TIC 9586662
An uncatalogued eclipsing-binary candidate from TESS.
Eclipsing-binary candidate: 1.1131-day period, a 2.88% primary eclipse, a 1.64% secondary eclipse at phase 0.504. Automated cross-checks question this period - see below.
TIC 9586662 is a candidate eclipsing binary star with an orbital period of 1.1131 days. Automated analysis of TESS photometry detected a primary eclipse causing a 2.77 percent dimming of the star's light, with a box least-squares detection signal-to-noise of 84.1. Pixel-level image analysis produced a difference-imaging peak signal-to-noise of 6.2, though the centroid offset of 10.8 arcsec from the target position warrants attention. No secondary eclipse was detected, and the candidate does not appear in six major variable-star catalogs. The machine-learning screening score of 0.46 suggests moderate confidence in this target. All data quality checks passed without flags.
- Surface brightness ratio
- 0.57
- Companion temperature
- ~4,472 K
- Companion / star radius
- ~0.17
- Face hidden at primary eclipse
- ~3%
- Separation
- ~7.2 x the star's radius
- Eccentricity
- consistent with circular
- Secondary eclipse phase
- 0.504 measured, 0.500 in this orbit
Zoomed: both stars drawn about 1x larger than their real size relative to the orbit, so they overlap for longer than the real eclipse lasts. A star's surface never gets dimmer during an eclipse - part of it is simply hidden. What drops is the total light we receive, shown exactly by the readout and bar below from the real light curve; the glow dims with it, exaggerated so small dips show. Colours follow temperature on a stellar colour scale, saturated so the differences show; the star's is its catalogue value (5,162 K). The companion's colour, sizes and orbit shape are estimates from the eclipse depths, duration and timing, assuming central eclipses and spherical stars - good to perhaps tens of percent. Only the relative orbit is shown; both stars really circle their common centre of mass. Animated about 4,007x faster than real on average, slowing down through each eclipse, and starting from where the system is in its orbit right now. Hover to pause.
- Secondary2026-10-19 10:18 UTC
- Primary2026-10-19 23:34 UTC
- Secondary2026-10-20 13:01 UTC
Computed from the fitted ephemeris. Approximate - not corrected for your location or for light-travel time across Earth's orbit.
The signal
A repeating, consistent dip in brightness.
Residual scatter 23339123732939592.000% (observed minus binned median).
Automated cross-checks question this period - see Caveats below.
- Period
- 1.11307 d
- Primary depth
- 2.88%
- Secondary depth
- 1.64%
- Epoch (T0)
- 1569.737 BTJD
- Duration
- 1.39 h
The catalog check
Cross-matched against known variable-star catalogs to rule out anything already listed.
- VSXNot found
- ASAS-SNNot found
- Gaia eclipsing-binary tableNot found
- Gaia variable classificationNot found
- TESS EB catalog (Prsa+2022)Not found
- ExoFOP TOI listNot found
0/6 catalogs list a known variable at this position.
No known variable star or catalogued match at this position.
- Catalogs checked
- 6
- Matches
- 0
The pixel check
Confirms the dimming is on the target star, not a nearby source.
Out/in share one sqrt colour scale; in-eclipse = out-of-eclipse minus difference. TESS sector 10.
- 6.2
- 0.52 px11"
- 0.0000 phase
- TIC 95866834.51 px, dT 2.4
- 0.95
- 10
The dimming is centred on the target star. No nearby contaminant detected.
- Centroid offset
- 0.52 px
- Difference SNR
- 6.2
- Capable neighbour
- TIC 9586683
- TESS sector
- 10
The Gaia view
A second spacecraft's measurements: how far away the star is, how bright and what colour, and whether its position fits a single star.
The latest Gaia context file does not include this candidate yet, so there is no Gaia view to show.
The ground-survey check
An independent instrument, different years: does real ZTF photometry show the eclipse at the period TESS measured?
- ZTF g (145 pts, 0 outliers)Too few outliers to test
- ZTF r (163 pts, 0 outliers)Too few outliers to test
Folded at the TESS-measured period of 1.11307 d, no band shows a phase cluster tight enough to rule out chance. Ground-survey cadence is sparse - a handful of epochs per orbit - so this is the expected outcome for most real eclipses, not evidence against this one.
Source: ZTF public light-curve archive (IRSA), independent of the TESS data used to detect this candidate.
Fold it yourself
Adjust the period and watch the eclipse appear.
Shown at the true period. The raw light curve needed to re-fold at other periods has not been exported yet - this slider unlocks automatically once it is.
The period the pipeline measured. Drag the slider away from it and the eclipse smears out.
- True period
- 1.11307 d
- BLS period
- 1.11307 d
- Odd/even z
- 0.82
Caveats
Known limitations and things to check.
Cross-check:Eclipse duration (1.39 h) is too short relative to this light curve's ~30-minute cadence for any single predicted eclipse to hold enough points to measure on its own. The primary depth below is the whole-light-curve fold measurement from the vetting step, not a per-epoch one.
VIIIInstrument
Raw values, fits and technical details.
Instrument
Raw values, fits and technical details.
Full statistics
- 1.11307 d
- 1.11307 dsame
- 2.88% +/- 0.08%seen 0/0
- ML screening score
- 0.460logistic_regression
- 1.64% +/- 0.09%phase 0.504, 19 sigma
- 0.82< 3
- 13.1043 dpower 0.01
- 1.4 h
- Distance (TIC, Gaia-based)
- 672 pc+/- 52
- 13.84 / 13.27
- 5162 K / 1.34 Rsun
- RA / Dec (J2000)
- 12h 53m 29.1s -27d 23m 33s
- 84.1 / 6.2
- 1,075 ptsover 26 d
Eclipse close-ups
Same flux scale on both panels. Line: binned median. Shown in place of an orbit animation - this pipeline measures eclipses, it does not fit an orbit.
Period alias analysis
Odd/even depth z = 0.82 (gate 3.0): alternate eclipses match, so the BLS period stands.