Notes on individual sources:
    Classification as DA of the white-dwarf star counterparts of the
    following EUV sources has been provided by M.A. Barstow et al.
    (private communication): 2RE J0029-632, J0053+360, J0148-253,
    J0317-853, J0512-004, J0512-414, J0521-102, J0632-050, J0648-252,
    J0715-702, J0902-040, J0957+852, J1019-140, J1024-302, J1027+322,
    J1032+532, J1845+682.

    For all the sources identified with DA+dM binary systems, the DA white
    dwarf is expected to dominate the EUV flux.

    In the notes below, the phrase `other close-by objects' is used to
    denote cases where there are objects, in addition to those given in
    Table 2, that cannot be excluded on positional grounds, and about
    which there is insufficient information to judge whether the object(s)
    are likely to contribute (and if so at what level) to the catalogued
    EUV flux.

2RE J0024-741. The IDP (Mason et al. 1995) finds no evidence of 
    chromospheric activity in HD 2133.

2RE J0039+103. Spectroscopic binary (SB1), H-alpha emission 
    (Jeffries et al. 1995).

2RE J0041+342. Strong Li 6708 line, H-alpha emission, probably single 
    (Jeffries 1995).

2RE J0044+093. The WD is estimated to contribute at least 90 per cent 
    of the EUV flux. However, the late-type star is very active, showing
    strong CaII H/K emission, and has vsini about km/s; it is clearly
    detected at higher X- ray energies, 0.4-2.4 keV (Barstow et al. 1994c;
    Kellett et al. 1994).

2RE J0106-225. We suggest SAO 166806 (=HD 6628) as a possible RS CVn 
    system, and certainly as a very active star, on the following basis.
    From the G5 V spectral type we estimate a distance of about 33 pc, and
    hence, from the mean S1-band count rate of 0.078 count/s, an EUV
    luminosity LEUV(erg/s) of log.LEUV about 29.8 (see Hodgkin & Pye 1994,
    fig. 2a). Such a high value strongly suggests that SAO 166806 is an
    active spectroscopic binary (see Hodgkin & Pye 1994, figs 5, 6 and 8).

2RE J0116-022. The DA WD star, with Teff=18000+/-3000 K (Simon, Fekel & 
    Gibson 1985), is too cool to contribute to the EUV emission.

2RE J0135-295. Other close-by objects: GJ 60B (K4 V,m V= 8:0), 
    GJ 60C (M2 V,m V= 10:4).

2RE J0137+183. Close visual binary(*) 2-arcsec separation, similar 
    components, both showing H-alpha emission and strong Li 6708 line
    (Jeffries 1995).

2RE J0155-513. Visual double system, separation a few arcsec. 
    Components are Gl 81A = HD 11937 = HR 566 (G8 III,m V= 3:7) and 
    Gl 81B = CPD-52 241B (unclassified, Vmag=10.7).

2RE J0228-611. The WD appears to dominate the EUV emission 
    (Barstow et al. 1993b, 1994c; Landsman, Simon & Bergeron 1993).

2RE J0255+474. Close visual binary 3-arcsec separation, similar components, 
    both showing H-alpha emission and strong Li 6708 line (Jeffries 1995).

2RE J0317-853. The DAp white-dwarf star has a high magnetic field 
    (M. A. Barstow et al., private communication).

2RE J0333+461. Close visual binary 10-arcsec separation, G5+dMe; 
    the brighter star has a strong Li 6708 line (Jeffries 1994).

2RE J0415-073. The DA4 WD 40 Eri B is too cool to contribute 
    significantly to the catalogued EUV flux. 
    Other close-by object: 40 Eri A (K1 Ve, Vmag=4.4).

2RE J0425-571. Identified with a Seyfert 1 galaxy
    (Brissenden et al. 1987; D. A. Buckley, private communication).

2RE J0426+153. Spectroscopic binary (SB3), V777 Tau = 71 Tau = VB 141, 
    one of the brightest X-ray and EUV sources in the Hyades star cluster.
    Which of the components contribute to the X-ray/EUV emission is
    unclear (Stern et al. 1992, 1994).

2RE J0437-022. Visual double system, separation about 65 arcsec. 
    Components are HR 1474 = HD 29391 (F0 V, Vmag=5.2) and 
    Steph 497 (M1, Vmag=10.6).

