Electroanatomy of the thalamic ventro-oral nucleus based on stereotaxic stimulation in man

Schaltenbrand, Georg; Spuler, H.; Wahren, W; Rümler, B

doi:10.1007/bf00316765

Cited by 28 publications

(25 citation statements)

References 15 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…V Cen has been included as a possible cluster member in the color-magnitude diagram of Figure 3 by applying the space reddening obtained earlier to the data for V Cen published by Schaltenbrand and Tammann (1971). Its inferred luminosity as a cluster member, (M F ) = -3.24 ± 0.09 m.e., is typical of a 5?5 classical cepheid.…”

Section: Observations and Analysismentioning

confidence: 99%

On the possibility of cluster membership for the cepheid V Centauri

Turner

1982

PASP

View full text Add to dashboard Cite

UBV photometry is presented for ten stars lying within 5 arc min of the bright 5^5 cepheid V Cen. An analysis of these data and similar published data for members of the nearby cluster NGC 5662 leads to a newly-determined distance of 661 ± 24 pc for the cluster, and indicates that V Cen is an excellent candidate for membership in the cluster corona. In particular, the derived space reddening of E B _ X {OB) = 0.31 ± 0.01 for likely cluster coronal members near V Cen agrees with published values for the cepheid's photometric reddening, the derived ages for V Cen and cluster stars are both near 6 X 10 7 years, and the inferred luminosity of the cepheid as a cluster member, (M v ) = -3.24 ± 0.09, is consistent with predictions based upon the period-luminosity relation.

show abstract

Section: Observations and Analysismentioning

confidence: 99%

On the possibility of cluster membership for the cepheid V Centauri

Turner

1982

PASP

View full text Add to dashboard Cite

show abstract

“…What do they mean? Schaltenbrand & Tammann (1971) introduced Fourier series to describe the light curves of Galactic Cepheids simply as an objective way to derive many properties of the curves such as the amplitude, phase of maximum light, and fraction of the period between minimum and maximum light. They did not list the Fourier coefficients because these authors used them only as an intermediate step to derive accurate values of these observed parameters that are manifest from the observations.…”

Section: The Significance Of the Break At Log P =mentioning

confidence: 99%

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

Sandage

Tammann²,

Reindl³

2004

A&A

154

268

View full text Add to dashboard Cite

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.

show abstract

“…16) respectively. For these, we used the UBV data listed by Schaltenbrand & Tammann (1971). The extremes of variability are also indicated.…”

Section: Cluster Membership Of the Cepheid Variablesmentioning

confidence: 99%

Multicolour deep CCD photometric study of the moderately young southern open star clusters NGC 3228, NGC 4103, NGC 5662 and NGC 6087

Sagar

Cannon

1997

Astron. Astrophys. Suppl. Ser.

View full text Add to dashboard Cite

Abstract. CCD observations in the U , B, V , R and I passbands have been used to generate colourcolour and deep colour-magnitude diagrams for the young open star clusters NGC 3228, NGC 4103, NGC 5662 and NGC 6087. The sample consists of about 2000 stars reaching down to V = 20 mag. The interstellar extinction across the face of the imaged cluster regions seems to be uniform with average values of E(B − V ) = 0.31, 0.34 and 0.22 mag for NGC 4103, NGC 5662 and NGC 6087 respectively. The distances to the clusters NGC 3228, NGC 4103, NGC 5662 and NGC 6087 have been estimated as 0.5 ± 0.05, 2.0 ± 0.3, 0.8 ± 0.1 and 1.0 ± 0.1 kpc respectively, while the corresponding ages estimated from the theoretical stellar evolutionary isochrones fitted to the bright proper motion cluster members are ∼ 100, 30, 80 and 65 Myr respectively. Present data are consistent with the membership of the Cepheid variable V Cen to NGC 5662 and of S Norm to NGC 6087. Heavy contamination by foreground and background field stars has unfortunately made it impossible to reach definite conclusions about the faint luminosity function, and the data do not reach faint enough limits to investigate pre-main sequence stars.

show abstract

Electroanatomy of the thalamic ventro-oral nucleus based on stereotaxic stimulation in man

Cited by 28 publications

References 15 publications

On the possibility of cluster membership for the cepheid V Centauri

On the possibility of cluster membership for the cepheid V Centauri

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

Multicolour deep CCD photometric study of the moderately young southern open star clusters NGC 3228, NGC 4103, NGC 5662 and NGC 6087

Contact Info

Product

Resources

About