Linear Radii of 51 Red Giants in Galactic Clusters

Coleman, L. A.

doi:10.1086/113108

Cited by 17 publications

(14 citation statements)

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“…These entries concern a "consensus" database for M67 giants assembled by Taylor (2007) and cited in Table 11 of that paper. The contributing data are initially from Eggen & Sandage (1964), Coleman (1982), Janes & Smith (1984), and Sanders (1989), and are solely from photomultiplier measurements.…”

Section: A B − V Analysis For M67mentioning

confidence: 99%

“…For measurements published by Janes & Smith (1984), the offset from the Sanders (1989) Miller et al 2001) is >95%. c "SC" refers to data from Sturch (1973) and Coleman (1982) that are combined without a zero-point adjustment. d For the range B − V < 0.62, the formal correction to the Sanders data calculated using data from Eggen & Sandage (1964) and Sturch (1973) is +8.0 ± 4.2 mmag.…”

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confidence: 99%

“…g This entry is based on data from Table 2 that have been corrected by −9 mmag (see entry 4 of Table 4). h This entry refers to combined data from Janes & Smith (1984), Coleman (1982), Eggen & Sandage (1964), and Sanders (1989). The adopted zero-point adjustments to these data are (in order) 0, 0, −11, and −15 mmag, with the last correction applying only at B − V > 0.6 mag.…”

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confidence: 99%

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Tests of Broadband Photometric Consistency for Standard Stars, the Hyades, and M67

Joner

Taylor

Laney

et al. 2008

The Astronomical Journal

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New South African Astronomical Observatory (SAAO) BV(RI) C measurements of 19 Hyades stars and 11 M67 stars are reported. The zero points of the new color indices conform closely to those of SAAO data reported in a previous paper. In addition, the new M67 measurements of (V − R) C and (R − I ) C are compared to data published previously by Taylor, Joner, and Jeffery. The results support conclusions drawn by those authors that the scale factors of their data are correct and that a scale factor problem exists in measurements published by Montgomery, Marshall, and Janes. The new values of B − V are used with Tycho data in tests of extant Hyades and M67 measurements and of the accuracy of the SAAO B − V system. A problem encountered previously with the Hyades B − V zero point is resolved, and an extant Hyades relation between B − V and (R − I ) C is re-zeroed. A satisfactory zero point is also obtained for M67, and published photomultiplier values of B − V are reduced to that zero point, averaged, and tabulated. It is found that the zero point of B − V data published by Sandquist is satisfactory. However, tests of B − V measurements made by Montgomery et al. suggest that those data are not on a single zero point. Finally, the scale factor of the E region B − V system is found to be satisfactory, but a well-supported interim conclusion is drawn that E region values of B − V should be corrected by about −9 mmag. It is suggested that this conclusion be tested by using instrumental systems that have not yet contributed to the testing process.

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Section: A B − V Analysis For M67mentioning

confidence: 99%

mentioning

confidence: 99%

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confidence: 99%

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Tests of Broadband Photometric Consistency for Standard Stars, the Hyades, and M67

Joner

Taylor

Laney

et al. 2008

The Astronomical Journal

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“…(e) Star names from Klein Wassink (1927); Coordinates from Perryman et al (1997); B, V and R magnitudes from Coleman (1982); I J magnitudes from Mendoza (1967); Johnson et al (1966), K S magnitudes from 2MASS.…”

Section: Introductionmentioning

confidence: 99%

Chemical abundance analysis of the open clusters Berkeley 32, NGC 752, Hyades, and Praesepe

