Duty Cycle and the Increasing Star Formation History of z \geq 6 Galaxies

Details Duty Cycle and the Increasing Star Formation History of z \geq 6 Galaxies Duty Cycle and the Increasing Star Formation History of z \geq 6 Galaxies

2012-04-21

arxiv.org/abs/1204.4846v1

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

11 pages, 8 figures, 5 tables

Scientific paper

We examine the duty cycle and the history of star formation (SFH) for high-redshift galaxies at z \geq 6 using cosmological hydrodynamic simulations. We find that, even though individual galaxies have bursty SFH, the averaged SFH between z ~ 15 to z = 6 can be characterized well by either an exponentially increasing functional form with characteristic time-scales of 70 Myr to 200 Myr for galaxies with stellar masses Ms \sim 10^6 M\odot to > 10^10 M\odot respectively, or by a simple power-law form which exhibits a similar mass dependent time-scales. Using the SFH of individual galaxies, we measure the duty cycle of star formation (DC_SFH); i.e., the fraction of time a galaxy of a particular mass spends above a star formation rate (SFR) threshold which would make it observable to the Hubble Space Telescope (HST) during a given epoch. We also examine the fraction of galaxies at a given redshift that are brighter than a rest-frame UV magnitude Muv, which is sufficient enough to make them observable (DC_Muv). We find that both DC_SFH and DC_Muv make a sharp transition from zero (for galaxies with Ms \leq 10^7 M\odot) to unity (for Ms > 10^9 M\odot). The measured duty cycle is also manifested in the intrinsic scatter in the Ms-SFR relationship (\sim 1 dex) and Ms-Muv relationship (\Delta Muv \sim \pm 1 mag). We provide analytic fits to the DC as a function of Ms using a sigmoid function, which can be used in semi-analytic models of galaxy formation. We consider the effects of duty cycle to the observational estimate of galaxy stellar mass functions (GSMF) and the star formation rate density (SFRD), and find that it results in a much shallower low-mass end slopes of the GSMF and a reduction of \geq 70% of our intrinsic SFRD, making our simulation results more compatible with observational estimates.

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