Date and Time of the Query: 2019-05-23 T22:34:29 PDT
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Notes for object NGC 7468

11 note(s) found in NED.

1. 2005A&A...429..115N
Re:MRK 0314
4.1 Mkn 314 (NGC 7468, UGC 12329)
As an iE-classified system, Mkn 314 represents the most common
morphological BCD type (LT86). Optical surface photometry as well as
deep H{alpha} imaging have been presented in C01a and Cairos et al.
(2001b, hereafter C01b). This intrinsically luminous BCD (M_B_=
-18.5) was morphologically selected as a candidate polar-ring galaxy
(Whitmore et al. 1990; van Driel et al. 2001), and was included in
the study of Markarian galaxies with multiple nuclei by Mazzarella &
Boroson (1993). Optical broad-band images by the latter authors
revealed three prominent maxima, roughly arranged along the major
axis of the galaxy (labeled a through c in Fig. 1a). Nordgren et al.
(1995) found that regions a and c, situated at comparable projected
distances (~10.5" or 0.57 kpc and 9.4" or 0.52 kpc, respectively)
from the optically brightest, central source b, show velocity
differences to the latter of 30 +/- 17 and 20 +/- 14 km s^-1^. These
values are of the order of typical H I velocity dispersions in BCDs
(van Zee et al. 1998), and do not provide any strong evidence for
kinematical distortions which might indicate a previous merger event.
Narrow band images reveal that SF activity in the galaxy is
distributed along the northeast-southwest direction, in a bar-like
structure, which extends to about 5 kpc southwest from the nuclear
region (Deeg et al. 1997, C01b). BCDs showing such bar-structures are
relatively frequent (for instance Mkn 370, this paper; Mkn 35, II Zw
71, C01b; II Zw 33, Walter et al. 1997) and are morphologically
classified as "chain starburst" in C01b. The total H{alpha}
luminosity of the galaxy amounts to ~ 6.1 x 10^{40}^ erg s^-1^(C01b,
for the distance adopted here). In the H{alpha} frames, three strong
SF regions are detected, aligned with the central sources detected in
the broad-band frames. The peak of the H{alpha} emission is located
at knot c, whereas b and a are moderate sources.
The morphologies in the optical and in the NIR basically coincide,
though the NIR frames provide a better spatial resolution. Smaller
condensations, surrounding the latter three major sources, were
identified (named d-h in Fig. 1a).
The starburst population is immersed in an extended older population
of stars, which displays elliptical isophotes and red colors (B-R ~ 1,
C01ab). Since the chain of SF sources along the major axis of
Mkn 314 is less prominent in the NIR than in optical wavelengths (cf.
C01b), slight differences in the outer slope of optical and NIR SBPs
of the LSB component are to be expected. In J and H we derive a scale
length of ~1 kpc, somewhat smaller than the optical value (~1.2 kpc,
C01a). NIR SBPs reveal a slight curvature for R^*^ >20" pointing to a
type V SBP; however, the S/N level in this outermost region is too
low to corroborate this conclusion.
A tail structure, formed by several SF knots, departs from the
central regions to the south-west, connecting with an extended source
named "S1" in Fig. 1a. This object, which we detect in all NIR bands,
splits into two compact H II regions on H{alpha} frames (C01b). The
blue optical colors (B-R ~ 0.5 mag; C01b) of S1 are comparable to
those observed in the central part of the BCD (regions a through c,
C01b). From the present data we cannot judge whether S1 is a gaseous
or stellar interloper infalling into Mkn 314: the projected velocity
difference of 30 km s^-1^ (Nordgren et al. 1995) to Mkn 314 is not
unusual for close dwarf companions of BCDs (Noeske et al. 2001a).
Also, Taylor et al. (1994) find from interferometric H I observations
of Mkn 314 little indication for an interaction and describe merely
an "oval distortion" of the gaseous component.