Carrera

Pancino

2011

A&A

130

139

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Context. Open clusters are ideal test particles for studying the chemical evolution of the Galactic disc. However, the number and accuracy of existing high-resolution abundance determinations, not only of [Fe/H], but also of other key elements, remains largely insufficient. Aims. We attempt to increase the number of Galactic open clusters that have high quality abundance determinations, and to gather all the literature determinations published so far. Methods. Using high-resolution (R ∼ 30 000), high-quality (S /N ≥ 60 per pixel), we obtained spectra for twelve stars in four open clusters with the fibre spectrograph FOCES, at the 2.2 Calar Alto Telescope in Spain. We employ a classical equivalent-width analysis to obtain accurate abundances of sixteen elements: Al, Ba, Ca, Co, Cr, Fe, La, Mg, Na, Nd, Ni, Sc, Si, Ti, V, and Y. We derived oxygen abundances by means of spectral synthesis of the 6300 Å forbidden line. Results. We provide the first determination of abundance ratios other than Fe for NGC 752 giants, and ratios in agreement with the literature for the Hyades, Praesepe, and Be 32. We use a compilation of literature data to study Galactic trends of [Fe/H] and [α/Fe] with Galactocentric radius, age, and height above the Galactic plane. We find no significant trends, but some indication for a flattening of [Fe/H] at large R gc , and for younger ages in the inner disc. We also detect a possible decrease in [Fe/H] with |z| in the outer disc, and a weak increase in [α/Fe] with R gc .

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“…(3) Photoelectric UBV photometry from ES, Sturch (1973) and Eggen (1983). (4) Photoelectric UBV photometry from ES, Sturch (1972Sturch ( , 1973, Coleman (1982) and Eggen (1983). (5) Photoelectric UBV photometry from ES, Coleman (1982), Schild (1983) and Eggen (1983).…”

Section: M67 (Ngc 2682)mentioning

confidence: 99%

Giants in old open clusters - Temperatures, luminosities, and abundances from infrared photometry

Houdashelt¹,

Frogel²,

Cohen³

1992

The Astronomical Journal

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We present infrared observations for more than 100 red giants and clump stars in eight old open clusters. We have assembled the best available optical photometry for these stars and determined a consistent set of integrated physical parameters (reddening, distance modulus, abundance, and age) for the clusters. From color-color and color-magnitude diagrams that make use of both the infrared and optical data, we are able to identify quite a few stars as probable field stars rather than cluster members. However, because of a general scarcity of bright stars, it is often difficult to distinguish between cluster members on the asymptotic giant branch and field interlopers. In a (U-V) 0 , (V-K) 0 plot, stars from the most metal-poor open clusters tend to lie between the relations defined by field and globular cluster giants. On the other hand, nearly all of the open cluster stars lie near the field giant line in a (H-K) 0 plot. The mean CO strengths of the giants in each open cluster show a range consistent with the optically determined range in [Fe/H], but the correlation between these two quantities is weak, probably because of the small total range of each and the significant uncertainties in [Fe/H]. The results for the open clusters, though, are consistent with the relation between CO and [Fe/H] established for globular clusters and considerably strengthen that relation near the solar metallicity end. For these eight open clusters, there is a modest linear correlation between [Fe/H] and age which shows a gradient in metallicity of about-0.1 dex per Gyr and gives [Fe/H] 0.6 for r = 5 Gyr, the age of the sun. The relation is quite similar in slope and zero point to that exhibited by clusters in the Large Magellanic Cloud. If the open cluster data are adjusted for the galactic radial metallicity gradient, the age-metallicity relation becomes intermediate to those of the Large Magellanic Cloud and the solar neighborhood. This could be an indication that the old open clusters are representative of the stellar population of the galactic thick disk. The temperatures of the cluster giant branches determined from infrared observations are tightly correlated with the optically derived values for age and [Fe/H]. Also, there is general agreement between the location of the cluster giant branches in an H-R diagram determined from infrared photometry and the predictions of the Revised Yale Isochrones. Specific differences that exist between the theoretical and semiempirical parameters can at least partially be attributed to uncertainties in the (primarily) optical data and/or the presence of convective overshooting. 163 Astron. J. 103 (1), January 1992 tometry, reddening, distance modulus, age, metallicity, and membership probability. We describe the infrared observing program in Sec. 3. Sections 4 and 5 present the color-magnitude diagrams (CMDs) and color-color plots, respectively; stars which may be field stars or otherwise peculiar are noted here. Section 4 also provides an extensive review of the literature pertaining to th...

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Linear Radii of 51 Red Giants in Galactic Clusters

Cited by 17 publications

References 0 publications

Tests of Broadband Photometric Consistency for Standard Stars, the Hyades, and M67

Tests of Broadband Photometric Consistency for Standard Stars, the Hyades, and M67

Chemical abundance analysis of the open clusters Berkeley 32, NGC 752, Hyades, and Praesepe

Giants in old open clusters - Temperatures, luminosities, and abundances from infrared photometry

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