COMÉRCIO ELETRÔNICO E MÍDIAS SOCIAIS PARA ALAVANCAR AS VENDAS DA R &amp; R DOCES E EMBALAGENS COMÉRCIO LTDA

Cunha, Renata Aguiar Da; Oliveira, Rodrigo Cesar Reis De; Walter, José; Ribeiro, Ulisses Jose; Cedraz, Aline

doi:10.14488/enegep2018_tn_sto_265_521_35116

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“…Thus, our results demonstrate that the position of DSFGs in the IRX − β plane does not necessarily imply that they are short-lived starbursts, contrary to the claim of Casey et al (2014); instead, DSFGs well above the M99 relation can be steadily star-forming, massive, gas-rich disks as long as they are sufficiently dust-obscured, which is a natural outcome for high-gas-fraction, metal-enriched galaxies. Consequently, high-z DSFGs may represent a heterogeneous population of massive, gas-rich, steadily starforming galaxies, merger-induced starbursts, and obscured AGN (e.g., Hopkins et al 2010;Hayward et al 2011Hayward et al , 2012Hayward et al , 2013bda Cunha et al 2015;Koprowski et al 2016). We do find that all of the simulated galaxies with L IR > 10 13 L (see also Hopkins et al 2010) and, of the lower-luminosity simulated galaxies, those with the highest IRX values (log IRX 2.5) are exclusively mergers, and in the simulations, these HyLIRGs are typically powered by combination of merger-induced starbursts and obscured AGN (Roebuck et al, submitted).…”

Section: Dsfgs In the Irx-β Planementioning

confidence: 99%

The IRX–β Relation: Insights from Simulations

Safarzadeh

Hayward

Ferguson

2017

ApJ

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We study the relationship between the UV continuum slope and infrared excess ( º L L IRX IR FUV ) predicted by performing dust radiative transfer on a suite of hydrodynamical simulations of galaxies. Our suite includes both isolated disk galaxies and mergers intended to be representative of galaxies at bothz 0 and~-z 2 3. Our lowredshift systems often populate a region around the locally calibrated Meurer et al. relation but move above the relation during merger-induced starbursts. Our high-redshift systems are blue and IR luminous and therefore lie above the Meurer et al. relation. The value of β strongly depends on the dust type used in the RT simulation: Milky-Way-type dust leads to significantly more negative (bluer) slopes compared with Small-Magellanic-Cloudtype dust. The effect on β due to variations in the dust composition with galaxy properties or redshift is the dominant model uncertainty. The dispersion in β is anticorrelated with specific star formation rate (sSFR) and tends to be higher for the~-z 2 3 simulations. In the actively star-forming~-z 2 3 simulated galaxies, dust attenuation dominates the dispersion in β, whereas in thez 0 simulations, the contributions of star formation history (SFH) variations and dust are similar. For low-sSFR systems at both redshifts, SFH variations dominate the dispersion. Finally, the simulated~-z 2 3 isolated disks and mergers both occupy a region in the b -IRX plane consistent with observed~-z 2 3 dusty star-forming galaxies (DSFGs). Thus, contrary to some claims in the literature, the blue colors of high-z DSFGs do not imply that they are short-lived starbursts.

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