2RE J0449+065. Other close-by object: BD+06 762B (unclassified star, Vmag=8.8).

2RE J0453-421. Identified as an AM Her-type CV (Beuermann & Thomas 1993).

2RE J0457-280. The DA WD counterpart has a very low line-of-sight neutral 
    hydrogen column density through the ISM, nH=1.3x10^17^atom/cm2
    (Barstow et al. 1994a).

2RE J0459-101. Although the WD appears to account for most of the EUV 
    emission, there may be a contribution from the active, late-type
    companion (Barstow et al. 1993b, 1994c).

2RE J0503-285. The DO WD counterpart has a very low line-of-sight neutral 
    hydrogen column density through the ISM, nH=1.3x10^17^atom/cm2, and is
    the only DO WD in the 2RE Catalogue (Barstow et al. 1994b).

2RE J0512-115. Other close-by object: iota Lep (= HD 33802, B8 V, Vmag=4.4).

2RE J0515+324. The WD appears to dominate the EUV emission, though there 
    is also a (as yet unidentified) source of higher-energy X-ray emission
    seen at 0.4-2.4 keV (Barstow et al. 1993b, 1994c; Hodgkin et al. 1993).

2RE J0524+172. Other close-by object: HD 243294 (K0, Vmag=8.6).

2RE J0531-462. Identified with an AM Her-type CV, period 2.22 h 
    (Mason et al. 1995; Buckley et al., in preparation).

2RE J0557-380. TY Col = EXO 055609-3804.4; photometry appears to exclude 
    a single star; possible spectroscopic binary (SB1); may be young (high
    Li abundance); possible alternative spectral types G4 V+K2 V (yielding
    distance about 88 pc) or K0 IV+F7 V (yielding distance about 233 pc)
    (Tagliaferri, Cutispoto & Pallavicini 1994).

2RE J0622-601. Visual double system, separation=16.2 arcsec (Wilson 1979). 
    Components are CPD-60 604 = HD 45270 (G1 V, Vmag=6.6) and CPD-60 604B
    (unclassified, Vmag=10:6).

2RE J0637-613. The IDP (Mason et al. 1995) finds no evidence of 
   chromospheric activity in HR 2468.

2RE J0650-003. Other close-by object: BD-00 1462B (unclassified star, 
    Vmag=11.3). The IDP (Mason et al. 1995) finds no evidence of
    chromospheric activity in BD-00 1462.

2RE J0720-314. DAO+dM binary system, period about 1.2d 
    (Barstow et al. 1995b; Vennes & Thorstensen 1994).

2RE J0725-002. Spectroscopic binary (SB2), period=1.40d; both components 
    show H-alpha emission (Jeffries et al. 1995).

2RE J0731+361. Other close-by object: GJ 277B (M4 Ve, Vmag=11.8).

2RE J0743+224. Spectroscopic binary (SB1), H-alpha in emission 
    (Jeffries et al. 1995).

2RE J0751+144. CV, intermediate polar system (Mason et al. 1992).

2RE J0914+021. Other close-by object: 
    BD+02 2167B (unclassified star, Vmag=9.8)

2RE J0933+624. Spectroscopic binary (SB2), period=3.3d (Jeffries et al. 1995).

2RE J1016-052. DAO+dM binary system (Tweedy et al. 1993; Jomaron et al. 1993).

2RE J1101+223. Spectroscopic binary (SB2), period=1.53d (Jeffries et al. 1995).

2RE J1104-041. Visual multiple system, separation about 10 arcsec. 
    Components are BD-03 3040 (= ADS 8048) A (G5e, Vmag=7.6), 
    B (M3Ve, Vmag=10.3), C (no separate information found). 
    The IDP (Mason et al. 1995) finds both components A and B to be active.

2RE J1111-224. The WD appears to dominate the EUV emission 
    (Fleming et al. 1991; Barstow et al. 1993b, 1994c).

2RE J1118+313. Other close-by object: xi UMa A (= HD 98231, G0 Ve, Vmag=4.3).

