Color Excesses on a Uniform Scale for 328 Cepheids

Fernie, J. D.

doi:10.1086/191412

Cited by 53 publications

(68 citation statements)

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“…5 Following the recommendation at that site, we chose the values in column FE1 that are the EðB À V Þ clus values of Fernie (1990). These reddenings are listed in Table 1.…”

Section: Interstellar Reddeningmentioning

confidence: 99%

A Bayesian Analysis of the Cepheid Distance Scale

Barnes¹,

Jefferys

Berger

et al. 2003

ApJ

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We develop and describe a Bayesian statistical analysis to solve the surface brightness equations for Cepheid distances and stellar properties. Our analysis provides a mathematically rigorous and objective solution to the problem, including immunity from Lutz-Kelker bias. We discuss the choice of priors, show the construction of the likelihood distribution, and give sampling algorithms in a Markov chain Monte Carlo approach for efficiently and completely sampling the posterior probability distribution. Our analysis averages over the probabilities associated with several models rather than attempting to pick the '' best model '' from several possible models. Using a sample of 13 Cepheids we demonstrate the method. We discuss diagnostics of the analysis and the effects of the astrophysical choices going into the model. We show that we can objectively model the order of Fourier polynomial fits to the light and velocity data. By comparison with theoretical models of Bono et al. we find that EU Tau and SZ Tau are overtone pulsators, most likely without convective overshoot. The period-radius and period-luminosity relations we obtain are shown to be compatible with those in the recent literature. Specifically, we find logð R h iÞ ¼ ð0:693 AE 0:037Þ logðPÞ À 1:2 ½ þ ð2:042 AE 0:047Þ and M v h i ¼ Àð2:690 AE 0:169Þ logðPÞ À 1:2 ½ À ð 4:699 AE 0:216Þ.

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“…5 Following the recommendation at that site, we chose the values in column FE1 that are the EðB À V Þ clus values of Fernie (1990). These reddenings are listed in Table 1.…”

Section: Interstellar Reddeningmentioning

confidence: 99%

A Bayesian Analysis of the Cepheid Distance Scale

Barnes¹,

Jefferys

Berger

et al. 2003

ApJ

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“…(It is to be noted that this system differs substantially from the Johnson I photometric system, Sandage 1997.) The Cepheids listed in Table 1 have been selected such that they also have E(B − V) color excesses from Fernie (1990), as updated by Fernie et al (1995).…”

Section: The Basic Datamentioning

confidence: 99%

New Period-Luminosity and Period-Color relations of classical Cepheids: I. Cepheids in the Galaxy

Tammann

Sandage

Reindl

2003

A&A

229

262

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Abstract. 321 Galactic fundamental-mode Cepheids with good B, V, and (in most cases) I photometry by Berdnikov et al. (2000) and with homogenized color excesses E(B − V) based on Fernie et al. (1995) are used to determine their period-color (P-C) relation in the range 0.4 < log P < ∼ 1.6. The agreement with colors from different model calculations is good to poor. 0 . Also the (B − V) 0 , (V − I) 0 twocolor diagrams differ between Cepheids in the Galaxy and the Clouds, attributed both to the effects of metallicity differences on the spectral energy distributions of the Cepheids and to a shift in the effective temperature of the middle of the instability strip for LMC and SMC relative to the Galaxy by about ∆ log T e ∼ 0.02 at M V = −4. m 0, hotter for both LMC and SMC. Differences in the period-color relations between the Galaxy and the Clouds show that there cannot be a universal P-L relation from galaxy-to-galaxy in any given color. The inferred non-uniqueness of the slope of the P-L relations in the Galaxy, LMC, and SMC is born out by the observations. The Cloud Cepheids follow a shallower overall slope of the P-L relations in B, V, and I than the Galactic ones. LMC and SMC Cepheids are brighter in V than in the Galaxy by up to 0. m 5 at short periods (log P = 0.4) and fainter at long periods (log P > ∼ 1.4). The latter effect is enhanced by a suggestive break of the P-L relation of LMC and SMC at log P = 1.0 towards still shallower values as shown in a forthcoming paper.

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“…Using the temperature scale from Kiss & Szàtmary (1998), with B − V photometry and the color excess from Fernie (1990), we derive T eff = 5500 K for phase 0.901. Together with the extrapolated VINCI LD angular diameter for this phase (θ LD 2.70 mas), we obtain the blackbody spectrum represented as a solid curve in Fig.…”

Section: Spectral Energy Distributionmentioning

confidence: 99%

“…This list is limited to Cepheids brighter than m V = 6.0 at maximum present in the catalogue assembled by Heiles (2000), apart from RS Pup. The color excess E(B − V) reported by Fernie (1990) is given for each star, and the p values larger than 1% are marked in bold characters. Bastien et al (1988). pulsating yellow supergiants having spectral types F-G at maximum visible light and K-M at minimum.…”

Section: The Rv Tauri Star Ac Hermentioning

confidence: 99%

Extended envelopes around Galactic Cepheids

Kervella¹,

Mérand²,

Perrin³

et al. 2006

A&A

106

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We present the results of long-baseline interferometric observations of the bright southern Cepheid Carinae in the infrared N (8−13 µm) and K (2.0−2.4 µm) bands, using the MIDI and VINCI instruments of the VLT Interferometer. We resolve in the N band a large circumstellar envelope (CSE) that we model with a Gaussian of 3 R (≈500 R ≈ 2−3 AU) half width at half maximum. The signature of this envelope is also detected in our K band data as a deviation from a single limb darkened disk visibility function. The superimposition of a Gaussian CSE on the limb darkened disk model of the Cepheid star results in a significantly better fit of our VINCI data. The extracted CSE parameters in the K band are a half width at half maximum of 2 R , comparable to the N band model, and a total brightness of 4% of the stellar photosphere. A possibility is that this CSE is linked to the relatively large mass loss rate of Car. Though its physical nature cannot be determined from our data, we discuss an analogy with the molecular envelopes of RV Tauri, red supergiants and Miras.

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Color Excesses on a Uniform Scale for 328 Cepheids

Cited by 53 publications

References 0 publications

A Bayesian Analysis of the Cepheid Distance Scale

A Bayesian Analysis of the Cepheid Distance Scale

New Period-Luminosity and Period-Color relations of classical Cepheids: I. Cepheids in the Galaxy

Extended envelopes around Galactic Cepheids

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