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Dynamics and Statistics
M/M 10
4

statistics

R = 0.9992

2

103

dynamics

R = 0.9401
10
2

2

log(/o)
-1.8 -1.7 -1.6 -1.5 -1.4 -1.3 -1.2 -1.1 -1

Comparison of results of mass estimation which is received by means of our method (dynamics) for 18 clusters of Milky Way with suspected BH with data in [2] (Safonova, Shastri, Aph. Sp Sci. 325, 47, 2010) (statistics) received with formula:

log (Mc/M

) = 8.19 ± 0.06 + 4.20 + 0.02 log(/o) ;

where ­ radial velocities dispersion ;



o = 200 km/c


/
104
[1]

Ce n

Radio

M15

G1

[2]
- statistics

103

[1]
Radio
NGC 6388

47 Tuc

-dy namics

102

(our results)

10

NGC 6397

Log(

/

o)

-2

-1.5

-1

-0.5

0


Comparison our results with statistics and radio observations

Name

,
km/s

D, kpc 5.3 3.8 780 9.9 10.4 2.3

Mass , 103 M , Dynamics

Mass ,
103 M

,

Statistics

[1]

Mass, 103 M , Radio [2] 5.2В1.1



Cen

23.0 11.6 25.1 18.9 14.1 4.5

28 В 44 1.1/4.4 16 В 40 1.6/6.4 2.4/9.6 0.03/1.2

40

(NGC 5139)

47 Tuc (NGC 104) G1 NGC 6388 NGC 7078 ( M15) NGC 6397

1.0 18 5.7 2.5

4.9В0.5 4.5 1.5В0.73 2.4

0.02

0.05


The use of the gravitation's theory with additional space measurements for NGC 6397.
The gravitation's theory with additional spatial measurements is one of variants of all kinds of interactions association. In new theory the gravitation characteristic time of quantum evaporation of a black hole is equal:
3 -2

ev = 120

M l yr M 1 mm
BH

Comparison of this time with characteristic time of age of a globular cluster with a black hole of intermediate mass in the center allows to define characteristic scale l
( see, O.Yu. Gnedin et al., Aph.J.,705, L168 ,2009 ; Postnov and Cherepaschuk, astro-ph/0401466, 2004).

For globular cluster NGC 6397 so it is comparable with results which there are low-mass X-ray A 0620-00) and globular cluster In the theory: if MBH = 20 M

l

is received in the range 0.04 -0.15 mm, accorded to some other exotic objects, within double stars in our Galaxy (XTEJ1118+480, RZ 2109 in ecliptic galaxy NGC 4472, see Table 2. , and = 1.42 109 years, then l = 0.007 mm.


Table 2. Results of observations of BH.
Objects XTEJ1118+480 A 0620-00 NGC 6397 MBH (M) 8.5 ± 0.6 10 ± 5 30В120 13.4 ± 0.7 ·10
9

Age (years) >10
7

l () 0.08 0.16 0.02В0.14

RZ 2109

~10

~10

10

0.003

Conclusions.
1. We offered the simple approximate method for estimate of central bodies of globular clusters masses. 2. We considered the limits of central bodies masses for 4 clusters in our Galaxy (47 Tuc, Cen, NGC 6388, M15) and G1 Globular cluster in the Galaxy Andromeda. Our method gives with other ones and equal to IMBH. 3. In our graphics we gives the low limits of masses according to hypothesis about regular rotation of stars around center. In the cases of accidental orientation of orbits the mass will be more in some times (denominator of the fraction in column 4 of the table 1). 4. It is possible to receive more precise results with more precise effective radius R and with more confident value of radius and with proved hypothesis concerning character of movement of stars in a cluster.


Thank you!