2019MNRAS.488.3014P

Query : 2019MNRAS.488.3014P

2019MNRAS.488.3014P - Mon. Not. R. Astron. Soc., 488, 3014-3023 (2019/September-3)

Constraining the evolution of [C II] intensity through the end stages of reionization.

PADMANABHAN H.

Abstract (from CDS):

We combine available constraints on the local [C II] 158 µm line luminosity function from galaxy observations (Hemmati et al. 2017), with the evolution of the star formation rate density and the recent [C II] intensity mapping measurement in Pullen et al. (2018, assuming detection), to derive the evolution of the [C II] luminosity-halo mass relation over z ∼ 0-6. We develop convenient fitting forms for the evolution of the [C II] luminosity-halo mass relation and forecast constraints on the [C II] intensity mapping power spectrum and its associated uncertainty across redshifts. We predict the sensitivities to detect the power spectrum for upcoming PIXIE-, STARFIRE-, EXCLAIM-, CONCERTO-, TIME-, and CCAT-p-like surveys, as well as possible future intensity mapping observations with the ALMA (Atacama Large Millimetre Array) facility.

Abstract Copyright: © 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): cosmology: observations - cosmology: theory - radio lines: galaxies

Simbad objects: 1

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Number of rows : 1
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 NAME Hubble Deep Field reg 12 36 49.5 +62 12 58           ~ 1967 1

Query : 2019MNRAS.488.3014P

Basic data :
NAME Hubble Deep Field -- Region defined in the Sky
Other object types: otypes_help 		reg ()
ICRS coord. (ep=J2000) : 		12 36 49.5 +62 12 58 [ ] D ~
FK4 coord. (ep=B1950 eq=1950) : 		12 34 35.5 +62 29 28 [ ]
Gal coord. (ep=J2000) : 		125.8875 +54.8282 [ ]
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Identifiers (7) :
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NAME HDF NAME HDFN NAME Hubble Deep Field NAME Northern Hubble Deep Field
NAME HDF-N NAME NHDF NAME Hubble Deep Field North

References (1967 between 1850 and 2026) (Total 1967)
Simbad bibliographic survey began in 1850 for stars (at least bright stars) and in 1983 for all other objects (outside the solar system).
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