Herschel and ALMA Observations of Massive SZE-selected Clusters
  We present new Herschel observations of four massive, Sunyaev-Zel'dovich
Effect (SZE)-selected clusters at $0.3 \leq z \leq 1.1$, two of which have also
been observed with ALMA. We detect 19 Herschel/PACS counterparts to
spectroscopically confirmed cluster members, five of which have redshifts
determined via CO($4-3$) and [CI](${}^3P_1 - {}^3P_0$) lines. The mean [CI]/CO
line ratio is $0.19 \pm 0.07$ in brightness temperature units, consistent with
previous results for field samples. We do not detect significant stacked ALMA
dust continuum or spectral line emission, implying upper limits on mean
interstellar medium (H$_2$ + HI) and molecular gas masses. An apparent
anticorrelation of $L_{IR}$ with clustercentric radius is driven by the tight
relation between star formation rate and stellar mass. We find average specific
star formation rate log(sSFR/yr$^{-1}$) = -10.36, which is below the SFR$-M_*$
correlation measured for field galaxies at similar redshifts. The fraction of
infrared-bright galaxies (IRBGs; $\log (L_{IR}/L_\odot) > 10.6$) per cluster
and average sSFR rise significantly with redshift. For CO detections, we find
$f_{gas} \sim 0.2$, comparable to those of field galaxies, and gas depletion
timescales of about 2 Gyr. We use radio observations to distinguish active
galactic nuclei (AGNs) from star-forming galaxies. At least four of our 19
Herschel cluster members have $q_{IR} < 1.8$, implying an AGN fraction $f_{AGN}
\gtrsim 0.2$ for our PACS-selected sample.
