View allAll Photos Tagged Redshift
ARP 294, Interacting Galaxies with Stellar Streams, NGC 3786 and NGC 3788, Ursa Major
NGC3786 and NGC3788 are a tight pair of apparently interacting spiral galaxies in the constellation of Ursa Major, first documented by W. Herschel around 1790. They are listed as ARP 294 in the Atlas of Peculiar Galaxies which includes examples of unusual structures found among galaxies. As the chart below indicates, the galaxies are very similar in angular size, around 2.2 arcmin, apparent magnitude of 13.3 (g), and morphological classification as peculiar intermediate spirals with a ring. Their redshift-based distances are 125.4 and 123.8 million light years respectively, suggesting a separation between them of 1.6 Mly. However, redshift-based distance estimates assume that redshift recession is due exclusively to the expansion of space, and do not correct for galaxies' "peculiar velocities" through space. For redshifts less than 0.01, or distances less than 138 Mly, it is generally accepted that redshift-independent distance measurements, such as the Cepheid period-luminosity relation, are more accurate. According to the NED extragalactic database, median redshift-independent distances for the pair are 158 and 183 Mly respectively, indicating a separation between them of 25 Mly. In either case, as their relatively undisturbed spiral arms confirm, the galaxies appear close due to similar lines of sight, and have not yet undergone major deformations due to close physical contact.
However, both galaxies are still interacting, although not with each other. Each one displays a faint stellar stream of a dwarf falaxy which appears to be in the process of merging. And, each displays a bright blue sector in its galactic disk where its intersecting stellar stream causes a blaze of starburst activity. On the annotated image the streams are marked as A and B, while the starburst regions are marked as S1, S2, and S3. Stream A appears to follow a straight line resulting from gravitational dispersal of a dwarf galaxy as it directly approached NGC3788, causing an explosion of starburst activity (S1) as it traversed the N perimeter of the spiral disk. Meanwhile, Stream B appears as a faint oval loop formed by stellar debris from a disrupted dwarf galaxy which has merged with NGC3786, and made at least one full orbit around it. Along the S and E perimeter of the main galaxy, two luminous blue regions (S2 and S3) indicate starburst activity at the intersections between the looping stellar stream and the main galactic disk.
Physical properties of the galaxies are listed in the chart on the annotated image. Values enclosed in parentheses are based on median redshift-independent distance measurements obtained from the NED database. Depending on the distance method used, the galaxies are between 25 and 50% smaller than the Milky Way, 30 to 70% less bright, and of approximately equal size to each other. Although both galaxies have faint emission lines in the spectrum of their nuclei, and the nucleus of NGC3786 appears bright in the X-ray band, NED extragalactic database does not register an active galactic nucleus in either galaxy.
Since galactic interactions and mergers significantly influence stellar dynamics, the rates of consumption, production, and the distribution of gas and dust, synthesis of new elements (metallicity), and the nature of the galactic nucleus, galactic encounters are of great interest in the study of galactic evolution.
The attached image includes a number of remote background galaxies and two quasars listed in the chart below. The most remote of these is LAMOST J114003.83+315503.5, lying at a light travel (lookback time) distance of 8.85 Bly. The object labeled G1 is identified by Simbad as a galaxy LAMOST J113941.45+315442.2, no angular size specified, which is not listed in the NED database. The object appears starlike on high resolution HST photographs, and is most likely mis-categorized.
HST image
Image details:
-Remote Takahashi TOA 150 x 1105mm, SBIG STF-8300C, Paramount GT GEM
-OSC 36 x 300 sec, 2x drizzle, 40% linear crop
-Software: DSS, XnView, StarNet++ v2, StarTools v1.3 and 1.8, Cosmological Calculator v3
This photo is really just meant to be informative and educational for those that are curious about the Universe, and want to know how things work. As photographers we capture Photons after all, so here is a bit of the Physics behind the light that we love to capture.
This image shows the Electromagnetic Spectrum of light from the Sun, after traveling through Earth's blue Nitrogen rich skies (photographed through a Quantitative Spectroscope).
The nanometer scale in the Spectroscope shows the wavelengths of visible light, that range from 400 nm - 700 nm. Invisible light at shorter wavelengths (beyond violet) include Ultraviolet (UV), X-Ray and Gamma Ray. Longer wavelengths of light (beneath red) include Infrared, Microwave and Radio Waves.
