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Table 1

Some global properties and observational details for the four galaxies studied here.

Properties EGS 13003805 EGS 13004291 EGS 12007881 EGS 13019128

z1 1.2318 1.19705 1.16105 1.3494
DA[Mpc]2 1753.0 1745.3 1736.4 1772.8
DL[Mpc]2 8731.5 8424.7 8108.8 9785.1
Scale [kpc/′′] 8.50 8.46 8.42 8.60

DEEP2 slit size 6.863′′ × 1′′ 5.149′′ × 1′′ 5.762′′ × 1′′ 10.343′′ × 1′′
DEEP2 slit orientation (PA) −53.858° −27.649° 11.142° 46.142°
IRAM CO(3–2) beam 0.8′′ × 0.6′′ 0.6′′ × 0.5′′ 1.1′′ × 0.9′′ 1.6′′ × 1.4′′

SFR[OII] [M  yr-1]3 98 182 119 202
SFRUV+24μm [M  yr-1]4 200 630 94 87
SFR[OII],B [M  yr-1]5 63 231 265 213

Mgas [1011  M]6 2.2 2.8 1.3 1.2
Mstar [1011  M]7 3.4 5.0 5.0 3.8
fgas8 0.39 0.36 0.21 0.24

R1/2 [kpc]9 5.7 3.1 5.7 5.2
log 10gas/ [M  pc-2])10 3.03 3.67 2.80 2.86
log 10SFR/ [M  yr-1  kpc-2])10 −0.193 0.604 −0.095 0.204
log 10star/ [M  pc-2])10 3.22 3.92 3.39 3.36

A Hα11 1.25 1.28 1.06 1.21
A V11 1.56 1.60 1.30 1.50
A [OII]11 2.28 2.26 2.04 2.19
A[OII]/AHα12 1.82 1.77 1.92 1.81

Notes.

(1)

The redshift, as determined in the AEGIS catalogues from the [OII] line using DEEP2 spectra;

(2)

the angular distance DA and the luminosity distance DL;

(3)

the SFR from the [OII] line luminosity in the galaxy-integrated “1D” spectrum, obtained according to Kewley et al. (2004) calibration;

(4)

the extinction-corrected SFR obtained from 24 μm and UV continuum by Tacconi et al. (2013);

(5)

the SFR extrapolated from the empirical calibration of Moustakas et al. (2006);

(6)

the gas mass derived from the IRAM Plateau de Bure observations;

(7)

the total star mass obtained by SED fittings from CFHT B, R, and I bands photometric data using kcorrect (Blanton & Roweis 2007), corrected for a Universe with H0 = 70  km   s-1   Mpc-1;

(8)

the gas fraction fgas = Mgas/(Mgas + Mstar);

(9)

the optical half light radius R1/2 as indicated in Tacconi et al. (2013);

(10)

the surface densities associated to the gas mass, the star formation rate, and the star mass, calculated within R1/2, for example as ;

(11)

Hα, visible, and [OII] extinctions as derived from the kcorrect SED reconstruction; and

(12)

the extinction ratio AHα/A[OII]. AV, A[OII], AHα/A[OII], SFR24μm+UV and SFR[OII],B are given for information only. O’Donnell (1994) predicts that AHα/A[OII] is around 1.86 for a diffuse interstellar medium, and the variations here observed from one galaxy to the other are representative of the quality of the kcorrect fit. The comparison between SFR[OII], SFR24μm+UV, and SFR[OII],B gives an idea of the uncertainties in the SFR.

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