2. Astronomy

NIGHT OVER ONTARIO

These photos were taken by Lynn Hilborn of Grafton, Ontario.
Pictures have appeared on the cover and inside editions of SkyNews magazine and in Sky & Telescope and Astronomy magazine, and as NASA's Astronomy Picture of the Day.

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The Trifids, M20. LRGB Lum 7x10m bin 1x1, RGB each 12x5m bin 2x2. Taken with TEC 140 @f7 and FLI ML8300 camera at -30C.<br /> Shot July 05,09,10, 2012 by Lynn Hilborn, WhistleStop Obs,Grafton, Ontario. COVER PHOTO, SkyNews Magazine, September 2012.<br /> M20 (Trifid Nebula) (Barnard 85) (NGC 6514)<br /> <br /> Distance: 5500 to 9000 light years<br /> <br /> Right Ascension: 18 : 02.3 (hours : minutes)<br /> Declination: -23 : 02 (degrees : minutes)<br /> <br /> Text Copyright Robert Gendler 2006<br /> A gem of the summer sky, M20 allows us a view into the exciting science of star birth. M20 is a young HII region (300,000 years old) about 30 light years across and is illuminated by the O-type supergiant HD 164492 at the center of its trilobed emission cloud. The ionizing star is about 30 times the mass of our sun and is the "A" component of a triple system ( A, B, and C components). In all there are seven members (HD 164492 A through G) of the small cluster packed within a half light year at the center of M20. As an HII region M20 is similar to M42 in its complexity and relationship to its parent molecular cloud but is much younger. A large blue reflection cloud forms the northern border of M20 and is illuminated solely by the F-type supergiant HD 164514. Recent X-ray and infrared observations have discovered an amazing array of very early stars and protostars within M20 giving us a rare glimpse of the earliest stages of star birth.<br /> <br /> Stars in the earliest formative stages are difficult to detect optically as they are shrouded from view by their parent molecular cloud. They reveal their presence by jets and outflows of gas which characterize their unstable and turbulent beginnings. The power of infrared observations (Spitzer Observatory) allows astronomers to "see" beyond the cloak of gas and dust that obscures young stars. Large populations of the earliest protostars or pre- main sequence stars (Class O and I) have been detected along the filamentary dark lanes near the reflection component. More evolved protostars (Class II) are found along ionization fronts within the rounded brighter parts of the emission cloud. Text with thanks to Robert Gendler.
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The Trifids, M20. LRGB Lum 7x10m bin 1x1, RGB each 12x5m bin 2x2. Taken with TEC 140 @f7 and FLI ML8300 camera at -30C.
Shot July 05,09,10, 2012 by Lynn Hilborn, WhistleStop Obs,Grafton, Ontario. COVER PHOTO, SkyNews Magazine, September 2012.
M20 (Trifid Nebula) (Barnard 85) (NGC 6514)

Distance: 5500 to 9000 light years

Right Ascension: 18 : 02.3 (hours : minutes)
Declination: -23 : 02 (degrees : minutes)

Text Copyright Robert Gendler 2006
A gem of the summer sky, M20 allows us a view into the exciting science of star birth. M20 is a young HII region (300,000 years old) about 30 light years across and is illuminated by the O-type supergiant HD 164492 at the center of its trilobed emission cloud. The ionizing star is about 30 times the mass of our sun and is the "A" component of a triple system ( A, B, and C components). In all there are seven members (HD 164492 A through G) of the small cluster packed within a half light year at the center of M20. As an HII region M20 is similar to M42 in its complexity and relationship to its parent molecular cloud but is much younger. A large blue reflection cloud forms the northern border of M20 and is illuminated solely by the F-type supergiant HD 164514. Recent X-ray and infrared observations have discovered an amazing array of very early stars and protostars within M20 giving us a rare glimpse of the earliest stages of star birth.

Stars in the earliest formative stages are difficult to detect optically as they are shrouded from view by their parent molecular cloud. They reveal their presence by jets and outflows of gas which characterize their unstable and turbulent beginnings. The power of infrared observations (Spitzer Observatory) allows astronomers to "see" beyond the cloak of gas and dust that obscures young stars. Large populations of the earliest protostars or pre- main sequence stars (Class O and I) have been detected along the filamentary dark lanes near the reflection component. More evolved protostars (Class II) are found along ionization fronts within the rounded brighter parts of the emission cloud. Text with thanks to Robert Gendler.

