{"paper":{"title":"When galaxies burst: enhanced shot-noise for line-intensity mapping in the JWST era","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"JWST-observed bursty star formation multiplies LIM shot-noise power by a line-dependent factor of up to 7.","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Eleonora Vanzan, Ely D. Kovetz, Hovav Lazare, Julian B. Mu\\~noz, Sarah Libanore","submitted_at":"2026-05-13T18:00:04Z","abstract_excerpt":"Recent JWST observations indicate that star formation at $z\\!\\sim\\!4-6$ is more stochastic than previously assumed, with rms log-SFR scatter $\\sim\\!0.6$ dex at $M_h\\!\\sim\\!10^{11}M_{\\odot}$, growing toward smaller halos and time-correlated on $\\sim\\!25$ Myr. This is significantly higher than the typical $\\sim\\!0.3$ dex phenomenological lognormal scatter assumed in standard line-intensity mapping (LIM) forecasts. We propagate the JWST-era burstiness through to the LIM shot-noise power spectrum and show that the result is a simple multiplicative correction: the deterministic shot noise multiplie"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"We propagate the JWST-era burstiness through to the LIM shot-noise power spectrum and show that the result is a simple multiplicative correction: the deterministic shot noise multiplied by a line-dependent boost factor B_λ derived in closed form by convolving the SFR correlation function with the stellar-population-synthesis kernel of each line.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"The JWST-measured rms log-SFR scatter of ~0.6 dex and its ~25 Myr time correlation at z~4-6 for M_h~10^11 M_sun can be directly inserted into the SFR correlation function and convolved with SPS kernels to obtain the boost factor at z~6 without additional astrophysical corrections or selection effects.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Bursty high-redshift star formation boosts LIM shot-noise by line-dependent factors B_λ of 2.5-7 at z~6 via convolution of SFR correlations with SPS kernels, improving auto-spectrum detectability while degrading clustering measurements.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"JWST-observed bursty star formation multiplies LIM shot-noise power by a line-dependent factor of up to 7.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"832513051a0225669fe2f985b9274883fce6c466dd58935e6ca70ee0ac0cdf24"},"source":{"id":"2605.13967","kind":"arxiv","version":1},"verdict":{"id":"b1063026-10f8-4683-9239-cdc99f4e5f23","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-15T02:25:43.606671Z","strongest_claim":"We propagate the JWST-era burstiness through to the LIM shot-noise power spectrum and show that the result is a simple multiplicative correction: the deterministic shot noise multiplied by a line-dependent boost factor B_λ derived in closed form by convolving the SFR correlation function with the stellar-population-synthesis kernel of each line.","one_line_summary":"Bursty high-redshift star formation boosts LIM shot-noise by line-dependent factors B_λ of 2.5-7 at z~6 via convolution of SFR correlations with SPS kernels, improving auto-spectrum detectability while degrading clustering measurements.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"The JWST-measured rms log-SFR scatter of ~0.6 dex and its ~25 Myr time correlation at z~4-6 for M_h~10^11 M_sun can be directly inserted into the SFR correlation function and convolved with SPS kernels to obtain the boost factor at z~6 without additional astrophysical corrections or selection effects.","pith_extraction_headline":"JWST-observed bursty star formation multiplies LIM shot-noise power by a line-dependent factor of up to 7."},"references":{"count":63,"sample":[{"doi":"","year":2023,"title":"The brightest galaxies at cosmic dawn","work_id":"a32616da-514f-4f39-9424-ff5fa271f9f9","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2023,"title":"A Comprehensive Study of Galaxies at z∼9−16 Found in the Early JWST Data: Ultraviolet Lu- minosity Functions and Cosmic Star Formation History at the Pre-reionization Epoch","work_id":"c091d2da-8a22-44b5-b3bb-90b231fa5664","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2024,"title":"The Complete CEERS Early Uni- verse Galaxy Sample","work_id":"6b3e78d7-ecc9-4259-8a85-33708b56ee1d","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2024,"title":"JWST PRIMER: a new multifield determination of the evolving galaxy UV luminosity func- tion at redshiftsz≃9−15","work_id":"6629a17c-882c-4fe3-8294-382f93542137","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2024,"title":"Earliest Galaxies in the JADES Origins Field: Luminosity Function and Cosmic Star For- mation Rate Density 300 Myr after the Big Bang","work_id":"8b0f8477-d3e8-4e21-9b90-f0dbbea3ec02","ref_index":5,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":63,"snapshot_sha256":"e2f677f28680b2417b711ba26802a50ce6fc7d17edcbd530f549473e962fb4fe","internal_anchors":4},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}