3EG J0010+7309 Suggested (Lamb & Macomb, 1997ApJ...488..872L) as possibly 3EG J0010+7309 associated with the SNR CTA 1. Brazier et al. 3EG J0010+7309 (1998MNRAS.295..819B) have suggested that this source might be 3EG J0010+7309 a Geminga-like pulsar associated with CTA 1. 3EG J0222+4253 Verbunt et al. (1997ApJ...483L..49V), Kuiper et al. (1999, in 3EG J0222+4253 Proc. Third INTEGRAL Workshop, The Extreme Universe, in press), 3EG J0222+4253 and Hermsen et al. (1999, Adv. Space Res., submitted) have shown 3EG J0222+4253 indications from EGRET data for pulsed gamma-ray emission 3EG J0222+4253 between 100 and 1000 MeV from PSR 0218+42, which is 10 from 3EG J0222+4253 3C 66A, and 10 from the catalog position. Those authors conclude 3EG J0222+4253 that the data are consistent with the pulsar being the 3EG J0222+4253 counterpart below 1 GeV (based on timing and spatial analysis) 3EG J0222+4253 and 3C 66A above 1 GeV (spatial analysis). The analysis done for 3EG J0222+4253 this catalog (>100 MeV) found only one source near this 3EG J0222+4253 position. The catalog position given is based on the >1 GeV map, 3EG J0222+4253 which gives the smallest error contours; the contours of that 3EG J0222+4253 map agree well with the position of the BL Lac object 3C 66A and 3EG J0222+4253 exclude the pulsar. The 100-300MeV map, however, has 3C 66A 3EG J0222+4253 outside the 99% contour, while PSR 0218+42 is within the 95% 3EG J0222+4253 contour. The spectral index (2.01) given in the catalog assumes 3EG J0222+4253 only one source; if there are actually two, the 3C 66A spectrum 3EG J0222+4253 will be substantially harder and the PSR 0218+42 spectrum will 3EG J0222+4253 be correspondingly softer. 3EG J0530-3626 Considered a strong identification with 0521-365 in 2EG. However, 3EG J0530-3626 the position in this catalog, based on a much stronger detection 3EG J0530-3626 in cycle 4, is well outside the 99% confidence contour. 3EG J0542+2610 Suggested (Sturner & Dermer, 1995A&A...293L..17S) as possibly 3EG J0542+2610 associated with the SNR G180.0-1.7 (S147). 3EG J0617+2238 Suggested (Sturner & Dermer, 1995A&A...293L..17S; Esposito et 3EG J0617+2238 al., 1996ApJ...461..820E) as possibly associated with the SNR 3EG J0617+2238 G189.1+3.0 (IC 443). 3EG J0628+1847 Since this source is only 1.6{deg} from the very bright Geminga 3EG J0628+1847 pulsar, it could conceivably be an artifact resulting from 3EG J0628+1847 imperfections in the PSF. 3EG J0631+0642 Suggested (Sturner & Dermer, 1995A&A...293L..17S; Esposito et 3EG J0631+0642 al., 1996ApJ...461..820E) as possibly associated with 3EG J0631+0642 SNR G205.5+0.5 (Monoceros). 3EG J0824-4610 Almost certainly an artifact associated with the proximity of the 3EG J0824-4610 very bright Vela pulsar. It does not show up in a map which 3EG J0824-4610 excludes the Vela pulsation intervals. 3EG J0827-4247 Almost certainly an artifact associated with the proximity of the 3EG J0827-4247 very bright Vela pulsar. It does not show up in a map which 3EG J0827-4247 excludes the Vela pulsation intervals. 3EG J0828-4954 Almost certainly an artifact associated with the proximity of the 3EG J0828-4954 very bright Vela pulsar. It does not show up in a map which 3EG J0828-4954 excludes the Vela pulsation intervals. 3EG J0834-4511 The identification of this source, the brightest in the sky on 3EG J0834-4511 average, is not in doubt, because essentially all of the gamma 3EG J0834-4511 radiation is pulsed at the frequency of PSR 0833-45. The large 3EG J0834-4511 discrepancy between the position contours and the true position 3EG J0834-4511 of the pulsar is due to the 0.5{deg} binning of the standard 3EG J0834-4511 maps, compared with the 0.25{deg} size of the position map. A 3EG J0834-4511 similar but less dramatic effect is seen in the Geminga pulsar. 3EG J0834-4511 This effect is not apparent for the Crab pulsar because its 3EG J0834-4511 steeper spectrum makes the position determination less accurate. 