Date and Time of the Query: 2019-05-19 T09:48:14 PDT
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Notes for object NGC 2775

16 note(s) found in NED.

1. 2012ApJ...754...67F
Re:NGC 2775
NGC 2775 .SAR2..-The HST F606W image shows a very clear classical morphology,
the F450W image shows very little amounts of dust in the central region. We see
a depression in the velocity dispersion profile inward of 5" in the major axis
profile as well as in the minor axis profile which coincides with a steeper part
in the rotation curve. Eskridge et al. (2002) describe a large, slightly
elliptical bulge which contains a bright nuclear point source. The Spitzer MIPS
24 {mu}m image shows a resolved nuclear source of emission which clearly stands
out from a region of low emission which again in size roughly corresponds to the
bulge radius. This may hint at a cold nuclear component with active star
formation which dominates the kinematics. We exclude the data inward of 5" from
our analysis but note that this choice does significantly affect the position of
NGC 2775 in the plane of Sersic index versus velocity dispersion slope.

2. 2008MNRAS.388..500E
Re:UGC 04820
UGC 4820 (NGC 2775, KIG 309). H{alpha} imaging from Hameed & Devereux (2005) is
comparable with our data, showing a flocculent ring of H{alpha} emission.
Stellar dynamics from Kregel, van der Kruit & Freeman (2005) suggest a maximum
velocity of 283 km s^-1^ lower than that suggested by the H{alpha} kinematics.
No H I velocity map is available in the literature. The width of the H I profile
at 20 per cent (435 km s^-1^ from Bottinelli et al. 1990) is in agreement with
our H{alpha} velocity field amplitude.

3. 2008A&A...487..485H
Re:KIG 0309
CIG 309. The NED classification for this galaxy is SA(r)ab. Tight arms with
strong inner star forming regions and dust lanes can be appreciated forming a
ring that encloses a uniformly redder and soft bulge. Our optical images as well
as the RGB color image show how the spatial distribution of the inner star
forming regions and dust lanes trace the arms. A few small galaxies (square
symbols) can be appreciated in the neighborhood of this galaxy. The total B-V
color index is representative of the E/S0 types. We classify this galaxy as

4. 2007AJ....134.2286H
Re:KIG 0309
CIG 309: The galaxy was classified as SA(r)ab (NED). The optical and JHK images
show an inner and outer ring. The optical images show an intermediate region of
strongly wound and knotty arms. The total (B - V) color is representative of
S0Sa types. We classify this galaxy as RS(r)a. The smooth behavior of the
photometric I- and JHK-band ({epsilon} and P.A.) is consistent with an
early-type galaxy.

5. 2005ApJS..157...59L
Re:NGC 2775
This nearly face-on ring Sab spiral galaxy (at a distance of 17.0 Mpc) shows
multiple arms of fine structure. ULX1 is on the outer edge of the galaxy
and close to a faint object with B2 = 21.58 mag and R2 = 20.15 mag.

6. 2002ApJS..143...73E
Re:NGC 2775
NGC 2775.---S0/a: Very bright nuclear point source embedded in large
slightly elliptical bulge. Disk extends from bulge with nearly the
same isophotal shape. There is evidence for two very faint, symmetric
spiral dust absorption bands in the outer disk.

7. 2001ApJS..137..139S
Re:NGC 2775
NGC 2775 and NGC 2777. - We use an H_0_ distance, based on the mean
velocity of the two group members.

8. 2001A&A...368...16M
Re:NGC 2775
8. NGC 2775 is an Sa galaxy of low inclination. The nearly perfect
residuals show nicely the fine structure of the highly multiple arms
(Fig. 3). Corsini et al. (1999) measured the profile of the stellar
velocity dispersion of the bulge of NGC 2775: their radius of ~50"
coincides well with our value (32") for the effective radius.