2RE J1126-684. The proposed counterpart for this source is X-ray 
    nova/transient Muscae 1991. The WFC observations spanned the period
    1991 January 19-25. The WFC detection is likely to be due to leakage
    of soft X-ray photons, since the estimated column density from
    the ROSAT-PSPC measurements is nH about 2x10^21^cm-2, but the source 
    was very bright: about 6 `Crab' (Greiner et al. 1994).

2RE J1132+121. Spectroscopic binary (SB1), period=0.786d (Jeffries et al. 1995).

2RE J1135-630. Visual double system. Components are 
    lam Cen=HR 4467=HD 100841 (B9 III, Vmag=3.1) and
    HD 100841B (B9 V, Vmag=11.5) (Lindroos 1985).

2RE J1147+125. Strong Li 6708 line, H-alpha in emission, probably single 
    (Jeffries 1995).

2RE J1149+284. CV, AM Her system (Mittaz et al. 1992).

RE J1158+140. Spectroscopic binary (SB1), period=0.92 d (Jeffries et al. 1995).

2RE J1212+773. HR 4646 = HD 106112 = 4 Dra;
    spectroscopic binary, period=1.27 d (Margoni, Munari & Stagni 1992).

2RE J1257+351. Other close-by object: Gl 490B (= BD+36 2322B, M4Ve, Vmag=13.2).

2RE J1307+535. CV, AM Her system, orbital period=79.69min (Osborne et 
    al. 1994). This CV has the largest broad-band circular polarization
    amplitude and peak value observed so far in any astronomical object;
    the polarization is variable (+50 to-20 per cent) (Hakala et al. 1994).

2RE J1426+500. Resolved DA ( Vmag=14.0) + dMe ( Vmag=13.9) pair, 
    plus non-active dM star (IDP, Mason et al. 1995).

2RE J1442+352. ROSATEUV observations of Mkn 478 are discussed by 
    Gondhalekar et al. (1992).

2RE J1507+761. Strong Li 6708 line, probably single (Jeffries 1995).

2RE J1529+802. Visual multiple system, separations A-B=31 arcsec, 
    A-C=136arcsec (HIC, Turon et al. 1992). Components are 
    ADS 9696 A (= HD 139777, G0 IV- V, Vmag=6.6), 
    B (= HD 139813, G5, Vmag=7.3), C (unclassified, Vmag=11.4). 
    The IDP (Mason et al. 1995) finds component A to be active.

2RE J1601+664. AG Dra, symbiotic star.

2RE J1601+512. Spectroscopic binary (SB2), period=1.67 d 
    (Jeffries et al. 1995; see also Mullis & Bopp 1994).

2RE J1605+104. HD 144515 consists of two SB1 systems (HD 144515 A/B). 
    There appears to be at least moderate activity measured in
    chromospheric lines (see Mullis & Bopp 1994, and references therein).

2RE J1623-391. Vedder et al. (1993) report detection, in an EUVE pointed 
    observation, of both the WD and a much fainter source, about 7 arcmin
    away, identified with the G5V star HR 6094. HR 6094 is also visible in
    the WFC survey data, but is below the catalogue threshold due to
    contamination by counts from the EUV-bright WD. However, the
    reported WFC count rates for the WD are not affected by HR 6094.

2RE J1636+525. Other close-by objects (distance about 100 arcsec): 
    ADS 10129A (= HD 150117, B9 V, Vmag=5.1),
    ADS 10129B (= HD 150118, A1 V, Vmag=6.6).

2RE J1656-390. Other close-by objects: GJ 2123B (M4Ve, Vmag=13), 
    HD 152705 (= CD-38 11340, K4 V, Vmag= 8.5).

2RE J1657+352. Her X-1. Variability in WFC sky-survey observations 
    reported by Rochester et al. (1994).

2RE J1717+102. Spectroscopic binary (SB1), period=0.655 d 
    (Jeffries et al. 1995).

2RE J1737+665. Hottest DA WD in the 2RE Catalogue,Teff= 90000K 
    (Barstow et al. 1994d).

2RE J1738+611. HD 160934 shows a high level of chromospheric activity 
    (Mullis & Bopp 1994).

2RE J1755+361. HD 163621 is an active binary (RS CVn?) system; 
    it is a synchronously rotating system with a period of 3.3 d 
    (Griffin et al. 1994; Mullis & Bopp 1994, and references therein).

