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19-4-2021 Messier 63 or M63, also known as NGC 5055 or the seldom-used Sunflower Galaxy, is a spiral galaxy in the northern constellation of Canes Venatici with approximately 400 billion stars.
Distance to Earth: 27 million light years
Distance: 29.3 Mly (8.99 Mpc)
Apparent size (V): 12′.6 × 7′.2
Group or cluster: M51 Group
Redshift: 484 km/s
Constellation: Canes Venatici
39 light frames 32 dark frames 180sec's iso800.
Nikon D750-Nikon600mm Fl f4 prime & Nikon 2x teleconverter on SWNEQ6-R-Pro mount PHD2 guide- deepsky stacker - Photoshop, bortle 4.
UGC 4277 Distant Galaxy Group, Lynx
UGC4277 is a giant edge-on spiral galaxy, morphological type SC, which is gravitationally bound to, but not tidally interacting with, two smaller galaxies, MCG+09-14-017 and MCG+09-14-012. Since they have similar redshifts and distances, their relative sizes and separation on the image are essentially to scale. From the measurable properties (redshift, apparent magnitude, and angular size), we can derive UGC4277 light travel distance (lookback time) of 250 Mly, redshift recession velocity of 5,407 km/s, and actual diameter of 284,000 ly. This is about 30% larger than the Andromeda Galaxy, and nearly twice the size of the Milky Way. Due to its edge-on orientation, its integrated apparent magnitude and the calculated absolute magnitude are significantly underestimated for two reasons. First, it presents to the observer a much smaller surface area than a face-on galaxy. And second, much of its starlight is absorbed and scattered by thick layers of gas and dust in its galactic plane. Prominent dark dust lanes are easily visible even at the low resolution and small scale of the attached image. UGC4277 has an active galactic nucleus (AGN), which indicates the presence of an accreting central supermassive black hole (SMBH.
Edge-on galaxies are of great interest in the study of galactic evolution because the dynamic distribution of stars, dust, and atomic gas can be analyzed both along the galactic plane and perpendicularly to it. Radio frequency studies of UGC4277 by Allaert et al. (2015) revealed the presence of a primordial atomic hydrogen envelope, three times thicker than the visible disk. As this gas gravitates toward the galactic plane, it condenses into clouds of molecular gas, which eventually collapse to form a "rain" of low metallicity stars. Metals (in astronomy all elements heavier that helium) are produced by stellar nucleosynthesis, and are dispersed into the interstellar medium (ISM) by stellar winds, supernova explosions, and neutron star collisions. Through various processes, a fraction of metals condenses into small dust grains which on average constitute about 0.1% of the galactic baryonic mass. While most of the dust resides in the galactic plane, a part of it can be detected in the form of a "dust-scattered ultraviolet halo" around the galaxy. This "extraplanar" dust appears to be defying gravity, probably suspended by radiation pressure and the plumes of hot gases arising from the galactic disk and bulge. Assuming similar total dust mass fraction, it is expected that starburst galaxies with numerous hot, blue stars and more intense ultraviolet radiation would manifest more prominent extraplanar dust halos. Jong-Ho Shinn (2018), who compared visible band to GALEX ultraviolet images of 23 edge-on galaxies reported, among other findings, a moderate to low extraplanar dust halo around UGC4277, implying a similarly moderate to low star formation rate.
The other two galaxies in the group are MCG+09-14-017 and MCG+09-14-012. The former is oriented face-on, and has a LINER type active galactic nucleus. It is approximately half the diameter and half the brightness of the Milky Way. Both appear to be barred spirals with slightly deformed spiral arms probably due to mild tidal interaction in the remote past. A number of small, background galaxies, listed in the chart on the annotated image, lie at distances between 540 and 1,610 million light years. Four bright quasars are also identified. The most remote of these is SDSS J081428.78+524045.2, located at a light travel distance (lookback time) of 10.4 billion light years. In the present cosmological epoch, its proper (comoving) distance is 17 Bly, and proper recesion velocity 367,941 km/s. Since its recession velocity is presently superluminal, the quasar lies beyond the cosmic event horizon, and the light it is presently emitting can never reach us.
