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Table D.1

Physical properties of AzTEC/C2a, C4, C5, C17, and C42, and the CR electron cooling times and diffusion length scales.

Parameter C2a C4 C5 C17 C42
z a 3.179 4.3415 4.542
Mgasb [1011M⊙] 5.6 4.7 5.5 3.8 3.1
c [kpc] 4.5 3.7 2.6 2.3 2.4
c [kpc] 3.8 2.4 2.1 1.2 1.7
d
he [kpc] 1.0 1.0 1.0 1.0 1.0
nHf [cm-3] 598 967 1840 2515 1388
Bg [μG] 245 311 429 502 373
LIRh [1013L⊙] 2.6 2.0 1.8 0.8 3.8
uradi [keV cm-3] 8.2 12.1 17.7 15.6 49.9
uCMBi [eV cm-3] 80.3 414.9 214.4 248.5 121.0
τsynch [105 yr] 1.0 0.6 0.4 0.3 0.5
τIC [103 yr] 19.3 11.9 10.4 12.5 3.7
τIC, CMB [105 yr] 19.6 3.5 8.6 7.9 15.2
τbrem [105 yr] 1.4 0.9 0.5 0.3 0.6
τion [104 yr] 4.6 3.1 1.3 0.9 1.7
j [103 yr] 11.0 6.8 4.5 3.9 2.7
lescj [pc] 17 14 9 8 7

Notes.

(a)

See Table C.1 for the redshift references.

(b)

The gas mass estimated by using the Scoville et al. (2016) dust continuum method (Miettinen et al., in prep.). The CO-based gas masses for AzTEC/C5 (Yun et al. 2015) and AzTEC/C17 (Schinnerer et al. 2008) agree with the quoted values within a factor of two when the values are scaled according to the assumptions used in the calculation.

(c)

The parameters and refer to the major and minor axis FWHM sizes, respectively. The FWHM of the rest-frame FIR-emitting region of AzTEC/C2a and C4 was derived through subarcsec resolution SMA 870 μm observations by Younger et al. (2010), while that of AzTEC/C5, C17, and C42 was derived from the subarcsec resolution ALMA submm continuum data (PI: A. Karim). The AzTEC/C42 size refers to the northern ALMA component, which is coincident with the 3 GHz emission peak (M15).

(d)

The ratio between the observed-frame 3 GHz radio size and the rest-frame FIR size.

(e)

A disk scale height is assumed to be 1 kpc, i.e. that of high-z puffy starbursts considered by Lacki & Thompson (2010).

(f)

The average hydrogen number density was calculated from the Mgas, FIR-emitting size, and h values (see text for details).

(g)

The magnetic field strength was estimated using the formula .

(h)

The total IR (8–1000 μm) luminosity adopted from Miettinen et al. (in prep.).

(i)

The radiation field and CMB energy densities (urad and uCMB, respectively).

(j)

For the formulas used to calculate the electron cooling times and escape scale lengths, we refer to Appendix E in M15, and references therein.

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