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The 2011 Mobius Wearable Art Runway Show
Friday, May 6 · 7:00pm - 9:00pm - Boston
Created By - Mobius, Inc., Alison Safford, James Ellis Coleman
Program Order and Erratae Mobius Wearable Art 1) Inflatable Metamophosis artist: Charlie Roberts model: Liz Roncka MC talk-introduce the show 2) Liv Chaffee Students -The John Marshall School in Dorchester, MA Deandre Dewhollis, Kyshuari Santana-Everet Jose Pene Rayuana Martin-Milton Xavier Barrietos 3) Marie Ghitman – Two Group Skirts Models: Luke Burrows, Neige Christensen, Sage Dowser, Lisa Hiserodt, Sam Lanier, Jean Martin, Madelyn Medeiros, Jane Messere, Jason Picard, Q, Madelaine Ripley, and Artist 4) Jennifer Hicks - steam punk 5) Amy Keefer (SF) you all know me 6) Katie Pray-zip tease CSW 7) Becky Savitt 8) Ellla Williams- broken Record 9) Ella williams-garbage bag dress 10) Emily D’Angelo – 100% Recyclable 11) Grace Lynn Wilson – Fairy 12) Kaela Cote-Stemmermann - Pagan Sunset 13) Kaela Cote-Stemmermann - Stamp coat, model: Caroline Hickey 14) Mikaela Dalton – Mikaela Dalton – The Devil’s Tune 15) Mikaela Dalton – Untitled (cassette top), Model: Sarah Smith 16) Mikaela Joyce – Bell Jar Dress, Model: Sarah Hertel-Fernandez 17) Mikaela Joyce – Safety Pin Top 18) SeungHye Kim –The Pad Dress 19) Sonya Thorne – Apocalyptic Pieces 1-3, Model: self, Lilia Gaufberg, Zoe Cohen 20) Tess McCabe – Redshift, Model: Molly Harrison 21) William Everston (Representing Seeking Kali) -Sari Scroll for Two, Model: Artist, Karen Everston 22a) Ashley Conchieri – hand Woven and Hand Sewn, Model: Rebecca Chabot 22b) Ashley Conchieri – hand Woven and Hand Sewn, Model: 22c) Ashley Conchieri – hand Woven and Hand Sewn, Model: Monika Plioplyte 23) Julia Dusman – “Tarantula” Necklace 24) Ellen Shea - Little Red Re-Design, Model: Rebecca Woodbury 25) LeeLoo – Fallen post-apocalyptic cyber angel 26) L. Mylott Manning – Insides Out 28) Alyssa Fishenden - Plastic bag and stretch nylon halter dress 29) Robyn Giragosian and Caleb Cole – Pom Prom 30) Rachel Jayson – Dress of sheet music 31) Bethany Haeseler – Fruitloops 32) June Monteiro – “SMARTIE Dress”, Model: Chantal Lima Marquis 33) Jennifer Sherr Designs – Collage and hand painted leather vest, Model: Jess Barnett 34) Stacy A. Scibelli –Sabotage, Models: Meg Kuker, Toni Scibelli 35a) Selina Narov – Silk painted art couture clothing - Model: A. Dorian Rose 35b) Selina Narov – Silk painted art couture clothing - Model: Liz Roncka 35c) Selina Narov – Silk painted art couture clothing - Model: Jennifer Hicks 37) Albert Negredo – RECORDS (word game text) Red dress/Silver bag fabricated by Jane Wang - Model: sara june 38) Stacy A. Scibelli – plated skirt with leather head-piece (Models: tbd) 39) Stephanie Skier – Ephemeral dynamic fiberoptic fiber arts 40) the Bureau of cyberSurreal investigation international webCam Bra for Living I/O Model: Carol Susi 41) Elly Jessop – Glow Dress 42) Raphaela Riepl –Tentacles Flying Teeth, Models: Kira Lorenza Althaler as William Haugh, Florian Maria Sumerauer as Aaron Diskin Finale- 43) Word Game Design Competition Winner: June Monteiro - Model: northern sire
ONLINE BLOG for 2011 Mobius Wearable Art Runway Show: mobius-wearableart2011.blogspot.com/
@ Mobius
725 Harrison Avenue, Suite One
Boston MA 02118
Related Exhibition: A Tool Is A Mirror
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...
NGC 7331, Deer Lick Galaxy Group, Pegasus
NGC 7331, also identified as UGC 12113, PGC 69327, and Caldwell 30, is an unbarred spiral galaxy in the constellation of Pegasus. It is the brightest and largest member of a visual field of galaxies called the Deer Lick Galaxy Group that includes NGC 7325, 7326, 7335, 7336, 7337, 7340, and LEDA 2051985, all of which lie in the background at distances between 290 and 400 million light years. The group was first documented in 1784 by William Herschel.
Based on its measurable features (redshift of 0.002732, apparent magnitude 9.48, and angular size 10.47) we can estimate the following NGC 7331 physical properties: actual diameter 115,000 ly, absolute magnitude -20.86, distance 38 million ly, and recession velocity due to the expansion of the Universe (Hubble flow) 818 km/s. The galaxy is remarkably similar to the Milky Way in size and luminosity, but not strictly speaking in morphology. Although both are spiral galaxies, NGC 7331 is unbarred, while the Milky Way is presently thought to be a barred spiral. Further, NGC 7331 has peculiar features which are most likely due to a merger of large component galaxies in the remote past. Unlike the majority of spiral galaxies, its central bulge and the spiral arm disk rotate in opposite directions, and the central bulge is eccentric toward the N relative to the disk and the stellar halo.
