When is the best time to observe Gamma Piscis Austrini?

Gamma Piscis Austrini is best observed from July through September, with peak visibility during August when it transits around midnight in the Northern Hemisphere.

Where is Gamma Piscis Austrini located in the sky?

Gamma Piscis Austrini lies in the constellation Piscis Austrinus at right ascension 22h 53m and declination -32° 53′.

What telescope do I need to split Gamma Piscis Austrini?

Splitting Gamma Piscis Austrini requires an aperture of roughly 100 mm or larger — the components are separated by about 4.1″ at magnitudes near 4.5. The companion is about 3.7 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

Gamma Piscis Austrini — Double Star in Piscis Austrinus

Observable Double Star Good (59/100)

Sep: 4.1", Companion: mag 8.2

Magnitude 4.5^m DoubleStar Piscis Austrinus (PsA) Visible

Star Map + List + Plan

Observe

1Physical Properties

Magnitude 4.46

Spectral Type A0III* giant

Star Color Blue-white (B-V -0.04)

Distance 76 ly

2Position & Identifiers

RA 22h 52m 31.6s

Dec -32° 52' 32.0"

Constellation Piscis Austrinus (PsA)

HR 8695

HIP 112948

HD 216336

SAO 214153

Bayer Gamma

Flamsteed 22 PsA

SIMBAD

3How easy to split?

Primary 4.5 mag Companion 8.2 mag Separation 4.1″

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Telescope	Bortle 3	Bortle 4	Bortle 5
80 mm refractor 80mm refr.	Hard	Hard	Hard
150 mm Newton 150mm Newt.	Medium+	Medium+	Medium+
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 Jul – Sep (peak: Aug)

5Multiple Star System

Separation 4.1″

Companion Mag 8.2

Position Angle 255°

Star Colors A: Blue-white B: Yellow

Discoverer HJ 5367

Notes

Binary, companion F5V.

Separation over time

Measured 1834 → 2016 (182 y)

Separation drift 2.5" → 4.1" (+1.60")

Rate +0.0088" / y

PA drift 275° → 255° (-20°, -0.110°/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.