Table 3: Summary of projected rotational velocities (1 $\sigma$ detection limit) and stellar parameters of all stars from this paper and Papers I and II.
WD $T_{{\rm eff}}$ $\log g$ $v_0 \sin i$ $v_{\rm max}\sin i$ Ref. WD $T_{{\rm eff}}$ $\log g$ $v_0 \sin i$ $v_{\rm max}\sin i$ Ref.

1710+683 6825 7.94 72 ⁺¹¹_-10 III 1919+145 14 600 8.09 <6 II

0807+484 7000 8.01 <18 III 0352+096 14 770 8.16 <13 I

2253-081 7160 8.43 36 ⁺¹⁵_-7 III 2007-303 15 150 7.86 <7 II

0251-008 7700 8.05 24 ⁺⁴_-5 III 0406+169 15 190 8.30 <20 I

1953-011 7950 8.41 $173\pm10^b$ II 0810+234 15 220 7.99 <16 III

2359-434^d,e 8850 8.57 <20 II 1143+321 15 489 7.97 <2 I

0518+333^f 9140 8.30 <7 III 0310-688 15 700 8.16 <4 II

1510+566 9280 7.98 <11 III 0220+222 15 840 7.95 <9 III

2258+406 9860 8.20 20 ⁺⁶_-5 III 2039-682 16 050 8.44 $78\pm6$ ^b II

2115-560 9950 8.13 <35 II $82\pm5$ M&M

0906+296 10 000 7.86 41 ⁺⁶_-5 III 0413-077 16 570 7.86 <1 I

2007-219^d 10 000 8.18 <20 II 0836+201 16 630 8.04 $66\pm14$ III

1840-111^d 10 230 8.18 <20 II 0837+199 17 100 8.32 <9 I

1147+255 10 260 8.12 $24\pm{7}$ III 2149+021 17 650 7.99 $16\pm5$ <21 II

0030+444 10 440 8.02 27 ⁺⁵_-4 III 0047-524 18 750 7.83 $1\pm11$ <12 II

2105-820 10 760 8.25 $65\pm5^b$ II 1211+392 18 800 7.70 <18 III

1544-377^d 11 250 8.09 <20 II 1531-022 18 850 8.39 $50\pm6$ ^b II

2326+049^a 11 600 8.05 $45\pm5$ II 2039-202 19 350 7.95 <15 II

1422+095^a 11 950 7.87 $29\pm7$ II 1943+163 19 400 7.80 $16\pm8$ <24 II

1240+754 12 000 7.96 30 ⁺⁷_-10 III 0421+162 19 570 8.09 <8 I

1425-811^a 12 200 7.99 $38\pm3$ II 2032+248 19 900 7.87 $11\pm5$ <16 II

0921+354^a 12 830 7.92 36 ⁺⁷_-5 III 0431+125 21 340 8.04 15 ⁺⁷_-5 I

0726+393 13 600 7.76 <7 I 0836+197 21 900 8.45 <22 I

1706+332 13 600 7.79 23 ⁺³_-4 III 1620-391 24 250 8.05 <8 II

1716+020 13 620 7.79 <11 III 0425+168 24 420 8.11 <18 I

1827-106 13 800 7.61 <20 II 2014-575 26 850 7.80 <14 II

1743-132 13 950 7.71 28 ⁺³_-4^c III 0438+108 27 390 8.07 <14 I

1911+135 14 040 7.83 <2 I 1615-154 29 600 7.95 <13 II

1314+293 49 000 7.70 <11 I

Paper I: Heber et al. (1997). ^b broadening probably caused by a magnetic field.

Paper II: Koester et al. (1998). ^c $v \sin i = 13$ km s^-1 (Paper II).

Paper III: this Paper. ^d poor fit (see Paper II).

M&M: Maxted & Marsh (1999). ^e possibly magnetic.

^a Known ZZ Ceti variable star. ^f probably binary.

