NGC 604

H-II-Gebiet
NGC 604
NGC 604, aufgenommen mit der Kamera WFPC 2 des Hubble-Weltraumteleskops
NGC 604, aufgenommen mit der Kamera WFPC 2 des Hubble-Weltraumteleskops
SternbildDreieck
Position
Äquinoktium: J2000.0
Rektaszension01h 34m 33,2s[1]
Deklination+30° 47′ 06″[1]
Weitere Daten
Helligkeit (visuell)

12 mag[2]

Winkelausdehnung

1,95[2]

Entfernung

ca. 3 Mio. Lj /
ca. 900 kpc

Zugehörigkeit

Dreiecksnebel, Lokale Gruppe

Rotverschiebung

(−754 ± 40) · 10−6

Heliozentrische Radialgeschwindigkeit

(−226 ± 12) km/s

Durchmesser1500 Lj
Geschichte
Entdeckung

Wilhelm Herschel

Datum der Entdeckung

11. September 1784[3]

Katalogbezeichnungen
NGC 604 • IRAS 01317+3031 •
AladinLite

NGC 604 ist ein H-II-Gebiet in der Galaxie Messier 33 im Sternbild Dreieck am nördlichen Fixsternhimmel. Es hat eine Winkelausdehnung von etwa 1,95′ × 1,95′ und wurde am 11. September 1784 vom deutsch-britischen Astronomen Wilhelm Herschel entdeckt. Die Bezeichnung ergibt sich aus dem Eintrag des Objektes in dem in den 1880er Jahren zusammengestellten New General Catalogue. NGC 604 ist eines der größten bekannten H-II-Gebiete.

NGC 604 liegt in einem Spiralarm der Galaxie M33, die auch als „Dreiecksnebel“ bekannt ist. Mit einer Entfernung von 2,8 Millionen Lichtjahren ist uns M33 verhältnismäßig nahe; sie ist ein Mitglied der Lokalen Gruppe, der auch unsere Milchstraße angehört. M33 enthält noch weitere H-II-Regionen, etwa NGC 595 und NGC 592.

NGC 604 ist eines der größten Sternentstehungsgebiete, das Astronomen in unseren direkten Nachbargalaxien gefunden haben. Das Gebiet hat eine Ausdehnung von rund 1300 Lichtjahren und enthält mehr als 200 junge und sehr heiße Sterne (der hohen Temperatur entsprechend bläulich gefärbt), die erst binnen der letzten drei Millionen Jahre entstanden sind.[4] Spektralanalysen legen außerdem nahe, dass die Region ungefähr so viele aktive, massereiche Wolf-Rayet-Sterne wie blaue Sterne enthält. Rund 50 davon haben sich während einer einzigen Phase gesteigerter Sternentstehung vor rund 4 Millionen Jahren gebildet.[5]

Das interstellare Medium in NGC 604 weist komplexe Blasenstrukturen und Filamente auf. Nach heutigem Wissen sind diese Strukturen einerseits durch den starken Sternwind der jungen, heißen Sterne, andererseits durch Supernova-Explosionen entstanden.[6]

Siehe auch

  • Liste der diffusen Nebel

Einzelnachweise

  1. ↑ NASA/IPAC EXTRAGALACTIC DATABASE
  2. ↑ a b SEDS: NGC 604
  3. ↑ Seligman
  4. ↑ Firestorm of Star Birth Seen in a Local Galaxy. Pressemitteilung des Space Telescope Science Institute vom 4. Dezember 2003.
  5. ↑ S. Dodorico und M. Rosa: Wolf-Rayet stars in the giant H II region NGC 604. In: Astrophysical Journal. Bd. 248, 1981, S. 1015–1020. bibcode:1981ApJ...248.1015D
  6. ↑ Hui Yang u. a.: The Violent Interstellar Medium of NGC 604. In: Astronomical Journal. Bd. 112, 1996, S. 146. bibcode:1996AJ....112..146Y

Literatur

  • König, Michael & Binnewies, Stefan (2019): Bildatlas der Galaxien: Die Astrophysik hinter den Astrofotografien, Stuttgart: Kosmos, S. 50
Commons: NGC 604 – Album mit Bildern, Videos und Audiodateien

