Date and Time of the Query: 2019-05-23 T23:25:50 PDT
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Notes for object NGC 4697

17 note(s) found in NED.

1. 2009MNRAS.397.2148G
Re:NGC 4697
The nuclear dust disc in this galaxy was masked out prior to the extraction of
the light profile (Byun et al. 1996). In Fig. A5, we have simultaneously fit the
inner component of NGC 4697's surface brightness profile, taken from Byun et al.
(1996), with an n= 1 Sersic model and the main galaxy with an n= 4 Sersic
model (Soria et al. 2006). This yields a magnitude for the inner component of
17.5 F555W-mag and a half-light radius of 4.4 pc. Using a distance modulus of
30.34 (Tonry et al. 2001) and V-F555W= 0.0 (Fukugita, Shimasaku & Ichikawa
1995), one obtains an absolute magnitude of -12.8 V-mag. Based on the properties
of the preceding galaxies, we have adopted M/L_V_= 2.5 for the NC.

2. 2009ApJ...703.1034Y
Re:NGC 4697
NGC 4697. This is another good source to test the prediction of YC05 since the
luminosity is again extremely low. Consistent with YC05, the X-ray spectrum is
fitted very well by a jet. Like NGC 4621, the application of the correlation of
YC05 (Equation (3)) predicts the observed radio flux to be {nu}L_{nu}_(8.5 GHz)
= 3.5 * 10^35^ erg s^-1^, which agrees well with the observed value of
{nu}L_{nu}_(8.5 GHz) = 1.3 * 10^35^ erg s^-1^, as pointed out by Wrobel et al.

3. 2005ApJS..157...59L
Re:NGC 4697
This E6 elliptical galaxy at a distance of 11.75 Mpc has an appreciable globular
cluster population. ULX1 is on the outer edge of the galaxy and coincident with
a faint object with B1 = 18.81 mag, R1 = 19.15 mag, B2 = 19.39 mag, and R2 =
19.04 mag. It showed a luminosity drop from 3.4 * 10^39^ to below 0.4 * 10^39^
ergs s^-1^ between two observations over 1 year.

4. 2005ApJ...635.1031B
Re:NGC 4697
NGC 4697.-The redshift of this galaxy would place the redshifted O VI
{lambda}1032 line (1036.2 A) into the strong Galactic C II absorption line
(1036.34 A). There is no strong line to the blue side of the C II line (Fig.

5. 2001ApJ...556..533S
Re:NGC 4697
7.1. Nature of the Central Source
The position of source 1 agrees with the optical
position of the center of NGC 4697 to within the
combined X-ray and optical errors. This suggests that
this source is actually an AGN. The luminosity of this
source, L_X_ = 8 x 10^38^ ergs s-1, is higher than most
LMXBs, but there are four sources that are brighter in
the S3 field. Of these, the two brightest sources in the
field (sources 72 and 82) are probably background AGNs
(source 72 definitely is), while the other two
(sources 36 and 40) are probably LMXBs in NGC 4697. On
the other hand, the hardness ratios for the central source
(H21 = -0.22 ^+0.09^_-0.09_, H31 = -0.34 ^+0.09^_-0.08_)
are very typical of those for the LMXBs (Table 2; Fig. 4
in Paper I), which have average hardness ratios of
(H21, H31) = (-0.14, - 0.37) within the inner effective
radius. Thus, based on the X-ray evidence alone, the
central source might be either the active nucleus in
NGC 4697 or one or more LMXBs seen in projection against
the nucleus. The central source appears to be slightly
extended, which might indicate that it is the result of
more than one point source.
NGC 4697 is not a radio source at a fairly restrictive
level (Birkinshaw & Davies 1985). We were unable to find
any other clear evidence for nuclear activity in the
literature. This might argue that the central source is not
due to an AGN.
Stellar dynamical measurements indicate that NGC 4697
has a central black hole (BH) with a mass
M_BH_ = 1.6 x 10^8^ M_sun_, assuming our adopted distance of
15.9 Mpc (Gebhardt et al. 2000). If we take the observed X-ray
luminosity of the central source to be an upper limit to the
luminosity of an associated active nucleus, then the AGN
luminosity is <= 4 x 10^-8^ of the Eddington luminosity of the
central BH.

6. 2000A&AS..145...71K
Re:NGC 4697
NGC 4697: Large E6 galaxy with only slight rotation, it also features a
dust lane of intrinsically circular shape, located in the equatorial
plane. The galaxy is flattened and may be an S0, the spheroidal part of
NGC 4697 may well be a large bulge (Dejonghe et al. 1996).