**Table 3:** Summary of projected rotational velocities (1 $\sigma$ detection limit) and stellar parameters of all stars from this paper and Papers I and II.
WD	$T_{{\rm eff}}$	$\log g$	$v_0 \sin i$	$v_{\rm max}\sin i$	Ref.	WD	$T_{{\rm eff}}$	$\log g$	$v_0 \sin i$	$v_{\rm max}\sin i$	Ref.
1710+683	6825	7.94	72 ⁺¹¹_-10		III	1919+145	14 600	8.09		<6	II
0807+484	7000	8.01		<18	III	0352+096	14 770	8.16		<13	I
2253-081	7160	8.43	36 ⁺¹⁵_-7		III	2007-303	15 150	7.86		<7	II
0251-008	7700	8.05	24 ⁺⁴_-5		III	0406+169	15 190	8.30		<20	I
1953-011	7950	8.41	$173\pm10^b$		II	0810+234	15 220	7.99		<16	III
2359-434^d,e	8850	8.57		<20	II	1143+321	15 489	7.97		<2	I
0518+333^f	9140	8.30		<7	III	0310-688	15 700	8.16		<4	II
1510+566	9280	7.98		<11	III	0220+222	15 840	7.95		<9	III
2258+406	9860	8.20	20 ⁺⁶_-5		III	2039-682	16 050	8.44	$78\pm6$ ^b		II
2115-560	9950	8.13		<35	II				$82\pm5$		M&M
0906+296	10 000	7.86	41 ⁺⁶_-5		III	0413-077	16 570	7.86		<1	I
2007-219^d	10 000	8.18		<20	II	0836+201	16 630	8.04	$66\pm14$		III
1840-111^d	10 230	8.18		<20	II	0837+199	17 100	8.32		<9	I
1147+255	10 260	8.12	$24\pm{7}$		III	2149+021	17 650	7.99	$16\pm5$	<21	II
0030+444	10 440	8.02	27 ⁺⁵_-4		III	0047-524	18 750	7.83	$1\pm11$	<12	II
2105-820	10 760	8.25	$65\pm5^b$		II	1211+392	18 800	7.70		<18	III
1544-377^d	11 250	8.09		<20	II	1531-022	18 850	8.39	$50\pm6$ ^b		II
2326+049^a	11 600	8.05	$45\pm5$		II	2039-202	19 350	7.95		<15	II
1422+095^a	11 950	7.87	$29\pm7$		II	1943+163	19 400	7.80	$16\pm8$	<24	II
1240+754	12 000	7.96	30 ⁺⁷_-10		III	0421+162	19 570	8.09		<8	I
1425-811^a	12 200	7.99	$38\pm3$		II	2032+248	19 900	7.87	$11\pm5$	<16	II
0921+354^a	12 830	7.92	36 ⁺⁷_-5		III	0431+125	21 340	8.04	15 ⁺⁷_-5		I
0726+393	13 600	7.76		<7	I	0836+197	21 900	8.45		<22	I
1706+332	13 600	7.79	23 ⁺³_-4		III	1620-391	24 250	8.05		<8	II
1716+020	13 620	7.79		<11	III	0425+168	24 420	8.11		<18	I
1827-106	13 800	7.61		<20	II	2014-575	26 850	7.80		<14	II
1743-132	13 950	7.71	28 ⁺³_-4^c		III	0438+108	27 390	8.07		<14	I
1911+135	14 040	7.83		<2	I	1615-154	29 600	7.95		<13	II
						1314+293	49 000	7.70		<11	I
Paper I: Heber et al. (1997).	^b broadening probably caused by a magnetic field.
Paper II: Koester et al. (1998).	^c $v \sin i = 13$ km s^-1 (Paper II).
Paper III: this Paper.	^d poor fit (see Paper II).
M&M: Maxted & Marsh (1999).	^e possibly magnetic.
^a Known ZZ Ceti variable star.	^f probably binary.

Source LaTeX | All tables | In the text

	1 Introduction
	2 Atmospheric parameters and stellar masses
	3 Model atmospheres and spectral analysis
	4 Projected rotational velocities
	5 Discussion
	References