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 2:

Observed H $\alpha$ fluxes and extinction corrected luminosities for the sample galaxies.
Galaxy	$F(\rm {H}\alpha)_{\rm {obs}}$ ^a	$F(\rm {H}\alpha)_{\rm {nuclear/total}}$ ^b	$L(\rm {H}\alpha)_{\rm {obs}}$ ^c	$L(\rm {H}\alpha)_{\rm {ext corr}}$ ^d	$L(\rm {H}\alpha)_{\rm {med-ext}}$ ^e	$L_{\rm {nuc}}(\rm {H}\alpha)_{\rm {obs}}$ ^f	$L_{\rm {nuc}}(\rm {H}\alpha)_{\rm {corr}}$ ^g
IRAS 13156+0435N	0.9	0.12	3.0	21.0	27.1	0.36	4.6
IRAS 13156+0435S	1.2	0.09	3.9	9.0	6.1	0.35	1.3
IRAS 18580+6527	2.5	[E] 0.01	21.6	78.0	68.2	0.22	0.4
		[W] 0.28				6.05	15.9
IRAS 16007+3743	2.6	[E] 0.03	25.1	152.0	134.7	0.75	17.7
		[W] 0.22				5.52	97.0
IRAS 06268+3509	0.6	[N] 0.09	4.7	121.0	28.0	0.42	66.5
		[S] 0.18				0.85	4.4
IRAS 08572+3915	5.8	[N] 0.08	4.6	15.5	21.1	0.37	2.0
		[S] 0.05				0.23	0.3
IRAS 14348-1447	15.0	[N] 0.03	25.6	381.0	333.0	0.77	52.3
		[S] 0.08				2.05	31.5
Arp 299/NGC 3690	181.0	0.03^h	4.0	29.0	21.5	0.12	0.9
Arp 299/IC 694	89.0	0.03^h	2.0	16.0	11.9	0.06	6.2
IRAS 12112+0305	5.8	[N] 0.08	7.6	213.0	34.0	0.60	9.0
		[S] 0.02				0.15	155.0
Mrk 463	36.9	[E] 0.25	21.8	56.0	48.2	5.45	10.4
		[W] 0.02				0.44	1.8
IRAS 06487+2208	2.5	0.19	13.9	117.0	96.3	2.64	23.3
IRAS 11087+5351	0.8	0.12	4.4	11.0	12.0	0.53	7.4
Mrk 273ⁱ	-	0.08	-	-	-	-	-
IRAS 17208-0014	17.9	0.10	7.7	160.2	-^j	0.7	43.0
IRAS 15250+3609	4.4	0.26	3.2	87.5	25.0	0.83	4.4
IRAS 12490-1009	1.0	0.13	2.6	12.0	8.1	0.34	0.9
IRAS 14060+2919	2.3	0.18	8.2	45.0	30.8	1.48	10.7
IRAS 15206+3342	42.7	0.38	171.8	322.0	348.7	65.3	158.5

^a Integrated H $\alpha$ observed flux, with units $\times$ 10^-14 erg s^-1 cm^-2. Note that in the cases of IRAS 13156+0435 and Arp 299 we derived the integrated flux for each galaxy of the interacting pair using their individual pointings; ^b ratio between the H $\alpha$ nuclear, identified as the peak position in the optical continuum and total observed fluxes; ^c observed H $\alpha$ luminosity derived from the integrated flux in Col. 2. Units in $\times$ 10⁴¹ erg s^-1; ^d integrated two-dimensional extinction corrected H $\alpha$ luminosity, with units in $\times$ 10⁴¹ erg s^-1; ^e integrated H $\alpha$ extinction-corrected luminosity, derived using the total observed flux and the median extinction, with units in $\times$ 10⁴¹ erg s^-1; ^f observed nuclear H $\alpha$ luminosity with units in $\times$ 10⁴¹ erg s^-1; ^g extinction corrected nuclear H $\alpha$ luminosity, derived using the nuclear extinction of each individual galaxy. Units in $\times$ 10⁴¹ erg s^-1; ^h for this particular galaxy we have calculated the ratio using the position of the true nucleus of the galaxy, which does not coincide with the optical one (García-Marín et al. 2006); ⁱ the data for Mrk 273 do not have an absolute flux calibration. Hence, only the relative measurement between the nuclear and integrated H $\alpha$ flux is given here; ^j as shown in Fig. 1b, the area of this galaxy with available extinction values is limited, also presenting a very large peak value. The use of this value for correcting the integrated flux is not valid and therefore is not included in the table.

Source LaTeX | All tables | In the text

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