ING Home Page > Public Information > Astronomy Images > ING Picture Gallery > Stars, stellar systems and nebulae

Stars, Stellar Systems, and Nebulae

Emission Nebulae

Emission nebulae are clouds of high temperature gas. The atoms in the cloud are energized by ultraviolet light from a nearby star and emit radiation as they fall back into lower energy states (in much the same way as a neon light). These nebulae are usually red because the predominant emission line of hydrogen happens to be red (other colours are produced by other atoms, but hydrogen is by far the most abundant). Emission nebulae are usually the sites of recent and ongoing star formation.

Description: Part of the nebula IC 1396B in the constellation Cepheus imaged in the red light from hydrogen atoms. This image was obtained as part of the INT/WFC Photometric Hydrogen-Alpha Survey of the Northern Galactic Plane (IPHAS).
Date: 2005.
Credits: Nick Wright (University College London) and the IPHAS collaboration.
Technical information: Image obtained using the Wide-Field Camera on the Isaac Newton Telescope. The image scale here is roughly 15 × 15 square arcminutes, with N to the left and E down.
Available formats: JPEG | TIFF | PDF (with text).

Description: This image of the Rosette Nebula (NGC 2237) is thought to be the most-detailed ever produced. Compiled from data taken from IPHAS, the Isaac Newton Telescope Photometric Hydrogen-Alpha Survey of the Northern Galactic Plane, the image spans four square degrees, about twenty times the size of the full moon.
Date: 2007.
Credits: Nick Wright (University College London) and the IPHAS collaboration.
Technical information: Image obtained using the Wide-Field Camera on the Isaac Newton Telescope. Resolution is 1 arcsecond per pixel, and North is up, east is left.
Available formats: JPEG (360K) | JPEG (1.1M) | JPEG (3.0M) | BMP (157M) | PDF (with text).

Description: Dust lanes in the centre of the Rosette Nebula or NGC 2237. Size is 30×20 arcmin, north to the left, east is down. This image was obtained as part of the IPHAS survey.
Date: 2005.
Credits: Nick Wright (University College London) on behalf of the IPHAS collaboration.
Technical information: Image obtained using the Wide-Field Camera on the Isaac Newton Telescope.
Available formats: JPEG (3593 K) | TIFF (26,723 K) | PDF (with text).

1 23 4
Description: This is the star-formation region M42, also known as the Orion nebula. The gas and dust in the nebula emits light because it is irradiated by nearby emerging stars. Located at a distance of about 1,600 light years, the Orion nebula is the brightest diffuse nebula in the sky, visible to the naked eye. It is the main part of a much larger cloud of gas and dust which extends over 10 degrees well over half the constellation Orion.
Date: Images 1, 2: 1999. Image 3: 1995. Image 4: 2007.
Credits: Images 1, 2: Simon Tulloch (ING) and Nik Szymanek. Image 3: ING Archive and Nik Szymanek. Image 4: Jonathan Irwin.
Technical information: Images 1 and 2 are 10s true-colour images using BVR imaging on the WHT prime focus camera. Image 3: Jacobus Kapteyn Telescope, Tek CCD, B, V and R filters. Image 4: Wide-Field Camera on the Isaac Newton Telescope.
Available formats:
Image 1: JPEG (167 K) | TIFF (1,045 K) | PDF (with text)
Image 2: JPEG (35 K)
Image 3: JPEG (125 K) | TIFF (12,390 K). Image 4: JPEG | TIFF

Title: M43 Nebula.
Description: M43 is actually a part of the Great Orion Nebula, M42, which is separated from the main nebula by an impressive, turbulent dark lane.
Date: 2002.
Credits: Nik Szymanek (University of Hertfordshire) and Simon Tulloch (ING).
Technical information: Wide-Field Camera on Isaac Newton Telescope. This is a 300 second exposure in H-alpha combined with colour information from an amateur CCD image.
Available formats: JPEG (261 K) | TIFF (4608 K) | PDF (with text).

Description: NGC 7635, the Bubble nebula. A massive star that is not only bright and blue, but also emitting a fast stellar wind of ionized gas, created this huge space bubble. The Bubble nebula is actually the smallest of three bubbles surrounding massive star BD+602522, and part of gigantic bubble network S162 created with the help of other massive stars. As fast moving gas expands off BD+602522, it pushes surrounding sparse gas into a shell. The energetic starlight then ionizes the shell, causing it to glow. The Bubble Nebula is about 10 light-years across and visible with a small telescope towards the constellation of Cassiopeia. PDF (with text).
Date: 1992.
Copyright: Malin-IAC-RGO.
Technical information: Photographic 3-colour composition from the Isaac Newton Telescope.