Dwarf galaxy LGG 459 lies in-line with the S edge of the NGC 7331 disk, may be merging with it, and may have gravitationally disrupted the S spiral arm into 4 or 5 branches. Although redshift based distance between the two galaxies is around 4 Mly (assuming redshift is due exclusively to Hubble flow), the actual distance between them could be much smaller if LGG 459 redshift were in part due to "peculiar velocity" through space toward the background, away from the observer.
Spectroscopic analysis of NGC 7331 central region revealed an Hii/LINER active galactic nucleus. Filho et al. (2004) reported core radio luminosity 10 times higher and X-ray emission 10,000 times higher than the Sagittarius A* source in the center of our Galaxy. These studies suggest the presence of an obscured central supermassive black hole of approximately 175 million Solar masses, about 44 times larger than the Milky Way's
arxiv.org/abs/astro-ph/0401593
The distant members of the Deer Lick Group are gravitationally bound to each other and also to the nearby Stephan's Quintet (NGC 7320) Group. Even at the scale of this image, NGC 7337 and 7336 show evidence of tidal interactions. The S side of the field contains a very remote galaxy cluster whose members are annotated with letter G. Unfortunately, none of these galaxies carry identifiers in Simbad or NED extragalactic databases. Comparing their average angular size to that of the Deer Lick Group, I very roughly estimate their distance at 2 billion light years.
Image Details:
-Remote Takahashi TOA 150 x 1105mm
-Paramount GT GEM
-25 x 300 sec subs, OSC, 2x drizzle, 50% linar crop
-Software: DSS, XnView, StarNet++, StarTools v1.3 and 1.7, Cosmological Calculator v2
IC 284 (UGC 2581, PGC 11643 and others) is appears to be a low surface brightness spiral located approximately 123 million light-years away (by redshift) in Perseus.
PGC 11646 (2MASX J03060656+4221569, ZW V 319 and others) is the companion on the right (west). Some sources say this one is behind IC 284.
Luminance – 24x600s – 240 minutes – binned 1x1
RGB – 8x300s – 40 minutes each – binned 2x2
360 minutes total exposure – 6 hours
Imaged December 21st and 22nd, 2022 from Dark Sky New Mexico at Rancho Hidalgo (Animas, New Mexico) with a SBIG STF-8300M on an Astro-Tech AT12RCT at f/8 2432mm.
Edited Hubble Space Telescope image of the galaxy LRG-3-817 distorting light into arcs.
Original caption: This NASA/ESA Hubble Space Telescope image features the galaxy LRG-3-817, also known as SDSS J090122.37+181432.3. The galaxy, its image distorted by the effects of gravitational lensing, appears as a long arc to the left of the central galaxy cluster. Gravitational lensing occurs when a large distribution of matter, such as a galaxy cluster, sits between Earth and a distant light source. As space is warped by massive objects, the light from the distant object bends as it travels to us and we see a distorted image of it. This effect was first predicted by Einsteinâs general theory of relativity. Strong gravitational lenses provide an opportunity for studying properties of distant galaxies, since Hubble can resolve details within the multiple arcs that are one of the main results of gravitational lensing. An important consequence of lensing distortion is magnification, allowing us to observe objects that would otherwise be too far away and too faint to be seen. Hubble makes use of this magnification effect to study objects beyond the sensitivity of its 2.4-metre-diameter primary mirror, showing us the most distant galaxies humanity has ever encountered. This lensed galaxy was found as part of the Sloan Bright Arcs Survey, which discovered some of the brightest gravitationally lensed high-redshift galaxies in the night sky.Â
With all this driving snow outside today I had time to do a bit of advent handicraft. ;-) Mounted the ShockStop Suspension Stem from redshift sports on my Orient.
Very keen to try it out on the road now.
--
Mit dem Schneetreiben heute den ganzen Tag hatte ich mal Zeit für etwas Adventsbastelei. ;-) Habe den ShockStop Suspension Vorbau von Redshift Sports an mein Orient montiert.
Bin nun sehr gespannt, ihn draußen auf der Straße auszuprobieren.
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/2eNGDRE
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 24.50° clockwise from up.
NGC5907 (NGC5906, UGC09801), Draco, Knife Edge Galaxy, and Five Quasars
NGC 5907 is a large nearly edge-on spiral galaxy, first documented by W. Herschel in 1788. On a large scale it is one of the brightest members of the small NGC5866 Galaxy Group in the constellation of Draco. Although the designation generally refers to the entire galaxy, it was not until 1850 that George Stoney identified the faint W part of the galaxy obscured by prominent equatorial dust lanes as NGC 5906. According to NED (NASA Extragalactic Database), the galaxy is 12.8 arcmin in angular size and 9.18 (V) in integrated apparent magnitude Other values found in the literature for the visible band magnitude include 11.12, 11.8, and 12.46, which simply appear too low when compared to the object's photographic brightness. 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 the galactic plane. Its redshift of 0.002225 indicates light travel distance of 30.88 Mly, assuming redshift is due exclusively to the expansion of space (Hubble Flow). For redshifts < 0.01, redshift-independent distance measurements, such as the Cepheid method, are generally more accurate because a fraction of the redshift value is due to an object's motion through space. For NGC5907 the median redshift-independent distance value is 14.275 Mpc, or 46.54 Mly.
