A dip in a stellar light curve is only a transit candidate until it survives checks for repeatability, data quality, source contamination and known instrumental effects. To assess one, retrieve the target’s light curve and pixel-level products from the Mikulski Archive for Space Telescopes (MAST), record the sectors and cadence, inspect the unmodified data, apply documented cleaning, fold the series on trial periods, and compare the result with TESS pipeline diagnostics and current catalog status.
A transit-like signal, a Threshold Crossing Event (TCE) or a TESS Object of Interest (TOI) is not proof of a planet. Eclipsing binaries, spacecraft systematics and other false alarms can produce similar shapes. The defensible outcome of an archival screen is usually “possible transit-like signal” or “candidate for follow-up,” not “confirmed exoplanet.”
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What a genuine transit test must establish
A planetary transit is the small dimming produced when a planet passes in front of its host star from the observer’s viewpoint. A single dip cannot establish that geometry. It could be a bad measurement, a spacecraft-related disturbance, a data gap edge, stellar variability or an eclipsing binary.
Your analysis should answer four separate questions:
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- Is the feature present in the original measurements, rather than created by a processing choice?
- Does a similar event recur at a consistent interval and phase?
- Does the target’s pixel context support the target as the source of the signal?
- Do pipeline diagnostics and the current archive status leave unresolved alternatives?
Those questions produce an evidence trail. They do not by themselves confirm a planet; confirmation requires additional observations or analysis that rules out plausible alternatives.
Find the correct observations in MAST
The official archive for TESS mission data products is the Mikulski Archive for Space Telescopes (MAST), hosted at the Space Telescope Science Institute. Kepler and K2 material is also available through the archive. Search by the star’s name, catalog identifier or coordinates, then verify that the returned target is the intended object rather than a nearby source with a similar name.
Record the observation metadata first
Before downloading anything, make a small record for every observation:
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- Target identifier and sky position.
- Mission and sector or campaign.
- Observation start and end dates.
- Cadence represented by the file.
- Whether an extracted Light Curve File (LCF), Target Pixel File (TPF), Full Frame Image (FFI) cutout or Data Validation product is available.
- Gaps, quality flags and whether the target was observed in more than one sector.
A target observed in several TESS sectors may have separate files for each sector. Do not assume that one downloaded light curve represents the full time span. Sector boundaries, different observing windows and missing products can change the number of events you are able to test.
Choose a product that matches the question
| Product | What it contains | Best use | Important limitation |
|---|---|---|---|
| Light Curve File (LCF) | An extracted photometric time series | Quickly plotting brightness against time and testing repeatability | The extraction and aperture choices are already made |
| Target Pixel File (TPF) | Time-resolved pixels around the target | Checking the aperture, neighboring stars and whether the dimming is centered on the target | Requires more interpretation or a custom extraction |
| Full Frame Image (FFI) cutout | A wider image field that can be used to build a light curve | Searching many stars or creating a custom measurement when a standard product is unsuitable | More processing work and source-selection decisions |
| Data Validation (DV) products | Pipeline reports, diagnostic plots and parameter references for TCEs and known candidates | Reviewing transit consistency, eclipsing-binary indicators and instrumental checks | Available products and coverage depend on the target and sector |
Use an LCF for the first time-series inspection, then move to a TPF or FFI when the source or aperture context matters. MAST also provides sector-stitched DV curves for known planets and TOIs when those products exist.
Inspect the raw light curve before cleaning
Plot flux (or relative brightness) against time exactly as delivered. Keep the raw plot beside every processed version. This prevents a detrending operation from becoming the only evidence for the event.
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- Mark gaps. Note long interruptions, sector joins and isolated missing points. An apparent pair of dips on either side of a gap may not be a recurring signal.
- Read the quality information. Mark intervals carrying data-quality flags, including spacecraft events or other conditions identified in the file.
- Inspect the target’s pixel context when available. In a TPF, check which pixels are in the photometric aperture and whether a nearby star could contribute light.
- Identify suspicious intervals. Look for sudden level changes, clusters of outliers, ramps or visibly noisy stretches. NASA’s Lightkurve tutorial shows a noisy interval associated with spacecraft jitter and masks that interval before further analysis.
- Save an observation log. Record every excluded time range, point-removal rule and later detrending setting, with a reason for each choice.
