SH2-86 imaged with 18 Ha data set 1800 seconds each, OIII 16 data set 1800 seconds each and SII 16 data set of 1800 seconds each.

LBN 468 Gyulbudaghian's variable nebula. This is a bipolar reflection nebula similar to NGC 2261. This was discovered by a Russian astronomer in 1977 by Armen Gyulbudaghian. The nebula has undergone different shapes and luminosity throughout its lifetime from the shockwave of its contracting pulsar  PV cephei.

Rho Ophiuchi cloud complex has an angular area of 4.5 x 6.5 degrees and consists of two major regions of dense gas and dust. Temperature of the clouds range from 13-22K, and there is a total of about 3,000 times the mass of the Sun in material.. The gas diameter of Rho is nearly twice the mass of Jupiter. The star system is only 400 light years away in the constellation Ophiuchi. 

   This is an ongoing project that will require from 3 to 6 panels of imaging to complete the full area of the sky and may take an additional year to complete.

​This particular frame was imaged on 041616.

California Nebula imaged on 110116 with a Takahashi ED-106 III using a Paramount Mty Mount and a QSI-683 CC Camera. This is from a 2 panel mosaic of 151 600 Second sub exposures in LRGB for a total of 25 hours imaging.

The Iris Nebula imaged with the QSI-683 CCD Camera from 25 hours of data collection.

These clouds of interstellar dust and gas are from 1,300 light years away in the constellation Cepheus which is called The Iris Nebula. Within the Iris are dusty nebula material surrounding hot young stars. The dominant color of the brighter reflection nebula is blue, which are characteristics of the dust grains reflecting starlight. The blue petals of The Iris Nebula span about six light-years.

The Orion Nebula

Cassiopea's Ghost imaged from 16 subs green, 16 subs blue, 16 subs red all 600 seconds, plus 23 subs of 900 seconds in Ha 5nm Astrodon filter. for a total of about 15 hours imaging time. The telescope used is a Takahashi 106-ED III with a Paramount Mty Mount and a QSI 683 WGS-8.

   IC 59 is on the right side of frame with IC 63 located in the center of frame. These two nebula are a combination of faint shaped emission and reflection nebula located about 600 light years away in the constellation Cassiopeia.. The two nebula together are about 10 light years across.

    The blueish glow shinning down on IC 59 from the top comes from the intense radiation of the bright hot blue star Gama Cassiopeia that is located 3 light years away from the nebula. The radiation from the nebula is slowly evaporating and lighting up these shapes of gas and dust.

  IC 63 is dominated by red H-alpha light emitted as the ionized hydrogen atoms recombine with electrons.

A wonderful example of IC 447, IC 446, B37 and the red cone nebula. Captured in HaLRGB Subsets of 16 sub- exposures each at 900 seconds and the Ha set at 10 subs. of 1800 seconds each.

Cacoon Nebula imaged from Deep Sky West in New Mexico

The Crescent Nebula recently imaged in the month of June 2018 from 10 subexposures each in Ha and OIII from 30 minute guided exposures for a total of 10 hours image time. I may go back and attempt to gather more data as night time temperatures drop.

M82 & M81 imaged on 021216 with the QSI-683 CCD Camera using 39 900 second Luminance  filter subs,  18   300 second Blue filter subs, 19 300 second Red filter subs, 14 300 second green filter subs for a total of about 13 hours image run.

Forming a striking pair in a small telescope with nearby spiral galaxy M81 on the right, M82 the Cigar Galaxy on the left is being physically affected by its larger neighbor. Tidal forces caused by gravity have deformed this galaxy, a process that started about 100 million years ago. This interaction has caused star formation to increase tenfold compared to "normal" galaxies.

​Recently, M82 has undergone at least one tidal encounter with M81 resulting in a large amount of gas being funneled into the galaxy's core over the last 200 million years.

​Just to ponder the distance looks close between the two galaxies, but in reality they are actually separated by about 130,000 light years  from each other.

