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.

“ Had I the heavens' embroidered cloths,
Enwrought with golden and silver light,
The blue and the dim and the dark cloths
Of night and light and the half light,”
W.B.Yeats



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June 07,2011 Super Nova data added to March 24,2011 color data. Super nova at approx 6 0'clock...Lynn Hilborn, WhistleStop Obs
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June 07,2011 Super Nova data added to March 24,2011 color data. Super nova at approx 6 0'clock...Lynn Hilborn, WhistleStop Obs

  • The Workhorse...WhistleStop Observatory, Grafton,Ontario
  • M101, Pinwheel Galaxy taken March 25.2011 ...prior to super nova explosion.<br /> TEC 140 2 f5.6 with FLI ML8300 camera, L 9x10m, RGB each 5x10m, Ha 9x20m, all binned 1x1.<br /> Taken by Lynn Hilborn, WhistleStop Obs, Grafton, Ontario
  • March 24 2011 data pre Super Nova
  • June 07,2011 Super Nova data added to March 24,2011 color data. Super nova at approx 6 0'clock...Lynn Hilborn, WhistleStop Obs
  • M51 Whirlpool Galaxy. TEC140 @f7 and FLI ML8300 camera, 70m L,60m each RGB, 120m Ha all binned 1x1.<br /> Taken March 2011 by Lynn Hilborn, WhistleStop Observatory, Grafton, Ontario.
  • Rho Antares...Canon 50D modified, Canon 200mm shot at f 4. 4x 10 minutes. Taken May 2009 by Lynn Hilborn, Grafton, Ontario.
  • M51 Whirlpool Galaxy 4 hours exposure LRGB (130m L 40m each RGB) . Taken @ f 6.3 with C9.25 and FLI ML8300 camera. June 07, 2010 by Lynn Hilborn, Grafton, Ontario <br /> M51 (NGC 5194 and NGC 5195) (The Whirlpool Galaxy)<br /> <br /> Distance: 37 million light years<br /> <br /> text copyright Robert Gendler 2006<br /> <br /> M51 was the first spiral structure ever observed by Lord Rosse in 1850 at a time when the true nature of galaxies was unknown. Its undeniable beauty explains its recognition as a true showpiece of the night sky. Probably less appreciated is that M51 represents a dramatic demonstration of an interacting pair of galaxies. As truly immense structures, galaxies are relatively large compared to the average distance between them. Most galaxies are separated by a distance of only 20 times their diameter compared to stars which are separated by 10 million times their diameter. As a result most galaxies are likely to encounter other galaxies at least a few times over their immense lifetimes. The encounters run the gamut from "major" mergers involving the collision of two comparable mass galaxies to more "minor" mergers involving the consumption of a small companion or satellite galaxy by the more dominant galaxy.<br /> <br /> Astronomers currently believe that galaxy formation is an ongoing hierarchical process. The basic form of a galaxy is established early in its history as the galaxy emerged from its primordial cloud. Billions of years later galaxies continue to evolve even in the present time, through major and minor mergers. Collisions and mergers certainly occurred with greater frequency in the early universe but without question continue into the present epoch as we observe many galaxies in the local universe, such as the M51 complex, showing the strong signatures of ongoing interactions. When encounters happen, the close proximity of the massive structures set up powerful gravitational forces known as tides. As the galaxies move closer the enormous attractive forces act to dramatically and often violently alter the structures of both participants.<br /> <br /> <br /> <br /> The 51st entry in Messier's list actually represents 2 galaxies. NGC 5194 (also known as M51A) represents the magnificent spiral, while NGC 5195 (also known as M51B) is likely an irregular type dwarf galaxy now located behind the larger spiral galaxy.<br /> There have been many attempts to explain the morphology and evolution of the NGC 5194/5195 system including its apparent tidal bridges and grand design spiral shape. Classic papers by Toomre (1972), Howard (1990), and Rots (1990) have provided valuable insight into the evolution of the M51 complex and are summarized below.