000162226 001__ 162226
000162226 005__ 20190316235018.0
000162226 0247_ $$2doi$$a10.1088/0004-637X/703/2/1890
000162226 022__ $$a0004-637X
000162226 037__ $$aARTICLE
000162226 245__ $$aA virtual sky with extragalactic HI and CO lines for the Square Kilometre Array (SKA) and the Atacama Large Millimeter/submillimeter Array (ALMA)
000162226 269__ $$a2009
000162226 260__ $$bAmerican Astronomical Society$$c2009
000162226 336__ $$aJournal Articles
000162226 520__ $$aWe present a sky simulation of the atomic HI-emission line and the first 10 rotational CO emission lines of molecular gas in galaxies beyond the Milky Way. The simulated sky field has a comoving diameter of 500 Mpc/h; hence, the actual field-of-view depends on the (user-defined) maximal redshift zmax; e. g., for zmax=10, the field of view yields 4x4 deg^2. For all galaxies, we estimate the line fluxes, line profiles, and angular sizes of the Hi and CO-emission lines. The galaxy sample is complete for galaxies with cold hydrogen masses above 10^8 Msun. This sky simulation builds on a semi-analytic model of the cosmic evolution of galaxies in a Lambda-cold dark matter (Lambda CDM) cosmology. The evolving CDM distribution was adopted from the Millennium Simulation, an N-body CDM-simulation in a cubic box with a side length of 500 Mpc/h. This side length limits the coherence scale of our sky simulation: it is long enough to allow the extraction of the baryon acoustic oscillations in the galaxy power spectrum, yet the position and amplitude of the first acoustic peak will be imperfectly defined. This sky simulation is a tangible aid to the design and operation of future telescopes, such as the Square Kilometre Array, Large Millimeter Telescope, and Atacama Large Millimeter/submillimeter Array. The results presented in this paper have been restricted to a graphical representation of the simulated sky and fundamental dN/dz-analyses for peak flux density limited and total flux limited surveys of Hi and CO. A key prediction is that HI will be harder to detect at redshifts z>2 than predicted by a no-evolution model. The future verification or falsification of this prediction will allow us to qualify the semi-analytic models.
000162226 6531_ $$acosmology: theory
000162226 6531_ $$agalaxies: evolution
000162226 6531_ $$agalaxies: high-redshift
000162226 6531_ $$aISM: atoms
000162226 6531_ $$aISM: molecules
000162226 6531_ $$aGalaxy Redshift Survey
000162226 6531_ $$aIntegral Field Spectroscopy
000162226 6531_ $$aStar-Forming Galaxies
000162226 6531_ $$aTully-Fisher Relation
000162226 6531_ $$a21 Cm Signal
000162226 6531_ $$aLuminosity Functions
000162226 6531_ $$aNeutral Hydrogen
000162226 6531_ $$aMolecular Gas
000162226 6531_ $$aCosmological Simulations
000162226 6531_ $$aCosmic Evolution
000162226 700__ $$aObreschkow, D.
000162226 700__ $$aKloeckner, H.-R.
000162226 700__ $$aHeywood, I.
000162226 700__ $$aLevrier, F.
000162226 700__ $$aRawlings, S.
000162226 773__ $$j703$$q1890-1903$$tAstrophysical Journal
000162226 8564_ $$s2430649$$uhttps://infoscience.epfl.ch/record/162226/files/obreschkow_paper6.pdf$$yPostprint$$zPostprint
000162226 909C0 $$0252446$$pIGM$$xU10306
000162226 909CO $$ooai:infoscience.tind.io:162226$$pSTI$$particle$$qGLOBAL_SET
000162226 917Z8 $$x130271
000162226 917Z8 $$x130271
000162226 917Z8 $$x130271
000162226 917Z8 $$x148230
000162226 937__ $$aEPFL-ARTICLE-162226
000162226 973__ $$aOTHER$$rREVIEWED$$sPUBLISHED
000162226 980__ $$aARTICLE