The morphological classification as determined by us is indicated in
parentheses next to the galaxy name, with our "chaotic circumnuclear
dust" (C) category now not including those galaxies with obvious dust
lanes (DL). Where the classification has already been made by Martini
et al. (2003), we indicate this with "-mp."
3.35. NGC 5879 (DL)
Figure 17 (top).
Spectra: Faint continua and lines. Also H II regions?
Images: There is a north-south dust lane in the STIS image that is not
present in the NICMOS image.
NGC 5879. - No radio structure was detected on the untapered or the
tapered maps. NVSS detected a 21 mJy source, which hence must arise in
an extended low surface brightness region.
However, we did detect a 292.1 mJy, slightly resolved background
source, about 2' northeast of our target. It shows up only on the POSS
red plate as a noiselike source. We have identified this source as
QSO 1508+5714, at a redshift of 4.301 (Hook et al. 1995). It is in the
WENSS (Rengelink et al. 1997) and in BWE91 (282 mJy) as well as in WB92
(149 mJy). Patnaik et al. (1992) have observed the source with the VLA A
configuration at 8.5 GHz and measured 153 mJy: 1508+5714 must be a
variable flat-spectrum quasar.
April 28/29, 1979
NGC 5879 is later in the Sb morphological
box than either NGC 3675, NGC 2613, or NGC 5005,
shown on this panel, because the recent
star-formation rate in the MAS arms is higher.
The multiple arms are thin but are less regular
than those in luminosity class II Sb galaxies.
Although the redshift is small at v_o = 929 km/s,
the HII regions do not resolve at the 1.5" level.
Such small HII regions are common in galaxies of
this morphological and luminosity class (Sandage
and Tammann 1974a).
IAU Circ. No. 1476, 1954.
Zs.f.Ap., 49, 202, 1961.
SA(rs)bc:? (de Vaucouleurs), Sb+ (Holmberg)
Very small, bright nucleus. Many filamentary, knotty arms. Poorly resolved.
Ap. J., 85, 325, 1937.
H.A.C. 1275, 1954.
P.A.S.P., 72, 104, 1960.