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Date and Time of the Query: 2019-05-25 T22:16:13 PDT
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Notes for object NGC 3185

10 note(s) found in NED.


1. 2007ApJS..173..538T
Re:NGC 3185
NGC 3185 (Fig. 16.12).-The ultraviolet morphology of this (R)SB(r)a Seyfert 2
galaxy is dominated by a UV-bright, inner ring and a luminous nuclear source.
Outside of this and lying toward the southeast major axis, our GALEX data reveal
a string of blue (FUV - NUV ) clumps qualifying the galaxy as an XUV-disk,
although quite limited in nature. Background galaxies may be confused with some
of this emission. NGC 3185 is a member of the group dominated by NGC 3190. SDSS
imaging also shows the SF disk in the main disk, but does not detect the XUV
clumps.

2. 2002A&A...392..817F
Re:NGC 3185
3.2 NGC 3185
This source is the farthest in our sample, and inside its small
angular size (D_25_=2.34'), we find one clear ULX, for which the
low statistics do not allow a spectral fit. No clear optical
counterpart is visible in the DSS.

3. 2001ApJS..133...77H
Re:NGC 3185
NGC 3185 (S2:). - Marginally detected at 6 cm but not at 20 cm. Hummel
et al (1987) quote an uncertain detection of 0.7 mJy at 20 cm
({DELTA}{theta} = 1.3"), considerably stronger than our upper limit of
0.16 mJy at a similar resolution.

4. 1999A&AS..135..437G
Re:NGC 3185
NGC 3185 is a SBa galaxy (Sandage & Bedke 1994). Its emission-line
spectrum is power-law photoionized according to Stauffer (1982). Ho et
al. (1997a) called it a Seyfert 2, although the published line ratios
indicate a "transition" spectrum. We have fitted the lines with two sets
of Gaussian profiles: one system is a H II region; the other corresponds
to a Seyfert nebulosity, although the [O I] lines are quite weak
({lambda}6300/H{alpha} = 0.04).

5. 1997ApJS..108..155G
Re:NGC 3185
An S1 nucleus in an SBA galaxy. The disk shows a ring of H II regions at
35" (2.7 kpc) from the nucleus. The nuclear emission might be extended
6" in the direction of the stellar bar.

6. 1994CAG1..B...0000S
Re:NGC 3185
Hubble Atlas, p. 43
SBa(s)
(Ring type, 1/2)
PH-685-S
Feb 9/10, 1954
103aO + WG2
30 min
NGC 3185 is in a group with NGC 3187 (Sc pec, encounter; v_o =
1500 km/s; separation 11.4'; panel 276), NGC 3190 (Sa; v_o = 1384
km/s; separation 10.9'; panel 76), and NGC 3193 (E2; v_o = 1307 km/s;
separation 16.6'; panel 5).
The morphology of the external regions of NGC 3185, described in
the Hubble Atlas (p. 43), is similar to that described for NGC 3081,
above. The two separate spiral arms nearly overlap to form an apparent
ring if seen on low-resolution plates. This pattern is seen to better
advantage here than in the tighter pattern of NGC 3081 above.

7. 1976RC2...C...0000d
Re:NGC 3185
In the NGC 3190 Group.
Radio Observations:
Austral. J. Phys., 19, 565, 883, 1966.

8. 1973UGC...C...0000N
Re:UGC 05554
(R)SB(r)a (de Vaucouleurs), Sa (Holmberg)

9. 1964RC1...C...0000d
Re:NGC 3185
Small, very bright nucleus. Knotty (r): 1.3 arcmin x 0.75 arcmin in a lens:
1.6 arcmin x 1.0 arcmin. Weak outer arms form (R): 2.5 arcmin x 1.8 arcmin.
In the NGC 3190 Group.
Heidelberg Veroff. Vol. 9, 1926, Lund 9 and HA 88, 4 dimensions are for
the lens only.
Photograph:
P.A.S.P., 59, 161, 1947.

10. 1961Hubbl.B...0000S
Re:NGC 3185
SBa(s)
PH-685-S
Feb. 9/10, 1954
103aO + WG2
30 min
Enlarged 5.9X
At first glance this galaxy appears to have a complete external
ring. The bar seems to terminate on the ring, but close
inspection shows that the "ring" is composed of two closely
coiled spiral arms. Each arm can be traced from its starting
place at the end of the bar, through 180 degrees, until it
passes near and almost joins the opposite end of the bar.
Each arm passes beyond the opposite end of the bar and
can be traced on the outside of the beginning of the other
arm. This closely coiled spiral pattern of nearly overlapping
arms is repeated in other galaxies such as NGC 2217(left) and
NGC 3081 (Sa, pg. 11 of the Hubble Atlas).
A very faint external elliptical ring or possibly spiral
arm system is visible on the original plate. It has a
semi-major diameter of about 70 sec of arc, which is about 35mm
on the scale of the iilustration. It is difficult to trace,
but the major axis of the ring appears to have the same
orientation as the major axis of the arm system.


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