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Notes for object NGC 7552

22 note(s) found in NED.


1. 2008MNRAS.385..553D
Re:NGC 7552
NGC 7552: This SBab galaxy is completely dominated by its bar, making
the extraction of kinematical parameters impossible. The velocity field
shows a central S-shaped disturbance indicating non-circular motions
caused by the bar. A steep velocity gradient (~150 km s^-1^ kpc-1) is
present in the nuclear region as well as a bright H{alpha} centre
representative of a LINER galaxy.

2. 2008A&A...483...79R
Re:NGC 7552
NGC 7552 contains three star forming rings of radii 1.0 kpc, 1.9 kpc, and 3.4
kpc at the co-rotation and Lindblad resonance radii of the bar. The inner-most
ring is seen in radio continuum (Forbes et al. 1994a). Our continuum image (Fig.
6f) shows the ring structure seen previously by Forbes et al. A number of
Br{gamma} knots lie along the inner ring which show weak correlation with radio
knots, but these are not spatially resolved in our observations.
We used the upper limits on the H91{alpha} + H92{alpha} line emission to
constrain the properties of the nuclear emission-line regions. Parameters
derived for typical allowed models are given in Table 3.

3. 2006ApJS..164...52S
Re:NGC 7552
This is a nuclear starburst galaxy. The H{alpha} and radio images (Fig. 13, top)
show the presence of a circumnuclear ring, as well as star formation along the
bar of the galaxy (similar structures were detected by Hameed & Devereux 1999).
The H{alpha} image also shows some emission along the spiral arms, which is too
faint to be detected by our radio observations.

4. 2004MNRAS.355.1251L
Re:NGC 7552
NGC 7552 (Fig. 8g, available in the online version; see also Fig. 2).
This is a peculiar case of a bar and two spiral arms forming an outer
pseudo-ring (type R'_1_; Buta 1995). One of the spiral arms, starting
from the end of the bar, is more prominent than the other arm, which
seems to have no clear continuation with the bar. The bar itself is
very dusty and shows a lot of structure. The polar angle map shows how
the spiral arm attached to the bar is superimposed with the bar. While
looking at the original image, this galaxy has similarities with NGC
3504: in both cases, there are blobs at the two ends of the bar showing
some characteristics of spiral arms. Also, as in NGC 3504, the small
spiral arm segments are not a continuation of the global spiral
patterns. The main difference, compared with NGC 3504, is that NGC 7552
has no inner ring.

5. 2004MNRAS.355.1251L
Re:NGC 7552
NGC 7552 (Fig. 8g, available in the online version; see also Fig. 2). This is a
peculiar case of a bar and two spiral arms forming an outer pseudo-ring (type
R'_1_ ; Buta 1995). One of the spiral arms, starting from the end of the bar, is
more prominent than the other arm, which seems to have no clear continuation
with the bar. The bar itself is very dusty and shows a lot of structure. The
polar angle map shows how the spiral arm attached to the bar is superimposed
with the bar. While looking at the original image, this galaxy has similarities
with NGC 3504: in both cases, there are blobs at the two ends of the bar showing
some characteristics of spiral arms. Also, as in NGC 3504, the small spiral arm
segments are not a continuation of the global spiral patterns. The main
difference, compared with NGC 3504, is that NGC 7552 has no inner ring.

6. 2004A&A...419..501F
Re:NGC 7552
NGC 7552 - Verma et al. (2003) published Br{alpha} and Br{beta} fluxes
obtained with SWS in a 14" x 20" aperture which matches fairly well our
circular aperture of 21.8". We used Br{alpha} only because of possible
blending of Br{beta} with H_2_ 1 - 0 O(2), and combined it with the
H{alpha} flux integrated over the same region from an H{alpha} + [N II]
map to derive the extinction. The nucleus is slightly saturated in the
LW3 map. From the data of Veron-Cetty & Veron (1986) for the central
4" x 4", [N II]{lambda}6583 {Angstrom}/(H{alpha} + [N II] {lambda}6583
{Angstrom}) = 0.37 and the H{alpha} flux is 24% of the flux in 21.8".

7. 2002ApJS..143...73E
Re:NGC 7552
NGC 7552.---(R)SBa: Irregular nuclear region. At lower intensity,
bulge becomes regular and elliptical. Prominent, long bar aligned with
bulge major axis. Bar surface brightness is irregular, with several
knots/lumps of enhanced brightness. Bar appears to end in points, with
faint, very open spiral arms emerging from the bar ends. The arms are
quite smooth, with few knots or irregularities. At low surface
brightness levels, the winding of the arms tightens, and they wrap at
least 180deg around the galaxy.

