VLT-VIMOS integral field spectroscopy of luminous and ultraluminous infrared galaxies - II. Evidence for shock ionization caused by tidal forces in the extra-nuclear regions of interacting and merging LIRGs

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Volume 517 (July 2010)

A&A, 517 (2010) A28

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Table 3:

Ionization in the extra-nuclear ionized regions of LIRGs.
Galaxy	Mechanism^a	r^b	Comment
(IRAS number)
Class 0
F06295-1735	Young stars	0.22
F06592-6313	...	0.42	No [O I] $\lambda$ 6300 nor [S II] $\lambda \lambda$ 6717,6731 data. r based on [N II] $\lambda$ 6584/H $\alpha$ .
F07027-6011 N^c	Young stars and shocks (100-200 km s^-1)	0.44	Part of the shocks may be associated to the nucleus according [O I] $\lambda$ 6300/H $\alpha$ map.
F07027-6011 S	Young stars	0.21	r based on [S II] $\lambda \lambda$ 6717,6731/H $\alpha$ . r based on [O I] $\lambda$ 6300/H $\alpha$ not reliable.
F07160-6215	Shocks (100-300 km s^-1)	0.31	r based on [S II] $\lambda \lambda$ 6717,6731/H $\alpha$ . No [O I] $\lambda$ 6300 data.
F10015-0614	Young stars	0.15
F10409-4556	...	0.37	r based on [N II] $\lambda$ 6584/H $\alpha$ . No [O I] $\lambda$ 6300 nor [S II] $\lambda \lambda$ 6717,6731 data.
F10567-4310	Young stars	0.23	r based on [S II] $\lambda \lambda$ 6717,6731/H $\alpha$ . No [O I] $\lambda$ 6300 data.
F11254-4120	Young stars	0.71	r based on [N II] $\lambda$ 6584/H $\alpha$ . r based on [S II] $\lambda \lambda$ 6717,6731/H $\alpha$ not reliable. No [O I] $\lambda$ 6300 data. Possible shocks associated to the bar according to the [S II] $\lambda \lambda$ 6717,6731/H $\alpha$ map.
F11506-3851	Young stars	0.19	Some small areas better explained with low velocity shocks.
F12115-4656	Young stars	-0.24
F13229-2934^d	Shocks (100-300 km s^-1)	0.47	Some areas explained by stars, mostly associated with the arms. Part of the high excitation may be associated to the nucleus according to the [O I] $\lambda$ 6300/H $\alpha$ map.
F22132-3705	Young stars	0.10	Small areas better explained with low velocity (<100 km s^-1) shocks.
Class 1
F01159-4443	Low velocity (<100 km s^-1) shocks	0.23	Some regions explained by stars.
ESO 297-G011	Young stars	-0.12	Some small areas explained by shocks. r based on [S II] $\lambda \lambda$ 6717,6731/H $\alpha$ . r based on [O I] $\lambda$ 6300/H $\alpha$ not reliable.
ESO 297-G012	Young stars and shocks	-0.56	r based on [N II] $\lambda$ 6584/H $\alpha$ . r based on [O I] $\lambda$ 6300/H $\alpha$ or [S II] $\lambda \lambda$ 6717,6731/H $\alpha$ not reliable.
F06076-2139	...	0.75	r based on [N II] $\lambda$ 6584/H $\alpha$ data. No [O I] $\lambda$ 6300 nor [S II] $\lambda \lambda$ 6717,6731 data.
F06259-4708 P1	Young stars	0.74	Low velocity (100-150 km s^-1) shocks also present.
F06259-4708 P2	Shocks (100-150 km s^-1) and young stars	0.31
08424-3130	Stars and shocks ( ${\sim}100$ km s^-1)	0.61	r based on [S II] $\lambda \lambda$ 6717,6731/H $\alpha$ . r based on [O I] $\lambda$ 6300/H $\alpha$ not reliable. Northern galaxy mainly shocks; southern one mainly stars.
F08520-6850	Stars and shocks ( ${\sim}100$ km s^-1)	0.40
