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Date and Time of the Query: 2019-03-23 T20:03:21 PDT
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Notes for object NGC 3319

12 note(s) found in NED.


1. 2007ApJS..173..538T
Re:NGC 3319
NGC 3319 (Fig. 16.46).-GALEX observations of this SB(rs)cd H II: galaxy,
belonging to the NGC 3198 group of at least 5 optically bright galaxies, show a
highly filled UV disk with prominent spiral arms beginning at the end of the bar
structure. SDSS imaging shows the brightest parts of the spiral arms in the form
of a string of blue clumps with some more diffuse underlying emission at redder
wavelengths. The H I distribution of NGC 3319 was studied by Moore & Gottesman
(1998) using the VLA. They detected a gas-rich companion lying 11' south of NGC
3319 and an H I tail (also to the south), which they postulate was created by an
interaction of the two galaxies.

2. 2002ApJS..143...73E
Re:NGC 3319
NGC 3319.---SBd: No bulge. Nuclear point source embedded in thin HSB
bar. The point source is SW of the bar center. There are a number of
other lumps along the bar. Two-armed, grand-design spiral pattern
emanates from the ends of the bar, but arms are LSB. Arms can be
traced through ~240deg before fading. The knots are mainly in the
outer parts of the arms: The inner disk is quite smooth. The south arm
has many more bright knots than does the north arm.

3. 2002AJ....124..675C
Re:UGC 05789
Diffuse source, too faint for the NVSS.

4. 2002A&A...387..821G
Re:UGC 05789
UGC 5789 (NGC 3319)
This barred galaxy has an asymmetric distribution of H{alpha}
emission, the northern spiral arm and the bar being rather poor
whereas the southern arm exhibits bright HII regions. The rotation
curve is fairly symmetric, slowly climbing with a solid body shape
up to about 2 arcmin from the center, where it reaches a maximum
around 100 km s^-1^. The same behavior can be seen on the WHISP
data. Our better spatial resolution enables one to see a pause in
the climbing part of the curve, at about 40 arcsec from the center,
marking the end of the bar. Martin & Friedly (1997) have studied
the morphology of this bar and concluded that it is young (less
than 1 Gyr).

5. 1997A&A...326..449M
Re:NGC 3319
NGC 3319. The HII region distribution in the bar is almost perfectly symmetric
with respect to the galaxy centre. No misalignment is observed. There appears
to be slight enhancement of SF at both ends of the bar. The central part of the
galaxy is very gas-rich (Hunter & Gottesman 1996). According to Moore &
Gottesman (1996), the HI distribution is asymmetric but the galaxy is isolated
and does not show signs of interaction. There is some indication of a break in
the radial O/H gradient of this galaxy (Zaritsky et al. 1994), suggesting that
the bar may be young (Roy 1996).

6. 1994CAG1..B...0000S
Re:NGC 3319
SBc(s)II.4
PH-7126-S
Jan 31/Feb 1, 1976
103aO + GG385
35 min
NGC 3319 is a highly resolved, nearby
galaxy, in which robust star formation is
occurring in the high-surface-brightness, lumpy bar.
The two spiral arms spring from the ends of the
bar in the (s) configuration of the NGC 1300
(SBb; panels 154, S8) type. The arms are
moderately chaotic; hence the late luminosity
class is shown.
Individual brightest stars are clearly
resolved in the arms, starting at about B = 19,
but more-precise data require photometry and
the separation of stars from the several bright
HII-region candidates using standard methods.
The largest of the HII regions probably
resolve into disks at the 2" level. The redshift of
NGC 3319 is v_o = 776 km/s.

7. 1993A&AS...97..887B
Re:NGC 3319
NGC 3319 has a prominent blue bar but was not detected by IRAS at 60
microns so it is difficult to estimate a dust temperature. We have no
clear CO detection with a noise level of 15 mK in 5.2 km/s channels,
placing an upper limit of about 0.4 K km/s. The combination of optical
blueness and star formation combined with low FIR, CO and 20 cm emission
is difficult to understand. Possibly a galaxy with very little dust and
gas?

8. 1976RC2...C...0000d
Re:NGC 3319
Rotation Curve and Systemic Velocity:
Astr. Ap., 8, 364, 1970.
HII Regions:
"Atlas and Catalogue", Univ. Washington, Seattle, 1966.
Ap. J., 155, 417, 1969.

9. 1973UGC...C...0000N
Re:UGC 05789
SB(rs)cd (de Vaucouleurs), Sc+ (Holmberg)

10. 1973AISAO...8....3K
Re:KIG 0428
Condensations in the arms.

11. 1964RC1...C...0000d
Re:NGC 3319
Very bright, narrow bar: 0.85 arcmin x 0.08 arcmin. 3 main branching,
partially resolved, filamentary arms.

12. 1956AJ.....61...97H
Re:NGC 3319
HMS Note No. 094
Slit on two emission patches [south-west] of central bar.
Larger and brighter of two patches.
HMS Note No. 095
Smaller and fainter of two patches.
HMS Note No. 096
Slit on central bar.
Fairly strong, broad hydrogen absorption lines.
Difference in velocity between bar and patches probably due to rotation.


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