When is the best time to observe Kappa Apodis?

Kappa Apodis is best observed from April through June, with peak visibility during May when it transits around midnight in the Northern Hemisphere.

Where is Kappa Apodis located in the sky?

Kappa Apodis lies in the constellation Apus at right ascension 15h 32m and declination -73° 23′.

What telescope do I need to split Kappa Apodis?

Splitting Kappa Apodis requires an aperture of roughly 60 mm or larger — the components are separated by about 27.4″ at magnitudes near 5.5. The companion is about 5.8 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

Kappa Apodis — Double Star in Apus

HIP 76013; Kappa1 Apodis

Magnitude 5.4–5.6^m DoubleStar Apus (Aps) Visible

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1Physical Properties

Magnitude 5.49

Range 5.34 - 5.61

Variable Type Gamma Cassiopeiae (Eruptive Be Star)

Spectral Type B3IVe supergiant

Star Color Blue-white (B-V -0.12)

2Position & Identifiers

RA 15h 31m 30.8s

Dec -73° 23' 22.0"

Constellation Apus (Aps)

HR 5730

HIP 76013

HD 137387

SAO 257289

Bayer Kappa1

Variable ID Kap1 Aps

SIMBAD Wikipedia

3How easy to split?

Primary 5.5 mag Companion 11.3 mag Separation 27.4″

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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

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Best season Apr – Jun (peak: May)

5Multiple Star System

Separation 27.4″

Companion Mag 11.3

Position Angle 255°

Star Colors A: Blue-white

Discoverer HJ 4764

Notes

Companion K5IV.

Separation over time

Measured 1835 → 2015 (180 y)

Separation drift 25.0" → 27.4" (+2.40")

Rate +0.0133" / y

PA drift 249° → 255° (+6°, +0.033°/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.