Image details:
-Remote Takahashi TOA 150 x 1105 mm, Paramount GT GEM
-OSC 35 x 300 sec, 2x drizzle, 50% linear crop
-Software: DSS, XnView, Starnet++ v2, StarTools v1.3 and 1.7, Cosmological Calculator v3
It's hard to find a spiral with arms this long. Depending on what you're willing to count as a single arm, one of them seems to wrap around almost two times. Upon realizing this I searched around for some other galaxies with more wraps, but couldn't seem to find any with distinct arms. Malin 1 comes to mind, but it's hard to read.
If anyone has any other galaxies with arms similar to this one, let me know.
A color image comprised of DES DR1 data is available:
legacysurvey.org/viewer?ra=351.9539&dec=-47.3811&...
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 29.01° clockwise from up.
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 9.48° clockwise from up.
Interesting faint arm or tidal stream feature encircling this one like a halo. Looking at DSS data to see the surrounding sky, I don't see any obvious interaction partners. I suppose this is a late stage of some kind of interaction, and all galaxies involved have now merged. I wonder if some kind of small, diffuse galaxy could interact in such a way that it got pulled around nearly into a circle like this. If that were the case, then this would be more of a middle stage than an end stage. Anyway, that's just a lot of speculation.
I was interrupted in the middle of processing this by a rather large earthquake.
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 6.4° counter-clockwise from up.
Model: Taylor Freeze
Photographer: Justin Bonaparte
Very pretty pair of interacting spiral galaxies.
There's a color view available from the ground-based Legacy Survey here: legacysurvey.org/viewer?ra=122.8032&dec=25.2003&z...
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 13.19° clockwise from up.
An apparently disk-shaped, clumpy galaxy with a bit of star formation going on. The hook at one end is interesting.
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 10.80° clockwise from up.
Quite a long galaxy, stretched out due to some kind of recent interaction. Exactly what, I'm not sure. A rather large, diffuse filter ghost (faint, slightly brighter annular feature) is overlapping the right side of the image. There are two bright stars flanking this galaxy to the east or west. Either one could be the culprit, though I think the one to the west was responsible.
Check the widefield view out at the Legacy Survey to get a better view of the situation: legacysurvey.org/viewer?ra=7.1450&dec=-11.5858&la...
Establishing HST's Low Redshift Archive of Interacting Systems
(I might have hit this one too hard with the noise reduction. It looks funny.)
All Channels: ACS/WFC F606W
North is 59.33° counter-clockwise from up.
NGC 4565 (Caldwell 38), Coma Berenices, (Needle Galaxy)
NGC 4565 is an edge-on spiral galaxy in the constellation of Coma Berenices, first documented by William Herschel in 1785. Due to its narrow profile, it is known as the Needle Galaxy. On large scales it is one of the nearest, biggest, and brightest members of the Coma I Galaxy Group. Considerable inconsistencies are found in the literature regarding the apparent and derived properties of this galaxy. According to the NED database, its blue apparent magnitude is 10.42 (8.21 V), and angular size 15.85 arcmin. Its redshift derived distance is 58.5 Mly, and distance based on the median value of 34 redshift-independent distance measurements is 38.47 Mly. Its redshift-based recession velocity is 1,259 km/s, and estimated diameter range between 177,000 and 268,000 light years. Although the galaxy is substantially larger than the Milky Way, its calculated intrinsic brightness is not proportionally higher. Due to its smaller surface area because of edge-on orientation and to thick layers of absorbing dust and gas, its integrated apparent magnitude and calculated absolute magnitudes are significantly lower than expected.
The galaxy's edge-on aspect obscures the nature of the central bulge in the optical band. Infrared studies with the Spitzer Space Telescope suggest the presence of a central bar as well as an inner ring. Meanwhile, the galaxy's orientation allows spectacular view of the dust lanes in the thin galactic disk. Spectroscopic studies of the central region indicate NGC 4565 has an active galactic nucleus of the LINER type powered by accretion around a central supermassive black hole.
