Date and Time of the Query: 2019-02-20 T05:08:17 PST
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Notes for object NGC 7625

14 note(s) found in NED.

1. 2001ApJS..136..393C
Re:III Zw 102
III Zw 102. - B-V + H{alpha}. This galaxy has quite a spectacular
appearance. The H{alpha} emission is concentrated in the central region,
which is resolved into numerous individual knots. There are plenty of
holes, loops, and filamentary structures. Especially interesting are the
large curvilinear structures, which depart from the main body of the galaxy
and extend to ~4 kpc from the center, with a striking similarity to the
famous Antennae galaxy. These structures can be interpreted as signs of
recent interaction. The color maps show that the northern half is bluer
than the other, possibly because it is less obscured by dust. A strong
dust lane is clearly visible.

2. 2001ApJS..133..321C
Re:III Zw 102
4.1.26. III Zw 102
This is quite an interesting object. It shows regular external isophotes
but a very clumpy morphology in its inner parts, which could be explained
by the presence of strong dust lanes. Whitmore et al. (1990) considered
III Zw 102 to be "related to polar-ring galaxies." Brosch & Loinger (1991)
remarked that this galaxy does not qualify as a dwarf and attributed its
classification as a BCD to the fact that it was included in TM list.

3. 2000ApJS..131..413Z
Re:NGC 7625
5.2.18. NGC 7625
NGC 7625 is a type Sa/S pec galaxy with a comparatively modest
luminosity. Unlike most early-type galaxies, it happens to have a great
deal of gas and dust associated with it and a large star formation rate
(Li et al. 1993). A dust lane is conspicuous in the DSS image (Fig. 19).
The optical size of the galaxy extends to 1.5' x 1.5' (Nilson 1973), but
comparisons of the sizes of the blue light, the CO, the H{alpha}, and the
20 cm-emitting regions along the major axis of rotation (P.A. ~ 28^deg^)
show that each of these tracers give a FWHM of ~10" (Li et al. 1993).
NGC 7625 has a molecular gas mass of ~2.4 x 10^9^ M_sun_ and an atomic mass
of about the same amount (Li et al. 1993).
Our 100 micron profile (Fig. 19) is peaked between detectors 4 and 5,
while the optical peak should have been between detectors 5 and 6. This
suggests that the FIR is skewed slightly to the south away from the optical
(Li et al. 1993) and large-beam 1.49 GHz radio (CHSS) position, which was
our target. That pointing position also corresponds well to the H{alpha}
and H I center, while the CO and small-beam radio centers appear to be
several arcseconds to the northwest. Significantly, the FIR peak
corresponds spatially better with the prominent dust lane and the centroid
of the outer optical contours.
Though our point-source flux is consistent with that of IRAS, there is
some slight evidence for extension of NGC 7625 in the profile (Fig. 19),
and D_g_ = 21.8" and D_e_ = 13" is obtained, which matches the sizes of the
other tracers of the starburst activity. Using the derived disk size of 13"
in the single-slab model, T_d_ = 32 K and a {tau}_100_ = 1.2 x 10^-2^ are
derived, which translates into an A_V_ = 9.

4. 1999A&A...349..424T
Re:III Zw 102
III Zw 102: Despite its relatively high optical luminosity
(M_B_ = -19.2), this galaxy is often included in studies of dwarf
galaxies (e.g. Thuan & Martin 1981). Li et al. 1993b obtained ^12^CO 1-0
maps with OVRO, and also single dish spectra in the 2-1 and 1-0
transitions with the IRAM 30-m telescope. The distance to III Zw 102 is
large (23.5 Mpc), so structures like GMCs could not be resolved in the
observations. They found a 2-1/1-0 line ratio of 0.66 +/- 0.12, quite
similar to what we found for GMCs 3 and 4 although, given the large
errors on our line ratios, the value for GMC 1+2 is also consistent.
This line ratio for III Zw 102 is measured over the 23" beam of the 30-m
telescope at 115 GHz. This corresponds to ~ 2.6 kpc within the galaxy,
so the line ratio is clearly an average over a large number of GMCs. The
distribution of the CO emitting gas is roughly correlated with the star
formation as traced by H{alpha} and radio continuum images, but the peak
of the CO emission is offset relative to the peak of the optical
emission. This is quite similar to NGC 1569, in which we find molecular
material associated with HII regions, but not with the SSCs.