LBN 777 Imaged with 25 hours of data from the Takahashi 106-ED Telescope with the Paramount MTY Mount using the QSI 683 CCD Camera.

​LRGB set of 900 seconds each with 17 subs each in RGB and Luminance with 43 subsets at 900 seconds each during Nov. 2015 capture.

​This nebula is known  as the Vulture Head Nebula and is a very faint reflection nebula 5 degrees northeast of Pleiades. LBN 777 is surrounded by a dusty molecular cloud and Bernard 207 which can be seen  as a brown patch of the Eagles Eye.

IC 1318 is the diffuse emission nebula surrounding Sadr which lies in the center of Cygnus's cross.  In this captured image Sadr is located on near the upper right corner of frame. This was imaged from approximately 14 hours of data in RGB.  Imaged with Takahashi 106-ED with the Paramount MTY-Mount and the QSI-683 CCD Camera on 051216. 

 This is the new updated version with 11 additional subs of Ha 1800 seconds each depicting so well this spectrum in the image.

The Wizard Nebula imaged using 17 subs. in SII 1800 seconds each, 18 OIII subs. 1800 seconds each and 21 Ha subs. 1800 seconds each using a Takahashi 106-ED III Telescope on a Paramount Mty Mount attached to a QSI-683 WSG-8 ccd camera. The data was obtained in October 2016.

The Crab Nebula from a single 2400 second set using Ha,SII and OIII filters with Red assigned to SII , Ha Green filter and OIII blue filter.

VDB 141 imaged on 103016 from 23 luminance subs of 900 seconds each, and 16 subs each in RGB of 600 seconds each.

The Leo Triplet imaged with the QSI 683 CCD Camera from 14. hours of integration time. This is a small group of galaxies about 35 million light years away in the constellation Leo. The galaxy group consists of spiral galaxies M65, M66 and NGC 3628.

Westerhout 5 (Sharpless 2-199, LBN 607, Soul Nebula) is an emission nebula located in Cassiopeia. Several small clusters are embedded in the nebula, in the head CR 34,632 and 634.. IC 1848 are  located in the body and the cluster designation is IC 1848.

   Small emission nebula IC 1871 is present just left of the top of the head, and small emission nebula 670 and 669 are just below the lower back area.

   The galaxies Maffei 1 and Maffei 2 are both nearby the nebula, although light extinction from the Milky Way makes them hard to see. Once thought to be part of our local group, they are now known to belong to their group- the IC 342/Maffei Group.

​Below this  image is the same Soul Nebula ; but with just the Ha data to bring out finer details in the dust.

The Rosette Nebula assigned straight Hubble Palette of SHO with SII using 20 subs of 1800 seconds each, OIII at 16 subs. 1800 seconds each, and Ha at 16 subs. 1800 seconds each for a total of 26 hours exposure time.. The telescope used is a Takahashi 106-ED- III at f5 520mm, attached to a QSI-683 CCD camera. The mount is a Paramount MTY Mount. The other images of The Rosette are using the same equipment and subexposures, but processing the filters in different color palette's.

The inner core cluster NGC 2244 and the nebula NGC 2237 lie at a distance of 5,000 light years away and measures 50 light years in diameter. The radiation from the young stars excites the atoms in the nebula, causing the to emit radiation themselves producing the emission nebula we see. The mass of the nebula is estimated to be around 10,000 solar masses.

May 2nd 2018 image of The Bubble Nebula from 2  30 minute guided exposures in Ha using the Celestron C14 at F7 2650mm. Looking forward to collecting 15 hours of data from this DSO as it rises higher in the night sky earlier. This image capture started at 3 A.M. local time P.S.T. and wanted to capture more 1800 second guided exposures but the Sun slowly rising 5 A.M. kept me from continuing.

Comet P67  

The above image was captured on April 3rd 2016 with a rare capture of Comet Churyumov-Gerasimenko P67 flying at incredible speed outside the frame in upper right of image.Discovered in 1969 it is a Jupiter family comet measuring 4.5 km. across. It has an orbital period of 6.5 years with its closest approach to the sun at 186m kilometers. Although it won't ever be close to Earth , the Rosetta spacecraft will give stunning 3D closeups of this speeding bullet.

