When is the best time to observe 52 Sagittarii?

52 Sagittarii is best observed from June through August, with peak visibility during July when it transits around midnight in the Northern Hemisphere.

Where is 52 Sagittarii located in the sky?

52 Sagittarii lies in the constellation Sagittarius at right ascension 19h 37m and declination -24° 53′.

What telescope do I need to split 52 Sagittarii?

Splitting 52 Sagittarii requires an aperture of roughly 280 mm or larger — the components are separated by about 2.3″ at magnitudes near 4.6. The companion is about 4.6 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

52 Sagittarii — Double Star in Sagittarius

Magnitude 4.6^m DoubleStar Sagittarius (Sgr) Visible

Star Map + List + Plan

Observe

1Physical Properties

Magnitude 4.60

Spectral Type B9

Star Color Blue-white (B-V -0.07)

Distance 1,631 ly

2Position & Identifiers

RA 19h 36m 42.4s

Dec -24° 53' 01.0"

Constellation Sagittarius (Sgr)

HR 7440

HIP 96465

HD 184707

SAO 188337

Flamsteed 52 Sgr

Double Cat 12654

SIMBAD

3How easy to split?

Primary 4.6 mag Companion 9.2 mag Separation 2.3″

Sign in and configure your equipment and default location to see a personalized row.

Telescope	Bortle 3	Bortle 4	Bortle 5
80 mm refractor 80mm refr.	V. hard	V. hard	V. hard
150 mm Newton 150mm Newt.	Hard	Hard	Hard
Celestron C8 (203 mm SCT) C8 203mm	Hard	Hard	Hard

Easy Medium Hard Very hard Impossible

Bortle 3 = rural · 4 = outer suburbs · 5 = suburbs

To reach "Medium" at Bortle 3, you'd need at least a 280 mm reflector.

4Visibility

Set a location in User Settings to see visibility data.

Best season Jun – Aug (peak: Jul)

5Multiple Star System

Separation 2.3″

Companion Mag 9.2

Position Angle 175°

Star Colors A: Blue-white B: Yellow

Discoverer BU 654

Notes

CPM.

Separation over time

Measured 1878 → 2016 (138 y)

Separation drift 2.9" → 2.3" (-0.60")

Rate -0.0043" / y

PA drift 161° → 175° (+14°, +0.101°/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.