TY - JOUR
T1 - An intensity mapping detection of aggregate co line emission at 3mm
AU - Keating, Garrett K.
AU - Marrone, Daniel P.
AU - Bower, Geoffrey C.
AU - Keenan, Ryan P.
N1 - Publisher Copyright:
© 2020 Institute of Physics Publishing. All rights reserved.
PY - 2020/10/1
Y1 - 2020/10/1
N2 - We present a detection of molecular gas emission at z ∼ 1-5 using the technique of line intensity mapping. We make use of a pair of 3mm interferometric data sets, the first from the Atacama Large Millimeter/submillimeter Array (ALMA) Spectroscopic Survey in the Hubble Ultra Deep Field, and the second from a series of Atacama Compact Array (ACA) observations conducted between 2016 and 2018, targeting the COSMOS field. At 100 GHz, we measure nonzero power at 97.8% and 99.9% confidence in the ACA and ALMA data sets, respectively. In the joint result, we reject the zeropower hypothesis at 99.99% confidence, finding Is (ν)= 770 ±210 μK2 Hz sr . After accounting for sample variance effects, the estimated spectral shot power is I2s (ν) = - 1010+550-390μ μK2 Hz sr s . We derive a model for the various line species our measurement is expected to be sensitive to, and estimate the shot power to be - 120+70-50 μK2 h-3 Mpc3 - 210+110-80 μK2 h-3 Mpc3 , and 100+50-40 μK2 h-3 Mpc3 for CO(2-1) at z = 1.3, CO(3-2) at z = 2.5, and CO(4-3) at z = 3.6, respectively. Using line ratios appropriate for high-redshift galaxies, we find these results to be in good agreement with those from the CO Power Spectrum Survey. Adopting αCO = 3.6M⊙ (Kkms-1 pc2)-1, we estimate a cosmic molecular gas density of ρH2 (z) ∼ 108M⊙ Mpc-3 between z = 1-3.
AB - We present a detection of molecular gas emission at z ∼ 1-5 using the technique of line intensity mapping. We make use of a pair of 3mm interferometric data sets, the first from the Atacama Large Millimeter/submillimeter Array (ALMA) Spectroscopic Survey in the Hubble Ultra Deep Field, and the second from a series of Atacama Compact Array (ACA) observations conducted between 2016 and 2018, targeting the COSMOS field. At 100 GHz, we measure nonzero power at 97.8% and 99.9% confidence in the ACA and ALMA data sets, respectively. In the joint result, we reject the zeropower hypothesis at 99.99% confidence, finding Is (ν)= 770 ±210 μK2 Hz sr . After accounting for sample variance effects, the estimated spectral shot power is I2s (ν) = - 1010+550-390μ μK2 Hz sr s . We derive a model for the various line species our measurement is expected to be sensitive to, and estimate the shot power to be - 120+70-50 μK2 h-3 Mpc3 - 210+110-80 μK2 h-3 Mpc3 , and 100+50-40 μK2 h-3 Mpc3 for CO(2-1) at z = 1.3, CO(3-2) at z = 2.5, and CO(4-3) at z = 3.6, respectively. Using line ratios appropriate for high-redshift galaxies, we find these results to be in good agreement with those from the CO Power Spectrum Survey. Adopting αCO = 3.6M⊙ (Kkms-1 pc2)-1, we estimate a cosmic molecular gas density of ρH2 (z) ∼ 108M⊙ Mpc-3 between z = 1-3.
KW - Cosmological evolution (336)
KW - Early universe (435)
KW - Molecular gas (1073)
KW - Star formation (1569)
UR - http://www.scopus.com/inward/record.url?scp=85092915722&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85092915722&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/abb08e
DO - 10.3847/1538-4357/abb08e
M3 - Article
AN - SCOPUS:85092915722
SN - 0004-637X
VL - 901
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - abb08e
ER -