Date and Time of the Query: 2019-05-25 T07:26:50 PDT
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Notes for object NGC 3390

8 note(s) found in NED.

1. 2007MNRAS.378..594P
Re:NGC 3390
There is a nearby, low surface brightness companion, of unknown distance,
visible at (R, z) = (+140 arcsec, -125 arcsec) and another unusually small and
round object at R = + 85 arcsec on the major axis. This galaxy exhibits a quite
unusual appearance. The inner high surface brightness part looks like a normal
edge-on Sb galaxy with a well-defined dust-lane. However, the outer low surface
brightness part shows that the galaxy is embedded in a huge spheroidal envelope
much more like an S0. The galaxy was already classified as an S0-a by Lauberts
(1982) and S0? by Sandage & Tammann (1980), whereas de Vaucouleurs et al. (1991)
and Prugniel & Heraudeau (1998) quote Sb or Sbc. The radial profiles close to
the major axis, similar to other S0 galaxies, decline almost straight into the
noise with only a mild break at R ~= +/-90 arcsec in cuts higher above the
plane. This structure makes it impossible to fit a sharply truncated or broken
exponential model. Even the edge-on profiles show clearly a decrease in the o
uter slope with increasing z (see below).
The face-on-equivalent profile of IC 3390 is reasonably well described as a
Type I (see discussion in main text, Section 4.1). For NGC 3390 we find an
increase in scalelength by a factor of 3.1 between the major axis (steepest) and
a vertical distance of 26 arcsec (flatter) in the inner disc region as expected
from the S0 envelope. A scaleheight of 5.3 arcsec, measured in the I band by de
Grijs (1998), is used in Figs 6 and 7.

2. 2005MNRAS.358..481K
Re:ESO 437- G 062
ESO 437-G62. This lenticular remained undetected in the H i (Paper II) and in
the H{beta} and O iii emission lines (Paper III). Instead, the systemic velocity
was estimated by symmetrizing the stellar velocity curve (Paper I). For the
rotation curve, the function [IMAGE] was adopted, adjusting the parameters such
that the best fit of the stellar kinematics is obtained. This yielded v_max_=
277 +/- 10 km s^[IMAGE]1^, d< 1 arcsec, essentially a flat rotation curve.
Overall, the model yields a good fit. It fails, however, to closely match the
line-of-sight projected stellar velocity in the outermost bins and to reproduce
the h_4_ parameter.

3. 2004MNRAS.351.1247K
Re:ESO 437- G 062
ESO 437-G62. The poor quality of the H I data (Paper III) did not allow
a determination of the systemic velocity. Instead, the dynamical centre
and systemic velocity were determined by symmetrizing the stellar
velocity curve. The observed kinematics may be influenced by dust
attenuation since, unfortunately, the slit was positioned 'on' the dust
lane during the service observing. The h 3 and h 4 curves show
remarkably strong deviations from Gaussianity (Section 5). The stellar
kinematics are highly symmetric with respect to the centre, in contrast
with the optical emission-line kinematics (Bureau & Freeman 1999).

4. 2000MNRAS.313..800D
Re:ESO 437- G 062
Outside the region where its dust lane creates a red feature in its
vertical colour profiles, ESO 437-G62 shows essentially unchanging
colours with increasing height above the plane. The galaxy image looks
very smooth and does not show any evidence for residual extinction
effects (Fig. 2g; T = 3.0).

5. 1994CAG1..B...0000S
Re:NGC 3390
S0_3_(8) or Sb
Feb 20/21, 1979
103aO + GG385
45 min
The internal dust ring with the outside ansae is similar to
features of NGC 5866 and NGC 4710 on this page. The fact that the ring
does not define the rim of the image but stops inside the edge of the
luminous disk suggests that the classification is S0_3_ (because of
the internal dust ring) rather than an Sb on edge, but the Sb
classification is also possible. The central bulge is boxy.

6. 1985SGC...C...0000C
Re:NGC 3390
Plate 515
Overexposed with dark lane, similar to NGC 0891.

7. 1982ESOU..C...0000L
Re:ESO 104543-3116.1
=ESO 437- G 62
absorption lane

8. 1979AJ.....84..472S
Re:NGC 3390
Exactly on edge.
Need better plate to positively decide between Sb or S0a
(i.e., with central dust lane such as NGC 4710 or NGC 5688).

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