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Notes for object NGC 0772

14 note(s) found in NED.


1. 2007MNRAS.380..506G
Re:NGC 0772
NGC 772, also called Arp78, is an Sb galaxy characterized by a particularly
strong spiral arm; it forms a pair at 3.3 arcmin with the E3 galaxy NGC 770.
From the kinematical point of view, NGC 772 is characterized by a clear drop of
the stellar velocity dispersion in the central zones, possibly corresponding to
an inner disc, as suggested also by the anticorrelation between velocity and the
Gauss-Hermite moment h3 (Ganda et al. 2006). In the line strength maps we can
clearly see an extended central region with high Fe5015 and Mgb and low H{beta};
indeed, from the central aperture values reported in Table 2 we can see that
this galaxy is one of those with the highest metal indices, surpassed only by
NGC 488. In the H{beta} map it is possible to see, surrounding the central
depression, regions with higher values corresponding to the spiral arms. A
similar behaviour can be seen in the [O III]/H{beta} map presented by Ganda et
al. (2006), which shows a structure resembling the spiral pattern. Estimating
ages and metallicity by comparison with SSP models, we infer that ages are
mainly young-intermediate and the central metallicity is among the highest in
our sample. The age and abundance ratio maps display the spiral arms structure
as well, like the index maps. Fig. 29 (third column) demonstrates that for this
galaxy constant star formation can be ruled out at a high confidence level: high
{tau} values are never likely. The {tau} map shown in Fig. 7 (for age fixed to
10 Gyr in the fitting procedure) presents a spatial structure that partially
resembles the H{beta} map and the spiral arms pattern. NGC 772 is part of the
sample studied in the series of papers by Cid Fernandes et al. (2004); Gonzalez
Delgado et al. 2004; Cid Fernandes et al. 2005, who are engaged in a project to
examine the stellar populations of low-luminosity active galactic nuclei (AGN).
They classify this object as 'young-TO', that is, a transition object between a
LINER and an H II nucleus, with weak [O I] {lambda}6300 emission; they find th
at the nuclear spectrum is dominated by 10^8^-10^9^ yr old stellar populations,
with a contribution up to ~=32 per cent from populations younger than 10^7^ yr
and a similar contribution also from older stellar populations (>=10^9^ yr).
Their data probe distances up to several hundred parsecs from the nucleus; they
measure in NGC 772 significant radial variations of the stellar populations,
with absorption line strengths increasing in the inner 3 arcsec indicating a
younger population in the very centre, especially referring to the Ca II K line;
the Mg I absorption strength presents instead less prominent variations over the
spatial range of their data. Our data cover a different spectral range and a
different spatial extension, but we also concluded that the populations in the
inner parts have intermediate ages, and that the age (from the one-SSP analysis)
increases in the inner ~=5 arcsec (see Fig. A1).

2. 2007ApJS..173..538T
Re:NGC 0772
NGC 772 (Fig. 16.3).-GALEX imaging of this SA(s)b galaxy shows a complex,
asymmetric spiral structure with an anomalously bright arm extending to the
northwest of the nucleus for approximately 3'. This UV morphology (and the
visible appearance) is highly suggestive of past or present galaxy interaction,
probably with NGC 770 (3.3' southwest). Such excitation of one-armed spiral
modes has been discussed by Taga & Iye (1998) and Lovelace et al. (1999). The
inner part of the NGC 772 disk is surrounded by tightly wrapped, generally
continuous spiral features, which attain their greatest extent (7.1') to the
south of the galaxy. NGC 772 dominates a NOG group (NOGG 124) of three bright
galaxies. Zaritsky et al. (1997) further associate three lower mass companions
with NGC 772. Of these, NGC 772b appears optically disturbed (Gutierrez et al.
2006). NGC 772 has a comparatively large H I disk (Rao & Briggs 1993; Iyer et
al. 2001).

3. 2007AJ....134.2286H
Re:KIG 0080
CIG 80: The major axis of this galaxy is longer than our CCD frame. However, we
comment on the structure found within 4.3'. The galaxy was classified as SA(s)b
(NED). The gray-scale R-band and sharp-filtered images show a multiarmed and
strongly asymmetric pattern enhanced by the presence of dust lanes, resembling a
strongly perturbed system. The (B - I) color map shows an inner ring and bluer
arms. The composed JHK image shows a barlike structure from which two prominent
arms seem to emerge and confirms the red nature of a ring oriented in the
direction of the bar. We classify this galaxy as SB(r)b. The (B - V) color is
consistent with Sab types. The photometric ({epsilon} and P.A.) profiles show
weak evidence of a bar within the inner 25" of this galaxy. We noticed that this
galaxy might not necessarily be isolated, because it appears in the LEDA
database as part of a group.

