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Notes for object MESSIER 105

22 note(s) found in NED.


1. 2008MNRAS.386.2242H
Re:NGC 3379
NGC 3379 - The black hole mass is measure by stellar kinematics ( M_bh_=
1.0^+1.0^_-0.4_ x 10^8^ M_sun_ ; Gebhardt et al. 2000b) and gas
kinematics ( M_bh_= 1.4+^0.3^_-0.8_ x 10^8^ M_sun_ ; Shapiro et al.
2006), we take the average value of M_bh_= (1.2 +- 0.6) x 10^8^ M_sun_.

2. 2008MNRAS.386.2242H
Re:NGC 3379
NGC 3379 - The black hole mass is measure by stellar kinematics (M_bh_=
1.0^+1.0^_-0.4_*10^8^ M_{sun}_; Gebhardt et al. 2000b) and gas kinematics
(M_bh_=1.4^+0.3^_-0.8_*10^8^ M_{sun}_; Shapiro et al.2006), we take the
average value of M_bh_=(1.2+/-0.6)*10^8^ M_{sun}_.

3. 2006MNRAS.369..497K
Re:NGC 3379
NGC 3379 (M105). This rather round object shows normal metal line strengths
gradients consistent with the isophotes. The H{beta} map shows weakly increasing
line strength towards larger radii, as found by other authors (e.g. Davies et
al. 1993; Sanchez-Blazquez 2004, see also Fig. 4).

4. 2006MNRAS.366.1151S
Re:NGC 3379
The largest member of the Leo Group, this galaxy displays a central disc of gas
and a number of isolated sources of emission. The direction of maximum rotation
of the central disc is consistent with the orientation of the nuclear dusty ring
visible in the HST images, and indicates a ~45^deg^ kinematic misalignment
between gas and stars. The impact of template mismatch in biasing the ?gas
measurements towards overestimated values (Section 3.3.2) is visible at the edge
of the central disc, where the strength of the emission lines approaches the
detection limit. However, all isolated sources show very narrow [O III] lines
and undetected H{beta} emission, consistent with large [O III]/H{beta} ratios.
These characteristics suggest that these sources are in fact PNe. The two
sources with the largest EW values ~20 arcsec south and south-west from the
centre, have positions and velocities consistent with the PNe 4 and 7 of
Ciardullo, Jacoby & Dejonghe (1993), respectively.

5. 2006ApJ...647..140F
Re:NGC 3379
This galaxy (T2, E1) harbors a cluster of 10 point sources in its nucleus. One
of these point sources (not the brightest one) is at the exact center of the
galaxy. The spectrum of this source had only 89 counts; thus, its luminosity was
estimated by fitting an absorbed power law: L_0.5-10_ keV = 6.3 x 10^37^ ergs
s^-1^. An unresolved radio source of S_{nu}_ = 0.7 mJy has been detected at 5
GHz at the center of this galaxy (Wrobel & Heeschen 1991). We calculate log R_X_
= -2.3, which makes this source radio-loud and suggests that it is an LLAGN. The
luminosity of the central 2.5" region was evaluated to be L_2-10_ keV = 1.0 x
10^38^ ergs s^-1^, and the LLAGN has L_2-10_ keV = 1.7 x 10^37^ ergs s^-1^. The
candidate LLAGN contributes ~20% to the luminosity of the central 2.5" region,
making this LINER a composite. However, age estimates indicate a stellar
population of intermediate age, in the range of 6-9 Gyr (Terlevich & Forbes
2002; Gregg et al. 2004). We were able to fit the brightest source in the
nucleus with a number of models involving a power law and a soft component
(diskbb, bb, MEKAL). The addition of the soft component to the simple power law
is not strongly justified by the F-test (chance probability between 14% and 44%
depending on the model for the soft component; a plasma model to the power law
gives the smallest chance probability). The total luminosity of this source is
L_0.5-10 keV_ = 1.4 x 10^39^ ergs s^-1^. From its spectrum, luminosity, and
off-center position, one can infer that this source is probably an XRB.

