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Start with the Asteroid Lightcurve Database (LCDB) for published rotation periods, then use NASA/JPL’s Small-Body Database (SBDB) to confirm that the record belongs to the object you intend to study. For a single asteroid, search the LCDB by its number or designation, read the period and its U reliability code, and verify the identity in SBDB. For a list of candidates, query SBDB for the rot_per field, filter the returned periods, and then inspect each candidate’s LCDB record and observing paper. Treat a period below 2.2 hours as a screening signal—not proof by itself—that an asteroid is a securely measured super-fast rotator.
What each database is for
No single catalog answers every question about a rapidly rotating asteroid. The two services have different jobs, and using them in the right order prevents identity mistakes and overconfident claims.
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LCDB: the literature record for rotation
The Asteroid Lightcurve Database is the primary literature compilation for published asteroid lightcurves and rotation periods. Its records can include a preferred period, lightcurve amplitude, period-quality information, notes and citations to the observations. The NASA Planetary Data System archive for LCDB version 4.0 describes 34,967 targets; that archive’s data context ends on 2021-09-02. This is a versioned archive, not a promise that every asteroid observed since that date appears in it.
NASA’s Open Data Portal also has a separate LCDB version 3.0 catalog record describing more than 24,500 targets. That catalog record shows an update date of July 17, 2025. The v3.0 count and the v4.0 archive count come from different version records and dates, so they must not be combined into one current total.
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SBDB: identity, orbit and cross-checking
NASA/JPL’s Small-Body Database resolves an object’s identity and supplies orbital and selected physical parameters when those fields are available. Its lookup accepts an IAU number, provisional designation, name or SPK-ID. This makes it the place to check whether two differently formatted designations refer to the same body before you copy a period into a spreadsheet or article.
JPL describes its service in the official API documentation as follows: “The SBDB (Small-Body DataBase) API provides a method of requesting machine-readable data for a specified small body within JPL’s SSD/CNEOS Small-Body DataBase (SBDB).” SBDB is not a replacement for the LCDB’s literature-quality context. Some objects have sparse or no physical-parameter fields, and a missing SBDB value does not prove that no period has ever been reported.
Find one asteroid’s published rotation period
Use this path when you already know the object’s number, name or provisional designation.
- Collect the exact identifier. Start with the designation used in the observing paper, if you have it. A numbered asteroid, provisional designation and name may all be valid ways to identify the same body, but punctuation, spaces and year codes can affect a database search.
- Search the LCDB interface. Enter the numbered name or provisional designation. If a name returns several possibilities or no result, retry with the designation exactly as printed in the source paper. Keep the search string in your notes so another reader can reproduce it.
- Read the preferred period and units. Record the period in hours exactly as displayed, along with any alternate period solution, amplitude, notes and citation. Do not silently convert a value from hours to minutes or days without preserving the original value and conversion.
- Capture the U reliability code. The code is a compact assessment of the evidence behind the period. It is a judgment aid, not a substitute for examining the observations. Record subclasses such as 2− or 2+ rather than reducing every value to a single integer.
- Resolve the object in SBDB. Open the JPL lookup using the number, designation, name or SPK-ID. Compare the returned designation and name with the LCDB record. Check the orbit and any available physical parameters for context, but do not infer that an absent field contradicts the LCDB.
- Inspect the cited paper when the period matters. A very short period, a surprising result or a value you plan to publish deserves a look at the underlying lightcurve study. Confirm whether the authors report a secure rotation solution, an alias, a double-peaked interpretation or unresolved alternatives.
Build a candidate list with SBDB queries
Opening thousands of object pages manually is inefficient. JPL’s SBDB query tools can request information for sets of small bodies and include the rotation-period field rot_per. JPL documents rot_per as the body’s synodic rotation period in hours.
Filter by a period range
- Choose the screening boundary. For a super-fast-rotator search, begin with periods below 2.2 hours. You can use a narrower range, such as below 2 hours, if your project requires it, but state that choice in the methods record.
