When is the best time to observe Delta Canis Minoris?

Delta 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 Delta Canis Minoris located in the sky?

Delta Canis Minoris lies in the constellation Canis Minor at right ascension 07h 34m and declination +03° 22′.

What telescope do I need to split Delta Canis Minoris?

Splitting Delta Canis Minoris requires an aperture of roughly 60 mm or larger — the components are separated by about 72.9″ at magnitudes near 5.8. The companion is about 5.0 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

Delta Canis Minoris — Double Star in Canis Minor

HIP 36812; Delta3 Canis Minoris; 9 Canis Minoris

Magnitude 5.8^m DoubleStar Canis Minor (CMi) Visible

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Observe

1Physical Properties

Magnitude 5.81

Spectral Type A0Vnn

Star Color Blue-white (B-V -0.02)

2Position & Identifiers

RA 07h 34m 15.8s

Dec +03° 22' 17.0"

Constellation Canis Minor (CMi)

HR 2901

HIP 36812

HD 60357

SAO 115644

Bayer Delta3

Flamsteed 9 CMi

SIMBAD Wikipedia

3How easy to split?

Primary 5.8 mag Companion 10.8 mag Separation 72.9″

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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 Triple

Components 3 (triple)

Component IDs AB

Separation 72.9″

Companion Mag 10.8

Position Angle 112°

Star Colors A: Blue-white

Discoverer J 2835

Separation over time

Measured 1945 → 2000 (55 y)

Separation drift 100.0" → 72.9" (-27.10")

Rate -0.4927" / y

PA drift 110° → 112° (+2°, +0.036°/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.