About the Sun:
The Sun is a G-type Main-Sequence Yellow Dwarf (G2V) Star. Through the process of fusion, the Sun burns approximately 600 million tonnes (metric tons) of Hydrogen each second, turning it into 596 million tonnes of Helium. As the Hydrogen nuclei fuse, Photons are emitted, which in short is why the Sun shines (and all the other stars). The Hydrogen Atom is the simplest and most abundant element in the Universe (with only 1 Proton and 1 Electron).
Through the process of fusion, more complex elements are made at different stages of a star's life and death cycle. This is what Carl Sagan meant with one of his well known quotes from Cosmos, “The nitrogen in our DNA, the calcium in our teeth, the iron in our blood, the carbon in our apple pies were made in the interiors of collapsing stars. We are made of starstuff.”
The Sun is roughly 150,000,000 km from Earth. The speed of light is 300,000 km/sec (186,000 miles/sec), which means that the light took just over 8 light-minutes (8 minutes and 26 seconds) to reach the Spectroscope in front of my camera lens.
Here is a very simplistic explanation of Spectroscopy, and how the Electromagnetic Light Spectrum is used in Astrophysics:
This image was photographed through a basic "High School Science Classroom" Quantitative Spectrometer (100 line resolution). With higher resolution Spectrometers on Telescopes, Astronomers can determine what chemical elements Stars and Planets are made of, as each chemical element has a unique light absorption fingerprint, that shows up as dark lines in the spectrum.
The amount that the absorption lines are shifted to red or blue (redshift and blueshift), is due to the Doppler effect and gives an indication if the celestial object is moving towards or away from us, and at what speed. This is how Scientists and Physicists know what the observable Universe is made of, and that the Universe is expanding.
More Info:
en.wikipedia.org/wiki/Spectral_line
en.wikipedia.org/wiki/Fraunhofer_lines
www.space.com/25732-redshift-blueshift.html
science-edu.larc.nasa.gov/EDDOCS/Wavelengths_for_Colors.html
Interested in Science, Physics & Astronomy?
Visit my Flipboard with lots of interesting articles:
flipboard.com/@mheigan/brain-food
Martin
-
The NASA/ESA/CSA James Webb Space Telescope is giving scientists their first detailed glimpse of supernovae from a time when our Universe was just a small fraction of its current age. A team using Webb data has identified 10 times more supernovae in the early Universe than were previously known. A few of the newfound exploding stars are the most distant examples of their type, including those used to measure the universe’s expansion rate.
To make these discoveries, the team analyzed imaging data obtained as part of the JWST Advanced Deep Extragalactic Survey (JADES) program. Webb is ideal for finding extremely distant supernovae because their light is stretched into longer wavelengths — a phenomenon known as cosmological redshift.
Prior to Webb’s launch, only a handful of supernovae had been found above a redshift of 2, which corresponds to when the universe was only 3.3 billion years old — just 25% of its current age. The JADES sample contains many supernovae that exploded even further in the past, when the universe was less than 2 billion years old. Previously, researchers used the NASA/ESA Hubble Space Telescope to view supernovae from when the universe was in the “young adult” stage. With JADES, scientists are seeing supernovae when the universe was in its “teens” or “pre-teens.” In the future, they hope to look back to the “toddler” or “infant” phase of the universe.
To discover the supernovae, the team compared multiple images taken up to one year apart and looked for sources that disappeared or appeared in those images. These objects that vary in observed brightness over time are called transients, and supernovae are a type of transient. In all, the JADES Transient Survey Sample team uncovered 79 supernovae in a patch of sky only about the thickness of a grain of rice held at arm’s length.
The team identified a number of high-redshift supernovae, including the farthest one ever spectroscopically confirmed, at a redshift of 3.6. Its progenitor star exploded when the universe was only 1.8 billion years old. It is a so-called core-collapse supernova, an explosion of a massive star.
These findings were presented in a press conference at the 244th meeting of the American Astronomical Society in Madison, Wisconsin. Learn more about these results here.
[Image description: Six space telescope images show close-ups of two different observations (rows) of three different galaxies (columns). Arrows point to bright blobs that are visible in one observation of the galaxy, but not the other.]
Credits: NASA, ESA, CSA, STScI; CC BY 4.0
M100 (NGC 4321), NGC 4322, NGC 4328 Interacting Galaxy Group, Coma Berenices
This galaxy was discovered by Pierre Mechain in 1781, then confirmed by Messier 29 days later, and listed as entry 100 in his catalog of nebulae and star clusters. He described the object as a faint nebula without a star. It was later documented by William Herschel who noted a brighter center presumably composed of stars, and by his son John Herschel in 1833 who initially found it to be not very remarkable. Observational notes of the nebula became more interesting as telescope technologies improved over the years. By 1850, M100 appears on the list of 16 "spiral nebulae" identified with Lord Rosse's giant reflector. And by 1888, entry 4321 in Dreyer's New General Catalogue describes the nebula as a "very remarkable... 2-branched spiral... with a bright mottled nucleus." In 1990, M100 was the very first object photographed by the Hubble Space Telescope, revealing a serious spherical aberration flaw in its mirror.
