Date and Time of the Query: 2019-05-24 T03:21:59 PDT
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Notes for object NGC 4570

11 note(s) found in NED.

1. 2006MNRAS.369..497K
Re:NGC 4570
This edge-on S0 galaxy features multiple kinematic components such as an outer
and a nuclear disc (van den Bosch & Emsellem 1998). The Mg b map and to a lesser
extent the Fe maps show a central peak surrounded by a region depressed in line
strength. At larger radii, the onset of the outer disc, showing strong metal
lines, can be seen. The H{beta} map is relatively flat.

2. 2006MNRAS.366.1151S
Re:NGC 4570
This object displays several scattered sources of emission. The observed
emission is characterized by narrow lines, which appear to trace gas clouds
coherently rotating in the same sense as the stars. We found no traces of dust
in the HST image, where the nuclear disc studied by van den Bosch, Jaffe & van
der Marel (1998) is clearly visible.

3. 2006ApJS..164..334F
Re:VCC 1692
VCC 1692 (NGC 4570).This galaxy shows a thin, circumnuclear stellar ring,
centered on the nucleus (which appears resolved), extending just less than 2" on
either side and aligned with the main body of the galaxy. Although almost
edge-on, the structure indeed appears to be a ring rather than a disk; an inner
gap is apparent from the images. The ring is bluer than the surrounding galaxy.
The galaxy is very elongated, with a thin, edge-on disk that appears to become
slightly thicker toward the center, where it joins the main bulge.

4. 2006ApJ...639...95P
Re:VCC 1692
VCC 1692.The blue and red GCs are particularly well separated in color.

5. 2004MNRAS.352..721E
Re:NGC 4570
NGC 4570: The inner part of the velocity field and h_3_ map suggest the
presence of a fast rotating disc-like structure. This component was also
seen in long-slit observations (van den Bosch, Jaffe & van der Marel
1998) and interpreted as due to bar-driven evolution (van den Bosch &
Emsellem 1998).

6. 1994CAG1..B...0000S
Re:NGC 4570
VCC 1692
May 27/28, 1925
50 min
There is no sharp disk in NGC 4570 as
there is in NGC 3115. Nevertheless, the original
plate shows a clear separation between bulge and
envelope, slightly burned out in the facing print.
A diffuse disk is present, and the luminosity
profile from the bulge outward is not continuous
in its first derivative as in E galaxies, but the S0
zone form is subtly evident.

7. 1994AJ....108.1579v
Re:NGC 4570
NGC 4570 shows a strong decrease in ellipticity, running from 0.55 at
15" to 0.2 at 1.4" after which the ellipticity increases again to
{epsilon} ~0.35 at 0.5". The position angle remains fairly constant. The
cos 4{theta} terms shows remarkable behavior. Going outward, the
isophotes start slightly disky, become boxy around 3" and become disky
again at larger radii. The residual image [Fig. 7(a)] clearly reveals a
disky structure of ~2.8" in diameter, aligned with the main body of the
galaxy. The diskiness of the isophotes outside 9" is also due to a disk
(see Sec. 3.7), and we therefore conclude that NGC 4570 closely resembles
a lenticular (as defined by van den Bergh 1990), harboring a small
nuclear disk in addition to its main disk. The small irregular variations
of order 3% in the 3{theta} profile for 0.5" < a < 3" may indicate faint
dust patches at these radii.

8. 1994A&AS..105..481M
Re:NGC 4570
NGC 4570: This is a case of "E - like S0" with the disk embedded in a
spheroidal halo (although the axis-ratio remains below 0.5 in the
measured range).

9. 1976RC2...C...0000d
Re:NGC 4570
Ap. J., 146, 28, 1966.

10. 1973UGC...C...0000N
Re:UGC 07785
S0 (de Vaucouleurs)

11. 1964RC1...C...0000d
Re:NGC 4570
Small, very bright nucleus. Bright, diamond-shaped lens.
M.N.R.A.S., 94, 806, 1934.
Ap. J., 132, 306, 1960.

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