NGC 4565 has at least two satellite galaxies. Slightly curved tips of its galactic disk suggest minor gravitational interaction. LEDA 2793674, lying in the foreground, is a small irregular dwarf, less than 10,000 ly in diameter. NGC 4562, in the background, is a minor barred spiral with a gravitationally distorted disk, about one quarter in diameter compared to the Milky Way.
Image details:
Meade 8'' ACF, AP 0.7x compressor (200 x 1400mm)
iEQ30pro mount, Orion 60mm f/4 SSAGpro autoguider
Canon T3i modified camera, Astronomik L3 filter
OSC 25 x 300 sec subexposures, iso 1600, 30 darks, 30 bias, 50% crop
Software: PHD2, DSS, XnView, StarNet++ v2, StarTools v1.3 and 1.7, Cosmological Calculator v3.
Sometimes the detector just isn't quite big enough. Two spirals; one fell off the edge. The telescope seems to have been preferentially pointed towards the more irregularly shaped spiral. Did the southern galaxy pass by the northern one recently and pull on its arms to get it this way, or was there something we can no longer see?
The southern galaxy looks so regular that I would doubt it interacted with anything recently if I saw it by itself.
Maybe there wasn't any interaction. Maybe that's just how they're both shaped.
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 35.34° clockwise from up.
Stephan's Quintet in the constellation Pegasus is a visual grouping of five galaxies of which four form the first compact galaxy group ever discovered. The brightest member of the visual grouping is NGC7320. These galaxies are of interest because of their violent collisions. Four of the five galaxies in Stephan's Quintet form a physical association -,Hickson Compact Group 92.
NGC 7320 (to the lower left of the group) indicates a small redshift (790 km/s) while the other four exhibit large redshifts (near 6600 km/s). Since galactic redshift is proportional to distance, NGC 7320 is only a foreground projection and is ~39 million ly from Earth versus the 210-340 million ly of the other five. (Text source Wikipedia)
Planewave 17” Corrected Dall-Kirkham Astrograph f/4.5, FLI-PL6303E CCD – Remotely imaged T21 Mayhill New Mexico
35 mins Luminance, 5mins R, G & B Image Cropped
A golden egg floats above its pedestal. Here an assumed spiral galaxy has been strangely transformed in a way that makes it difficult to recognize. Its nucleus is now off center—way off center—and its arms are disorganized, forming a kind of irregular ring. The golden egg is an elliptical galaxy which is the major participant in this process.
Turned 90° clockwise I think the composition looks remarkably like a phoenix with its egg.
Some color data is available from the PanSTARRS survey: ps1images.stsci.edu/cgi-bin/ps1cutouts?pos=Apg+141&fi...
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 2.49° counter-clockwise from up.
I'm a bit bothered by the cropping on this one, but otherwise it is a nice pair of interacting galaxies and some tidal tails.
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 128.30° clockwise from up.
Stellar streams looping around a disturbed spiral galaxy with a bit of dust and star formation evident. A widefield view shows barred spiral galaxy NGC 7682 just to the east. NGC 7682 seems relatively undisturbed by comparison, so one wonders if the two have anything to do with one another.
Check the color widefield view from Legacy Survey here: legacysurvey.org/viewer?ra=352.1989&dec=3.5200&la...
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 50.87° counter-clockwise from up.
Fabulous pair of interacting galaxies. Wish I had color data.
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 1.37° counter-clockwise from up.
This view reminds me somewhat of a smaller Coma Cluster, with smooth galaxies of varying shape and size gathered together. Most eye-catching is the large, irregularly shaped galaxy with features shaped by tidal forces and dust lanes crossing it at multiple angles.
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 23.06° clockwise from up.
Arp 297 is a group of four interacting galaxies.
