Milky Way rotation and the distance to the galactic center from Cepheid variables

Caldwell, J. A. R.; Coulson, I. M.

doi:10.1086/114393

Cited by 85 publications

(71 citation statements)

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“…Table 1 gives the CC and PLC relations used in the present paper, as obtained from fundamental pulsating models with the labeled metal content. Since empirical studies adopt different methods of averaging observed magnitudes and colors over the full pulsation cycle, the 1 To the intensity mean BV magnitudes we added the Imagnitudes as derived from < V > − < I > − (V − I) = −0.03 mag, where the magnitude-averaged (V − I) colors are by Caldwell & Coulson (1987). For details see Caputo et al (2000).…”

Section: The Adopted Bv I Methodsmentioning

confidence: 99%

Pulsational constraints to the metallicity gradient in the Galactic disk

Caputo

Marconi

Musella

et al. 2001

A&A

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Abstract. BVI data of Galactic Cepheids observed in the solar neighborhood and in the outer disk are analyzed on the basis of nonlinear, non-local and time-dependent convective pulsating models computed for different assumptions on the chemical composition. We show that the theoretical color-color, period-luminosity, and period-luminosity-color relations, as predicted by the models with varying metal content, provide the way to simultaneously estimate the true distance modulus µ0 and the metal content Z of each individual variable. On this basis, we estimate that the metallicity distribution of Cepheids with Galactocentric distances d from ∼6 to ∼19 kpc can be represented by a linear gradient of −0.05 ± 0.01 dex kpc −1 , which is close to previous empirical determinations based on Cepheids, Planetary Nebulae and HII regions. However, our results are not excluding a different scenario, such as a two-zone model with a discontinuity in metallicity near d = 10 kpc (see Twarog et al. 1997).

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Section: The Adopted Bv I Methodsmentioning

confidence: 99%

Pulsational constraints to the metallicity gradient in the Galactic disk

Caputo

Marconi

Musella

et al. 2001

A&A

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“…First the distance modulus for YZ Car V 0 -M v is computed (top row of Table lb). (V) and (B) are taken from Caldwell and Coulson ( 1987). M v for the Cepheid is computed from the period-luminosity color relation from Feast and Walker (1987).…”

Section: Iue Spectramentioning

confidence: 99%

The companion of the 18-day classical Cepheid YZ Carinae

Evans¹,

Butler²

1993

PASP

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ABSTRACT. We have obtained a deep IUE spectrum of the 18-day Cepheid YZ Carinae. Flux has been detected at the level of 1-2 X 10" 15 ergs cm -2 Â -1 s -1 from 1200 to 2000 Â, which we identify as the companion in the binary system. Since this is at least partly a result of "camera artifacts" built up during a long exposure, this is an upper limit to the flux of the companion. The contribution of camera artifacts to the spectrum is discussed. Both la) are consistent with a B8 V to A0 V star.

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“…by Cardelli et al 1989;Caldwell & Coulson 1987;Laney & Stobie 1994) and E B−V is the B − V color excess (difference between the observed and the intrinsic B − V ). Similarly, the I-band magnitude can be corrected through the relation:…”

Section: The Methods Of Calculationmentioning

confidence: 99%

Calibration of the distance scale from galactic Cepheids

Paturel

Teerikorpi

Theureau³

et al. 2002

A&A

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Abstract. New estimates of the distances of 36 nearby galaxies is presented. These are based on the calibration of the V -and I-band Period-Luminosity relations for galactic Cepheids measured by the HIPPARCOS mission. The distance moduli are obtained in a classical way. The statistical bias due to the incompleteness of the sample is corrected according to the precepts introduced by Teerikorpi (1987). We adopt a constant slope (the one obtained with LMC Cepheids). The correction for incompleteness bias introduces an uncertainty that depends on each galaxy. On average, this uncertainty is small (0.04 mag) but it may reach 0.3 mag. We show that the uncertainty due to the correction of the extinction is small (propably less than 0.05 mag). The correlation between the metallicity and the morphological type of the host galaxy suggests that we should reduce the application to spiral galaxies in order to bypass the problem of metallicity. We suspect that the adopted PL slopes are not valid for all morphological types of galaxies. This may induce a mean systematic shift of 0.1 mag on distance moduli. A comparison with the distance moduli recently published by Freedman et al. (2001) shows there is a reasonably good agreement with our distance moduli.

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Milky Way rotation and the distance to the galactic center from Cepheid variables

Cited by 85 publications

References 0 publications

Pulsational constraints to the metallicity gradient in the Galactic disk

Pulsational constraints to the metallicity gradient in the Galactic disk

The companion of the 18-day classical Cepheid YZ Carinae

Calibration of the distance scale from galactic Cepheids

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