6. 2006A&A...460...45G
Re:NGC 3379
NGC 3379 (UGC 5902, M 105). Very recently, David et al. (2005) published their
study of the X-ray emission as traced by ACIS-S Chandra observations. It is
mainly devoted to the analysis of extra-nuclear X-ray sources and diffuse
emission, and they derive a power-law index for the diffuse emission of 1.6-1.7,
in agreement with the value reported by Georgantopoulos et al. (2002). David et
al. (2005) do not fit the spectrum of the nuclear source (their source 1) due to
the too low net counts in the S3 chip data for this object. This is also the
reason for having neither a fit nor an estimation of the spectral parameters
(see Table 6).

7. 2005ApJ...635.1031B
Re:NGC 3379
NGC 3379.-The redshift of this galaxy places the O VI lines in a part of the
spectrum uncontaminated by Galactic absorption. No O VI emission is found (Fig.
8).

8. 2004MNRAS.352..721E
Re:NGC 3379
NGC 3379: This roundish galaxy has h_3_ values being anticorrelated with
the mean velocity, and has fairly constant positive h_4_ values: this is
consistent with other published data (e.g. Statler & Smecker-Hane 1999;
Gebhardt et al. 2000; Halliday et al. 2001).

9. 2001MNRAS.326..473H
Re:NGC 3379
A3 NGC 3379
NGC 3379 is a member of the Leo-I group and is a well observed elliptical,
classified as E1 in RC3.
For the major axis, rotation decreases at r ~ 4 arcsec and then
increases again at larger radius. Both h_3_ and h_4_ show small non-zero
values but there is no clear trend. For the minor axis, both h_3_ and
h_4_ are mostly consistent with zero (see Fig. A3).

10. 2001MNRAS.322..702M
Re:NGC 3379
NGC 3379 Our models use the minor-axis dispersion profile measured by
Statler & Smecker-Hane (1999), and the 29 PNe radial velocities from
Ciardullo, Jacoby & Dejonghe (1993). We have subtracted a systemic velocity
of 900 km s^-1^ from the PNe velocities for the model plotted in Fig. 3.
The results are almost identical if we instead assume a systemic velocity
of 916 km s^-1^, equal to the mean recession velocity of the PNe sample, or
if we use the 881 km s^-1^ quoted in Tully (1988). Statler & Smecker-Hane
(1999) discovered that this galaxy has a kink in its dispersion profile at
a radius of ~15 arcsec. Our models fit the data beyond the kink by having
{UPSILON}(r) increase by a factor of three between 15 and 60 arcsec, then
becoming flat further out in order to fit the PNe radial velocities. An
alternative explanation is that NGC 3379 may be a face-on S0 (e.g.,
Capaccioli et al. 1991), or a weakly triaxial system viewed face on
(Statler & Smecker-Hane 1999). We note that the evidence for positive
h_4_ in this galaxy could be due either to radial anisotropy
(Gebhardt et al. 2000) or to the galaxy being flattened system viewed face
on (Section 2).

11. 2001AJ....122..653R
Re:NGC 3379
NGC 3379: The weak dust ring seen in optical images (van Dokkum & Franx
1995; Tomita et al. 2000) is not present in the NIR. The features in the
residual image are due to slight deviations from the Nuker-law fit.

12. 2001AJ....121.2974L
Re:NGC 3379
NGC 3379: Also known as M105, NGC 3379 is the dominant elliptical galaxy
in the nearby Leo Group. Along with NGC 3377, it has a relatively low
specific frequency, S_N_ ~ 1.2 (Ashman & Zepf 1998). Here we detect only
55 GCs with bimodality likely but not certain.

13. 2000A&AS..144...53K
Re:NGC 3379
The data taken along the major axis of the galaxy follow closely the
results of Statler & Smecker-Hane (1999) (Fig. 4). The data along the
shifted direction reach 100 arcsec from the center and show a declining
(cylindrical) velocity, with negative values at 100 arcsec confirmed in
the 8 separate frames.
The velocity dispersions and h_4_ values along the major axis given in
BSG94 (not shown here) appear slightly larger. The h_3_ values and
velocities agree well.

