Liller 1 / C1730-333
RA: 17:33:24.50 DEC: -33:23:20.4  (J2000)

(Most recent updates: 
Membership probability flag - 2024; Remaining data - April 2014)
============================================================
Bytes  Format      Explanation
1-8      A8        Star ID
10-32  A11,1x,A11  Position
34-35    A2        Membership probability flag based on data published
                   by Prudil & Arellano Ferro (2024)
                    m1: prob >=0.85;  m2: prob >=0.7 and <0.85;
                    m3: prob >= 0.5 and <0.7; f: prob <0.5
                    u:  no data available
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
=========================================================================
ID       Position               Mem   Period <mag>  ampl  C Type  Notes/
         RA          Dec        Flag                              Remarks
=========================================================================
No known variables.
=========================================================================
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 

Prudil Z., Arellano Ferro, A. 2024, MNRAS, 534, 3654

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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