Date and Time of the Query: 2019-06-18 T03:44:31 PDT
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Notes for object NGC 3190

8 note(s) found in NED.

1. 2008MNRAS.385..553D
Re:NGC 3190
NGC 3190: This early-type galaxy has very little H{alpha}. A close
companion lies just 5 arcsec north-west and both galaxies are in
interaction. No kinematical parameters are given for this peculiar

2. 2005A&A...442..137N
Re:UGC 05559
UGC 5559 (NGC 3190) is part of Hickson compact group of galaxies 44, together
with UGC 5554, 5556 and 5562 (Hickson et al. 1989). All group members lie in our
field of view, but the observations for these galaxies were done with the "old"
Westerbork receivers and the sensitivity is insufficient to detect any emission
in UGC 5554 and 5562. UGC 5559 itself is only barely detected, and the
signal-to-noise ratio of the data is too low to make a detailed study of the gas
distribution in this galaxy. Only for the more gas-rich, late-type spiral UGC
5556 useful H I surface density maps and velocity fields could be obtained, but
as this galaxy does not meet our selection criteria, it is not discussed here

3. 1997ApJS..112..391H
Re:NGC 3190
NGC 3190.--The narrow lines are unusually broad (FWHM~500 km s^-1^) and have a
clear red asymmetry, but there is no evidence for a broad component of H{alpha}
(Fig. 9h). The H{alpha} line has a noticeably smaller width than [N II], most
likely resulting from imperfect starlight subtraction.

4. 1994CAG1..B...0000S
Re:NGC 3190
April 12/13, 1950
30 min
NGC 3190 is a member of a group of diverse
galaxy types having similar redshifts, composed
of NGC 3185 (SBa; panel 99), NGC 3187
(Sc/SBc; panel 276), NGC 3190 (Sa; this panel),
and NGC 3193 (E2; panel 5), with a mean
redshift of = 1196 km/s (Humason,
Mayall, and Sandage 1956).
The major dust lane in NGC 3190 cuts
nearly centrally across the bulge, which can be
seen also below the dust lane on this print. A
thinner double dust lane is seen on the left of the
bulge center; the double lane appears to be tilted
relative to the main plane.
The galaxy forms a close pair with NGC
3187, which itself is a distorted Sc with two
oppositely directed features that may be tidal
plumes (panel 276). The result of this interaction
may have distorted the dust plane in NGC 3190
The projected separation of NGC 3187 and
NGC 3190 is 300", which at the redshift
distance of 24 Mpc (H = 50) is a projected linear
separation of 35 kpc. At this small distance,
there of course is a good case for tidal distortion.
NGC 3190 shows little or no sign of HII
regions either in the bulge or the disk. The type
is not S0, Sb, or Sc. By elimination, the type,
therefore, is Sa.

5. 1976RC2...C...0000d
Re:NGC 3190
= Arp 316
= VV 307
= Holm 175a
Brightest of group.
Interacting pair with NGC 3187 at 4.8 arcmin.
Interacting pair with NGC 3193 at 5.5 arcmin.
Rotation Curve and Systemic Velocity:
Astr. Ap., 8, 364, 1970.

6. 1973UGC...C...0000N
Re:UGC 05559
VV 307a, Arp 316b
SA(s)a pec (de Vaucouleurs), Sa (Holmberg)
See UGC 05556
"Edge-on spiral shows sign of interaction" (Arp)

7. 1964RC1...C...0000d
Re:NGC 3190
= Holm 175a
Large, bright central bulge: 1.3 arcmin x 0.5 arcmin. Strong dark lane
with outer arms tilted to principal plane.
NGC 3189 is part of this galaxy.
Brightest in a group.
Interacting pair with NGC 3187 at 4.8 arcmin.
Ap. J., 97, 114, 1943.
Ap. J., 104, 219, 1946.
P.A.S.P., 59, 161, 1947.
Orientation and Rotation,
Ap. J., 97, 117, 1943.
Ap. J., 127, 487, 1958.

8. 1959VV....C...0000V
Re:VV 307a
= NGC 3190
V = +1,220 km/sec; V = +1,284 km/sec.
Yerkes Type: gkS4

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