8. 2002A&A...391...83B
Re:NGC 7552
NGC 7552 (Fig. 24), a member of the Grus Quartet, has a starburst
circumnuclear ring of 8" (~0.8 kpc) radius, observed in radio continuum
and near-infrared, a nuclear bar (observed in radio continuum and
near-infrared) lying perpendicular to the primary bar, but no active
nucleus (Forbes et al. 1994a,b). It is notable for strong, highly
polarized radio emission from the centre, the bar and the inner parts
of the spiral arms. Our resolution is insufficient to resolve the radio
ring. Polarized emission is strong upstream of the dust lanes, with
magnetic field lines oriented at large angles to the bar major axis
(Fig. 26); these features make this galaxy similar to NGC 1097 and
NGC 1672. The outer extensions in Fig. 24 are artifacts due to
unsufficient uv coverage. A detailed discussion of this galaxy will
be given in Paper III.

9. 2002A&A...389...68G
Re:NGC 7552
NGC 7552: the HII regions are mainly concentrated in and around
the bar region and thus can not give useful information for the
deprojection. We thus adopt the values from RC3 (1991).

10. 1996ApJS..103...81C
Re:NGC 7552
NGC 7552.--ATCA map of the central starburst ring at 8.64 GHz in Forbes et al.
(1994).

11. 1994CAG1..B...0000S
Re:NGC 7552
SBb(s)I-II
CD-1587-S/Br
Aug 11/12, 1980
103aO + GG385
45 min
The same original plate was used to make
the two prints of different contrast of NGC 7552
offered here. The low-contrast print shows the
detail of the intricate dust pattern in the oval,
which is the weak bar. The high-contrast print
shows the generally low-surface-brightness spiral
pattern of the (s) type, where the arms begin at
the end of the bar (the oval here).
The two straight dust lanes characteristic of
SBb types are best seen in the low-contrast print,
which shows the center well. These lanes, as in
NGC 1300, start from opposite sides of the
nucleus and are straight almost to the end of the
oval. They are not as well defined as in NGC 1300
but are obviously present. It is well understood
that these lanes are due to hydrodynamic
shocks in the gas in response to the gravitational
perturbation of the rotating bar. The stronger
the bar, the stronger are the shocks, according to
the calculated models (see Prendergast 1983 for
a review).
Dust lanes, curved into spiral fragments,
exist in the central oval starting from the two
straight lanes on opposite sides of the oval.
The outer luminous arms shown in the high-contrast
print start from the ends of the oval. On
one side the principal arm branches into three
fragments, the inner of which nearly overlaps the
other principal arm, which starts from the
opposite side of the oval. This arm remains single
for the half-revolution over which it can be
traced.
Only a few HII regions exist in the arms, the
largest of which resolve at about the 2" level. The
redshift is v_o = 1565 km/s.

12. 1993ApJS...86....5K
Re:NGC 7552
NGC 7552; SBbc, starburst.
NGC 7552 is one of the components of the Grus quartet. The center shows
the absorption features of early-type stars, presumably from a burst of
recent star formation (Alloin & Kunth 1979). Spectral population
synthesis by Bica (1988) indicates a population component younger than 5
X 10^7^ yr and with solar metallicity. The UV spectrum, in addition to
having many absorption lines from young stars, is rising toward longer
wavelengths and also has absorption features between 1850 and 2000 A of
Al II, Al III, Fe II, and Fe III - the latter two are both signs of a
dominant A star population. The UV slope of this galaxy is one of the
"reddest" of the starbursts, with F_{lambda}_ is proportional to
{lambda}^+0.3^. The complex optical spectrum of NGC 7552 has been
attributed to the presence of three or four cycles of star formation
(Dottori & Pastoriza 1986).

13. 1988A&AS...75..273D
Re:NGC 7552
NGC 7552 is a spiral galaxy, in which Sersic and Pastoriza (1965)
noted the presence of an amorphous nucleus. Buta (1984) described it
as being of SB(s)ab type with <> features, and it belongs to
the Southern Grus group of galaxies. NGC 7552 is a radio source
(Whiteoak, 1970, Wright, 1974), mapped by Ward et al. (1980) and which
has also been detected in X-rays (Maccacaro and Perola, 1981, Charles
and Phillips, 1982). A giant ionized nebulosity was discovered through
narrow band imaging (DB87).
We find for this galaxy a redshift z = 0.0053 +/- 0.0001,
corresponding to a galactocentric velocity of 1555 km s^-1^, and to a
distance of 31.1 Mpc.
Our long slit spectroscopy reveals the ionized gas over 11.1" (16.8
kpc) along PA = 271^deg^, with a somewhat larger extent towards the
east than the west. This overall size is just a little smaller than
the 120" detected through narrow band imaging. The latter may have
been slightly overestimated since it was difficult to determine the
continuum contribution to the narrow band image due to the great
similarity between the narrow and broad band images. As seen in figure
7a and table IX, the [OI] 6300 line is present in several extranuclear
zones at a 2-4 sigma level but is not detected in the nucleus;
therefore, NGC 7552 is at most a weak LINER. Regions W2 and E4 are of
higher excitation than the nucleus and other zones.