4. 2002AJ....124..675C
Re:UGC 01466
There are two NVSS sources in this galaxy, one on the northwest arm,
the other on the nucleus.

5. 2002AJ....123..159C
Re:NGC 0772
Red (dust) spiral lane down to blue center

6. 2002A&A...388...50F
Re:NGC 0772
According to the dynamical modelling of Pignatelli et al.
(2001), the velocity of the ionized gas traces the circular
speed in gravitational equilibrium. The PV diagram of NGC 772
derived from the [O III] {lambda}5007 emission line is
classified as Type III since the integrated flux of the
emission line in the nucleus is greater than that measured
in the outer regions.

7. 2001A&A...368...16M
Re:NGC 0772
3. NGC 772 = Arp 78 is an Sb galaxy with one especially strong spiral arm.
Nevertheless the fit of the disk works fairly good and shows very low
residua.

8. 1996A&AS..115..439E
Re:NGC 0772
NGC 772 is a large SA galaxy with asymmetric arm structure. It has faint H II
regions (Oey & Kennicutt 1993) and a large H I radius (about 75 kpc) (Rao &
Briggs 1993). There is a faint material bridge towards two dwarf companions
and its satellite (NGC 770) has a retrograde orbit (Zaritsky et al. 1993).
There is a tendency for CO emission to be present in all our observed
positions; we have, however, only observed the inner region of the galaxy.

9. 1994CAG1..B...0000S
Re:NGC 0772
Pair
Sb(rs)I
PH-7564-S
Nov 7/8, 1978
103aO
12 min
NGC 772 is an early Sb. The arms, although well formed, are
relatively smooth, indicating only a small current rate of star
formation except in the single high-surface-brightness arm which
contains several evident HII regions.
The relatively smooth multiple arms on the opposite side from the
prominent arm are defined primarily by the fragments of spiral dust
lanes.
The spiral pattern is intermediate between that of the grand
design and the multiple-armed spiral (MAS) types.
NGC 772 and NGC 7710 (E3), at a separation of 3.3', form a binary
pair. The redshifts are v_o(770) = 2639 km/s and v_o(772) = 2660 km/s.
At a mean redshift distance of 53 Mpc (H = 50) the projected linear
separation of the pair is 51 kpc.

10. 1976RC2...C...0000d
Re:NGC 0772
= Arp 078
Possibly interacting with NGC 0770 at 3.3 arcmin north.
Photograph:
Ap. J., 139, 1056, 1964.
Astrophys. Lett., 5, 257, 1970.
IAU Symp. No. 44, 386, 1972.
Photometry and Spectrum:
Astrophys. Lett., 5, 257, 1970.
HI 21cm:
M.N.R.A.S., 150, 337, 1970.

11. 1973UGC...C...0000N
Re:UGC 01466
Several tightly coiled arms, one strongly asymmetric crossing the disk
westwards
Extremely diffuse extension not included in diameter
Arp 78, in Arp's class `small, high surface brightness companions'
See UGC 01463, broad very faint arc opposite UGC 01463 suggests interaction
Companions at 4.1 and 5.7, probably extremely diffuse plumes, `faint material
toward each of the two dwarf companions' (Arp). These objects have anomalous
redshifts (Astrophys. Letters 5, pp 257-260), v = 20174 and 19680

12. 1973AISAO...8....3K
Re:KIG 0080
Multi-armed spiral; arms are of different brightness.

13. 1964RC1...C...0000d
Re:NGC 0772
Interacting pair (?) with NGC 0770 at 3.3 arcmin.
Small, very bright, diffuse nucleus.
Many weak, tightly coiled arms, one abnormally strong.

14. 1918PLicO..13....9C
Re:NGC 0772
A beautiful, rather symmetrical spiral about 5' x 3' in p.a. 120^deg^. The
nucleus is bright and almost stellar. There are several faint condensations; one
whorl is much brighter than the rest. 27 s.n.


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