Spitzer observations of red galaxies: Implication for high-redshift star formation

My colleagues and I identified distant red galaxies (DRGs) with J − Ks > 2.3 in the southern Great Observatories Origins Deep Surveys (GOODS-S) field. These galaxies reside at z ∼ 1–3.5, (〈z〉 ≃ 2.2) and based on their ACS (0.4–1 μm), ISAAC (1–2.2 μm), and IRAC (3–8 μm) photometry, they typically have stellar masses M ⩾ 1011 M⊙. Interestingly, more than 50% of these objects have 24 μm flux densities ⩾50 μJy. Attributing the IR emission to star-formation implies star-formation rates (SFRs) of ≃100–1000 M⊙ yr−1. As a result, galaxies with M ⩾ 1011 M⊙ have specific SFRs equal to or exceeding the global value at z ∼ 1.5–3. In contrast, galaxies with M ⩾ 1011 M⊙ at z ∼ 0.3–0.75 have specific SFRs less than the global average, and more than an order of magnitude lower than that for massive DRGs at z ∼ 1.5–3. Thus, the bulk of star formation in massive galaxies is largely complete by z ∼ 1.5. The red colors and large inferred stellar masses in the DRGs suggest that much of the star formation in these galaxies occurred at redshifts z ≳ 5–6. Using model star-formation histories that match the DRG colors and stellar masses at z ∼ 2–3, and measurements of the UV luminosity density at z ≳ 5–6, we consider what constraints exist on the stellar initial mass function in the progenitors of the massive DRGs at z ∼ 2–3.