Molecular gas properties of a lensed star-forming galaxy at z ~ 3.6: a case study

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Volume 605 (September 2017)

A&A, 605 (2017) A81

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Table 1

From optical to radio photometry and CO line integrated fluxes of MACSJ0032-arc.

Band/line	Multiple images								Total
	B		C		D		E		B+C+D+E

Magnification	12.7 ±	3	24.7 ±	2	12.6 ±	3	10.8 ±	4	62 ±	6

ACS F606W (μJy)	1.169 ±	0.002	1.722 ±	0.004	0.679 ±	0.003	0.794 ±	0.002	4.365 ±	0.010
ACS F814W (μJy)	2.109 ±	0.005	3.133 ±	0.007	1.180 ±	0.005	1.585 ±	0.003	8.017 ±	0.019
IRAC 3.6 μm (μJy)	15.56 ±	0.07	blended		blended		blended		58.08 ±	0.27^a
IRAC 4.5 μm (μJy)	17.54 ±	0.07	blended		blended		blended		66.07 ±	0.27^a
SPIRE 250 μm (mJy)	blended		blended		blended		blended		58 ±	8
SPIRE 350 μm (mJy)	blended		blended		blended		blended		72 ±	10
SPIRE 500 μm (mJy)	blended		blended		blended		blended		52 ±	9
PdBI 2 mm (mJy)	<0.16^†		0.37 ±	0.07	<0.12^†		<0.14^†		0.65 ±	0.25^b, ^c
JVLA 5 GHz (μJy)	18.9 ±	3.0	25.9 ±	4.4	7.8 ±	2.9	40.8 ±	4.1^d	93.4 ±	14.4
PdBI CO(6–5) (Jy km s^-1)	0.68 ±	0.15	0.86 ±	0.15	0.53 ±	0.20	0.71 ±	0.10^d	2.78 ±	0.60
30 m CO(4–3) (Jy km s^-1)	–		–		–		–		2.30 ±	0.55^e
JVLA CO(1–0) (Jy km s^-1)	0.047 ±	0.020^†	0.08 ±	0.02	0.030 ±	0.015^†	0.035 ±	0.018^†	0.21 ±	0.06^b, ^f

Notes. Observed (not lensing-corrected) continuum fluxes and CO line integrated fluxes, all with 1σ uncertainties. The “total” refers to the sum of the signal coming from the multiple images B, C, D, and E, the contribution of the counter-image F being negligible.

^(†)

Tentative detections below 3σ.

^(a)

Estimated by propagating the IRAC–F814W colors properly measured in the counter-image B over the sum of multiple images B, C, D, and E (“total”).

^(b)

Obtained by integrating the flux over the same apertures as those used for the CO(6–5) emission detected over all multiple images B, C, D, and E.

^(c)

By applying the 2 mm–F814W color conservation over the multiple images, we get a higher total 2 mm continuum flux of 0.9 mJy.

^(d)

The color conservation is not satisfied, the measured flux is in excess.

^(e)

All the multiple images B, C, D, and E contribute to the observed CO(4–3) line integrated flux given the IRAM 30 m telescope half power beam width of 24′′ at the redshifted frequency of the CO(4–3) line.

^(f)

By applying the CO(1–0)–F814W color conservation over the multiple images, we get a similar total CO(1–0) line integrated flux of 0.20 Jy km s^-1.

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