   The galaxy NGC 3628 also known as the Hamburger Galaxy is about 36 million light years away in the constellation Leo. The tidal wave is approximately 300,000 light years long.

​This was imaged from a combination of 69 subexposures from LRGB Astrodon filters for a total of 14.2 hours image time with the Takahashi 106-ED telescope and a Paramount Mty Mount. The ccd camera is a QSI-683

This is an updated version of The Crescent Nebula from about 80 hours of imaging time to produce the OIII shell depicted in image.

A rare image of LBN 782 imaged in 120116 using 23 luminance, 16 red, 16 green and 15 blue filters of 900 seconds each using a Takahashi 106-ED III telescope with a Paramount Mty telescope. The camera is a  QSI 683 WSG-8 CCD Camera.

The Needle Galaxy NGC 4565 ; a recent image from April 2018 using my updated system consisting of a modified Classic C14 captured at 2650mm F7 with a Starizona coma corrector focal reducer. Camera is a QSI 683 WSG-8. Mount used is a Paramount PME. This so far is a total of about 15 hours combined LRGB data set.

The Cave Nebula is featured by the dusty reddish glow from the Sharpless catalog emission region SH2-155. This is about 2,400 light years away in the constellation Cepheus. The Cave Nebula was formed at the boundary from the massive Cepheus B molecular cloud and the hot, young, blue stars of Cepheus OB3.  The stellar nursery is about a staggering 10 light years across.

Copyright Protected Don Curry Please do not share or copy without permission from Originator

The above image is a cropped​ version of the above M81/M82 image. I wanted to bring out the core details of M82 known as the Cigar Galaxy or the Starburst Galaxy. I had to rescale and enlarge considerably in Photoshop so you can see the inner core activity going on in intense drama with so much energy being released and new star births forming.


​In 2005 , the Hubble Space Telescope revealed 197 young massive clusters in the starburst core. The average mass of these clusters is around 200,000 solar masses, thus making the starburst so active. Within the galaxy's center young stars are being born 10 times faster then they are in our entire Milky Way galaxy. In the core of M82 four high surface brightness regions or clumps (designated A , C, D, and E) are detectable in this region at visible wavelengths. M82's unique bipolar outflow  or superwind appears to be concentrated on clumps A and C and is fueled by energy released by supernovae within the clumps which occur at a rate of about one every ten years.

The Chandra x-ray Observatory detected fluctuating x-ray emissions from a location approximately 600 light-years away from the center of M82. Astronomers have postulated that this fluctuating emission comes from the first known intermediate-mass black hole, of roughly 200 to 5000 solar masses. M82, like most galaxies, hosts a supermassive black hole at its center with a mass of approximately  (3 x 10 to the 7th power)  solar masses as measured from stellar dynamics.

In 2010, radio astronomers discovered an unknown object in its core. The object started sending out radio waves, and the emission did not look like anything  seen in the universe before. theory's suggest it may be a microquasar SS 433.

The object is located at several arcseconds from the center of M82 which makes it unlikely associated with  the supermassive black hole. It has an apparent superluminal motion of four times the speed of light relative to the galaxy center. Apparent superluminal motion is consistent with relativistic jets in massive black holes and does not indicate that the source itself is moving above lightspeed.

Most recent image The Markarian Chain imaged with equipment previously listed on this page taken in LRGB 900 second subs of 15 each L channel was 19 on 010717 in Rowe New Mexico. The NGC galaxies are vast and plentiful in this capture. consisting of : NGC 4479, 4477, 4474, 4473, 4461, 4459, 4458, 4440, 4438, 4436, The Eyes 4435, 4425 , 4413,, M86, NGC 4406, 4402, 4388, 4387, M84, NGC 4374


Bubble Nebula captured from about 32 hours of data imaging. I'll go back to this after monsoon season is over and attempt at full resolution in September 2018.

