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Nearby Early-Type Galaxies with Ionized Gas. II. Line-Strength Indices

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Nearby Early-Type Galaxies with Ionized Gas. II. Line-Strength Indices Astronomy & Astrophysics manuscript no. paper April 23, 2017 (DOI: will be inserted by hand later) Nearby early–type galaxies with ionized gas.II. Line-strength indices for 18 additional galaxies⋆ Annibali F.1, Bressan A.1,2, Rampazzo R.2, Zeilinger W.W.3 1 SISSA, via Beirut 4 - 34014 Trieste - Italy 2 INAF - Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, 35122 Padova, Italy 3Institut f¨ur Astronomie der Universit¨at Wien, T¨urkenschanzstraße 17, A-1180 Wien, Austria Received date; accepted date Abstract. Rampazzo et al. 2005 (hereafter Paper I) presented a data-set of line-strength indices for 50 early-type galaxies in the nearby Universe. The galaxy sample is biased toward galaxies showing emission lines, located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. The present addendum to Paper I enlarges the above data-set of line-strength indices by analyzing 18 additional early-type galaxies (three galaxies, namely NGC 3607, NGC 5077 and NGC 5898 have been already presented in the previous set). As in Paper I, we measured 25 line–strength indices, defined by the Lick IDS “standard” system (Trager et al. 1998; Worthey & Ottaviani 1997), for 7 luminosity weighted apertures and 4 gradients of each galaxy. This addendum presents the line-strength data-set and compares it with the available data in the literature. Key words. Galaxies: elliptical and lenticular, cD – Galaxies: fundamental parameters – Galaxies: formation – Galaxies: evolution 1. Introduction lution with time (see e.g. Buzzoni et al. 1992; Worthey 1992; Gonz´alez 1993; Buzzoni et al. 1994; Worthey et al. The aim of our study is to improve the understanding 1994; Leonardi & Rose 1996; Worthey & Ottaviani 1997; of the nature of the ionized gas in early-type galaxies by Trager et al. 1998; Longhetti et al. 1998a; Vazdekis 1999; studying its physical conditions, the possible ionization arXiv:astro-ph/0508520v1 24 Aug 2005 Longhetti et al. 1999; Longhetti et al. 2000; Trager et al. mechanisms, relations with the other gas components of 2000; Kuntschner 2000; Beuing et al. 2002; Kuntschner et the Inter Stellar Medium (ISM) and the connection with al. 2002; Thomas et al. 2003; Mehlert et al. 2003) . the stellar population of the host galaxy. By investigating issues such as the evolution of stellar populations and the This addendum intends to enlarge the sample of the ISM, we will both explore the complex, evolving ecosys- early-type galaxies analyzed in Paper I providing the data- tem within early–type galaxies and build a database of set of line–strength indices for 18 objects. Three galax- well studied galaxies to be used as a reference set for the ies, namely NGC 3607, NGC 5077 and NGC 5898 have study of intermediate and distant objects. Our target is to been already presented in the previous set and are used characterize the stellar populations, with particular con- in this paper in order to check the internal consistency cern for those in the extended emission regions, through of our results on repeated observations. Eight galaxies the modelling of the complete (lines and continuum) spec- in the present sample, namely NGC 3818, NGC 4374, trum characteristics. This will allow us to constrain the NGC 4697, NGC 5044, NGC 5638, NGC 5812, NGC 5813 galaxy formation/evolution history. and NGC 5831, belong to the Trager et al. 1998 sample, six of which to the original Gonz´alez 1993 sample. The adopted strategy, described in Rampazzo et al. 2005 (hereafter Paper I), consists in investigating the This note is organized as follows. Section 2 presents the galaxy underlying stellar populations and the emission characteristics of the sample of the 18 galaxies. Sections 3 line properties at different galactocentric distances. The and 4 summarize the observations, the reduction proce- study of stellar populations in early-type galaxies is of fun- dure, the line-strength index measurements at different damental importance to the understanding of their evo- galactocentric distances and the corrections applied to conform the indices to the Lick IDS system. Finally in Send offprint requests to: F. Annibali Section 5 we present the results and the comparison with Correspondence to: [email protected] the literature. 