Section \[sec:simul\]. The discussion and summary follow in Section \[sec:discussion\]. Throughout the paper, we adopt a concordance $\Lambda$CDM cosmology with $H_0 = 70$ km s$^{-1}$ Mpc$^{-1}$, $\Omega_M = 0.3$, and $\Omega_{\Lambda} = 0.7$. We use the AB magnitude system [@oke83] and a @salpeter55 initial mass function (IMF) between 0.1 [$M_{\odot}$]{} and 100 [$M_{\odot}$]{}. We refer to the [*Hubble Space Telescope*]{} ([*HST*]{}) bands F435W, F606W, F775W, F814W, F850LP, F098M, F105W, F125W, F140W, and F160W as *B$_{435}$, V$_{606}$, i$_{775}$, I$_{814}$, z$_{850}$, Y$_{098}$, Y$_{105}$, J$_{125}$, JH$_{140}$, [and]{} H$_{160}$*, respectively. All quoted uncertainties are at 68% confidence intervals.

Data {#sec:data}
====

*HST* Data and Sample Selection
-------------------------------

The targets were selected in the GOODS-S field from the parent sample from @finkelstein15b. The parent sample was selected via photometric redshifts, which were estimated with [EAZY]{} [@brammer08], using the [*HST*]{} data set from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey [CANDELS; @grogin11; @koekemoer11] which incorporates all earlier imaging data over the field as described by @koekemoer11 [@koekemoer13]. The MOSFIRE slit design was prepared using the MAGMA configurable slit unit (CSU) design tool. This tool takes as an input a list of objects, along with relative priorities. Our priority scheme was based on two quantities: the 