When is the best time to observe 2 Canum Venaticorum?

2 Canum Venaticorum is best observed from February through April, with peak visibility during March when it transits around midnight in the Northern Hemisphere.

Where is 2 Canum Venaticorum located in the sky?

2 Canum Venaticorum lies in the constellation Canes Venatici at right ascension 12h 16m and declination +40° 40′.

What telescope do I need to split 2 Canum Venaticorum?

Splitting 2 Canum Venaticorum requires an aperture of roughly 60 mm or larger — the components are separated by about 11.6″ at magnitudes near 5.7. The companion is about 3.1 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

2 Canum Venaticorum — Double Star in Canes Venatici

Observable Double Star Excellent (63/100)

Sep: 11.6", Companion: mag 8.7

Magnitude 5.7^m DoubleStar Canes Venatici (CVn) Visible

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Observe

1Physical Properties

Magnitude 5.66

Spectral Type M1III+F7V giant

Star Color Red (B-V 1.55)

Distance 815 ly

2Position & Identifiers

RA 12h 16m 07.6s

Dec +40° 39' 37.0"

Constellation Canes Venatici (CVn)

HR 4666

HIP 59831

HD 106690

SAO 44097

Flamsteed 2 CVn

Double Cat 8489

SIMBAD

3How easy to split?

Primary 5.7 mag Companion 8.7 mag Separation 11.6″

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

Easy Medium Hard Very hard Impossible

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

4Visibility

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Best season Feb – Apr (peak: Mar)

5Multiple Star System

Separation 11.6″

Companion Mag 8.7

Companion Sp F7V

Position Angle 260°

Star Colors A: Red B: Yellow

Discoverer STF1622

Notes

Binary. Companion 8.77V, +0.57(B-V), +0.09(U-B), F7V.

Separation over time

Measured 1782 → 2017 (235 y)

Separation drift 12.2" → 11.6" (-0.60")

Rate -0.0026" / y

PA drift 259° → 260° (+1°, +0.004°/y)

Essentially fixed on human timescales — the same view your grandchildren will see.

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.