2 Annibali et al.: Nearby early–type galaxies with ionized gas.I Addendum. Fig. 1. Distribution of B-magnitudes (top left panel), morphological types (top right panel), heliocentric velocity (bottom left panel) and galaxy density (bottom right panel) for the total sample (50 galaxies of Paper I + 15 new galaxies of this paper). 2. Characterization of the sample a combination of active galactic nuclei and star formation regions within the galaxies. Table 1 summarizes the ba- As the original sample of 50 early–type galaxies presented sic characteristics of the galaxies available from the lit- in Paper I, this sample of 18 galaxies is selected from a erature. Column (1) provides the identification; columns compilation of galaxies showing ISM traces in at least one (2) and (3) the R.A. & Dec. coordinates; columns (4) of the following bands: IRAS 100 µm, X-ray, radio, HI and and (5) the galaxy morphological classifications accord- CO (Roberts et al. 1991). All galaxies belong to Revised ing to the RSA (Sandage & Tamman 1987) and RC3 (de Shapley Ames Catalog of Bright Galaxies (RSA) (Sandage Vaucouleurs et al. 1991) respectively. Columns (6), (7), (8) & Tammann 1987) and have a redshift of less than 5500 and (9) give the position angle of the isophotes along the km s−1. The sample should then be biased towards ob- major axis, the total corrected magnitude and the total jects that might be expected to have ongoing and recent (B-V) and (U-B) corrected colors from RC3 respectively. star formation, at least in small amounts, because of the The heliocentric systemic velocity from HYPERCAT presence of emission lines. The emission should come from (http://www-obs.univ-lyon1.fr/hypercat) is reported Annibali et al.: Nearby early–type galaxies with ionized gas.IAddendum. 3 Table 1 Overview of the observed sample ident R.A. (2000) Dec. RSA RC3 P.A. B0 (B-V)0 (U-B)0 Vhel re ρxyz ǫ NGC 3607 11 16 54.3 18 03 10 S03(3) SA(s)0: 120 11.08 0.88 0.43 934 43.4 0.34 0.11 NGC 3818 11 41 57.3 -06 09 20 E5 E5 103 12.47 0.91 1701 22.2 0.20 0.36 NGC 4374 12 25 03.7 12 53 13 E1 E1 135 10.01 0.94 0.50 1060 50.9 3.99 0.11 NGC 4696 12 48 49.3 -41 18 40 (E3) E+1 pec 95 10.85 2958 85.0 0.00 0.34 NGC 4697 12 48 35.9 -05 48 03 E6 E6 70 10.07 0.89 0.39 1241 72.0 0.60 0.32 NGC 5011 13 12 51.8 -43 05 46 E2 E1-2 154 11.90 0.89 3104 23.8 0.27 0.15 NGC 5044 13 15 24.0 -16 23 08 E0 E0 11 11.67 2704 82.3 0.38 0.11 NGC 5077 13 19 31.6 -12 39 26 S01/2(4) E3+ 11 12.52 0.98 0.54 2764 22.8 0.23 0.15 NGC 5090 13 21 12.8 -43 42 16 E2 E2 136 11.97 3421 62.4 0.15 NGC 5193 13 31 53.5 -33 14 04 S01(0) E pec 71 12.35 0.86 3711 26.7 0.07 NGC 5266 13 43 02.1 -48 10 10 S03(5) pec SA0-: 109 11.50 3074 76.7 0.35 0.31 NGC 5638 14 29 40.4 03 14 00 E1 E1 150 12.06 0.91 0.46 1676 28.0 0.79 0.11 NGC 5812 15 00 55.7 -07 27 26 E0 E0 130 11.83 0.94 1930 25.5 0.19 0.13 NGC 5813 15 01 11.2 01 42 07 E1 E1-2 145 11.42 0.94 0.52 1972 57.2 0.88 0.28 NGC 5831 15 04 07.0 01 13 12 E4 E3 55 12.31 0.92 0.55 1656 25.5 0.83 0.13 NGC 5898 15 18 13.6 -24 05 51 S02/3(0) E0 30 12.41 0.95 2267 22.2 0.23 0.07 NGC 6758 19 13 52.3 -56 18 36 E2 (merger) E+: 121 12.31 0.96 0.44 3404 20.3 0.22 NGC 6776 19 25 19.1 -63 51 37 E1 pec E+ pec 15 12.71 0.86 0.44 5480 17.7 0.17 Notes: The value of re of NGC 4696, NGC 5090 and NGC 5266 have been derived from ESO-LV (Lauberts & Valentijn (1989) while the value for NGC 5044 is derived from Goudfrooij (1994) . in column (10). The effective radius, derived from Ae, the its possible origin. Information for NGC 3607, NGC 5077 diameter of the effective aperture from RC3, is given in and NGC 5898 are given in Paper I. column (11). A measure of the richness of the environ- Several classes of galaxies are present in this addi- −3 ment, ρxyz (galaxies Mpc ), surrounding each galaxy tional sample: interacting or post-interacting galaxies, is reported in column (12) (Tully 1988). Column (13) galaxies showing evidence of kinematical decoupling be- lists the average ellipticity of the galaxy as obtained from tween galaxy sub-components, elliptical galaxies with a HYPERCAT. dust lane along the minor axis, radio galaxies and galax- ies hosting an AGN nucleus.
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