Disk galaxies with broken luminosity profiles from cosmological simulations Export

@article{citeulike:4774521, abstract = {We simulate the cosmological formation of three disk galaxies using the zoom-in technique and including a detailed treatment of chemical evolution and cooling. The resulting galaxies have a rather high disk-to-total ratio for a cosmological simulation and thin stellar disks. They present a break in the luminosity profile at 3.0 +- 0.5 disk scale lengths, while showing an exponential mass profile without any apparent breaks, in line with recent observational results. Since the stellar mass profile is exponential, only differences in the stellar populations can be the cause of the luminosity break. Although we find a cutoff for the star formation rate imposed by a density threshold in our star formation model, it does not coincide with the luminosity break and is located at 4.3 +- 0.4 disk scale lengths, with star formation going on between both radii. The color profiles and the age profiles are "U-shaped", with the minimum for both profiles located approximately at the break radius. The SFR to stellar mass ratio increases until the break, explaining the coincidence of the break with the minimum of the age profile. Beyond the break we find a steep decline in the gas density, possibly due to late gas accretion with an angular momentum that is not aligned with the disk. This prompts a sudden decline in the SFR and redder colors. The stellar mass profile remains exponential, we show that most stars in the outer disk originate in the inner disk and likely got there by means of migrations.}, archivePrefix = {arXiv}, author = {Mart\&\#xed;nez-Serrano, Francisco J. and Serna, Arturo and Dom\&\#xe9;nech-Moral, Mariola and Dom\&\#xed;nguez-Tenreiro, Rosa}, citeulike-article-id = {4774521}, citeulike-linkout-0 = {http://arxiv.org/abs/0906.1118}, citeulike-linkout-1 = {http://arxiv.org/pdf/0906.1118}, day = {5}, eprint = {0906.1118}, keywords = {disk, formation, simulation}, month = {Jun}, posted-at = {2009-06-08 09:08:01}, priority = {2}, title = {Disk galaxies with broken luminosity profiles from cosmological simulations}, url = {http://arxiv.org/abs/0906.1118}, year = {2009} }

TY - JOUR ID - citeulike:4774521 L3 - citeulike-article-id:4774521 N2 - We simulate the cosmological formation of three disk galaxies using the zoom-in technique and including a detailed treatment of chemical evolution and cooling. The resulting galaxies have a rather high disk-to-total ratio for a cosmological simulation and thin stellar disks. They present a break in the luminosity profile at 3.0 +- 0.5 disk scale lengths, while showing an exponential mass profile without any apparent breaks, in line with recent observational results. Since the stellar mass profile is exponential, only differences in the stellar populations can be the cause of the luminosity break. Although we find a cutoff for the star formation rate imposed by a density threshold in our star formation model, it does not coincide with the luminosity break and is located at 4.3 +- 0.4 disk scale lengths, with star formation going on between both radii. The color profiles and the age profiles are "U-shaped", with the minimum for both profiles located approximately at the break radius. The SFR to stellar mass ratio increases until the break, explaining the coincidence of the break with the minimum of the age profile. Beyond the break we find a steep decline in the gas density, possibly due to late gas accretion with an angular momentum that is not aligned with the disk. This prompts a sudden decline in the SFR and redder colors. The stellar mass profile remains exponential, we show that most stars in the outer disk originate in the inner disk and likely got there by means of migrations. TI - Disk galaxies with broken luminosity profiles from cosmological simulations KW - disk KW - formation KW - simulation AU - Martínez-Serrano, Francisco AU - Serna, Arturo AU - Doménech-Moral, Mariola AU - Domínguez-Tenreiro, Rosa PY - 2009/Jun/05/ UR - http://arxiv.org/abs/0906.1118 ER -