Evidence for C ii diffuse line emission at redshift z ∼ 2.6
Abstract
ABSTRACT C ii is one of the brightest emission lines from star-forming galaxies and is an excellent tracer for star formation. Recent work measured the C ii emission line amplitude for redshifts 2 < z < 3.2 by cross-correlating Planck High Frequency Instrument emission maps with tracers of overdensity from the Baryon Oscillation Spectroscopic Sky Survey, finding $${I}_{{\text C}\,\rm {\small II}}=6.6^{+5.0}_{-4.8}\times {10}^{4}$$ Jy sr−1 at $$95\,{\text{per cent}}$$ confidence level. In this paper, we present a refinement of this earlier work by improving the mask weighting in each of the Planck bands and the precision in the covariance matrix. We report a detection of excess emission in the 545 GHz Planck band separate from the cosmic infrared background (CIB) present in the 353–857 GHz Planck bands. This excess is consistent with redshifted C ii emission, in which case we report $$b_{{\text C} \,\rm {\small II}}I_{{\text C} \,\rm {\small II}} =2.0^{+1.2}_{-1.1}\times 10^5$$ Jy sr−1 at $$95\ {\text {per cent}}$$ confidence level, which strongly favours many collisional excitation models of C ii emission. Our detection shows strong evidence for a model with a non-zero C ii parameter, though line intensity mapping observations at high spectral resolution will be needed to confirm this result.
- Authors:
- Publication Date:
- Sponsoring Org.:
- USDOE
- OSTI Identifier:
- 1560910
- Resource Type:
- Published Article
- Journal Name:
- Monthly Notices of the Royal Astronomical Society: Letters
- Additional Journal Information:
- Journal Name: Monthly Notices of the Royal Astronomical Society: Letters Journal Volume: 489 Journal Issue: 1; Journal ID: ISSN 1745-3925
- Publisher:
- Oxford University Press
- Country of Publication:
- United Kingdom
- Language:
- English
Citation Formats
Yang, Shengqi, Pullen, Anthony R., and Switzer, Eric R. Evidence for C ii diffuse line emission at redshift z ∼ 2.6. United Kingdom: N. p., 2019.
Web. doi:10.1093/mnrasl/slz126.
Yang, Shengqi, Pullen, Anthony R., & Switzer, Eric R. Evidence for C ii diffuse line emission at redshift z ∼ 2.6. United Kingdom. https://doi.org/10.1093/mnrasl/slz126
Yang, Shengqi, Pullen, Anthony R., and Switzer, Eric R. Mon .
"Evidence for C ii diffuse line emission at redshift z ∼ 2.6". United Kingdom. https://doi.org/10.1093/mnrasl/slz126.
@article{osti_1560910,
title = {Evidence for C ii diffuse line emission at redshift z ∼ 2.6},
author = {Yang, Shengqi and Pullen, Anthony R. and Switzer, Eric R.},
abstractNote = {ABSTRACT C ii is one of the brightest emission lines from star-forming galaxies and is an excellent tracer for star formation. Recent work measured the C ii emission line amplitude for redshifts 2 < z < 3.2 by cross-correlating Planck High Frequency Instrument emission maps with tracers of overdensity from the Baryon Oscillation Spectroscopic Sky Survey, finding ${I}_{{\text C}\,\rm {\small II}}=6.6^{+5.0}_{-4.8}\times {10}^{4}$ Jy sr−1 at $95\,{\text{per cent}}$ confidence level. In this paper, we present a refinement of this earlier work by improving the mask weighting in each of the Planck bands and the precision in the covariance matrix. We report a detection of excess emission in the 545 GHz Planck band separate from the cosmic infrared background (CIB) present in the 353–857 GHz Planck bands. This excess is consistent with redshifted C ii emission, in which case we report $b_{{\text C} \,\rm {\small II}}I_{{\text C} \,\rm {\small II}} =2.0^{+1.2}_{-1.1}\times 10^5$ Jy sr−1 at $95\ {\text {per cent}}$ confidence level, which strongly favours many collisional excitation models of C ii emission. Our detection shows strong evidence for a model with a non-zero C ii parameter, though line intensity mapping observations at high spectral resolution will be needed to confirm this result.},
doi = {10.1093/mnrasl/slz126},
journal = {Monthly Notices of the Royal Astronomical Society: Letters},
number = 1,
volume = 489,
place = {United Kingdom},
year = {Mon Aug 12 00:00:00 EDT 2019},
month = {Mon Aug 12 00:00:00 EDT 2019}
}
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