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Notes for object NGC 3115

20 note(s) found in NED.


1. 2009MNRAS.397.2148G
Re:NGC 3115
This is another lenticular galaxy with a large-scale rotating disc (Rubin,
Peterson & Ford 1980). Kormendy et al. (1996) and Emsellem, Dejonghe & Bacon
(1999) have noted the presence of a nuclear point source, while Lauer et al.
(2005) provide a V-band magnitude for this NC which equates to -12.1 mag for a
galaxy distance of 9.7 Mpc (Tonry et al. 2001). TheV-I colour in Lauer et al.
(2005) is 1.2, corresponding to 0.18 < log[M/L_V_] < 0.56 for all combinations
of stellar metallicities and ages. We again adopt M/L_V_= 2.5 for the NC.

2. 2008MNRAS.386.2242H
Re:NGC 3115
NGC 3115 and NGC 3245 have boxy bulges, while their bulge Sersic index
is n~= 4 . We suggest central classical bulges and outer boxy bulges
coexist in these galaxies.

3. 2008MNRAS.386.2242H
Re:NGC 3115
NGC 224 (M31), NGC 3031 (M81) and NGC 3115 in our sample are typical classical
bulges listed in KK04.

4. 2008MNRAS.386.2242H
Re:NGC 3115
NGC 3115 and NGC 3245 have boxy bulges, while their bulge Sersic index is n~=
4. We suggest central classical bulges and outer boxy bulges coexist in these
galaxies.

5. 2006ApJ...639..136H
Re:NGC 3115
NGC 3115. We extracted the spectrum from a 2' (5 kpc) aperture. The
diffuse component was dominated by the undetected point-source component.
However, there is still some evidence of a single ~0.4 keV gas component.
The abundances were very poorly constrained.

6. 2005ApJ...635.1031B
Re:NGC 3115
NGC 3115.-Galactic molecular absorption lines are strong, but the redshifted O
VI lines lie in uncontaminated parts of the spectrum. There is no emission from
O VI (Fig. 7).

7. 2002ApJ...574..740T
Re:NGC 3115
NGC 3115.
The black hole mass is based on stellar kinematics (Kormendy
et al. 1996a). Although NGC 3115 does not have three-integral
axisymmetric dynamical models, it does have a compact,
high-contrast stellar nucleus, and the mass of the nucleus plus
black hole can be estimated from the virial theorem. In
estimating the dispersion, we have excluded the region near
the center that is strongly perturbed by the black hole (see
Fig. 6). See also Emsellem, Dejonghe, & Bacon (1999)

8. 2001AJ....122..653R
Re:NGC 3115
NGC 3115: The residual image shows a nuclear disk in addition to the
large-scale disk; neither is well fitted with the Nuker law. NGC 3115 is
known to have a V ~ 17 mag central star cluster in the optical
(Kormendy et al. 1996). Our NIC3 image does not detect the cluster,
presumably because of its low contrast and the poor pixel resolution.
The optical images show no dust features (Lauer et al. 1995;
Tomita et al. 2000).

9. 2001AJ....121.2974L
Re:NGC 3115
NGC 3115: This bulge-dominated S0 galaxy is also very nearby. It has a
modest GC system, which has been examined using HST by Kundu & Whitmore
(1998). They identified 144 GCs with a color distribution similar to that
listed in Table 3. In addition, they noted that the red GCs were smaller
than the blue ones by ~20%. Mainly because of our selection criteria,
designed for somewhat more distant galaxies than NGC 3115 and therefore
with a brighter lower magnitude limit, we detect fewer GCs in NGC 3115 than
did Kundu & Whitmore (1998).

10. 1999A&AS..138..253B
Re:NGC 3115
NGC 3115 - SN 1935B: one red and compact object is visible to the
south-east of the SN location and at the edge of the ring. Several other
patches of the same kind are found all around the region.

11. 1997AJ....113..950F
Re:NGC 3115
NGC 3115. The h_3_ profile along the major axis of this S0 indicates that a
low-speed tail is present at all radii. However, between 2"-7" the strength of
the asymmetry declines with radius before rising again at larger radius.

12. 1996ApJ...459..110F
Re:NGC 3115
NGC 3115
NGC 3115 is a bulge-dominated S0 galaxy. Our major-axis surface brightness
profile indicates that the bulge of NGC 3115 contributes more light than the
disk for r >~ 5 kpc. The major-axis H{beta} profile of NGC 3115 displays a
measurable rise in H{beta} strength with radius (from 1.8 A in the central
regions to ~ 2.0A for r >~ 9"). The color image of NGC 3115 (Fig. 5) displays
a thin (<~ 4") disk of constant color along the major axis surrounded by a
bluer bulge region.

13. 1994CAG1..B...0000S
Re:NGC 3115
Hubble Atlas, p. 1
S0_1_(7)/a
(P)
PH-61-S
Nov 30/Dec 1, 1951
103aO + WG2
30 min
At one time called an E7, NGC 3115 is a
type example of an edge-on thin disk galaxy
having a prominent, thick envelope (a thick
disk). The well-developed, high-surface-brightness,
very thin disk is shown well in the insert.
The overprinted main print shows the problem of
classifying early-type galaxies using small-scale
and/or overexposed plates where features are
buried and lost in the high-surface-brightness
envelope. The classification would have been E7
from such plate material if based on images
similar to the main print here. The galaxy is
classed E7/S0_1_ in the Hubble Atlas.
However, deep CCD exposures, which have
a large dynamic range, show hooks at the two
ends of the major axis of the disk, showing that
NGC 3115 in fact has a spiral structure (Silva,
Boroson, and Thompson 1989), requiring the
mixed classification notation S0/a. This, of
course, is uncertain because of the nearly edge-on
aspect angle, but the spiral hooks are real.
The plate used for the reproduction here is
different from the one used in the Hubble Atlas.
The description there contains information not
contained here.

