2002A&A...389..779P


Query : 2002A&A...389..779P

2002A&A...389..779P - Astronomy and Astrophysics, volume 389779-786 (2002/7-3)

The metallicities of UM 151, UM 408 and A 1228+12 revisited.

PUSTILNIK S.A., KNIAZEV A.Y., MASEGOSA J., MARQUEZ I., PRAMSKIJ A.G. and UGRYUMOV A.V.

Abstract (from CDS):

We present the results of new spectrophotometry and heavy element abundance determinations for 3 dwarf galaxies UM 151, UM 408 and A 1228+12 (RMB 132). These galaxies have been claimed in the literature to have very low metallicities, corresponding to log(O/H)+12≤7.65, that are in the metallicity range of some candidate local young galaxies. We present higher S/N data for these three galaxies. UM 151 and UM 408 have significantly larger metallicities: log(O/H)+12=8.5 and 7.93, respectively. For A 1228+12 our new log(O/H)+12=7.73 is close to that recalculated from earlier data (7.68). Thus, the rederived metallicities allow us to remove these objects from the list of galaxies with Z≲1/20Z☉.

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Journal keyword(s): galaxies: dwarf - galaxies: stellar content - galaxies: abundances - galaxies: individual: UM 151 = Mkn 1169, UM 408, A 1228+12 = RMB 132

Simbad objects: 11

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Number of rows : 11
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 Mrk 1169 H2G 01 57 38.9298229056 +02 25 24.542404968   17.0       ~ 27 0
2 LEDA 8377 H2G 02 11 23.38 +02 20 29.7   18       ~ 43 0
3 SBSG 0335-052 AGN 03 37 44.06 -05 02 40.2     16.65     ~ 500 1
4 LGG 103 GrG 03 43 07.8 -04 18 07           ~ 13 0
5 Mrk 116 AGN 09 34 02.1 +55 14 25           ~ 1179 1
6 IC 3105 AG? 12 17 33.750 +12 23 17.15   15.0       ~ 97 0
7 NAME HI 1225+01 HI 12 27 19 +01 30.4           ~ 84 1
8 NGC 4478 GiP 12 30 17.4160005576 +12 19 42.790577160 12.82 12.36 11.45   10.17 ~ 508 1
9 NAME Virgo Cluster ClG 12 30 47.8 +12 23 07           ~ 7107 0
10 RMB 132 bCG 12 30 48.6089418912 +12 02 42.805457196     16.78   16.44 ~ 102 0
11 M 87 AGN 12 30 49.42338414 +12 23 28.0436859 10.16 9.59 8.63   7.49 ~ 7815 3

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