tokens: different cell sizes in the CMDs, they are fixed each time, i.e. they do not vary across the CMDs. From our experience in cleaning the field star contamination in the cluster CMDs, we have identified some situations which still need our attention. It frequently happens that some parts of the CMDs are more populated than others, so that fixing the size of the cells in the CMDs becomes a difficult task. Small cells do not usually carry out a satisfactory job in CMD regions with a scarce number of field stars, while big cells fail in populous CMD regions. Thus, relatively bright field red giants with small photometric errors could not be subtracted and, consequently, the cluster CMD could show spurious red giant features. A compromise between minimizing the residuals left after the subtractions of field stars from the cluster CMDs and maximizing the cleaning of field stars is always desirable. In this paper, we present a comprehensive multiband photometric analysis of Haffner9 from BVI and Washington CT 1 photometry. The cluster has been previously studied from 2MASS and BVI photometry. However, a relatively lower photometric accuracy and shallower limited magnitude, in combination with a not much pinpointed treatment of field decontamination led those studies to discordant results. In Section 2 , we describe the collection and reduction of the available photometric data and their thorough treatment in order to build an extensive and reliable data set. The cluster structural and fundamental parameters are derived from star counts and CMD and colourcolour (CC) diagrams, respectively, as described in Section 3 . The analysis of the results of the different astrophysical parameters obtained is carried out in Section 4 , where implications about the stage of its dynamical evolution are suggested. Finally, Section 5 summarizes the main conclusion of this work. 2 DATA COLLECTION AND REDUCTION We used CCD images 1 obtained on the nights of 2004 December 18 and 19 with a 2048 2048pixel Tektronix CCD attached to the 0.9-m telescope (scale 0.396 arcsecpixel 1 ) at Cerro Tololo Inter-American Observatory (CTIO, Chile). Its field of view (FOV) is 13.6 13.6arcmin 2 . We used the Washington C (Canterna 1976 ) and KronCousins R filters. The latter has a significantly higher throughput as compared with the standard Washington T 1 filter so that R magnitudes can be accurately transformed to yield T 1 magnitudes Geisler ( 1996 ). We used a series of bias, dome and sky flat-field exposures per filter to calibrate the CCD instrumental signature. We also utilized images for the Small Magellanic Cloud cluster Lindsay106, which was previously observed at La Silla (ESO, Chile) with the C and T 1 filters (Piatti etal. 2007 ). Lindsay106 was used here only as control cluster, i.e. to verify the quality of the present CTIO photometry. Table 1 shows the log of the observations with filters, exposure times, airmasses and seeing estimates. A large number (typically 20) of
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