Based on the measurable properties, we can estimate NGC5907 to be 172,000 ly in diameter, approximately 40% larger and two times brighter than the Milky Way. Its redshift indicates a recession velocity of 666 km/s. Its morphological classification is SAc (or Sc), indicating a spiral galaxy with loosely wound arms and no evidence of a nuclear bar. Considering the galaxy's nearly edge-on presentation with 87.2* inclination to our line of sight, the presence of a bar can not be confidently ruled out because a view of the nucleus is obscured by dust, gas, and luminous matter in the galactic disk. Garcia-Burillo et al. (1997) suggest that anomalies in molecular gas kinematics can be explained by the presence of a stellar bar. The galaxy has a thin disk with a nearly absent central bulge, resulting in a bulge-to-disk luminosity ratio of only 0.05. Prominent equatorial dust lanes extend nearly to the edges of the galactic disk. While there is some controversy about the presence of extraplanar dust, Xilouris et al. (1999) report that the thickness of extraplanar dust is about 10% larger than the thickness of the stellar disk. As indicated by the light blue floccules of hot newborn stars and by the presence of numerous ionized hydrogen (Hii) regions in the galactic disk, the galaxy displays an above average star formation rate (SFR). This was initially perplexing since the galaxy was thought to be an isolated field spiral with no evidence of tidal disruption. However, deep-sky images by R Jay GaBany (2006) revealed a complex interweaved structure of stellar debris surrounding the galaxy, resulting from an accretion event over four billion years ago. Gravitational perturbations caused by this stream explain elevated SFR and the slight warp in its galactic disk.
www.cosmotography.com/images/small_ring_ngc5907.html
Although it is statistically very likely that NGC5907 contains a central supermassive black hole (SMBH), literature search reveals no information regarding detection of radio wave or high energy emissions from the galactic nucleus. If a central SMBH is present, it shows no evidence of active accretion at this time. Nor can a central SMBH be confirmed by spectroscopy and stellar kinematics. Due to the edge-on orientation, the nucleus is obscured in the optical band by equatorial gas, dust, and luminous matter.
The annotated image indicates the position of an ultra-luminous X-ray source (ULX) within the galaxy's disk. The precise nature of these objects is not confidently known. In order of probability, their energy source is explained as accretion around an intermediate mass black hole (IMBH), super-Eddington accretion around a neutron star or large stellar-mass black holes (BH), or beamed emissions from high mass X-ray binary stars. Pintore et al. (2018) reported an X-ray transient event in this ULX implying a flux increase by a factor of >35. They find the event is consistent with a ~30 solar mass black hole accreting at the Eddington limit, or with beamed emissions from an accreting neutron star.
Other objects of interest on the annotated image include an irregular dwarf galaxy LEDA 54419. Its redshift is very similar to that of NGC5907 suggesting the two might be bound. Distinct blue color indicating high SFR further increases the possibility of tidal interaction. Unfortunately, no redshift-independent distance measurements have been made for this galaxy, and their interaction can not be confirmed. A number of remote galaxies lie in the background. Four of these which carry identifiers are located at distances between 1.6 and 1.73 Bly. Another six even more remote galaxy candidates are marked with letter G. The image also includes five identified quasars. Three of these appear brigher than their listed apparent magnitudes. They are marked with the "+" sign on the chart below. Since quasar luminosity depends on its SMBH accretion rate, quasars often manifest variability up to several magnitudes over a period of days to years. The last two quasars on the list have super-luminal recession velocities in the present cosmological epoch. They have crossed the cosmic event horizon, and the light they are presently emitting can never reach us. The most remote of the quasars is SDSS J151538.77+560520.4 at a light travel distance (lookback time) of 10.86 billion light years.
Image details:
-Remote Takahashi TOA 150 x 1105mm, SBIG STF-8300C, Paramount GT GEM
-OSC 32 x 300 sec, 2x drizzle, 50% linear crop
-Software: DSS, XnView, StarNet++ v2, StarTools v1.3 and 1.8, Cosmological Calculator v3
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
Taken with my Pentax 67 with 200mm lens and Ilford HP5 Plus film. Scanned with my Plustek OpticFilm 120
The Einstein Tower, designed by Erich Mendelsohn, was built in 1919-1921 for the Astrophysical Observatory Potsdam (AOP) to prove the relativistic redshift of light in the gravitational field of the sun. Though the (unexpected) turbulent surface of the sun prevented astronomers from confirming this effect until the 1950ies, the Einstein Tower has been a successful solar observatory for nearly 100 years now. It is still used today, especially for obervations of magnetic fields on the surface of the sun.
The dome houses a Coelostat, a combination of two mirrors that track the sun and reflect it's light down inside the tower. The tower is built around a fixed, vertical solar telescope with a lens of 60cm aperture and a focal length of 14 meters. The light is analyzed by spectrographs installed in the basement of the building.
Besides astronomy, the Einstein Tower is known as a noteable example of expressionistic architecture.
