NGC 2655 is a lenticular galaxy in the constellation Camelopardalis. It is at a distance of 60 million light years from Earth. NGC 2655 is a Seyfert galaxy. This means it has an extremely luminous core powered by matter falling into a supermassive black hole.
The galaxy has asymmetric dust lanes in its center. It features tidal arms and extended neutral hydrogen gas. It may have recently experienced a merger. It is situated near the north celestial pole, making it circumpolar and visible year-round for observers in the Northern Hemisphere.
Imaging session management and control using Astro Photography bTool (APT 4.70.1). Subframe calibration, debayer, alignment, integration, and processing using PixInisght. Astrobin link for acquisition details and annotated image.
NGC 3384 (also known as NGC 3371) is a lenticular galaxy. It is located approximately 35 million light-years away. This galaxy is in the constellation Leo. It is a prominent member of the M 96 Group. This group is also called the Leo I Group. It includes the well-known Messier objects M 95, M 96, and M 105.
NGC 3384 and its neighbor M 105 are surrounded by a massive ring of neutral hydrogen. This ring is 650,000 light-years wide. Sparse star formation still occurs there. In the night sky, NGC 3384 forms a visual trio with the elliptical galaxy M 105. It forms this trio with (NGC 3379) and the spiral galaxy NGC 3389.
While M 105 and NGC 3384 are physical companions, NGC 3389 is a background galaxy located significantly further away. The galaxy hosts a supermassive black hole at its core. It has an estimated mass of 16 million times that of the Sun. This black hole is considered “quiet,” producing very little radio energy.
Image acquisition details in Astrobin. APT used for image acquisition and session automation. PixInsight used for subframe processing.
Sh2-282 (Sharpless 282) is a very faint Hii emission nebula in the constellation Monoceros. It is approximately 4,075 to 5,000 light-years away from Earth. It belongs to the second Sharpless catalog. It is situated in the north-central part of its constellation. The nebula is roughly 3° south of the famous Rosette Nebula.
The nebula is characterized by red hydrogen gas energized by radiation from nearby bright blue stars. It spans approximately 40 light-years in diameter. In apparent view, that’s 35 arc-minutes. The nebula contains eight cometary globules. These are dense, eroded pillars of gas and dust that are sculpted by stellar winds.
Sh2-223 is a faint emission nebula (H II region) located in a dense starfield in the constellation Auriga. It is a huge H II region, a large cloud of partially ionized gas where star formation can occur. It appears as a large, faint red arc or “wing” in deep-sky images. Its red glow comes from ionized hydrogen-alpha (Hα) emissions. The nebula is believed to be ionized by the star BD +41 1144 (an O7.5 V star) or possibly LS V +40 46.
In addition to the predominant Hii, there is also a significant amount of Oiii in the area. This leads to a bluish tinge or a slight purplish hue in parts of the image.
It is considered a difficult target for astrophotographers because of its extreme faintness. It often requires long total integration times, such as 25+ hours, to resolve clearly. Separating the IFN from the Hii nebula requires data. This photograph is only 11.4 hours. More to come in the future if the opportunity presents itself.
Messier 88 (M88 or NGC 4501) is a bright, multi-arm spiral galaxy located in the constellation Coma Berenices. As a prominent member of the Virgo Cluster, it is roughly 47 to 60 million light-years from Earth. M88 is one of the fifteen Messier objects that belong to the nearby Virgo Cluster of galaxies. It is galaxy number 1401 in the Virgo Cluster Catalogue (VCC). The catalogue includes 2096 galaxies that are candidate members of the cluster.
The galaxy is inclined at about 30 to 64 degrees to our line of sight. This inclination gives it an elongated, elliptical appearance through telescopes. It spans about 100,000 to 130,000 light-years in diameter, making it comparable in size to our Milky Way. It contains about 400 billion stars.
With an apparent magnitude of 9.6, it is visible in large binoculars as a blurry patch and reveals its spiral structure in larger amateur telescopes. The galaxy is best observed during the spring months, particularly in May.
NGC 4038 and NGC 4039 are known as the Antennae Galaxies. They are a famous pair of interacting spiral galaxies. They are located in the constellation Corvus. They are currently undergoing a violent galactic collision that began approximately 900 million years ago.
Key Characteristics Nicknames: Commonly known as the Antennae Galaxies or the Ringtail Galaxy. They are also cataloged as Caldwell 60/61 and Arp 244.
Distance: Estimates of their distance from Earth range between 45 million and 65 million light-years.
Appearance: Their name comes from two long “tidal tails” of ejected stars, gas, and dust that resemble an insect’s antennae. These tails span over 500,000 light-years.
Starburst Activity: The collision has led to a massive “starburst” phase. In this phase, clouds of gas and dust are being compressed. This compression forms billions of new stars and super star clusters.
