The clustering of submillimeter galaxies detected with ALMA
  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
$M_{\rm{halo}}\leq2.4\times10^{12}\,\rm\,M_{\odot}$ for SMGs with flux
densities $S_{870}\geq4.0\,$mJy, which is at least $3.8^{+3.8}_{-2.6}$ 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 $S_{870}\geq1.2\,\rm\,$mJy, we find that
such SMGs inhabit halos with median mass
$M_{\rm{halo}}\leq3.2\times10^{11}\,\rm\,M_{\odot}$. We conclude that only the
brightest ($S_{870}\gtrsim5-6\,\rm\,$mJy) SMGs would trace massive structures
at $z\sim2$ and only SMGs with $S_{870}\gtrsim6\,\rm\,$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.
