Formation of S0 galaxies through mergers - Antitruncated stellar discs resulting from major mergers

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Volume 570 (October 2014)

A&A, 570 (2014) A103

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Table 5

Kolmogorov-Smirnov test to the 2D distributions of real Type III S0s data and of Type III S0-like remnants in several photometric planes related to the antitruncations.

No.	Photometric plane	p-value^a	KS test^b	Fig.

1	μ_brkIII vs. R_brkIII/R₂₅ (displaced^c )	0.021	S	5

2	V_rot vs. R_brkIII/R₂₅	0.068	S	6

3	(μ_0,i − μ_brkIII) vs. h_i/R₂₅	0.018	NS	10
4	(μ_0,i − μ_brkIII) vs. h_o/R₂₅	0.0054	NS	10
5	(μ_0,o − μ_brkIII) vs. h_o/R₂₅	0.017	NS	10
6	(μ_0,o − μ_brkIII) vs. h_i/R₂₅	0.035	NS	10

7	h_i/h_o vs. R_brkIII/R₂₅	0.0013	NS	11

8	(μ_0,i − μ_brkIII) vs. h_i/R_brkIII	0.044	NS	12
9	(μ_0,i − μ_brkIII) vs. h_o/R_brkIII	0.0009	NS	12
10	(μ_0,o − μ_brkIII) vs. h_i/R_brkIII	0.0008	NS	12
11	(μ_0,o − μ_brkIII) vs. h_o/R_brkIII	0.023	NS	12
12	(μ_0,i − μ_brkIII) vs. R_brkIII/R₂₅	0.026	NS	12
13	(μ_0,o − μ_brkIII) vs. R_brkIII/R₂₅	0.0086	NS	12

14	h_i/R₂₅ vs. R_brkIII/R₂₅	0.71	S	13
15	h_o/R₂₅ vs. R_brkIII/R₂₅	0.066	S	13
16	μ_0,i vs. R_brkIII/R₂₅ (displaced^c )	0.23	S	13
17	μ_0,o vs. R_brkIII/R₂₅ (displaced^c )	0.67	S	13

18	(μ_0,i − μ_brkIII) vs. h_i/h_o	0.00048	NS	14
19	(μ_0,o − μ_brkIII) vs. h_i/h_o	0.00073	NS	14
20	(μ_0,o − μ_0,i) vs. h_i/h_o	0.00030	NS	14

21	h_i/h_o vs. R_brkIII/h_i	0.00079	NS	15
22	h_i/h_o vs. R_brkIII/h_i (with Y07)	0.024	NS	15
23	h_i/h_o vs. R_brkIII/h_o	0.0012	NS	15
24	h_i/h_o vs. R_brkIII/h_o (with Y07)	0.030	NS	15

Notes.

^(a)

The p-values have been computed using the implementation of the KS test in 2D by P. Yoachim (KS2D, see the text).

^(b)

According to the KS test, the distributions of observational data and of simulations are similar (S) in a 95% confidence level if p>α = 0.05. If not, the null hypotesis is rejected, meaning that both samples have been taken from different parent distributions and cannot be considered as similar (NS).

^(c)

Displaced relations assume an offset in mag arcsec^-2 to overlap the distributions of real and simulated data in the photometric plane. The offset has been set to the difference between the y-intercepts of the linear fits performed to each sample in the plane (see Table 4).

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