Molecular gas content in strongly lensed z ~ 1.5−3 star-forming galaxies with low infrared luminosities

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Volume 577 (May 2015)

A&A, 577 (2015) A50

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Table 1

Physical properties derived from SED fitting.

Source	z _Hα	μ ^a	L _IR ^b	M _∗ ^c	SFR ^c	M _dust ^d	T _dust ^d	L_ν(850 μm) ^d
			(10¹¹L_⊙)	(10¹⁰M_⊙)	(M_⊙ yr^-1)	(10⁷M_⊙)	(K)	(10²⁹ erg s^-1 Hz^-1)

A68-C0	1.5864	30	1.18 ± 0.07	2.0 ± 0.65		4.7	34.5	5.0
A68-HLS115	1.5869	15	3.42 ± 0.16			3.0	37.5	7.7
MACS0451-arc	2.013	49	1.36 ± 0.13 ^e	0.25 ± 0.02		0.6	47.4	3.4
A2218-Mult	3.104	14	2.26 ± 0.15
A68-h7	2.15^f	3			76 ± 3.4	18.2	43.3	27.6
MS 1512-cB58	2.729	30	3.04 ± 0.07	0.44 ± 0.03		1.2	50.1	2.0
Cosmic Eye	3.0733	28		2.4 ± 0.06	33 ± 0.6	2.2	46.3	3.3

Notes. All values correspond to intrinsic values corrected from magnification factors and come from Sklias et al. (2014) except for A2218-Mult.

^(a)

Magnification factors derived from robust lens modeling (Richard et al. 2007, 2011).

^(b)

Infrared luminosities integrated over the [8, 1000] μm interval.

^(c)

Stellar masses and SFRs as derived from the best energy conserving SED fits, obtained under the hypothesis of an extinction, A_V, fixed at the observed ratio of L_IR over L_UV following the prescriptions of Schaerer et al. (2013).

^(d)

Dust masses, dust temperatures, and rest-frame 850 μm luminosities derived from a modified blackbody fit applied to the Herschel photometry with the β-slope fixed to 1.5 for T_dust and to 1.8 for M_dust and L_ν(850 μm).

^(e)

IR luminosity corrected from the AGN (Active Galactive Nuclei) contribution identified by the excess of the flux in the Herschel/PACS 100 μm band observed in the southern part of the MACS0451-arc, indicating very hot dust. The decomposition of the IR emission of the southern part between the AGN and stellar emission indicates a starburst-component contributing to about 45% of the total L_IR in the southern part (for a detailed analysis, see Zamojski et al., in prep.).

^(f)

Redshift determined from weak absorption lines in the rest-frame UV instead of the Hα line.

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