When is the best time to observe Pi Geminorum?

Pi Geminorum is best observed from December through February, with peak visibility during January when it transits around midnight in the Northern Hemisphere.

Where is Pi Geminorum located in the sky?

Pi Geminorum lies in the constellation Gemini at right ascension 07h 48m and declination +33° 25′.

What telescope do I need to split Pi Geminorum?

Splitting Pi Geminorum requires an aperture of roughly 60 mm or larger — the components are separated by about 19.0″ at magnitudes near 5.1. The companion is about 6.3 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

Pi Geminorum — Double Star in Gemini

Magnitude 5.1^m DoubleStar Gemini (Gem) Visible

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Observe

1Physical Properties

Magnitude 5.14

Spectral Type M1IIIa bright giant

Star Color Red (B-V 1.60)

Distance 272 ly

2Position & Identifiers

RA 07h 47m 30.3s

Dec +33° 24' 56.0"

Constellation Gemini (Gem)

HR 3013

HIP 38016

HD 62898

SAO 60340

Bayer Pi

Flamsteed 80 Gem

Double Cat 6364

SIMBAD

3How easy to split?

Primary 5.1 mag Companion 11.4 mag Separation 19.0″

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Telescope	Bortle 3	Bortle 4	Bortle 5
80 mm refractor 80mm refr.	Hard+	Hard	V. hard+
150 mm Newton 150mm Newt.	Medium+	Medium	Hard+
Celestron C8 (203 mm SCT) C8 203mm	Medium+	Medium+	Medium

Easy Medium Hard Very hard Impossible

Bortle 3 = rural · 4 = outer suburbs · 5 = suburbs

4Visibility

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Best season Dec – Feb (peak: Jan)

5Multiple Star System Triple C: optical

Components 3 (triple)

Component IDs AB

Separation 19.0″

Companion Mag 11.4

Position Angle 215°

Star Colors A: Red

Discoverer STF1135

Notes

C optical. Some disagreement as to which of B and C is the brighter.

Separation over time

Measured 1827 → 2017 (190 y)

Separation drift 25.0" → 19.0" (-6.00")

Rate -0.0316" / y

PA drift 220° → 215° (-5°, -0.026°/y)

Apparent motion is significant on a human timescale — worth revisiting in a decade.

Measured from the WDS observational archive. No orbital solution has been derived — most likely the period is too long to fit an orbit to the available measurement arc.