Messier 3
| Kugelsternhaufen Messier 3 | |
|---|---|
.jpg) | |
| SDSS-Aufnahme, Bildwinkel 24' × 24' | |
| AladinLite | |
| Sternbild | Jagdhunde |
| Position Äquinoktium: J2000.0, Epoche: J2000.0 | |
| Rektaszension | 13h 42m 11,2s [1] |
| Deklination | +28° 22′ 32″ [1] |
| Erscheinungsbild | |
| Konzentrationsklasse | VI [2] |
| Helligkeit (visuell) | 6,3 mag [3] |
| Winkelausdehnung | 18,0' |
| Physikalische Daten | |
| Zugehörigkeit | Milchstraße |
| Entfernung | 33,9 kLj (10,39 kpc) [4] |
| Durchmesser | 223 Lj |
| Geschichte | |
| Entdeckung | Charles Messier |
| Entdeckungsdatum | 3. Mai 1764 |
| Katalogbezeichnungen | |
| M 3 • NGC 5272 • C 1339+286 • GCl 25 • | |
Messier 3 = NGC 5272 ist ein galaktischer Kugelsternhaufen im Sternbild Jagdhunde am Nordsternhimmel. Er ist rund 34.000 Lichtjahre vom Sonnensystem entfernt, hat einen Durchmesser von etwa 125 Lichtjahren und ist mit einer halben Million Sterne ein sehr großer Kugelsternhaufen[5]. Der Haufen enthält mit 212 veränderlichen Sternen (davon 170 RR Lyrae Sterne) die größte Anzahl dieser Sternklasse in unserer Galaxie. Von 186 Sternen konnte eine Periode bestimmt werden.
Das Objekt wurde am 3. Mai 1764 von Charles Messier entdeckt und von ihm in seinem Katalog als drittes Objekt verzeichnet. Im New General Catalogue (NGC) trägt er die Nummer 5272.[6]
Messier 3 am Nachthimmel
M 3 ist leicht am Nachthimmel zu entdecken. Er ist genau zwischen Arktur im Sternbild Bärenhüter und α (Cor Caroli) aus dem Sternbild Jagdhunde. Messier 3 ist im Frühjahr sichtbar.
Position von Messier 3
Aufnahme mit einem 60-cm-Teleskop
(c) ESA/Hubble, CC BY 4.0Hochaufgelöste Aufnahme des Zentrums von Messier 3, erstellt mithilfe des Hubble-Weltraumteleskops, Bildwinkel 2.8' × 2.4'
Weblinks
- Spektrum.de: Amateuraufnahmen [1][2]
- Blue rejuvenation
- SIMBAD Astronomical Database
Einzelnachweise
- ↑ NASA/IPAC EXTRAGALACTIC DATABASE
- ↑ Harlow Shapley, Helen B. Sawyer: A Classification of Globular Clusters. In: Harvard College Observatory Bulletin. Band 849, 1927, S. 11–14, bibcode:1927BHarO.849...11S.
- ↑ SEDS: NGC 5272
- ↑ Messier 3
- ↑ Sterne und Weltraum April 2013 S. 74ff
- ↑ Seligman
Auf dieser Seite verwendete Medien
Autor/Urheber:
diverse
, Lizenz: CC-by 3.0Bildtafel der 110 Messier-Objekte.
Autor/Urheber: Sloan Digital Sky Survey, Lizenz: CC BY 4.0
Angle of view: 24' x 24' (0.3515625" per pixel), north is up.
Details on the image processing pipeline: https://www.sdss.org/dr14/imaging/jpg-images-on-skyserver/
(c) ESA/Hubble, CC BY 4.0
Blue rejuvenation
Globular clusters are inherently beautiful objects, but the subject of this NASA/ESA Hubble Space Telescope image, Messier 3, is commonly acknowledged to be one of the most beautiful of them all.
Containing an incredible half a million stars, this eight-billion-year-old cosmic bauble is one of the largest and brightest globular clusters ever discovered. However, what makes Messier 3 extra special is its unusually large population of variable stars — stars that fluctuate in brightness over time. New variable stars continue to be discovered in this sparkling stellar nest to this day, but so far we know of 274, the highest number found in any globular cluster by far. At least 170 of these are of a special variety called RR Lyrae variables, which pulse with a period directly related to their intrinsic brightness. If astronomers know how bright a star truly is based on its mass and classification, and they know how bright it appears to be from our viewpoint here on Earth, they can thus work out its distance from us. For this reason, RR Lyrae stars are known as standard candles — objects of known luminosity whose distance and position can be used to help us understand more about vast celestial distances and the scale of the cosmos.
Messier 3 also contains a relatively high number of so-called blue stragglers, which are shown quite clearly in this Hubble image. These are blue main sequence stars that appear to be young because they are bluer and more luminous than other stars in the cluster. As all stars in globular clusters are believed to have formed together and thus be roughly the same age. Only a difference in mass can give these stars a different colour: a red, old star can appear bluer when it acquires more mass, for instance stripping it from a nearby star. The extra mass changes it into a bluer star, which makes us think it is younger than it really is.
Credit:
ESA/Hubble & NASA, G. Piotto et al.
Coordinates Position (RA): 13 42 11.80 Position (Dec): 28° 22' 31.69" Field of view: 2.78 x 2.43 arcminutes Orientation: North is 10.5° right of vertical
Colours & filters Band Wavelength Telescope Optical U 336 nm Hubble Space Telescope WFC3 Ultraviolet UV 275 nm Hubble Space Telescope WFC3 Optical B 438 nm Hubble Space Telescope WFC3 Ultraviolet UV 275 nm Hubble Space Telescope WFC3 Optical U 336 nm Hubble Space Telescope WFC3 Optical V 606 nm Hubble Space Telescope WFC3 Optical B 438 nm Hubble Space Telescope WFC3 Optical V 606 nm Hubble Space Telescope WFC3 Optical I 814 nm Hubble Space Telescope WFC3.
Autor/Urheber: Credit Line and Copyright Adam Block/Mount Lemmon SkyCenter/University of Arizona, Lizenz: CC BY-SA 3.0 us
M3
Picture Details:
Optics 24-inch RC Optical Systems Telescope Camera SBIG STL11000 CCD Camera Filters Custom Scientific Dates May 30th 2009 Location Mount Lemmon SkyCenter Exposure LRGB = 25:25:25:25 minutes Acquisition ACP Observatory Control Software (DC-3 Dreams),TheSky (Software Bisque), Maxim DL/CCD (Cyanogen) Processing CCDStack (CCDWare), Mira (MiraMetrics), Photoshop CS3 (Adobe) Guest Astronomers: May 2009 CCD Image Processing ParticipantsCredit Line and Copyright Adam Block/Mount Lemmon SkyCenter/University of Arizona