<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mn>5</mml:mn> <mml:mi>σ</mml:mi> </mml:mrow> </mml:math> tension between <i>Planck</i> cosmic microwave background and eBOSS Lyman-alpha forest and constraints on physics beyond <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mi mathvariant="normal">Λ</mml:mi> <mml:mtext>CDM</mml:mtext> </mml:mrow> </mml:math>

Abstract

We find that combined cosmic microwave background, baryon acoustic oscillations, and supernovae data analyzed under <a:math xmlns:a="http://www.w3.org/1998/Math/MathML"> <a:mi mathvariant="normal">Λ</a:mi> </a:math> cold dark matter ( <c:math xmlns:c="http://www.w3.org/1998/Math/MathML"> <c:mrow> <c:mi mathvariant="normal">Λ</c:mi> <c:mi>CDM</c:mi> </c:mrow> </c:math> ) are in <e:math xmlns:e="http://www.w3.org/1998/Math/MathML"> <e:mrow> <e:mn>4.9</e:mn> <e:mi>σ</e:mi> </e:mrow> </e:math> tension with the extended Baryon Oscillation Spectroscopic Survey (eBOSS) <f:math xmlns:f="http://www.w3.org/1998/Math/MathML"> <f:mrow> <f:mi>Ly</f:mi> <f:mi>α</f:mi> </f:mrow> </f:math> forest in inference of the linear matter power spectrum at wave number <g:math xmlns:g="http://www.w3.org/1998/Math/MathML"> <g:mrow> <g:mo>∼</g:mo> <g:mn>1</g:mn> <g:mi>h</g:mi> <g:mspace width="0.16em"/> <g:msup> <g:mi>Mpc</g:mi> <g:mrow> <g:mo>−</g:mo> <g:mn>1</g:mn> </g:mrow> </g:msup> </g:mrow> </g:math> and redshift = 3. Model extensions can alleviate this tension: running in the tilt of the primordial power spectrum ( <i:math xmlns:i="http://www.w3.org/1998/Math/MathML"> <i:mrow> <i:msub> <i:mi>α</i:mi> <i:mi mathvariant="normal">s</i:mi> </i:msub> <i:mo>∼</i:mo> <i:mo>−</i:mo> <i:mn>0.01</i:mn> </i:mrow> </i:math> ); a fraction <k:math xmlns:k="http://www.w3.org/1998/Math/MathML"> <k:mrow> <k:mo>∼</k:mo> <k:mo>(</k:mo> <k:mn>1</k:mn> <k:mo>−</k:mo> <k:mn>5</k:mn> <k:mo>)</k:mo> <k:mo>%</k:mo> </k:mrow> </k:math> of ultralight axion dark matter (DM) with particle mass <l:math xmlns:l="http://www.w3.org/1998/Math/MathML"> <l:mrow> <l:mo>∼</l:mo> <l:msup> <l:mn>10</l:mn> <l:mrow> <l:mo>−</l:mo> <l:mn>25</l:mn> </l:mrow> </l:msup> </l:mrow> </l:math> eV or warm DM with mass <m:math xmlns:m="http://www.w3.org/1998/Math/MathML"> <m:mrow> <m:mo>∼</m:mo> <m:mn>10</m:mn> </m:mrow> </m:math> eV. The new Dark Energy Spectroscopic Instrument survey, coupled with high-accuracy modeling, will help distinguish the source of this discrepancy.

Topics & Concepts