The clustering of submillimeter galaxies detected with ALMA

Abstract

Previous studies measuring the clustering of submillimeter galaxies (SMGs) have based their measurements on single-dish detected sources, finding evidence for strong clustering. However, ALMA has revealed that, due to the coarse angular resolution of these instruments, single-dish sources can be comprised of multiple sources. This implies that the clustering inferred from single-dish surveys may be overestimated. Here, we measure the clustering of SMGs based on the ALESS survey, an ALMA follow-up of sources previously identified in the LABOCA ECDFS Submillimeter Survey (LESS). We present a method to measure the clustering of ALMA sources that have been previously identified using single-dish telescopes, based on forward modeling both the single-dish and the ALMA observations. We constrain upper limits for the median mass of halos hosting SMGs at $1<z<3$, finding $M_{\mathrm{halo}}\le 2.4\times 10^{12}{\mathrm{M}}_{\odot }$ for SMGs with flux densities $S_{870}\ge 4.0$mJy, which is at least $3.8_{-2.6}^{+3.8}$ times lower than the mass inferred based on the clustering of the LESS sources alone. This suggests that the strength of SMG clustering based on single-dish observations was overestimated and therefore SMGs might be hosted by dark matter halos less massive than has previously been estimated. By extrapolating our models down to flux densities of $S_{870}\ge 1.2$mJy, we find that such SMGs inhabit halos with median mass $M_{\mathrm{halo}}\le 3.2\times 10^{11}{\mathrm{M}}_{\odot }$. We conclude that only the brightest ($S_{870}\gtrsim 5-6$mJy) SMGs would trace massive structures at $z\sim 2$ and only SMGs with $S_{870}\gtrsim 6$mJy may be connected to massive local elliptical galaxies, quasars at intermediate redshifts and high-redshift star-forming galaxies, whereas fainter SMGs are unlikely linked to these populations.

arXiv comment20 pages, 14 figures, Accepted for publication in ApJ

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