NGC 4535, Virgo, The Lost Galaxy of Copeland, and Five Quasars
NGC 4535 is a low surface brightness (LSB) barred spiral galaxy in the constellation Virgo, first documented by William Herschel in 1785. Due to its hazy and "ghostly" visual presentation prominent amateur astronomer Leland Copeland named it "The Lost Galaxy" in the 1950s. Based on its median redshift-independent distance measurement of 51.53 Mly, apparent magnitude of 10.32 (g), and angular size of 7.80 arcmin, the galaxy is approximately 116,000 ly in diameter and 90% as bright as the Milky Way. Its redshift of 0.00657 corresponds to a recession velocity of 1,963 km/s, which is in part due to the expansion of space, and in part to its "peculiar velocity" through space relative to us. Its morphological classification is SAB(s)c, indicating an intermediate-barred spiral galaxy without a central ring, and with moderately wound spiral arms. The galaxy is one of the larger members of the Virgo Galaxy Cluster that includes up to 2,000 members. Like most "cluster spirals" it shows evidence of tidal interaction with other members in the form of spiral arm deformation and splitting, gas depletion, and low average star formation rate (SFR) in the current cosmological epoch. The blue floccules in the spiral structure represent "OB Associations", immense clusters of large and very hot young stars. However, unlike in similar galaxies, these are present in relatively low numbers due to gas depletion in the galactic disk. For this reason, NGC 4535 is regarded as a low surface brightness (LSB) galaxy. A number of curved, elongated structures in the disk strongly resemble "stellar streams", or gravitationally stretched remnants of merged dwarf galaxies. Many major galaxies in the Virgo Cluster show evidence of rapid mass assembly through the process of dwarf galaxy accretion.
NGC 4535 has been extensively investigated regarding the presence of a central supermassive black hole (SMBH). Central black holes have been detected in virtually all substantial galaxies studied. Spectroscopic analysis of the central region in the optical band shows evidence of numerous ionized hydrogen (Hii) clouds. These originate from molecular gas clouds ionized by the powerful ultraviolet radiation emanating either from an SMBH accretion disk and/or circumnuclear regions of new star formation. The width of the spectral lines indicates the "velocity dispersion" of luminous matter near the nucleus, which in turn depends on the intensity of the gravitational field generated by the mass in the galactic center. Studies of NGC 4535 refined the understanding of the relationship between the mass and activity of the central SMBH and the evolution of the galaxy within which it resides. For example, this galaxy's gas depletion and current low average star formation rate are in part due to the return of mass momentum and energy from the black hole to the galaxy by the mechanisms of "SMBH outflows" and "radiation pressure" respectively. These processes expel gas and dust from the galaxy, and are explained in more detail in section 40 here:
www.cloudynights.com/articles/cat/articles/basic-extragal...
While NGC 4535 does not have a central starburst ring structure visible in the optical band, it has been one of the major subjects in recent studies on galactic ring formation (Jiayi Sun et al. 2018). Observational evidence reveals a close association between galactic star formation rate (SFR), molecular gas clouds which are the gas reservoir for star formation, and ionized hydrogen (Hii) regions formed when molecular gas is exposed to ionizing ultraviolet radiation from newborn stars. The hydrogen molecule, H2, originating from the big bang, is by far the main component of molecular gas. The second most abundant component is the carbon monoxide molecule, CO, whose constituent atoms were formed during the preceding generations of "stellar nucleosynthesis". Its emission line at the wavelength of 2.6 mm is used in radio-astronomy to map the distribution of galactic molecular gas clouds. While low mass galaxies show faint and scattered CO emissions, massive spiral galaxies exhibit bright, contiguous ring-like emissions within the galactic bulge (Hughes et al. 2013a). These structures, named "Resonance Rings", are thought to accumulate in regions where the outward acting-forces on the molecules balance the centrally-acting gravitational forces. More precisely, resonance rings form where the kinetic energy of gas molecules, defined by the average "velocity dispersion", balances the gravitational potential energy. The evolution of molecular resonance rings also depends on other mechanisms, such as magnetic fields, central SMBH outflows and radiation pressure, and external gravitational effects and matter exchange related to merging or interacting galaxies. In NGC 4535, a resonance ring was detected approximately 1,500 ly from the center. Under favorable circumstances molecular resonance rings evolve into star-forming regions, and eventually become brightly luminous in the visible band.
Derived properties of identified faint objects are listed in the chart on the annotated image. The most remote are five quasars, four of which lie beyond the "cosmic event horizon", as their recession velocities in the present cosmological epoch are superluminal. Two of them, marked with (+) appear significantly brighter than their listed apparent magnitudes. Many quasars are variable up to several magnitudes with periods ranging from days to years, depending on the inflow of matter available for accretion. The most intrinsically luminous object is LBQS 1232+0815, which is nearly 5,000 times brighter than the Milky Way. The most distant quasar is SDSS J123352.16+080527.4 (z = 2.76700), lying at a light travel distance (lookback time) of 11.33 Bly.
Image details:
-Remote Takahashi TOA 150 x 1105 mm
-OSC 36 x 300 sec, (2021 + 2022), 2x drizzle, 40% linear crop, FOV 31x21 arcmin
-Software: DSS, XnView, Starnet++ v2, StarTools 1.3 and 1.8, Cosmological Calculator 3
The universe is expanding, and that expansion stretches light traveling through space in a phenomenon known as cosmological redshift. The greater the redshift, the greater the distance the light has traveled. As a result, telescopes with infrared detectors are needed to see light from the first, most distant galaxies.
Read more: www.nasa.gov/feature/goddard/2019/nasa-s-webb-to-explore-...