NGC 5754 is the large spiral and NGC 5752 is the smaller galaxy to the upper right. NGC 5754's internal structure has hardly been disturbed by the interaction while NGC5752 exhibits a long tidal tail. NGC5755 is the galaxy located to the left and NGC 5753 is in the 10 oclock position from NGC5755. Arp 297 is located in the constellation Boötes some 200 million light-years away. Detailed information can be found at arijmaki.wordpress.com/2011/11/09/ngc-5754-galaxy-with-hi...
Image Taken: 3 -5 June 14
Imaging scope: AT8RC CCDT67 1200mm
Imaging camera: Trius SX-694
Lights: Lum: 30 x 600 sec bin 1x1
Calibration: Flats, Bias
Guide scope: OAG Lodestar
Other details: Captured with SGP, guided with PHD, stacked in DSS processed in Photoshop
Below the event horizon, nothing, not even light, can escape.
Black hole is a fascinating and mind boggling subject that I know little about. You can find some elementary description in Wiki.
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 21.51° counter-clockwise from up.
M88 is a active spiral galaxy (Seyfert type 2)
M91 (left) is a barred spiral galaxy . Both are located 50-60 Mio light-years.
Many more distant galaxies are visible in this FOV , I checked only one near the bottom left IC3523 , redshift is 0.0739 or a distance of 1.02 Bio lightyears.
The image was recorded in 12 hours in August 2024 at my remote observatory in Hakos-Namibia with a SW Esprit 120ED , ZWO ASI2600MC camera on a 10 Micron 2000HPS mount
Just uploading a grayscale version of this so I can keep all the observations from this proposition organized better. The color version is here: flic.kr/p/2eGbVt7
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 45.34° counter-clockwise from up.
Tidal interaction between two galaxies. There seems to be a mini overlapper in the lower right corner. A nice, widefield color view is available at the Legacy Surveys Viewer: legacysurvey.org/viewer?ra=20.8636&dec=30.7820&zo...
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 21.04° counter-clockwise from up.
A soft and smooth disk of a galaxy with some arms that are both well-defined and impossible to circumscribe as they blend into one another. One thin lane of dust is visible in front of the nucleus about a third of the distance from the center point to the edge, while another thin lane is just discernible close to the brightest part of the nucleus.
There is another galaxy off to the left which is much smaller and can be partially seen at the edge of the composition. The larger galaxy hardly seems perturbed at all by the smaller one, while the smaller one seems to pulled and stretched thin at its periphery.
A color image comprised of SDSS data can be seen here:
legacysurvey.org/viewer?ra=130.6761&dec=14.2769&z...
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 13.51° clockwise from up.
In 2012, astronomers used the Hubble Space Telescope to revisit the Hubble Ultra Deep Field, peering even deeper than before at the near-infrared light of the cosmos. Astronomers use infrared light to study the distant universe because the expansion of space stretches wavelengths of light toward the red end of the electromagnetic spectrum, a phenomenon called "redshift."
The result was the Hubble Ultra Deep Field 2012. The observations uncovered a previously unseen population of seven primitive galaxies that formed more than 13 billion years ago, when the universe was less than 3 percent of its present age, or about 450 million years after the Big Bang.
The Hubble Ultra Deep Field 2012 was followed by the Hubble Ultra Deep Field 2014, which added ultraviolet light observations to obtain a more comprehensive view of this area in the constellation Fornax.
For an image of the Hubble Ultra Deep Field 2014, visit: hubblesite.org/contents/media/images/2014/27/3380-Image.html
Credit: NASA, ESA, R. Ellis (Caltech), and the UDF 2012 Team
For more information about this image, visit: hubblesite.org/contents/news-releases/2012/news-2012-48.h...
A delightful and unusual merger of galaxies, resulting in the comet-like appearance of one galaxy. Only a small amount of dust is visible, but many small dots which I presume are globular clusters are sprinkled within the pair. Edit: Upon looking at the color data, the clusters may be younger clusters, not necessarily globulars. It's bluer than I expected, which would indicate that star formation has been going on.
A color and widefield view is available in SDSS data at the Legacy Survey viewer: legacysurvey.org/viewer?ra=73.3523&dec=-4.7932&zo...
