Date and Time of the Query: 2019-05-21 T10:58:51 PDT
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Notes for object NGC 4125

14 note(s) found in NED.

1. 2009A&A...503..409H
Re:NGC 4125
In this elliptical galaxy, Braun et al. (2007) report a continuum source at the
nucleus, which we find is not polarized. They also report a double radio galaxy
just to the southwest, the southern component of which is polarized at about the
5% level. The three double sources in this field provide a very consistent
measurement of the Galactic foreground RM of +19 +/- 1rad m^-2^.

2. 2006ApJ...647..140F
Re:NGC 4125
This galaxy (T2, E6) has only one hard point source at its center surrounded by
diffuse emission. This point source did not have enough counts to justify
fitting various models to its spectrum, but its luminosity was estimated to be
L_0.5-10 keV_ = 9 x 10^38^ ergs s^-1^. This source was not detected in the
radio, but a limit was set: 0.5 mJy at 5 GHz (Wrobel & Heeschen 1991). This
means that log R_X_ < -2.7, so this source could be radio-loud. Due to its
central position and possible radio-loudness, this source could be an LLAGN. We
estimate that the luminosity of the central 2.5" region is L_2-10 keV_ = 6.7 x
10^38^ ergs s^-1^ and the LLAGN has L_2-10 keV_ = 5.4 x 10^38^ ergs s^-1^, i.e.,
~80% of the X-ray luminosity. The remaining X-ray luminosity is contributed by
the diffuse emission.

3. 2006A&A...460...45G
Re:NGC 4125
NGC 4125 (UGC 7118). Figure 5 shows the presence of a nuclear hard point source.
The best fit that Georgantopoulos et al. (2002) obtain for the central 2'
BeppoSAX spectrum is provided by an absorbed power-law with {GAMMA} = 2.52 and
N_H_ = 3 x 10^22^ cm^-2^, providing L(2-10 keV) = 0l.68 x 10^40^ erg s^-1^.
Based on Chandra ACIS imaging, Satyapal et al. (2004) class this galaxy among
those revealing a hard nuclear source embedded in soft diffuse emission; they
estimate the luminosity by assuming an intrinsic power-law slope of 1.8, which
results in (once adjusted to our adopted distance) L(2-10 keV) = 7.3 x 10^38^
erg s^-1^, in very good agreement with the value we estimate.

4. 2005ApJ...635.1031B
Re:NGC 4125
NGC 4125.-The stellar continuum is very weak in this galaxy, despite one of the
longest observations in the sample (Fig. 12). The continuum is so poorly
defined that no Galactic absorption lines can be identified. The night-only
data (40% of the total exposure time) set yields stricter upper limits to the O
VI emission. No emission features from any lines are detected, despite this
galaxy being listed as a LINER and classified as E6 pec.

5. 2002ApJS..142..223F
Re:NGC 4125
NGC 4125. There is no NVSS detection of this source. 1.4 GHz, 18"
resolution observations (Condon et al. 1998b) detect an uncertain 1.8
mJy source. Moderate-resolution observations at 1.4 and 5 GHz (Heckman
1980; Hummel 1980; Hummel et al. 1983) give an upper limit of 10 mJy to
any core emission, while the high-resolution, 5 GHz observations of
Wrobel & Heeschen (1991) establish a 0.5 mJy upper limit.

6. 1998AJ....116.2682C
Re:IRAS 12055+6527
NGC 4125. Elliptical galaxy, LINER spectrum. Both strong radio sources
in Figure 1 are probably background sources.

7. 1995A&A...297..643W
Re:NGC 4125
NGC 4125. This galaxy has dust and ionized gas aligned along the stellar
major axis (Kim 1989). The rotational velocity of the ionized gas is 230
km s^-1^ at a distance of 15" from the center. In addition there may also
be slow rotation along the minor axis (Bertola et al. 1984) indicating
triaxiality. We detect a weak J = 1-0 signal with an inferred H_2_ mass
of ~7x 10^7^ M_sun_. The CO linewidth is 400 km s^-1^. This estimate is
uncertain due to the low S/N in the spectrum, partly due to a resonance
in the 3-mm receiver. We therefore consider this detection as tentative.

8. 1994CAG1..B...0000S
Re:NGC 4125
Feb 6/7, 1981
12 min
An incipient disk exists in NGC 4125 which
is definite but much more subtle than in NGC
3115 (panel 50). It is seen almost edge on, and
is therefore presumed to be more easily identified
as a disk than are disks seen more nearly face on
in other galaxies in this E/S0 section. Indeed, if
a disk exists in nearly face on galaxies it appears
only as a subtle extended envelope.
Note the dust patch on the left side of the
bulge center in the insert print.

9. 1994A&AS..105..481M
Re:NGC 4125
NGC 4125: The diskyness of the isophotes continuously increases
outwards, contrary to the general case of the diE's. The disk is then
classified as "mixed" in the spheroidal envelope.

10. 1994A&AS..105..341G
Re:NGC 4125
The B isophotes are significantly distorted in the inner ~30" due to a
prominent dust lane (see also Kim 1989) which shows signs of warps in its
outer parts. The dust lane is inclined by ~10^deg^ with respect to the
apparent major axis of the galaxy, and more extended to the E side of the
centre. The H{alpha}+[NII] image shows line emission associated with the
dust lane. Detected by IRAS at 60 and 100 microns. Nuclear radio source.

11. 1994A&AS..104..179G
Re:NGC 4125
Prominent stellar disk along the major axis, detectable troughout the
image (i.e., out to r ~ 1.5'). The isophotes are significantly distorted
in the inner 25" due to a prominent major axis dust lane which is warped
in its outer parts (see also Kim 1989). Detected by IRAS at 60 & 100
microns. Nuclear radio source.

12. 1976RC2...C...0000d
Re:NGC 4125
= Holm 335a
Pair with NGC 4121 at 3.6 arcmin
Comm. Padova, No. 98, 1972.
Spectrum and Rotation Curve:
Comm. Padova, No. 98, 1972.
HI 21cm (upper limit):
A.J., 77, 568, 1972.

13. 1973UGC...C...0000N
Re:UGC 07118
E+6 (de Vaucouleurs)
12 05.5 +65 23 = NGC 4121 at 3.9, 195, 0.40 x 0.35, E2 (de Vaucouleurs),

14. 1964RC1...C...0000d
Re:NGC 4125
= Holm 335a
Non-interacting pair with NGC 4121 at 3.6 arcmin.
Ap. J., 132, 325, 1960.
Ap. J., 85, 325, 1937.

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