Four-color and H-beta photometry of open clusters - V - NGC 752.

Crawford, D. L.; Barnes, J. V.

doi:10.1086/111044

Cited by 41 publications

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“…j Applied luminosity corrections are from Fig. 6 of Crawford & Barnes (1970) and the c 1 term in the Crawford (1975) calibration. Data for giants are excluded from the analysis.…”

Section: Assessing M67 Color Indices: Further Results For Two Importamentioning

confidence: 99%

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Cousins Photometry and Temperatures for the Hyades, Coma, NGC 752, Praesepe, and M67

Taylor

Joner

Jeffery

2008

ASTROPHYS J SUPPL S

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In this paper, new Cousins VRI data are presented for NGC 752 and Praesepe, and new and extant data are combined into an augmented database for M67. For those three clusters, catalogs containing Cousins VRI photometry, reddening-corrected values of (V À K ) J , and temperatures are produced. The same is done for Coma by using both previously published and newly derived Cousins photometry. An extant set of catalogs for the Hyades is updated to include V magnitudes and values of (R À I ) C that were published after the original catalogs appeared. Finally, M67 V magnitudes published previously by Sandquist are corrected for an effect that depends on location on the face of the cluster. The corrected data and values of (V À I ) C given by Sandquist are then set out in a supplementary catalog. Data files containing all of these catalogs are deposited in the CDS archives. To assess the quality of the data in the catalogs, the consistency of extant Cousins VRI databases is tested by performing analyses with the following features: (1) quantities as small as a few millimags are regarded as meaningful; (2) statistical analysis is applied; (3) no use is made of data other than VRI measurements and comparable results; (4) no inferences are drawn from colormagnitude comparisons; (5) pertinent data that have not been included previously are analyzed; and (6) results based on direct comparisons of stellar groups at the telescope are featured. In this way, it is found that our updated M67 color data and those of Sandquist are on the E region zero point. In contrast, values of (V À I ) C from Montgomery and collaborators are found to be too red by 27 AE 3 mmag, with an even larger offset being likely for unpublished data from Richer and his collaborators. Zero-point tests of our Cousins VRI colors for Coma, Praesepe, and NGC 752 are also satisfactory. Scale factor tests of the M67 colors are performed, and a likely scale factor error in the Montgomery et al. colors is found. However, it appears at present that the scale factors of our M67 colors and those of Sandquist are satisfactory. For the most part, zero-point tests of the assembled V magnitudes are also satisfactory, although it is found that further work on the V magnitudes for Praesepe and M67 would be useful. To put these results in perspective, it is pointed out that photometric tests that are satisfactory at the few-millimag level have been published for some two decades and so are not appearing for the first time in this paper.

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“…j Applied luminosity corrections are from Fig. 6 of Crawford & Barnes (1970) and the c 1 term in the Crawford (1975) calibration. Data for giants are excluded from the analysis.…”

Section: Assessing M67 Color Indices: Further Results For Two Importamentioning

confidence: 99%

“…d These data have been standardized by using Landolt (1983) standards (see x 3.2 of TJ05). e The first abbreviation stands for Crawford & Barnes (1969). The zero-point consistency of data from the two papers is established by TJ92.…”

Section: Magnitudes: Establishing Zero Pointsmentioning

confidence: 99%

Cousins Photometry and Temperatures for the Hyades, Coma, NGC 752, Praesepe, and M67

Taylor

Joner

Jeffery

2008

ASTROPHYS J SUPPL S

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“…It should be emphasized in this particular case that, unlike NGC 3680, the DDO result (−0.16) differs from that of the spectroscopy (−0.05) by more than 0.1 dex. A significant improvement occurs in the results from uvbyHβ photometry, where the m 1 data of Twarog (1983) exhibited a systematic offset compared to that of Crawford & Barnes (1970) and Nissen (1988) Despite its proximity to the Sun, there have been surprisingly few spectroscopic studies of stars within NGC 752. At high (2004) dismiss all previous metallicity estimates as either irrelevant or unreliable, a careful analysis confirms that they are remarkably consistent, with most comparisons of the absolute scale distorted by differences among the metallicity zero points.…”

Section: Ngc 752mentioning

confidence: 95%

Lithium in the Intermediate-Age Open Cluster, NGC 3680

Anthony-Twarog

Deliyannis

Twarog

et al. 2009

The Astronomical Journal

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“…(b) Averages of measurements by Johnson (1953);Roman (1955);Johnson (1961); Rohlfs & Vanysek (1962); Arp (1962); Eggen (1963); Crawford & Barnes (1970); Patenaude (1978); Hardy (1979);Nicolet (1981); Twarog (1983); Barry et al (1987);Nissen (1988); Mazzei & Pigatto (1988); Eggen (1989); Francic (1989);Boesgaard (1991); Dzervitis & Paupers (1993);Carraro et al (1993); Meynet et al (1993);Daniel et al (1994); Piatti et al (1995); Dinescu et al (1995); Milone et al (1995); Claria et al (1996); Dutra & Bica (2000); Loktin & Beshenov (2001); Blake (2002); Blake & Rucinski (2004); Salaris et al (2004); Bartašiūtė et al (2007);Taylor (2007); and Giardino et al (2008).…”

Section: Referencesmentioning

confidence: 99%

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

Carrera

Pancino

2011

A&A

128

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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Four-color and H-beta photometry of open clusters - V - NGC 752.

Cited by 41 publications

References 0 publications

Cousins Photometry and Temperatures for the Hyades, Coma, NGC 752, Praesepe, and M67

Cousins Photometry and Temperatures for the Hyades, Coma, NGC 752, Praesepe, and M67

Lithium in the Intermediate-Age Open Cluster, NGC 3680

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

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