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We present V and I photometry for a field 5' from the center of 47 Tuc. Thefield was imaged with the HST WFPC2 as part of the Medium Deep Survey project.The luminosity function (LF) continually rises in the domain $5 < M_I < 9$ witha slope $\Delta log \Phi (M) / \Delta M \sim 0.15$ and then drops off sharply.We compare our LF with that derived by De Marchi \& Paresce for a neighbouringHST field. The two independent LFs are very similar in the entire range ofluminosities probed ($M_I < 10$). Comparisons are also made to other HST LFsderived by several authors for different clusters in the Galaxy. We use the KStest to assess the significance of the differences found. The LFs obtained withHST are consistent with being derived from the same population down to $M_I\sim 9.0$. Beyond that, statistically significant variations arise. Globularcluster LFs also differ according to the prominence of a plateau in the brightend ($5 < M_I < 6.5$). Mass functions are sensitive to the mass-luminosityrelation. Different approaches to deriving the 47 Tuc mass function from its LFlead to markedly different results at the low mass end. For $M > 0.4 M_\odot$,the 47 Tuc mass function is significantly different from that of \wcen. Thecalibrated HST $M_V(V-I)$ colour-magnitude diagrams (CMDs) show a trend withmetallicity in the sense of metal richer systems having redder CMDs for a fixedabsolute magnitude. The main-sequence becomes shallower with increasingmetallicity. For metal-rich systems, the CMDs derived from HST are in generalagreement with previous ground-based studies. However, the CMDs of metal poorsubdwarfs observed from the ground are shallower than those of globularclusters observed with HST.Comment: 17 pages plus 8 figures. Accepted for publication in MNRA

HST photometry of 47 Tuc and analysis of the stellar luminosity function in Milky Way clusters