When is the best time to observe V915 Scorpii?

V915 Scorpii is best observed from May through July, with peak visibility during June when it transits around midnight in the Northern Hemisphere.

Where is V915 Scorpii located in the sky?

V915 Scorpii lies in the constellation Scorpius at right ascension 17h 14m and declination -39° 46′.

What telescope do I need to split V915 Scorpii?

Splitting V915 Scorpii requires an aperture of roughly 60 mm or larger — the components are separated by about 13.8″ at magnitudes near 6.6. The companion is about 3.5 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

V915 Scorpii — Double Star in Scorpius

Magnitude 6.2–6.6^m DoubleStar Scorpius (Sco) Visible

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Observe

1Physical Properties

Magnitude 6.60

Range 6.22 - 6.64

Variable Type Semi-Regular Variable (F-K Giant)

Spectral Type G5Ia supergiant

Star Color Deep ruby red (B-V 2.21)

2Position & Identifiers

RA 17h 14m 27.7s

Dec -39° 46' 01.0"

Constellation Scorpius (Sco)

HR 6392

HIP 84332

HD 155603

SAO 208569

Variable ID V915 Sco

SIMBAD

3How easy to split?

Primary 6.6 mag Companion 10.1 mag Separation 13.8″

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Telescope	Bortle 3	Bortle 4	Bortle 5
80 mm refractor 80mm refr.	Medium+	Medium	Hard+
150 mm Newton 150mm Newt.	Easy	Easy	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 13.8″

Companion Mag 10.1

Position Angle 335°

Star Colors A: Red

Discoverer HJ 4926

Notes

Component B, 10.42V, +0.52(B-V); component C, 11.40V, +1.55(B-V).

Separation over time

Measured 1835 → 2013 (178 y)

Separation drift 11.0" → 13.8" (+2.80")

Rate +0.0157" / y

PA drift 334° → 335° (+1°, +0.006°/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.