Reflection Nebulae

Reflection nebulae are clouds of dust which are simply reflecting the light of a nearby star or stars. Reflection nebulae are also usually sites of star formation. They are usually blue because the scattering is more efficient for the blue light. Reflection nebulae and emission nebulae are often seen together and are sometimes both referred to as diffuse nebulae.

Description: The Crescent Nebula (NGC 6888), which surrounds the Wolf-Rayet star PPM 84423 or HD192163, seen in Hydrogen-α emission. This was observed as part of the Isaac Newton Telescope/Wide Field Camera Photometric Hydrogen-α Survey (IPHAS) of the Galactic Plane. NGC 6888 is the illuminated ejecta of the star HD192163.
Date: 2004.
Credits: Image based on data obtained as part of the INT Photometric Hα Survey of the Northern Galactic Plane: prepared by Jonathan Irwin (Institute of Astronomy, Cambridge).
Technical information: This image combines data from all three IPHAS survey passbands (Hα Sloan r' and i') in a false colour composite. Emission in the Hα narrow band is in red. The orientation is with N to the left and E down, and the image scale is about 20 × 18 square arcminutes.
Available formats: [ JPEG (328 K) | TIFF (2895 K) ].

Date: 1992.
Description: NGC 6914 and a group of reflection nebulae. PDF (with text).
Copyright: Malin-IAC-RGO.
Technical information: Photographic 3-colour composition from the Isaac Newton Telescope.

Dark Nebulae

Dark Nebulae are clouds of dust which are simply blocking the light from whatever is behind. They are physically very similar to reflection nebulae; they look different only because of the geometry of the light source, the cloud and the Earth. Dark nebulae are often seen in conjunction with reflection and emission nebulae.

1 2
Description: The Horse Head Nebula. This dark dust nebula, in the shape of a horse's head, protrudes into a bright emission nebula, IC 434, in the constellation Orion. A nearby naked-eye star illuminates the surface of an otherwise invisible dusty cloud, exciting the distinctive red emission from hydrogen. From this dark cloud projects yet more dust, which has the shape of the head of a horse, seen in silhouette against the glowing background.
Date: Image 1: 1999, Image 2: 1997.
Credit: Image 1 is credit Simon Tulloch (ING) and Nik Szymanek (SPA). Image 2 is credit Peter Bunclark (IoA).
Technical information: Image 1 is a 10s exposure using the 2-detector prime focus camera on the WHT. Image 2 is the same object as observed by the INT Wide Field Camera.
Available formats: Image 1 JPEG (343 K) | PDF (with text).

Description: NGC 281 and IC 1590. NGC 281 is a busy workshop of star formation. Prominent features include a small open cluster of stars, a diffuse red-glowing emission nebula, large lanes of obscuring gas and dust, and dense knots of dust and gas in which stars may still be forming. PDF (with text).
Date: 1992.
Copyright: Malin-IAC-RGO.
Technical information: This image is the result of combining 30 minute photographs taken at the INT prime focus in 3 different filters matching the standard B,V,R system.

Globular Clusters

Globular clusters are gravitationally bound groups of many thousands (sometimes as many as a million) of stars. They consist primarily of very old stars. Globular clusters are not concentrated in the plane of the galaxy but rather randomly distributed throughout the halo. There are several hundred globular clusters associated with our galaxy.

Title: M3 Globular Cluster (NGC 5272).
Description: M3 Globular Cluster.
Date: 16 January 2004.
Credit: Maureen Van den Berg (Leiden Univ.), Nik Szymanek (Univ. of Hertfordshire).
Technical information: 90s in B and Sloan r, 60s in V.
Available formats: JPEG (216 K) | TIFF (4826 K)

Description: M13 Globular Cluster. M13, also called the 'Great globular cluster in Hercules', is one of the most prominent and best known globular clusters of the Northern celestial hemisphere. It was selected in 1974 as target for one of the first radio messages addressed to possible extra-terrestrial intelligent races, and sent by the big radio telescope of the Arecibo Observatory.
Date: 1999.
Credit: Daniel Folha and Simon Tulloch (ING).
Technical information: This true-colour CCD image was taken using the Jacobus Kapteyn telescope and the SITe2 detector, which covers 11.3 arcminutes.
Available formats: JPEG (431 K) | PDF (with text).

