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Date and Time of the Query: 2019-02-20 T21:27:38 PST
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Notes for object NGC 7177

15 note(s) found in NED.


1. 2012ApJ...754...67F
Re:NGC 7177
NGC 7177 .SXR3..-A nuclear bar extends out to about r = 10". The bulge is
classified as a pseudobulge by Fisher & Drory (2010). The flattening of the
major axis rotational velocity coincides with bulge radius of r_b_ = 8.6". The
velocity dispersion rises from about 50 km s^-1^ in the disk to values of ~=115
km s^-1^ inside the bulge but remains relatively flat inside the bulge radius.
The h_3_ moments are weakly anti-correlated with velocity but remain small. The
h_4_ moments drop to values of -0.05 at ~= +/- 5". The minor axis shows an
asymmetric velocity profile with values of up to +/- 25 km s^-1^. The minor axis
velocity dispersion again rises from about 50 km s^-1^ in the disk to values of
about 115 km s^-1^ at 2.5" and remains flat inside. The h_3_ moments are
anti-correlated with velocity. The h_4_ moments are noisy and scatter around
zero.

2. 2008MNRAS.388..500E
Re:UGC 11872
UGC 11872 (NGC 7177). Our H{alpha} map has a mottled appearance, in agreement
with that of James et al. (2004); however, our observations suffer from bad
seeing conditions. Our H{alpha} rotation curve rapidly reaches a well-defined
and symmetric plateau, extending up to the optical radius. The rotation curve
obtained by Marquez et al. (2002) reaches the plateau more rapidly (10 arcsec
instead of 20 arcsec) but they find it at a lower value since they assume a
surprisingly high inclination (79^deg^, while we find 47^deg^from our H{alpha}
velocity field, which is closer to the morphological value of 54^deg^).
Furthermore, slit spectroscopy of the inner part of the galaxy by Heraudeau et
al. (1999) confirms that the maximum velocity is not reached before 20 arcsec.
No H I velocity map is available in the literature; however, H I linewidths have
been measured (314 km s^-1^ from Springob et al. 2005, 317 km s^-1^ from
Bottinelli et al. 1990) and are in agreement with our H{alpha} velocity field
amplit ude. Moreover, a radio synthesis observation has been done (Rhee & van
Albada 1996) to derive a position-velocity diagram. It shows a solid body
rotation as far out as 1 arcmin which is likely to be explained by beam smearing
effects.

3. 2005MNRAS.364..283E
Re:NGC 7177
NGC 7177. Bar and disc measurements are from an archival INT-WFC R-band image.
The outer-disc scalelength is from the r= 35-60 arcsec region and agrees very
well with measurements by de Jong & van der Kruit (1994) and Graham (2001).
Outside this region, the profile flattens; this is another Type III profile.

4. 2004MNRAS.350.1087S
Re:NGC 7177
NGC 7177: the surface brightness profile lies below the R^1/4^ law for
r< 3.8 arcsec; this behaviour cannot be explained in terms of a seeing
effect: we have computed the expected light distribution for a pure
R^1/4^ bulge with r_e_{approx} 6.5 arcsec convolved with the same seeing
PSF (about 1.2 arcsec FWHM) finding that the expected profile flattening
begins about r{approx} 0.65 arcsec. Therefore, the observed flattening
seems to be an intrinsic bulge characteristic.

5. 2003PNAOJ...7...37M
Re:KUG 2158+174
A bright knot is at the south of the disk. The nucleus is red.

6. 2003ApJS..146..353M
Re:NGC 7177
NGC 7177 (CS)
Almost all of the circumnuclear dust structures are to the south of
the nucleus, and several of the dust lanes imply the same sense of
rotation.

7. 2002ApJS..142..223F
Re:NGC 7177
NGC 7177. NVSS reports a 28 mJy source consistent with the 1.4 GHz, 54"
resolution observations of Condon (1987). Hummel et al. (1987)
establish an upper limit of 0.8 mJy to any emission at 1.4 GHz, 1.3"
resolution. We detect a somewhat resolved 0.8 mJy core, in the center
of the optical galaxy; comparison with the integrated NVSS flux density
otherwise indicates strong resolution effects.

8. 2002AJ....123..159C
Re:NGC 7177
Red (dust) disk/spiral-like lanes across center; blue large-scale bar

9. 1999A&AS..138..253B
Re:NGC 7177
NGC 7177 - SNe 1960L, 1976E: at the location of SN 1960L some patches
are seen. A blue one is seen at the location of the supernova, brighter
than a 5{sigma} detection. As already discussed the position of
SN 1960L is accurately known from Porter (1993) and thus the
identification of a blue patch at the location of the supernova is of
great interest and calls for further investigation. At the site of
SN 1976E a very bright and red compact object is observed. SN 1960L is
classified as a candidate (see Table 3).

10. 1999A&AS..138..253B
Re:NGC 7177
NGC 7177 - SNe 1960L, 1976E: at the location of SN 1960L some patches
are seen as in the JKT observations. A blue one is seen at the location
of the supernova and is within a 3{sigma} detection limit. SN 1960L is
classified as a candidate (see Table 3).

11. 1994CAG1..B...0000S
Re:NGC 7177
Sab(r)II.2
PH-7670-S
Sep 25/26, 1979
IIIaJ
75 min
The multiple-armed, fragmented spiral structure in NGC 7177 is
similar to that in NGC 488 in the outer regions but differs in the
inner. As shown in the insert, the inner arms begin on the rim of an
inner near-ring of high surface brightness.
The tightness of the outer arms, their thinness, and the
only-moderate recent star-formation rate explain the Sab morphological
classification.

12. 1973UGC...C...0000N
Re:UGC 11872
SAB(r)b (de Vaucouleurs)

13. 1964RC1...C...0000d
Re:NGC 7177
Extremely bright nucleus. Smooth (r): 0.5 arcmin x 0.3 arcmin in a lens:
1.3 arcmin x 0.8 arcmin. Many filamentary knotty arms.
Heidelberg Veroff. Vol. 9, 1926 dimensions are for the bright part only.
Description:
Ap. J., 46, 54, 1917.
SN 1960
P.A.S.P., 73, 175, 1961.

14. 1961AJ.....66..562V
Re:NGC 7177
7177 Isolated Sb. Has peculiar outer arm.

15. 1918PLicO..13....9C
Re:NGC 7177
Bright, compact, slightly oval spiral 3' long in p.a. 80^deg^. Nucleus rather
large and indistinct; no condensations in the whorls. 17 s.n.


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