Studyingcompactobjects(CO)suchaswhitedwarfs(WDs), neutron stars (NSs) and stellar-mass black holes (BH) with masses typically ranging from 3−20 M is important for understanding theendpointsofstellarevolutionandaccretion/ejectionprocesses, ubiquitousphenomenaintheUniverse. Itprovidesfurtherinsights into the gas state and distribution in the early Universe. Studying the cosmic history of supermassive BH (with masses ranging from 106−10 M) growth could shed light on the formation and evolution of galaxies. It tells us more about their role in the reionization of the Universe and their impact on their (interstellar and/or intergalactic) environment. COs are also excellent laboratories to study matter in extreme conditions, such as matter at super-nuclear density in the NS interior or matter under the effect of strong gravity and magnetic ﬁelds in the vicinity of BHs and NSs, respectively. Due to accretion of matter that goes on in their vicinity, most COs were first detected in X-rays. For these reasons, all-sky X-ray surveys are most suitable for ﬁnding and studying such sources. TheSwift observatory, inoperationsince2004, carriesanX-ray telescope (XRT) and two other co-aligned instruments, the Burst Alert Telescope (BAT) and the UV/Optical Telescope (UVOT). This enables a multi-wavelength study of CO behaviour from optical to hard X-rays. Swift is dedicated to the study of gammaray bursts that appear randomly on the sky. This implies that Swift pointingshavebeenperformedalloverthesky,covering1905 square degrees with the XRT, with many ﬁelds observed several timeswithinaday,overaperiodfrommanydaystoweeks/months (orevenyears),allowingtoprobevariabilityonvarioustimescales. In this work, I investigated the nature of the X-ray sources contained in the Swift-XRT catalog in order to isolate interesting objects possibly harbouring an accreting compact object (e.g. Xray binaries, active galaxy nuclei – AGN, ultra-luminous X-rays sources, tidal disruption events). To do so, I cross-correlated a subsample of the Swift X-ray Telescope Point Source (1SXPS) catalog, containing 98,762 sources with detections of best quality, with 16 external multi-wavelength catalogs which provide source type identiﬁcation (active galactic nuclei, stars, X-ray binaries etc.) using the Topcat software. This enabled me to build a golden sample of known objects, divided into three main classes (AGNs, COs and stars) that represent the main types of objects observed in the X-ray sky. Within this subsample, I found that it consists of 4929 AGNs, 1125 stars and 231 COs. I studied their temporal, spectral and spatial properties in order to deﬁne selection criteria which would enable me to classify the rest of the 1SXPS sources. I found that COs are the most variable group, followed by AGNs and stars. Using spectral indicators from the 1SXPScatalog(power-lawphotonindexΓPL andhardnessratios), I found that the ΓPL-distributions of COs, AGNs and stars diﬀer. ForAGNs,theΓPL-distributionisclusteringaround1.71,whichis consistent with typical values derived for these objects. For COs, the distribution of ΓPL-values is more widely spread, likely corresponding to the diﬀerent spectral states that can be seen in X-ray binaries. Stars also display scattered ΓPL-distribution, but with generally high values, implying that the PL model is not physical and that thermal emission is more likely. I found that most stars can be isolated from the rest of AGNs and COs thanks to their low X-ray to optical or IR flux ratio. After establishing the selection criteria, I applied them to the golden sample of identiﬁed sources, in order to investigate the reliability of the deﬁned selection scheme. 73% of the stars, 35% of the COs, and 95% of the AGNs were retrieved, with false classiﬁcation probability of 8%, 78% and 15%, respectively. The low number of retrieved COs and their high probability of false identiﬁcation is due both to the large fraction of AGN with respect to COs in the golden sample and the fact COs and AGNs share similar properties (ΓPL-distribution and X-ray to optical/IR distribution intervals coincide). Finally, the selection criteria were applied back to the rest of the 1SXPS source high quality sample, resulting in 78,918 AGN candidates (86%), 9294 star candidates (10%) and 3752 CO candidates (4%). I discuss the caveats of the method used and I propose possible improvements, in particular for helping decreasing the high probability of false identiﬁcation rate for COs. I also discuss further interesting works that could be done from the obtained results.