The nature of 500 micron risers I: SMA observations

ABSTRACT We present SMA observations at resolutions from 0.35 to 3 arcsec of a sample of 34 candidate high redshift dusty star forming galaxies (DSFGs). These sources were selected from the HerMES Herschel survey catalogues to have SEDs rising from 250 to 350 to 500 μm, a population termed 500-riser...

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Veröffentlicht in:Monthly notices of the Royal Astronomical Society 2020-08, Vol.496 (2), p.2315-2333
Hauptverfasser: Greenslade, J, Clements, D L, Petitpas, G, Asboth, V, Conley, A, Pérez-Fournon, I, Riechers, D
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container_issue 2
container_start_page 2315
container_title Monthly notices of the Royal Astronomical Society
container_volume 496
creator Greenslade, J
Clements, D L
Petitpas, G
Asboth, V
Conley, A
Pérez-Fournon, I
Riechers, D
description ABSTRACT We present SMA observations at resolutions from 0.35 to 3 arcsec of a sample of 34 candidate high redshift dusty star forming galaxies (DSFGs). These sources were selected from the HerMES Herschel survey catalogues to have SEDs rising from 250 to 350 to 500 μm, a population termed 500-risers. We detect counterparts to 24 of these sources, with four having two counterparts. We conclude that the remaining ten sources that lack detected counterparts are likely to have three or more associated sources which blend together to produce the observed Herschel source. We examine the role of lensing, which is predicted to dominate the brightest (F500 > 60 mJy) half of our sample. We find that while lensing plays a role, at least 35 per cent of the bright sources are likely to be multiple sources rather than the result of lensing. At fainter fluxes we find a blending rate comparable to, or greater than, the predicted 40 per cent. We determine far-IR luminosities and star formation rates for the non-multiple sources in our sample and conclude that, in the absence of strong lensing, our 500-risers are very luminous systems with LFIR > 1013 L⊙ and star formation rates >1000 M⊙ yr−1.
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title The nature of 500 micron risers I: SMA observations
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