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 Tools annual

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 monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

Intensity mapping provides a unique means to probe the epoch of reionization(EoR), when the neutral intergalactic medium was ionized by the energeticphotons emitted from the first galaxies. The [CII] 158$\mu$m fine-structureline is typically one of the brightest emission lines of star-forming galaxiesand thus a promising tracer of the global EoR star-formation activity. However,[CII] intensity maps at $6 \lesssim z \lesssim 8$ are contaminated byinterloping CO rotational line emission ($3 \leq J_{\rm upp} \leq 6$) fromlower-redshift galaxies. Here we present a strategy to remove the foregroundcontamination in upcoming [CII] intensity mapping experiments, guided by amodel of CO emission from foreground galaxies. The model is based on empiricalmeasurements of the mean and scatter of the total infrared luminosities ofgalaxies at $z < 3$ and with stellar masses $M_{*} > 10^{8}\,\rm M_{\rm \odot}$selected in $K$-band from the COSMOS/UltraVISTA survey, which can be convertedto CO line strengths. For a mock field of the Tomographic Ionized-carbonMapping Experiment (TIME), we find that masking out the "voxels"(spectral-spatial elements) containing foreground galaxies identified using anoptimized CO flux threshold results in a $z$-dependent criterion $m^{\rmAB}_{\rm K} \lesssim 22$ (or $M_{*} \gtrsim 10^{9} \,\rm M_{\rm \odot}$) at $z< 1$ and makes a [CII]/CO$_{\rm tot}$ power ratio of $\gtrsim 10$ at $k=0.1$$h$/Mpc achievable, at the cost of a moderate $\lesssim 8\%$ loss of totalsurvey volume.

A Foreground Masking Strategy for [CII] Intensity Mapping Experiments Using Galaxies Selected by Stellar Mass and Redshift