An Acknowledgment

Moffat, J. Alston

doi:10.4039/ent3535-2

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“…The differences of these data (see Fig. 9 and Table 11) show that they agree fairly well with the present photometry, except for the photoelectric data by Moffat (1974b).…”

Section: Comparison With Previous Photometrysupporting

confidence: 87%

“…A distance of to the cluster has been derived by Melnick & Grosbol (1982) using electronographic UBV photometry. A CCD UBV photometric study by Melnick, Tapia & Terlevich (1989) found a mean value of which is in agreement with the earlier estimate by Moffat (1974b). They derived an average age of ∼2 to 3 Myr and showed that star formation is an on‐going process in NGC 3603.…”

Section: Introductionsupporting

confidence: 78%

“…From photographic photometry, Sher (1965) obtained a distance of 3.5 kpc for this cluster. However, Moffat (1974b) derived a much larger distance of , in agreement with the kinematical distance of (van den Bergh 1978). A distance of to the cluster has been derived by Melnick & Grosbol (1982) using electronographic UBV photometry.…”

Section: Introductionsupporting

confidence: 69%

“…NGC 3603. The photoelectric data provided by Moffat (1974b) and van den Bergh (1978) have 10 and 11 stars respectively in common with present photometry, while the electronographic data of Melnick & Grosbol (1982) and the CCD data of Melnick et al (1989) have 12 and 131 stars respectively common. The differences of these data (see Fig.…”

Section: Comparison With Previous Photometrymentioning

confidence: 51%

“… This figure presents, for NGC 3603, a comparison of the present photometry with photoelectric data from van den Bergh (1978) (*) and Moffat (1974b)(×), with electronographic data from Melnick & Grosbol (1982) (○) and with CCD data from Melnick et al (1989)(●). Other details are the same as in Fig.…”

Section: Comparison With Previous Photometrymentioning

confidence: 85%

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A multicolour CCD photometric and mass function study of the distant southern open star clusters NGC 3105, NGC 3603, Melotte 105, Hogg 15, NGC 4815, Pismis 20 and NGC 6253

Sagar

Munari

Boer

2001

Monthly Notices of the Royal Astronomical Society

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We derive cluster parameters and mass functions from new UBVRI CCD photometric observations of ∼3500 stars reaching down to for the distant southern open star clusters NGC 3105, NGC 3603, Melotte 105, Hogg 15, NGC 4815, Pismis 20 and NGC 6253. For NGC 3105 and Hogg 15, CCD data are presented for the first time. The reddening is non‐uniform across the face of the young (age <300 Myr) clusters NGC 3105, NGC 3603, Melotte 105, Hogg 15 and Pismis 20, with average values of 1.44, 0.52, 1.15 and 1.20 mag respectively, while it is uniform with average values of and 0.20 mag for the older clusters NGC 4815 and 6253 respectively. The values of colour excess ratios indicate the presence of normal interstellar reddening across the cluster regions studied here. Well‐defined main sequences can be seen in all the clusters. However, main‐sequence turn‐off points and subgiant branches are well defined only in the older clusters NGC 4815 and 6253. The distances to the clusters NGC 3105, NGC 3603, Melotte 105, Hogg 15, NGC 4815, Pismis 20 and NGC 6253 are , , , , , and respectively, while the corresponding ages derived using theoretical convective core overshooting stellar evolutionary isochrones are , , , , , and respectively. In the mass range ∼, the mass functions of all clusters except for NGC 6253 have been studied. The slopes of their mass spectra agree within errors with the Salpeter value (1.35). The slope of the mass function for stars more massive than 10 M⊙ is almost the same as for the lower mass stars. The mass function slopes of clusters younger than 500 Myr seem to have no dependence on Galactic longitude, Galactocentric distance and cluster age. As the inherent uncertainties in the mass function determinations of young Galactic star clusters can produce internal scatter that is larger than the external scatter, we conclude that, above 1 M⊙, the initial mass function is universal with a slope of Salpeter value.

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“…The differences of these data (see Fig. 9 and Table 11) show that they agree fairly well with the present photometry, except for the photoelectric data by Moffat (1974b).…”

Section: Comparison With Previous Photometrysupporting

confidence: 87%

Section: Introductionsupporting

confidence: 78%