Date and Time of the Query: 2019-05-21 T09:53:08 PDT
Help | Comment | NED Home

Notes for object NGC 3359

15 note(s) found in NED.

1. 2007ApJS..173..538T
Re:NGC 3359
NGC 3359 (Fig. 16.15).-A two-arm SB(rs)c H II galaxy with XUV-disk complexes
distributed in long, wrapping spiral features beginning at the ends of the major
axis where the optical spiral arms cease. The eastern XUV arm is of higher
surface brightness near the inner disk, whereas the western XUV arm is more
prominent at large galactocentric distances. Nevertheless, both UV-bright
complexes in both arms can be seen out to nearly 3 times R_25_. NGC 3359 has
been categorized as an "isolated" galaxy in several studies (Karachentseva 1973;
Varela et al. 2004; Giuricin et al. 2000; Verdes-Montenegro et al. 2005),
although it is known to have a low-mass, LSB object detected in H I (Ball 1986)
and Palomar plates. This object is 15' southwest of the galaxy, beyond the
limits of the multiwavelength images we present. However, our GALEX data do
recover the Ball (1986) LSB object as a resolved FUV-bright clump. The H I
structure of NGC 3359 and this LSB companion has also been studied by Broeils
(1992) and with new WSRT data in van der Hulst & Sancisi (2005, who measure an
H I mass of 1.8 * 10^8^ M_sun_ for the companion). The van der Hulst & Sancisi
observations are sensitive enough to discern a connection between the outer LSB
cloud and NGC 3359's spiral structure, meaning our UV detection of the object
makes NGC 3359 among the most extended UV disks known (relative to optical
size). SDSS observations are sensitive to only the brightest of the XUV

2. 2005MNRAS.360.1201H
Re:NGC 3359
NGC 3359. NGC 3359 is a strongly barred galaxy. Its H II regions have been
studied (Martin & Roy 1995) and catalogued (Rozas, Zurita & Beckman 2000a). The
structure and kinematics of the H I were analysed in detail by Gottesman (1982)
and Ball (1986) showing a clumpy distribution and a low surface density within
the annular zone of strong star formation, which can be explained as due to the
effect of the bar sweeping up gas as it rotates. Analysis of the H{alpha}
velocity map shows a disc with an axisymmetric rotation and also evidence of
strong non-circular motions as confirmed by Rozas et al. (2000b). Analysis of
the H{alpha} residual velocity map (not shown here) shows strong streaming
motions in the spiral arms and a strong gradient of gas in the bar.

3. 2004A&A...415..941E
Re:NGC 3359
NGC 3359: Sempere (1999) and Rozas & Sempere (2000) suggested that this galaxy
might have two decoupled bars, based on attempts to match hydrodynamic
simulations to H I and H{alpha} morphology, and on evidence of isophote twisting
inside the "main" bar in an I-band image. However, analysis of a deep I-band
image from the BARS Project (Lourenso & Beckman 2001) and of the K-band image of
Mollenhoff & Heidt (2001) shows evidence for only one (stellar) bar, with a
radius of ~15-20". The isophote twisting in the I band is absent at K, and is
almost certainly due to dust rather than to an inner bar. (This does not rule
out multiple pattern speeds in the galaxy, however: the two pattern speeds
reported by Rozas & Sempere could be those of the bar and the outer spirals,

4. 2002AJ....124..675C
Re:UGC 05873
Very blobby radio source, flux density includes all nearby NVSS

5. 2002A&A...391...83B
Re:NGC 3359
NGC 3359 (Fig. 9) has enhanced total radio emission from the bar where
star formation is strong as well. The total emission from the southern
spiral arm peaks in star-forming regions, which are best visible at
{lambda}6 cm. Weak polarized emission has been detected in the
interarm regions with field lines parallel to the adjacent optical arm.
No polarized emission has been detected from the bar, possibly due to
insufficient angular resolution and depolarization.

6. 2002A&A...389...68G
Re:NGC 3359
NGC 3359: our methods are not adequate for this galaxy because
a lot of HII regions are located in the bar region. We thus keep
the mean of the kinematical values from the H{alpha} velocity
field from Rozas et al. (2000b) and HI velocity fields from
Gottesman (1982) and Ball (1986).

