1 Introduction

This is the second of a series of papers aimed at investigating the stellar populations and the dynamics of early-type galaxies in the Coma Cluster. Spanning about 4 dex in density, the Coma cluster is the ideal place to investigate these galaxy properties as a function of the environmental density. In the first paper of the series (Mehlert et al. 2000, hereafter Paper I) we presented the galaxy sample, its selection properties, the photometric observations and the long-slit major axis spectra for 35 E and S0 galaxies of the Coma Cluster. Here we complement the spectroscopic database with minor axis, offset major axis and one diagonal long slit spectra for 10 objects of the sample. The combined dataset allows the construction of dynamical axisymmetric models of the objects, to study the properties of the dark matter halos of flattened, rotating E and S0 galaxies. This study is complementary to the one presented by Gerhard et al. (2001), focusing on round, non-rotating ellipticals.

The properties of the stellar populations of the central regions of Coma cluster galaxies have been investigated in detail by means of long-slit (Davies et al. 1987; Jørgensen et al. 1995; Lucey et al. 1997) and fibre-fed spectrographs (Jørgensen 1999; Mobasher et al. 2001; Poggianti et al. 2001a, b; Komiyama et al. 2002; Carter et al. 2002). The data presented here and in Paper I allow the study of the stellar population gradients for a restricted number of galaxies and the empirical verification of the aperture corrections (Jørgensen et al. 1995). Morover, possible systematic differences between the disk and bulge components of S0 galaxies can be investigated.

The spectroscopic observations and data reduction are described in Sect. 2. We present the derived kinematics in Sect. 3 and the line indices in Sect. 4. Conclusions are drawn in Sect. 5.

   

Table 1: Log of spectroscopic observations.

Object	Run	PA	Position	Offset	Single Exp. Time	Total Exp. Time	Q
		[$^\circ$]		['']	[s]	[h]
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)
GMP 0144	4	1	MN	-	$5\times3600+1776$	5.5	3
GMP 0282	3	135	MN	-	$3\times3600$	3.0	2
GMP 0756	3	88	$\parallel$ MJ	5.8 N	$6\times3600$	6.0	3
	3	178	MN	-	$3\times4200$	3.5	2
GMP 1176	1	78	MJ	-	$3\times1800$	1.5	2
	1	78	$\parallel$ MJ	2.6 N	$5\times3600$	5.0	3
	1	168	MN	-	$4\times3600$	4.0	1
GMP 1750	1	150	MN	-	$3\times3600$	3.0	1
GMP 1990	1	135	$\parallel$ MJ	3.5 N	$6\times3600$	6.0	2
	1-2	45	MN	-	$3\times3600$	3.0	2
GMP 3510	2	79	MN	-	$2\times4200$	2.3	2
GMP 3792	1	127	MJ	-	$3\times1800$	1.5	2
	4	127	MJ	-	$3\times1800$	1.5	3
	1	37	MN	-	$3\times4200$	3.5	1
GMP 3818	3	127	DG	-	$3\times1800$	1.5	3
GMP 5975	4	113	MN	-	$3\times3600$	3.0	3

Column 1: GMP No. from Godwin, Metcalfe & Peach (1983). Column 2: observing run. Column 3: slit position angle measured North through East. Column 4: slit position. MJ = major axis; $\parallel$ MJ = parallel to major axis; MN = minor axis; DG = diagonal axis. Column 5: northward offset of the slit with respect to galaxy center. Column 6: number and exposure time of the single exposures. Column 7: total exposure time. Column 8: estimated quality of the resulting spectrum. 1: very good; 2: good; 3: medium (see Fig. 1).