TIC 348837498
An uncatalogued eclipsing-binary candidate from TESS.
Eclipsing-binary candidate: 4.3965-day period, a 8.43% primary eclipse, a 0.59% secondary eclipse at phase 0.500.
TIC 348837498 is a candidate eclipsing binary star identified through automated analysis of TESS photometry. The system shows a primary eclipse with a depth of 6.03% and an orbital period of 4.3965 days, with no secondary eclipse detected. The eclipse signal achieved a detection significance of 157.0 in the Box Least Squares search, and pixel-level image analysis confirmed the signal with a peak signal-to-noise ratio of 18.3, though the centroid offset of 7.7 arcseconds warrants further investigation. This candidate does not appear in six major variable-star catalogs, making it a newly identified target. The machine learning screening assigned it a score of 0.39, indicating moderate confidence for a real eclipsing system.
- Surface brightness ratio
- 0.07
- Companion temperature
- ~3,184 K
- Companion / star radius
- ~0.29
- Face hidden at primary eclipse
- ~8%
- Separation
- ~15 x the star's radius
- Eccentricity
- consistent with circular
- Secondary eclipse phase
- 0.500 measured, 0.500 in this orbit
Zoomed: both stars drawn about 3x 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 (5,855 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 15,827x 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 10:08 UTC
- Primary2026-10-22 14:51 UTC
- Secondary2026-10-24 19:39 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 25.414% (observed minus binned median).
Clear, repeating eclipses with a consistent period and depth.
- Period
- 4.39651 d
- Primary depth
- 8.43%
- Secondary depth
- 0.59%
- Epoch (T0)
- 1517.954 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 8.
- 18.3
- 0.37 px8"
- -0.0025 phase
- TIC 3488374992.09 px, dT 2.4
- 0.82
- 8
The dimming is centred on the target star. No nearby contaminant detected.
- Centroid offset
- 0.37 px
- Difference SNR
- 18.3
- Capable neighbour
- TIC 348837499
- TESS sector
- 8
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
- 4.39651 d
- BLS period
- 4.39651 d
- Odd/even z
- 1.31
Caveats
Known limitations and things to check.
No caveats flagged: this candidate cleared every gate with no named exception. Follow-up observations would still be needed to confirm the stellar parameters.
VIIIInstrument
Raw values, fits and technical details.
Instrument
Raw values, fits and technical details.
Full statistics
- 4.39651 d
- 4.39651 dsame
- 8.43% +/- 0.15%seen 3/5
- ML screening score
- 0.391logistic_regression
- 0.59% +/- 0.09%phase 0.500, 6 sigma
- 1.31< 3
- 8.4698 dpower 0.04
- 2.9 h
- Distance (TIC, Gaia-based)
- 574 pc+/- 8
- 13.51 / 13.04
- 5855 K / 1.06 Rsun
- RA / Dec (J2000)
- 08h 58m 49.3s -16d 38m 34s
- 157.0 / 18.3
- 862 ptsover 25 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 = 1.31 (gate 3.0): alternate eclipses match, so the BLS period stands.