{"work":{"id":"fd3ef6e2-8ead-4833-826f-482473d418ed","openalex_id":null,"doi":null,"arxiv_id":"2407.18292","raw_key":null,"title":"On the implications of the `cosmic calibration tension' beyond $H_0$ and the synergy between early- and late-time new physics","authors":null,"authors_text":"V","year":2024,"venue":"astro-ph.CO","abstract":"The `cosmic calibration tension' is a $> 5\\sigma$ discrepancy between the cosmological distance ladder built from baryonic acoustic oscillations (BAO) calibrated by the Planck/$\\Lambda$CDM sound horizon ($r_s$) and Type Ia supernovae (SN1a) calibrated instead with the S$H_0$ES absolute magnitude, assuming the distance-duality relationship (DDR) holds. In this work, we emphasize the consequences of this tension beyond the value of the Hubble constant $H_0$, and the implications for physics beyond $\\Lambda$CDM. Of utmost importance, it implies a larger physical matter density $\\omega_m\\equiv \\Omega_m h^2$, as both the fractional matter density $\\Omega_m$ and $h\\equiv H_0/100$ km/s/Mpc are well constrained from late-time data. New physics in the pre-recombination era must thus be able to decrease $r_s$ while either reducing the value of $\\Omega_m$, or increasing the value of $\\omega_m$. Assuming a $\\Lambda$CDM-like primordial power spectrum, this necessarily results in an increase in the clustering amplitude $\\sigma_8$. Deviations from $\\Lambda$CDM in the late-time expansion history cannot resolve the calibrator tension but can help relax the required shifts to the matter density and $\\sigma_8$: it is in that sense that a combination of early and late-time new physics may help alleviate the tension. More precisely, models that modify the pre-recombination expansion history can accommodate the increase in $\\omega_m$ without the need for additional modifications. It is those models which only affect recombination that require additional deviations at late-times to be successful. Hence, the `cosmic calibration tension' points either to a targeted modification of the pre-recombination expansion history, or to a broader change affecting multiple cosmic epochs.","external_url":"https://arxiv.org/abs/2407.18292","cited_by_count":null,"metadata_source":"pith","metadata_fetched_at":"2026-07-10T03:56:44.471636+00:00","pith_arxiv_id":"2407.18292","created_at":"2026-05-09T06:10:36.671564+00:00","updated_at":"2026-07-10T03:56:44.471636+00:00","title_quality_ok":true,"display_title":"Poulin, T","render_title":"Poulin, T"},"hub":{"state":{"work_id":"fd3ef6e2-8ead-4833-826f-482473d418ed","tier":"hub","tier_reason":"10+ Pith inbound or 1,000+ external citations","pith_inbound_count":18,"external_cited_by_count":null,"distinct_field_count":1,"first_pith_cited_at":"2025-03-18T21:14:17+00:00","last_pith_cited_at":"2026-07-09T16:24:29+00:00","author_build_status":"not_needed","summary_status":"needed","contexts_status":"needed","graph_status":"needed","ask_index_status":"not_needed","reader_status":"not_needed","recognition_status":"not_needed","updated_at":"2026-08-20T12:10:11.541898+00:00","tier_text":"hub"},"tier":"hub","role_counts":[{"context_role":"background","n":9},{"context_role":"method","n":3},{"context_role":"dataset","n":1}],"polarity_counts":[{"context_polarity":"background","n":9},{"context_polarity":"use_method","n":3},{"context_polarity":"use_dataset","n":1}],"runs":{},"summary":{},"graph":{},"authors":[]}}