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 12.84° clockwise from up.
NGC 2146 is a disrupted barred spiral galaxy in the constellation of Camelopardalis. It was discovered in 1876 by German astronomer Friedrich Winnecke, who was known for his work on comets, asteroids, and double stars. The galaxy is classified as SB(s)ab pec, indicating a barred spiral galaxy with tightly wound arms, and no ring around the central bulge. The "pec" descriptor refers to the "peculiar" appearance of the spiral arms, one of which is markedly stretched and inclined to the galactic plane by nearly 45*. Very high star formation rate (SFR) and densities within both spiral arms resembling large stellar trails suggest the galaxy recently merged with one or two substantial dwarf satellites, and is presently reforming into a larger object. Some sources suggest that NGC 2146 may have interacted with a nearby small galaxy, NGC 2146a, however that seems unlikely because the small galaxy's spiral structure appears quite well preserved. Aside from its disrupted aspect and starburst activity, NGC 2146 is also distinctive due to its conspicuous dust lanes extending across the background glow of the galactic core. Spectroscopy of the central region reveals widening of spectral lines. This indicates a high velocity dispersion of the stars in the nucleus due to the presence of a central supermassive black hole (SMBH). Absence of an active galactic nucleus means thet the central SMBH is not presently accreting matter.
Assuming its measured redshift of 0.00298 is caused exclusively by the expansion of space (Hubble Flow), NGC 2146 would lie at a distance of 41.3 Mly. However, the median value of 16 redshift-independent distance measurements is 17.40 Mpc, or 56.72 Mly. The two distance estimates differ because the measured redshift actually results from the combined motion due to Hubble Flow and the object's "peculiar velocity" through space. When available in a statistically valid number of measurements, redshift-independent estimates are generally regarded as more accurate for nearby galaxies, closer than approximately 140 Mly. From the apparent magnitude and angular size, accepting the distance of 56.72 Mly, we can derive the galaxy's actual diameter of 97,000 ly and absolute magnitude of -20.64. NGC 2146 is some 20-30% smaller, and about 15% less bright than the Milky Way.
Chandra CXC HIPS X-ray sky survey (SIMBAD) shows numerous X-ray sources within the NGC 2146 core, in the spiral arms, and in its halo. While it is possible that some of the sources may be local to the Milky Way, clustering of the sources around NGC 2146 suggests that most are of extragalactic origin.
The most common mechanism for X-ray emission in astronomical objects involves very hot ionized gases at temperatures of millions to hundreds of millions Kelvin (K). Stellar coronas, especially in young blue giants, emit X-rays, though they are regarded as relatively weak sources. Stronger emissions come from "X-ray binaries", "cataclysmic variable stars", supernova remnants, and hot gas clouds around stellar nurseries. Still stronger localized X-ray emissions are "ultra-luminous X-ray sources" or ULX. These are produced by actively accreting intermediate mass black holes (IMBH), usually identified in galactic disks, and by central supermassive black holes (SMBH) which define "active galactic nuclei" (AGN). By far the most powerful, but very diffuse, sources of X-rays are galaxy clusters.
While it is logical to expect numerous X-ray emissions in an actively merging starburst galaxy with accelerated stellar evolution, NGC 2146 has no identified ultra-luminous X-ray sources and no active galactic nucleus. This does not imply the galaxy contains no intermediate or supermassive black holes, but merely that they are not actively accreting.
On closer inspection, the attached image records a number of small, faint background galaxies, but only two of these have identifiers associated with measurable data. Based on a subjective estimate of their angular size and apparent brightness, the rest probably lie at approximate distances between 1 and 2 Bly. The image also records a single quasar (QSO) at a light travel distance (lookback time) of 9.2 Bly.