  • Venus and cloudy dawn in Aruba, Feb 2014. Taken by Lynn Hilborn with modified Canon 6D, Samyang14mm lens @f 2.8, 3200 ISO single 22 second exposure.<br /> Astronomy Magazine Picture of the Day June 21,2014.
  • Omega Centauri and Centaurus A <br /> Taken by Lynn Hilborn in Aruba, Feb 2014 with modified Canon 6D, 200mm Canon f2.8 lens and 1.4x telecompressor at f4.5. 7 x 20 second exposures 3200 ISO.<br /> <br /> At the top of this skyscape, Centaurus A (NGC 5128). Spanning over 60,000 light-years, the peculiar elliptical galaxy is apparently the result of a collision of two otherwise normal galaxies. The left over cosmic debris is steadily being consumed by a black hole with a billion times the mass of the Sun which lies at the center of Centaurus A. It's likely that such black hole central engines generate the radio, X-ray, and gamma-ray energy radiated by Centaurus A and other active galaxies. For an active galaxy Centaurus A is close, a mere 10 million light-years away, and is well-studied by earthbound astronomers. At the bottom of this image, globular star cluster Omega Centauri (NGC 5139) is some 15,000 light-years away and 150 light-years in diameter. Packed with about 10 million stars much older than the Sun, Omega Cen is the largest of 200 or so known globular clusters that roam the halo of our Milky Way galaxy. Though most star clusters consist of stars with the same age and composition, the enigmatic Omega Cen exhibits the presence of different stellar populations with a spread of ages and chemical abundances. In fact, Omega Cen may be the remnant core of a small galaxy merging with the Milky Way (text adapted from APOD).
  • The Trifids, M20. LRGB Lum 7x10m bin 1x1, RGB each 12x5m bin 2x2. Taken with TEC 140 @f7 and FLI ML8300 camera at -30C.<br /> Shot July 05,09,10, 2012 by Lynn Hilborn, WhistleStop Obs,Grafton, Ontario. COVER PHOTO, SkyNews Magazine, September 2012.<br /> M20 (Trifid Nebula) (Barnard 85) (NGC 6514)<br /> <br /> Distance: 5500 to 9000 light years<br /> <br /> Right Ascension: 18 : 02.3 (hours : minutes)<br /> Declination: -23 : 02 (degrees : minutes)<br /> <br /> Text Copyright Robert Gendler 2006<br /> A gem of the summer sky, M20 allows us a view into the exciting science of star birth. M20 is a young HII region (300,000 years old) about 30 light years across and is illuminated by the O-type supergiant HD 164492 at the center of its trilobed emission cloud. The ionizing star is about 30 times the mass of our sun and is the "A" component of a triple system ( A, B, and C components). In all there are seven members (HD 164492 A through G) of the small cluster packed within a half light year at the center of M20. As an HII region M20 is similar to M42 in its complexity and relationship to its parent molecular cloud but is much younger. A large blue reflection cloud forms the northern border of M20 and is illuminated solely by the F-type supergiant HD 164514. Recent X-ray and infrared observations have discovered an amazing array of very early stars and protostars within M20 giving us a rare glimpse of the earliest stages of star birth.<br /> <br /> Stars in the earliest formative stages are difficult to detect optically as they are shrouded from view by their parent molecular cloud. They reveal their presence by jets and outflows of gas which characterize their unstable and turbulent beginnings. The power of infrared observations (Spitzer Observatory) allows astronomers to "see" beyond the cloak of gas and dust that obscures young stars. Large populations of the earliest protostars or pre- main sequence stars (Class O and I) have been detected along the filamentary dark lanes near the reflection component. More evolved protostars (Class II) are found along ionization fronts within the rounded brighter parts of the emission cloud. Text with thanks to Robert Gendler.
  • North American nebula to the Dark Horse..Canon 60D modified 2000 ISO 10mm fisheye lens f2.8. 12 exposures x 1minute each.<br /> Taken by Lynn Hilborn, Grafton,Ontario July 15 2012.
