When is the best time to observe Jabbah?

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

Where is Jabbah located in the sky?

Jabbah lies in the constellation Scorpius at right ascension 16h 12m and declination -19° 28′.

What telescope do I need to split Jabbah?

Splitting Jabbah requires an aperture of roughly 60 mm or larger — the components are separated by about 41.4″ at magnitudes near 4.0. Larger apertures and steady seeing help resolve the pair cleanly.

Jabbah — Double Star in Scorpius

HIP 79374; Nu Scorpii; 14 Scorpii

Observable Double Star Good (58/100)

Sep: 41.4", Companion: mag 6.6

Magnitude 4.0^m DoubleStar Scorpius (Sco) Visible

Star Map + List + Plan

Observe

1Physical Properties

Magnitude 4.01

Spectral Type B3V

Star Color Blue (B-V 0.04)

Distance 109 ly

2Position & Identifiers

RA 16h 11m 59.7s

Dec -19° 27' 38.0"

Constellation Scorpius (Sco)

HR 6027

HIP 79374

HD 145502

SAO 159764

Bayer Nu

Flamsteed 14 Sco

Double Cat 9951

SIMBAD Wikipedia

3How easy to split?

Primary 4.0 mag Companion 6.6 mag Separation 41.4″

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Telescope	Bortle 3	Bortle 4	Bortle 5
80 mm refractor 80mm refr.	Easy	Easy	Easy
150 mm Newton 150mm Newt.	Easy	Easy	Easy
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 Apr – Jun (peak: May)

5Multiple Star System Quintuple E: optical

Components 5 (quintuple)

Component IDs AC

Separation 41.4″

Companion Mag 6.6

Position Angle 336°

Star Colors A: Blue C: White

Discoverer H 5 6

Notes

ADS 9951A is SB, 4.9, 6.9v, sep. 0.0003". AB, binary. Component B, 6.9v at 1". Components CD at 41" = HR 6026, q.v. | HR 6026, q.v.

Separation over time

Measured 1777 → 2021 (244 y)

Separation drift 42.0" → 41.4" (-0.60")

Rate -0.0025" / y

PA drift 335° → 336° (+1°, +0.004°/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.