- Request identity fields with
rot_per. Include the object number, provisional designation and name where the query tool permits. Identity columns are essential because a period without a stable designation is difficult to audit. - Export the returned rows. Preserve the query date, requested fields and any filters. A result set is a snapshot; later database revisions can add, remove or revise values.
- Separate missing and non-numeric values. Do not treat a blank
rot_peras zero, unknown-but-fast or evidence of a long period. Keep missing values in a separate status column. - Open each candidate in SBDB lookup. Verify that the designation, name and SPK-ID remain consistent. Check orbital and physical fields that may help you distinguish similarly named records.
- Match every candidate to LCDB. Locate the corresponding LCDB entry, copy its preferred period and U code, and compare the two values. If SBDB and LCDB differ, retain both reported values until the source papers explain the discrepancy.
SBDB’s query result is therefore a discovery and filtering tool. LCDB and the cited observing work supply the evidence needed to decide whether a short value is reliable.
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What “fast-spinning” means
A period under 2.2 hours is a commonly used threshold for a super-fast asteroid. The number is associated with the approximate spin barrier for many larger, gravity-bound rubble-pile bodies: if such a body rotates faster, gravity alone may not be sufficient to keep loose material together.
That interpretation has limits. Smaller asteroids can rotate faster because material strength or internal cohesion can contribute to structural support. Composition, size, shape, porosity and measurement uncertainty also affect what a period means physically. The 2.2-hour value is consequently a screening convention, not a universal classification that proves an asteroid’s internal structure.
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Use precise language in your records. “The database lists a synodic period of 2.05 hours” is a measurement statement. “The object is a confirmed super-fast rotator” is a stronger conclusion that requires a reliable period determination and, when the claim is consequential, review of the observing paper.
Understand the LCDB U reliability code
The U code summarizes how confidently the lightcurve evidence supports the listed period. It should travel with the number whenever you copy a result.
| Code | Meaning | How to use it |
|---|---|---|
| U=1 | Based on fragmentary lightcurve data; the result might be wrong. | Use as a lead only. Do not present the period as secure without independent evidence. |
| U=2 | Ambiguity remains, or coverage is more than half but still incomplete. | Report the value as uncertain and check alternate solutions and the source paper. |
| U=3 | Secure result. | Suitable for a confident database summary, while still retaining the citation and units. |
| 2− or 2+ | Modified subclasses that refine the subjective assessment around U=2. | Preserve the modifier; do not collapse it to an unqualified “2.” |
The code is not an independent reanalysis of the photometry. It reflects the compiler’s assessment of the published evidence. Two records with the same numerical period can therefore deserve different wording if their U codes differ.
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Why very short periods can be aliases
Rotation is inferred from repeating brightness changes. If observations are separated by long gaps or taken at an insufficient cadence, the number of completed cycles between lightcurves may be ambiguous. Several periods can then fit the available data, and a mathematically plausible short period may be an alias rather than the asteroid’s true rotation.
A 2025 study of super-fast-rotator candidates highlighted this problem: inadequate observing cadence produced aliases, while dense photometric follow-up reclassified some candidates and confirmed others. This is why a period below 2.2 hours should remain a candidate status until the cadence, lightcurve coverage and reliability assessment support it.
Warning signs in a record
- The U code is 1 or 2, especially when the period is far below 2.2 hours.
- The record lists multiple periods or notes an ambiguity.
- The source observations contain large time gaps between lightcurves.
- The period appears only in a secondary catalog and cannot be traced to a cited observing paper.
- SBDB and LCDB show different values and no explanation has been checked in the literature.
Track a project without losing provenance
A fast-rotator list becomes unreliable when identifiers, versions and citations are stripped away. Use one row per object and retain the following fields:
- Object number, provisional designation, name and, when available, SPK-ID.
- LCDB version or archive label used, plus the date you accessed it.
- Preferred synodic period and units; keep alternate solutions in a separate column.
- LCDB U code, including any 2− or 2+ modifier.
