1 Introduction

We have presented kinematical measurements from absorption spectroscopy on early-type galaxies (Simien & Prugniel 1997a, 1997b, 1997c, 1998: hereafter Papers I to IV, respectively); these data are intended to contribute to the study of several structural and evolutionary issues. As part of our ongoing effort to get reliable velocity dispersions and rotation curves on a statistically significant sample of objects, we presently report on observations on a fifth list of targets.

This work follows closely the technique already described in full detail in Paper I, for both observation and reduction, and only a minimum of explanations will be given here.

   

Table 1: Catalog elements and kinematical results

Object	Type	$\alpha_{1950}$	$\delta_{1950}$	$B_{\rm T}$	-MB	$r_{\rm e}$	$\epsilon$	PA	ref.	cz	$\sigma_0$	$V_{\rm max}$	$r_{\rm max}$
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)	(12)	(13)	(14)
IC 0464	-3	07 07 14.6	+50 13 09	14.94	20.02	7.2	.45	50	3	$4818 \pm 19$	$211 \pm08$	$180 \pm 09$	27
NGC 0194	-5	00 36 44.0	+02 45 42	13.09	21.13	19.7	.05	38	1	$5228 \pm 11$	$232 \pm08$	$48 \pm 13$	20
NGC 0474	-2	01 17 31.7	+03 09 16	12.31	20.06	34.5	.19	21	1	$2317 \pm 08$	$163 \pm05$	$30 \pm 06$	30
NGC 0524	-1	01 22 10.1	+09 16 45	11.46	21.27	36.2	.01	38	3	$2379 \pm 15$	$257 \pm08$	$124 \pm 07$	38
NGC 0680	-5	01 47 01.4	+21 43 22	12.66	20.54	19.2	.10	158	1	$2867 \pm 11$	$214 \pm06$	$108 \pm 07$	34
NGC 0731	-5	01 52 27.6	-09 15 20	13.09	20.68	14.1	.06	150	3	$3832 \pm 09$	$171 \pm05$	$36 \pm 06$	20
NGC 0855	-1	02 11 10.7	+27 38 39	13.53	16.82	13.8	.57	66	2	$595 \pm 09$	$40 \pm16$	$\le 28 \pm 10$	20
NGC 1550	-5	04 17 02.0	+02 17 25	13.22	20.85	13.9	.08	33	1	$3764 \pm 17$	$326 \pm14$	$\ge 30 \pm 20$	18
NGC 1573	-5	04 29 03.2	+73 09 33	12.82	21.63	32.2	.31	30	3	$4225 \pm 20$	$304 \pm18$	$50 \pm 12$	26
NGC 1601	-2	04 29 13.6	-05 09 56	14.73	19.47	9.4	.38	95	2	$4868 \pm 21$	$191 \pm10$	$\ge 193 \pm 20$	19
NGC 1603	-2	04 29 21.7	-05 11 59	14.54	19.67	15.4	.32	40	3	$4972 \pm 14$	$113 \pm07$	$88 \pm 08$	17
NGC 1684	-5	04 50 00.9	-03 11 18	12.82	21.38	25.9	.33	90	3	$4426 \pm 17$	$301 \pm11$	$110 \pm 16$	14
NGC 2314	-5	07 03 53.7	+75 24 28	13.16	20.78	11.9	.12	1	3	$3795 \pm 20$	$293 \pm09$	$164 \pm 18$	20
NGC 2340	-5	07 07 20.4	+50 15 24	12.86	22.11	44.0	.33	80	3	$5902 \pm 11$	$230 \pm09$	$\le 17 \pm 12$	26
NGC 2493	-2	07 57 01.5	+39 58 05	12.93	21.10	24.4	.00	35	3	$3910 \pm 15$	$233 \pm08$	$75 \pm 09$	30
NGC 2577	-5	08 19 46.6	+22 42 50	12.38	20.84	....	.38	105	2	$2057 \pm 11$	$230 \pm08$	$204 \pm 08$	32
NGC 2634	-5	08 42 56.0	+74 09 06	12.88	19.83	26.0	.00	0	3	$2250 \pm 09$	$191 \pm06$	$65 \pm 16$	34
NGC 2636	-5	08 42 58.9	+73 51 15	14.57	18.14	7.3	.00	90	3	$2072 \pm 09$	$59 \pm06$	$28 \pm 09$	12
NGC 2699	-5	08 53 17.6	-02 56 08	13.18	19.27	13.7	.06	45	2	$1846 \pm 09$	$144 \pm04$	$83 \pm 08$	19
NGC 2962	-1	09 38 16.7	+05 23 39	12.64	20.05	39.5	.25	175	3	$1955 \pm 09$	$182 \pm06$	$175 \pm 09$	39
NGC 2970	-5	09 40 32.8	+32 12 20	14.42	17.78	12.2	.22	75	3	$1618 \pm 08$	$43 \pm16$	$\le 22 \pm 09$	11
NGC 3619	0	11 16 28.6	+58 01 59	12.57	19.88	23.2	.22	35	3	$1553 \pm 09$	$168 \pm05$	$65 \pm 07$	26
NGC 3630	-1	11 17 42.1	+03 14 22	12.88	19.39	11.7	.59	42	3	$1485 \pm 09$	$176 \pm06$	$168 \pm 08$	28
NGC 7280	-1	22 24 01.6	+15 53 39	12.93	19.25	18.6	.30	75	3	$1832 \pm 11$	$107 \pm06$	$83 \pm 09$	18
NGC 7612	-1	23 17 12.2	+08 18 08	13.70	19.82	14.3	.50	0	3	$3213 \pm 11$	$182 \pm05$	$214 \pm 10$	28
NGC 7617	-1	23 17 37.1	+07 53 30	14.92	18.66	8.1	.28	29	3	$4094 \pm 17$	$108 \pm13$	$\ge 159 \pm 18$	12

Notes. Col. (2): morphological type from the LEDA database (status: January 17, 2000), coded with -5 for all ellipticals; Cols. (3), (4): coordinates, from Prugniel & Héraudeau (1998: hereafter PH98); Col. (5): $B_{\rm T}$, integrated blue magnitude, corrected for Galactic extinction according the Burstein & Heiles (1982) model, and for k term (from PH98, except for NGC 2577 which is from LEDA); Col. (6): M_B, absolute B magnitude; the distance moduli are computed using the flow-smoothed velocity from Hypercat (Prugniel et al. 1999) corrected for the particular streamings as in Prugniel & Simien (1997), and using $H_0={\rm 75 \, km \, s^{-1} \, Mpc^{-1}}$; except for NGC 2577: M_B from LEDA; Col. (7): $r_{\rm e}$, effective radius in arcsec, corrected for cosmological dimming effect, from PH98; Col. (8): $\epsilon$, ellipticity, derived from parameter R₂₅ in LEDA; Col. (9): PA, position angle of major axis, in degrees (North through East); Col. (10): reference for PA, 1 = Djorgovski (1985), 2 = LEDA, 3 = this work (value determined on an image from the Digitized Sky Survey); Col. (11): cz, heliocentric radial velocity, in kms^-1; Col. (12): $\sigma_0$, central velocity dispersion, in kms^-1; Col. (13): $V_{\rm max}$, maximum rotation velocity, in kms^-1(the $\ge$ sign indicates that the rotation is still rising at the outermost point, or that the PA of the slit was inclined with respect to the major axis); Col. (14): $r_{\rm max}$, the radius defining the range ( $-r_{\rm max}$, $r_{\rm max}$) in which $V_{\rm max}$ was measured, in arcsec.