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Notes for object NGC 4111

16 note(s) found in NED.


1. 2006ApJ...647..140F
Re:NGC 4111
This galaxy (L2, S0) has only one central point source with a hard X-ray
spectrum. There is also a fair amount of diffuse emission. The spectrum
extracted from the central source does not have enough counts to justify fitting
models to it, but the luminosity can be estimated to be L_0.5-10 keV_ = 4.4 x
10^39^ ergs s^-1^ and L_2-10 keV_ = 3.7 x 10^39^ ergs s^-1^. There is a
detection of a central source in the radio with S_5 GHz_ = 2.3 mJy (Wrobel &
Heeschen 1991), which means that log R_X_ = -3. The radio-loudness, the central
position of the source, and the hard X-ray spectrum suggest that this source is
an LLAGN. We evaluated the luminosity of the central 2.5" region to be L2-10 keV
= 4.8 x 10^39^ ergs s^-1^, meaning that the point source contributes to ~77% of
the X-ray luminosity. The age of the stellar population of NGC 4111 was
estimated to be less than 1 Gyr (Gregg 1989).

2. 2006A&A...460...45G
Re:NGC 4111
NGC 4111 (UGC 7103). A hard nuclear point source was detected for this galaxy
(Fig. 5). Previous X-ray spectral analysis comes from ASCA data by Terashima et
al. (2000, see also Terashima et al. 2002) who could not fit the spectrum with a
single-component model, but instead with a combination of a power-law together
with a Raymond-Smith plasma, with {GAMMA} = 0.9, kT = 0.65 keV (in reasonable
agreement with the parameters we estimate from its position in the color-color
diagrams, see Table 4) and N_H_ =1.4 x 10^20^ cm^-2^ reproduced the observed
spectrum well and gives an intrinsic L(2-10 keV) = 6.8 x 10^39^ erg s^-1^, a
factor of 3 higher than the one we estimate (see Table 5).

3. 2006A&A...453...27C
Re:UGC 07103
UGC 7103: we fitted the spectrum with an absorbed powerlaw (N_H_ = 4.6 X 10^22^
cm^-2^ and a photon index {GAMMA} fixed to 1.9) plus a thermal model.

4. 2001AJ....122..653R
Re:NGC 4111
NGC 4111: The central region appears to be composed of a point source,
a peanut-shaped bulge, and a dominant edge-on disk. Since parameterizing
this multicomponent light distribution by a single Nuker law is an extreme
oversimplification, we use the two-dimensional fit only as a guide to
extract the brightness of the nucleus. We consider the specific values of
the Nuker parameters to be unreliable. The archival V-band image shows
fan-shaped dust features emanating perpendicularly from the disk. This is
barely visible in the residual NIR image.

5. 2000ApJ...542..186N
Re:NGC 4111
NGC 4111.-FIRST lists this object's peak 20 cm flux density as
5.8 mJy beam^-1^ at 5" resolution. The emission is extended in
P.A. 70^deg^, along the minor axis of the host galaxy. We did not detect
this object at 2 cm.

6. 1998ApJ...496..133B
Re:NGC 4111
NGC 4111.--This S0 galaxy is nearly edge-on, with i = 87^deg^. Surrounding the
bright, compact nucleus is a dust lane oriented perpendicular to the galaxy's
plane; its morphology is suggestive of a polar ring having a radius of 3".

7. 1997AJ....113..950F
Re:NGC 4111
NGC 4111. The rotation curve of this edge-on S0 displays a rapid rise in the
inner 5". At larger radii a decline is observed in the rotation speed before
rising again and flattening. The effect is large, with a decrease of
{delta}V=40 km s^-1^ between the initial maximum and the minimum. The
minor-axis velocity dispersion profile of NGC 4111 shows a dip in the central
regions suggesting that the rapidly rotating feature seen along the major axis
is kinematically cold. In Fig. 9 radial plots of ellipticity and the
deviations from pure elliptical isophotes (as parametrized by the Cosine
4{theta} term) are given. The nuclear stellar disk dominates the light profile
within the innermost 5" and produces local maxima in these shape parameters
(also note the contour plot in Fig. 10). The surface brightness profile along
the major axis is exponential in the region of the nuclear disk and has a
scale length of 3.7" (300 pc) as compared to the outer disk scale length of
25" (2.1 kpc).
Magnesium line strengths along the major and minor axis of NGC 4111 display
shallow gradients (see Fig. 4 in FFI) throughout the nuclear disk and host
galaxy. These Mg_2_ gradients are amongst the shallowest in our entire sample
and suggest that the stellar population of the nuclear disk is consistent with
that of the main galaxy. The absence of a strong metallicity break in the
region of the nuclear disk would seem to argue for a coeval formation of the
nuclear disk and host galaxy. However, it is also possible to make the case
that the stellar disk is a more recent addition to NGC 4111. Our [O III]
measurements show that there is a gaseous disk in NGC 4111 which extends to a
radius 3 times that of the stellar nuclear disk (see Fig. 10) with high gas
velocity dispersion (reaching 150 km s^-1^) in the region cospatial with the
stellar nuclear disk. A disk of dust is also present within the inner <~10"
(see Fig. 5 in FFI) and the nucleus of NGC 4111 has been classified as a LINER
(Heckman 1980). Thus, the ingredients from which a nuclear stellar disk could
form seem to be present in NGC 4111 and the absorption line strength gradient
might be shallow for the very reason that a lower metallicity nuclear disk has
recently formed. This could account for the fact that the central Mg_2_
strength of NGC 4111 (as measured in FFI) falls 0.02 mag below the mean
Mg_2_-{sigma}_0_ relation of Bender et al. (1993).