  • The world revolves around Shelter Valley...Shelter Valley Folk Festival star trails. 95 x 1 minute each, Canon 60D sigma 10mm lens @ f2.8, 1000 ISO. Taken by Lynn Hilborn, Grafton, Ontario on June 26, 2012. Picture appeared in November 2012 SkyNews magazine
  • 'Best in Show', 2011 Starfest Image Salon<br /> vdB 141 'Cosmic Surfers' in constellation Cepheus . <br /> Lum 18x10m bin 1x1, RGB 12x5m each bin 2x2, taken with TEC140 and FLI ML8300 camera.<br /> Taken by Lynn Hilborn, WhistleStop Obs, Grafton Ontario on June 02 and 06, 2011.<br /> <br /> Published in Sky&Telescope Magazine, October 2011 edition
  • New Camera Lens...Tokina 300mm f2.8 connected to ML8300 camera. IC1396, 8 hours of exposure, Ha bin 1x1 6x30 minutes, OIII binned 2x2 6x30 minutes, SII binned 3x3 4x30 minutes. 3.5 arcsec/pixel. Still have to adjust for some coma but quite surprised and pleased with the light gathering power of this lens. October 06, 2011.<br /> Published as Cover photo...The Journal, Royal Astronomical Society of Canada, December 2011
  • Hickson Galaxy Group 68 and NGC 5371, in Canes Venatici. NGC 5371 is a spiral galaxy seen face-on. It is classified as an Sbc barred spiral galaxy and located about 100 million light years from Earth. Together with Hickson Galaxy Group 68, NGC 5371 makes up the Big Lick Galaxy Group. 6 hours of exposure. <br /> ***** Editors' Choice, Sky and Telescope magazine photo gallery.<br /> Taken by Lynn Hilborn, WhistleStop Obs, Grafton, Ontario on May 15 2012.<br /> Lum 1x1 19x10m, RGB each 2x2 12x5m. TEC 140 @f7 and FLI ML8300 camera with Baader filters
  • Flaming Star Nebula (IC405) and Tadpoles (IC410) in HaRGB...5 hours of Ha 15x20m binned 1x1, 4x5m each RGB binned 2x2.<br /> NP101is at f4.3 and FLI ML8300 camera. Taken by Lynn Hilborn, WhistleStop Obs, Grafton, Ontario November 10, 2009. Cover of SkyNews Magazine May/June 2010. ( Reprocessed in LAB, April 2011.)
  • NGC 3718 galaxy pair...TEC 140 @f7 and FLI ML8300 camera. Taken by Lynn Hilborn, WhistleStop Obs, Grafton, Ontario on March 17,2013. LRGB Lum 12x10m 1x1, RGB 8x5m each 2x2.<br /> <br /> NGC 3718 and its companion NGC 3729 are physically related members of the Ursa Major galaxy cluster. The two galaxies appear to orbit each other at a projected separation of 147,000 light years. NGC 3718 seems to have a rudimentary bar and spiral structure although it is recognized as a peculiar galaxy and as such is listed within Arp's Atlas of Peculiar Galaxies. Its most prominent feature is its extraordinary dust lane and strongly warped disk which gives an S-shaped appearance. The dust lane runs through the entire stellar bulge of the galaxy and stretches some 80,000 light years in its full extent. The disk is seen almost edge on at the center and is strongly warped to almost 90 degrees, a situation quite unique among galaxies.<br /> <br /> The peculiar dust lane covers a large part of the galaxy's main body and extends all the way into the nucleus. Because of the strong warp, features seen close to the nucleus are actually far from the center being seen in projection. The warp is also present in the very complex gaseous infrastructure of the galaxy observed at radio wavelengths. Three dimensional reconstructions of the galaxy suggest that in some viewing angles its appearance may seem quite normal suggesting that other galaxies with similar severe warps could go unnoticed. Warping of galactic disks is a relatively frequent phenomenon although the cause of disk warping is still uncertain. Warping in most cases is believed to be due to tidal forces exerted by neighboring galaxies. In the case of NGC 3718 the most reasonable explanation is its close proximity to NGC 3729 which is likely responsible for the strange configuration of the galaxy. Other explanations for warping such as twisting forces exerted by massive outer halo structures has been suggested and may possibly play a role. The prominent dust lane of NGC 3718 is remarkably similar to another well known southern galaxy, NGC 5128 (Centaurus A), which is considered to be its southern counterpart.<br /> <br /> NGC 3718 contains an active galactic nucleus (AGN) and is known as a Seyfert type 1.9 galaxy. HI mapping of the galaxy shows a suggestion of a tidal tail that starts on the eastern side of the galaxy and extends north towards its companion NGC 3729 strongly suggesting a gravitational relationship between the two galaxies.<br /> <br /> A grouping of 5 background galaxies 300 million light years distant are projected to the south of NGC 3718 and are designated Arp 322 (also Hickson 56). Several members of the group appear to be a strongly interacting. This field of interesting galaxies highlights the collection of peculiar galaxies published by the American Astronomer Dr. Halton C. Arp. In 1966 Arp published a catalog of 338 unusual or peculiar galaxies and interacting groups using film images taken by the Palomar 200 inch telescope. Description with permission of Dr. Robert Gendler.
