When is the best time to observe Xi Pavonis?

Xi Pavonis is best observed from May through July, with peak visibility during June when it transits around midnight in the Northern Hemisphere.

Where is Xi Pavonis located in the sky?

Xi Pavonis lies in the constellation Pavo at right ascension 18h 23m and declination -61° 30′.

What telescope do I need to split Xi Pavonis?

Splitting Xi Pavonis requires an aperture of roughly 100 mm or larger — the components are separated by about 3.7″ at magnitudes near 4.4. 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.

Xi Pavonis — Double Star in Pavo

Observable Double Star Excellent (60/100)

Sep: 3.7", Companion: mag 8.1

Magnitude 4.4^m DoubleStar Pavo (Pav) Visible

Star Map + List + Plan

Observe

1Physical Properties

Magnitude 4.36

Range 4.35 - 4.38

Variable Type Slow Irregular Variable

Spectral Type K4III giant

Star Color Red (B-V 1.48)

Distance 204 ly

2Position & Identifiers

RA 18h 23m 13.6s

Dec -61° 29' 38.0"

Constellation Pavo (Pav)

HR 6855

HIP 90098

HD 168339

SAO 254226

Bayer Xi

SIMBAD

3How easy to split?

Primary 4.4 mag Companion 8.1 mag Separation 3.7″

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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 May – Jul (peak: Jun)

5Multiple Star System Triple

Components 3 (triple)

Component IDs AB

Separation 3.7″

Companion Mag 8.1

Position Angle 159°

Star Colors A: Red

Discoverer GLE 2

Notes

Primary of visual double and a suspected astrometric binary.

Separation over time

Measured 1894 → 2016 (122 y)

Separation drift 4.0" → 3.7" (-0.30")

Rate -0.0025" / y

PA drift 140° → 159° (+19°, +0.156°/y)

Essentially fixed on human timescales — the same view your grandchildren will see.

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.