7. 2001A&A...368...16M
Re:NGC 3359
20. NGC 3359 is a nearly face-on SBc spiral with a fairly weak bar and
practically no bulge. Thus our disk/bulge fit treats the bar as a bulge of
high ellipticity (see the Q_b_ in Table 2) and works still satisfying
(Fig. 4). However, the residuum is asymmetric due to the slightly
banana-shaped light distribution in the bar.

8. 1997A&A...326..449M
Re:NGC 3359
NGC 3359. This is the best example of an H{alpha} bar. A spectacular chain of
HII regions is observed in the southern part of the bar but only one bright
region (the brightest of the whole galaxy) is present in the northern part. A
large apparent misalignment of about 15^deg^ is observed. SF is completely
absent in the galaxy nucleus but seems enhanced at the ends of the bar.
NGC 3359 is an isolated object except for a small HI cloud observed in its
vicinity (Ball 1986) and its bar is moderately gas-rich (Hunter & Gottesman
1996). Martin & Roy (1995) have estimated an age of 400 Myr for the bar.
According to Duval & Monnet (1985) and Ball (1992), there are no ILRs in this

9. 1994CAG1..B...0000S
Re:NGC 3359
Hubble Atlas, p. 49
SBc(s)I.8 pec
Oct 23/24, 1955
103aO + WG2
25 min
HII-region candidates and perhaps
brightest stars are present in the well-developed
but late-type bar in NGC 3359. The thin, multiple
arms are full of HII-region candidates, only
two of which resolve into disks at the 1.5" level.
Individual stars have not yet been distinguished
from the HII regions by standard methods.
The redshift is v_o = 1138 km/s.

10. 1993A&AS...97..887B
Re:NGC 3359
NGC 3359 is reported as detected by SEC and our observations are not

11. 1976RC2...C...0000d
Re:NGC 3359
P.A.S.P., 79, 152, 1967.
Izv. Crimea Obs., 45, 162, 1972.
Photometry (7 Color):
Izv. Crimea Obs. 45, 162, 1972.
IAU Symp. No. 44, 62, 1972.
Rotation Curve:
Systemic Velocity Astr. Ap., 8, 364, 1970.
HII Regions:
"Atlas and Catalogue", Univ. Washington, Seattle, 1966.
Ap. J., 155, 417, 1969.
Bull. A.A.S., 5, 349, 1973.
HI 21cm:
Ap. J., 150, 8, 1967.
Bull. A.A.S., 6, 435, 1974.

12. 1973UGC...C...0000N
Re:UGC 05873
SB(rs)c (de Vaucouleurs), Sc- (Holmberg)

13. 1964RC1...C...0000d
Re:NGC 3359
Small, bright, complex bar with a very small nucleus. Highly resolved.
Faint branching outer arms; one stronger. (r): 1.8 arcmin x 1.1 arcmin in a
lens: 2.2 arcmin x 1.9: arcmin.
P.A.S.P., 61, 124, 1949.
I.A.U. Symp., No. 5, 1958 = Lick Cont., II, No.81, 1958.

14. 1961Hubbl.B...0000S
Re:NGC 3359
Apr. 27/28, 1949
30 min
Enlarged 3.0X
This is of the broken-ring type. There is a high degree of
resolution of both the bar and the arms into knots. This
galaxy was illustrated by Hubble in his article showing
the first pictures from the 200-inch, Publ. A.S.P., 61,
121, 1949.

15. 1956AJ.....61...97H
Re:NGC 3359
HMS Note No. 097
Nucleus in patchy central bar.
Fairly strong hydrogen absorption lines.
HMS Note No. 098
Emission patch near end of bar approximately 30 arcsec
[south] of nucleus.
HMS Note No. 099
Emission patch approximately 10 arcsec [north] of nucleus.
HMS Note No. 100
Emission patch near end of bar approximately 55 arcsec
[north] of nucleus.

Back to NED Home