Credits: NASA, ESA, and L. Hustak (STScI)
A brand new pinhole camera from Reality So Subtle (35r). It has 2 pinholes, one on the front and one on the back, The back one is used dfor shooting "redscale". © www.johnfar.com
#87 astrodeep200407aab10a.png 16.38 MB 2483X2482 HUDF center NASA original
See also:
#91 astrodeep200407aab10aa.png 4.12 MB 1244X1243 HUDF top center NASA original
This image is 15.86% of the area of the Hubble Ultra Deep Field,
which is 186 arc-seconds wide and high = 3.1 arc-minutes
= 1/10 width of the Full Moon or Sun, about 0.5 degrees,
so the HUDF is about 1% of the area of the square that holds the Full Moon or Sun,
short introduction re viewing lovely subtle earliest structures in HUDF: AstroDeep, Rich Murray 2009.02.23
I've found since 2005 myriad ubiquitous bright blue sources, always on a darker fractal 3D web, along with a variety of sizes of irregular early galaxies, in the Hubble Ultra Deep Field, simply by increasing the gamma from 1.00 to 2.00 and saturating the colors, while minimizing the green band to simplify the complex overlays of complex fractal structures.
Dozens of these images, covering the entire HUDF in eight ~20 MB segments, are available for viewing at many scales [ To change the size of images on Windows PCs, use Control - and + ] on www.Flickr.com at the "rmforall" photostream. Try #86 for the central 16% of the HUDF.
ubiquitous bright blue 1-12 pixel sources on darker 3D fractal web in five 2007.09.06 IR and visible light HUDF images, Nor Pirzkal, Sangeeta Malhotra, James E Rhoads, Chun Xu, -- might be clusters of earliest hypernovae in recent cosmological simulations: Rich Murray 2008.08.17 2009.01.20
rmforall.blogspot.com/2008_08_01_archive.htm
Sunday, August 17, 2008
groups.yahoo.com/group/AstroDeep/25
groups.yahoo.com/group/rmforall/85
www.flickr.com/photos/rmforall/1349101458/in/photostream/
The 5 closeups are about 2.2x2.2 arc-seconds wide and high, about 70x70 pixels.
The HUDF is 315x315 arc-seconds, with N at top and E at left.
Each side has 10,500x10,500 pixels at 0.03 arc-second per pixel.
Click on All Sizes and select Original to view the highest resolution image of 3022x2496 pixels, which can be also be conveniently seen directly at their Zoomable image:
www.spacetelescope.org/images/html/zoomable/heic0714a.html
Notable in the deep background of the five closeups are ubiquitous bright blue sources, presumably extremely hot ultraviolet before redshifting, 1 to a dozen or so pixels, as single or short lines of spots, and a few irregular tiny blobs, probably, as predicted in many recent simulations, the earliest massive, short-lived hypernovae, GRBs with jets at various angles to our line of sight, expanding bubbles, earliest molecular and dust clouds with light echoes and bursts of star formation, and first small dwarf galaxies, always associated with a subtle darker 3D random fractal mesh of filaments of H and He atomic gases.
As a scientific layman, I am grateful for specific cogent, civil feedback, based on the details readily visible in images in the public domain.
www.spacetelescope.org/images/html/heic0714a.html
Hubble and Spitzer Uncover Smallest Galaxy Building Blocks
Rich Murray, MA Room For All rmforall@comcast.net 505-501-2298
1943 Otowi Road, Santa Fe, New Mexico 87505
groups.yahoo.com/group/rmforall/messages
groups.yahoo.com/group/AstroDeep/messages
www.sfcomplex.org Santa Fe Complex
You are welcome to visit me and share your comments as I share these images at home on a 4X8 foot screen -- no fee.
Anyone may view and download for free 91 images, presenting the HUDF in eight 20 MB pieces at rmforall at www.FlickR.com -- #86 is about 20% of the HUDF in their red and blue colors, as leaving out the green greatly simplifies interpreting the overlapping layers of transparent fractal webs of gas with a wide range of sizes of rather distant sources, beyond z = 5.
_____________________________________________________________
astrodeep200407aab10ada.png 3.10 MB flickr.com rmforall #90 astrodeep200407aab10ada.png 3.68 MB 1244X1243 px HUDF center top left: Lillian J Kelly: Rich Murray 2008.12.30
The attachment is my image from my hard drive:
astrodeep200407aab10ada.png
www.flickr.com/photos/rmforall/3103426063/
#90 astrodeep200407aab10ada.png 3.68 MB 1244X1243 px HUDF center top left
Click on All Sizes to see and download the Original
or find it directly at
farm4.static.flickr.com/3161/3103426063_df229d2202_o.png
In Windows Vista, use CTRL +/= over and over to magnify images,
and CRTL _/- to reduce.
You can also go to Control Panel to Ease of Access
to Ease of Access Center
to Optimize visual display
to turn on Magnifier,
which creates a box of any size and location that magnifies
from 1 to 16 times in width and height,
whatever area the cursor is pointed at on any image on the screen.
You can even make "stereo" pairs side by side,
by setting Magnifier to 1X,
and putting its box to the left or right half of the screen,
and using the cursor to adjust
until the two images are matching and side by side.
Then if you can, gaze with crossed eyes at the two images
to get a third image in between,
which may well look 3D and have much more detail.
This image is 3.965% of the area of the Hubble Ultra Deep Field,
which is 186 arc-seconds wide and high = 3.1 arc-minutes
= 1/10 width of the Full Moon or Sun, about 0.5 degrees,
so the HUDF is about 1% of the area of the square that holds the Full Moon or Sun,
while the image is .9765 times 1/1,000 of the area of the HUDF,
so the image is about 1/100,000 area of the square that holds the Full Moon or Sun.