5. 1998AJ....116.2166U
Re:NGC 7625
This galaxy has a tubelike dust lane in the Carnegie Atlas that cannot
be seen in our R-band image. Patchy H II regions and more diffuse
emission are seen in the H{alpha} image. This Arp galaxy occurs intense
star formation but does not have any companion galaxy. Li et al. (1993)
observed and studied this galaxy extensively.
The early-type spiral galaxies observed in the present study have the
extended H II regions at the central regions with some asymmetric
features. The intensities at faint extended H{alpha} emission are well
above the errors estimated from the uncertainties of continuum
subtraction and scaling factor between H{alpha} and R-band image, and
these features are real. For some barred or ringed galaxies, e.g.,
NGC 3504 and 4045, the star formation also takes place on the ends of
a bar or a ring. Nevertheless, it is at the central region that the
star formation takes place most intensely. The degree of the
concentration of the H II regions to the galactic center is discussed
quantitatively in Section 3.4.

6. 1997A&A...323..323D
Re:III Zw 102
4.8. III Zw 102
Whitmore et al. (1990) consider III Zw 102 as `related to polar-ring galaxies':
with its dust lanes being similar to polar rings without the luminosity.
Various catalogs and publications classify III Zw 102 among elliptical, Sa or
SO galaxies; most mention its peculiarity. Brosch and Loinger (1991) note that
III Zw 102's common classification among BCDGs is apparently the result of its
selection among the 115 BCDGs of Thuan & Martin (1981), as its diameter of 13
kpc hardly classifies it as a dwarf. Brosch and Loinger (1991) perform
extensive modeling of III Zw 102's internal extinction. Although the brightness
profile of the underlying disk agrees well with a fit to the de Vaucouleurs
r^1/4^ law which indicates elliptical structure, they are unable to decide on
its morphology. The colors of the disk are probably dominated by variations in
the dust extinction (Fig. 8a). The elongated reddish extinction feature in the
NE to SW direction near the center also appears prominently in the models of
III Zw 102's extinction by Brosch and Loinger. The radio-emission (Fig. 8b)
traces the H{alpha} emission quite well, implying that at least in the area of
the H{alpha} emission, optical extinction cannot be very large. The radio
emission does not reflect the extent of the dust envelope (Fig. 1f in DBDKS).

7. 1996ApJ...466..122R
Re:ARP 212
Arp 212.--Arp 212 is a well-studied starburst galaxy (Devereux 1989) with
exponential profile (disklike). The narrowband colors indicate a strong
starburst with equally strong dust extinction in the bulge as confirmed by
far-IR emission.

8. 1985ApJS...57..643D
Re:VV 280
Spiral with asymmetric dust lanes.

9. 1976RC2...C...0000d
Re:NGC 7625
= Arp 212
= VV 280
= III Zw 102
Ap. J., 157, 69, 1969.
Ap. J., 186, 445, 1973.
CGCG, 387, 1971.
Ap. J., 186, 445, 1973.
Bull. A.A.S., 5, 349, 1973.
Spectrum, Rotation Curve, and Mass Determination:
Ap. J., 157, 69, 1969.
HI 21cm:
A.J., 79, 767, 1974.

10. 1973UGC...C...0000N
Re:UGC 12529
VV 280, Arp 212, III Zw 102
SA(rs)a pec (de Vaucouleurs)
In Arp's class "galaxies with irregularities, absorption and resolution"
"Narrow chaotic absorption tubes across one end" (Arp)

11. 1971CGPG..C...0000Z
Re:CGPG 2318.0+1657
III Zw 102
NGC 7625
Neutral very large disrupted post-eruptive galaxy with
bright patches and dark absorption lanes.
= +1,700 km/sec. (Humason 1956).
Spectrum: Absorption: Balmer, Emission: H{alpha}, [OII] , [NII] , and others.
= +1,440 km/sec. (Zwicky 1965).
Literature: Zwicky 1965b.
m(pg) = 12.8 [CGCG]

12. 1964RC1...C...0000d
Re:NGC 7625
Small, bright, complex nucleus in a bright (r): 0.22 arcmin x 0.17 arcmin.
Complex lens with a strong, asymmetric dark lane. Very peculiar object.
Heidelberg Veroff. Vol. 9, 1926 dimensions are for the bright part only.
Yerkes 1 classification (1958): or faint ? "turbulent E with dust".

13. 1959VV....C...0000V
Re:VV 280
= NGC 7625
V = +1,930 km/sec
Yerkes Type: g?Ip or f?I?p
"Turbulent E with dust"
We consider two bodies are probable.

14. 1956AJ.....61...97H
Re:NGC 7625
HMS Note No. 216
Early-type continuum with faint absorption lines.

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