Date and Time of the Query: 2019-02-23 T04:35:18 PST
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Notes for object MESSIER 060

19 note(s) found in NED.

1. 2008MNRAS.386.2242H
Re:NGC 4649
NGC 4649 - We estimate the {sigma}_e_ using the stellar velocity
dispersion profile measured by Bridges et al. (2006).

2. 2008MNRAS.386.2242H
Re:NGC 4649
NGC 4649 - We estimate the {sigma}_e_ using the stellar velocity dispersion
profile measured by Bridges et al. (2006).

3. 2006ApJS..164..334F
Re:VCC 1978
VCC 1978 (M60, NGC 4649).This galaxy shows very regular isophotes, with no
evidence of a morphologically distinct nuclear component.

4. 2006A&A...447...97B
Re:UGC 07898
UGC 7898: Soldatenkov et al. (2003) detected nuclear emission at a 3 confidence
level only in the range 0.2-0.6 keV with a luminosity of 6 x 10^37^ erg s^-1^.
Conversely Randall et al. (2004) did not find conclusive evidence for a central
AGN. They give an upper limit for the X-ray luminosity converting count rate
(0.3-10 keV) into the un-absorbed luminosity L_x_(0.3-10 keV) using photon index
{GAMMA} = 1.78. We adopted the latter, more conservative, estimate.

5. 2005ApJ...635.1031B
Re:NGC 4649
NGC 4649.-The redshifted O VI {lambda}1032 line would be shifted (1035.8 A)
just to the blue side of the Galactic C II {lambda}1036 line (1036.3 A), but
there is no evidence for O VI emission above the level of the rather strong
stellar continuum, which is similar to the continuum of NGC 1399 (Fig. 21).
There are moderately strong Galactic H_2_ lines and atomic absorption lines
present, although these do not contaminate the locations of the O VI lines.

6. 2005ApJ...622..235T
Re:NGC 4649
Radio; H2; H I; no FIR dust; H{alpha} undetected at log(LH{alpha}) < 37.73; M60

7. 2004A&A...416...41X
Re:NGC 4649
NGC 4649. NGC 4649 shows no clear excess in the MIR (see Fig. 4 and
Table 4). IRAS fluxes indicate a dust mass of 4.5 x 10^4^M_{sun}_ (see
Table 3) although, as already stated in the introduction, background
contamination and other uncertainties may lead to an overestimation of
the FIR output of early-type galaxies (Bregman et al. 1998). The absence
of any significant amount of dust is also demonstrated by recent ISO
observations at 60, 90 and 180 micron where this galaxy show no emission
(Temi et al. 2003).

8. 2003ApJS..146....1W
Re:NGC 4649
NGC 4649.-The Galactic O VI line lies in the wing of the strong Ly{beta}
line associated with the galaxy itself, which is a galaxy in the Virgo
cluster. This substantially reduces the S/N ratio, but the Galactic O VI
line is still clearly visible and can easily be measured.

9. 2001AJ....121.2974L
Re:NGC 4649
NGC 4649: Another giant Virgo elliptical galaxy (known as M60), with
S_N_ ~ 6.7 (Ashman & Zepf 1998). Both we and Kundu (1999) detect clear

10. 2000ApJS..129..435B
Re:RXC J1243.6+1133
RXC J1229.7+0759 and RXC J1243.6+1133. - These are the X-ray halos
of the two Virgo Cluster galaxies M49 and M60, respectively. They are
included in this catalog, even though these halos are embedded within
the low surface brightness structure of the Virgo Cluster emission. But
since the two local halos stand out from the low surface brightness
emission environment and can be reasonably characterized by the present
source characterization technique, we have not excluded them from our
catalog as we have excluded M86 and M87.

11. 2000ApJ...542..761W
Re:NGC 4649
NGC 4647/9 is a bright, well-known pair in the Virgo Cluster (see the
B band image in Fig. 11). NGC 4647 (UGC 7896) is a spiral with flocculent
structure and heavy dust lanes, especially prominent at the edge of the
optical disk (see, e.g., the photograph in Arp 1966, where this pair is
number 116). They are projected at the large center-to-center separation
of 11.9 kpc (for a distance of 16 Mpc) even compared to the large scale
of the elliptical NGC 4649 (=M60=UGC 7898), so this pair offers a chance
to examine primarily any dust structure that might lie beyond the bright
optical disk (since the entire spiral is projected against detectable
light from NGC 4649). The elliptical was modeled in two stages, using
the STSDAS ellipse task for the inner parts of the galaxy and the
best-fit global r^1/4^ model beyond r = 106", to avoid the spiral's
influence on fitted isophotes. The outer regions are fitted by a
somewhat shallower profile (R_e_ = 82") than the global value of 68"
listed in the RC3 (de Vaucouleurs et al. 1991). After subtraction of
this model for the elliptical component NGC 4649, no absorption
structure is found beyond the edges of the disk of NGC 4647, with the
outermost detected absorption associated with the prominent dust lane on
the northern side of the disk. If the spiral is in fact in front, no
dust features large enough to resolve have A_B_ or A_I_ > 0.11 (dividing
by a face-on correction factor of a/b = 1.4). The range sampled here is
at and outside R_25_.

