1,276 research outputs found
COBE Constraints on a Local group X-ray Halo
We investigate the effect of a putative X-ray emitting halo surrounding the
Local Group of galaxies, and specifically the possible temperature anisotropies
induced in the COBE-DMR four-year sky maps by an associated Sunyaev-Zel'dovich
effect. By fitting the isothermal spherical halo model proposed by Suto et.al.
(1996) to the coadded four-year COBE-DMR 53 and 90 GHz sky maps in Galactic
coordinates, we find no significant evidence of a contribution. We therefore
reject the claim that such a halo can affect the estimation of the primordial
spectral index and amplitude of density perturbations as inferred from the DMR
data. We find that correlation with the DMR data imposes constraints on the
plausible contribution of such an X-ray emitting halo to a distortion in the
CMB spectrum (as specified by the Compton-y parameter), up to a value for R --
the ratio of the core radius of the isothermal halo gas distribution to the
distance to the Local Group centroid -- of 0.68. For larger values of R, the
recent cosmological upper limit derived by COBE-FIRAS provides stronger
constraints on the model parameters. Over the entire parameter space for R, we
find an upper limit to the inferred sky-RMS anisotropy signal of 14 microKelvin
(95% c.l.), a negligible amount relative to the 35 microKelvin signal observed
in the COBE-DMR data.Comment: 4 pages, 3 figures; accepted for publication in MNRAS pink page
Lyman-alpha forest-CMB cross-correlation and the search for the ionized baryons at high redshift
The intergalactic neutral hydrogen which is responsible for the Lyman alpha
forest of quasar absorption is a tracer of much larger amounts of ionised
hydrogen. The ionised component has yet to be detected directly, but is
expected to scatter CMB photons via the Sunyaev-Zel'dovich (SZ) effect. We use
hydrodynamic simulations of a LambdaCDM universe to create mock quasar spectra
and CMB sky maps. We find that the high-z Lya forest gas causes temperature
fluctuations of the order of 1 muK rms in the CMB on arcmin scales. The kinetic
and thermal SZ effects have a similar magnitude at z=3, with the thermal effect
becoming relatively weaker as expected at higher z. The CMB signal associated
with lines of sight having HI column densities > 10^18 cm^-2 is only marginally
stronger than that for lower column densities. The strong dependence of rms
temperature fluctuation on mean Lya absorbed flux, however, suggests that the
CMB signal effectively arises in lower density material. We investigate the use
of the cross-correlation of the Lya forest and the microwave background to
detect the SZ effect at redshifts 2-4. In so doing we are able to set direct
limits on the density of diffuse ionised intergalactic baryons. We carry out a
preliminary comparison at a mean redshift z=3 of 3488 quasar spectra from SDSS
Data Release 3 and the WMAP first year data. Assuming that the baryons are
clustered as in a LambdaCDM cosmology, and have the same mean temperature, the
cross-correlation yields a weak limit on the cosmic density of ionised baryons
Omega_(b,I), which is Omega_(b,I) < 0.8 at 95% confidence. With data from
upcoming CMB telescopes, we anticipate that a direct detection of the high
redshift ionised IGM will soon be possible, providing an important consistency
check on cosmological models.Comment: 14 pages, 10 figures, submitted to MNRA
On the Non-Gaussianity Observed in the COBE-DMR Sky Maps
In this paper we pursue the origin of the non-Gaussianity determined by a
bispectrum analysis of the COBE-DMR 4-year sky maps. The robustness of the
statistic is demonstrated by the rebinning of the data into 12 coordinate
systems. By computing the bispectrum statistic as a function of various data
partitions - by channel, frequency, and time interval, we show that the
observed non-Gaussian signal is driven by the 53 GHz data. This frequency
dependence strongly rejects the hypothesis that the signal is cosmological in
origin. A jack-knife analysis of the coadded 53 and 90 GHz sky maps reveals
those sky pixels to which the bispectrum statistic is particularly sensitive.
We find that by removing data from the 53 GHz sky maps for periods of time
during which a known systematic effect perturbs the 31 GHz channels, the
amplitudes of the bispectrum coefficients become completely consistent with
that expected for a Gaussian sky. We conclude that the non-Gaussian signal
detected by the normalised bispectrum statistic in the publicly available DMR
sky maps is due to a systematic artifact. The impact of removing the affected
data on estimates of the normalisation of simple models of cosmological
anisotropy is negligible.Comment: 14 pages, plus 8 Postscript and 3 GIF figures. LaTeX2e document using
AASTeX v5.0 macros. Revised version accepted for publication in the
Astrophysical Journal: small changes to the text, minor modifications to
figures 1 and
Testing physical models for dipolar asymmetry with CMB polarization
The cosmic microwave background (CMB) temperature anisotropies exhibit a
large-scale dipolar power asymmetry. To determine whether this is due to a
real, physical modulation or is simply a large statistical fluctuation requires
the measurement of new modes. Here we forecast how well CMB polarization data
from \Planck\ and future experiments will be able to confirm or constrain
physical models for modulation. Fitting several such models to the \Planck\
temperature data allows us to provide predictions for polarization asymmetry.
While for some models and parameters \Planck\ polarization will decrease error
bars on the modulation amplitude by only a small percentage, we show,
importantly, that cosmic-variance-limited (and in some cases even \Planck)
polarization data can decrease the errors by considerably better than the
expectation of based on simple -space arguments. We project
that if the primordial fluctuations are truly modulated (with parameters as
indicated by \Planck\ temperature data) then \Planck\ will be able to make a
2 detection of the modulation model with 20--75\% probability,
increasing to 45--99\% when cosmic-variance-limited polarization is considered.
We stress that these results are quite model dependent. Cosmic variance in
temperature is important: combining statistically isotropic polarization with
temperature data will spuriously increase the significance of the temperature
signal with 30\% probability for \Planck.Comment: 18 pages, 11 figures, 2 tables. Version updated to match PRD versio
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