Convert stellar parallax to distance in parsecs, light-years, and AU. Compute absolute magnitude, luminosity, and distance modulus with Gaia-era accuracy.
Stellar parallax is the apparent shift of a nearby star against the background of distant stars as Earth orbits the Sun. It is the most direct method for measuring stellar distances and the foundation of the cosmic distance ladder.
This calculator converts between parallax angle (in arcseconds) and distance (in parsecs, light-years, and AU) using the fundamental relation d = 1/p. It also computes the distance modulus, absolute magnitude, and luminosity relative to the Sun from the apparent magnitude.
The Gaia space telescope has measured parallaxes for nearly two billion stars with micro-arcsecond precision, revolutionizing stellar astrophysics. This tool includes a reference table of well-known stars with their parallaxes and distances. Preset buttons let you quickly explore Proxima Centauri, Sirius, Betelgeuse, and other famous stars.
Parallax is limited to relatively nearby stars (within ~10,000 pc for Gaia). Beyond that, other distance indicators (Cepheids, Type Ia supernovae) take over, but they are all ultimately calibrated by parallax measurements.
Parallax is the gold standard for astronomical distance measurement. This calculator makes it easy to convert between parallax angles, parsecs, and light-years, and to derive luminosity from apparent magnitude.
It is useful for astronomy students, amateur observers, and anyone working with stellar catalogs and distance data. It keeps the angle-to-distance relationship visible alongside the derived magnitude values so you can compare nearby stars without switching between references.
d = 1/p (distance in parsecs when p in arcseconds). 1 pc = 3.2616 ly = 206,265 AU = 3.086×10¹³ km. Distance modulus: µ = 5·log₁₀(d) − 5. Absolute magnitude: M = m − µ. Luminosity: L/L☉ = 10^((4.83−M)/2.5).
Result: d = 1.30 pc = 4.24 ly, M = 15.5, L = 0.0017 L☉
For Proxima Centauri: d = 1/0.7687 = 1.30 pc = 4.24 ly. µ = 5·log₁₀(1.30) − 5 = −4.37. M = 11.13 − (−4.37) = 15.5. It is a dim red dwarf with L ≈ 0.17% of the Sun.
Small parallaxes translate into large distances, so the input precision matters. A tiny angular error can move a star noticeably in or out on the distance scale, which is why astrometric catalogs report uncertainties alongside the measured angle.
Parallax anchors the first rung of the distance ladder. Once you move beyond the local neighborhood, parallax becomes too small to measure directly and other methods take over, but those secondary methods are still calibrated from parallax-based distances.
Use this calculator when comparing catalog values, checking derived absolute magnitude, or sanity-checking a published distance. The useful output is not just the parsec value itself, but the chain from angle to magnitude to luminosity.
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A parsec (parallax arcsecond) is the distance at which a star has a parallax angle of 1 arcsecond. It equals 3.26 light-years or 206,265 AU or 3.086×10¹³ km.
Gaia measures parallaxes to ~20 micro-arcseconds for bright stars and ~100 µas for fainter stars. This gives 1% distance accuracy out to ~5,000 parsecs.
The parallax angle decreases as 1/d. At large distances, the angle becomes smaller than the measurement error. Hipparcos was limited to ~100 pc; Gaia extends this to ~10,000 pc.
Parallax calibrates the first rung. Cepheid variables (calibrated by parallax) reach to nearby galaxies. Type Ia supernovae (calibrated by Cepheids) reach cosmological distances. Each rung bootstraps the next.
Apparent magnitude (m) is how bright a star looks from Earth. Absolute magnitude (M) is how bright it would look from 10 parsecs — a standard distance for fair comparison.
The standard baseline is 1 AU (Earth-Sun distance). In 6 months, Earth moves 2 AU, producing the maximum parallax angle. Space telescopes like Gaia use the same baseline but with far better angular resolution.