Title: M92 Globular Cluster (NGC 6341).
Description: M92 is a splendid object, visible to the naked eye under very good conditions and a showpiece for every optics. It is only slightly less bright but about 1/3 less extended than M13: its 11.2' angular extension corresponds to a true diameter of 85 light years, and may have a mass of up to 330,000 suns.
Credit: Daniel Bramich (ING) and Nik Szymanek.
Date: 2001.
Technical information
Telescope: Jacobus Kapteyn Telescope.
Instrument: JAG CCD Camera.
Detector: SITe2.
Filters and exposure times: This image was achieved by combining 25s exposures in Kitt Peak B, Sloan g' and Sloan r'.
Available formats: [ JPEG (229 K) | TIFF1 (8,316 K) | TIFF2 (32,474 K) | PDF (with text) ]

Title: M15 Globular Cluster.
Description: M15 is one of the brighest globular clusters in our Galaxy. Most stars in globular clusters are older and redder than our Sun, which is about 5 billion years old.
Credit: Image 1: Amanda Willmott, Aaron Shrimpton, Javier Méndez and Nik Szymanek. Image 2: Daniel Bramich (ING).
Date: Image 1: June 2000. Image 2: 4 July 2001.
Technical information: Image 1: This image was achieved by combining images taken in B, V, and R filters and a CCD camera on the JKT.
Image 2: Same as before but in better seeing conditions. Exposure length in every filter was 100 seconds.
Available formats: Image 1: JPEG (200 K) | TIFF (16,242 K)
Image 2: JPEG (282 K) | JPEG (68 K) | TIFF (4,558 K)

Title: M 56 or NGC 6779 Globular Cluster.
Description: It is one of the less bright Messier globulars, especially lacking the bright core which most globulars have. Nevertheless it is not too difficult to resolve, even at its rather large distance. This led to its classification in concentration class X. At its distance of 32,900 light-years. its diameter of 8.8 arc minutes corresponds to a linear extension of about 85 light years.
Date: 18 August 2001.
Credit: Robert Greimel (ING), Javier Méndez (ING) and Nik Szymanek.
Technical information: Site2 CCD on Jacobus Kapteyn Telescope. 4×9 second exposures in Kitt Peak V-band, 4×12 second exposures in Harris B-band and 5×6.4 second exposures in Harris R-band.
Available formats: JPEG (347 K) | TIFF (8976 K)

Open Clusters

Open clusters are physically related group of stars held together by mutual gravitational attraction. They are believed to originate from large cosmic gas and dust clouds in the Milky Way, and to continue to orbit the galaxy through the disk. In many clouds visible as bright diffuse nebulae, star formation takes still place at this moment, so that we can observe the formation of new young star clusters.

Title: M 103 or NGC 581.
Description: M 103 is one of the more remote open clusters in Messier's catalog, at about 8,000 light years or slightly more, the uncertainty mainly due to the less wellknown amount of obstruction for this cluster which lies well within the band of the Milky Way.
Date: 25 November 2001.
Credit: Thomas Hardy School.
Technical information: Site2 CCD on Jacobus Kapteyn Telescope. 2*60 second exposures in Harris V, B and R filters.
Available formats: JPEG (127 K) | TIFF (3141 K)

Description:M29 open cluster.
Date: August 2001.
Credit: Cornwall Astronomy School Project.
Technical information: This B, V, R image was taken using the Jacobus Kapteyn telescope and the SITe2 detector. In order not to saturate the images, many short exposures were taken.
Available formats: JPEG (40 K) | TIFF (4,154 K)

Planetary Nebulae

Planetary nebulae are shells of gas thrown out by some stars near the end of their lives. Our Sun will probably produce a planetary nebula in about 5 thousand million years. They have nothing at all to do with planets; the terminology was invented because they often look a little like planets in small telescopes. Planetary nebulae are formed in the process of mass loss during which red giant stars ultimately become white dwarfs.

Description: This image is a new planetary nebula discovered by the INT/WFC Photometric Hydrogen-Alpha Survey of the Northern Galactic Plane (IPHAS). The nebula was confirmed to be a relatively old planetary nebula using the ISIS spectrograph on the William Herschel Telescope.
Date: 2007.
Credits:Laurence Sabin, Nick Wright and the IPHAS collaboration.
Technical information: Image obtained using the Wide-Field Camera on the Isaac Newton Telescope. It is a two-colour image, red for H-alpha and green for [OIII]. North is to the right and East is to the top.
Available formats: JPEG | TIFF | PDF (with text).

