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Notes for object NGC 3367

15 note(s) found in NED.


1. 2008ApJ...677..926S
Re:NGC 3367
NGC 3367 is an isolated face-on Sc barred galaxy (de Vaucouleurs et al. 1976)
that is optically classified as an H II object. Its optical line ratios place it
well to the left of the Kewley et al. (2001) starburst theoretical-limit line,
as can be seen in Figure 1, indicating that there is no hint of the presence of
an AGN from its optical spectrum. The aperture from which the [Ne v] 14.3 micron
line was detected in this galaxy corresponds to a projected size of ~1 x 2.4
kpc. Although there is no hint of an AGN from optical observations, radio
observations reveal a bipolar synchrotron outflow from a compact unresolved
nucleus (of diameter less than 65 pc) and possibly two large lobes straddling
the nucleus that extend up to ~12 kpc (Garcia-Barreto et al. 1998). There are no
Chandra or XMM-Newton observations of NGC 3367, but it was detected by Einstein
(Fabbiano et al. 1992). The detection of the [Ne v] lines in this work firmly
establishes the existence of a weak AGN in this galaxy. There are no published
observations of the central stellar velocity dispersion in this galaxy.

2. 2002A&A...389...68G
Re:NGC 3367
NGC 3367: the values given by the various methods cover a broad
range of values. Our two methods give the same value for the IA,
which is furthermore in agreement with the value from
Danver (1942). The average of the two values of the PA are in
agreement with the photometry from Grosbol (1985). We thus adopt
the mean of our two methods.

3. 2000ApJ...530..688A
Re:NGC 3367
NGC 3367.-NGC 3367 is of special interest because its optical line
ratios do not correspond to those of an H II region photoionized by hot
stars, or a Seyfert 2 or a LINER (Dekker, D'Odorico, & Arsenault 1988).
The presence of a broad component of H{alpha} is not clear, owing to
important asymmetries (Ho et al. 1997c). In the optical it shows
evidence for the presence of Wolf-Rayet emission features (Ho et al.
1995). This galaxy shows one of the lowest [Fe II] 1.257 micron/Pa{beta}
line ratios in our sample, giving indication for youth of the
star-formation process. The upper limit to the He I/Br10 line ratio sets
an upper limit to the stellar temperature (<40,000 K), which is in good
agreement with the stellar temperature needed in the H II/SNR model to
reproduce its optical line ratios. NGC 3367 is clearly a
starburst-dominated transition object.

4. 1999A&AS..136...35S
Re:NGC 3367
NGC 3367 -- The presence of a broad WR bump in the LINER nucleus has
been signaled by Ho et al. (1995), who also note unusually broad and
asymmetric emission lines (e.g. H{beta}).

5. 1997ApJS..112..391H
Re:NGC 3367
NGC 3367.--This is an Sc galaxy with a prominent nucleus showing emission
features of Wolf-Rayet stars (Paper II). The narrow lines have distinctly
non-Gaussian profiles with obvious blue asymmetry (Fig. 10c). The relatively
wide bases of the narrow lines give the impression that there might be broad
H{alpha}, but this is not confirmed by detailed modeling, which shows that the
[S II] lines have the same profiles.

6. 1997ApJS..108..155G
Re:NGC 3367
A LINER in an SBc host. The nuclear emission is compact; 79 H II regions
are detected in the disk. The brightest H II regions are located in the
outskirts of the disk, at 40" (7 kpc) from the center.

7. 1997A&A...319...52V
Re:NGC 3367
In the spectrum of the nucleus of NGC 3367, the emission lines are strong and
broad (FWHM ~490 km s^-1^ for H{beta}); the line ratios are puzzling
({lambda}5007/H{beta}=0.50, {lambda}6584/H{alpha}=0.87, {lambda}6300/H{alpha}
=0.05) (Veron-Cetty & Veron, 1986b; Dekker et al., 1988; Ho et al., 1995). The
H{alpha}, [NII] complex, observed with a resolution of 180 km s^-1^ can be
very well fitted by two sets of three Gaussian components with 240 and 640
km s^-1^ FWHM respectively (uncorrected for the instrumental broadening),
having the same {lambda}6584/H{alpha} ratio (0.87) (Veron-Cetty & Veron, 1986b).
Further high resolution (160 km s^-1^) observations around H{beta} have shown
that the [OIII] lines probably have the same profile as the [NII] lines, while
H{beta} has a narrow component (185 km s^-1^ FWHM, corrected for the
instrumental profile) which could come from a HII region (Dekker et al., 1988);
the corresponding H{alpha} emission may not have been recognized due to
unsufficient resolution.