The image is 23.25 are-seconds wide and high,
while the pixels are 0.03 arc-seconds wide in the original HUDF.
The background of many small blue spots are about 1-10 pixels in area.
I have used a simple, low-cost program, MGI PhotoSuite 4.0 to process these images:
double the Gamma to 2.00,
raise the color saturation,
shift colors a bit to accentuate the reds,
remove most of the Green band,
so the image is mostly made of Blue (coding for visible blue),
with Red codes for the invisible infrared just longer in wavelength than visible red.
Mixed Blue and Red make green, yellow, orange, red, and white.
However these colors are downshifted in frequency (lengthened in wavelength)
more and more the more they are distant in space (light travel time from us):
The "Little Feller", like the figure "8" in the top center
to the right of the red galaxy with a red swirl on the right,
has been measured to be at redshift distance z = 4.88,
so its light is changed by a factor of 4.88 --
its apparent reds, oranges, and yellows represent radiation in the hot ultraviolet,
and its age from us is about 13 billion years,
about a billion years after the Big Bang,
13.7 billion = 13,700 million years ago.
The Sun and solar system are 4.6 billion = 4,600 million years ago.
The myriad tiny background blue spots,
along with some green ones,
always on a dark 3D fractal mesh,
are probably the first stars,
made of pure hydrogen and helium,
about 100-100 solar masses in size,
extremely hot and short-lived,
exploding as hypernovae after 1-2 million years,
often with intense bipolar jets,
often leaving relic neutron stars and black holes,
flinging new elements like carbon, nitrogen, and oxygen into space to become the substance of later generations of stars,
which are closer to us in space (nearer in time), smaller, more numerous, cooler, longer-lived,
collecting together by gravity to make clouds, clusters, dwarf galaxies, clump cluster galaxies, irregular galaxies, and mature galaxies,
flat slowly rotating spirals and rounded ellipticals,
which often collide, especially at first
before the constant expansion of space-time separated them more and more --
the expansion of space-time itself that originated from a minute region in a source reality
that had at least 10 dimensions of space and one of time -- the Big Bang.
So, we see far-away early gatherings of hot blue and green objects,
and closer (nearer to us in time) more numerous gatherings of cooler red objects,
which all seem exist as a 3D fractal network of twisted tubes,
rather transparent, as there was little dust in early time to darken light.
It is well known that for every mass of ordinary matter, gas, dust, stars,
there is about 6 times more mass of completely invisible dark matter,
which pulls itself together by gravity into a 3D fractal network, making
the scaffold that ordinary matter collects within.
Dark matter surrounds glalaxies and superclusters of galaxies,
bending light gently by gravity,
so that the dark matter appears as subtle transparent bubbles
against the complex background of deeper structures.
Additionally the cosmic zoo may include galaxy-wide strings of
condensed space-time geometry, formed during the Big Bang,
that are massive enough to bend light
and make double twin images of objects far behind them from us.
ubiquitous bright blue 1-12 pixel sources on darker 3D fractal web in five 2007.09.06 IR and visible light HUDF images, Nor Pirzkal, Sangeeta Malhotra, James E Rhoads, Chun Xu, -- might be clusters of earliest hypernovae in recent cosmological simulations: Rich Murray 2008.08.17
rmforall.blogspot.com/2008_08_01_archive.htm
Sunday, August 17, 2008
groups.yahoo.com/group/AstroDeep/25
groups.yahoo.com/group/rmforall/85
www.flickr.com/photos/rmforall/1349101458/in/photostream/
The 5 closeups are about 2.2x2.2 arc-seconds wide and high, about 70x70 pixels.
The HUDF is 315x315 arc-seconds, with N at top and E at left.
Each side has 10,500x10,500 pixels at 0.03 arc-second per pixel.
Click on All Sizes and select Original to view the highest resolution image of
3022x2496 pixels, which can be also be conveniently seen directly at their
Zoomable image:
www.spacetelescope.org/images/html/zoomable/heic0714a.html
Notable in the deep background of the five closeups are ubiquitous bright blue
sources, presumably extremely hot ultraviolet before redshifting,
1 to a dozen or so pixels,
as single or short lines of spots, and a few irregular tiny blobs,
probably, as predicted in many recent simulations, the earliest massive,
short-lived hypernovae, GRBs with jets at various angles to our line of sight,
expanding bubbles, earliest molecular and dust clouds with light echoes and
bursts of star formation, and first small dwarf galaxies, always associated with
a subtle darker 3D random fractal mesh of filaments of H and He atomic gases.
As a scientific layman, I am grateful for specific cogent, civil feedback, based
on the details readily visible in images in the public domain.
www.spacetelescope.org/images/html/heic0714a.html
Hubble and Spitzer Uncover Smallest Galaxy Building Blocks
In this image of the Hubble Ultra Deep Field, several objects are identified
as the faintest, most compact galaxies ever observed in the distant
Universe.
They are so far away that we see them as they looked less than one billion
years after the Big Bang.
Blazing with the brilliance of millions of stars, each of the newly
discovered galaxies is a hundred to a thousand times smaller than our Milky
Way Galaxy.
The bottom row of pictures shows several of these clumps (distance expressed
in redshift value).
Three of the galaxies appear to be slightly disrupted.
Rather than being shaped like rounded blobs, they appear stretched into
tadpole-like shapes.
This is a sign that they may be interacting and merging with neighboring
galaxies to form larger structures.
