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Searching Far and Long I: Pilot ALMA 2mm Follow-up of Bright Dusty Galaxies as a Redshift Filter
Authors
Caitlin M. Casey
Jaclyn B. Champagne
+6Â more
Olivia R. Cooper
Elisabete da Cunha
Arianna S. Long
Justin S. Spilker
Johannes Staguhn
Jorge A. Zavala
Publication date
28 March 2022
Publisher
View
on
arXiv
Abstract
A complete census of dusty star-forming galaxies (DSFGs) at early epochs is necessary to constrain the obscured contribution to the cosmic star formation rate density (CSFRD), however DSFGs beyond
z
∼
4
z \sim 4
z
∼
4
are both rare and hard to identify from photometric data alone due to degeneracies in submillimeter photometry with redshift. Here, we present a pilot study obtaining follow-up Atacama Large Millimeter Array (ALMA)
2
 
2\,
2
mm observations of a complete sample of 39
850
 
μ
m
850\,\rm\mu m
850
μ
m
-bright dusty galaxies in the SSA22 field. Empirical modeling suggests
2
 
2\,
2
mm imaging of existing samples of DSFGs selected at
850
 
μ
m
−
1
 
850\,\rm\mu m - 1\,
850
μ
m
−
1
mm can quickly and easily isolate the "needle in a haystack" DSFGs that sit at
z
>
4
z>4
z
>
4
or beyond. Combining archival submillimeter imaging with our measured ALMA
2
 
2\,
2
mm photometry (
1
σ
∼
0.08
 
1\sigma \sim 0.08\,
1
σ
∼
0.08
mJy
 
\,
beam
−
1
^{-1}
−
1
rms), we characterize the galaxies' IR SEDs and use them to constrain redshifts. With available redshift constraints fit via the combination of six submillimeter bands, we identify 6/39 high-
z
z
z
candidates each with
>
50
%
>50\%
>
50%
likelihood to sit at
z
>
4
z > 4
z
>
4
, and find a positive correlation between redshift and
2
 
2\,
2
mm flux density. Specifically, our models suggest the addition of
2
 
2\,
2
mm to a moderately constrained IR SED will improve the accuracy of a millimeter-derived redshift from
Δ
z
/
(
1
+
z
)
=
0.3
\Delta z/(1+z) = 0.3
Δ
z
/
(
1
+
z
)
=
0.3
to
Δ
z
/
(
1
+
z
)
=
0.2
\Delta z/(1+z) = 0.2
Δ
z
/
(
1
+
z
)
=
0.2
. Our IR SED characterizations provide evidence for relatively high emissivity spectral indices (
⟨
β
⟩
=
2.4
±
0.3
\langle \beta \rangle = 2.4\pm0.3
⟨
β
⟩
=
2.4
±
0.3
) in the sample. We measure that especially bright (
S
850
μ
m
>
5.55
 
S_{850\rm\mu m}>5.55\,
S
850
μ
m
​
>
5.55
mJy) DSFGs contribute
∼
10
\sim10
∼
10
% to the cosmic-averaged CSFRD from
2
<
z
<
5
2<z<5
2
<
z
<
5
, confirming findings from previous work with similar samples.Comment: 22 pages, 7 figures, accepted for publication in Ap
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oai:arXiv.org:2203.14973
Last time updated on 24/04/2022