Do not discard an inconvenient point merely because it weakens the dip. Remove a point or interval only when the quality flag, an obvious measurement failure or a documented spacecraft event provides a reason. A candidate that exists only after aggressive editing is not persuasive.
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Detrending removes slow changes caused by stellar variability, instrument response or spacecraft systematics so that short-duration events can be seen. It can also remove or reshape a real transit if the window is too short or the model follows the dip itself.
Use a reversible sequence
- Start from the unmodified flux and preserve that file or plot.
- Mask intervals already identified as unreliable, including flagged data and the spacecraft-jitter segment if it is present.
- Remove only clearly justified outliers, and keep a list of their timestamps.
- Fit or apply a smooth baseline to the remaining data, choosing a window long enough that a transit is not treated as ordinary baseline variation.
- Divide or subtract by that baseline to obtain a normalized curve.
- Plot raw, masked and detrended versions together, with the candidate times marked.
Repeat the analysis with a reasonable alternative detrending choice. If the event’s depth, duration or existence changes dramatically, report that sensitivity instead of selecting the most attractive plot. Detrending is a convenience for measurement, not independent confirmation.
Test whether the dip repeats at a consistent period
A repeating pattern is the central distinction between a one-off anomaly and a transit-like candidate. For a new target, the period is unknown, so treat every trial period as a hypothesis to test rather than as a known input.
Fold the cleaned series
- Select a trial period based on the spacing between plausible events and the total time span available.
- Convert each observation time to orbital phase using that trial period.
- Plot the phase-folded flux, keeping enough phase range to see the baseline on both sides of the event.
- Change the trial period slightly. A real repeating signal should sharpen near an appropriate period and smear when the period is wrong.
- Compare the individual events in time order and by sector before relying on the combined folded plot.
NASA’s tutorial demonstrates folding a TESS curve on the known period of an example planet. With an unknown object, that known period is not available: a convincing fold must be supported by separate events that align without being forced by the chosen period.
Check event-to-event consistency
- Do the dips occur at the predicted times in more than one sector when coverage allows?
- Are their widths and overall shapes broadly compatible?
- Does one apparent event disappear when flagged points or a noisy interval are restored?
- Does the signal remain when each sector is examined separately?
- Are there enough observations outside the dips to establish a stable baseline?
When only one event is covered, you can describe a possible single transit, but you cannot demonstrate a period from that light curve alone. A long gap can also hide intervening events, so state the coverage limitation explicitly.
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Use pixels and diagnostics to test alternative sources
An extracted light curve may combine the target with neighboring stars. A TPF lets you inspect the aperture and surrounding pixels, while an FFI cutout can provide a wider view for a custom extraction. If the apparent dimming is stronger in pixels associated with a nearby source than in the target’s pixels, the target may not be the object that faded.
Pixel inspection is a source check, not a complete false-positive analysis. Keep the aperture definition and any custom extraction settings with your results so another reader can see how the time series was made.
Understand TCE, TOI and Data Validation status
Threshold Crossing Event (TCE)
A TCE is a transit-like signal that passes a pipeline detection threshold and is sent for more analysis. It has little-to-no vetting at that stage. Instrumental false alarms and astrophysical false positives can both become TCEs.
TESS Object of Interest (TOI)
A TOI is a provisional catalog designation, not a confirmation. The catalog includes planet candidates and false positives, and a disposition can change when additional data or analysis arrive. Always record the status date or catalog version you used rather than presenting it as permanent.
Data Validation reports
The one-page DV summary is designed to show whether a TCE is consistent with a transit or instead points toward an eclipsing binary or instrumental noise. Read the plots and explanations together with your own raw and folded curves. A favorable DV page strengthens the case for follow-up; it does not replace follow-up.
NASA also lists Lightkurve, transit-modeling packages and false-positive assessment tools for deeper work. Treat their output as evidence to interpret. A software label is not a physical diagnosis, and different inputs or masks can change a result.
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Separate a transit-like signal from common false alarms
Spacecraft or detector effects
Jitter, flagged intervals, sudden baseline changes and clusters of bad points can create dips or distort their shape. If the feature coincides with a quality flag or a visibly noisy spacecraft interval, classify it as a data-quality concern until independent evidence says otherwise.
