Strong C+ emission in galaxies at z~1-2: Evidence for cold flow accretion powered star formation in the early Universe

TL;DR

This study detects strong [CII] emission in galaxies at redshifts 1-2, indicating star formation driven by cold gas accretion from the cosmic web, with implications for understanding early Universe galaxy growth.

Contribution

First comprehensive [CII] and [OI] observations in z~1-2 galaxies, linking high [CII] emission to cold flow accretion and elevated star formation rates in the early Universe.

Findings

High [CII]/FIR ratios indicating efficient gas heating.

Evidence of high molecular gas surface densities from infall of cosmic web gas.

Possible additional [CII] excitation mechanisms like shocks.

Abstract

We have recently detected the [CII] 157.7 micron line in eight star forming galaxies at redshifts 1 to 2 using the redshift(z) Early Universe Spectrometer (ZEUS). Our sample targets star formation dominant sources detected in PAH emission. This represents a significant addition to [CII] observations during the epoch of peak star formation. We have augmented this survey with observations of the [OI] 63 micron line and far infrared photometry from the PACS and SPIRE Herschel instruments as well as Spitzer IRS spectra from the literature showing PAH features. Our sources exhibit above average gas heating efficiency, many with both [OI]/FIR and [CII]/FIR ~1% or more. The relatively strong [CII] emission is consistent with our sources being dominated by star formation powered PDRs, extending to kpc scales. We suggest that the star formation mode in these systems follows a Schmidt-Kennicutt law similar to local systems, but at a much higher rate due to molecular gas surface densities 10 to 100 times that of local star forming systems. The source of the high molecular gas surface densities may be the infall of neutral gas from the cosmic web. In addition to the high [CII]/FIR values, we also find high [CII]/PAH ratios and, in at least one source, a cool dust temperature. This source, SWIRE 4-5, bears a resemblance in these diagnostics to shocked regions of Stephan's Quintet, suggesting that another mode of [CII] excitation in addition to normal photoelectric heating may be contributing to the observed [CII] line.