The distinctly blue galaxy Gaia DR3 1140883127890416128 may belong to a class of special objects: "Blue Compact Dwarf" galaxies (BCDs), which are field dwarf galaxies with inexplicably high star formation rates. BCDs are rare local versions of the "Faint Blue Galaxies" (FBGs), the most common galaxy type at redshifts between 0.1 and 2, but which are undetectable with small instruments. I estimate the apparent magnitude of this object around 20.5 and angular size at 0.15 arcmin. Unfortunately, no redshift information or color photometry is available in extragalactic databases, and the suspected nature of this galaxy can not be confirmed. For additional details on BCDs and FBGs please see section 32, Dwarf Galaxies, subsections 6 and 7 here:
www.cloudynights.com/articles/cat/articles/basic-extragal...
Image Details:
Remote Takahashi TOA 150x1105 mm
OSC 31x300 sec, 2x drizzle, 40% linear crop, 26x17'
Software:
DSS, XnView, StarNet++ v2, StarTools v1.8
Extragalactic Cosmological Calculator v2
www.cloudynights.com/gallery/image/123530-extragalactic-c...
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 33.11° counter-clockwise from up.
A color view from the Legacy Survey viewer is here: legacysurvey.org/viewer?ra=172.7533&dec=20.4686&z...
There's PANSTARRS data, too ps1images.stsci.edu/cgi-bin/ps1cutouts?pos=Apg+197&fi...
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 9.18° counter-clockwise from up.
This is some wonderful narrowband imagery of NGC 4449 captured by Hubble back in 2005. When I first found this, I thought for sure it had already been processed somewhere along the line but all I could find was a wideband mosaic, which is here if you want to check it out. Rob Gendler did his own take as well, more strongly emphasizing the narrowband but still utilizing the wideband. The wideband imagery is nice but wow, is there a lot of amazing emission structure revealed with the narrowband data isolated. There are simple, smallish spheres, larger complex clouds, and down the center, streaming outwards like a ruptured fissure, is some massive work being done by the prodigious number of young stars radiating fiercely along the seam.
Red here represents areas of H-alpha and [N II] while slightly bluer areas show where [O III] emissions are also present. Mediumband green data (F550M) was also available and I used this to bring the stars to slightly more natural, whiter colors. Rather than maximizing differentiation between emissions, this time I applied more "realistic" colors. There's so much overlapping that it hardly matters, anyhow.
Two HST Proposals are associated with these data:
NGC 4449: a Testbed for Starbursts in the Low- and High-Redshift Universe
Calibrating Star Formation: The Link between Feedback and Galaxy Evolution
Red: HST_10522_01_ACS_WFC_F660N_sci + HST_10585_03_ACS_WFC_F658N_sci
Green: HST_10585_03_ACS_WFC_F658N_sci + HST_10522_01_ACS_WFC_F550M_sci
Blue: HST_10522_01_ACS_WFC_F502N_sci1
North is NOT up. It is 47.5° counter-clockwise from up.
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 13.12° clockwise from up.
A spiral galaxy formed into a ring alongside its interacting elliptical partner. The ring may go on to become something like the Cartwheel Galaxy or Hoag's Object, or perhaps the structure is more transient than that. The Universe uses its boundless tracts of spacetime to keep its secrets from us.
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 4.01° clockwise from up.
the Multimedia Artist Danny "MushroomBrain" Hennesy
these are some of my eyes, I often use them when I make visional artistery but not always and not all at the same time!
Peace and Noise!
/ MushroomBrain the seer :::)
A neat, compact group of galaxies. The big one at the center steals the show with its large amount of dust and star formation. Somewhat unfortunately, the little one on the right didn't quite fit onto the detector. Not much can be done about it without more Hubble time.
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 51.96° clockwise from up.
–––
Crosspost by Koinup - original here
location: Redshift
"My warning meant nothing.
You're dancing in quicksand.
Why don't you watch where you're wandering?
Why don't you watch where you're stumbling?
You're wading knee deep and going in.
And you may never come back again.
This bog is thick and easy to get lost in.
cause you're a stupid, belligerent f***er.
This bog is thick and easy to get lost in.
cause you're a dumb and belligerent f***er.
I hope it sucks you down. down...down...down...
[...]" - "Swamp song", Tool