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

A. Monreal-Ibero; S. Arribas; L. Colina; J. Rodríguez-Zaurín; A. Alonso-Herrero; M. García-Marín

doi:10.1051/0004-6361/200913239

Home

All issues

Volume 517 (July 2010)

A&A, 517 (2010) A28

Full HTML

Free Access

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).

Source LaTeX | All tables | In the text

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.