<br /> <br /> Simulations suggest that NGC 5195 is located well behind NGC 5194 and that the two galaxies are now traveling away from each other. The two galaxies had their closest recent approach some 70 million years ago, when the less massive NGC 5195 encountered the disk of NGC 5194 in a highly inclined passage. The effects of that interaction include several conspicuous disturbed features as well as a general brightening and strengthening of the inner spiral arms of NGC 5194. The disturbed features include the marked asymmetry of the spiral arms both near and far (north and south) in relation to the companion NGC 5195. The near arm appears thin and extended and the far arm fans out as an extended tidally disturbed structure. The extraordinary plumes that extend north, northwest, and southeast from the companion were likely torn from it as it engaged the more massive spiral in its recent encounter. The apparent spiral arm-bridge (northern arm) between the two galaxies is an illusion as NGC 5195 is far behind the NGC 5194, the near spiral arm being superimposed over the disk of NGC 5195 in the same line of sight. A visible area of intense star formation is conspicuous near the nucleus of NGC 5195 and was almost surely triggered from the time of the recent approach. Not all the disturbed features of the M51 complex are believed to be from the recent encounter. Radio surveys have detected an immense gas cloud with no optical counterpart that fans out along the eastern side of the M51 complex, extending some 300,000 light years in length and carrying about 500 million solar masses. It appears to be an extension of the optically apparent far spiral arm but is most likely an independent feature and a relic from a previous crossing that occurred as much as 400 million years ago.<br /> <br /> The ultimate fate of the M51 complex will likely be a gradual decay in the orbit of the companion (the orbital period now is about 500 million years with a major axis of about 50,000 light years) towards a final merger with the spiral and eventual tidal breakup of the companion in about 1 to 2 billion years.
  • Heart Nebula (IC1805) done in narrowband with SII Ha OIII filters. Total exposure of 18 hours. Taken Sept 10,17,19,20,2010 by Lynn Hilborn, WhistleStop Obs, Grafton,Ontario.<br /> FLI ML8300 camera and NP101is @ f4.3
  • Now for something different....seen through our dining room window, looking towards the observatory. Ouch !!<br /> Taken by Lynn Hilborn, Grafton, On Sept 07, 2010. Canon XS.
  • BEST IN SHOW...Starfest Imaging Salon 2010...<br /> Iris Nebula, NGC 7023....8.5 hours ( 330m Lum 1x1, 60m each RGB 2x2). NP 101is @ f4.3 and FLI ML8300 camera. Taken Nov 16 and 17, 2009 by Lynn Hilborn, WhistleStop Obs, Grafton, Ontario.<br /> <br /> The bright star HD 200775 shines through the nebula NGC 7023 like a beacon through a celestial fog. The illuminating star of the nebula is designated HD 200775, a 10 solar mass star centrally imbedded in a region surrounded by ambient molecular cloud material. Optically the light we see from reflection nebulae such as NGC 7023 is starlight reflected from the surface of innumerable small dust particles. Historically this was proven by showing the similarity of the spectra of the central illuminating star and its nebula. Aside from the reflected light of its central star, the microscopic dust particles also emit radiation in the infrared. We see the optical counterpart of this emission in the low level light of the dark dust clouds surrounding the bright nebula on its south and west side, respectively catalogued as L 1172 and L1174. Recent infrared studies of NGC 7023 indicate the presence of complex molecules such as polyaromatic hydrocarbons formed within the dust cloud. NGC 7023 is located at the northern end of a vast and optically invisible molecular cloud in an area where low and intermediate star formation is occurring. The central star is at the center of a small cluster of low and intermediate mass pre-main sequence stars similar to HD 200775. HD 200775 is a variable star and part of an eccentric binary system with a periodicity of 3.7 years.