When is the best time to observe Gamma Canis Minoris?

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

Where is Gamma Canis Minoris located in the sky?

Gamma Canis Minoris lies in the constellation Canis Minor at right ascension 07h 28m and declination +08° 56′.

What telescope do I need to split Gamma Canis Minoris?

Splitting Gamma Canis Minoris requires an aperture of roughly 60 mm or larger — the components are separated by about 138.2″ at magnitudes near 4.3. The companion is about 6.4 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

Gamma Canis Minoris — Double Star in Canis Minor

DoubleStar Canis Minor (CMi) Visible

Star Map + List + Plan

Observe

1Physical Properties

Magnitude 4.32

Spectral Type K3-IIIFe-0.5

Star Color Red (B-V 1.43)

Distance 172 ly

2Position & Identifiers

RA 07h 28m 09.8s

Dec +08° 55' 32.0"

Constellation Canis Minor (CMi)

HR 2854

HIP 36284

HD 58972

Bayer Gamma

Flamsteed 4 CMi

Double Cat 6100

SIMBAD

3How easy to split?

Primary 4.3 mag Companion 10.8 mag Separation 138.2″

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Telescope	Bortle 3	Bortle 4	Bortle 5
80 mm refractor 80mm refr.	Medium	Hard+	Hard
150 mm Newton 150mm Newt.	Medium+	Medium+	Medium
Celestron C8 (203 mm SCT) C8 203mm	Easy	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 Quadruple D: optical

Components 4 (quadruple)

Component IDs AD

Separation 138.2″

Companion Mag 10.8

Position Angle 290°

Star Colors A: Red

Discoverer WAL 52

Separation over time

Measured 1944 → 2006 (62 y)

Separation drift 130.0" → 138.2" (+8.20")

Rate +0.1323" / y

PA drift 305° → 290° (-15°, -0.242°/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.