Evidence for a warm ISM in the Fornax dEs FCC046 and FCC207

Details Evidence for a warm ISM in the Fornax dEs FCC046 and FCC207 Evidence for a warm ISM in the Fornax dEs FCC046 and FCC207

2002-10-15

arxiv.org/abs/astro-ph/0210346v1

Mon.Not.Roy.Astron.Soc. 339 (2003) 225

Astronomy and Astrophysics

Astrophysics

11 pages, 14 figures, accepted for publication in MNRAS

Scientific paper

10.1046/j.1365-8711.2003.06171.x

We present Halpha+[NII] narrow-band imaging of FCC046 and FCC207, two dES in the Fornax Cluster. B-R and B-I color-maps clearly show signs of dust-absorption in FCC207. FCC046 has a very bright blue nucleus, offset by about 1.1'' with respect to the outer isophotes. Moreover, FCC046 shows a pronounced lopsided shape. The emitting regions differ considerably between the two galaxies. Whereas FCC207 has only one central emission region, FCC046 also contains fainter emission regions. Based on broad-band colours, its disturbed shape and its very bright nucleus, FCC046 is akin to the class of amorphous dwarfs. The central emission regions of both galaxies are resolved and we estimate their diameters at about 60 pc. Their Halpha luminosities can be explained as photo-ionisation by post-AGB stars in an old population. Some of the emission regions in FCC046 are resolved and have diameters of the order of 50-150 pc and H$\alpha$ luminosities of the order of 10^30 W, comparable to supernova remnants or nebulae around Wolf-Rayet stars. Hence, FCC046 is clearly undergoing star-formation while for FCC207 the case is not as clearcut. We estimate the mass of the HII gas in FCC046 at M(HII) = 40-150 Mo. The ionised-gas content of FCC207 is somewhat higher : M(HII) = 60-190 Mo.

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