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Start with the Asteroid Lightcurve Database (LCDB) for published rotation periods and lightcurve-quality information. Use NASA/JPL’s Small-Body Database (SBDB) to resolve an object’s identity, check orbital data, and query many bodies at once with the rot_per rotation-period field. Treat a period shorter than 2.2 hours as a screening clue—not proof of a confirmed “super-fast” rotator—until you check the LCDB reliability code and, for important claims, the original observing paper.
Which database should you use?
Fast-spinning asteroid research usually requires two complementary databases rather than one. LCDB is the literature compilation: it gathers published lightcurve periods, amplitudes, observing notes and a subjective reliability code. SBDB is the identity and small-body reference service: it accepts a number, provisional designation, name or SPK-ID and returns the matching object with orbital and selected physical information, including a rotation period when one is available.
| Database | Best use | What to record | Important scope note |
|---|---|---|---|
| Asteroid Lightcurve Database (LCDB), NASA Planetary Data System v4.0 archive | Find published synodic periods, lightcurve results, amplitudes, notes and the U reliability code. | Object designation, preferred period, units, amplitude, U code, cited paper and the archive/version context. | The archive describes 34,967 targets; its data context ends on 2021-09-02. |
| NASA Open Data LCDB v3.0 record | Access a separate catalog record for an earlier LCDB version. | Version and catalog date, not just the target count. | It describes more than 24,500 targets. The catalog record shows an update on July 17, 2025. This is not a later count for v4.0. |
| NASA/JPL Small-Body Database (SBDB) | Resolve identity, inspect orbital information and query sets of objects by available fields. | Accepted identifier, returned designation, rot_per value, units, and any missing-field caveats. |
Physical parameters are not available for every object. |
Do not combine the v3.0 and v4.0 target counts into one “current” total. They describe different version records and dates. The available records also do not provide a directly comparable total number of confirmed fast rotators, so a catalog target count cannot be used as a prevalence statistic.
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What counts as a fast-spinning asteroid?
A period below 2.2 hours is a commonly used literature threshold for a “super-fast” asteroid. The threshold is associated with the approximate spin barrier for many larger, gravity-bound rubble-pile bodies: if such an object spins faster, gravity alone may not hold its loose material together. It is not a universal physical classification.
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Why the 2.2-hour threshold is only a screening rule
- Small asteroids can rotate faster because material cohesion can become more important than self-gravity.
- Composition, size, shape and internal structure change the speed at which mass would begin to shed or fail.
- Photometric uncertainty and alternative period solutions can move an object across the threshold.
- A database period may be a candidate solution rather than a securely established rotation.
Use “below 2.2 hours” to select objects for review. Reserve “confirmed super-fast rotator” for a result supported by adequate lightcurve coverage, a strong LCDB reliability assessment and, when the claim matters, the cited observing study.
Workflow for a known asteroid
When you already have one asteroid in mind, identify it first, then read its period record in context.
- Collect the exact designation. Write down the numbered name, provisional designation or designation used by the observing paper. A paper may use a form that differs from a casual name or from another catalog entry.
- Search LCDB. Enter the numbered name or provisional designation in the LCDB search interface. If a name returns multiple possibilities or no result, search with the designation exactly as printed in the source paper.
- Read the complete period entry. Record the preferred rotation period, period units, lightcurve amplitude, any alternate period or notes, the U code and the cited publication. Do not copy only the shortest number shown in a search result.
- Resolve the identity in SBDB. Look up the same body by IAU number, designation, name or SPK-ID. Compare the returned designation with the LCDB entry and the paper before joining records from the two services.
- Check available context. Use SBDB for orbital elements and any listed physical parameters. A blank physical field means that value is not supplied there; it is not evidence that the object lacks the property.
- Assess the speed claim. Compare the period with 2.2 hours, then inspect the LCDB U code and the underlying paper. If the code is weak or the paper discusses aliases, report the object as a candidate.
- Save provenance. Keep the database version or access date, designation, period and units, U code, and full paper citation in your notes.
