{"id":"09fe87f9-b3e7-450d-8147-6336fc163063","arxiv_id":"2412.12867","paper_version":1,"verdict":"UNVERDICTED","confidence":"MODERATE","novelty_score":1.0,"correctness_risk":"low","formal_verification":"none","parameter_count":0,"one_line_summary":"A project-status report for CRÉME: 386 eclipsing binaries observed, 325 with component masses, and TESS light curves for over 330 targets, with detailed analyses of about 100 systems in 35 publications.","lead":"This 6-page status report describes the CRÉME survey of 386 detached eclipsing binaries and reports that masses have been estimated for 325 double-lined systems, with TESS photometry collected for over 330 targets. A smart generalist should read it as a progress report on a large survey that aims to deliver high-precision stellar masses and radii, though this paper itself contains no new measurements.","discovery_kind":"review","skeptic_critique":{"model":"deepseek-v4-flash","headline":"The 325-mass headline relies on treating M sin^3(i) as true mass; §3.1 calls them 'absolute masses' while footnote 1 concedes they are lower limits, and no inclination distribution is shown.","rationale":"The paper is a proceedings status report, so its evidence lies in cited publications. The reader's UNVERDICTED verdict is appropriate because the central numbers cannot be checked in this document. The most concrete scientific vulnerability is the unstated inclination assumption behind the word 'masses': M sin^3(i) equals M only for i=90°, and the eclipse condition alone does not guarantee that for all 325 systems. This is not an attack on the survey; it is a precise identification of what must be true for the headline count to be taken as benchmark masses. The proposed TESS light-curve test would settle it. If the test shows near-90° inclinations across the sample, the concern does not land. Until then, the paper remains unverdictable as a standalone result, matching the reader's verdict.","tokens_in":5275,"tokens_out":9569,"duration_ms":85154,"concrete_test":"Fit TESS 2-min light curves (329 targets; plus Kepler/K2 for the rest) to determine inclination i for all 325 mass systems. Compute sin^3(i) for each and the implied mass correction. If more than a few percent of systems have sin^3(i) < 0.98 (i < ~82°), the 'absolute mass' and <1% precision claims are unsupported; the catalogue should be presented as M sin^3(i) lower limits until inclinations are incorporated.","verdict_should_be":"UNCHANGED","load_bearing_attack":"Central claim: masses for 325 SB2 DEBs (§2.1, abstract). Masses come from RV fits alone, yielding M sin^3(i) (footnote 1). The assertion that sin^3(i) ≃ 1 for DEBs is not automatic: eclipse geometry requires only cos i < (R1+R2)/a. For long-period main-sequence pairs R/a is small and i > ~85°, but the full sample includes short-period and evolved systems where R/a can approach 0.3–0.5, allowing grazing eclipses at i ~ 60°–75° and sin^3 i ~ 0.65–0.90. Thus a non-negligible subset could have masses biased low by 10–35%. The 78 long-period systems used for the <1% precision claim may be safe, but the headline count is not restricted to them. §3.1 calls the products 'absolute masses', contradicting footnote 1. No inclination distribution or per-system light-curve results are given, so the fraction of systems where the bias exceeds the quoted precision is unknown.","agreement_with_reader":"agree"},"referee_report":{"model":"deepseek-v4-flash","summary":"This short conference proceedings paper reports the status of the CRÉME survey, a spectroscopic program targeting about 380 detached eclipsing binaries (DEBs), and its extension with TESS 2-minute-cadence photometry. The authors state that from more than 7000 high-resolution spectra they have obtained orbital solutions and component masses for 325 double-lined systems, with additional TESS data for 329 targets as of Sector 85. The paper also summarizes several sub-projects on low-mass stars, giants/sub-giants, pulsating components, and totally eclipsing systems, and quotes precision figures for a subset of 78 long-period systems.","tokens_in":5414,"tokens_out":4149,"duration_ms":38660,"significance":"If the survey result holds, CRÉME would provide one of the largest homogeneous samples of benchmark DEB masses, useful for testing stellar models in underpopulated parts of the H-R diagram. The TESS light-curve coverage for most