14. 1988A&AS...75..273D
Re:NGC 7552
The H{alpha}/H{beta} ratio suggests that NGC 7552 is highly
reddened, with colour excesses E(B-V) ranging from 0.51 to 1.27, the
central region being the most heavily reddened. However, as already
noted by Ward et al. (1980) the Balmer series is strongly seen in
absorption from H{gamma} downwards (see Fig. 7a); hence, the
uncertainties on the H{beta} and H{gamma} line intensities given in
table IX could be underestimated. Alloin and Kunth (1979) have used
absorption line measurements to fit stellar population models to
NGC 7552, and showed that the continuum of this galaxy revealed an
important contribution of young stars and little reddening if the
optical con- tinuum is entirely of stellar origin. Charles and
Phillips (1982) also suggested that strong star formation activity
could account for the X-ray and radio emission of NGC 7552. Ward et
al. (1980) used their own measurement of the NaI D absorption line
together with the results of Alloin and Kunth (1979) to derive an
H{alpha}/H{beta} ratio of 4.9 (corresponding to E(B-V) = 0.22 only).
Therefore, the reddening correction in NGC 7552 is not straightforward
and obviously the H{alpha}/H{beta} ratio gives a much too large
reddening correction for this galaxy.
We have therefore chosen to apply to NGC 7552 the correction
corresponding to its intrinsic reddening only, as recently estimated
by Bica and.Alloin (1987) by fitting a template to the continuum of
this galaxy: E(B-V) = 0.18. T_e_ then equals 5000 K in the nucleus,
and ranges from 4300 K to 6900 K elsewhere. These values are given in
table IX together with n_e_.
NGC 7552 shows solid body rotation in its central regions, with
flattening on either side of the nucleus (see Fig. 7b). The maximum
velocity spread is about 180 km s^-1^ along PA = 271^deg^, and the
velocity gradient in the central part is 100 km s^-1^ kpc^-1^. A
region more than 2 kpc in extent, centered about 7 kpc east of the
nucleus (corresponding roughly to region E3 defined in Tab. IX) has a
velocity larger by some 80 km s^-1^ than the adjacent zones towards
the west; it has also a higher excitation level than the surrounding
envelope. This suggests that it is a blob of gas with slightly
different kinematic and physical properties than the overall
nebulosity. The same may apply to the region to the far west of the
nucleus, which shows a decrease in velocity on figure 7b, but where
fewer emission lines have been measured. The presence of such blobs is
not unusual, since similar inhomogeneities have already been found in
other extended ionized nebulosities (e.g. in IC 5063, Bergeron et al.,
1983).

15. 1985SGC...C...0000C
Re:NGC 7552
= IC 5294
Plate 839
Overexposed.
Plate 2533
Overexposed center, patches and knotty arms form (R'): 2.8 x 2.5.

16. 1982ESOU..C...0000L
Re:ESO 231325-4251.4
=ESO 291- G 12
in cluster

17. 1977A&AS...28....1V
Re:VV 440
Plate 11 Galaxies of the M51 Type.
MCG -07-47-028 = NGC 7552. 11.50m.
Photo from Handb. Phys. 53, 294 (1959). Peculiar nucleus. V_0_=+1644,
(B-V)_0_=0.73, (U-B)_0_=0.09 (Shobbrook 1966). Early spectrum with
emissions of H and [O II]. V_0_=+1689 (RC1, C, E).

18. 1976RC2...C...0000d
Re:NGC 7552
= IC 5294
= PKS 2313-428
Description and Classification:
P.A.S.P., 77, 287, 1965.
P.A.S.P., 79, 152, 1967.
Photograph:
P.A.S.P., 77, 287, 1965.
Photometry (I.R.: 1-10.6 microns):
M.N.R.A.S., 162, 35P, 1973.
M.N.R.A.S., 164, 155, 1973.
Ap. J. (Letters), 191, L19, 1974.
Spectrum:
Observatory, 87, 38, 225, 1967.
Spectrophotometry:
Astr. Ap., 33, 331, 1974.
Astr. Ap., 33, 337, 1974.
Radio Observations:
Australian J. Phys., 19, 883, 1966.

19. 1964RC1...C...0000d
Re:NGC 7552
= IC 5294
Extremely bright nucleus in a bright complex bar and lens: 1.8 arcmin x
0.35 arcmin with a dark lane. 2 smooth regular arms with a few bright knots
form a pseudo (R): 3.0 arcmin x 2.4 arcmin.

20. 1957HPh....53..275d
Re:NGC 7552
(R')SB(s)a
(Plate 29)
A small, elliptical nucleus in a bar-like, elongated
lens with much internal structure marked by dark lanes.
Two main spiral arms (one stronger) emerge from extremities
of the bar and return to the opposite extremity after a
half-turn, thus simulating an outer ring structure.
Also illustrated on Plates 49 and 52.
Compare with NGC 2523 (Plate 27), NGC 5962 (Plate 23),
NGC (Plate 30) and (Plate X).

21. 1957HPh....53..275d
Re:NGC 7552
(R')SB(s)a
(Plate 49)
Face-on view.
Same as Plates 29 and 52
Note the outer loops.
Details of the bar and the lens, seen from "above" are in
Plate 52. Note the pattern of dark material.

22. 1957HPh....53..275d
Re:NGC 7552
(R')SB(s)a
(Plate 52)
Details of bar and lens.
See Plates 29 and 49.


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