3EG J0834-4511 Also, the apparent large time variation of the period-averaged 3EG J0834-4511 flux suggested by the individual observations is not supported 3EG J0834-4511 by careful analysis of the data (Ramanamurthy et al., 3EG J0834-4511 1995ApJ...450..791R; D. A. Kniffen 1998, private communication). 3EG J0841-4356 Almost certainly an artifact associated with the proximity of the 3EG J0841-4356 very bright Vela pulsar. It does not show up in a map which 3EG J0841-4356 excludes the Vela pulsation intervals. 3EG J0848-4429 Possibly an artifact associated with the proximity of the very 3EG J0848-4429 bright Vela pulsar. It shows up at 3.8{sigma} in a map which 3EG J0848-4429 excludes the Vela pulsation intervals. 3EG J0859-4257 Almost certainly an artifact associated with the proximity of the 3EG J0859-4257 very bright Vela pulsar. It does not show up in a map which 3EG J0859-4257 excludes the Vela pulsation intervals. 3EG J1102-6103 Suggested (Sturner & Dermer, 1995A&A...293L..17S) as possibly 3EG J1102-6103 associated with the SNR G291.0-0.1 (MSH 11-62). 3EG J1222+2841 BL Lac object 1219+295 = W Comae = ON +231 is well outside the 3EG J1222+2841 99% confidence contour. However, the identification with this 3EG J1222+2841 object is considered strong based on the position found for 3EG J1222+2841 E>1 GeV by Lamb & Macomb (1997ApJ...488..872L). 3EG J1324-4314 Good position agreement with Cen A, the nearest and brightest 3EG J1324-4314 radio galaxy. Although this is the only candidate detection of a 3EG J1324-4314 close radio galaxy by EGRET, we believe the identification is 3EG J1324-4314 robust, since the spectrum of this source agrees well with the 3EG J1324-4314 extension of the OSSE/COMPTEL spectrum (Sreekumar et al. 1998, 3EG J1324-4314 BAAS 29(5), 48.02b; 1999, Astroparticle Phys., in press ). That 3EG J1324-4314 spectrum, in turn, connects well with the spectrum at lower 3EG J1324-4314 X-ray energies, for which the Cen A identification is clear. 3EG J1410-6147 Suggested (Sturner & Dermer, 1995A&A...293L..17S) as possibly 3EG J1410-6147 associated with the SNR G312.4-0.4. 3EG J1627-2419 Although the gas in Rho Ophiuchus is included in the background 3EG J1627-2419 model, the scale of the variations is much smaller than the 3EG J1627-2419 pixel size in the EGRET maps. This may lead to apparent sources. 3EG J1638-5155 Roughly identified with 2EG J1648-5042; however, because of the 3EG J1638-5155 appearance in this catalog of three nearby sources, as well as 3EG J1638-5155 two below-threshold excesses, the position shown here is almost 3EG J1638-5155 20 away from the 2EG position. The suggestion by Mattox et al. 3EG J1638-5155 (1997, Cat. , 1997ApJ...476..692M) of 3EG J1638-5155 identification with radio source MRC 1646-506 = PMN J1650-5044 3EG J1638-5155 appears much less convincing with the new position. 3EG J1800-2338 Suggested (Sturner & Dermer, 1995A&A...293L..17S; Esposito et 3EG J1800-2338 al., 1996ApJ...461..820E) as possibly associated with the 3EG J1800-2338 SNR G006.6-0.1 (W28). 3EG J1823-1314 Suggested (Sturner & Dermer, 1995A&A...293L..17S) as possibly 3EG J1823-1314 associated with the SNR G018.8+0.3 (Kes 67). 3EG J1856+0114 Suggested (Sturner & Dermer, 1995A&A...293L..17S; Esposito et 3EG J1856+0114 al., 1996ApJ...461..820E) as possibly associated with the 3EG J1856+0114 SNR G034.7-0.4 (W44). de Jager & Mastichiadis 3EG J1856+0114 (1997ApJ...482..874D) have developed a model for the presumed 3EG J1856+0114 high-energy gamma-ray emission from W44. 3EG J1903+0550 Suggested (Sturner & Dermer, 1995A&A...293L..17S) as possibly 3EG J1903+0550 associated with the SNR G040.5-0.5. 3EG J2020+4017 Suggested (Sturner & Dermer, 1995A&A...293L..17S; Esposito et 3EG J2020+4017 al., 1996ApJ...461..820E) as possibly associated with the 3EG J2020+4017 SNR G078.2+2.1 ({gamma} Cygni). 3EG J2035+4441 Close to SNR W63, suggested (Esposito et al., 3EG J2035+4441 1996ApJ...461..820E) as a possible source of high energy gamma 3EG J2035+4441 radiation.