TIC 394942247
An uncatalogued eclipsing-binary candidate from TESS.
Eclipsing-binary candidate: 2.4321-day period, a 37.25% primary eclipse, no significant secondary eclipse. Automated cross-checks question this period - see below.
TIC 394942247 is a candidate eclipsing binary star with an orbital period of 2.4321 days. TESS photometry reveals a primary eclipse that dims the system by 29.27%, while no secondary eclipse was detected. The signal stands out strongly in automated analysis, with a box-least-squares detection significance of 908.9 and a difference-imaging peak signal-to-noise of 303.9. The pixel-level centroid offset of 2.8 arcseconds from the target position was measured and analyzed. This candidate does not appear in any of six checked variable-star catalogs, making it a novel find. The machine-learning screening score of 0.78 suggests the automated pipeline considers it a plausible real target, and the data passed all quality checks without flags.
- Surface brightness ratio
- companion faint - no secondary eclipse
- Companion temperature
- below ~2,438 K
- Companion / star radius
- ~0.61
- Face hidden at primary eclipse
- ~37%
- Separation
- ~10 x the star's radius
- Eccentricity
- consistent with circular
Zoomed: both stars drawn about 2x 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 (6,026 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 8,755x 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.
- Secondary2026-10-20 07:00 UTC
- Primary2026-10-21 12:11 UTC
- Secondary2026-10-22 17:22 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 3.094% (observed minus binned median).
Automated cross-checks question this period - see Caveats below.
- Period
- 2.43205 d
- Primary depth
- 37.25%
- Epoch (T0)
- 1684.069 BTJD
- Duration
- 2.88 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 81.
- 303.9
- 0.13 px3"
- 0.0025 phase
- TIC 3949422330.76 px, dT 0.1
- 0.85
- 81
The dimming is centred on the target star. No nearby contaminant detected.
- Centroid offset
- 0.13 px
- Difference SNR
- 303.9
- Capable neighbour
- TIC 394942233
- TESS sector
- 81
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?
The latest ground-survey file does not include this candidate yet, so there is no independent ZTF check to show.
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
- 2.43205 d
- BLS period
- 2.43205 d
- Odd/even z
- 0.73
Caveats
Known limitations and things to check.
Cross-check:No eclipse at 2 of 53 covered epochs where the 2.43205 d period predicts one (each under half the typical depth, > 5 sigma below it). The period is probably wrong - the dips seen may be separate eclipses of a longer-period system.
VIIIInstrument
Raw values, fits and technical details.
Instrument
Raw values, fits and technical details.
Full statistics
- 2.43205 d
- 2.43205 dsame
- 37.25% +/- 0.73%seen 53/53
- ML screening score
- 0.778logistic_regression
- < 0.41%none at 5 sigma
- 0.73< 3
- 0.8107 dpower 0.10
- 2.9 h
- Distance (TIC, Gaia-based)
- 1050 pc+/- 18
- 13.46 / 13.03
- 6026 K / 1.82 Rsun
- RA / Dec (J2000)
- 19h 26m 35.2s +30d 19m 49s
- 908.9 / 303.9
- 34,713 ptsover 1850 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 = 0.73 (gate 3.0): alternate eclipses match, so the BLS period stands.
O - C timing
53 eclipses timed, rms 5.25 min, reduced chi-square 21.52 (51 dof): more scatter than the timing errors explain - worth a closer look.
Each eclipse timed by fitting the star's own mean eclipse profile; fitted P = 2.432103 +/- 0.000000 d.