Frontier Fields: Combining HST, VLT, and Spitzer data to explore the z ∼ 8 Universe behind the lensing cluster MACSJ0416.1-2403

Context. The Hubble Space Telescope (HST) Frontier Fields (HFFs) project started at the end of 2013 with the aim of providing extremely deep images of six massive galaxy clusters. One of the main goals of this program is to push several telescopes to their limits to provide the best current view of the earliest stages of the Universe. The analysis of the initial data has already demonstrated the huge capabilities of the program. Aims. We present a detailed analysis of z similar to 8 objects behind the HFFs lensing cluster, MACSJ0416.1-2403, combining 0.3-1.6 mu m imaging from HST, ground-based K-s imaging from VLT HAWK-I, and 3.6 mu m and 4.5 mu m Spitzer Space Telescope. The images probe to 5 sigma depths of approximate to 29 AB for HST, 25.6 AB for HAWK-I, and approximate to 0.310 and 0.391 mu Jy at 3.6 and 4.5 mu m, respectively. With these datasets, we assess the photometric properties of z similar to 8 galaxies in this field, as well as their distribution in luminosity, to unprecedented sensitivity. Methods. We applied the classical Lyman break (LB) technique, which combines non detection criteria in bands blueward of the Lyman break at z similar to 8 and color-selection in bands redward of the break. To avoid contamination by mid-z interlopers, we required a strong break between optical and near-infrared data. We determined the photometric properties of z similar to 8 selected candidates using spectral energy distribution (SED)-fitting with standard library templates. The luminosity function at z similar to 8 is computed using a Monte-Carlo method taking advantage of the SED-fitting results. A piece of cautionary information is gleaned from new deep optical photometry of a previously identified z similar to 8 galaxy in this cluster, which is now firmly detected as a mid-z interloper with a strong approximate to 1.5 mag Balmer break (between F606W and F125W). Using the SED of this interloper, we estimated the contamination rate of our MACSJ0416.1-2403 sample, and that of previous samples in Abell 2744 that were based on HFF data, we highlight the dangers of pushing the LB technique too close to the photometry limits. Results. Our selection reliably recovers four objects with mflow ranging from 26.0 to 27.9 AB that are located in modestamplification regions (mu < 2.4). Two of the objects display a secondary break between the IRAC 3.6 mu m and 4.5 mu m bands, which could be associated to the Balmer break or emission lines at z similar to 8. The SED-fitting analysis suggests that all of these objects favor high-z solutions with no reliable secondary solutions. The candidates generally have star formation rates around similar to 10 M-circle dot/yr and sizes ranging from 0.2 to 0.5 kpc, which agrees well with previous observations and expectations for objects in the early Universe. The sample size and luminosity distribution are consistent with previous findings.