期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 428, 期 3, 页码 2529-2547出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/sts222
关键词
radiative transfer; stars: luminosity function, mass function; galaxies: high-redshift; galaxies: starburst; infrared: galaxies; submillimetre: galaxies
资金
- National Science Foundation [AST-1009452]
- NASA [HST-HF-51276.01-A]
- W. M. Keck Foundation
High-redshift submillimetre galaxies (SMGs) are some of the most rapidly star-forming galaxies in the Universe. Historically, galaxy formation models have had difficulty explaining the observed number counts of SMGs. We combine a semi-empirical model with 3D hydrodynamical simulations and 3D dust radiative transfer to predict the number counts of unlensed SMGs. Because the stellar mass functions, gas and dust masses, and sizes of our galaxies are constrained to match observations, we can isolate uncertainties related to the dynamical evolution of galaxy mergers and the dust radiative transfer. The number counts and redshift distributions predicted by our model agree well with observations. Isolated disc galaxies dominate the faint (S-1.1 less than or similar to 1 or S-850 less than or similar to 2 mJy) population. The brighter sources are a mix of merger-induced starbursts and galaxy-pair SMGs; the latter subpopulation accounts for similar to 30-50 per cent of all SMGs at all S-1.1 greater than or similar to 0.5mJy (S-850 greater than or similar to 1 mJy). The mean redshifts are similar to 3.0-3.5, depending on the flux cut, and the brightest sources tend to be at higher redshifts. Because the galaxy-pair SMGs will be resolved into multiple fainter sources by the Atacama Large Millimeter/submillimeter Array (ALMA), the bright ALMA counts should be as much as two times less than those observed using single-dish telescopes. The agreement between our model, which uses a Kroupa initial mass function (IMF), and observations suggests that the IMF in high-redshift starbursts need not be top heavy; if the IMF were top heavy, our model would overpredict the number counts. We conclude that the difficulty some models have reproducing the observed SMG counts is likely indicative of more general problems - such as an underprediction of the abundance of massive galaxies or a star formation rate and stellar mass relation normalization lower than that observed - rather than a problem specific to the SMG population.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据