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Date and Time of the Query: 2019-06-24 T10:46:05 PDT
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Notes for object NGC 2805

8 note(s) found in NED.


1. 2008MNRAS.390..466E
Re:UGC 04936
UGC 4936. The inclination found now is 17^deg^ lower than the one published
in Paper III. This value is more compatible with the absolute magnitude of the
galaxy as well as its optical radius.

2. 2007MNRAS.380..506G
Re:NGC 2805
NGC 2805 is an Sd galaxy seen nearly face-on and it is the brightest member of a
multiple interacting system containing also NGC 2814 (Sb), NGC 2820 (Sc) at 13
arcmin and IC2458 (I0). H I has been detected (Reakes 1979; Bosma et al. 1980)
and there are claims that the outer H I layers are warped (see e.g. Bosma et al.
1980). The galaxy seems to be also optically disturbed, since the spiral arms
appear to be broken up into straight segments.
The line strength maps are rather patchy, displaying though a central peak in
all three lines. By comparison of our measured indices with SSP models, we can
state that the ages are young-intermediate over most of the field; that the
metallicity peaks in the centre and that abundance ratios are supersolar.
The analysis of the {DELTA}{chi}^2^ contours, in the continuous star
formation approach, shows that this galaxy is not very well described by an SSP,
and that even a constant SFR cannot be excluded at all ages (see Fig. 29, sixth
column).

3. 2004MNRAS.349..225G
Re:UGC 04936
4.8 UGC 4936 This Sd galaxy belongs to the Ho124 group which contains
four galaxies. There is much ionized gas in the centre and some H II
regions all along the two spiral arms. The centre of rotation
corresponds to the nucleus on the continuum map. The rotation curve is
quite regular and symmetric, and reaches 70 km s^-1^ at 30 arcsec, then
rising slowly up to 85 km s^-1^ (beyond 120 arcsec). On the isovelocities
map, we can see that the position of the major axis is changing with the
radius. The approaching side rises beyond 120 arcsec up to 120 km s^-1^,
confirming the warp pointed out by the H I velocity field derived by
Bosma et al. (1980). The warp of this galaxy is likely to be caused by
one its neighbours: UGC 4952, IC 2458 and UGC 4961 are found
respectively at 10.3, 11.2 and 13.2 arcmin from UGC 4936 (with 1631,
1534 and 1574 km s^-1^ in recession velocity versus 1730 km s^-1^ for UGC
4936).

4. 2002AJ....124..675C
Re:UGC 04936
F09162+6418 is offset from the nucleus but is near the centroid of the
NVSS source.

5. 1976RC2...C...0000d
Re:NGC 2805
= Holm 124b
Multiply interacting system with NGC 2814.
NGC 2820 at 13 arcmin and IC 2458.

6. 1973UGC...C...0000N
Re:UGC 04936
SAB(rs)d (de Vaucouleurs), Sc+ (Holmberg)
Slightly asymmetric, row of bright patches opposite companions
UGC 04952 at 10.7
UGC 04961 at 13.2
09 17.5 +64 27 = IC 2458 at 11.2 north-following, 0.5 x 0.2, m=15.1

7. 1964RC1...C...0000d
Re:NGC 2805
= Holm 124b
In multiple interacting system with NGC 2814 and NGC 2820 at 13 arcmin.
Very small, bright nucleus in center of pseudo (r): 1.5 arcmin x 1.0 arcmin.
Many irregular, resolved, very faint, knotty arms. Similar to Messier 101.

8. 1956AJ.....61...97H
Re:NGC 2805
HMS Note No. 055
Nuclear absorption lines, and emission lines from area where slit
crossed spiral arm approximately 35 arcsec [west] of nucleus.
Nebula is among those listed
by Holmberg, E.E. 1950, Medd. Lunds Astr. Obs., Ser. II, No. 128.
as possible members of the M81 Group.
The redshift rules out membership.


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