14. 2000A&AS..144...53K
Re:NGC 3379
For this galaxy we used the CCD surface photometry of Davis et al.
(1985) in both the R- and B-bands.

15. 1999A&AS..136..269F
Re:NGC 3379
The dust is concentrated in a large asymmetric cloud in the S direction.
The H{alpha} image shows a very clear absorption feature South of the
nucleus of the galaxy.

16. 1994CAG1..B...0000S
Re:NGC 3379
Leo Group #25
E0
PH-270-S
Dec 10/11, 1952
103aD + GG11
25 min
NGC 3379 forms the central triplet with NGC 3384 (SB0; panels 54,
S7) and NGC 3389 (Sc; panel 253) of the extended Leo Group. The
redshifts of NGC 3379 and NGC 3384 are similar at v_o = 759 km/s and
v_o = 638 km/s respectively. Many dwarf ellipticals and dwarf Im
galaxies are associated with the group (Ferguson and Sandage 1990).

17. 1994A&AS..105..481M
Re:NGC 3379
NGC 3379: Does it contain a disk?? (see Capaccioli et al. 1991)

18. 1994A&AS..104..179G
Re:NGC 3379
Frequently used as "standard" elliptical. Small but significant S4 terms.
Nuclear radio source.

19. 1976RC2...C...0000d
Re:NGC 3379
= M105
= Holm 212a
In Leo (M 96) Group.
Non-interacting pairs with NGC 3384 at 7.2 arcmin, NGC 3389 at 10.3 arcmin
Diameter:
Ap. J., 173, 485, 1972.
Photograph:
Ap. J., 139, 284, 1964.
Photometry:
Ap. J., 139, 284, 1964.
Photometry (5 Color):
A.J., 73, 313, 1968.
Photometry (10 Color):
Ap. J., 179, 731, 1973.
Photometry (UBV):
Bull. A.A.S., 5, 348, 1973.
A.J., 79, 835, 1974.
Isodensitometry:
Ap. J. Suppl., 26, No. 230, 1973.
Spectrophotometry:
Ap. J., 154, 22, 1968.
Ap. J., 175, 649, 1972.
Ap. J., 177, 285, 1972.
A.J., 74, 50, 1969.
IAU Symp. No.58, p.160, 1974.
Dynamics and Mass Determination:
Ap. J., 139, 284, 1964.
HI 21cm (upper limit):
Astr. Ap., 25, 451, 1973.

20. 1973UGC...C...0000N
Re:UGC 05902
E+1 (de Vaucouleurs)
Paired with UGC 05911 at 7.2
UGC 05914 at 10.0, 108

21. 1964RC1...C...0000d
Re:NGC 3379
= Messier 105
= Holm 212a
Very bright nucleus, in a lens: 1.5 arcmin x 1.5 arcmin. Some globular
clusters?
Lund 10 dimensions are for the lens only.
One discordant value of B-V (source C) rejected.
Pair with NGC 3384 at 7.2 arcmin.
NGC 3389 at 10.3 arcmin.
In the Leo Group.
Photograph:
Ap. J., 64, 325, 1926.
Ap. J., 71, 235, 1930.
Photometry:
Ap. J., 50, 38, 1919.
Ap. J., 71, 231, 1930.
Ap. J., 136, 713, 1962.
Ap. J., 137, 733, 1963.
M.N.R.A.S., 98, 619, 1938.
Ann. d'Ap., 11, 247, 1948.
P.A.S.P., 74, 146, 1962.
A.J., 67, 120, 1962.
Dennison, Univ. of Michigan Thesis, 1954.
Spectrum:
Ap. J., 135, 734, 1962.
Mass and Luminosity:
Ap. J., 134, 251, 1961.
Ap. J., 134, 910, 1961.
Ap. J., 138, 849, 1963.

22. 1918PLicO..13....9C
Re:NGC 3379
This, with 3384 and 3389, forms a striking group, a right-angled triangle
whose shorter sides are 7' long. 3379 is nearly round, 2' in diameter; very
bright; no spiral strueture discernible. 33 s.n.


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