Date and Time of the Query: 2019-04-20 T08:21:39 PDT
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Notes for object NGC 0541

8 note(s) found in NED.

1. 2003ApJS..148..419N
Re:NGC 0541
NGC 541 (UGC 1004).-This cD S0 galaxy has a nuclear dust disk (b/a =
0.91). It has a radio core on VLBA scales and a core-jet morphology on
VLA scales. The STIS slits were aligned to a mean of the position angles
of the central isophotes measured from our WFPC/2 images, which vary
considerably. We allowed considerable flexibility in position angle to
enable reasonable observing windows. The central kinematic and flux
properties are listed in Table 9; the gas does not exhibit a regular
rotation profile. The fit to the central spectrum is not significantly
improved by the addition of a broad component, though the fit improves
somewhat when judged by eye. Data for this galaxy are shown in Figure 5
(see key in Fig. 1 for an explanation of these plots).

2. 2002AJ....124..675C
Re:UGC 01004
Very extended head-tail radio source (O'Dea & Owen 1985); the 1.4 GHz
flux density is from Condon & Broderick (1988).

3. 2000AJ....120.2950X
Re:UGC 01004
UGC 01004 (NGC 541)-A weak radio core was detected in this source,
which may be marginally resolved in our VLBA image.

4. 1999AJ....118.2592V
Re:NGC 0541
NGC 541 is located in Abell cluster 194 (Abell, Corwin, & Olowin
1989). It is located at 4.5' (96 kpc) from the dumbbell pair NGC 545 /
NGC 547, identified with the radio source 3C 40. NGC 541 has a central
disk (diameter 640 pc/1.8"), which appears to be nearly face-on. The
disk has an outer rim that is darker, especially on the north side.
There is also an inner ring with a radius of ~0.22" (78 pc) that shows
enhanced obscuration. These darker ringlike structures could be part of
an otherwise hardly visible spiral structure. The V-I image shows a hint
of a linear dust feature with P.A. ~ 267^deg^ sticking out of the disk.
This is within 10^deg^ of the VLA radio jet axis (CB88). At the center
of the dust disk there is a central H{alpha} + [N II] emission peak. A
ring of emission surrounds the peak just inside the darker rim of the
disk. There is a slightly brighter emission spot at P.A. ~ 51^deg^ and
on the opposite side in the ring. The central pixels are slightly bluer
than their surroundings. Our isophotal analysis agrees well with the
study by De Juan et al. (1994). They find that the abrupt increase in
ellipticity outward of ~10" continues until 0.2 at 20", and they find a
rise in the fourth-order Fourier coefficient c_4_ to 0.02 at ~25". The
radio jets form a small head-tail source (O'Dea & Owen 1985) that might
have triggered the starburst in Minkowski's object, an irregular dwarf
located in the path of the jet at 45" (16 kpc) northeast of NGC 541
(van Breugel et al. 1985).

5. 1999A&AS..136...35S
Re:Minkowski's Object
Minkowski's Object -- A weak broad He II {lambda}4686 feature and
possible nebular He II has been found by Breugel et al. (1985) in this
"starburst triggered by a radio jet". They also point out a close
similarity of the emission line spectrum with the NGC 7714, a
prototypical starburst galaxy.

6. 1994ApJS...91..507D
Re:NGC 0541
NGC 541 - This is an elliptical galaxy located in the cluster Abell 194.
It is associated with PKS 0123-016A, a small headtail radio source (van
Breugel et al. 1985) near the larger and more powerful radio galaxy 3C 40
(PKS 0123-016B), which is associated with the nearby dumbbell system
NGC 545/547.
The parameters are described below:
1. Large gradients in ellipticity. This galaxy shows rounder isophotes
in the inner 10" and an increase of {DELTA}{epsilon}~0.2 between 10" and
2. Nonconcentric isophotes. The isophote centers keep constant until
r~14", moving then to the southwest, being the outer isophotes (e.g.,
at r~45") displaced 3.7".

7. 1976RC2...C...0000d
Re:NGC 0541
= Arp 133
In the cluster Abell 0194, including NGC 0535, NGC 0545, NGC 0547, and NGC 0548.
Peculiar distorted system 0.8 arcmin north-following.

8. 1973UGC...C...0000N
Re:UGC 01004
See UGC 00997
2 faint objects in the envelope at 1.0 following and 0.9 north-following center
Arp 133

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