Description: The central star of Sharpless 2-188 is 850 light years away and it is travelling at 125 kilometres per second across the sky. Observations show a strong brightening in the direction in which the star is moving and faint material stretching away in the opposite direction. The astronomers believe that the bright structures in the arc observed ahead of Sharpless 2-188 are the bowshock instabilities revealed in the simulations, which will form whirlpools as they spiral past the star downstream to the tail. This image was obtained as part of the INT/WFC Photometric Hydrogen-Alpha Survey of the Northern Galactic Plane (IPHAS).
Date: 2007.
Credits: Nick Wright (University College London) and the IPHAS collaboration.
Technical information: Image obtained using the Wide-Field Camera on the Isaac Newton Telescope.
Available formats: JPEG | BMP | PDF (with text).

Title: Planetary Nebula NGC 7293 or Helix Nebula.
Description: Image of the planetary nebula NGC 7293.
Date: 2001.
Credit: Romano Corradi (ING).
Technical information: Image obtained with the Wide Field Camera at the 2.5m INT telescope. A narrow filter has been used to isolate the emission from the nebular gas in the hydrogen Halpha line (at wavelength 656 nm) and in the nitrogen doublet [NII] at lambda 655 and 658 nm.
Available formats: JPEG (66 K) | TIFF (2936 K)

Title: Planetary Nebula NGC 3242.
Description: Image of the planetary nebula NGC 3242.
Date: 2001.
Credit: Romano Corradi (ING).
Technical information: Image obtained with the Wide Field Camera at the 2.5m INT telescope. A narrow filter has been used to isolate the emission from the nebular gas in the hydrogen Halpha line (at wavelength 656 nm) and in the nitrogen doublet [NII] at lambda 655 and 658 nm.
Available formats: JPEG (316 K) | TIFF (13,175 K)

Title: Planetary Nebula Sh 2 - 200.
Description: Image of the planetary nebula Sharpless 2-200. This is a very evolved planetary nebula, whose central star has already faded to a low luminosity after exhausting all circumnuclear fuel. Around the filamentary inner nebula, a large faint halo is observed. This halo might be interstellar gas ionized by the central star of the planetary nebula, or alternatively ancient material ejected by the star itself when it was a red giant some 50 to 100 thousand years ago. These haloes provide very precious information about the various events of strong mass loss at the end of life of solar type stars. These mass loss events are the ultimate cause leading to the death of these stars.
Date: Image 1, 2, 3: 2001.
Credit: Image 1: Romano Corradi (ING) and Nik Szymanek. Image 2: Romano Corradi (ING). Image 3: Romano Corradi (ING) and Nik Szymanek.
Technical information: Images 1, 2 and 3 were obtained with the Wide Field Camera at the 2.5m INT telescope. A narrow filter has been used to isolate the emission from the nebular gas in the hydrogen Halpha line (at wavelength 656 nm) and in the nitrogen doublet [NII] at lambda 655 and 658 nm.
Available formats:
Image 1: JPEG (593 K) | TIFF (3,038 K)
Image 2: JPEG (158 K) | TIFF (362 K)
Image 3: JPEG (180 K) | TIFF (14,276 K)

Title: M 76 or NGC 650. The Little Dumbell Nebula.
Description:M76 is among the fainter Messier objects. It is known under the names Little Dumbbell Nebula (the most common), Cork Nebula, Butterfly Nebula, and Barbell Nebula, and it was given two NGC numbers as it was suspected to be a double nebula with two components in contact, a hypothesis brought up by William Herschel, who numbered the "second component" H I.193 on November 12, 1787. NGC 651 is the North following (East) part of the nebula.
Date: 25 November 2001.
Credit: Thomas Hardy School.
Technical information: Site2 CCD on Jacobus Kapteyn Telescope. 2*300 second exposures in Harris V, B and R filters.
Available formats: JPEG (181 K) | TIFF (4097 K)

