The dust properties of z ~ 3 MIPS-LBGs from photo-chemical models

Abstract

The stacked spectral energy distribution (SED) of Multiband Imaging Photometer for Spitzer (MIPS) 24$\mu m$ detected Lyman break galaxies (MIPS-LBGs) is fitted by means of spectro-photometric model GRASIL with an "educated" fitting approach which benefits from results of chemical evolution models. The star formation rate(SFR)-age-metallicity degeneracies of SED modelling are broken by using SFH and chemical enrichment history suggested by chemical models, which also provide dust mass, dust abundance and chemical elements locked in dust component. We derive the total mass $M_{tot}$, stellar mass $M_{\ast }$, gas mass $M_g$, dust mass $M_d$, age and SFR of the stacked MIPS-LBG in a self-consistent way. Our estimate of $M_{\ast }=8\times 10^{10}$ agrees with other works based on UV-optical SED fitting. We suggest that MIPS-LBGs at $z\sim 3$ are young (0.3-0.6 Gyr), massive ($M_{tot}\sim 10^{11}{M}_{\odot }$), dusty ($M_d\sim 10^8{M}_{\odot }$), metal rich ($Z\sim Z_{\odot }$) progenitors of elliptical galaxies suffering a strong burst of star formation (SFR $\sim 200M_{\odot }/yr$). Our estimate of $M_d=7\times 10^7{M}_{\odot }$ of the stacked MIPS-LBG is about a factor of eight lower than the estimated value based on single temperature grey-body fitting, suggesting that self-consistent SED models are needed to estimate dust mass. By comparing with the Milky Way molecular cloud and dust properties, we suggest that denser and dustier environments and flatter dust size distribution are likely in high redshift massive star forming galaxies. These dust properties, as well as the different types of SFHs, can cause different SED shapes between high redshift star-forming ellipticals and local star-burst templates. This discrepancy of SED shapes could in turn explain the non detection at submillimeter wavelengths, of IR luminous ($L_{IR}⪰10^{12}{L}_{\odot }$) MIPS-LBGs.

31pages,9 figures, accepted for publication in ApJ

References in corpus (21)

• Infrared Emission from Interstellar Dust. IV. The Silicate-Graphite-PAH Model in the Post-Spitzer Era
• The Mass-Metallicity Relation at z~2
• The Stellar, Gas and Dynamical Masses of Star-Forming Galaxies at z~2
• Multi-Wavelength Constraints on the Cosmic Star Formation History from Spectroscopy: the Rest-Frame UV, H-alpha, and Infrared Luminosity Functions at Redshifts 1.9<z<3.4
• Dust size distributions in coagulation/fragmentation equilibrium: Numerical solutions and analytical fits
• Vigorous star formation with low efficiency in massive disk galaxies at z=1.5
• Dust in starburst nuclei and ULIRGs: SED models for observers
• Rest-Frame Optical Spectra of Three Strongly Lensed Galaxies at z~2
• Dust retention in protoplanetary disks
• The cycle of interstellar dust in galaxies of different morphological types
• The 1-1000 micron SEDs of far-infrared galaxies
• An HST/WFC3-IR Morphological Survey of Galaxies at z = 1.5-3.6: II. The Relation between Morphology and Gas-Phase Kinematics
• The insignificance of major mergers in driving star formation at z~2
• Lyman Break Galaxies at z~1 and the evolution of the dust attenuation in star-forming galaxies with the redshift
• SPITZER Observations of z~3 Lyman Break Galaxies: stellar masses and mid-infrared properties
• The complex physics of dusty star-forming galaxies at high redshifts as revealed by Herschel and Spitzer
• Modeling the effects of dust evolution on the SEDs of galaxies of different morphological type
• AEGIS: Infrared Spectroscopy of An Infrared Luminous Lyman Break Galaxy at z=3.01
• Modelling galaxy spectra in presence of interstellar dust. II. From the UV to the far infrared
• IRAC Photometric Analysis and the Mid-IR Photometric Properties of Lyman Break Galaxies
• Massive Lyman Break Galaxies at z~3 in the Spitzer Extragalactic First Look Survey

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