  • NGC 7822 Taken with Tec140@f5.6 Ha 12x30m (bin1x1), OIII 8x30m (bin 2x2), SII 5x30m (bin2x2). Total 12.5 hours. FLI ML8300 camera and Takahashi NJP mount.<br /> Imaged Nov 1,4,5,2011 at WhistleStop Obs, Grafton, Ontario by Lynn Hilborn. <br /> Editor's Choice, Sky & Telescope photo gallery<br /> <br /> Hot, young stars and cosmic pillars of gas and dust seem to crowd into NGC 7822. At the edge of a giant molecular cloud toward the northern constellation Cepheus, the glowing star forming region lies about 3,000 light-years away. Within the nebula, bright edges and dark shapes are highlighted in this colorful skyscape. The image includes data from narrowband filters, mapping emission from atomic oxygen, hydrogen, and sulfur into blue, green, and red hues. The atomic emission is powered by energetic radiation from the hot stars, whose powerful winds and radiation also sculpt and erode the denser pillar shapes. Stars could still be forming inside the pillars by gravitational collapse, but as the pillars are eroded away, any forming stars will ultimately be cutoff from their reservoir of star stuff. This field spans around 40 light-years at the estimated distance of NGC 7822. Text from APOD.
  • Garradd, galaxies and a globular....Comet Garradd ((C2009 P1), background galaxies and globular cluster M92. Lum 1x1 300seconds, RGB 2x2 each 120 seconds. TEC 140 @ f5.6 and FLI ML8300 camera at -30. Taken by Lynn Hilborn, February 3, 2012 at 4am, WhistleStop Observatory, Grafton, Ontario.<br /> When comets float by deep-sky objects, the combination can be beautiful. But it’s also deceiving. Here, Comet C/2009 P1 (Garradd) passes globular cluster M92, which lies in the constellation Hercules. At the time of this image, Comet Garradd shone at magnitude 7.1 and was approximately 154 million miles (248 million kilometers) from the Sun. M92, on the other hand, shines at magnitude 6.5 and lies some 26,000 light-years away — 990 million times more distant than the comet! <br /> Image was published in SkyNews magazine (May/June 2012)
  • M106 and NGC 4217. Taken by Lynn Hilborn, WhistleStop Obs, Grafton, Ontario, March 11,13,14,21,25,2012. TEC 140 @f5.6 and FLI ML8300 camera with Baader filters. 9 hours Ha, 5.5 hours Lum, 6hours RGB total ( 2 hours each) for total of 20.5 hours of exposure.<br /> Shown here in red are the high energy jets of M106 emanating from the supermassive black hole in the galaxy's center. The jet creates a shock wave that excites material in the galaxy's halo, seen here in the ionized light emitted by hydrogen atoms. Photo appeared on back cover of the RASC magazine The Journal
  • IC 1311 in Cygnus<br /> The field in this image is from the constellation of Cygnus. IC 1311 is the designation for a star cluster with nebulosity. The main core of the cluster is a small dense knot of stars toward the right of center in this image. The general region is rich with hydrogen emission as evidenced by the red nebulosity. The cluster is located approximately 4,000 light years from Earth. North is up in this image.<br /> Image center is located approximately - Equatorial 2000: RA: 20h 12m 54s Dec: +41°12'18"<br /> Taken June 30, 2012 and Aug 24, 2012 by Lynn Hilborn<br /> TEC 140 @ f7<br /> ML 8300 -30<br /> WhistleStop Obs, Grafton<br /> <br /> RGB 9x5m 2x2<br /> Ha 1x1 11x20m
