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Date and Time of the Query: 2019-04-25 T04:47:10 PDT
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Notes for object NGC 5077

8 note(s) found in NED.


1. 2004MNRAS.350.1087S
Re:NGC 5077
NGC 5077: this E3-4 galaxy is the main member in a group of eight; a
luminosity excess (halo) is detected from r~ 5 kpc outwards (Fig. 1).

2. 1999ApJS..120..209N
Re:NGC 5077
NGC 5077 (misclassified Seyfert; LINER type 1.9; Fig. 12) - Gaussian
deconvolution shows that the galaxy is unresolved at both 3.6 and
20cm. The source has a flat spectrum between 3.6 and 20cm. Previous
high-resolution VLA observations of this source (Wrobel & Heeschen
1984) give fluxes of 109, 90, and 111 mJy at 1.5, 4.9, and 15 GHz,
respectively; the source was unresolved in high-resolution maps at all
three frequencies. The large-scale features in the 20cm self-calibrated
map were not seen by Wrobel & Heeschen (1984) but may be real
considering the morphology of the extended emission seen in the [O III]
and H{alpha}+[N II] images of MWZ.

3. 1997ApJS..112..391H
Re:NGC 5077
NGC 5077.--The derived strength of the broad H{alpha} component in this object
(Paper I) depends critically on the assumption about the intrinsic [S II]
profile, which, unfortunately, is rather uncertain with the present S/N of the
spectrum. In particular, different (equally acceptable) assumptions about the
[S II] profile can lead to a factor of 3 discrepancy in the final broad
H{alpha} flux. In Figure 14c, we have chosen the set of parameters that gives
the smallest probable broad H{alpha} flux.

4. 1994CAG1..B...0000S
Re:NGC 5077
NGC 5077 Group
S0_1/2_(4)
(S)
CD-1874-HB
April 10/11, 1981
103aO
75 min
NGC 5077 is the eponymous member of a group of about seven
galaxies (Humason, Mayall, and Sandage 1956; Sandage 1975b). The
redshift of NGC 5077 is v_o = 2561 km/s. Other Dreyer galaxies close
to NGC 5077 are NGC 5070, 5072, 5076, 5079, and 5088. NGC 5088 (Sc;
panel 292), with redshift v_o = 1230 km/s, is evidently in the
foreground.
The extended envelope of NGC 5077 requires the S0
classification. The E3 classification in the RC2 is not supported
here.
Dust patches exist at the top and bottom of the main body along
the minor axis. They resemble, but are weaker than, the dust lanes in
the prolate S0 galaxies shown on panel 45. The presence of this
near-polar-ring dust lane (presumed to be a complete ring) is the
reason for the S0_1/2_ subclass.

5. 1976RC2...C...0000d
Re:NGC 5077
= Holm 514b
Non-interacting pair with NGC 5079 at 3.0 arcmin.
Brightest in a group.
Photometry (BVR):
Ap. J., 183, 731, 1973.
Spectrum:
Ap. J. (Letters), 164, L35, 1971.
Radio Observations:
A.J., 75, 523, 1970.
Astrophys. Lett., 6, 49, 1970.
Ap. J., 157, 481, 1969.
Ap. J., 189, 399, 1974.
IAU Symp. No.44, 222, 1972.

6. 1974UGCA..C...0000N
Re:UGCA 347
UGCA 347:
= NGC 5077
E3/4 (RC1)
brightest in the NGC 5077 Group with
companion at 1.0, 119, 0.35 x 0.35, compact;
NGC 5079 at 2.9, 150, 1.5 x 0.7 , chaotic Sc, disturbed?;
NGC 5076 at 5.1, 184, 0.9 x 0.7 , SB0-a

7. 1968MCG4..C...0000V
Re:MCG -02-34-027
Main member of group consisting of eight galaxies.
In a pair with MCG -02-34-030
{rho} = 3.0 arcmin.
Type:
Sand - E3
vdB - E3
Morg - kED4
deV - E3-4
Redshift = +2,515 km/sec
G2e
Cp' = 1.15.

8. 1964RC1...C...0000d
Re:NGC 5077
= Holm 514b
Brightest of a group. Very bright, diffuse nucleus. There is a star at
16 arcsec.
Non-interacting pair with NGC 5079 at 3.0 arcmin.


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