2013/04/03 by Christopher C. Hayward · 1 citation
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Flux (metallurgy) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Limit (mathematics) #Physics #Population #Radio Astronomy Observations and Technology #Redshift #Star (game theory) #Star formation #Stellar mass #astro-ph.CO
paper · pdf · doi:10.1093/mnrasl/slt047
published as MNRAS 432 (2013) L85-L89 · Accepted for publication in MNRAS Letters. 6 pages, 2 figures, and 1 table
arxiv created 2013/04/03 · openalex publication_date 2013/04/20 · arxiv updated 2014/06/02 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Abstract Explaining the observed number counts of submillimetre (submm) galaxies (SMGs) has been a longstanding challenge for theoretical models. Surprisingly, recent observations have suggested that the brightest SMGs are almost exclusively multiple fainter sources blended into a single source in the single-dish surveys. This result is in contrast with the predictions of our previously presented theoretical model, which includes some effects of blending. In this Letter, we consider the implications of an upper limit on the submm flux density for the demographics of the SMG population. Using a relation amongst submm flux, star formation rate (SFR) and dust mass (Md) from our previous work, we infer the maximum SFR for a range of flux density limits. For Md = 2 × 109(5 × 108) M⊙, the SFR limit that corresponds to an 870-μm flux density (S870) limit in the range 9–12.5 mJy is in the range ∼ 630\hbox--1400 (3600\hbox--7700) \mathrmM_\odot \rm yr-1. The SFR limit implies a correspondingly sharp, redshift-dependent cutoff in the stellar mass (M⋆) function, the value of which we predict using the S870–M⋆ relation predicted by our model. The M⋆ limit decreases with increasing redshift: for an S870 limit of 9–12.5 mJy, the M⋆ limit ranges from ∼4–7 × 1012 M⊙ at z ∼ 1 to ∼3–5 × 1011 M⊙ at z ∼ 6. We discuss the few interferometrically detected SMGs that may be brighter than the proposed cutoff. Although such objects are certainly interesting, inferences based on such objects may not apply to most SMGs.