Description: NGC 6543, nicknamed the the Cat's Eye Nebula, is one of the most complex of the planetary class nebula, stars that throw of spheres of gas at the end of their lives. It is located in the constellation Draco and is thought to have been created 1,000 years ago by two stars orbiting each other.
Date: August 2001.
Credit: Cornwall Astronomy School Project.
Technical information: This B, V, R image was taken using the Jacobus Kapteyn telescope and the SITe2 detector.
Available formats: JPEG (93 K) | TIFF (1,973 K)

Description: M57 planetary nebula, also known as the "Ring Nebula". The famous ring nebula M57 is often regarded as the prototype of a planetary nebula, and a showpiece in the northern hemisphere summer sky. Recent research has confirmed that it is, most probably, actually a ring (torus) of bright light-emitting material surrounding its central star, and not a spherical (or ellipsoidal) shell.
Date: Image 1: 1999. Image 2: 1995.
Credit: Image 1: Daniel Folha and Simon Tulloch (ING). Image 2: ING Archive and Nik Szymanek.
Technical information: Image 1: This true-colour image was taken using the Jacobus Kapteyn telescope and the SITe2 detector. Image 2: Jacobus Kapteyn Telescope, Tek CCD, B, V and R filters.
Available formats: Image 1 JPEG (49 K) | Image 2 JPEG (59 K) | Image 2 TIFF (11,746 K)

Description: NGC 3242 planetary nebula. The "Ghost of Jupiter" is a planetary nebula which has a nearly spherical outer shell with an elliptical inner ring that gives it the appearance of an "eye". In this image it's also possible to see the central illuminating star.
Date: 2000.
Credit: Javier Méndez (ING).
Technical information: Image acquired with the Auxiliary Port Camera on the WHT, through filter R. Exposure time was 100 seconds.
Available formats: GIF (92 K)

Decription: M2-9 planetary nebula. M2-9, a butterfly planetary nebula 2100 light-years away, has wings that tell a strange but incomplete tale. In the center, two stars orbit inside a gaseous disk 10 times the orbit of Pluto. The expelled envelope of the dying star breaks out from the disk creating the bipolar appearance.
Date: 2000.
Credit: Javier Méndez (ING).
Technical information: Image acquired with the Auxiliary Port Camera on the WHT, through filter R. Exposure time was 100 seconds.
Available formats: GIF (94 K)

Title: M27, NGC 6853, the Dumbell nebula.
Description: The Dumbell nebula was the first planetary nebula ever discovered. We happen to see this one approximately from its equatorial plane; from near one pole, it would probably have the shape of a ring, and perhaps look like we view the Ring Nebula M57.
Credit: Image 1: Copyright Malin-IAC-RGO. Image 2: Amanda Willmott, Aaron Shrimpton and Javier Méndez. Image 3: Amanda Willmott, Aaron Shrimpton, Javier Méndez and Nik Szymanek.
Date: Image 1: 1992. Image 2: 2000. Image 3: 2000.
Technical information: Image 1 1: Photographic 3-colour composition from the Isaac Newton Telescope. Image 2: True-colour composition from B, V, and R imaging using a CCD camera on the JKT. Image 3: Same as before but colour-processed by Nik Szymanek.
Available formats: Image 1: PDF (with text). Image 2: JPEG (248 K) | Compressed TIFF (9,177 K). Image 3: JPEG (109 K) | TIFF (14,392 K)

Decription: The "Príncipes de Asturias" nebula or IPHAS PN-1. The discovery of the first new PN from the IPHAS survey is an unusual object located at a large galactocentric distance and has a very low oxygen abundance. The so-called "Príncipes de Asturias" nebula shows an intricate morphology: there is an inner ring surrounding the central star, bright inner lobes with an enhanced waist, and very faint lobular extensions reaching up to more than 100 arcseconds.
Date: 2006.
Credit: Credit: Antonio Mampaso, Romano Corradi and the IPHAS Collaboration.
Technical information: Image acquired using the Wide-field Camera on the Isaac Newton Telescope.
Available formats: JPEG | TIFF

Supernovae

A supernova is a catastrophic stellar explosion in which so much energy is released that the supernova alone can outshine an entire galaxy of billions of stars. In addition to the radiant energy produced, ten times as much energy goes into the kinetic energy of the material blown out by the explosion, and a hundred times as much is carried off by neutrinos.

Two distinct kinds of supernova are recognized, known as Type I and Type II. They are distinguished by the presence of hydrogen features in the spectrum of Type II supernovae, which are absent from Type I. Both types include other subclasses.

