Liller 1 / C1730-333
(Updated April 2014)

RA: 17:33:24.50 DEC: -33:23:20.4  (J2000)

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Bytes  Format      Explanation
1-8      A8        Star ID
10-32  A11,1x,A11  Position
34-35    A2        Units for position
                    R0 denotes RA, DEC in the J2000 coordinates
                    R5 denotes RA, DEC in the 1950 coordinates
                    XA denotes X, Y in arcseconds 
                    XP denotes X, Y in pixels
37-44   F8.4       Period  (days)
46-51   F6.3       Mean magnitude (or maximum magnitude if "max" 
                      is indicated in the remarks column)
53-57   F5.3       Light amplitude (range of variability)
59      A1         Colour for mean magnitude and amplitude
                    e.g.  B, V, R, I, J, K
                    or P (for photographic).
61-65   A5         Type of variable (draft 2006 GCVS classifications)
                      CST denotes non variable stars previously designated
                      as variables
67-80   A19        Notes and Remarks  (f denotes field star)
 
 "--" or "----" indicates no data available
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ID       Position                     Period <mag>  ampl  C Type  Notes/
         RA/X        Dec/Y     Units                              Remarks
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No known variables.
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Supplementary Notes 

This cluster, located in the error box of the X-ray burster MXB 1730-33,
was discovered by Liller (1977) on deep plates taken in the near IR with
the CTIO 4 metre telescope.
It was subsequently found by Tam et al. (2011) to be a Gamma-ray 
emitting cluster 

An infrared colour magnitude diagram by Ortolani et al. (2001) showed 
a red HB morphology, characteristic of a metal rich population and
Origlia et al (2002) derived [Fe/H] = -0.3, based on H-band echelle
spectra of two of the brightest giant stars in the cluster.
Thus it is unlikely that there will be any RR Lyrae or Cepheid
variables.  
The cluster lies in a heavily reddened field near the Galactic centre 
with V(HB) = 24.84 according to the 2010 version of the Harris (1996) 
catalogue.  
Blue stragglers would be too faint to be detected. 
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References

Harris, W. E. 1996, AJ, 112, 1487

Liller, W. 1977, ApJ, 213, L21

Origlia, L., Rich, R. M., Castro, S. 2002, AJ, 123, 1559

Ortolani, S., Barbuy, B., Bica, E., Renzini, A., Zoccali, M., Rich, R.
M., Cassisi, S. 2001, A&A, 376, 878 

Tam, P. H. T., Kong, A. K. H., Hui, C. Y., Cheng, K. S., Li, C., Lu,
T.-N., 2011, ApJ, 729, 90
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