Auf dieser Seite verwendete Medien

NGC 604 (MIRI image) (weic2407b).jpg
(c) NASA, ESA, CSA, STScI, CC BY 4.0
This image from the NASA/ESA/CSA James Webb Space Telescope’s MIRI (Mid-Infrared Instrument) of star-forming region NGC 604 shows how large clouds of cooler gas and dust glow at mid-infrared wavelengths. This region is a hotbed of star formation and home to more than 200 of the hottest, most massive kinds of stars, all in the early stages of their lives.In the MIRI view of NGC 604, there are noticeably fewer stars than Webb’s NIRCam image. This is because hot stars emit much less light at these wavelengths. Some of the stars seen in this image are red supergiants — stars that are cool but very large, hundreds of times the diameter of our Sun. The blue tendrils of material signify the presence of polycyclic aromatic hydrocarbons, or PAHs.[Image description: At the centre of the image is a nebula on the black background of space. The nebula is composed of wispy filaments of light blue clouds. At the centre-right of the blue clouds is a large cavernous bubble. The bottom left edge of this cavernous bubble is filled with hues of pink and white gas. Hundreds of dim stars fill the area surrounding the nebula.]
Grand Stellar Nursery NGC 604 From HST & Chandra (31805576447).png
Autor/Urheber: geckzilla, Lizenz: CC BY 2.0
The brightest x-ray object in this scene is an unknown object at the upper left. The next brightest thing seems to be a distant active galaxy nucleus (AGN) coincidentally positioned just above the nebula. In third place comes NGC 604 itself. It's hard to compete with an AGN, but these young stars are doing an admirable job. X-rays are generated when things get super hot, and that's what's happening within the cavernous interior bubble of the nebula.

There's a better explanation and additional imagery at Chandra's website here: chandra.harvard.edu/photo/2009/n604/

This image was possible thanks to data from the following Chandra proposal: The Giant Extragalactic Star-Forming Region NGC 604

In addition, all HST proposals listed under this image were also used: https://www.flickr.com/photo.gne?short=S5kLbG

Chandra data: Violet / Magenta overlay: ACIS .30-7.00 keV

PHAT data: Red: WFC3/IR F160W Yellow-Green: ACS/WFC F814W Cyan: ACS/WFC F475W Blue: WFC3/UVIS F336W

WFPC2/WFC data: F673N, F658N, and F656N combined together into a pinkish "screen" layer

North is NOT up. It is 90° clockwise from up.
NGC 604 (NIRCam image) (weic2407a).jpg
(c) NASA, ESA, CSA, STScI, CC BY 4.0
This image from the NASA/ESA/CSA James Webb Space Telescope’s NIRCam (Near-Infrared Camera) of star-forming region NGC 604 shows how stellar winds from bright, hot young stars carve out cavities in surrounding gas and dust.The bright orange streaks in this image signify the presence of carbon-based molecules known as polycyclic aromatic hydrocarbons, or PAHs. As you travel further from the immediate cavities of dust where the star is forming, the deeper red signifies molecular hydrogen. This cooler gas is a prime environment for star formation. Ionised hydrogen from ultraviolet radiation appears as a white and blue ghostly glow.NGC 604 is located in the Triangulum Galaxy (M33), 2.73 million light-years away from Earth. It provides an opportunity for astronomers to study a high concentration of very young, massive stars in a nearby region.[Image description: At the centre of the image is a nebula on the black background of space. The nebula is composed of clumpy, red, filamentary clouds. At the centre-right of the red clouds is a large cavernous bubble, and at the centre of the bubble there is an opaque blue glow with speckles of stars. At the edges of the bubble, the dust is white. There are several other smaller cavernous bubbles at the top of the nebula. There are also some smaller, red stars and a few disc-shaped galaxies scattered about the image.]
Nursery of New Stars - GPN-2000-000972.jpg
This is a Hubble Space Telescope image (right) of a vast nebula called NGC 604, which lies in the neighboring spiral galaxy M33, located 2.7 million light-years away in the constellation Triangulum.

This is a site where new stars are being born in a spiral arm of the galaxy. Though such nebulae are common in galaxies, this one is particularly large, nearly 1,500 light-years across. The nebula is so vast it is easily seen in ground-based telescopic images (left).

At the heart of NGC 604 are over 200 hot stars, much more massive than our Sun (15 to 60 solar masses). They heat the gaseous walls of the nebula making the gas fluoresce. Their light also highlights the nebula's three-dimensional shape, like a lantern in a cavern. By studying the physical structure of a giant nebula, astronomers may determine how clusters of massive stars affect the evolution of the interstellar medium of the galaxy.

The nebula also yields clues to its star formation history and will improve understanding of the starburst process when a galaxy undergoes a "firestorm" of star formation. The image was taken on January 17, 1995 with Hubble's Wide Field and Planetary Camera 2. Separate exposures were taken in different colors of light to study the physical properties of the hot gas (17,000 degrees Fahrenheit, 10,000 degrees Kelvin