2. 2001ApJS..136..393C
Re:MRK 0314
Mrk 314. - B-R + H{alpha}. In the broadband images, a large knot
stretches along the major axis of the galaxy; in the H{alpha} map, with
better seeing, it is resolved into a chain of smaller knots. Other knots
are visible in the south and present blue colors.

3. 2001ApJS..133..321C
Re:MRK 0314
4.1.24. Mrk 314
This object shows elliptical isophotes surrounding a nucleus which has
been resolved into at least three sources of emission aligned along the
major axis of the galaxy (MB; Nordgren et al. 1995). An extended feature
connected with the galaxy is clearly visible to the south. The small
feature located farther to the southwest may be part of the same structure.
Whitmore et al. (1990) consider this galaxy to be a possible polar-ring
galaxy, with these structures being part of the polar ring.

4. 1997A&A...323..323D
Re:MRK 0314
4. 6. Mkn 314
Mkn 314 (=NGC 7468=UGC 12329=CGCG 453-052=CGCG 2300.5+1620) is considered a
possible polar ring galaxy by Whitmore et al. (1990), with the polar rings
being the outer extensions at the northern and southern end, visible in the
contour lines of the B-band image (Fig. 6). The galaxy has at least two optical
nuclei distributed along a line in the NNE-SSW direction of which only the
northernmost one has significant H{alpha} emission.

5. 1995ApJS...99..461N
Re:MRK 0314
The image of Mrk 314 (MBo93) shows the three sources of Mrk 314 to be
arranged in a line along the major axis of the galaxy. Source a is the
southwestern source while c is the northeastern one with b in the
apparent geometrical center of the galaxy. Velocities derived from
spectra in Figure 22 show that the recessional velocity increases more or
less evenly from c to a. Sources a and c have velocity differences
relative to b of 30 (+/-17) km s^-1^ and 20 (+/- 14) km s^-1^
respectively and are found to lie at almost equal distances from b ( 0.5
kpc for a and 0.4 kpc for c). For all three sources the spectra are very
similar with continua at a level of about 2 x 10^-15^ erg/cm^-2}/A/sec
and very prominent emission lines well above the continua. The
heliocentric velocity of source b places Mrk 314 at a distance of 28 Mpc.

6. 1995A&A...297..643W
Re:NGC 7468
NGC 7468. This galaxy (also Mrk 314) is a very blue, (B-V)^0^_T_ =
0.38, and morphologically peculiar system. It has a high surface
brightness nucleus, which is resolved into three HII region-like
condensations, separated by a few arcseconds (Grimley 1987). The outer
halo is smooth and extended. The optical spectrum has strong emission
lines of HII region-like character but with a low metal abundance. The
O/H ratio indicates an abundance of ~40% of the solar value (Hunter &
Gallagher 1986). We detected a broad, double-peaked CO(J= 1-0) profile.
The velocity width is in excess of 650 km s^-1^, which is much broader
than the HI profile of 158 km s^-1^ (Brinks & Klein 1989). The inferred
H_2_ mass is 2 x 10^8^ M_sun_. The very broad CO profile and the rather
low signal-to-noise of our spectrum make us consider NGC 7468 as a
tentative detection.

7. 1994AJ....107...99R
Re:NGC 7468
C-69 = NGC 7468= UGC 12329. The GB 140' makes a strong detection of
3.6 x 10^9^ M_sun_ of H I in this system. NED lists no other companions
within 20', so this system appears to be quite gas-rich, with an
M_HI_/L_B_ = 0.98.

8. 1985AnTok..202.237T
Re:KUG 2300+163
Jets extend north and south.

9. 1976RC2...C...0000d
Re:NGC 7468
= MRK 0314
Spectrum, Spectrophotometry, and HI 21cm:
Astr. Ap., 41, 61, 1975.
Radio Observations:
P.A.S.P., 86, 649, 1974.

10. 1973UGC...C...0000N
Re:UGC 12329
Very bright central region 0.45 x 0.25
2 thin jets

11. 1971Afz.....7..299M
Re:MRK 0314
Elongated, the major axis is inclined at an angle
of 30 degrees to the declination circle.
The spectrum is very diffuse.

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