  • The 'Angel Nebula' (Integrated Flux Nebula - IFN). I only know of 3 other images of this object. Captured with a Canon 200mm f2.8 lens and FLI ML 8300 camera with a total 9 hours of exposure. Taken on April 12 and 13, 2012 by Lynn Hilborn, WhistleStop Obs, Grafton,Ontario. Central star is HIP51521 about 4.5 degrees from M82.<br /> As noted astrophotographer Rogelio Bernal Andreo writes...<br /> in simple terms, the IFN is dust clouds. However, unlike most known nebulae, they do not reflect, <br /> scatter or fluoresce due to the radiation of any individual star or cluster of stars, but do so <br /> from the integrated flux of all the stars in the Milky Way Galaxy. In other words, the IFN is <br /> illuminated by the glow of our own galaxy.<br /> Because the IFN is so faint, capturing it is a challenge, as even under good skies it will sit barely above the noise. This means that once you've captured the data and try to bring the signal from the IFN, you will bring it along with the noise in the image, making it almost impossible to discern between noise and nebulae. This is the main reason most images won't show any or almost any IFN - as astrophotographers deal with the noise - trying to make it dissapear - the IFN will dissapear with it. The IFN is relatively faint and not very well studied. . In addition to the blue hue characteristic of reflection nebulae, the galactic cirrus also emits a faint reddish glow as UV light from the Milky Way’s stars is absorbed and re-emitted in the red spectrum. Text with the kind permission of Rogelio Bernal Andreo (DeepSkyColors.com)
  • Dark Nebula LDN 1235 and LDN 1251 shot with 200mm camera lens. 8 hours of exposure with FLI ML8300 camera and Baader LRGB filters.<br /> Taken with Canon 200mm f2.8 lens. Imaged on September 11,12,13,2012 by Lynn Hilborn,Grafton,Ontario.<br /> 21x10min Lum, 9x10m each RGB all binned 1x1.
  • Heart and Soul nebula in narrowband Hubble colors. Taken with 200mm Canon lens @ f2.8 and ML8300 camera. Ha,OIII,SII each 3x30 minutes for total 4.5 hours exposure. Taken by Lynn Hilborn March 31, April 5, 6 2012 at WhistleStop Obs,Grafton,Ontario.
  • Giant molecular cloud and dust lanes in Perseus. On the left is IC348 a bright young cluster settled in the reflection nebula of this giant cloud. On the right side of this 2 frame mosaic is NGC 1333 and area of star birth surrounded by dark lanes of cosmic dust.<br /> The data was gathered eighteen months ago and reprocessed March 2012 to enhance the image. This is a two panel mosaic with a total 18 hours of exposure. Taken by Lynn Hilborn at WhistleStop Observatory, Grafton, Ontario.<br /> The actual imaging was done Oct 10, 12, 31 and Nov 1,2, 2010. The scope was a NP101is @ f4.3 and FLI ML8300 camera.<br /> The image is LRGB plus Ha. <br /> Original image was Editor's Choice ,Photo Gallery- Sky and Telescope magazine; published in Sky and Telescope magazine, May 2011 edition; published as back cover RASC Journal April 2011; Astronomy Magazine 'Picture of the Day'
  • NGC 2264 (Christmas Tree cluster) (Cone Nebula Region) in HaRGB. 9.5 hours of exposure with TEC 140@f5.6 and FLI ML8300 camera. Taken by Lynn Hilborn, WhistleStop Obs, Grafton, Ontario. Imaged on Feb 19 and 20, 2012.<br /> <br /> NGC 2264 is a young galactic cluster of stars in the Monoceros OB 1 association which resides in the Orion arm of the galaxy. The cluster has a total of over 600 stars ranging in age from from 1 to 4 million years old. The diverse population of the cluster includes several dozen OB stars and over 400 lower mass stars. The brightest members of the cluster resemble a "Christmas Tree" with S Monocerotis at its base and the Cone Nebula at its apex. The juxtaposition of dark dust clouds and glowing gas has carved out the landscape we see in the cone nebula region. The conical shaped pillar of gas and dust is called the Cone Nebula. It spans about 7 light years in length. A protruding portion of the cloud near S Monocerotis has been compared to the shape of a fox and was nicknamed the "Foxfur" nebula. Text with kind permission of Robert Gendler
  • Planetary Nebula IC 2448 Hubble Space Telescope data from the Hubble Legacy Archive processed by Lynn Hilborn, March 13,2013.<br /> IC 2448 is an elliptical planetary nebula in the constellation of Carina. Lying near the bright star Beta Carinae.
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