New constraints on dust emission and UV attenuation of z = 6.5–7.5 galaxies from millimeter observations

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Volume 574 (February 2015)

A&A, 574 (2015) A19

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Table 1

Summary of millimeter observations and derived quantities.

Source

rms_cont

σ_line

L_{[C II]}

L_IR(T_d = 25)

L_IR(T_d = 35)

L_IR(T_d = 45)

[GHz]

[mJy beam^-1]

[mJy beam^-1]^e

10⁸ [L_⊙]

10¹¹ [L_⊙]

A1703-zD1

6.8^a

241.500

0.165

1.517

< 2.55 /μ

< 3.96 /μ

< 7.32 /μ

< 14.38 /μ

z8-GND-5296

7.508

223.382

0.124

1.824

< 3.56

< 3.84

< 6.65

< 12.67

IOK-1^b

6.96

238.76

0.021

0.215

< 0.38

< 0.53

< 0.96

< 1.87

HCM6A^c

6.56

251.40

0.16

0.849

< 1.36 /μ

< 3.47 /μ

< 6.49 /μ

< 12.81 /μ

4.5

Himiko^d

6.595

250.00

0.017

0.167

< 0.28

< 0.36

< 0.67

< 1.30

Notes. All luminosity upper limits are 3σ and are not corrected for lensing. For A1703-zD1 and HCM6A the true luminosity limits are therefore lower by the magnification factor μ. The dust temperature T_d indicated here is corrected for the CMB heating, i.e., it corresponds to the temperature dust would have if it were heated by stars alone.

^(a)

Approximate photometric redshift (cf. text).

^(b)

Observations from Ota et al. (2014).

^(c)

Observations from Kanekar et al. (2013).

^(d)

Observations from Ouchi et al. (2013).

^(e)

In Δv = 50 km s^-1 channels.

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