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 3:

H $\alpha$ - and IR-based star formation rates for the sample of ULIRGs.
Galaxy	$log(L_{\rm {IR}}$ )^a	$SFR(L(\rm {H}\alpha)_{\rm {obs}}$ )^b	$SFR(L(\rm {H}\alpha)_{\rm {med-ext}}$ ^c)	$SFR(L(\rm {H}\alpha)_{\rm {corr}}$ )^d	SFR(IR)^e
IRAS 13156+0435	12.13	5.5	26.2	23.7	232.9
IRAS 18580+6527^f	12.26	17.1	53.8	61.6	318.7
IRAS 16007+3743	12.11	19.8	106.4	120.	222.5
IRAS 06268+3509	12.51	3.7	22.1	95.6	493.5
IRAS 08572+3915	12.17	3.6	16.7	12.2	255.5
IRAS 14348-1447	12.39	20.2	263.1	301.0	424.1
Arp 299^f	11.81	4.7	26.3	35.3	111.5
IRAS 12112+0305	12.37	6.0	26.9	168.3	405.0
Mrk 463^f	11.81	17.2	38.0	44.2	111.5
IRAS 06487+2208	12.57	11.0	76.0	92.4	641.8
IRAS 11087+5351^f	12.13	3.5	9.5	8.7	233.0
Mrk 273^f	12.18	-	-	-	216.5
IRAS 17208-0014	12.43	6.1	-	126.5	465.0
IRAS 15250+3609	12.09	2.5	19.7	69.1	212.5
IRAS 12490-1009	12.07	2.0	6.4	9.5	203.0
IRAS 14060+2919	12.18	6.4	24.3	35.5	261.5
IRAS 15206+3342	12.27	135.7	275.5	254.3	321.6

^a IR luminosity derived following Sanders & Mirabel (1996); ^b SFR derived using the total observed H $\alpha$ flux given in Col. 2 of Table 2. Units are $M_\odot$ yr^-1; ^c SFR derived using the H $\alpha$ median extinction corrected values as specified in Table 2 Col. 6. Units are $M_\odot$ yr^-1; ^d SFR calculated using the two-dimensional extinction corrected H $\alpha$ luminosity as given in Table 2 Col. 5. Units are $M_\odot$ yr^-1; ^e SFR based on the IR-based luminosity values as given in Col. 2 of the present table. Units are $M_\odot$ yr^-1; ^f strong evidence for a Seyfert nucleus, for which we have not corrected this values.

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