<br /> <br /> The distinct hourglass shape of the nebula was formed by the interactions of the central star with the surrounding ambient dust cloud. HD 200775 is a B3 type pre-main sequence star known as a Herbig Be star. Herbig Ae/Be stars are intermediate mass (1-10 solar masses) pre-main sequence stars similar to their lower mass "solar size" counterparts, the T-Tauri stars. They are usually associated with dust and reflection clouds but unlike their more massive OB cousins they cannot form extended HII regions. That said, HD 200775 is one of the brightest Herbig Be stars known. With a temperature of 17000 degrees Kelvin it is hot enough to form a small HII region within a small radius of the central star. The small HII region is apparent optically as the ruby lips of the nebula just to the north and south of the central star. Studies of the star and nebula at radio wavelengths show the star is located within a bilobed cavity of gas whose walls delineate the exact borders of the optical nebula. The cavity is about 5 by 2.5 light years in dimension and lies in a northeast-southwest orientation. There is a small region of ionized gas (small HII region) surrounding the central star which is perpendicular to the lobes. HD 200775 most likely formed the bilobed cavity at an earlier stage in its evolution. Bipolar outflows from the contracting pre-main sequence star most likely excavated the bilobed cavity which formed the template for the physical structure of the nebula. The lack of any high velocity gas within the nebula at present suggests that the outflows no longer exist. The lobes show a slightly off center symmetry. The center of symmetry is located about 1/3 of a light year west of the star indicating that the central star has since moved since the earlier time of its outflows. (Text from Robert Gendler)
  • M8 and M20..the Lagoon nebula and the Trifids. Taken with a DSLR, Canon 50D modified and Canon 200mm f2.8 lens. Imaged May 25,2009 by Lynn Hilborn, WhistleStop Obs, Grafton...reprocessed Feb, 2013.<br /> Image is a stack of 9 exposures - 3x1minute,3x5minute,3x10minute, tracked on a Losmandy G11 mount
  • NGC 3718 and 3729 (ARP 214), 200 minutes Lum and 70 minutes each of RGB with C 9.25 @ f6.3 and FLI ML 8300 camera.<br /> Taken over 2 nights in May 2010 by Lynn Hilborn, WhistleStop Obs, Grafton, Ontario. Reprocessed Feb 2013.<br /> <br /> Text by Robert Gendler...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.
  • California Nebula NGC 1499<br /> Drifting through the Orion Arm of the spiral Milky Way Galaxy, this cosmic cloud by chance echoes the outline of California on the west coast of the United States. Our own Sun also lies within the Milky Way's Orion Arm, only about 1,500 light-years from the California Nebula. Also known as NGC 1499, the classic emission nebula is around 100 light-years long. It glows with the red light characteristic of hydrogen atoms recombining with long lost electrons, stripped away (ionized) by energetic starlight. In this case, the star most likely providing the energetic starlight is the bright, hot, bluish Xi Persei, just near the nebula and at the bottom of picture center. (Text adapted from Astronomy Picture of the Day)<br /> ..5 hours of Ha (20m x 9 and 15m x 8) binned 1x1, 2x10m each RGB binned 2x2.<br /> NP101is @ f4.3 and FLI ML8300 camera. Taken on March 7 and 8, 2010 by Lynn Hilborn at WhistleStop Obs, Grafton, Ontario.
  • WhistleStop Observatory...roof open at 3:45am Sept 18,2010.<br /> 1600 ISO f4 12mm 40 seconds.
  • PACMAN Nebula in Hubble narrowband colours SII/Ha/OIII for RGB. Cropped version taken with NP101is @f4.3 and ML8300 camera August 26-29, 2010 by Lynn Hilborn, WhistleStop Observatory, Grafton,On<br /> Ha bin 1x1 8x20m, OIII bin 2x2 9x15m, SII bin 2x2 12x15m
  • The Wizard , NGC 7380 , done in Hubble palette (SII Ha OIII) with 3 hours of Ha binned 2x2 and 1.5 hours each of SII and OIII binned 3x3...total 6 hours. C 9.25 @ f 6.3 and ML8300 camera. Taken by Lynn Hilborn, Grafton, Ontario on July 2 and 4, 2010
  • Crescent Nebula 3 hours of Ha and 30m each RGB. Taken May 24 with C 9.25 @ f6.3 and ML 8300 camera.<br /> Whistle Stop Obs.
  • Edge-on spiral galaxy NGC891 some 30 million light-years from earth. Taken Nov 8, 2010 by Lynn Hilborn, WhistleStop Obs, Grafton, Ontario. Look at this under the "original" view (put cursor on image and hit "O") and count the number of background galaxies.<br /> TEC 140 @f7 (980mm) and FLI ML8300 camera. LRGB L 7x20m 1x1, RGB each 9x5m 2x2.
  • The Witch's Broom...4.5 hours of exposure with a modded Canon50D. Taken by Lynn Hilborn at WhistleStop Obs, Grafton, Ontario...June/July 2009. NP101is, G11 Gemini, PHD guiding, ISO1600.
  • Christmas Tree Nebula<br /> Lynn Hilborn, November 2009. ML8300 and NP101is at f4.3
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