The Palomar-Groningen field #3 (hereafter referred to as PG3)
was searched for variable stars by Plaut (1971).
The variables discovered by Plaut were re-examined by Wesselink
(1987), using UKST 
and 
Schmidt plates.
A new blink done on 10% of the total PG3 area
on the original 103aO plate material used by
Plaut, resulted in the discovery of some additional variables.
It demonstrated that the completeness of the variable star
catalogue is better for variables with larger amplitudes.
The variables from this catalogue were the subject of various
studies: the RR Lyrae (Oort & Plaut 1975; Wesselink 1987),
the Mira variables (Blommaert 1992), and the
semiregular variables (Schultheis et al. 1996, hereafter
referred to as Paper II).
The non-variable stars in PG3 were studied by Ng (1994)
and Ng et al. (1995).
The Sagittarius dwarf galaxy was first identified by Ibata et al. (1994, hereafter referred to as IGI). Alard (1996) and Mateo et al. (1996) found that this galaxy is spatially more extended than found by IGI. Some stars from the Sagittarius dwarf galaxy could be present in the PG3 variable star catalog from Plaut (1971) and Wesselink (1987). In this paper we present a small catalogue of PG3 variable stars, which are likely member of the Sagittarius dwarf galaxy. The selection criteria and the catalogue are presented in Sect. 2. A discussion is given in Sect. 3, about the implications, that the carbon star in this sample has, on those found in the direction of the galactic bulge by Azzopardi et al. (1991).