Star forming and gas rich brightest cluster galaxies at $z\sim 0.4$ in the Kilo-Degree Survey

Abstract

Brightest Cluster Galaxies (BCGs) are typically massive ellipticals at the centers of clusters. They are believed to experience strong environmental processing, and their mass assembly and star formation history are still debated. We have selected three star forming BCGs in the equatorial field of the Kilo-Degree Survey (KiDS) at intermediate redshifts. We have observed them with the IRAM-30m telescope in the first three CO transitions. We remarkably detected all BCGs at high signal-to-noise ratio $S/N\simeq (3.8-10.2)$, for a total of 7 detected lines out of 8, corresponding to a success rate of $88\%$. This allows us to double the number of distant BCGs with clear detections in at least two CO lines. We have then combined our observations with available stellar, star formation, and dust properties of the BCGs, and we have compared them with a sample of $\sim 100$ distant cluster galaxies with observations in CO. Our analysis yields large molecular gas reservoirs $M_{H_2}\simeq (0.5-1.4)\times 10^{11}{M}_{\odot }$, excitation ratios $r_{31}=L_{\mathrm{CO}(3\to 2)}^{\prime }/L_{\mathrm{CO}(1\to 0)}^{\prime }\simeq (0.1-0.3)$, long depletion times ${\tau }_{\mathrm{dep}}\simeq (2-4)$~Gyr, and high $M_{H_2}/M_{\mathrm{dust}}\simeq (170-300)$. The excitation ratio $r_{31}$ of intermediate-$z$ BCGs appears to be well correlated with the star formation rate and efficiency, which suggests that excited gas is found only in highly star forming and cool-core BCGs. By performing color-magnitude plots and a red sequence modeling we find that recent bursts of star formation are needed to explain the fact that the BCGs are measurably bluer than photometrically selected cluster members. We suggest that a substantial amount of the molecular gas has been accreted by the KiDS BCGs, but still not efficiently converted into stars.

16 pages, 8 figures, version after the proof corrections, A&A in press

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