Integral field optical spectroscopy of a representative sample of ULIRGs - II. Two-dimensional kpc-scale extinction structure

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Volume 505 / No 3 (October III 2009)

A&A, 505 3 (2009) 1017-1026

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Table 1:

Extinction and structural properties for the sample of galaxies.
Galaxy^a	log( $L_{\rm {IR}}$ )^b	z	$A_{\rm {V}}$ $_{\rm {median}}$ ^c	$A_{\rm {V}}$ $_{\rm {nuc}}$ ^d	$A_{\rm {V}}$ $_{\rm {max}}$ ^e	Sep^f	Scale	$R_{\rm {eff}}$ (optical)	$R_{\rm {eff}}$ ^g	$R_{\rm {eff}}$ ^h	Morphologyⁱ
	$L_{\odot}$		(mag)	(mag)	(mag)	(kpc)	(kpc/arcsec)	(kpc)	(kpc)	(kpc)
IRAS 13156+0435N	12.13	0.113	2.5 $\pm$ 0.8	3.3	3.7	3.9 $\pm$ 1.0	2.058		5.9		IP at 36.0 kpc
IRAS 13156+0435S			0.9 $\pm$ 0.4	1.5	1.7	2.2 $\pm$ 1.0	2.058		4.9
IRAS 18580+6527E	12.26	0.176	1.3 $\pm$ 0.8	0.5	3.9	20.3 $\pm$ 1.5	2.986	11.3^j	6.5		IP at 15.0 kpc
IRAS 18580+6527W				0.8	3.9	8.7 $\pm$ 1.5	2.986	9.4^j	4.3
IRAS 16007+3743E	12.11	0.185	1.9 $\pm$ 1.0	4.5	5.0	12.7 $\pm$ 1.5	3.100		4.0		IP at 14.2 kpc
IRAS 16007+3743W				4.7	5.0	1.4 $\pm$ 1.5	3.100		4.2
IRAS 06268+3509N	12.51	0.169	2.0 $\pm$ 1.2	5.7	6.9	3.2 $\pm$ 1.4	2.895	8.3^j	2.0	2.1	IP at 9.1 kpc
IRAS 06268+3509S				2.2	6.9	10.5 $\pm$ 1.4	2.895	6.3^j	1.5	1.1
IRAS 08572+3915N	12.17	0.058	1.7 $\pm$ 1.1	2.3	5.8	0.0 $\pm$ 0.6	1.130	2.9^k	2.8	0.6	IP at 6.1 kpc
IRAS 08572+3915S				0.4	5.8	1.3 $\pm$ 0.6	1.130	4.3^k	1.4	0.6
IRAS 14348-1447N	12.39	0.083	2.9 $\pm$ 1.0	5.4	5.8	5.6 $\pm$ 0.8	1.556	5.3^l	1.4	1.5	IP at 5.5 kpc
IRAS 14348-1447S				4.1	5.8	0.8 $\pm$ 0.8	1.556	4.1^l	3.0	1.3
Arp 299/NGC 3690	11.81	0.010	1.9 $\pm$ 0.6	3.7	4.3	0.5 $\pm$ 0.1	0.205		1.2	0.9	IP at 5.0 kpc
Arp 299/IC 694			2.0 $\pm$ 0.6	2.7	3.4	0.3 $\pm$ 0.1	0.205		2.0	0.4
IRAS 12112+0305N	12.37	0.073	1.7 $\pm$ 1.3	3.0	7.7	5.5 $\pm$ 0.7	1.395	3.3^l	2.0	1.7	IP at 4.0 kpc
IRAS 12112+0305S				7.7	7.7	0.0 $\pm$ 0.7	1.395	4.5^l	1.5	1.1
Mrk 463-E	11.81	0.050	0.9 $\pm$ 0.5	0.7	3.0	4.7 $\pm$ 0.5	0.984		1.0	0.2	DN at 3.8 kpc
Mrk 463-W				1.5	3.0	8.4 $\pm$ 0.5	0.984		1.0	1.0
IRAS 06487+2208	12.57	0.144	2.2 $\pm$ 0.6	2.4	3.5	4.3 $\pm$ 0.6	2.522		1.5		DN at 1.5 kpc
IRAS 11087+5351	12.13	0.143	1.2 $\pm$ 1.0	3.0	3.0	0.0 $\pm$ 0.6	2.507		8.9		DN at 1.5 kpc
Mrk 273	12.18	0.038	1.9 $\pm$ 1.0	3.1	4.9	2.1 $\pm$ 0.4	0.749	4.3^l	4.4	2.0	DN at 0.7 kpc
IRAS 17208-0014	12.43	0.043	5.5 $\pm$ 2.6	5.0	9.0	0.8 $\pm$ 0.4	0.844	3.6^l	3.2	1.5	SN
IRAS 15250+3609	12.09	0.055	2.3 $\pm$ 1.7	2.5	7.9	2.4 $\pm$ 0.5	1.072	2.2^l	1.9	1.4	SN
IRAS 12490-1009	12.07	0.101	1.3 $\pm$ 0.7	1.1	3.3	3.6 $\pm$ 0.9	1.854		7.6		SN
IRAS 14060+2919	12.18	0.117	1.5 $\pm$ 0.5	2.2	2.5	2.3 $\pm$ 1.0	2.113		4.8		SN
IRAS 15206+3342	12.27	0.124	0.8 $\pm$ 0.5	1.0	2.0	2.4 $\pm$ 1.0	2.232	2.2^k	2.9		SN

^a The galaxies are listed according to decreasing nuclear separation (see García-Marín et al. 2009); ^b $L_{\rm {IR}}$ (8-1000 $\mu$ m) was derived following Sanders & Mirabel 1996); ^c median extinction of the entire system with the deviation that effectively represents the distribution of the extinction values over the entire area where the H $\alpha$ and H $\beta$ measurements can be obtained. For pre-coalescence systems with one pointing per nuclei, the median has been calculated for each pointing; ^d nuclear extinction of the galaxy. The uncertainties are about 20%; ^e maximum extinction of the system; ^f separation between the optical nucleus, identified as the peak position in the F814W band of the HST images, and the position of the peak of extinction; ^g effective radius measured from the HST WFPC2 camera, with the filter F814W, corresponding to a central wavelength of 0.82 $\mu$ m and a filter width of 0.17 $\mu$ m; ^h effective radius measured from the HST NICMOS2 camera, with the filter F160W, corresponding to a central wavelength of 1.55 $\mu$ m and a filter width of 0.40 $\mu$ m; ⁱ IP means interacting pair, DN double nucleus and SN single nucleus; ^j effective radius measured from the HST WFPC2 camera, with the filter F606W, corresponding to a central wavelength of 0.58 $\mu$ m, and a filter width of 0.16 $\mu$ m; ^k effective radius measured from the HST WFPC2 camera, with the filter F439W, corresponding to a central wavelength of 0.43 $\mu$ m and a filter width of 0.05 $\mu$ m; ^l effective radius measured from the HST ACS camera, with the filter F435W, corresponding to a central wavelength of 0.43 $\mu$ m and a filter width of 0.14 $\mu$ m.

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