targets adds valuable photometric information, and the reported sub-1% mass precision for the 78-system subset is promising. However, the paper is a status report without data tables, target lists, or a quantitative description of uncertainties, and the central mass claim rests on an approximation that the text itself concedes in a footnote. These issues should be fixed before the results can be used by the community.","major_comments":[{"comment":"","section":"§2.1 footnote 1 and §3.1 'Masses of 650 stars'"},{"comment":"","section":"§3.1 'Masses of 650 stars'"}],"minor_comments":[{"comment":"","section":"Title page"},{"comment":"","section":"Abstract and §2.2"},{"comment":"","section":"Abstract"},{"comment":"","section":"§2.1"}],"recommendation":"major_revision","confidential_remarks":"This is a conference proceedings contribution rather than a full research article. The main weakness is the treatment of M sin^3 i as absolute mass in the headline count, which the text itself contradicts between the footnote and §3.1. This is fixable by rewording the abstract and main text, and by adding a caveat about the sin^3 i approximation or providing a quantitative check. The lack of a target list and detailed uncertainties is of less concern for a status report, but should be addressed if this is intended as a citable data announcement. The self-citations are appropriate for a project status report."},"author_rebuttal":null,"desk_editor":{"model":"deepseek-v4-flash","letter":"Quick take: this is a conference-proceedings status report, not a research paper. The headline number—325 binary masses—is self-reported and not checkable from the text, and the paper contradicts itself about what those masses actually are. Still, as a program update it is honest, well-organized, and useful for anyone tracking the CRÉME survey.\n\nWhat it does well: it documents the scale of the spectroscopic and TESS campaigns (386 targets, 329 TESS light curves, 35 publications), lists the sub-projects, and shows in Figure 1 that the sample reaches H-R diagram regions DEBCat barely covers. That last point is a legitimate and useful observation. The authors are upfront that the detailed analyses live elsewhere.\n\nThe biggest problem is the mass claim. The §2.1 footnote says RV fits give M sin^3(i), treated as proxies because sin^3(i) ≈ 1 for DEBs. §3.1 then calls these \"absolute masses.\" That is a real internal contradiction. For long-period main-sequence pairs the inclination is probably near 90°, but the sample includes short-period and evolved systems where R/a can be large enough that grazing eclipses occur at i ≈ 60–75°, biasing sin^3(i) down by 10–35%. The paper gives no inclination distribution, so we cannot tell what fraction of the 325 are affected. The precision claim (<1% for 90% of a 78-system subset) may be right for that subset, but it does not license the headline count. Also, no target list, no mass table, no uncertainties are provided—so the 325 is just a statement of intent. Minor: the header date says 2020 while the text says November 2024; presumably a template artifact, but it should be fixed.\n\nWho it is for: people tracking the CRÉME program or looking for interesting DEB targets. General readers get no scientific result here. I would not cite this paper for any mass; I would cite the per-system papers. It is a pointer, not a data release.\n\nRecommendation: as a journal submission, I would desk-reject unless the authors add a machine-readable table of the 325 systems with masses, references, and a discussion of the inclination bias. As a proceedings note, it is fine with a light review. I would not send it to a rigorous referee as-is. If they fix the contradiction and link the data, it becomes a citable status record.","headline":"Status report for the CRÉME survey: useful program update, but the 325-mass headline is an unverifiable claim and internally inconsistent about M sin^3(i).","tokens_in":6003,"tokens_out":3333,"would_cite":false,"duration_ms":30971,"reading_group":"no","serious_thinker":"yes","would_accept_peer_review":false},"rs_alignment":null,"lean_confirmation":null,"pith_extraction":{"msc":[],"pacs":[],"model":"deepseek-v4-flash","headline":"The CRÉME survey has produced component masses for 325 double-lined detached eclipsing binaries, a homogeneous sample that will test stellar models in underpopulated parts of