9. 1994CAG1..B...0000S
Re:NGC 2775
Hubble Atlas, p. 10
Dec 30/31, 1989
103aO + GG385
60 min
The place of NGC 2775 in the Sa section is
later than that of NGC 4698, above, because the
spiral pattern is more fully developed. However,
it is earlier than NGC 4699, at the upper right,
because the bulge for NGC 2775 here is smooth
and provides no evidence of spiral arms. In NGC
4699 the arms exist throughout the bulge and
reach very close to the center of the very inner
disk, burned out in the reproduction here.
The spiral-arm pattern in NGC 2775 is
highly multiple. It starts abruptly at the edge of
the smooth central bulge. Several small knots
exist in some of the bright fragments of arms,
especially in the lower-left section of this print.
Most of these knots are invisible on a companion
Las Campanas yellow (103aD + GG495) plate.
Hence, the knots are likely to be HII regions,
indicating a low but finite rate of recent star
The remarkable outer dust lane surrounding
the entire pattern is not well seen in the
low-contrast print here, but it is well seen in the
negative print in the Sa summary, panel 87, if the
print is viewed from a distance.

10. 1994CAG1..B...0000S
Re:NGC 2775
Hubble Atlas, p. 10
Dec 30/31, 1980
103aO + GG385
60 min
NGC 2775 is the latest Sa of the MAS type
with fragmentary arms shown in this atlas. It is
the late-Sa example of the NGC 2841 (Sb; Hubble
Atlas, p. 14; panels 142, S4, S12 here)
multiple-armed forms in the Sb section, and NGC
628 (Sc; Hubble Atlas, pp. 29, 31; panel 220
here) or NGC 1232 (Sc; Hubble Atlas, p. 32;
panels 216, S13 here) in the Sc section. As was
emphasized in commentaries in the Hubble Atlas
and now throughout this atlas, both the MAS and
the grand design strains of spiral structure can
be traced separately along the entire spiral
sections of the classification sequence, in both
the ordinary and the barred spirals.
A summary of the grand design Sa
prototypes is on the next panel.

11. 1993A&AS...97..887B
Re:NGC 2775
NGC 2775 is a ringed Sa galaxy reported as detected by Y89 and a dubious
detection by PR. The velocity given by Y89, 1135 km/s, is at the edge of
the HI profiles (Haynes 1981; Balkowski & Chamaraux 1983) which is rather
odd. We consider our observations to be non-detections in both lines. One
should note that the HI column density is low, making it a galaxy with
very little gas if the CO "detection(s)" are inaccurate. The IRAS flux
densities are quite low and the dust is cold. P89 found no ionized gas in
or near the nucleus and K83 classified it as a LINER but commented that
the data were poor. NGC 2775 may be interacting with
NGC 2777(12'= 58 kpc away) but shows no signs of disturbance.

12. 1976RC2...C...0000d
Re:NGC 2775
Pair with NGC 2777 at 11 arcmin

13. 1973UGC...C...0000N
Re:UGC 04820
SA(r)ab (de Vaucouleurs)

14. 1964RC1...C...0000d
Re:NGC 2775
Small, bright, diffuse nucleus in a bright smooth lens: 0.8 arcmin x 0.6 arcmin.
Many knotty branching arms form (r): 1.4 arcmin x 1.1 arcmin. Strong, narrow,
outer dark lane.
Pair with NGC 2777 at 11 arcmin.
Ap. J., 127, 487, 1958.

15. 1961Hubbl.B...0000S
Re:NGC 2775
Mar. 24/25, 1939
Agfa Blue
80 min
Enlarged 9.2X
This beautiful spiral is similar to NGC 3898. The spiral
pattern is more easily seen because NGC 2775 is observed
almost face on. Notice that the arms cannot be traced as
individual structures but rather as separate segments, as
is true in all multiple-arm galaxies of types Sa and Sb.
The arms, with their associated dust lanes, start abruptly
at the edge of a completely amorphous central nucleus
and lens. The boundary between the lens and the spiral
structure is sharp.
Note the thin dust lane on the outside of the entire pattern
(about 45 mm from the center on this illustration,
along the major axis).

16. 1918PLicO..13....9C
Re:NGC 2775
A fine, slightly oval spiral 2.1' long; there il!l a stellar nucleus surrounded
by relatively bright matter; outside this are faint, delicate, nearly merging
spiral whorls. 31 s.n.

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