UVBY and beta photometry for stars in the open cluster NGC 1502

Crawford, D. L.

doi:10.1086/133391

Cited by 18 publications

(40 citation statements)

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“…This is maybe caused due to the different ratios of A V to the absorptions of different bands in different directions, which contradicts the constant ratios assumed by the models, mentioned before. We calculated the medians of the A V values and their standard deviation and list them in Tables 3 and 4. While the median value of absorption of the unresolved binary SZ Cam is A V = 2.13 ± 0.04 mag from our calculations (and 2.16 ± 0.18 mag from B − V only), Crawford (1994) lists 2.32 mag from B − V . Lorenz, Mayer & Drechsel (1998) give a total visual magnitude of V = 6.92 mag for SZ Cam (6.910 ± 0.018 from own photometry) and www.an-journal.org Table 5 Spectral types as listed in Simbad (for second line from Lorenz, Mayer & Drechsel 1998) and masses for NGC 1502.…”

Section: Magnitudes Colours Absorptions and Spectral Typescontrasting

confidence: 59%

Photometric study of the OB star clusters NGC 1502 and NGC 2169 and mass estimation of their members at the University Observatory Jena

Hohle

Eisenbeiss²,

Mugrauer³

et al. 2009

Astron Nachr

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In this work we present detailed photometric results of the trapezium like galactic nearby OB clusters NGC 1502 and NGC 2169 carried out at the University Observatory Jena. We determined absolute BVRI magnitudes of the mostly resolved components using Landolt standard stars. This multi colour photometry enables us to estimate spectral type and absorption as well as the masses of the components, which were not available for most of the cluster members in the literature so far, using models of stellar evolution. Furthermore, we investigated the optical spectrum of the components ADS 2984A and SZ Cam of the sextuple system in NGC 1502. Our spectra clearly confirm the multiplicity of these components, which is the first investigation of this kind at the University Observatory Jena.

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Section: Magnitudes Colours Absorptions and Spectral Typescontrasting

confidence: 59%

Photometric study of the OB star clusters NGC 1502 and NGC 2169 and mass estimation of their members at the University Observatory Jena

Hohle

Eisenbeiss²,

Mugrauer³

et al. 2009

Astron Nachr

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“…For reasons of homogeneity in the colour transformations, the majority of the adopted standard Strömgren indices were taken from the work of a single group of researchers. The standard stars were chosen from the papers on NGC 1502 (Crawford 1994), IC 4665 , NGC 2169 (Perry et al 1972), NGC 6910 and NGC 6913 (Crawford et al 1977), O-type stars (Crawford 1975), h and χ Per , Cep OB3 (Crawford & Barnes 1970), Lac OB1 (Crawford & Warren 1976), and on three field stars Knude 1977). …”

Section: Selection Of Standard Starsmentioning

confidence: 99%

“…It is a subtle process to obtain accurate standard photometry of reddened early-type stars, see, e.g., Crawford (1994) for a discussion.…”

Section: Are the Present Data On The Standard System?mentioning

confidence: 99%

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uvbyβphotometry of early type open cluster and field stars

Handler

2011

A&A

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Context. The β Cephei stars and slowly pulsating B (SPB) stars are massive main sequence variables. The strength of their pulsational driving strongly depends on the opacity of iron-group elements. As many of those stars naturally occur in young open clusters, whose metallicities can be determined in several fundamental ways, it is logical to study the incidence of pulsation in several young open clusters. Aims. To provide the foundation for such an investigation, Strömgren-Crawford uvbyβ photometry of open cluster target stars was carried out to determine effective temperatures, luminosities, and therefore cluster memberships. Methods. In the course of three observing runs, uvbyβ photometry for 168 target stars was acquired and transformed into the standard system by measurements of 117 standard stars. The list of target stars also included some known cluster and field β Cephei stars, as well as β Cephei and SPB candidates that are targets of the asteroseismic part of the Kepler satellite mission. Results. The uvbyβ photometric results are presented. The data are shown to be on the standard system, and the properties of the target stars are discussed: 140 of these are indeed OB stars, a total of 101 targets lie within the β Cephei and/or SPB star instability strips, and each investigated cluster contains such potential pulsators. Conclusions. These measurements will be taken advantage of in a number of subsequent publications.

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“…The calculation is performed by using photometry from sources whose zeropoint consistency has been checked (see Taylor & Joner 1992;Joner et al 1995, and sources listed in the footnotes to Table 8). At least three ways to represent the required relation have been published (see Crawford 1978Crawford , 1994Shobbrook 1983), so it is derived afresh here. The form of the relation is assumed to be c 1 = S(b − y) + Z, and two-error least-squares analysis is used to obtain it (see Section 2.1 of Taylor Table 8, they should be used only in the spectral-type range from B2 to B8.…”

Section: Appendix a Notes On The Newly Adopted Reddening Techniques Fmentioning

confidence: 99%

The Benchmark Cluster Reddening Project. Iv. A Statistical Test for Nonuniform Reddening in the Pleiades

Taylor

2008

The Astronomical Journal

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Using a protocol developed in previous papers in this series, the character of the Pleiades reddening is investigated. The protocol includes (1) analyses that yield results at the few-millimag level of precision and accuracy, (2) derivation of rigorous foundations for reddening values, (3) use of reddening techniques with limited metallicity sensitivity, (4) explicit zero-point control of input data, and (5) use of statistical analysis. It is found that in the eastern part of the Pleiades (as defined in a paper by Breger), E(B − V ) = 34 ± 11 mmag, with the quoted standard error depicting the amount of nonuniform reddening. In the western part of the Pleiades outside the "Southwest Nebula" (where E(B − V ) > 0.2 mag), the mean value of E(B − V ) = 57 ± 5.8 mmag, and the intrinsic rms scatter in E(B − V ) is 32 mmag. These results show that a widely adopted model in which E(B − V ) = 0.04 mag everywhere in the Pleiades outside the Southwest Nebula is not correct for any extended region in the Pleiades. They also show that the photometric properties of brown dwarfs in the western part of the Pleiades are not yet well established. In a collateral analysis, published high-dispersion values of [Fe/H] are used to derive mean metallicities for the Pleiades and Praesepe. The resulting values of [Fe/H] are −0.039 ± 0.014 dex and +0.057 ± 0.022 dex, respectively. When these results are combined with a mean high-dispersion metallicity for the Hyades, it is found that they are strongly inconsistent with a published explanation for the Pleiades distance modulus problem that is based specifically on photometric metallicities.

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UVBY and beta photometry for stars in the open cluster NGC 1502

Cited by 18 publications

References 10 publications

Photometric study of the OB star clusters NGC 1502 and NGC 2169 and mass estimation of their members at the University Observatory Jena

Photometric study of the OB star clusters NGC 1502 and NGC 2169 and mass estimation of their members at the University Observatory Jena

uvbyβphotometry of early type open cluster and field stars

The Benchmark Cluster Reddening Project. Iv. A Statistical Test for Nonuniform Reddening in the Pleiades

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