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Central Bodies Masses of Selected Globular Clusters
N.A.Shakht, A.A.Kiselev, Yu.N.Gnedin and E.A.Grosheva. The Main Astronomical (Pulkovo) Observatory RAS


47 Tuc ­NGC 104
RA 00 24 .1 Dec -72° 04 .9 Size = 30.9 mvis + 4. 0 m D from = 12,1 kpc,
h m



Cen - NGC 5139

NGC 6397 (Ara)
RA 17 h40.m7 Dec -53o 40'.4 Size = 31',0 mvis + 5,3m D from =2.3 kpc

RA 13h 26m .8 Dec -47° 28 6 Size = 36.3 m vis +3. 7 m D from =15.8 ±1.1 kpc, 12109 years,

Age:

10109 years,

(13.4 ± 0.8)109 years.

Cen belongs to our Galaxy Milky Way and is a largest globular cluster known at present, but it is assumed, that in the past it was the dwarf- galaxy absorbed by Milky Way. It is proposed also, that G1 is the remains of dwarf-galaxy absorbed by galaxy of Andromeda many centuries back .




NGC 6388 (Sco)
RA = 17h 36 m .6 Dec= -44°44' .1 D= m vis 6m,8 Size 10.4` Age 10x109

Globular cluster G1 in Galaxy M31 Andromeda
M15 NGC 7078 (Peg) RA 21h 30m.0 Dec +12o 10' D = 10,3 kpc mvis +6,2 Size 18.0 Age ~12109 RA 00h 32m.8 Dec+39° 34 .7 D = 770 ± 40 kpc mvis +13m.8 Size 0.6' Age~ 12 109 years


Introduction
dispersions of their radial velocities Vr according data published in the astronomical literature. We fulfilled the estimation of masses of the central bodies for selected globular clusters on the base of to

Radial velocities of stars are considered near to the center of cluster for two prospective extreme cases: 1) regulated rotation of stars around the center and 2) rotation on the orbits with accidental orientation. We made the assumption that stars are on short distance (about 0.001 of tidal radius Rt) to the proposed blackhole and are rotating around it as planets around the Sun, according to laws of Newton, and thus their masses are near to the mass of the Sun, but the mass of the central body is more by factor of 103. For instance, for M15 we used the results of STIS-observations with HST for 13 stars in region 1"x1" according to Gerssen et al.

AJ,124,2000.


The research of globular clusters was always and remains now an actual problem. One of the very interesting problems in the modern astronomy is the problem of existence of black holes of intermediate masses (IMBH) in the range: 102 M
Ting-Ni Lu, Albert K.H.Kong, arXiv:1102.1668v1 [Astro-ph.SR]8 Feb 2011 .


Processing and results.
We have estimated a mass of the system: the central body + a star (m), proceeding from integral of energy, as in a problem of two bodies at determination of double star mass. Here the integral of energy has a following form:

V

2

=k

2

(

21 - ra

)

, where

k2 =42 (M1+M2) or k2 = 42 M

Corresponding dimensions:
[V ] = / A .U . = 4.74 yr

[r] = A.U. , [M]=

Thus we considered two extreme cases. 1) it was supposed, that stars rotate around the black hole on circular orbits parallel to the direction of line of sight and dispersion = Vr = V rV 2 rV 2 M = = = 0.025 rV 2 4 2 39.48 2) the chaotic movement of stars on the accidental orbits has been assumed also the statistical method has been applied, based on theorem Kleiber, where = Vr = Ѕ V and

rV M = 4

2 2

rV 2 = = 0.104 rV 39.48

2