the H-R diagram.","keywords":["detached eclipsing binaries","double-lined spectroscopic binaries","stellar masses","radial velocities","TESS photometry","stellar evolution benchmarks","multiple star systems","pulsating stars in binaries"],"falsifier":"For a random subset of the 325 systems, fit the TESS light curves to recover the orbital inclination $i$; if more than a few percent come out with $\\sin^3(i) < 0.95$ (i below about 80 degrees), the survey's mass values are biased and must be corrected per system, and the claimed sub-1% precision would not hold for those objects.","tokens_in":5039,"feed_emoji":"🌟","tokens_out":6714,"duration_ms":59518,"temperature":0.7,"pith_summary":"This paper reports the current state of CRÉME, a long-running survey that collects high-resolution spectra of detached eclipsing binaries, pairs of stars that regularly pass in front of each other without touching. The central claim is that the survey has now gathered enough radial-velocity data to estimate component masses for 325 double-lined systems, meaning both stars' spectra are visible, totalling 650 individual stars. For a subsample of 78 long-period pairs, the reported mass uncertainty is below 1% in 90% of cases and below 0.5% in roughly 60%. The survey has also obtained TESS 2-minute-cadence photometry for 329 targets, so the same systems now have the light curves needed to derive radii, temperatures, and ages. If these numbers hold, CRÉME delivers one of the largest homogeneous sets of benchmark stellar masses, aimed at regions of the H-R diagram where precise data are scarce.","feed_headline":"Survey measures masses of 325 eclipsing binaries","feed_subtitle":"7,000 high-resolution spectra plus TESS light curves place benchmark stars in sparse H-R diagram regions.","key_machinery":"The load-bearing machinery is the double-lined detached eclipsing binary (SB2 DEB), a pair of stars whose mutual eclipses prove they are edge-on and whose spectra show both components, so that radial-velocity amplitudes from echelle spectroscopy give the orbit and hence the masses. The measured quantity is $M\\sin^3(i)$; the paper relies on the DEB geometry to set $\\sin^3(i)\\simeq 1$, turning a lower limit into a true mass. TESS 2-minute photometry supplies the light curves that fix radii and temperatures, and the combination of the two data streams yields the physical parameters that populate the survey's science cases, from low-mass dwarfs to pulsating stars and compact triples.","core_discovery":"The survey's core result is a homogeneous census: from more than 7000 spectra taken with 19 spectrographs, the CRÉME team has derived orbital parameters and component masses for 325 of the 386 detached eclipsing binaries in its sample, with the remaining systems set aside as single-lined, poorly sampled, or otherwise unqualified. Masses are published as $M\\sin^3(i)$, which the paper equates to true mass because detached eclipsing binaries are assumed to be seen nearly edge-on. On the photometric side, TESS 2-minute cadence data now exist for 329 targets, some observed across more than 13 sectors. The survey has already found 76 low-mass and 19 high-mass stars, 14 confirmed and 8 candidate pulsators, and 80 multiple systems including compact hierarchical triples and quadruples; about 100 binaries have been modelled so far, with 35 publications. The precision claim is that for 78 long-period systems selected for clean radial velocities, 90% of the component masses are accurate to better than 1%.","pith_inferences":["The $\\sin^3(i)\\simeq 1$ assumption could be checked directly with the TESS light-curve shapes; systems with grazing eclipses would show up as shallow or flat-bottomed minima, and their masses could be corrected or excluded.","If the homogeneous mass precision holds across the full sample, these 650 stars would form a calibration set for testing mass–luminosity relations and for anchoring distance and age estimates in the H-R diagram regions the survey targets.","A natural next step, not stated in the paper, would be to search the TESS light curves for tertiary eclipses or transit-like signals, potentially revealing new compact triples or circumbinary planets."],"forward_implications":["The 325 systems with component masses add a large homogeneous sample to the small set of benchmark DEBs, directly populating the low-mass (<0.9 M_sun) and high-mass (>3 M_sun) regions that DEBCat-style catalogs underrepresent.","With TESS light curves in hand, the same stars can be carried from mass measurements to full physical characterisation — radii, temperatures, ages, distances — allowing direct tests of stellar evolution models.","The sub-1% mass precision reported for long-period systems makes these binaries suitable anchors for calibrating mass–luminosity and mass–radius relations.","The identification of 80 multiples, including compact hierarchical triples, provides a sample for studying binary formation and dynamical evolution.","The 14 confirmed and 8 candidate pulsating stars in eclipsing binaries open the way to combine eclipse-based masses with asteroseismic mode identifications."],"supporting_citations":[{"why":"Supplied the ASAS variable-star catalogue from which the original southern CRÉME targets were selected.","marker":"Pojmanski, 2002"},{"why":"Defines the DEBCat benchmark catalogue of detached eclipsing binaries that the survey's precision goals are measured against.","marker":"Southworth, 2015"},{"why":"Describes the earlier low-mass DEB search that CRÉME grew out of, establishing the survey lineage.","marker":"Helminiak et al., 2011"},{"why":"Presents HD 187669, the first Galactic double-giant DEB with high-precision parameters, demonstrating the project's methodology.","marker":"Helminiak et al., 2015"},{"why":"Uses total-eclipse spectroscopy to reduce age and distance uncertainties in 11 DEBs.","marker":"Helminiak et al., 2024"},{"why":"Analyses triple-lined systems BD+44 2258 and KIC 06525196, a sub-project on compact hierarchical triples.","marker":"Moharana et al., 2023"},{"why":"Extends the triple analysis to low-mass double-lined and triple-lined systems.","marker":"Moharana et al., 2024"},{"why":"Provides a comprehensive study of five delta Scuti pulsators in DEBs, a sub-project of CRÉME.","marker":"Pawar et al., 2024"}],"fun_headline_variants":["Masses for 325 eclipsing binaries from 7,000 spectra","7,000 spectra pin down masses of 325 eclipsing binaries","CRÉME delivers masses for 325 eclipsing binaries","TESS and spectra yield masses for 325 binaries","CRÉME pinpoints masses of 325 binary stars"],"cache_read_input_tokens":3200,"weakest_assumption_plain":"The published masses assume every one of the 325 detached eclipsing binaries is seen almost exactly edge-on, so the measured $M\\sin^3(i)$ can be read as the true mass; if a significant fraction have shallower, grazing eclipses, their masses would be systematically low.","fun_headline_variants_meta":{"raw":{"variants":["Masses for 325 eclipsing binaries from 7,000 spectra","7,000 spectra pin down masses of 325 eclipsing binaries","CRÉME delivers masses for 325 eclipsing binaries","TESS and spectra yield masses for 325 binaries","CRÉME pinpoints masses of 325 binary stars"]},"model":"deepseek-v4-flash","effort":"low","cost_usd":0.00125,"raw_usage":{"total_tokens":5109,"prompt_tokens":912,"completion_tokens":4197,"prompt_tokens_details":{"cached_tokens":384},"prompt_cache_hit_tokens":384,"prompt_cache_miss_tokens":528,"completion_tokens_details":{"reasoning_tokens":4109}},"tokens_in":528,"tokens_out":4197,"duration_ms":27483,"temperature":1.0,"reasoning_tokens":4109,"cache_read_input_tokens":384,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-08-11T13:39:07.590526+00:00","model_set":{"reader":"deepseek-v4-flash"},"falsifier":"For a random subset of the 325 systems, fit the TESS light curves to recover the orbital inclination $i$; if more than a few percent come out with $\\sin^3(i) < 0.95$ (i below about 80 degrees), the survey's mass values are biased and must be corrected per system, and the claimed sub-1% precision would not hold for those objects.","supporting_citations":[{"cited_title":"2015, in Astronomical Society of the Pacific Conference Series, Vol","cited_arxiv_id":null,"evidence_quote":"Defines the DEBCat benchmark catalogue of detached eclipsing binaries that the survey's precision goals are measured against."},{"cited_title":"G., Marcadon , F., et al","cited_arxiv_id":null,"evidence_quote":"Analyses triple-lined systems BD+44 2258 and KIC 06525196, a sub-project on compact hierarchical triples."},{"cited_title":"G., Marcadon , F., et al","cited_arxiv_id":null,"evidence_quote":"Extends the triple analysis to low-mass double-lined and triple-lined systems."}],"review_version":1}