7. 1994CAG1..B...0000S
Re:NGC 4697
May 5/6, 1951
103aO + GG11
30 min
The insert print of NGC 4697 is made from a Mount Wilson 100-inch
plate. In the printing, the major axis of the photograph has been
rotated slightly relative to the main print.

8. 1994CAG1..B...0000S
Re:NGC 4697
Hubble Atlas, p. 1
May 5/6, 1951
103aO + GG1
30 min
NGC 4697 in the southern extension of the Virgo Cluster has an
appreciable globular cluster population, visible on this Palomar
200-inch plate, taken in poor seeing. Even so, the globular cluster
images are clearly visible near the limit of the negative print. The
specific globular cluster frequency listed by Harris (1988) is S =
4.1, which seems low in view of the large number of images seen here.
The galaxy is also shown on panel 13.

9. 1994A&AS..105..481M
Re:NGC 4697
NGC 4697: This often quoted disky E has been here classified from
literature data, notably BDM88. The q and e_4_ profiles show double
maxima, just like the many S0's with inner ring.

10. 1994A&AS..105..341G
Re:NGC 4697
E6 galaxy with stellar disk along the apparent major axis (cf. also
Carter 1987). Neither Veron-Cetty & Veron (1988) nor Kim (1989) found
evidence for the presence of dust, and our B-I image only reveals a very
red nucleus. However, the presence of cool gas in this galaxy is strongly
suggested by its significant IRAS flux densities (e.g., S_100_ = 1.10
Jy), and the detection of molecular gas (Sofue & Wakamatsu 1993). This
suggests that the dust is primarily distributed like the stars; this may
partially be the cause of the radial colour gradient of NGC 4697, which
is quite large compared with its radial metallicity gradient as measured
by the Mg_2_ index (see Peletier 1989). A marginal detection of ionized
gas was reported by Trinchieri & di Serego Alighieri (1991); Kim (1989)
reported a nondetection. However, we find quite significant detections in
both our H{alpha}+[NII] image and our emission-line spectrum. The ionized
gas is extended over a radius of ~35". Marginal detection of X-ray
emission, with a possibly large contribution from discrete stellar
sources (Canizares et al. 1987).

11. 1994A&AS..104..179G
Re:NGC 4697
Stellar disk along the major axis (cf. also Carter 1987) causing C4
deviations <~+0.03. Detected by IRAS at 60 & 100 microns. Marginal X-ray

12. 1976RC2...C...0000d
Re:NGC 4697
Interacting pair with anonymous SAB(s)c pec at 5.9 arcmin
Classification and Photograph:
Ap. J., 143, 1002, 1966.
Spectrum and Velocity Dispersion:
IAU Symp. No.15, p.112, 1962.
Ap. J., 143, 1002, 1966.
Ap. J., 175, 649, 1972.
Dynamics, Rotation Curve, and Mass Determination:
Ap. J., 139, 284, 1964.
Comm. Padova, No. 98, 1972.

13. 1974UGCA..C...0000N
Re:UGCA 300
UGCA 300:
= NGC 4697
E6 (RC1)
companion at 5.9, 281, 0.9 x 0.6 , Sa?

14. 1964RC1...C...0000d
Re:NGC 4697
Very bright center. Smooth nebulosity. Several globular clusters.
Interacting pair with an anonymous SAB(s)cp at 5.9 arcmin.
Lick 13 minor dimension is in error.
Heidelberg Veroff., Vol. 9, 1926 dimensions are for the bright part only.

15. 1963MCG3..C...0000V
Re:MCG -01-33-010
Type: Sand - E5, Hub - E6, vB - E4, Morg - gE6. Redshift: +1177, G4.
Photo: AnAp 23. Photo: Sand - globular clusters are visible in it.

16. 1961Hubbl.B...0000S
Re:NGC 4697
May 5/6, 1951
103aO + GG1
30 min
Enlarged 5.0X
NGC 4697 is a normal E5 galaxy in the southern extension
of the Virgo Cluster. There are a number of condensations
whose distribution is centered on the nucleus; they
are probably globular clusters. If this galaxy has a modulus
of (m-M) = 30.7, which probably applies to the nucleus
of the Virgo Cluster, then M(pg) for NGC 4697 is -20.3.
The value m(pg) = 10.4 is from Humason et al. (A. J., 61,
97, 1956, Table A1).

17. 1918PLicO..13....9C
Re:NGC 4697
3' x 0.7' in p.a. 68{deg}. Bright, almost stellar nucleus; slight trace of
spiral whorls. 7 s.n.

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