A low [CII]/[NII] ratio in the center of a massive galaxy at z = 3.7: Evidence for a transition to quiescence at high redshift?

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Volume 646 (February 2021)

A&A, 646 (2021) A68

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This article has an erratum: [https://doi.org/10.1051/0004-6361/201936460e]

Table 1.

Measured line fluxes from the image analysis, corresponding ionized gas fractions, and infrared luminosities.

	I_[C II]	I[N II]	[C II]/[N II]	f_[C II],ion	f_IR,ISM	log₁₀(L_IR/L_⊙)	log₁₀(L_IR, BC/L_⊙)
Flux origin	Jy km s⁻¹	Jy km s⁻¹	^(e)	%	%	^(f)
Total ^(a)							^(g)
Central ^(b)
Outskirts ^(c)
Peak pixel ^(d)

Notes.

^(a)

Summed flux inside a 3.5 kpc radius.

^(b)

Summed flux inside a 0.5 kpc radius.

^(c)

Summed flux between 0.5 and 3.5 kpc radius.

^(d)

Flux of the peak pixels on the ALMA image (warning: because of the poorer resolution, this method measures flux on a larger scale for [C II] than for [N II]).

^(e)

Ratio of the [C II] to [N II] flux, with fluxes expressed in W m².

^(f)

Total infrared luminosity (8−1000 μm), computed from the total L_IR estimated in Schreiber et al. (2018b) scaled by the fraction of [N II] continuum flux in each region.

^(g)

Computed as the sum of the central and outskirts luminosities.

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