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Journal Article

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

MPS-Authors

Sun,  G.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Moncelsi,  L.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Viero,  M. P.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Silva,  M. B.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Bock,  J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Bradford,  C. M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Chang,  T. -C.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Cheng,  Y. -T.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Cooray,  A. R.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Crites,  A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Hailey-Dunsheath,  S.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Uzgil,  B.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Hunacek,  J. R.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Zemcov,  M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

External Resource

https://ui.adsabs.harvard.edu/abs/2018ApJ...856..107S
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Citation

Sun, G., Moncelsi, L., Viero, M. P., Silva, M. B., Bock, J., Bradford, C. M., et al. (2018). A Foreground Masking Strategy for [C II] Intensity Mapping Experiments Using Galaxies Selected by Stellar Mass and Redshift. The Astrophysical Journal, 856.


Cite as: https://hdl.handle.net/21.11116/0000-0005-CADC-0
Abstract
Intensity mapping provides a unique means to probe the epoch of reionization (EoR), when the neutral intergalactic medium was ionized by energetic photons emitted from the first galaxies. The [C II] 158 μm fine-structure line is typically one of the brightest emission lines of star-forming galaxies and thus a promising tracer of the global EoR star formation activity. However, [C II] intensity maps at 6 ≲ z ≲ 8 are contaminated by interloping CO rotational line emission (3 ≤ J upp ≤ 6) from lower-redshift galaxies. Here we present a strategy to remove the foreground contamination in upcoming [C II] intensity mapping experiments, guided by a model of CO emission from foreground galaxies. The model is based on empirical measurements of the mean and scatter of the total infrared luminosities of galaxies at z < 3 and with stellar masses {M}* > {10}8 {M}☉ selected in the K-band from the COSMOS/UltraVISTA survey, which can be converted to CO line strengths. For a mock field of the Tomographic Ionized-carbon Mapping Experiment, we find that masking out the “voxels” (spectral-spatial elements) containing foreground galaxies identified using an optimized CO flux threshold results in a z-dependent criterion {m}{{K}}AB}≲ 22 (or {M}* ≳ {10}9 {M}☉ ) at z < 1 and makes a [C II]/COtot power ratio of ≳10 at k = 0.1 h/Mpc achievable, at the cost of a moderate ≲8% loss of total survey volume.