Table 9: The nature of lines having white dwarf wind profile in AG Peg in symbiotic stars.
Object He II $\lambda $1640 C IV $\lambda $1548 N IV $\lambda $1486 N V $\lambda $1238 Si IV $\lambda $1393 Comment
EG And (tcp) 52 (s, pc) 36   34 B
CH Cyg 42 (s) 730 (pc*)   321 str B
T CrB 573 (pc*) 821 (pc*) 320 788   B
PU Vul   166     982 (pc) B
V1329 Cyg 159 226       b
Z And 113 64 67 114 69 N*
RX Pup 68 128 (s) 118 111 112 N*
HBV475 142 130       N*
R Aqr   112     110 N*
HM Sge 137 111 130 131 110 N*
AG Dra 110 58 41 70 (pc) 56 N*
RW Hya 64 56 55     N
SY Mus 66 67 36 58 39 N
BF Cyg 38 65 (s, pc) 65   69 N
CI Cyg 68 44 53 55 50 N
V1016 Cyg 65 65 51 52 64 N
RR Tel 70 68 39 51 43 N
AX Per 64 52 46 58 58 N
KX Tra 69 50 36 58 54 N
AG Pega 770 (tcp, pc) (tcp) 800 (tcp) B
AG Pegb 66 45   56 36 N
N) All five lines have FWHM less than 70 km s-1.
N*) One, a few or all of the five lines have a FWHM between 120 and 150 km s-1, which is significantly broader than for the majority of lines in their spectra.
b) Two of the five lines are observable in IUE spectra of V1329 Cyg, the widths of those lines are broader than for the stars denoted N* but narrower than 400 km s-1.
B) Very broad lines (FWHM > 400 km s-1) are observed as single lines or as narrow lines superimposed on broad sockets (str).
pc) P cygni profile.
pc*) Inverted P cygni profile.
tcp = Two component profile as the spectral line has a narrow emission component superimposed on the broad white dwarf wind profile.

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