12. 1994CAG1..B...0000S
Re:NGC 4649
[Pair with NGC 4647]
VCC 1978
Jan 26/27, 1920
Seed 30
75 min
The two galaxies here form a close optical
pair with an angular separation of 2.5' in the
Virgo Cluster region but south and far to the east
of the core of subcluster A. The redshifts are
similar at v_o(4647) = 1331 km/s and v_o(4649)
= 1142 km/s. The lack of evidence of tidal
interaction, either as tidal plumes in the S0
component or as a distortion of the spiral structure
of NGC 4647, suggests that the galaxies are at
different distances. At the common distance
scaled to 22 Mpc for the Virgo Cluster, their
projected linear separation would be small at 16
kpc; some sign of an encounter would be
NGC 4649 is Messier 60. It has a prominent
extended envelope characteristic of S0_1_
morphology. The E2 classification in the RC2, based
on a Palomar 200-inch plate, is inappropriate.

13. 1994A&AS..105..481M
Re:NGC 4649
NGC 4649: This appears to be a good case of boE. The envelope is again
above the r^1/4^ law.

14. 1976RC2...C...0000d
Re:NGC 4649
= M60
= Holm 448a
= Kara[72] 353b
In Arp 116 = VV 206
Non-interacting pair with NGC 4647 at 2.5 arcmin
Ap. J., 139, 384, 1964.
Ap. J., 169, 209, 1971.
Photometry (5 Color):
A.J., 73, 313, 1968.
Photometry (10 Color):
Ap. J., 179, 731, 1973.
Ap. J. Suppl., 26, No. 230, 1973.
Ap. J., 139, 532, 1964.
Observatory, 88, 239, 1968.
Dynamics and Mass Determination:
Ap. J., 139, 284, 1964.
Radio Observations:
M.N.R.A.S., 167, 251, 1974 (with NGC 4647).

15. 1973UGC...C...0000N
Re:UGC 07898
VV 206a, Arp 116b
E 2 (de Vaucouleurs), E (Holmberg)
See UGC 07896
In Arp's class "E and E-like galaxies close to and perturbing spirals"
"Absorption heavier on spiral side away from E galaxy" (Arp)
{12 41.3 +11 44} at 5.7, 153, 0.9 x 0.4, spiral, m=15.7
{UGC incorrectly notes "12 41.0 +11 52". H. Corwin}

16. 1964RC1...C...0000d
Re:NGC 4649
= Messier 060
= Holm 448a
Very bright center. Smooth nebulosity. Many globular clusters.
Uppsala 21, Lick 13, and Heidelberg Veroff. Vol. 9, 1926 dimensions are for
the bright part only.
Non-interacting pair with NGC 4647 at 2.5 arcmin.
B magnitude (source F) is for the NGC 4647 + NGC 4649.
Ap. J., 56, 166, 1922.
Ap. J., 166, 64, 1952.
Ap. J., 135, 6, 1962.
M.N.R.A.S., 98, 613, 318.
B.A.N., 16, 1, 1961.
Ap. J., 71, 231, 1930.
Ap. J., 132, 306, 1960.
M.N.R.A.S., 94, 807, 1934.
M.N.R.A.S., 98, 619, 1938.
Ann. d'Ap., 11, 247, 1948.
Ann. d'Ap., 14, 347, 1951.
B.A.N., 16, 1, 1961.
Ap. J., 112, 66, 1952.
A.J., 61, 97, 1956.

17. 1959VV....C...0000V
Re:VV 206a
= NGC 4649
V = +1,379 km/sec
V = +780 km/sec
(Page, T., Ap. J., 116, 63, 1952)
Yerkes Type: kE2

18. 1956AJ.....61...97H
Re:NGC 4649
HMS Note No. 148
Slit simultaneously on both nebulae: NGC 4647 and NGC 4649
(HMS Plate IVs).

19. 1918PLicO..13....9C
Re:NGC 4649
2' in diameter, growing rapidly brighter to a very bright central portion, which
shows no true nucleus in short exposures; no spiral whorls discernible.

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