The above image depicting the Eastern Veil Nebula above and part of the Western Veil Nebula below imaged from a Takahashi 106-ED Telescope with the Paramount MTY Mount and the QSI 683 WSG-8 CCD camera .

The image is from an LRGB set of approximately 25 hours total on 08/25/16; which includes a blend of the Ha data set.

​The above data  set of 13 1800 second subs in Ha depicts the image in full frame uncropped.

​The Veil Nebula is a cloud of heated and ionized gas and dust in the constellation Cygnus.. It constitutes the visible portion  of the Cygnus Loop, a large faint remnant. The supernova exploded sometime near 3,000 to 6,000 B.C. and the remnants since then have expanded to cover and area 3 degrees in diameter or roughly 6 times the size of a full moon. The analysis of the emissions suggest the presence of oxygen, sulfur and hydrogen..

" The Elephant Trunk is a concentration of interstellar gas and dust within the much larger ionized gas region IC 1396 located in Cepheus about 2,400 light years away from Earth. The dense bright rim is the surface of a dense cloud that is being illuminated and ionized by the massive (HD 206267 star) that is just west of IC 1396A. 

    The Elephant's Trunk nebula is now thought to be a sight of star formation containing several young ( less than 100,000 yr) stars that were discovered in infrared in 2003. Two of the older stars which have lived for billions of years are present in the small, circular cavity in the head globule. Winds from these young stars may have emptied the cavity.

  The combined action of the light from the massive star ionizing and compressing the rim of the cloud, and the wind from the young stars shifting gas from the center outward lead to very high compression in the Elephant's Trunk nebula. This pressure has triggered the current generation of protostars." Source Cite Wikipedia"

Total image time approximately 25 hours using SHO Narrowband filters in Sulfur, Hydrogen Alfa, and Oxygen III. Subs were 1800 seconds each using the same equipment as above from previous image. Imaged on 092215 at Deep Sky West observatory in Rowe New Mexico.

The Rosette Nebula imaged 10/25/16 in SHO Palette assigned Ha, OIII , OIII with a Takahashi 106-ED telescope on a Paramount MTY- Mount with the QSI-683 CCD camera from about 26 hours of exposure.

NGC 3628

Here is the same image in Ha using 18 x 1800 second exposure subs and 5 x 2400 second exposure subs in Ha as well. This was imaged on 033116 using the Takahashi 106-ED III Telescope with the QSI -683 ccd camera and the Paramount Mty Mount.

SH2-64 is a emission nebula published by Stewart Sharpless in 1959. It is in the constellation Serpens. SH2-64 is the red nebula  Also depicted is a huge amount of expansive gas along with obvious dark nebula as well. The dust is from the Aquila Rift dust clouds which are located between W 40 an our solar system.

 Subexposure total 35 600 second Luminance, and 16 each subs. 600 seconds each in RGB filters during 070116 at Rowe New Mexico. The telescope is a Takahashi 106-ED III attached to a Paramount MTY Mount. The camera employed is a QSI-683 WSG-8.

This is Messier 101 from nearly 30 hours of collected data. 18 hours of Luminance and 13 hours of RGB with most images at 900 seconds each and along with many 10 minute unguided images in Luminance as well.

Here is the same image in HaHaOIII palette where red filter is assigned Ha, green Ha, and Blue OIII.

NGC 6888 The Crescent Nebula in Bi-Color OIII & Ha filters used 18 subs 1800 seconds each on 033116.. Also the rare Bubble Nebula can be seen in the lower left of the image.

​The Crescent Nebula is an emission nebula in the constellation Cygnus about 5,000 light years away. It was discovered by Friedrich Wilhelm Herschel in 1792. It is formed by fast intense stellar wind from the Wolf-Raylet star WR 136 colliding with and energizing the slower moving wind ejected by the star when it became a red giant 250,000 years ago. The result of the collision is a shell and two shock waves, one moving outward and one moving forward. The inward moving shock wave heats the stellar wind to x-ray- emitting temperatures.