Date and Time of the Query: 2019-03-21 T03:09:54 PDT
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Notes for object NGC 7770

8 note(s) found in NED.

1. 2004AJ....127..736H
Re:NGC 7770
NGC 7770 (Fig. 2c) is a strong H{alpha} source, showing double peaks in
both H{alpha} and continuum emission, and has a comparable flux to
NGC 7771. The western peak in H{alpha} is coincident with the continuum
peak, while the eastern one is offset by ~2" to the north of the eastern
continuum peak. In addition, there is a tail-like structure extending to
the west from the northern part of the main body. This structure cannot
be seen in our continuum image or in the I-band image shown in Smith et
al. (1999). We also detected faint H{alpha} emission from NGC 7771A (not

2. 1997A&AS..126..471T
Re:KAZ 347
KAZ 347: According to Humason et al. (1956) NGC 7770 has a strong ultraviolet
continuum of early type, broad and weak absorption lines of the Balmer series
as well as weak emission at {lambda}3727A [O II] which is possibly inclined. In
pair with NGC 7771 located at 1.1 arcmin and disturbed; member of NGC 7769
group. Investigated photometrically by Tamazian (1984). Integral colors U-B=
+0.13, B-V=+0.49, but the bright nucleus is bluer with U-B-0.27, B-V=+0.34.
According to Humason et al. (1956) the radial velocity is V=4338 km/s, but more
precise measurements indicate smaller radial velocity V=4077 km/s(see Table 1).
Our HI line appears disturbed. NCC 7771 (V(opt)=4311 km/s, [7][10][17][19][22]
[26][29][30][37][38][42][45]) is located within the Nancay beam and there is HI
confusion: what is expected is a narrow emission from the face-on galaxy KAZ
347=NGC 7770 (around V~4300 km/s) superimposed on a relatively wide HI
emission, centered at a nearby velocity, from the large inclined EW spiral NGC
7771. Note that Schneider et al. (1986) have observed the system NGC 7769/7770/
7771 at Arecibo (HPSW=3.6 and state that NGC 7770 "has a broad peculiar wing
on the high-velocity side of its HI profile". This feature is also present here
and is typical of interacting galaxies.

3. 1994CAG1..B...0000S
Re:NGC 7770
Group [with NGC 7769 and NGC 7771]
Sa pec
Nov 6/7, 1978
12 min
The galaxies shown here form at least a
triplet with closely the same redshift, as
measured by Mayall (Humason, Mayall, and
Sandage 1956). The orientation of the print is
north at the top, east at the left.
NGC 7769 is the large galaxy at the upper
right. The type listed in the RSA is
Sbc(s)II(tides?). The tightly wound, interior very
bright arms show a high recent-star-formation
rate evidenced by the many high-surface-brightness
HII regions. Faint, smooth outer arms are
well seen in this negative print. These arms alone
would give a classification of Sa. However, the
inner arms are of type Sbc. NGC 7769 is an
example of the Sc/Sa class (panel 86), whose type
examples are NGC 5665, NGC 4580, and NGC 7679.
NGC 7770 is the small Sa pee galaxy slightly
south and west of the large SBab pec galaxy NGC
7771. Star formation (induced?) is present in the
center of NGC 7770. The smooth stubby arms
visible on the negative print may be tidal plumes
from the evident close encounter with NGC 7771.
The three major galaxies form a physical
triplet. The redshifts are v_o(7769) = 4349 km/s,
v_o(7770) = 4338 km/s, and v_o(7771) =
4276 km/s. The projected angular separations
of the two galaxies from NGC 7771 are 60" for
NGC 7770 and 315" for NGC 7769. From the
mean redshift of = 4321 km/s, the redshift
distance of 86 Mpc (H = 50) gives projected
linear separations from NGC 7771 of 25 kpc for
NGC 7770 and 130 kpc for NGC 7769.

4. 1994CAG1..B...0000S
Re:NGC 7770
[Triplet with NGC 7769 and NGC 7771]
Karachentsev 592 [with NGC 7771]
Sa pec
Nov 6/7, 1978
12 min
The triplet evidently forms a physical
group; the redshifts (Mayall, in Humason,
Mayall, and Sandage 1956) are v_o = 4565 km/s,
v_o = 4554 km/s, and v_o = 4492 km/s for
NGC 7769 (Sbc), NGC 7770 (Sa pec), and NGC 7771
(SBab pec), respectively. At the mean redshift
distance of 91 Mpc the angular separations
of NGC 7771 from NGC 7769 of 315" and from
NGC 7770 of 60" correspond to the small
projected linear separations of 93 kpc and 26
kpc, respectively.
The morphologies of NGC 7770 and NGC 7771
suggest tidal interactions due to a close
encounter. Both have smooth luminous outer
regions, which are either well-defined (tidal?)
outer arms as in NGC 7771, or compose an outer
envelope that has a broken symmetry, as in
NGC 7770.

5. 1976RC2...C...0000d
Re:NGC 7770
= Holm 820b
Pair with NGC 7769 at 5 arcmin, NGC 7771 at 1.1 arcmin

6. 1973UGC...C...0000N
Re:UGC 12813
Sb: (de Vaucouleurs)
Asymmetric halo
Paired with UGC 12815 at 1.1, 25

7. 1964RC1...C...0000d
Re:NGC 7770
= Holm 820b
Pair with NGC 7769 at 5 arcmin.
Pair with NGC 7771 at 1.1 arcmin.

8. 1956AJ.....61...97H
Re:NGC 7770
HMS Note No. 228
Strong early-type continuum and {lambda} 3727, possibly inclined.
Broad and faint H and K lines were measured with considerable
uncertainty, which accounts for the large average deviation.
Nebular type in the list by Pettit, E. (1954, Ap. J., 120, 413)
list probably interchanged with that for NGC 7771.

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