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J/AJ/109/663                       BV photometry in Terzan 7 (Buonanno+ 1995)
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Terzan 7: a young metal-rich globular cluster in the Milky Way
     Buonanno R., Corsi C.E., Pulone L., Fusi Pecci F., Richer H.B.,
     Fahlman G.C.
    <Astron. J. 109, 663 (1995)>
    =1995AJ....109..663B
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ADC_Keywords: Clusters, globular ; Photometry, CCD

Abstract:
    The first extensive CCD color-magnitude diagram for the metal-rich
    galactic globular cluster Terzan 7 is presented. All age indicators
    derived from this diagram suggest that the cluster is young, about 70%
    of the age of 47 Tuc, which has similar metallicity. A rich population
    of blue straggler stars is also found in this cluster. With Terzan 7,
    the anomaly of young clusters is thus extended to cover almost the
    entire range of galactic globular cluster metallicities. Several
    possibilities for the origin of young galactic globular clusters are
    discussed.

File Summary:
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 FileName    Lrecl    Records   Explanations
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ReadMe          80          .   This file
table2.dat      29       1731   Magnitudes, colors, and positions of stars in
                                Terzan 7
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Objects:
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       RA   (2000)   DE    Designation(s)
    ----------------------------------------------------------
      19 17 42   -34 39.4  Cl Terzan 7 = C 1914-347
    ----------------------------------------------------------

Byte-by-byte Description of file: table2.dat
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   Bytes Format  Units    Label      Explanations
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   1-  5  I5     ---      Star       Star number
   7- 11  F5.2   mag      Vmag       V magnitude
  13- 17  F5.2   mag      B-V        B-V color
  19- 23  I5     pix      Xpos       X pixel position (1)
  25- 29  I5     pix      Ypos       Y pixel position (1)
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Note (1): The Xpos and Ypos coordinates are in pixels relative to the cluster
           center. The location of this reference point was determined by
           evaluating the unweighted means of the X and Y positions of the
           stars falling within a radius of 300 pixels from a provisional
           center fixed by eye, until the procedure has converged to a stable
           value. A small subset of bright stars has been indicated in Fig. 1
           of the printed paper to provide a reference grid for the
           identification of the stars in Table 2.
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Origin: AAS CD-ROM series, Volume 5, 1995         Lee Brotzman [ADS] 26-Sep-1995
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(End)                                                         [CDS]  09-Jan-1996