Relative Parallax to Absolute Correction Adder
Add independently measured field relative-to-absolute correction, preserving nonpositive results; distinct from subtraction of catalog source zero point, no distance inversion. Caller independently establishes frames, units, epoch, covariance and instrument context; not an identity, association or astrometric quality certification.
Description
An absolute-parallax correction adjusts a relative parallax under a calibrated reference frame.
An absolute-parallax correction adjusts a relative parallax under a calibrated reference frame.1
Addition alone does not derive the correction or infer distance. Use Relative Parallax to Absolute Correction Adder to evaluate the supplied inputs under the model explained below.
When to use Relative Parallax to Absolute Correction Adder
Use Relative Parallax to Absolute Correction Adder to evaluate the supplied inputs under the model explained below. Establish the units, measurement scope and model assumptions before entering values.
How to use Relative Parallax to Absolute Correction Adder and understand its results
- Establish the units, measurement scope and model assumptions before entering values.
- Enter Relative parallax mas, Independently calibrated absolute correction mas using the field table and validation rules below, then run the tool.
- Read Corrected absolute parallax mas; interpret the units, signs, ordering and unknown-value placeholders described below.
- Correct reported input errors and rerun. Apply successful results according to their specific meanings and check the assumptions before using them in a decision.
| Input field | Meaning | Value type | Requirement |
|---|---|---|---|
| relativeParallaxMas | Relative parallax mas | number | Required; constraints below |
| independentlyCalibratedAbsoluteCorrectionMas | Independently calibrated absolute correction mas | number | Required; constraints below |
Enter finite relative parallax and independently calibrated correction in mas. Add them, preserving sign. No positive-parallax requirement, correction catalog or distance estimate is provided.
absoluteParallaxMas=relativeMas+callerCorrectionMas Use the field order, units and branch conditions described above.
| Output field | Meaning | Value type |
|---|---|---|
| correctedAbsoluteParallaxMas | Corrected absolute parallax mas | number |
{
"input": {
"relativeParallaxMas": -1,
"independentlyCalibratedAbsoluteCorrectionMas": 0.2
},
"output": {
"correctedAbsoluteParallaxMas": -0.8
}
}Limitations and assumptions
Addition alone does not derive the correction or infer distance. Apply the exact scope and assumptions explained above.
All listed fields require explicit values. Unexpected fields, incorrect types, nonfinite numbers and sparse arrays fail validation. Domain-specific bounds, alignments and supported tokens are explained above; extremely large inputs or outputs can also be rejected. Input errors differ from successful false results, empty match lists and unknown-evidence placeholders.
Alternative or Complementary methods
Use Spectroscopic Photometric Parallax Cross-Check Delta Calculator for a related task: Comparing two parallax estimates needs an independently established uncertainty for their difference.
Use Peculiar Velocity versus Local Standard of Rest Residual Calculator for a related task: A local-standard-of-rest comparison requires consistent UVW axes and solar-motion conventions.
References
Similar or alternative tools
- Spectroscopic Photometric Parallax Cross-Check Delta Calculator
Comparing two parallax estimates needs an independently established uncertainty for their difference.
- Peculiar Velocity versus Local Standard of Rest Residual Calculator
A local-standard-of-rest comparison requires consistent UVW axes and solar-motion conventions.