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Date and Time of the Query: 2019-06-16 T20:35:38 PDT
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Notes for object NGC 4941

12 note(s) found in NED.


1. 2007AJ....134..648M
Re:NGC 4941
NGC 4941 (Figs. 7.54, 9.54, 20.54): This shows extended emission crossed by dark
dust lanes. The nucleus has a compact clumpy structure with a bright compact
core.

2. 2005MNRAS.364..283E
Re:NGC 4941
[NGC 4941].Greusard et al. (2000) argued that this galaxy has a nuclear bar but
no large-scale bar, based on their near-IR images; on the other hand, Eskridge
et al. (2002) classified it as SAB using lower-resolution H-band images, so it
is not clear whether this is a single- or double-barred galaxy.

3. 2004A&A...415..941E
Re:NGC 4941
NGC 4941: Greusard et al. (2000) found a nuclear bar in their near-IR images of
this SABab galaxy, but argued that there was no outer bar. On the other hand,
Eskridge et al. (2002) classify the galaxy as SAB based on their low-resolution
near-IR images, and Kormendy (1982b) includes it in his list of galaxies with
"oval disks", so it may be similar to NGC 1068 and NGC 4736: a galaxy with a
strong inner bar and a weak outer bar. For the time being, the evidence for an
outer bar remains too tenuous to classify this as a double-barred galaxy.

4. 2003ApJS..146..353M
Re:NGC 4941
NGC 4941 (LW)
This is a prototype of the loosely wound spiral class and also
illustrates the effect of galaxy inclination on the relative contrast
between dust features on the near and far sides of the galaxy.

5. 2002ApJS..143...73E
Re:NGC 4941
NGC 4941.---SABa: Marginally resolved nucleus in an elliptical bulge
with a strong isophotal twist. Smooth, low-contrast, bisymmetric
two-armed spiral pattern emerges from the major-axis ends of the
bulge. Arms can be traced for ~180deg before fading into the ambient
disk.

6. 2002ApJS..139....1T
Re:NGC 4941
NGC 4941 (S2). -The observed luminosity of this Seyfert 2 galaxy
before correction of absorption is only 6.4 x 10^39^ ergs s^-1^, which
is among the weakest Seyfert 2s observed thus far in the
X-rays. Comparing with the results obtained with BeppoSAX
(Maiolino et al. 1998) suggests variability of the absorption column.

7. 2001ApJS..132..199S
Re:NGC 4941
4.2.21. NGC 4941
Maiolino et al. (1999) presented the X-ray spectrum of this galaxy,
which has a soft band flux F_0.5-2 keV_ = 2.08 x 10^-13^ ergs cm^-2^ s^-1^,
a hard band flux F_2-10 keV_ = 6.63 x 10^-13^ ergs cm^-2^ s^-1^, and can be
fitted with a power law absorbed by a column density
N_H_ = 4.5 x 10^23^ cm^-2^. The [O III] emission (Pogge 1989) has a
halo-like morphology, and the H{alpha} image shows H II regions along the
spiral arms. This is the smallest extended source in our sample, presenting
a double radio source extended by 15 pc along P.A. = -25^deg^. This source
was only slightly resolved in previous radio observations
(Ulvestad & Wilson 1989).

8. 1994CAG1..B...0000S
Re:NGC 4941
Hubble Atlas, p. 10
Sab(s)II
CD-1310-S/Br
March 11/12, 1980
103aO + GG385
60 min
The multiple-fragment pattern of the spiral arms in NGC 4941 is
similar to, but not as pronounced as, the individual fragments in NGC
0488 (preceding two panels), which define the MAS class. The dust
lanes, generally on the inside of the luminous arms, as usual, are
seen more clearly on one side of the image than the other, presumably
owing to different silhouetting against the disk on the near (bottom)
and far sides.
A set of very-low-surface-brightness outer arms exist that can
just be traced in the negative insert print on this panel.

9. 1974UGCA..C...0000N
Re:UGCA 321
UGCA 321:
= NGC 4941
(R)SAB(r)ab: (RC1)

10. 1964RC1...C...0000d
Re:NGC 4941
Small, very bright nucleus in weak diffuse bar. Knotty (r): 1.7 arcmin x
0.8 arcmin in lens: 2.4 arcmin x 1.05 arcmin. Extremely faint (R) (or outer
whorls): 3.1 arcmin x 2.4 arcmin.
Heidelberg Veroff., Vol. 9, 1926, Lund 9, and all Helwan dimensions are for the
bright part only.

11. 1963MCG3..C...0000V
Re:MCG -01-33-077
Very thin, clear arms inside a bright disk. Type: Sand - Sa, vB -
Sbp. Red shift: +729, F8. Photo: Sand (Sa/Sb) - "difficult to classify
because of conflicting criteria. The spiral arms are tightly wound.
There are only two arms, and they overlap after each has turned through
180 degrees. There is little or no dust in the arms, which are
relatively smooth textured with not much resolution into lumps or HII
knots. The arrms therefore suggest a classification of Sa. The nucleus
is very small, however, suggesting a classification of Sb or even Sc.
This galaxy shows that the three classification criteria are not always
consistent." This is not the first note in Sandage which claims the
nonapplicability of the classification of Hubble and the others. The
more the galaxy is examined, the clearer it becomes, which made us
depart from the catalogue classifications, and instead describe the
galaxy. The photo in Sandage agrees with our description. A possible
description would be [L; Lab; 2Sffab --> R]. In the improved photo with
the middle overexposed it is [Ne; H or Ne; Da], where in [Ne] is a hidden
inside structure.

12. 1961Hubbl.B...0000S
Re:NGC 4941
Sa/Sb
S-1655-H
May 4/5, 1937
Imp. Ecl.
50 min
Enlarged 10.2X
This galaxy is difficult to classify because of conflicting
criteria. The spiral arms are tightly wound. There are
only two arms, and they overlap after each has turned
through 180". There is little or no dust in the arms,
which are relatively smooth textured with not much resolution
into lumps or HII knots. The arms therefore suggest a
classification of Sa. The nucleus is very small, however,
suggesting a classification of Sb or even Sc. This
galaxy shows that the three classification criteria are not
always consistent.


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