Depth of maximum of air-shower profiles above <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:msup> <mml:mn>10</mml:mn> <mml:mn>17.7</mml:mn> </mml:msup> <mml:mtext> </mml:mtext> <mml:mtext> </mml:mtext> <mml:mi>eV</mml:mi> </mml:math> measured with the fluorescence detector of the Pierre Auger Observatory

We present measurements of the depth of shower maximum, <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"> <a:msub> <a:mi>X</a:mi> <a:mi>max</a:mi> </a:msub> </a:math> , for cosmic-ray-induced extensive air showers recorded by the fluorescence detector of the Pierre Auger Observatory over 17 years. The dataset covers primary energies from <c:math xmlns:c="http://www.w3.org/1998/Math/MathML" display="inline"> <c:msup> <c:mn>10</c:mn> <c:mn>17.7</c:mn> </c:msup> <c:mtext> </c:mtext> <c:mtext> </c:mtext> <c:mi>eV</c:mi> </c:math> to beyond <e:math xmlns:e="http://www.w3.org/1998/Math/MathML" display="inline"> <e:msup> <e:mn>10</e:mn> <e:mn>19.6</e:mn> </e:msup> <e:mtext> </e:mtext> <e:mtext> </e:mtext> <e:mi>eV</e:mi> </e:math> . With improved event reconstruction and an exposure 2.4 times larger than in our previous analysis, this work confirms and refines our conclusions on the mass composition at ultrahigh energies. The energy evolution of the mean <g:math xmlns:g="http://www.w3.org/1998/Math/MathML" display="inline"> <g:msub> <g:mi>X</g:mi> <g:mi>max</g:mi> </g:msub> </g:math> exhibits a pronounced break at a cosmic-ray energy of about <i:math xmlns:i="http://www.w3.org/1998/Math/MathML" display="inline"> <i:msup> <i:mn>10</i:mn> <i:mn>18.4</i:mn> </i:msup> <i:mtext> </i:mtext> <i:mtext> </i:mtext> <i:mi>eV</i:mi> </i:math> , providing direct, model-independent evidence for a change in the evolution of the mass composition. Independently, the observed decrease of the <k:math xmlns:k="http://www.w3.org/1998/Math/MathML" display="inline"> <k:msub> <k:mi>X</k:mi> <k:mi>max</k:mi> </k:msub> </k:math> fluctuations with energy indicates a transition toward a heavier and less diverse primary mass composition. No statistically significant declination dependence of the <m:math xmlns:m="http://www.w3.org/1998/Math/MathML" display="inline"> <m:msub> <m:mi>X</m:mi> <m:mi>max</m:mi> </m:msub> </m:math> distributions is observed within the exposure of the Observatory, consistent with an isotropic mass composition at the sensitivity of this analysis. The mean and standard deviation of the <o:math xmlns:o="http://www.w3.org/1998/Math/MathML" display="inline"> <o:msub> <o:mi>X</o:mi> <o:mi>max</o:mi> </o:msub> </o:math> distributions, interpreted with air-shower simulations, yield the energy dependence of the average and variance of the logarithmic mass of cosmic rays arriving at Earth. Furthermore, energy-dependent fractional abundances of four representative primary-mass groups (p, He, CNO, Fe) are obtained by fitting the observed <q:math xmlns:q="http://www.w3.org/1998/Math/MathML" display="inline"> <q:msub> <q:mi>X</q:mi> <q:mi>max</q:mi> </q:msub> </q:math> distributions in each energy bin with a weighted sum of elemental templates. These results provide strong evidence against a long-standing assumption that ultrahigh-energy cosmic rays are predominantly protons: above <s:math xmlns:s="http://www.w3.org/1998/Math/MathML" display="inline"> <s:mo>∼</s:mo> <s:msup> <s:mn>10</s:mn> <s:mn>18.4</s:mn> </s:msup> <s:mtext> </s:mtext> <s:mtext> </s:mtext> <s:mi>eV</s:mi> </s:math> , the average cosmic-ray mass increases, accompanied by a steadily decreasing diversity in the elemental composition.

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