Spectroscopic binaries in the open cluster Trumpler 16

Levato, H.; Malaroda, S.; Morrell, N.; Garcia-Pinto, D.; Hernández, Carlos

doi:10.1086/191551

Cited by 37 publications

(51 citation statements)

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“…References Morgan et al 1943;(10) Mendoza 1956;(11) Morgan et al 1953;(12) Osawa 1959;(13) Cowley et al 1969;(14) Metreveli 1968;(15) Guetter 1968;(16) Boulon & Fehrenbach 1959;(17) Buscombe 1962;(18) Roman 1955;(19) Georgelin et al 1973;(20) Bouigue 1959;(21) Wenzel 1951;(22) Smith 1972;(23) Penston et al 1975;(24) Barbier & Boulon 1960;(37) Young 1978;(38) Claria 1974;(39) Feast et al 1955;(40) Moffat & Fitzgerald 1974;(41) Houk 1978;(42) Feast et al 1961;(43) Denoyelle 1977;(44) Hoffleit 1956;(45) Turner et al 1980;(46) Morrell et al 1988;(47) Massey & Johnson 1993;(48) Levato et al 1991;(49) Morris 1961;(50) Hiltner et al 1969;(51) Houk & Cowley 1975;(52) Seidensticker 1989;(53) Feast et al 1957;(54) Perry et al 1976;(55) Schild 1970;(56) Vrba & Rydgren 1984;(76) H...…”

Section: The Survey Stars and Their Dataunclassified

An Analysis of the Shapes of Interstellar Extinction Curves. V. The IR‐through‐UV Curve Morphology

Fitzpatrick

Massa

2007

ApJ

704

844

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We study the IR-through-UV wavelength dependence of 328 Galactic interstellar extinction curves affecting normal, near-main-sequence B and late O stars. We derive the curves using a new technique that employs stellar atmosphere models in lieu of unreddened ''standard'' stars. Under ideal conditions, this technique is capable of virtually eliminating spectral mismatch errors in the curves. In general, it lends itself to a quantitative assessment of the errors and enables a rigorous testing of the significance of relationships between various curve parameters, regardless of whether their uncertainties are correlated. Analysis of the curves gives the following results:1. In accord with our previous findings, the central position of the 2175 8 extinction bump is mildly variable, its width is highly variable, and the two variations are unrelated.2. Strong correlations are found among some extinction properties within the UV region, and within the IR region.3. With the exception of a few curves with extreme (i.e., large) values of R(V ), the UVand IR portions of Galactic extinction curves are not correlated with each other.4. The large sight lineYtoYsight line variation seen in our sample implies that any average Galactic extinction curve will always reflect the biases of its parent sample.5. The use of an average curve to deredden a spectral energy distribution (SED) will result in significant errors, and a realistic error budget for the dereddened SED must include the observed variance of Galactic curves.While the observed large sight lineYtoYsight line variations, and the lack of correlation among the various features of the curves, make it difficult to meaningfully characterize average extinction properties, they demonstrate that extinction curves respond sensitively to local conditions. Thus, each curve contains potentially unique information about the grains along its sight line.

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Section: The Survey Stars and Their Dataunclassified

An Analysis of the Shapes of Interstellar Extinction Curves. V. The IR‐through‐UV Curve Morphology

Fitzpatrick

Massa

2007

ApJ

704

844

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“…Buscombe & Kennedy (1969) report on one velocity measurement in their table containing "stars with variable velocities or incomplete observations," but no further information is given. Levato et al (1991) report on nine measurements that led them to conclude that the star has constant velocity within uncertainties. Their mean of −24.0 ± 1.1 km s −1 is lower than ours, which may be due to differences in the line sample.…”

Section: Cpd-26mentioning

confidence: 99%

Radial Velocities of Galactic O-Type Stars. I. Short-Term Constant Velocity Stars

Gies

Hillwig

McSwain

et al. 2011

The Astronomical Journal

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“…We use this period to rematch the misidentified radial velocities from Levato et al (1991) and apply them in an analysis using the method of Lehmann-Filhes. We find that CPD −59…”

Section: Abstract the Spectroscopic Binary Cpd −59mentioning

confidence: 99%

On the eclipsing nature of $\mathsf{CPD-59\degr2628}$

Freyhammer

Clausen²,

Arentoft³

et al. 2001

A&A

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Abstract. The spectroscopic binary CPD −59• 2628 (Sp = O9.5 V) has been discovered to be a detached eclipsing binary, and we present an analysis based on new light curves, published spectroscopy and two new high-resolution spectra. uvby light curves from more than 2000 observations are analysed with the WINK and the Wilson-Devinney (WD) programs. Geometric distortions and photometric effects from the proximity of the components are included in the computations. The detached system has a close circular orbit of high inclination and high maximum projected velocities. We find a photometric period P = 1.d 47 which is consistent with the spectroscopy-binary period by Solivella & Niemela (1999). We use this period to rematch the misidentified radial velocities from Levato et al. (1991) and apply them in an analysis using the method of Lehmann-Filhes. We find that CPD −59• 2628 is a young system close to the ZAMS. Its distance is 2.6 ± 0.1 kpc and it has a systemic velocity of −19 km s

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Spectroscopic binaries in the open cluster Trumpler 16

Cited by 37 publications

References 0 publications

An Analysis of the Shapes of Interstellar Extinction Curves. V. The IR‐through‐UV Curve Morphology

An Analysis of the Shapes of Interstellar Extinction Curves. V. The IR‐through‐UV Curve Morphology

Radial Velocities of Galactic O-Type Stars. I. Short-Term Constant Velocity Stars

On the eclipsing nature of $\mathsf{CPD-59\degr2628}$

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