Globular Cluster NGC 5466

Object Description

NGC 5466
NGC 5466: Globular cluster in Bootes; 500 mm Cassegrain 3625 mm f/7.2; SBIG STL11K; 175+3*30 min LRGB; Bernese Highlands; © 2015 Radek Chromik

The globular cluster NGC 5466 was discovered on May 17, 1784 by the German-British astronomer Wilhelm Herschel. It is a loose globular cluster of concentration class XII. [196]

Like most globular clusters, NGC 5466 consists of very metal-poor stars, indicating a very high age, estimated at 12.88 billion years. Incidentally, in astrophysics all elements heavier than helium are considered «metals». The globular cluster is located in the galactic halo of our Milky Way, about 16 kpc (about 52'000 light years) from Earth.

In 2005, a tidal tail was discovered emanating from NGC 5466 and extending about 45° across the sky. The orientation of the tidal tail agrees well with the highly elliptical orbit of the globular cluster, which is 6.4 kpc (about 21'000 light-years) at the pericenter and 43 kpc (about 140'000 light-years) at the apocenter from the galactic center. While the inner portion of the globular cluster appears normal, the outer portions are severely deformed, stretching to either side. The brightness of the tidal tail is about 11% of the globular cluster. There is also evidence that the globular cluster had interacted with the galactic disk and lost mass. [212, 335]

NGC 5466
NGC 5466: Proper motion of NGC 5466 over 10 years compared to background galaxies. Images taken with the Hubble Space Telescope. © ESA/Hubble & NASA [210]

Behind the globular cluster is a distant cluster of galaxies. Based on this, recordings from ten years ago could be compared with recordings from the Hubble Space Telescope in order to precisely determine the proper motion of the globular star cluster NGC 5466. This precise measurement combined with other data showed that our Milky Way must have about 1.5 trillion (1.5·1012) solar masses. Only a very small part of this comes from the approximately 200 billion (200·109) stars. Most of the rest is invisible «dark matter». [210]

«Revised NGC/IC», «Historic NGC/IC», Version 2022-09-01, © Dr. Wolfgang Steinicke [277]
DesignationNGC 5466
TypeGCL (XII)
Right Ascension14h 05m 27.3s
Declination+28° 32' 06"
Diameter9 arcmin
Visual magnitude9.2 mag
Metric Distance16.000 Mpc
Dreyer DescriptionCl, L, vRi, vmC, st 11…
Identification, RemarksGCL 27

Finder Chart

The globular cluster NGC 5466 is located in the constellation of Bootes, somewhat in the shadow of the magnificent globular cluster M 3 in Canes Venatici. The best viewing time is December to September.

Bootes: NGC 5466
Chart NGC 5466
Chart created using SkySafari 6 Pro and STScI Digitized Sky Survey. [149, 160]

Visual Observation

400 mm Aperture: In the 21 mm Ethos eyepiece (85x) NGC 5466 presents itself as a very loose globular cluster with many small stars irregularly distributed, which appears as an oval, washed-out spot when seen indirectly. The bright orange star really dazzles here. With increasing magnification (16 mm Nagler, 112x) the disturbing star comes to lie outside the field of view and the fine stars in the globular cluster appear more prominent. In the 11 mm DeLite eyepiece (163x) the view is most brilliant. The globular cluster then looks somewhat like a crab with upstretched claws. — 400 mm f/4.5 Taurus Dobsonian, Glaubenberg, SQM 21.34, a bit windy, Sahara dust and hazy, 22. 5. 2022, 00:00, Bernd Nies

References

149SkySafari 6 Pro, Simulation Curriculum; skysafariastronomy.com
160The STScI Digitized Sky Survey; archive.stsci.edu/cgi-bin/dss_form
196Celestial Atlas by Curtney Seligman; cseligman.com/text/atlas.htm (2020-12-28)
210NGC 5466 Visualization; hubblesite.org/video/1200/news
212«Fossils of the distant Galaxy: NGC 5466 and its stellar stream» Jaclyn Jensen, University of Victoria, 2020; dspace.library.uvic.ca/handle/1828/12440 (2021-05-19)
277«Historische Deep-Sky Kataloge» von Dr. Wolfgang Steinicke; klima-luft.de/steinicke (2021-02-17)
335«The Discovery of Tidal Tails around the Globular Cluster NGC 5466» Belokurov, V.; Evans, N. W.; Irwin, M. J.; Hewett, P. C.; Wilkinson, M. I.; The Astrophysical Journal, Volume 637, Issue 1, pp. L29-L32. January 2006; DOI:10.1086/500362; Bibcode:2006ApJ...637L..29B