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NGC 2451 - What is it?
During the last decade, a debate has arisen whether the grouping ofstars called NGC 2451 is a real star cluster. We investigate thecorresponding area of the sky kinematically, using proper motions of thePPM catalogue. The group of stars that was originally called NGC 2451shows a large scatter of their proper motions, which proves that they donot form a cluster. However, close-by we find a group of 24 PPM starswith common proper motion. A colour-magnitude diagram of 19 of theseshows an extremely well-defined main sequence, giving a distance ofabout 220 pc. This cluster is not NGC 2451. We tentatively call itPuppis Moving Group (PMG). There is strong indication for a secondcluster at about 400 pc. Photometry, radial velocities and propermotions of stars fainter than the magnitude limit of PPM are needed tofurther investigate the matter.
| Membership and photometric abundances of red evolved stars in open clusters
UBV and DDO photometric observations of 31 red evolved stars toward 11open clusters, obtained with the 41-cm and 91-cm telescopes at CerroTololo Interamerican Observatory on four nights in 1978, are reported.The data are compiled in tables and characterized for each cluster, andtwo criteria are used to determine the probability that a star is amember of a cluster. Six of the clusters are found to contain oneevolved red star, one has two, one has four, and three have none; theother 19 stars are seen as red field objects. The estimated cluster Fe/Habundance ratios range from -0.2 to +0.3, and the red giants in theclusters NGC 2335 and NGC 2567 are found to have CN strengths like thoseseen in Hyades giants. The unusual weakness of the 421.6-nm band of CNfor star 108 in NGC 2548 is attributed either to unusual composition andproper motion or to its nonmembership in the cluster despite meeting thephotometric criteria.
| DDO photometry on red giants in the open clusters NGC 2232, NGC 2287, and NGC 2451
From DDO photometry combined with U, B, V photometry of red stars in theopen clusters NGC 2232, NGC 2287, and NGC 2451, the mean color excess E(B-V), the distance modulus, and the mean metal abundance (Fe/H) werederived for the clusters. The physical parameters, surface gravity,effective temperature, and spectral type were also obtained for the redstars. Estimation of age yielded 1.1 x 10 to the 8th yr for NGC 2287,and for NGC 2451, 4.8 x 10 to the 8th. The cluster NGC 2232 should beolder than 10 to the 9th yr.
| Evolved stars in open clusters.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1976ApJS...30..451H&db_key=AST
| Spectral types in the open cluster NGC 2451.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1975PASP...87..823L&db_key=AST
| Error analysis of the photoelectric catalogue
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1973A&AS....9..297F&db_key=AST
| Narrow- and Broad-Band Photometry of Red Stars. V. Luminosities and Temperatures for Young Disk-Population Red Stars of High Luminosity
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1971ApJ...163..313E&db_key=AST
| Photoelectric Photometry of NGC 2451
Not Available
| The Open Cluster NGC 2451
Not Available
| Photometry of NGC 2451
Not Available
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| Takýmyýldýz: | Pupa |
| Sað Açýklýk: | 07h46m33.41s |
| Yükselim: | -37°46'21.2" |
| Görünürdeki Parlaklýk: | 6.325 |
| Uzaklýk: | 183.15 parsek |
| özdevim Sað Açýklýk: | -51.1 |
| özdevim Yükselim: | -29.7 |
| B-T magnitude: | 8.084 |
| V-T magnitude: | 6.471 |
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