Deconstructing the Planck TT Power Spectrum to Constrain Deviations from $Lambda$CDM. (arXiv:2008.01785v2 [astro-ph.CO] UPDATED)

<a href="http://arxiv.org/find/astro-ph/1/au:+Kable_J/0/1/0/all/0/1">Joshua A. Kable</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Addison_G/0/1/0/all/0/1">Graeme E. Addison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bennett_C/0/1/0/all/0/1">Charles L. Bennett</a>

Consistency checks of $Lambda$CDM predictions with current cosmological data

sets may illuminate the types of changes needed to resolve cosmological

tensions. To this end, we modify the CLASS Boltzmann code to create

phenomenological amplitudes, similar to the lensing amplitude parameter $A_L$,

for the Sachs-Wolfe, Doppler, early Integrated Sachs-Wolfe (eISW), and

Polarization contributions to the CMB temperature anisotropy, and then we

include these additional amplitudes in fits to the Planck TT power spectrum. We

find that allowing one of these amplitudes to vary at a time results in little

improvement over $Lambda$CDM alone suggesting that each of these physical

effects are being correctly accounted for given the current level of precision.

Further, we find that the only pair of phenomenological amplitudes that results

in a significant improvement to the fit to Planck temperature data results from

varying the amplitudes of the Sachs-Wolfe and Doppler effects simultaneously.

However, we show that this model is really just refinding the $Lambda$CDM +

$A_L$ solution. We test adding our phenomenological amplitudes as well as

$N_{textrm{eff}}$, $Y_{textrm{He}}$, and $n_{textrm{run}}$ to $Lambda$CDM +

$A_L$ and find that none of these model extensions provide significant

improvement over $Lambda$CDM + $A_L$ when fitting Planck temperature data.

Finally, we quantify the contributions of both the eISW effect and lensing on

the constraint of the physical matter density from Planck temperature data by

allowing the phenomenological amplitude from each effect to vary. We find that

these effects play a relatively small role (the uncertainty increases by

$3.5%$ and $16%$ respectively) suggesting that the overall photon envelope

has the greatest constraining power.

Consistency checks of $Lambda$CDM predictions with current cosmological data

sets may illuminate the types of changes needed to resolve cosmological

tensions. To this end, we modify the CLASS Boltzmann code to create

phenomenological amplitudes, similar to the lensing amplitude parameter $A_L$,

for the Sachs-Wolfe, Doppler, early Integrated Sachs-Wolfe (eISW), and

Polarization contributions to the CMB temperature anisotropy, and then we

include these additional amplitudes in fits to the Planck TT power spectrum. We

find that allowing one of these amplitudes to vary at a time results in little

improvement over $Lambda$CDM alone suggesting that each of these physical

effects are being correctly accounted for given the current level of precision.

Further, we find that the only pair of phenomenological amplitudes that results

in a significant improvement to the fit to Planck temperature data results from

varying the amplitudes of the Sachs-Wolfe and Doppler effects simultaneously.

However, we show that this model is really just refinding the $Lambda$CDM +

$A_L$ solution. We test adding our phenomenological amplitudes as well as

$N_{textrm{eff}}$, $Y_{textrm{He}}$, and $n_{textrm{run}}$ to $Lambda$CDM +

$A_L$ and find that none of these model extensions provide significant

improvement over $Lambda$CDM + $A_L$ when fitting Planck temperature data.

Finally, we quantify the contributions of both the eISW effect and lensing on

the constraint of the physical matter density from Planck temperature data by

allowing the phenomenological amplitude from each effect to vary. We find that

these effects play a relatively small role (the uncertainty increases by

$3.5%$ and $16%$ respectively) suggesting that the overall photon envelope

has the greatest constraining power.

http://arxiv.org/icons/sfx.gif