IC 563	Young stars	0.22	Low velocity (100-150 km s^-1) shocks could be also present.
IC 564 N	Young stars	0.44	Low velocity (100-150 km s^-1) shocks also present. r based on [N II] $\lambda$ 6584/H $\alpha$ . No [O I] $\lambda$ 6300 data. r based on [S II] $\lambda \lambda$ 6717,6731/H $\alpha$ not reliable.
IC 564 S	Young stars	0.34	r based on [N II] $\lambda$ 6584/H $\alpha$ . No [O I] $\lambda$ 6300 data. r based on [S II] $\lambda \lambda$ 6717,6731/H $\alpha$ not reliable.
12042-3140	Young stars and shocks (100-150 km s^-1)	0.81	Northern galaxy mainly stars, Southern one shocks.
12596-1529	Young stars and low velocity shocks	0.47	rbased on [S II] $\lambda \lambda$ 6717,6731/H $\alpha$ data. No [O I] $\lambda$ 6300 data. r based on [S II] $\lambda \lambda$ 6717,6731/H $\alpha$ not reliable.
F14544-4255 E	Young stars	0.67	r based on [S II] $\lambda \lambda$ 6717,6731/H $\alpha$ . No [O I] $\lambda$ 6300 data.
F14544-4255 W^d	High velocity (100-300 km s^-1) shocks	0.67	Shocks may be associated to the nucleus according to the [O I] $\lambda$ 6300/H $\alpha$ map.
18093-5744 N	Young stars	0.09	Low velocity shocks also possible.
18093-5744 C	Stars older than 3 Myr and/or with $Z <Z_\odot$	-0.65	r based on [S II] $\lambda \lambda$ 6717,6731/H $\alpha$ . r based on [O I] $\lambda$ 6300/H $\alpha$ not reliable.
18093-5744 S	Young stars	0.27
Class 2
F04315-0840	Shocks (100-200 km s^-1) and young stars	0.63	Young stars in the inner region and arms/tidal tails. Shocks at 2-3 kpc from the nucleus.
08355-4944	Young stars	0.14	Low velocity shocks also present at $\sim$ 2 kpc from the nucleus.
F10038-3338	Shocks (100-200 km s^-1)	0.50	Shocks may be associated to the nucleus.
10257-4338	Shocks (100-150 km s^-1) and stars	0.63
12116-5615	Young stars and low velocity shocks	0.57
13001-2339	Shocks (100-150 km s^-1)	0.48	All data with [O I] $\lambda$ 6300/H $\alpha$ > -1.2. Part of the shocks may be associated to the nucleus
17138-1017	Young stars and low velocity shocks	-0.23	No [O I] $\lambda$ 6300data; r according to [S II] $\lambda \lambda$ 6717,6731/H $\alpha$ data
21453-3511^d	High velocity (100-300 km s^-1) shocks and/or AGN.	0.76	Young stars (spiral arms). Shocks may be associated to the nucleus according [O I] $\lambda$ 6300/H $\alpha$ map.

Notes. ^(a) At least otherwise indicated, based on the comparison of the data with several ionization models in the [O I] $\lambda$ 6300/H $\alpha$ - [N II] $\lambda$ 6584/H $\alpha$ diagnostic diagram. For the present analysis solar metallicity has been considered as baseline. If higher metallicity (e.g. $Z=2~Z_\odot$ ) is considered, a higher presence of shocks with respect to stars would have been obtained (see Fig. 9).
^(b) Pearson coefficient inferred from the [O I] $\lambda$ 6300/H $\alpha$ - ${\sigma }$ relation (see text). For objects where [O I] $\lambda$ 6300 was not detected or the r coefficient did not reach a confidence level of 90%, r was obtained from the [S II] $\lambda \lambda$ 6717,6731/H $\alpha$ or [N II] $\lambda$ 6584/H $\alpha$ , as indicated.
^(c) Classified as Seyfert (Kewley et al. 2001a).
^(d) Classified as Seyfert (Corbett et al. 2003).

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