161 research outputs found
Tracing the cosmological evolution of stars and cold gas with CMB spectral surveys
A full account of galaxy evolution in the context of LCDM cosmology requires
measurements of the average star-formation rate (SFR) and cold gas abundance
across cosmic time. Emission from the CO ladder traces cold gas, and [CII] fine
structure emission at 158 um traces the SFR. Intensity mapping surveys the
cumulative surface brightness of emitting lines as a function of redshift,
rather than individual galaxies. CMB spectral distortion instruments are
sensitive to both the mean and anisotropy of the intensity of redshifted CO and
[CII] emission. Large-scale anisotropy is proportional to the product of the
mean surface brightness and the line luminosity-weighted bias. The bias
provides a connection between galaxy evolution and its cosmological context,
and is a unique asset of intensity mapping. Cross-correlation with galaxy
redshift surveys allows unambiguous measurements of redshifted line brightness
despite residual continuum contamination and interlopers. Measurement of line
brightness through cross-correlation also evades cosmic variance and suggests
new observation strategies. Galactic foreground emission is times
larger than the expected signals, and this places stringent requirements on
instrument calibration and stability. Under a range of assumptions, a linear
combination of bands cleans continuum contamination sufficiently that residuals
produce a modest penalty over the instrumental noise. For PIXIE, the
sensitivity to CO and [CII] emission scales from kJy/sr
at low redshift to ~2 kJy/sr by reionization.Comment: 11 pages, 9 figures, accepted in Ap
Ionizing radiation from hydrogen recombination strongly suppresses the lithium scattering signature in the CMB
It has been suggested that secondary CMB anisotropies generated by neutral lithium could open a new observational window into the universe around the redshift z~400, and permit a determination of the primordial lithium abundance. The effect is due to resonant scattering in the allowed Li i doublet (2s2S1/2-2p2P1/2,3/2), so its observability depends on the formation history of neutral lithium. Here we show that the ultraviolet photons produced during hydrogen recombination are sufficient to keep lithium in the Li ii ionization stage in the relevant redshift range and suppress the neutral fraction by ~3 orders of magnitude from previous calculations, making the lithium signature unobservable
Evidence for C II Diffuse Line Emission at Redshift z2.6
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(CII)=6.6(sup +5.0, sub 4.810(exp 4) Jy/sr at 95per 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 353857 GHz Planck bands. This excess is consistent with redshifted C II emission, in which case we report b(CII)I(CII)=2.0(sup +1.2, sub 1.110(exp 5) Jy/sr at 95 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
Erasing the Variable: Empirical Foreground Discovery for Global 21 cm Spectrum Experiments
Spectral measurements of the 21 cm monopole background have the promise of revealing the bulk energetic properties and ionization state of our universe from z approx. 6 30. Synchrotron foregrounds are orders of magnitude larger than the cosmological signal, and are the principal challenge faced by these experiments. While synchrotron radiation is thought to be spectrally smooth and described by relatively few degrees of freedom, the instrumental response to bright foregrounds may be much more complex. To deal with such complexities, we develop an approach that discovers contaminated spectral modes using spatial fluctuations of the measured data. This approach exploits the fact that foregrounds vary across the sky while the signal does not. The discovered modes are projected out of each line-of-sight of a data cube. An angular weighting then optimizes the cosmological signal amplitude estimate by giving preference to lower-noise regions. Using this method, we show that it is essential for the passband to be stable to at least approx. 10(exp 4). In contrast, the constraints on the spectral smoothness of the absolute calibration are mainly aesthetic if one is able to take advantage of spatial information. To the extent it is understood, controlling polarization to intensity leakage at the approx. 10(exp 2) level will also be essential to rejecting Faraday rotation of the polarized synchrotron emission. Subject headings: dark ages, reionization, first stars - methods: data analysis - methods: statistica
Primordial helium recombination III: Thomson scattering, isotope shifts, and cumulative results
Upcoming precision measurements of the temperature anisotropy of the cosmic
microwave background (CMB) at high multipoles will need to be complemented by a
more complete understanding of recombination, which determines the damping of
anisotropies on these scales. This is the third in a series of papers
describing an accurate theory of HeI and HeII recombination. Here we describe
the effect of Thomson scattering, the He isotope shift, the contribution of
rare decays, collisional processes, and peculiar motion. These effects are
found to be negligible: Thomson and He scattering modify the free electron
fraction at the level of several . The uncertainty in the
rate is significant, and for conservative estimates gives
uncertainties in of order . We describe several convergence
tests for the atomic level code and its inputs, derive an overall
error budget, and relate shifts in to the changes in , which
are at the level of 0.5% at . Finally, we summarize the main
corrections developed thus far. The remaining uncertainty from known effects is
in .Comment: 19 pages, 15 figures, to be submitted to PR
Intensity mapping from the sky: synergizing the joint potential of [OIII] and [CII] surveys at reionization
We forecast the ability of future-generation experiments to detect the
fine-structure lines of the carbon and oxygen ions, [CII] and [OIII] in
intensity mapping (IM) from the Epoch of Reionization (). Combining
the latest empirically derived constraints relating the luminosity of the
[OIII] line to the ambient star-formation rate, and using them in conjunction
with previously derived estimates for the abundance of [CII] in haloes, we
predict the expected auto-correlation IM signal to be observed using new
experiments based on the Fred Young Submillimetre Telescope (FYST) and the
balloon-borne facility, Experiment for Cryogenic Large-Aperture Intensity
Mapping (EXCLAIM) over . We describe how improvements to both
the ground-based and balloon-based surveys in the future will enable a
cross-correlation signal to be detected at 10-30 over . Finally, we propose a space-based mission targeting the [OIII] 88 and
52 m lines along with the [CII] 158 m line, configured to enhance the
signal-to-noise ratio of cross-correlation measurements. We find that such a
configuration can achieve a high-significance detection (hundreds of )
in both auto- and cross-correlation modes.Comment: 11 pages, 7 figures, 2 tables; accepted for publication in MNRA
The Nonlinear Cosmological Matter Power Spectrum with Massive Neutrinos I: The Halo Model
Measurements of the linear power spectrum of galaxies have placed tight
constraints on neutrino masses. We extend the framework of the halo model of
cosmological nonlinear matter clustering to include the effect of massive
neutrino infall into cold dark matter (CDM) halos. The magnitude of the effect
of neutrino clustering for three degenerate mass neutrinos with m_nu=0.9 eV is
of order ~1%, within the potential sensitivity of upcoming weak lensing
surveys. In order to use these measurements to further constrain--or eventually
detect--neutrino masses, accurate theoretical predictions of the nonlinear
power spectrum in the presence of massive neutrinos will be needed, likely only
possible through high-resolution multiple particle (neutrino, CDM and baryon)
simulations.Comment: v2: matches PRD versio
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