A Physical Model for z~2 Dust Obscured Galaxies Export

@article{citeulike:5938019, abstract = {We present a physical model for the origin of z\~{}2 Dust-Obscured Galaxies (DOGs), a class of high-redshift ULIRGs selected at 24 micron which are particularly optically faint (F24/FR\>1000). By combining N-body/SPH simulations of high redshift galaxy evolution with 3D polychromatic dust radiative transfer models, we find that luminous DOGs (with F24 \> 0.3 mJy at z\~{}2) are well-modeled as extreme gas-rich mergers in massive (\~{}5x10^12-10^13 Msun) halos, with elevated star formation rates (\~{}500-1000 Msun/yr) and/or significant AGN growth (Mdot(BH) \> 0.5 Msun/yr), whereas less luminous DOGs are more diverse in nature. Merger-driven DOGs are caught in a stage transitioning from being starburst dominated to AGN dominated, evolving from a "bump" to a power-law shaped mid-IR (IRAC) spectral energy distribution (SED). While canonically power-law galaxies are associated with being AGN-dominated, we find that the power-law mid-IR SED can owe both to direct AGN contribution, as well as to a heavily dust obscured stellar bump at times that the galaxy is starburst dominated. Thus power-law galaxies can be either starburst or AGN dominated. Less luminous DOGs (100 \< F24 \< 300 microJy at z=2) can be well-represented either by mergers, or by less extreme secularly evolving gas-rich disk galaxies (with SFR \> 50 Msun/yr). We find that some merger-driven DOGs can be selected as Submillimeter Galaxies (SMGs), while both merger-driven and secularly evolving DOGs typically satisfy the BzK selection criteria. Our models provide testable predictions of the physical masses, dust temperatures, CO line widths and location on the M*-MBH relation of DOGs. Finally, we provide public SED templates derived from these simulations.}, archivePrefix = {arXiv}, author = {Narayanan, Desika and Dey, Arjun and Hayward, Christopher and Cox, Thomas J. and Bussmann, R. Shane and Brodwin, Mark and Jonsson, Patrik and Hopkins, Philip and Groves, Brent and Younger, Joshua D. and Hernquist, Lars}, citeulike-article-id = {5938019}, citeulike-linkout-0 = {http://arxiv.org/abs/0910.2234}, citeulike-linkout-1 = {http://arxiv.org/pdf/0910.2234}, day = {15}, eprint = {0910.2234}, keywords = {agn, co, dog, dust, formation, highz, mir, sed, smbh, starburst}, month = {Oct}, posted-at = {2009-10-14 16:05:12}, priority = {2}, title = {A Physical Model for z\~{}2 Dust Obscured Galaxies}, url = {http://arxiv.org/abs/0910.2234}, year = {2009} }

TY - JOUR ID - citeulike:5938019 L3 - citeulike-article-id:5938019 N2 - We present a physical model for the origin of z~2 Dust-Obscured Galaxies (DOGs), a class of high-redshift ULIRGs selected at 24 micron which are particularly optically faint (F24/FR>1000). By combining N-body/SPH simulations of high redshift galaxy evolution with 3D polychromatic dust radiative transfer models, we find that luminous DOGs (with F24 > 0.3 mJy at z~2) are well-modeled as extreme gas-rich mergers in massive (~5x10^12-10^13 Msun) halos, with elevated star formation rates (~500-1000 Msun/yr) and/or significant AGN growth (Mdot(BH) > 0.5 Msun/yr), whereas less luminous DOGs are more diverse in nature. Merger-driven DOGs are caught in a stage transitioning from being starburst dominated to AGN dominated, evolving from a "bump" to a power-law shaped mid-IR (IRAC) spectral energy distribution (SED). While canonically power-law galaxies are associated with being AGN-dominated, we find that the power-law mid-IR SED can owe both to direct AGN contribution, as well as to a heavily dust obscured stellar bump at times that the galaxy is starburst dominated. Thus power-law galaxies can be either starburst or AGN dominated. Less luminous DOGs (100 < F24 < 300 microJy at z=2) can be well-represented either by mergers, or by less extreme secularly evolving gas-rich disk galaxies (with SFR > 50 Msun/yr). We find that some merger-driven DOGs can be selected as Submillimeter Galaxies (SMGs), while both merger-driven and secularly evolving DOGs typically satisfy the BzK selection criteria. Our models provide testable predictions of the physical masses, dust temperatures, CO line widths and location on the M*-MBH relation of DOGs. Finally, we provide public SED templates derived from these simulations. TI - A Physical Model for z~2 Dust Obscured Galaxies KW - agn KW - co KW - dog KW - dust KW - formation KW - highz KW - mir KW - sed KW - smbh KW - starburst AU - Narayanan, Desika AU - Dey, Arjun AU - Hayward, Christopher AU - Cox, Thomas AU - Bussmann, Shane AU - Brodwin, Mark AU - Jonsson, Patrik AU - Hopkins, Philip AU - Groves, Brent AU - Younger, Joshua AU - Hernquist, Lars PY - 2009/Oct/15/ UR - http://arxiv.org/abs/0910.2234 ER -