8. 1996ApJ...459..110F
Re:NGC 4111
NGC 4111
NGC 4111 is a member of the edge-on subsample. This galaxy displays shallow
Mg_2_ profiles along both the major and minor axes with an enhancement only in
the inner few arcseconds. The color map (Fig. 5) shows the presence of a
compact red nucleus and central disk in this object. Extended [O III] 5007 A
emission is apparent along both the major and minor axes. Bad columns in our
CCD detector prevented Fe5270 and Fe5335 indices from being derived.

9. 1994CAG1..B...0000S
Re:NGC 4111
Hubble Atlas, p. 6
S0_2_(9)
(P)
PH-1854-B
April 17/18, 1958
103aO + GG1
25 min
NGC 4111 is midway between the extreme
example for the decrease in luminosity in the
intermediate region seen in NGC 4215 (left) and
the subtler expression of the effect in the edge-on
galaxy NGC 2549 (panel 40). The decrease in
luminosity between the edge of the bulge and the
beginning of the disk in NGC 4111, seen well in
the insert here, may be due to a weak dust ring
or to a separation of material. The presence of
the decrease calls for the S0_2_ subtype.
The galaxy has a very high rotational
velocity. An early measurement and discussion by
Mayall and Lindblad (1970) gave a velocity
difference between the center and the disk at 30"
distance of 400 km/s, making NGC 4111 one
of the fastest rotators known.

10. 1994CAG1..B...0000S
Re:NGC 4111
Hubble Atlas, p. 6
S0_2_(9)
(P)
PH-1854-B
April 17/18, 1958
103aO + GG11
25 min
[This is] a typical high-surface-brightness S0_2_ disk galaxy.

11. 1994A&AS..105..481M
Re:NGC 4111
NGC 4111: A typical edge-on, disk dominated, S0 with a "peanut bulge"
possibly due to a polar dust ring. See Paper I for graphs and references,
and MS93 for modelling of the minor-axis asymmetry.

12. 1993ApJS...86....5K
Re:NGC 4111
NGC 4111; S0, LINER.
NGC 4111 is a normal S0 galaxy with an old stellar population (cf. Gregg
1989), showing Mg II and Fe absorption features longward of 2600 A which
are typical of F-G dwarfs. The short- wavelength spectrum is lacking a
hot star component (Burstein et al. 1988). Although NGC 4111 has at
least eight much fainter companions, they have no apparent effect on the
galaxy itself (van der Burg 1985). NGC 4111 is classified as a LINER by
Heckman( 1980), but there is little evidence of nonthermal activity from
the UV spectrum. NGC 4111 may be on the boundary between active and
normal galaxies.

13. 1976RC2...C...0000d
Re:NGC 4111
= Holm 333a
Pair with NGC 4109 at 4.8 arcmin
Photometry:
Atti. Conv. Sci. Osserv. Cima Ekar, Padova-Asiago, p.101, 1973
= Cont. Asiago No. 300b.
Spectrum and Velocity Dispersion:
IAU Symp. No.15, p.112, 1962.
Rotation Curve and Mass Determination:
Astr. Ap., 8, 364, 1970.
Cont. Asiago Obs. No. 300bis, 101, 1973.

14. 1973UGC...C...0000N
Re:UGC 07103
SA(r)0+: (de Vaucouleurs), S0 (Holmberg)
Brightest in a subgroup
{12 04.3} +43 16 = NGC 4109 at 4.6, 206, 0.6 x 0.5, m=15.1
{UGC incorrectly notes: "12 04.5". H. Corwin}

15. 1964RC1...C...0000d
Re:NGC 4111
= Holm 333a
Very small, very bright nucleus cut by a dark lane. Extremely thin, smooth,
equatorial component. Traces of ansae or (r?): 0.7 arcmin x - in a lens:
1.0 arcmin x 0.2 arcmin.
Pair with NGC 4109 at 4.8 arcmin.
Photograph:
B.A.N., 16, 1, 1961.
Photometry:
M.N.R.A.S., 98, 619, 1938.
B.A.N., 16, 1, 1961.
Spectrum:
I.A.U. Symp., No. 5, 1958 = Lick Contr.II, No. 81, 1958.
Ap. J., 135, 734, 1962.

16. 1961Hubbl.B...0000S
Re:NGC 4111
S02
H-1751-H
May 24/25, 1936
Imp. Ecl.
15 min
Enlarged 8.2X
NGC 4111 is classified as an S02 seen on edge. The nucleus,
lens, and outer envelope are all easily visible on the
original plate and can probably be made out in this
illustration. The surface brightness of the lens is not uniform,
but two absorbing streaks appear, in projection,
perpendicular to the fundamental plane. They cross the lens
near its junction with the nucleus. Such a pattern would
be reproduced if NGC 3065 were seen on edge. The internal
absorption lane of the galaxy would then appear
silhouetted against the bright background.


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