14. 1994A&AS..105..481M
Re:NGC 3115
NGC 3115: This famous galaxy has a modest disk embedded in a spheroidal
halo. See also Paper I, the modelling by Capaccioli et al. (1987,1988),
the color study by Silva et al. (1989).

15. 1976RC2...C...0000d
Re:NGC 3115
Pair with a very faint dwarf E with stellar nucleus at 5.5 arcmin.
Photometry: (12 Color)
Ap. J., 145, 36, 1966.
Photometry (Isophotometry):
Ap. J., 152, 35, 1968.
Photometry (BV):
Ap. J., 169, 209, 1971.
Photometry (2.2 microns):
"Nuclei of Galaxies," 195, 1971.
Spectrum and Velocity Dispersion:
IAU Symp. No. 15, 112, 1962.
Ap. J., 179, 55, 1973.
Bull. A.A.S., 3, 476, 1971.
IAU Symp., No. 58, 20, 1974.
Spectrophotometry:
Ap. J., 169, 209, 1971.
Ap. J., 175, 649, 1972.
Ap. J., 177, 285, 1972.
A.J., 74, 50, 1969.
A.J., 77, 333, 1972.
Mem. S.A. Ital., 43, 263, 1972.
Rotation Curve and Mass Determination:
IAU Symp. No. 15, 142, 1962.
Ap. J., 179, 55, 1972.

16. 1974UGCA..C...0000N
Re:UGCA 199
UGCA 199:
S0 (RC1)

17. 1964RC1...C...0000d
Re:NGC 3115
Very bright nucleus in a flat disk: 2.7 arcmin x 0.1 arcmin with some
weak knots near the tips. Extensive envelope. Possibly E+7
Pair with a very faint dwarf elliptical with a stellar nucleus at 5.5 arcmin.
Photograph:
Ap. J., 64, 325, 1926.
Ap. J., 71, 235, 1930.
Ap. J., 98, 47, 1943.
Handbuch der Ap., 5, 2, 843, 1933.
Photometry:
Ap. J., 71, 231, 1930.
Ap. J., 91, 289, 1940.
Ap. J., 120, 439, 1954.
Ann. d'Ap. II 247, 1948.
B.A.N. 16, 1, 1961.
Spectrum:
Ap. J., 135, 734, 1962.
Dynamics, Rotation, Mass,
Ap. J., 91, 296, 1940.
A.J., 59, 273, 1954.
P.A.S.P., 71, 104, 1959.
SN 1935? suspected
Lund Ann. 7, 161, 1938.

18. 1963MCG3..C...0000V
Re:MCG -01-26-018
Objects like these, visible from the side and departing from the
elliptical form, we denote as lenses rather than elliptical galaxies.
This is undoubtedly a form intermediate to a nucleus, surrounded by a
narrow, but "flat" ring, close to the nucleus. This form is close to
a nucleus with a disk. Vaucouleurs also denotes it like this. If it
is considered as an elliptical, it is of largest possible flatness.
{omega} = 81.6 degrees, Type: SAnd - E7, vB - E6, Vauc - S0- sp, Morg
- k D7. Redshift: +423, G5; Photo: AnAp 23, where the radial velocities
are given which show the rotation; Cp' = 0.97; B-V = 0.94, U-B = 0.56.
Photo: Lick 8; ApJ 46, No1, 64, 324, 73, No4; Lund A No 7; Hub; Jeans;
Hd Ap; Sh; PG; PASP 70; Sand (E7/S01) - plane around the nucleus is
clearly visible. It is even more visible in PASP 70. Objects are in
the corona, which are undoubtedly globular clusters, but Sandage says
nothing about these. Data: Photometry - ApJ 71, 231; 91, 273; 98, 47;
120, 439; AJ 58, 50; AnAp 11, 247; BAN 16 No 509. Rotation and mass:
ApJ 91, 273; AJ 59, 273.

19. 1961Hubbl.B...0000S
Re:NGC 3115
E7/S01
PH-20-Bm
Mar.30/31, 1952
103aE + E.K. no. 25
6Omin
Enlarged 4.1X
NGC 3115 was classified as a true E7 on the basis of plates
taken with the 60- and the 1OO-inch telescopes. Plates
taken with the 200-inch clearly show two subsystems:
one an almost spherical nuclear system; and the second,
a thin fundamental plane. The plane was detected in the
photometry of Hubble (Ap. J., 71, 231, 1930) and of Oort
(Ap. J., 91, 273, 1940). NGC 3115 is now classed as
either a transition between E7 and S01 or a pure S01.

20. 1918PLicO..13....9C
Re:NGC 3115
Vol. VIII, Plate 22. An exceedingly bright spindle 4' x 1' in p.a. 45^deg^,
with an almost spherical central portion; no stellar nucleus apparent in
short exposures. There are no traces of spiral whorls, but it is doubtless
a spiral of the Andromeda type seen edgewise. 16 s.n.


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