The detection required joint observations between Hubble and NASA's Spitzer
Space Telescope.
Blue light seen by Hubble shows the presence of young stars.
The absence of red light from Spitzer observations conclusively shows that
these are truly young galaxies without an earlier generation of stars.
Credit: NASA, ESA, and N. Pirzkal (European Space Agency/STScI)
Id: heic0714a
Object: HUDF, UDF, Hubble Ultra Deep Field
Type: Cosmology
Instrument: ACS
Width: 2750
Height: 3312
Downloads
Images
www.spacetelescope.org/images/original/heic0714a.tif
Fullsize Original 17.085 MB
view with free software AlternaTIFF
alternatiff-1_8_4.exe for Firefox browser
Large JPEG
3,422 KB
Screensize JPEG
387 KB
www.spacetelescope.org/images/html/zoomable/heic0714a.html
Zoomable
Copyright-free material (more info).
www.esa.int/esaSC/SEMCGRMPQ5F_index_1.html
hubblesite.org/newscenter/archive/releases/2007/31
hubblesite.org/newscenter/archive/releases/2007/31/image/
www.spacetelescope.org/news/html/heic0714.html
www.spacetelescope.org/news/text/heic0714.txt
HEIC0714: EMBARGOED UNTIL 18:00 (CEST)/12:00 PM EDT 06 September, 2007
www.spacetelescope.org/news/html/heic0714.html
News release:
Hubble and Spitzer Space Telescopes find "Lego-block" galaxies in early
Universe
06-September 2007 The NASA/ESA Hubble Space Telescope and the NASA
Spitzer Space Telescope have joined forces to discover nine of the
smallest, faintest, most compact galaxies ever observed in the distant
Universe. Blazing with the brilliance of millions of stars, each of the
newly discovered galaxies is a hundred to a thousand times smaller than
our Milky Way Galaxy.
The conventional model for galaxy evolution predicts that small galaxies
in the early Universe evolved into the massive galaxies of today by
coalescing. Nine Lego-like "building block" galaxies initially detected
by Hubble likely contributed to the construction of the Universe as we
know it. "These are among the lowest mass galaxies ever directly
observed in the early Universe" says Nor Pirzkal of the European Space
Agency/STScI.
Pirzkal was surprised to find that the galaxies' estimated masses were
so small. Hubble's cousin observatory, NASA's Spitzer Space Telescope
was called upon to make precise determinations of their masses. The
Spitzer observations confirmed that these galaxies are some of the
smallest building blocks of the Universe.
These young galaxies offer important new insights into the Universe's
formative years, just one billion years after the Big Bang. Hubble
detected sapphire blue stars residing within the nine pristine galaxies.
The youthful stars are just a few million years old and are in the
process of turning Big Bang elements (hydrogen and helium) into heavier
elements. The stars have probably not yet begun to pollute the
surrounding space with elemental products forged within their cores.
"While blue light seen by Hubble shows the presence of young stars, it
is the absence of infrared light in the sensitive Spitzer images that
was conclusive in showing that these are truly young galaxies without an
earlier generation of stars," says Sangeeta Malhotra of Arizona State
University in Tempe, USA, one of the investigators.
The galaxies were first identified by James Rhoads of Arizona State
University, USA, and Chun Xu of the Shanghai Institute of Technical
Physics in Shanghai, China. Three of the galaxies appear to be slightly
disrupted -- rather than being shaped like rounded blobs, they appear
stretched into tadpole-like shapes. This is a sign that they may be
interacting and merging with neighbouring galaxies to form larger,
cohesive structures.
The galaxies were observed in the Hubble Ultra Deep Field (HUDF) with
Hubble's Advanced Camera for Surveys and the Near Infrared Camera and
Multi-Object Spectrometer as well as Spitzer's Infrared Array Camera and
the European Southern Observatory's Infrared Spectrometer and Array
Camera. Seeing and analysing such small galaxies at such a great
distance is at the very limit of the capabilities of the most powerful
telescopes. Images taken through different colour filters with the ACS
were supplemented with exposures taken through a so-called grism which
spreads the different colours emitted by the galaxies into short
"trails". The analysis of these trails allows the detection of emission
from glowing hydrogen gas, giving both the distance and an estimate of
the rate of star formation. These "grism spectra" -- taken with Hubble
and analysed with software developed at the Space Telescope-European
Coordinating Facility in Munich, Germany -- can be obtained for objects
that are significantly fainter than can be studied spectroscopically
with any other current telescope.
# # #
Notes for editors
The Hubble Space Telescope is a project of international cooperation
between ESA and NASA.
Pirzkal's main collaborators were Malhotra, Rhoads, Xu, and the GRism
ACS Program for Extragalactic Science (GRAPES) team.
Image credit: NASA, ESA and N. Pirzkal (European Space Agency/STScI)
If you wish to no longer receive these News and Photo Releases, please
send an email to distribution@spacetelescope.org with your name.
