English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We present a sky simulation of the atomic HI emission line and the first tenCO rotational emission lines of molecular gas in galaxies beyond the Milky Way.The simulated sky field has a comoving diameter of 500/h Mpc, hence the actualfield-of-view depends on the (user-defined) maximal redshift zmax; e.g. forzmax=10, the field of view yields ~4x4 sqdeg. For all galaxies, we estimate theline 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 10^8Msun. This sky simulation builds on a semi-analytic model of the cosmicevolution of galaxies in a Lambda-cold dark matter (LCDM) cosmology. Theevolving CDM-distribution was adopted from the Millennium Simulation, an N-bodyCDM-simulation in a cubic box with a side length of 500/h Mpc. This side lengthlimits the coherence scale of our sky simulation: it is long enough to allowthe extraction of the baryon acoustic oscillations (BAOs) in the galaxy powerspectrum, yet the position and amplitude of the first acoustic peak will beimperfectly defined. This sky simulation is a tangible aid to the design andoperation of future telescopes, such the SKA, the LMT, and ALMA. The resultspresented in this paper have been restricted to a graphical representation ofthe simulated sky and fundamental dN/dz-analyzes for peak flux density limitedand total flux limited surveys of HI and CO. A key prediction is that HI willbe 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 toqualify the semi-analytic models.

A Virtual Sky with Extragalactic HI and CO Lines for the SKA and ALMA