= 31.31 ± 0.15. The extinction towards the SN was measured by three different methods by Smartt et al (2003) to be E ( B − V ) = 0.17 ± 0.09, giving A I = 0.25 ± 0.13, which is similar to that adopted ( A I ≃ 0.2) by Van Dyk et al (2003c).…”

Section: The Masses Of the Progenitors Of Type Ii‐p Supernovaementioning

confidence: 99%

The death of massive stars - I. Observational constraints on the progenitors of Type II-P supernovae

Smartt¹,

Eldridge²,

Crockett³

et al. 2009

Monthly Notices of the Royal Astronomical Society

718

1,114

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We present the results of a 10.5‐yr, volume‐limited (28‐Mpc) search for supernova (SN) progenitor stars. In doing so we compile all SNe discovered within this volume (132, of which 27 per cent are Type Ia) and determine the relative rates of each subtype from literature studies. The core‐collapse SNe break down into 59 per cent II‐P and 29 per cent Ib/c, with the remainder being IIb (5 per cent), IIn (4 per cent) and II‐L (3 per cent). There have been 20 II‐P SNe with high‐quality optical or near‐infrared pre‐explosion images that allow a meaningful search for the progenitor stars. In five cases they are clearly red supergiants, one case is unconstrained, two fall on compact coeval star clusters and the other twelve have no progenitor detected. We review and update all the available data for the host galaxies and SN environments (distance, metallicity and extinction) and determine masses and upper mass estimates for these 20 progenitor stars using the stars stellar evolutionary code and a single consistent homogeneous method. A maximum likelihood calculation suggests that the minimum stellar mass for a Type II‐P to form is mmin= 8.5+1−1.5 M⊙ and the maximum mass for II‐P progenitors is mmax= 16.5 ± 1.5 M⊙, assuming a Salpeter initial mass function holds for the progenitor population (in the range Γ=−1.35+0.3−0.7). The minimum mass is consistent with current estimates for the upper limit to white dwarf progenitor masses, but the maximum mass does not appear consistent with massive star populations in Local Group galaxies. Red supergiants in the Local Group have masses up to 25 M⊙ and the minimum mass to produce a Wolf–Rayet star in single star evolution (between solar and LMC metallicity) is similarly 25–30 M⊙. The reason we have not detected any high‐mass red supergiant progenitors above 17 M⊙ is unclear, but we estimate that it is statistically significant at 2.4σ confidence. Two simple reasons for this could be that we have systematically underestimated the progenitor masses due to dust extinction or that stars between 17–25 M⊙ produce other kinds of SNe which are not II‐P. We discuss these possibilities and find that neither provides a satisfactory solution. We term this discrepancy the ‘red supergiant problem’ and speculate that these stars could have core masses high enough to form black holes and SNe which are too faint to have been detected. We compare the 56Ni masses ejected in the SNe to the progenitor mass estimates and find that low‐luminosity SNe with low 56Ni production are most likely to arise from explosions of low‐mass progenitors near the mass threshold that can produce a core‐collapse.

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Calibration of the distance scale from galactic Cepheids

Cited by 31 publications

References 67 publications

New period-luminosity and period-color relations of classical Cepheids

New period-luminosity and period-color relations of classical Cepheids

The extragalactic Cepheid bias: significant influence on the cosmic distance scale

The death of massive stars - I. Observational constraints on the progenitors of Type II-P supernovae

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