For more information, please contact:
Nor Pirzkal ;
European Space Agency/Space Telescope Science Institute, Baltimore, USA
Tel: 410-338-4879
Lars Lindberg Christensen ;
Hubble/ESA, Garching, Germany
Tel: +49-(0)89-3200-6306
Cellular: +49-(0)173-3872-621
Ray Villard ;
Space Telescope Science Institute, Baltimore, USA
Tel: +1-410-338-4514
Whitney Clavin
Jet Propulsion Laboratory, Pasadena, USA
Tel: +1-818-354-4673
AST HUDF Spitzer IR 9 galaxies z 4-5.7, N Pirzdal, S Malhotra, JE Rhoads, C Xu,
2007.05.01 28p
www.spacetelescope.org/news/science_paper/0612513.pdf
arXiv:astro-ph/0612513v2 1 May 2007
Optical to mid-IR observations of Lyman-a galaxies at z about 5 in the HUDF: a
young and low mass population
N. Pirzkal 1,2,
S. Malhotra 3,
J. E. Rhoads 3,
C. Xu 4
ABSTRACT
High redshift galaxies selected on the basis of their strong Lyman-a emission
tend to be young ages and small physical sizes.
We show this by analyzing the spectral energy distribution (SED) of 9 Lyman-a
emitting (LAE) galaxies at 4.0 < z < 5.7 in the Hubble Ultra Deep Field (HUDF).
Rest-frame UV to optical 700A < wavelength < 7500A luminosities, or upper
limits, are used to constrain old stellar populations.
We derive best fit, as well as maximally massive and maximally old, properties
of all 9 objects.
We show that these faint and distant objects are all very young, being most
likely only a few millions years old, and not massive, the mass in stars being
about 10E6 to 10E8 M sun.
Deep Spitzer Infrared Array Camera (IRAC) observations of these objects,
even in cases where objects were not detected,
were crucial in constraining the masses of these objects.
The space density of these objects, about 1.25 x 10E-4 per cubic Mpc is
comparable to previously reported space density of LAEs at moderate to high
redshifts.
These Lyman-a galaxies show modest star formation rates of about 8 M sun per
year, which is nevertheless strong enough to have allowed these galaxies to
assemble their stellar mass in less than a few 10E6 years.
These sources appear to have small physical sizes, usually smaller than 1 Kpc,
and are also rather concentrated.
They are likely to be some of the least massive and youngest high redshift galaxies observed to date.
Subject headings: galaxies: evolution, galaxies: high redshift, galaxies:
formation, galaxies: structure, surveys, cosmology
1 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
2 Affiliated with the Space Science Telescope Division of the European Space
Agency, ESTEC, Noordwijk, The Netherlands
3 School of Earth and Space Exploration, Arizona State University, Tempe, AZ
4 Shanghai Institute of Technical Physics, 500 Yutian Road, Shanghai, P.R. China 200083
____________________________________________________________
See similar images:
notable bright blue tiny sources on darker 3D fractal web in HUDF VLT ESO
28 images from 506 galaxies, z about 6 , RJ Bouwens, GD Illingworth,
JP Blakeslee, M Franx 2008.02.04 draft 36 page: Rich Murray 2008.08.17
rmforall.blogspot.com/2008_08_01_archive.htm
Sunday, August 17, 2008
groups.yahoo.com/group/AstroDeep/26
groups.yahoo.com/group/rmforall/86
bright blue 1-4 pixel sources on darker 3D fractal web in IR and visible light
HUDF images -- might be the clusters of earliest hypernovae in the
Naoki Yoshida and Lars Hernquist simulation: Rich Murray 2008.07.31
rmforall.blogspot.com/2008_07_01_archive.htm
Thursday, July 31, 2008
groups.yahoo.com/group/AstroDeep/24
groups.yahoo.com/group/rmforall/84
____________________________________________________________
Rich Murray, MA Room For All rmforall@comcast.net
505-501-2298 1943 Otowi Road Santa Fe, New Mexico 87505
groups.yahoo.com/group/rmforall/messages
groups.yahoo.com/group/AstroDeep/messages
____________________________________________________________
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/2dR8ctN
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 20.91° clockwise from up.
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/2dpzXVt
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 13.50° clockwise from up.
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/2f2iquC
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 25.17° counter-clockwise from up.
NGC 3631 (Arp 27 = PGC 34767)
Discovered (Apr 14, 1789) by William Herschel
Also observed (date?) by John Herschel
A magnitude 10.4 spiral galaxy (type SA(s)c?) in Ursa Major (RA 11 21 02.9, Dec +53 10 10)
Historical Identification: Per Dreyer, NGC 3631 (= GC 2379 = JH 858 = WH I 226, 1860 RA 11 13 06, NPD 36 03.1) is "pretty bright, large, round, suddenly very much brighter middle and mottled but not resolved nucleus".
Physical Information: Based on recessional velocity of 1155 km/sec, about 50 million light years away, in fair agreement with a redshift-independent distance estimate of 70 million light years. Given those values and an apparent size of 4.5 by 4.5 arcmin, about 80 thousand light years across.
"Excerpt courtesy of Courtney Seligman"
cseligman.com/text/atlas/ngc36.htm#3631
Image... Cherryvalley Observatory (I83). Telescope: 0.2-m SCT & SBIG STL-1301E CCD Camera @f7.6. Image Scale 2.17 arcsec/pixel, Field of View 46 x 37 arcmins.
Flat field and dark subtract calibration frames. Combined Stack of three images of 120 seconds each unfiltered and unbinned. CCD operating temperature: -35 degrees. Image acquisition and processing: CCD Soft v5, TheSky6 Professional and Mira Pro v7. February 18th 2016.
Dr. Halton Arp originally compiled the Atlas of peculiar galaxies with photographs he made mainly using the Palomar 200-inch telescope and the 48-inch Schmidt telescope between the years 1961 to 1966. Original image can be found here:
