This chapter describes the set of commands implemented in MIDAS to
do crowded field photometry on digital astronomical images. The
package has been developed by
R. Buonanno, G. Buscema, C. Corsi,
I. Ferraro, and G. Iannicola, all at the Osservatorio Astronomico di
Roma. The package runs as a part of the data reduction system at Rome
Observatory and is well known from its name: ROMAFOT.
Since in Italian the suffix ``fot'' refers also to the word ``photometry'',
the name ROMAFOT was chosen as an easy homophony with DAOPHOT.
The idea of ROMAFOT was born (and realised) in the second half of the
seventies. The need for such a package has arisen from the technical
evolution (for instance the arrival of the PDS etc.) and from
the huge amounts of data becoming manageable. A rich bibliography
of authors who worked on the same objective (e.g. Newell and O'Neil,
1974 [1], Van Altena and Auer, 1975 [2], Butcher, 1977
[3], Herzog and Illingworth, 1977 [4],
Chiu, 1977 [5], Auer and Van Altena, 1978 [6]
Buonanno et al., 1979 [7], Buonanno et al., 1983 [8]
Stetson, 1979 [9], Stetson, 1979 [10]) shows that
efficient handling of digital
astronomical images was widely felt for the astronomical community.
In addition, since the numerical problem requires very classic solutions,
neither the idea nor the solution asks for particular emphasis.
Where ROMAFOT has perhaps merit is in having taken dozens of decisions
such as:
In this description Section 
gives some theoretical
background about how ROMAFOT operates. Section
presents an overview of the commands available in the ROMAFOT context.
Section describes the commands in detail. The
section is split into a part for the automatic reduction and a part for
the more interactive reduction. Finally, Section
gives a summary of all ROMAFOT commands.