Finding candidates by period instead of opening objects one by one
For a survey, use the SBDB query tools or API to request a set of small bodies and include the rotation-period field rot_per. JPL documents rot_per as the body’s synodic rotation period in hours. A set query is more efficient than manually opening thousands of object pages.
A practical candidate-list sequence
- Choose the interval. For a super-fast screen, request periods below 2.2 hours. You can use a narrower interval for a focused search, but state the exact limits in your methods.
- Request identity and period together. Include the object designation or number and
rot_perin the returned fields. Without an identifier, a short period cannot be tied safely to a physical object. - Export the returned rows. Preserve the raw period value, units and any null or missing values. Do not treat a blank period as zero or as a failed fast-rotation test.
- Deduplicate designations. The same body can appear under a number, provisional designation or name. Normalize identifiers before counting candidates.
- Open each candidate in SBDB. Verify that the returned designation is the intended object and inspect the available orbital and physical context.
- Cross-check every candidate in LCDB. Confirm the preferred period, U code, amplitude and cited paper. A query result identifies records; it does not independently validate the photometry.
- Classify the result. Separate secure measurements, ambiguous measurements and unverified candidates in your spreadsheet or publication.
SBDB’s official API documentation describes its service as “a method of requesting machine-readable data for a specified small body within JPL’s SSD/CNEOS Small-Body DataBase (SBDB).” Use the documented query syntax and field names for the version you are calling; do not assume that every physical parameter is populated for every returned body.
How to read the LCDB reliability code
The LCDB U code is a judgment aid summarizing how convincingly a period has been established. It is not a replacement for reading the observations, and it is not an independent reanalysis of the lightcurve.
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| Code | Meaning | How to report it |
|---|---|---|
| U=1 | Fragmentary lightcurve data; the reported period might be wrong. | Use “reported candidate period” and identify the uncertainty. |
| U=2 | Ambiguity remains, or coverage exceeds half a rotation but is incomplete. | Call the period tentative or ambiguous unless the source paper supplies stronger evidence. |
| U=3 | Secure period determination. | You can describe it as a secure measured period, while still citing the source. |
Modified forms such as 2− and 2+ refine the subjective assessment around U=2. Keep the modifier when you transcribe the record; collapsing it to “U=2” loses information about the reviewer’s confidence.
Why coverage and cycle counts matter
Asteroid periods are inferred from repeating brightness changes. Gaps between lightcurves can leave the number of elapsed cycles uncertain, allowing several aliases to fit the observations. A short numerical period is therefore not automatically the true spin period, especially when observations were sparse or unevenly spaced.
Aliasing: the main reason a very short period can be wrong
Aliasing occurs when the observation cadence cannot distinguish the true repetition rate from another frequency that produces a similar sampled pattern. The problem is especially important for claims of extremely rapid rotation: a sparse sequence can make a longer period appear shorter, or select an incorrect multiple or fraction of the actual period.
Warning signs in a candidate record
- The LCDB entry has U=1, U=2 or a modified U=2 code.
- The source paper lists multiple period solutions or notes incomplete rotational coverage.
- Observations are separated by long gaps, with uncertain cycle counts between runs.
- A later study reports a different period or says that dense follow-up changed the classification.
- The claimed period lies just below 2.2 hours, where a small alias or uncertainty changes the label.
A 2025 study of super-fast-rotator candidates found that insufficient cadence could produce aliases; dense photometric follow-up reclassified some candidates and confirmed others. For a consequential claim, read that object’s cited observing paper and any later validation rather than relying on the query output alone.
How to verify that records describe the same object
Identity mistakes can be as damaging as period mistakes. Names, provisional designations and numbers are not interchangeable unless they resolve to the same body.
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- Copy the identifier exactly as shown in the source paper.
- Search SBDB using that identifier and note every returned designation, including a number, provisional designation and name when supplied.
- Compare those designations with the LCDB record. If they disagree, stop and resolve the discrepancy before combining periods or amplitudes.
- Check the object’s orbital context in SBDB. A substantially different orbit is a strong signal that you have matched the wrong record.
- Retain the SPK-ID when available as an additional machine-readable identity key.