8. 1995ApJS...98..477H
Re:NGC 3367
The emission lines of NGC 3367 are unusually broad (FWHM ~ 490 km s^-1^
for H{beta}) and show a blue asymmetry; their intensity ratios suggest a
mixture of an H II region and a LINER (as in NGC 3504 - see below). A
broad emission complex near 4650 A is evident, suggesting the presence of
W-R stars.

9. 1994CAG1..B...0000S
Re:NGC 3367
Hubble Atlas, p. 49
SBc(s)II.2
CD-1731-S
Jan 10/11, 1981
103aO
75 min
NGC 3367 is in the field of the Leo Group
(Ferguson and Sandage 1990) but is judged to be
in the background based on its high redshift of
v_o = 2906 km/s. The mean redshift of the Leo
Group proper is = 909 km/s.
Many bright HII regions are strung along
the inner parts of the two major arms that begin
at the ends of the bar in the (s) configuration
whose prototype is NGC 1300 (SBb; panels 154,
S8). The two major arms fragment after about
half a revolution, creating the multiple-arm
pattern in the outer regions.

10. 1976RC2...C...0000d
Re:NGC 3367
The identification with 4C 14.37 has been rejected.
Photometry:
Publ.Byurakan Obs., No. 40, 15, 1969.
Isodensitometry:
Ap. J. Suppl., 26, No. 230, 1973.
HII Regions:
"Atlas and Catalogue", Univ. Washington, Seattle, 1966.

11. 1973UGC...C...0000N
Re:UGC 05880
SB(rs)c (de Vaucouleurs)
Complex spiral structure, strongly asymmetric, 3 main arms
(rs) 0.9 x 0.6
Appears disturbed by UGC 05899 at 21.5 north-following, but redshift for
UGC 05899 is 4 times larger than for UGC 05880

12. 1964RC1...C...0000d
Re:NGC 3367
Very small, extremely bright nucleus. Narrow bar: 0.5 arcmin x 0.05 arcmin.
(r): 0.55 arcmin x 0.45 arcmin. 3 main knotty filamentary arms. Strongly
asymmetric. Sharp semi-circular outline on side opposite to NGC 3377 at
22 arcmin. See also M.N.R.A.S., 76, 647, 1916.
Projects onto the Leo Group, but its redshift is more than 3 times the mean
redshift of the Leo Group (see Humason et al., 1956).

13. 1961Hubbl.B...0000S
Re:NGC 3367
SBc(sr)
H-2268-H
May 4/5, 1946
103aO
30 min
Enlarged 8.1X
This is basically of the NGC 1300 type, but the arms almost
coalesce to form an internal ring. The arm starting at the
northeast end of the bar winds through about 200 degrees and
then branches. The arm coming from the southwest end
of the bar is not well defined at its beginning. It branches
for the first time after about a 90 degree turn. Other branching
takes place after about 340 degrees. The arm can be traced
through a turn of about 400 degrees.

14. 1957HPh....53..275d
Re:NGC 3367
SB(r)cd
(Plate 28)
The nucleus and bar are smaller and fainter.
The elliptical ring is weaker and begins to break up into knots.
The arms are branching and filamentary.
Note the strong asymmetry.
Compare with NGC 6643 (Plate 24), NGC 2523 (Plate 27),
and NGC 7741 (Plate 31).

15. 1918PLicO..13....9C
Re:NGC 3367
Nearly round; 2' in diameter; a beautiful, rather bright spiral, showing across
its central portion of the band of matter characteristic of the {phi}-type.
Nucleus bright, and stellar. Whorls are rather open and show a few almost
stellar condensations. I can not locate 3371 and 3373 in the positions given.
30 s.n.


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