When is the best time to observe Eta Antliae?

Eta Antliae is best observed from January through March, with peak visibility during February when it transits around midnight in the Northern Hemisphere.

Where is Eta Antliae located in the sky?

Eta Antliae lies in the constellation Antlia at right ascension 09h 59m and declination -35° 53′.

What telescope do I need to split Eta Antliae?

Splitting Eta Antliae requires an aperture of roughly 60 mm or larger — the components are separated by about 31.2″ at magnitudes near 5.2. The companion is about 6.1 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

Eta Antliae — Double Star in Antlia

Magnitude 5.2^m DoubleStar Antlia (Ant) Visible

Star Map + List + Plan Star Hop

Observe

1Physical Properties

Magnitude 5.23

Spectral Type F1III-IV giant

Star Color Yellow-white (B-V 0.31)

Distance 112 ly

2Position & Identifiers

RA 09h 58m 52.3s

Dec -35° 53' 28.0"

Constellation Antlia (Ant)

HR 3947

HIP 48926

HD 86629

SAO 200926

Bayer Eta

SIMBAD

3How easy to split?

Primary 5.2 mag Companion 11.3 mag Separation 31.2″

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.	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

Set a location in User Settings to see visibility data.

Best season Jan – Mar (peak: Feb)

5Multiple Star System

Separation 31.2″

Companion Mag 11.3

Position Angle 319°

Star Colors A: Yellow-white

Discoverer HJ 4271

Notes

CPM.

Separation over time

Measured 1836 → 2016 (180 y)

Separation drift 27.5" → 31.2" (+3.70")

Rate +0.0206" / y

PA drift 313° → 319° (+6°, +0.033°/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.