Type Ia supernovae are thought to be white dwarfs in binary systems, where mass transfer from the companion takes place. A wave of carbon burning through the newly acquired material could account for the energy released. The explosion may represent the total disintegration of the white dwarf. Type II supernovae appear to be stars of eight solar masses or more that have run the course of stellar evolution and totally exhausted the nuclear fuel available in their cores. In the absence of energy generation, the pressure balancing the weight of the overlying layers is removed. When the crunch comes, the core collapses in less than a second and when the density of nuclear matter is reached, there is a sudden strong resistance to further pressure, the imploding material bounces back and an outward shock wave is generated. The outer layers of the star are blown outwards at thousands of kilometres per second, leaving the core exposed as a neutron star.

Description:Supernova SN 1994D in galaxy NGC 4526. The supernova is the brightest star, and it lies between the fainter star on the left and the galaxy nucleus. As it can be seen, the supernova is as bright as the whole galaxy which hosts the progenitor. SN 1994D was a type Ia supernova.
Date: 1994.
Credit: Javier Méndez (ING).
Technical information: Image acquired using a CCD camera on the Jacobus Kapteyn Telescopes.
Available formats: GIF (39 K)

Description:SN 1994I in galaxy M51. SN 1994I was type Ic.
Date: 1994.
Credit: Javier Méndez (ING).
Technical information: Image acquired using a CCD camera on the Jacobus Kapteyn Telescopes.
Available formats: GIF (49 K)

Description: Supernova 2001dc. This is a sub-luminous type IIp supernova. The supernova is situated within the galaxy to the top right, the first bright spot in the North-East direction from the nucleus.
Date: 2001.
Credit: Daniel Bramich (ING).
Technical information: BVR CCD composite. Images from the CCD camera on the Jacobus Kapteyn Telescope.
Available formats: JPEG (86 K)

Supernova Remnants

A supernova remnant is the expanding shell of material created by the ejection of the outer layers of a star that explodes as a supernova. A shock wave precedes the ejected shell, colliding with and heating the interstellar gas. The ejected material breaks up into clumps, so the radiation emitted from the shell often does not make up a uniform ring. NGC 6995, part of the Cygnus Loop is the remnant of a type II supernova. For a few days the supernova emitted as much energy as a whole galaxy. When it was all over, a large fraction of the star was blown into space, as shown on this picture. Remnants are tipically at most few light-years across.

Description: A 5°×3.5° mosaic of the supernova remnant S147 in Hα. North is to the top and East to the left. This is a continuum subtracted Hα image of the supernova remnant S147, located on the sky toward the anti-galactic centre. A strength of IPHAS is that it offers the chance to construct images of parts of the Galactic Plane on any scale from arcseconds up to degrees. This is a very large-scale image, built up by mosaicking a large number of overlapping IPHAS fields together. The bright blob to the left of the picture is a more typically compact Galactic nebula.
Date: 2004.
Credit: Image based on data obtained as part of the INT Photometric Hα Survey of the Northern Galactic Plane: prepared by Albert Zijlstra, University of Manchester and Jonathan Irwin, IoA Cambridge.
Technical information: A continuum subtracted Hα image of the supernova remnant S147, observed as part of the INT Photometric Hα Survey of the Northern Galactic Plane.
Available formats: JPEG (4549 K) | TIFF (30,667 K)

Description: NGC 6995, part of the Cygnus Loop. The Cygnus Loop is the remnant of a type II supernova. For a few days the supernova emitted as much energy as a whole galaxy. When it was all over, a large fraction of the star was blown into space as a supernova remnant, which it's typical at most few light-years across. PDF (with text).
Date: 1992.
Copyright: Malin-IAC-RGO.
Technical information: Photographic 3-colour composition from the Isaac Newton Telescope.

Title: M1, the Crab Nebula.
Description: M1, the Crab Nebula.
Credit: Image 1: Peter Sorensen and Nik Szymanek.
Image 2: ING archive and Nik Szymanek.
Date: Image 1: 02/01/2001. Image 2: 1995.
Technical information: Image 1: H-alpha, OIII and HeII images taken using the Wide Field Camera on the Isaac Newton Telescope. 1200s per filter.
Image 2: Tek CCD detector on Jacobus Kapteyn Telescope. Filters B, V and R.
Available formats: Image 1: JPEG (84 K) | TIFF (14,994 K)
Image 2: JPEG (125 K) | TIFF (11,953 K)

Back to the top | Back

Public Relations Officer
Last Modified: 09 September 2009