2RE J1805+212. Other close-by objects: 
    ADS 11060B (= BD+21 3302B, G8 V,m B= 8:5), 
    ADS 11060C (= BD+21 3302C, K7 V, Vmag=10.6), 
    ADS 11060D (= BD+21 3302D, unclassified, Vmag=9.6), 
    ADS 11060E (= BD+21 3302E, unclassified, Vmag=9.6).

2RE J1809+295. HD 166435 appears to be, at most, mildly active in 
    chromospheric lines (Mason et al. 1995; Mullis & Bopp 1994).

2RE J1816+541. Rapidly rotating, single dM1-2e star (vsini= 61 km/s) 
    (Jeffries, James & Bromage 1994).

2RE J1834+184. HD 171488 has a strong Li line and appears to be 
    very young, with an age less than that of the Pleiades 
    (Mullis & Bopp 1994).

2RE J1844-741. CV, AM Her system (O'Donoghue et al. 1993).

2RE J1846+191. H-alpha in emission, probably single (Jeffries 1995).

2RE J1906+274. Spectroscopic binary (SB2), period=2.73d 
    (Jeffries et al. 1995; see also Mullis & Bopp 1994).

2RE J1925-563. Although the WD is expected to dominate the EUV emission, 
    some contribution from the little-studied, but active, late-type
    companion cannot yet be ruled out (Barstow et al. 1994c).

2RE J1938-461. CV, AM Her system (Buckley et al. 1993).

2RE J2013+400. DAO+dM binary system, period about 0.7d (Barstow et al. 1995a).

2RE J2047-363. Variability in WFC sky-survey observations reported by 
    Matthews et al. (1994). HD 197890 appears to be single, has CaII H/K
    emission and is rapidly rotating (Matthews et al. 1994). Anders et al.
    (1993) report vsini about 170km/s, period=8.04 h. Jeffries (1993) 
    reports detailed H-alpha measurements of `prominence' activity.

2RE J2100+400. Other close-by object: 
    Gl 815B (= Feige 54 = LHS 3609, unclassified, Vmag=12.3).

2RE J2107-051. CV, AM Her system (Hakala et al.  1993).

2RE J2126+192. The WD is expected to dominate the EUV emission 
    (Wonnacott, Kellett & Stickland 1993; Barstow et al. 1993b, 1994c).

2RE J2157-505. Gl 841A is a dM3-5e SB2 binary system with a period of 
    1.124d. The DQ7 common-propermotion companion Gl 841B is too cool to
    contribute to the EUV emission (Jeffries & Bromage 1993).

2RE J2158+825. ADS 15571B (= HD 209943) is an RS CVn binary system, 
    spectral type G5 V, orbital period=1.15 d (Vilhu & Heise 1986; Drake,
    Simon & Linsky 1992). Other close-by object: ADS 15571A (= HD 209942,
    F6 IV- V, Vmag=7.0). Separation A-B = 13 arcsec.

2RE J2158-301. ROSATEUV observations of PKS 2155-304 are discussed 
    by Gondhalekar et al. (1992).

2RE J2220+493. Strong Li 6708 line, probably single (Jeffries 1995; 
    see also Mullis & Bopp 1994).

2RE J2223+322. Wolf 1225 (Gl 856AB) is a visual binary with a separation 
    of about 1 arcsec ( Vmag(A) = 11:4; Vmag(B) = 11:6). It shows a very
    high level of chromospheric activity (Mullis & Bopp 1994).

2RE J2238-203. FK Aqr (= Gl 867A = HD 214479, M2 Ve, Vmag=9.1) and 
    FL Aqr (=Gl 867B, M3 Ve, Vmag=11.5), close pair of dMe flare stars,
    separation about 18 arcsec.

2RE J2300-070. Although the WD is expected to dominate the EUV emission, 
    some contribution from the chromospherically active late-type
    companion cannot be ruled out 
    (Barstow et al. 1994c; Mullis & Bopp 1994).

2RE J2309+475. Other close-by object: ADS 16557A (= HD 218739, G5, Vmag=7.2).

2RE J2353-702. The WD is expected to dominate the EUV emission 
    (Barstow et al. 1993b, 1994c).

Note (*): As used in these notes, the term visual binary (or visual dou-
ble / multiple) is not intended imply that there is necessarily a
physical association.