Average weekly food waste disposal for southern Ontario households and impact of waste auditor, sampling area type, access to food waste diversion programs and season.

<p>Average weekly food waste disposal for southern Ontario households and impact of waste auditor, sampling area type, access to food waste diversion programs and season.</p

Multiple regression on summer food waste disposal (kg/household/week).

<p>Multiple regression on summer food waste disposal (kg/household/week).</p

Overall waste composition.

<p>Overall waste composition.</p

Multiple regression on spring food waste disposal (kg/household/week).

<p>Multiple regression on spring food waste disposal (kg/household/week).</p

Food waste disposal by season and sampling area type.

<p>Food waste disposal by season and sampling area type.</p

Avoidable and unavoidable food waste disposal.

<p>Avoidable and unavoidable food waste disposal.</p

Life beyond 30: Probing the −20 < MUV < −17 Luminosity Function at 8 < z < 13 with the NIRCam Parallel Field of the MIRI Deep Survey

We present the ultraviolet luminosity function and an estimate of the cosmic star formation rate density at 8 8 galaxy candidates based on their dropout nature in the F115W and/or F150W filters, a high probability for their photometric redshifts, estimated with three different codes, being at z > 8, good fits based on χ 2 calculations, and predominant solutions compared to z < 8 alternatives. We find mild evolution in the luminosity function from z ∼ 13 to z ∼ 8, i.e., only a small increase in the average number density of ∼0.2 dex, while the faint-end slope and absolute magnitude of the knee remain approximately constant, with values α = − 2.2 ± 0.1, and M * = − 20.8 ± 0.2 mag. Comparing our results with the predictions of state-of-the-art galaxy evolution models, we find two main results: (1) a slower increase with time in the cosmic star formation rate density compared to a steeper rise predicted by models; (2) nearly a factor of 10 higher star formation activity concentrated in scales around 2 kpc in galaxies with stellar masses ∼108 M ⊙ during the first 350 Myr of the universe, z ∼ 12, with models matching better the luminosity density observational estimations ∼150 Myr later, by z ∼ 9.</p