NGC 1999 is a bright reflection nebula in the Orion constellation, located about 1,500 light-years away near the Orion Nebula. Illuminated by the variable star V380 Orionis, it features a distinctive, T-shaped dark void in its center. Once thought to be a dust cloud, this “cosmic keyhole” is actually a hole in the nebula. Energetic stellar winds likely caused this hole. It is also called the “Rubber Stamp” nebula. This name is for those familiar with the use of stamps for marking items.
The nebula is part of the remnants of star formation, surrounded by a network of dusty filaments. It is often observed alongside Herbig-Haro objects, which are small, glowing patches of gas associated with newly formed stars.
The “Keyhole” Void: The most distinctive feature is a dark, T-shaped patch at its center. The region was long thought to be a dense Bok globule. A Bok globule is a cold cloud of dust and gas that blocks light. However, 2010 observations from the Herschel Space Observatory revealed it is actually an empty region of space. It is a literal hole in the nebula.
It is part of the Orion Molecular Cloud Complex and is located just south of the famous Orion Nebula (M42). The region is rich in Herbig-Haro (HH) objects, which are luminous shock waves created by jets from newborn stars. The entire field of view is but a tiny portion of the massive Orion molecular cloud (the Orion A Cloud). A surprise for me is the amount of Oiii in the region. The blue hues highlight its presence.
Session management and automation with APT. I Captured 262 subframes with 180s exposure each. This amounts to about 13 hours of exposure from my driveway. I used an RC8 telescope and an ASI071MC Pro camera cooled to 14f.
I generally like to image open star clusters, globular clusters, and galaxies. However, it is fairly rare for a “starfield” to actually be a galaxy cluster. Hundreds of galaxies within my single field of view at 840mm fl. Challenges the mind.
Abell 1656, also known as the Coma Galaxy Cluster, is a massive and dense collection of galaxies. It contains more than 1,000 identified galaxies. These galaxies are located in the constellation Coma Berenices. It is situated approximately 321 million light-years from Earth. The cluster has a diameter of about 20 million light-years.
The central region is dominated by two supergiant elliptical galaxies: NGC 4874 and NGC 4889. Most central members are ellipticals, while spiral galaxies like NGC 4921 are typically found on the outskirts. Important to look at the astrobin platesolve for this image to see what’s actually in there.
NGC 4449, the Box Galaxy, (also known as Caldwell 21) is an irregular dwarf starburst galaxy. It is located approximately 12 to 13 million light-years from Earth in the constellation Canes Venatici. It is a member of the M94 group of galaxies. Its exceptionally high rate of star formation is notable. This feature earns it the “starburst” designation.
Unlike many galaxies where star formation is central, NGC 4449 exhibits widespread star formation. It reaches all the way to its edges. This is likely triggered by gravitational interactions or past mergers with smaller companion galaxies. The galaxy is rich in blue star clusters, which are young and massive stars. It also contains reddish regions of ionized hydrogen. In these regions, new stars are actively being born.
vdB 30 is a very faint reflection nebula located in the northern constellation Camelopardalis. This nebula is part of the van den Bergh (vdB) catalog of reflection nebulae. Astronomer Sidney van den Bergh originally published the catalog in 1966.
It is primarily a reflection nebula, meaning it consists of interstellar dust that reflects the light of nearby stars. The nebula surrounds the bright star Alpha Camelopardalis. Because this star is quite brilliant (magnitude ~4.3), the faint nebulosity can be difficult to capture and is often overwhelmed by the star’s glare. While categorized as a reflection nebula, it is rich in ionized hydrogen (HII) and some sulfur.
Modern narrowband imaging often reveals a bow shock in the gas. These are visible as curved structures in hydrogen-alpha (Ha) light. This phenomenon is caused by the star moving through the interstellar medium. It is estimated to be approximately 5,000 light-years away from Earth.
vdB 30 is considered a very faint and challenging target for amateur astronomers. It requires long exposure times (often 5 to 10+ hours) to detect the subtle dust and gas structures. Its coordinates place it at a high northern declination (+66 degrees), making it a circumpolar object for many observers in the Northern Hemisphere.
VdB 30 is a reflection nebula in the constellation Camelopardalis. It is a very extensive gas cloud. Observing it is difficult due to the low amount of light reflected and its relatively low temperature. It appears to surround the star α Camelopardalis. This star is located in the centre of the image. It is a blue supergiant from apparent magnitude 4.26 and spectral class O9Ia. The cloud extends for about 29 parsecs. It is composed of cold dust. The dust emits infrared radiation due to the weak heating received from the supergiant. The emissions from the supergiant are especially ultraviolet because of its surface temperature equal to 30,000 Kelvin.
The nebula has a ring shape. It is impressed by the strong stellar wind of the supergiant. This wind is responsible for creating a bubble in the interstellar medium surrounding it. As a result, it disperses the cloud itself.
I photographed this difficult target from my driveway in the foothills of the Blue Ridge Mountains in Burke County, NC. I use APT for image acquisition and session automation to capture 159 5 minute exposures across 4 nights. Subframes calibrated, debayered, aligned, integrated, and processed in PixInsight 1.9.3
