Colors and Magnitudes for 45 Cepheids of the Northern Milky way.

Bahner, K.; Hiltner, W. A.; Kraft, Robert P.

doi:10.1086/190068

Cited by 22 publications

(13 citation statements)

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“…Lesyunina (1963) 34 695.747 −3129 0.240 1 pg Lesyunina (1963) 36 882.452 −2650 −0.042 3 pe Bahner et al (1962) 37 631.265 −2486 −0.009 3 pe Mitchell et al (1964) 49 981.675 0 −0.011 3 CCD Schmidt & Seth (1996) 49 990.720 221 0.008 3 pe Berdnikov et al (1997) The radial velocity data clearly indicate a spectroscopic companion (see Fig. 7): Joy's (1937) data are systematically less negative (but a single point) than the CORAVEL-measurements, the difference being significant, about 15 km s −1 .…”

Section: Ux Perseimentioning

confidence: 99%

New spectroscopic binaries among classical Cepheids. II.

Szabados

Pont

1998

Astron. Astrophys. Suppl. Ser.

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Section: Ux Perseimentioning

confidence: 99%

New spectroscopic binaries among classical Cepheids. II.

Szabados

Pont

1998

Astron. Astrophys. Suppl. Ser.

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“…The program, executed at the 36-inch and 82-inch Cassegrain foci over 1.5 years, proved successful and provided estimates of reddening for more than 38 Cepheids (Kraft 1961). Central to the project were the light and color curves of Bahner, Hiltner & Kraft (1962) and the excellent new photometry of M25 and U Sgr by Joe Wampler and Al Hiltner (Wampler et al 1961). The derived intrinsic color versus spectral-type relation for supergiants, based on G-band strengths, generally agreed with that derived by Kron & Svolopoulos (1959) based on the intrinsic colors of nearby virtually unreddened supergiants.…”

Section: Indiana University and Yerkes Observatorymentioning

confidence: 99%

An Astronomical Life Salted by Pure Chance

Kraft

2009

Annu. Rev. Astron. Astrophys.

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My childhood upbringing in no way suggested that I would become an astronomer, but accidents of fate pushed me in the direction of science, and I have benefited greatly from being in the right place at the right time. I grew up in Seattle, earned B.S. and M.S. degrees in mathematics at the University of Washington, and eventually a Ph.D. in astronomy from the University of California, Berkeley. I was a postdoc at the Mt. Wilson Observatory, an assistant professor at Indiana University, later the Yerkes Observatory (University of Chicago), and still later I became a staff member of the Mt. Wilson and Palomar Observatories. After several years, I returned to the University of California, this time with the Lick Observatory staff at its new academic home on the Santa Cruz campus, where I have been ever since. My research has focused on the relation of Cepheids and RR Lyrae stars to problems of Galactic structure, the binary nature of cataclysmic variables, the decay of angular momentum of solar type stars, and the chemical history of the Galaxy as revealed by the abundances of very old stars in globular clusters and the Galactic halo field. None of this work would have been possible without the help of excellent teachers and mentors, great colleagues, and superb postdocs and graduate students. Most of all, I am grateful for the educational opportunities afforded me by state-supported public Universities.

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“…Quantities in columns 4-16 are excesses relative to the results of this paper to the nearest hundredth of a magnitude in E(b-y); a plus sign indicates a greater excess than that obtained herein. * Corrected and/or transformed E(B-V) data as given by Fernie (1967), multiplied by 0.7 a Transformed by E(b-y) = 0.7 E(B-V) b Transformed by E(b-y) = (0.7/1.89) E(G-I) c McNamara and Potter (1969) found 0.052 for 6 Cep and 0.154 for n Aql d Bahner, Hiltner and Kraft (1962) …”

Section: Color Excesses Of Cepheidsmentioning

confidence: 99%

Color excesses of classical cepheids. I

Feltz

McNamara

1976

PASP

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The color excesses of eleven cepheids have been determined with the aid of photometry of field stars found in the proximity of the variables. A comparison of the color excesses with previous color-excess results is given. Four cepheids: RT Aur, DT Cyg, £ Gem, and T Vul, have relatively small and wellestablished reddening values. These four stars, along with a UMi, can serve as standards to calibrate reddening-free indices with intrinsic color indices such as (b-y)o or (B-V)o-

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Colors and Magnitudes for 45 Cepheids of the Northern Milky way.

Cited by 22 publications

References 0 publications

New spectroscopic binaries among classical Cepheids. II.

New spectroscopic binaries among classical Cepheids. II.

An Astronomical Life Salted by Pure Chance

Color excesses of classical cepheids. I

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