- Lightcurve amplitude if supplied, with the database’s notes.
- SBDB query date, requested fields and filter range.
- Underlying observing-paper citation and a link or identifier stored exactly as published in your own bibliography.
- Status such as candidate, ambiguous or secure, with the reason for that status.
Version and date details matter because the available records are not a single continuously updated count. The LCDB v4.0 archive’s 34,967-target context ends on 2021-09-02, while the separate v3.0 catalog record reports more than 24,500 targets and was updated in the portal on July 17, 2025. State which record you used instead of calling either number “the current LCDB total.”
How to report a candidate responsibly
For a database-only note
Use wording such as: “SBDB returned a rot_per value of 1.9 hours for [object designation]. The corresponding LCDB record lists 1.9 hours with U=2; the object is treated here as a super-fast-rotator candidate.” This separates the database observation from your interpretation.
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For a secure result
When the LCDB code is U=3 and the cited paper supports the solution, identify the object, period, units, U code, database version or access date and paper citation. Explain that the 2.2-hour threshold is a conventional screening boundary and does not by itself establish composition or internal strength.
For conflicting values
Report the competing periods rather than selecting the shorter one because it better fits your hypothesis. Identify which value LCDB marks as preferred, note the U codes, and consult the observing papers for aliases, harmonics or later revisions.
Independent reader supportYour contribution helps us test, update, and keep practical guides available for everyone.Common mistakes and fixes
Mixing database versions
Mistake: Adding the v3.0 “more than 24,500” figure to the v4.0 “34,967” figure or presenting one as a 2025 update of the other.
Fix: Name the version, archive or catalog record and its date context beside every count.
Using SBDB as a quality grade
Mistake: Treating a populated rot_per field as proof that the period is secure.
Fix: Use SBDB for identity and filtering, then read the LCDB U code and source paper.
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Mistake: Inferring that a short period proves a body is cohesive or that it should disrupt.
Fix: Explain the rubble-pile spin-barrier context and qualify the roles of size, composition, cohesion, shape and uncertainty.
Ignoring aliases
Mistake: Publishing a dramatic period from sparse observations without checking cadence.
Fix: Look for alternate solutions, gaps between lightcurves and follow-up photometry; retain candidate wording until ambiguity is resolved.
Dropping the identifier
Mistake: Saving only a name or only a period in a spreadsheet.
Fix: Preserve number, provisional designation, name and SPK-ID when available, and verify them in SBDB before merging records.
A repeatable decision workflow
- Discover: Query SBDB for
rot_perwhen you need a set of objects, or search LCDB directly when you already know the asteroid. - Screen: Mark periods below 2.2 hours as candidates for review, not automatic confirmations.
- Identify: Resolve each object in SBDB using its number, designation, name or SPK-ID.
- Verify: Match the object to LCDB and copy the preferred period, U code, notes and citation.
- Investigate: Read the underlying observing paper for short, disputed or consequential periods, paying attention to cadence and aliases.
- Classify: Label the row candidate, ambiguous or secure according to the evidence you actually reviewed.
- Publish: Include the period, units, identifier, reliability code, database version or access date and paper citation.
This division of labor keeps the fast search efficient while preserving the caution needed for scientific interpretation: SBDB finds and identifies records; LCDB supplies the compiled lightcurve result and its quality context; the original paper determines how strongly you can state the conclusion.
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Can I find a rotation period in SBDB without opening LCDB?
SBDB may provide a rot_per value, but it does not replace LCDB’s reliability code and literature context. Use LCDB to assess how secure the period is.
Does a period below 2.2 hours prove an asteroid is made of solid rock?
No. The threshold is a screening convention tied mainly to larger gravity-bound rubble piles. Size, cohesion, composition, shape and measurement uncertainty all affect the interpretation.
What should I do when LCDB and SBDB list different periods?
Preserve both values, compare the preferred LCDB entry and U codes, and consult the cited observing papers for aliases, harmonics or later revisions before choosing wording.
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