Do not infer identity from a similar-looking name alone. A designation copied from a paper is the safest starting point when a casual name search is ambiguous.
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Recording results so they remain reproducible
A useful asteroid-period record preserves both the number and the conditions under which it was found. Use one row per object and include these columns:
- Object designation exactly as published.
- SBDB-resolved number, provisional designation, name and SPK-ID, when available.
- Rotation period in hours, explicitly labeled as synodic when taken from
rot_per. - LCDB preferred period and any alternate solution.
- Lightcurve amplitude and relevant notes.
- LCDB U code, including a 2− or 2+ modifier.
- Paper authors, title, journal or archive citation and publication year.
- LCDB archive/version and the date you accessed the record.
- Classification: secure, ambiguous or candidate.
- Reason for any exclusion, such as a missing period, identity conflict or alias concern.
For a published table, put the qualification beside the value. For example: “1.84 h, LCDB U=2, candidate; source paper reports incomplete cycle coverage.” Do not present “1.84” alone as if it were a definitive physical constant.
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Mixing LCDB version statistics
Problem: Reporting 34,967 targets from the NASA PDS v4.0 archive together with “more than 24,500” from the NASA Open Data v3.0 record as one current total.
Correction: Label each count with its version and date context. The v4.0 archive covers data through 2021-09-02; the v3.0 catalog record was updated July 17, 2025 but describes the earlier catalog version.
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Calling every sub-2.2-hour entry confirmed
Problem: Treating a threshold filter as a physical diagnosis.
Correction: Use the threshold to make a candidate list, then check U code, observing coverage and the paper. Report a candidate when the period is ambiguous.
Using SBDB as if it were a lightcurve review
Problem: Assuming a returned rot_per value proves that the period is secure.
Correction: Use SBDB for machine-readable retrieval and identity/orbital context. Use LCDB and the underlying paper for period quality and evidence.
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Problem: Treating a null, blank or unavailable rot_per field as a period outside your search range.
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Correction: Keep missing values separate. They indicate that SBDB did not supply a rotation period for that record.
Dropping units or the period type
Problem: Publishing “1.9” without saying hours or whether it is synodic.
Correction: Write the value as “1.9 hours” and identify rot_per as the synodic rotation period when that is the source field.
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A rapid period can motivate questions about cohesion, shape, density and mass shedding, but the database entry alone cannot determine those properties. The 2.2-hour framing applies most directly to larger bodies held together primarily by gravity. A small, cohesive asteroid can rotate faster without violating that simple rubble-pile picture.
Keep three statements separate in your notes and writing:
- Measurement: what period the lightcurve analysis reports.
- Confidence: how securely the observations establish that period.
- Physical interpretation: what the period may imply given size, composition, shape and cohesion.
Only the first two are directly represented by the database fields. The third requires additional physical data and a reasoned analysis.
A concise decision framework
| If your task is… | Start with… | Then do… |
|---|---|---|
| Check one named asteroid | LCDB search | Resolve the same identifier in SBDB; read U code and the cited paper. |
| Find many objects below a period threshold | SBDB query with rot_per |
Export identities, deduplicate, then verify each row in LCDB. |
| Decide whether a short period is publishable as confirmed | LCDB U code and source paper | Look for cadence gaps, aliases and later dense follow-up. |
| Compare catalog coverage | Versioned LCDB records | Keep v3.0 and v4.0 counts and dates separate. |
What a careful conclusion looks like
A defensible report might say: “SBDB returned a synodic period of 1.84 hours for the object identified by its number and provisional designation. The LCDB entry lists the same period with U=2 and cites a lightcurve study reporting incomplete coverage. We therefore classify it as a super-fast-rotator candidate, not a confirmed secure measurement.”
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1Repair Windows errors before they cause bigger problems2Scan for outdated or missing drivers - takes under a minute3Clear out junk files and repair common Windows errorsIf the LCDB code is U=3 and the observing paper provides adequate coverage with no unresolved aliases, you can state that the object has a secure measured period below 2.2 hours. Keep the database version, access date and paper citation with the claim so another reader can reproduce the identification and understand which record you used.
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