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Adding TESS to CR\'EME. Light curves and masses of 300+ eclipsing binaries

T0 review · 2 major / 4 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read 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.

desk verdict 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). read the letter →

arxiv 2412.12867 v1 pith:DOYWPXC7 submitted 2024-12-17 astro-ph.SR

Krzysztof G. He{l}miniak , Ayush Moharana , Tilak B. Pawar , Ganesh Pawar This is my paper · ORCID
classification astro-ph.SR
keywords detachedeclipsingbinariesdouble-linedspectroscopicstellarmassesradialvelocitiesTESSphotometryevolutionbenchmarksmultiplestarsystemspulsatingstarsin
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

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.

What carries the argument

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.

What would settle it

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.

Watch

Extended reading notes

Core claim

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%.

Load-bearing premise

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.

Editorial extensions

If this is right

  • 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.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • 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.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

2 major / 4 minor

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.

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 (2)
  1. [§2.1 footnote 1 and §3.1 'Masses of 650 stars']
  2. [§3.1 'Masses of 650 stars']
minor comments (4)
  1. [Title page]
  2. [Abstract and §2.2]
  3. [Abstract]
  4. [§2.1]

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the paper is a project status report whose mass estimates are direct products of radial-velocity fits, with the M sin^3(i) caveat openly stated.

full rationale

This paper is a survey/project status report rather than a derivation of a new result from first principles. The main quantitative claim is that radial-velocity data for 325 double-lined systems allow orbital parameters and component masses to be estimated. Those masses are obtained by standard Keplerian fitting, which yields M sin^3(i); the paper explicitly acknowledges this in footnote 1: 'Technically only the lower mass limits M sin^3(i), but in DEBs sin^3(i) ≃ 1, therefore they are good proxies of true stellar masses.' The later phrase 'absolute masses' in Section 3.1 is a labeling/convention choice and a possible accuracy concern, but it is not circular reasoning: no output quantity is defined in terms of the claim it is supposed to support, and no fitted parameter is renamed as an independent prediction. Self-citations in the paper refer to the project's own earlier spectroscopic and photometric analyses; they serve as documentation of prior work, not as an external authority invoked to force the present count of 325 systems. The TESS photometry statistics are observational bookkeeping. The skeptical worry about grazing eclipses and systematically underestimated masses is a legitimate scientific caveat about the DEB assumption, but it does not make the argument circular. Under the specified circularity criteria, the honest finding is no significant circularity with score 0.

Assumptions & free parameters 0 free parameters · 2 assumptions · 0 invented entities

The paper contributes a survey status report; it introduces no free parameters or new physical entities. Its claims rely on standard spectroscopic binary analysis and on the DEB classification of the target sample.

assumptions (2)
  • domain assumption M sin^3(i) is a good proxy for the true stellar mass because sin^3(i) is approximately 1 for detached eclipsing binaries.
    Footnote 1 states that the masses are technically lower limits M sin^3(i), but for DEBs sin^3(i) is close to 1, so they are treated as true masses. If a significant subset of targets has inclination significantly below 90 degrees, masses would be underestimated.
  • domain assumption The 386 targets classified as detached eclipsing binaries from ASAS and Kepler photometry are genuine DEBs with no third-light contamination significant enough to affect mass estimates.
    The paper relies on the existing DEB classification of the target sample (Section 2.1) and does not re-derive it. Misclassification or undetected companions could bias the inferred masses.

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Cite this review

Pith. "Pith review of Adding TESS to CR\'EME. Light curves and masses of 300+ eclipsing binaries." pith.science (2026). https://pith.science/paper/DOYWPXC7

@misc{pith2026241212867,
  author       = {Pith},
  title        = {Pith review of: Adding TESS to CR\'EME. Light curves and masses of 300+ eclipsing binaries},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/DOYWPXC7}},
  note         = {Machine review of arXiv:2412.12867}
}
abstract

The Comprehensive Research with Echelles on the Most interesting Eclipsing binaries (CR\'EME) projects was aimed to collect high-resolutions spectra of about 380 detached eclipsing binaries (DEBs), which mostly do not have literature RV data. From this vast observational material we were able to estimate masses of components of 325 double-lined system. Since the launch of the TESS mission we have been collecting 2-min cadence photometry for the CR\'EME targets through successful GI proposals. As by Sector 85, we obtained data for $>$330 of them. We are thus now in the process of comprehensively analyzing our targets. This paper presents the recent status of the CR\'EME project and its space photometry counterpart, and describes several sub-projects within CR\'EME that focus on specific classes of targets.

Figures

Figures reproduced from arXiv: 2412.12867 by the authors.

Figure 1
Figure 1. Left: On-sky distribution of CREME targets. Right: Masses and radii of ´ binary components from the DEBCat catalogue (orange and green for primaries and secondaries, respectively) and CREME DEBs published so far (black and purple for ´ primaries and secondaries, respectively). Masses alone, or even the orbital solutions, can already point towards some of the interesting properties, such as: location on the cool (<0.… view at source ↗

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Reference graph

Works this paper leans on

13 extracted references · 7 canonical work pages

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    ENTRY address archiveprefix author booktitle chapter edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year doi label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts #0 'before.all :=...

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    " write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 global.max substring 't := if while FUNCTION word.in bbl.in " " * FUNCTION format....

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