When is the best time to observe Gamma Velorum?

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

Where is Gamma Velorum located in the sky?

Gamma Velorum lies in the constellation Vela at right ascension 08h 09m and declination -47° 21′.

What telescope do I need to split Gamma Velorum?

Splitting Gamma Velorum requires an aperture of roughly 60 mm or larger — the components are separated by about 60.9″ at magnitudes near 4.3. Larger apertures and steady seeing help resolve the pair cleanly.

Gamma Velorum — Double Star in Vela

HIP 39953; Gamma1 Velorum

Observable Double Star Good (52/100)

Sep: 60.9", Companion: mag 7.3

DoubleStar Vela (Vel) Visible

Star Map + List + Plan

Observe

1Physical Properties

Magnitude 4.27

Spectral Type B1IV

Star Color Blue (B-V -0.23)

2Position & Identifiers

RA 08h 09m 29.3s

Dec -47° 20' 45.0"

Constellation Vela (Vel)

HR 3206

HIP 39953

HD 68273

Bayer Gamma1

SIMBAD Wikipedia

3How easy to split?

Primary 4.3 mag Companion 7.3 mag Separation 60.9″

Sign in and configure your equipment and default location to see a personalized row.

Telescope	Bortle 3	Bortle 4	Bortle 5
80 mm refractor 80mm refr.	Easy	Easy	Easy
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

Set a location in User Settings to see visibility data.

Best season Dec – Feb (peak: Jan)

5Multiple Star System Quintuple

Components 5 (quintuple)

Component IDs AB

Separation 60.9″

Companion Mag 7.3

Companion Sp O9I

Position Angle 113°

Star Colors A: Blue B: Blue

Discoverer DUN 65

Notes

Component B of 5 stars within 2' of HR 3207.

Separation over time

Measured 1846 → 2015 (169 y)

Separation drift 61.5" → 60.9" (-0.60")

Rate -0.0036" / y

PA drift 112° → 113° (+1°, +0.006°/y)

Slow change over generations — observable in lifetime comparisons.

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.