Table 4: The distribution of observations of perturbed asteroids. In the columns N₁, N₂, N₃, N₄, N₅ are given number of observations, number of discarded preenc. observations, number of used preenc. observations, number of discarded postenc. observations and number of used postenc. observations. T₁ and T₂ are time intervals covered by preencounter and postencounter observations. The standard deviations of orbital residuals are given in the last column.
Perturbed
N₁ N₂ N₃ T₁ N₄ N₅ T₂ rms

asteroid
[ $\hbox{$^{\prime\prime}$ }$ ]

(3057) Malaren
307 3 11 1952-1981 15 278 1983-2004 0.63

(5205) 1988CU7 321 2 3 1954-1961 36 280 1988-2003 0.58

(8331) Dawkins 368 2 5 1982 16 345 1990-2003 0.68

(21225) 1995GQ1 180 0 4 1972 5 171 1995-2003 0.66

**Table 4:** The distribution of observations of perturbed asteroids. In the columns N₁, N₂, N₃, N₄, N₅ are given number of observations, number of discarded preenc. observations, number of used preenc. observations, number of discarded postenc. observations and number of used postenc. observations. T₁ and T₂ are time intervals covered by preencounter and postencounter observations. The standard deviations of orbital residuals are given in the last column.
Perturbed	N₁	N₂	N₃	T₁	N₄	N₅	T₂	rms
asteroid								[ $\hbox{$^{\prime\prime}$ }$ ]
(3057) Malaren	307	3	11	1952-1981	15	278	1983-2004	0.63
(5205) 1988CU7	321	2	3	1954-1961	36	280	1988-2003	0.58
(8331) Dawkins	368	2	5	1982	16	345	1990-2003	0.68
(21225) 1995GQ1	180	0	4	1972	5	171	1995-2003	0.66

Source LaTeX | All tables | In the text

	1 Introduction
	2 Procedure of mass determination
	3 Results and discussion
	4 Conclusion
	References