NGC 533 was studied by Piffaretti et al. (2005; XMM-Newton) and G07 (Chandra +
XMM-Newton). The explored radial range in spectral analysis is similar in all
three work (up to 240-260 kpc). Our temperature profile agrees well with that
derived by G07. Our c_500_ (4.58^+3.90^_-2.34_) is still consistent with the
results by Piffaretti et al. (2005; 8.6 +/- 0.7) and G07 (9.0 +/- 0.7).
NGC 533. - We detect no features in this galaxy.
This galaxy has a filamentary dust distribution. Its morphology and
distribution corresponds to that of the ionized gas.
3.1. NGC 533
Fig. 1 shows an emission distribution in the central part of NGC 533 with minor
deviations from radial symmetry. The emission is clearly peaked in the central
area, with some more low surface brightness emission around it. The ROSAT PSPC
observations by Trinchieri et al. (1997; hereafter TFK97) indicate that this
emission is part of a more extended envelope.
Sep 2/3, 1980
103aD + GG11
NGC 533 is the brightest galaxy in an apparently associated group
of E and S0 galaxies. Many candidate dE dwarf ellipticals exist over
a field of radius < 15' surrounding NGC 533.
NGC 533 forms a pair with NGC 521 (SBc; panel 293) at 14.6'
separation. The redshifts are similar, at v_o(533) = 5664 km/s and
v_o(521) = 5223 km/s. At the mean redshift distance of 109 Mpc (H =
50), the projected linear separation is 460 kpc, similar to distances
within the Local Group.
The pair is 3 deg north of the Abell cluster A194, whose
brightest member is NGC 545 (radio source 3C 40) at a similar mean
redshift of 5400 km/s (Sandage 1972 for the cluster photometry). The
similarity of the redshifts of the NGC 533/521 pair with that of the
cluster A194 at a projected separation of 6 Mpc suggests that the
region is part of a larger complex at a mean redshift of about 5500
E3 (de Vaucouleurs)
See UGC 00962
Many small galaxies near, 10 inside 5.0
Non-interacting pair with NGC 0521 at 14.5 arcmin.
Radio Source: (possible identification)
Austral. J. Phys., 11, 360, 1958.