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Eclipsing binaries
An eclipsing stellar companion can produce a periodic dimming that resembles a planetary transit. DV products are specifically intended to expose indicators of this alternative. A signal that is deep, changes shape between events or shows evidence inconsistent with a small companion deserves an eclipsing-binary assessment rather than a planet label.
Blended or neighboring sources
Flux from another star inside the aperture can dilute or create the apparent event. Use TPF or FFI pixels to check the aperture and nearby sources, and compare sectors if the spacecraft roll changes which stars fall in the aperture.
Processing artifacts
An event that appears only after a particular smoothing, clipping or detrending choice is not robust. Re-run the documented workflow with a reasonable alternative and show both results.
Compare coverage before drawing a conclusion
| Coverage situation | What you can responsibly say | What remains unresolved |
|---|---|---|
| One short sector, one apparent dip | Possible transit-like event or data anomaly | Period, recurrence and many false-positive scenarios |
| One sector, several aligned events | Periodic transit-like candidate if quality checks pass | Source contamination and eclipsing-binary alternatives |
| Multiple sectors with consistent events | Stronger repeatability evidence and a better period estimate | Confirmation and independent validation |
| LCF plus TPF/FFI and DV diagnostics | A more defensible archival assessment | Follow-up observations needed for a planetary interpretation |
Cadence matters as much as sector count. Short events can be poorly sampled in a long cadence, while gaps can hide expected repeats. State the cadence and time span alongside any period or duration estimate.
Report the result at the correct confidence level
Use language that matches the evidence:
- Data-quality issue: the feature coincides with flags, a gap edge, spacecraft jitter or unstable processing and does not persist under reasonable checks.
- Possible transit-like signal: a dip remains in the original data and has some coherent behavior, but recurrence or source attribution is incomplete.
- Candidate for follow-up: repeated events align at a consistent period across available coverage, the pixel context is plausible and diagnostics do not identify an obvious alternative.
- Confirmed planet: do not use this label for an archival light-curve screen alone. Confirmation requires additional observations or analysis that addresses eclipsing binaries, instrumental effects and other false positives.
Include the target identifier, sectors, dates, cadence, products examined, masks, detrending choices, trial period, events used and unresolved alternatives. This makes the result reproducible and prevents a later catalog update from being mistaken for a contradiction in your original assessment.
When and how to pursue follow-up
If the signal remains plausible, compare it with the current TCE or TOI entry and its DV products, then seek independent evidence. NASA Exoplanet Watch provides robotic-telescope observations to process and free EXOTIC software for turning images into light curves. Its guidance recommends checking predicted visibility and transit timing before observing. This is an additional follow-up route, not a prerequisite for examining archival data.
For citizen-science screening, the NASA Exoplanet Archive FAQ identifies Planet Patrol for assessing which TESS candidates are real and Planet Hunters TESS for finding planets in TESS data. These projects can help prioritize targets, but their classifications still require appropriate scientific vetting.
A practical checklist
- Target name or coordinates verified.
- Mission, sectors, dates and cadence recorded.
- LCF inspected, with TPF or FFI checked when source context matters.
- Raw flux plotted before any cleaning.
- Quality flags, gaps, outliers and spacecraft-related noise marked.
- Masks and detrending settings saved.
- Raw and processed curves compared.
- Trial periods folded and individual events inspected.
- Coverage checked sector by sector.
- TCE, TOI and DV status reviewed with its date or version.
- Instrumental, eclipsing-binary and blending alternatives considered.
- Conclusion labeled as anomaly, possible signal or follow-up candidate—not confirmation.
Frequently Asked Questions
Do I need my own telescope to check a TESS light curve?
No. MAST provides public TESS light curves and pixel products, and software such as Lightkurve is available for analysis. A telescope becomes relevant only if you choose to collect independent follow-up photometry.
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Report it as a possible single transit and document the observing window. Without a second event, the period and repeatability cannot be established from that light curve alone.
Can a TOI be removed or reclassified?
Yes. TOI dispositions are provisional; later observations and analysis can move an entry between candidate and false-positive categories.
Why keep the raw curve if the detrended plot is clearer?
The raw curve shows whether the feature was present before processing. Keeping both versions reveals when a mask or baseline model changes the apparent event.
Which product should I download first?
Start with an extracted Light Curve File for a quick time-series check. Add a Target Pixel File or FFI cutout when neighboring sources, aperture selection or a custom extraction could affect the interpretation.
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