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We propose obtaining COS G130M spectra of QSOs lying behind dwarf galaxies (with stellar masses of logCORCHETE_OPENM*(M_solar)CORCHETE_CLOSE < 9.0) to study the absorption lines that the galaxies. circumgalactic medium (CGM) produces along the sightlines to the background probes. The galaxies are selected to lie at low redshifts so that a range of techniques can be used to complement the results from the absorption line spectroscopy (such as 21 cm emission line mapping). We define two samples of dwarf galaxiesdoublePoint (a) SINGLE isolated dwarf galaxies and (b) PAIRS of isolated dwarf galaxies. For both samples comma we aim to determine the extent of the neutral and metal-enriched CGM around the galaxies comma search for changes in the phases of the CGM with distance from the galaxies comma and measure comma when possible comma the metallicity of the CGM. A principal goal is to examine whether the CGM of dwarf galaxy pairs is different from that of single dwarf galaxies that is comma we aim to use the sample of single dwarf galaxies as a control sample for the pairs of dwarf galaxies. This comparison will enable us to examine whether interactions between dwarf galaxies lead to substantial amounts of baryons being 'parked. in the outskirts of their CGM comma acting as reservoirs that fuel their star formation (SF). A direct comparison between the properties of the CGM of the dwarf galaxy pairs with the single dwarf galaxies will demonstrate whether the CGM is dominated by tidal interactions or comma instead comma by outflows of gas instigated by the SF that the interactions ignite.