Table 1: Sample of PCEBs with orbital periods $P\protect\la~2$ days, $\mbox{$M_{\rm 1}$ }>\mbox{$M_{\rm sec}$ }$ and a main-sequence secondary star.

Object		 alt. name Sp1 $P_{\rm orb}$ [d] $M_{\rm 1}$  $[M_{\odot}]$ $M_{\rm sec}$  $[M_{\odot}]$ $R_{\rm sec}$  $[R_{\odot}]$ $T_{\rm eff}$ [K] Ref.

RR Cae		 LFT 349 WD 0.304 0.467 0.095 0.189 7000 3,4
EG UMa Case 1 WD 0.668 $0.64\pm0.03$ $0.42\pm0.04$ $0.40^{\%}$ $13~125\pm125$ 5
EC 13471-1258   WD 0.151 $0.77\pm0.04$ $0.58\pm0.05$ 0.42 $14~085\pm100$ 6
BPM 71214   WD 0.201 $0.77\pm0.06$ 0.4 $0.38^{\%}$ $17~200\pm1000$ 4
HR Cam GD 448 WD 0.103 $0.41\pm0.01$ $0.096\pm0.004$ $0.125\pm0.020$ 19 000 7,8
UZ Sex PG 1026+002 WD 0.597 $0.65\pm0.23$ $0.22\pm0.05$ $0.25\pm0.03$ $17~600\pm2000$ 9
              $19~900\pm330$ 10
BPM 6502 LTT 3943 WD 0.337 $0.5\pm0.05$ $0.16\pm0.09$ $0.204^{\%}$ $20~640\pm200$ 11
              $21~380\pm258$ 2
              $20~311\pm532$ 12
HZ 9   WD 0.564 $0.51\pm0.1$ $0.28\pm0.04$ $0.296^{\%}$ $20~000\pm2000$ 13,14,15
              17 400 this work
MS Peg GD 245 WD 0.174 $0.48\pm0.02$ $0.22\pm0.02$ $0.27\pm0.02$ 22 170 16
CC Cet PG 0308+096 WD 0.284 $0.39\pm0.1$ $0.18\pm0.05$ $0.21\pm0.02$ $26~200\pm2000$ 7
HW Vir BD $-07^{\circ}4377$ sdB 0.117 $0.48\pm0.09$ $0.14\pm0.02$ $0.180\pm0.011$ $28~488\pm208 $ 17
HS 0705+6700   sdB 0.096 0.483 0.134 0.186 28 800 18
LM Com Ton 617$^\dag $ WD 0.259 $0.45\pm0.05$ $0.28\pm0.05$ $0.296^{\%}$ 29 300 19
PG 1017-086   sdB 0.073 0.5 0.078+0.005-0.006 $0.085\pm0.04$ 30 300 20
V471 Tau BD $+16^{\circ}516$ WD 0.521 $0.84\pm0.05$ $0.93\pm0.07$ $0.98\pm0.10$ $34~500\pm1000$ 21
NY Vir PG 1336-018 sdB 0.101 0.5 0.15 $0.205\pm0.01$ $33~000\pm3000$ 22
AA Dor LB 3459 sdO 0.262 $0.330\pm0.003$ $0.066\pm0.001$ $0.10\pm0.01^{!}$ $42~000\pm1000$ 23
RE 2013+400   WD 0.706 $0.56\pm0.03$ $0.18\pm0.04$ $0.221^{\%}$ $49~000\pm700$ 24
              $47~800\pm2400$ 25
GK Vir PG 1413+015 WD 0.344 $0.51\pm0.04$ 0.1 0.15 $48~800\pm1200$ 26,27
MT Ser PN A66 41* sdO,PN 0.113 0.6 $0.2\pm0.1$ $0.2\pm0.1$ 50 000 28,29
IN CMa RE J0720-318 WD 1.26 $0.57\pm0.02$ $0.39\pm0.07$ $0.375^{\%}$ $53~000\pm1100$ 22
NN Ser PG 1550+131 WD 0.130 $0.57\pm0.04$ $0.12\pm0.03$ $0.166^{\%}$ $55~000\pm8000$ 30
TW Crv EC 11575-1845 sdO 0.328       $95~000\pm40000$ 31
RE 1016-053   WD 0.789 $0.6\pm0.02$ $0.15\pm0.02$ $0.195^{\%}$ $55~000\pm1000$ 22
              $56~400\pm1200$ 23
UU Sge PN A66 63* sdO,PN 0.465 $0.63\pm0.06$ $0.29\pm0.03$ $0.53\pm0.02$ $87~000\pm13~000$ 32,33,34
              $57~000\pm8000$ 32
V477 Lyr PN A66 46* sdOB,PN 0.472 $0.51\pm0.07$ $0.15\pm0.02$ $0.46\pm0.03$ 60 000 35
PN A66 65 Abell 65 sd?,PN 1.00       80 000 36,37
KV Vel LS 2018 sdO,PN 0.357 $0.63\pm0.03$ $0.25\pm0.06$ $0.402\pm0.005$ $77~000\pm3000$ 38
              90 000 39
HS 1136+6646   WD 1       100 000 40
BE UMa PG 1155+492 sdO,PN 2.291 $0.7\pm0.07$ $0.36\pm0.07$ $0.72\pm0.05$ $105~000\pm5000$ 41,42
Other frequently used designations: *Abell 41, 46 & 63 (to be used with care as the object numbers in Abell 1955 and Abell 1966 are not consistent); $^\dag $PG 1224+309.
! The radius of the secondary is estimated using the mass-radius relation shown by Kudritzki et al. (1982) (their Fig. 8).
$^{\%}$ Radii of the secondary calculated by using the mass-radius relation given by Politano (1996).
References: (1) Bruch (1999), (2) Bragaglia et al. (1995), (3) Bleach et al. (2000), (4) Kawka et al. (2002), (5) Marsh & Duck (1996), (6) Maxted et al. (1998), (7) Saffer et al. (1993), (8) Kepler & Nelan (1993), (9) Kawka et al. (2000), (10) Koester et al. (1979), (11) Stauffer (1987), (12) Lanning & Pesch (1981), (13) Guinan & Sion (1984), (14) Schmidt et al. (1995), (15) Wood & Saffer (1999), (16) Drechsel et al. (2001), (17) Orosz et al. (1999), (18) Maxted et al. (2002), (19) O'Brien et al. (2001), (20) Kilkenny et al. (1998), (21) Rauch (2000), (22) Vennes et al. (1999), (23) Bergeron et al. (1994), (24) Fulbright et al. (1993), (25) Green et al. (1978), (26) Green et al. (1984), (27) Grauer & Bond (1983), (28) Catalan et al. (1994), (29) Chen et al. (1995), (30) Miller et al. (1976), (31) Pollacco & Bell (1993), (32) Bell et al. (1994), (33) Pollacco & Bell (1994), (34) Bond & Livio (1990), (35) Walsh & Walton (1996), (36) Hilditch et al. (1996), (37) Herrero et al. (1990), (38) Sing et al. (2001), (39) Wood et al. (1995), (40) Ferguson et al. (1999).

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