In most amateur telescopes this galaxy remains a humble visual target. However, with even modest apertures, it presents a captivating photographic subject surrounded by a cluster of dwarf companions. M 100 is a nearly face-on grand design spiral galaxy with two well defined spiral arms. Infrared studies of the central region reveal a delicate bar structure, which classifies it as an intermediate spiral of the SAB morphological type. Together with all the galaxies marked in white or blue on the annotated image, M100 is a rapidly moving member of the large Virgo Galaxy Cluster. Since this group has high peculiar velocity, or rapid movement through space relative to the Milky Way, redshifts of these galaxies do not accurately reflect Hubble Flow, or the expansion of space itself, and should not be used to estimate galaxy distances. In the chart below, physical properties of the group are calculated from the redshift-independent distance measurements listed in the NASA Extragalactic Database (NED). Based on the specified median distance of 51.67 million ly, we can calculate M100's diameter of 131,000 ly, and an absolute magnitude (V) of -21.65. In terms of morphology, dimensions, and mass (approximately 400 billion stars), the galaxy is quite similar to the Milky Way. Its greater overall brightness may be due to an active galactic nucleus (AGN) of the Hii LINER type, caused by ionizing radiation emanating from the accretion disk of a central supermassive black hole (SMBH) and/or from central regions of starburst activity.
Even at low resolution, the galaxy reveals many features typical of grand design spirals. Blue floccules in the spiral arms are OB Associations - immense clusters of recently formed large, hot stars. These are typically surrounded by parent clouds of hydrogen gas, which can glow red where they re-emit energy absorbed from starlight. Yellowish color toward the middle is due to a multitude of smaller, ancient stars remaining from the early stages of galaxy formation. Dark stripes and bands weaving through the galaxy disk are large clouds of obscuring dust and gas. And, the bright region in the center is generated by a dense population of ancient stars and by emissions from a central supermassive black hole (SMBH). In some galaxies, M100 included, this nuclear region is surrounded with a ring of rapid new star formation probably driven by nuclear outflows caused by SMBH radiation pressure, SMBH winds and jets, convection plumes, and increased supernova activity.
While it displays localized areas of starburst activity around the nucleus and within spiral arms, like most other spiral galaxies in the Virgo Cluster M100 has a low neutral hydrogen content and a lower average star formation rate (SFR) than what is found in isolated, field galaxies. Hydrogen gas is lost by a process called ram-pressure stripping as a cluster galaxy with high peculiar velocity moves through a relatively dense intergalactic medium (IGM) within a cluster. For more details, see section 41 here:
www.cloudynights.com/articles/cat/articles/basic-extragal...
The attached image demonstrates a number of smaller galaxies, annotated in blue, surrounding M100. Angular proximity and similar redshift values imply - but do not prove - physical proximity and gravitational connection in 3 dimensional space. Unfortunately, redshift-independent distance estimates for five of these galaxies are not available in the literature. In order to guesstimate their physical properties, in the attached chart we make a "reasonable" assumption that their distances are approximately 52 Mly, similar to the fairly well determined M100 distance. Recent studies regarding matter distribution in our local universe reveal that most major galaxies, the Milky Way and the Andromeda included, are surrounded by substantial numbers of irregular, spheroidal, and elliptical dwarf galaxies, and that most of these are passersby rather than satellites. While complex kinematic studies are required to determine which of the galaxies in the image are gravitationally bound, streams of luminous debris between M100, NGC4322, and NGC4328 are conclusive indicators of tidal interaction. Based on their redshifts, NGC4328 had a close encounter with M100 while moving toward its foreground, and NGC4322 while moving toward its background.
The other prominent galaxy in the field is NGC4312, a nearly edge-on unbarred spiral, discovered by W. Herschel in 1787. Based on its median redshift-independent distance estimate of 35.534 Mly and angular size of 4.37 arcmin, this galaxy is about one third the diameter of the Milky Way, and about one ninth as bright. It is another high peculiar velocity member of the Virgo Galaxy Cluster which has lost much of its neutral hydrogen through ram-pressure stripping. Based on X-ray images, the galaxy is suspected of hosting an intermediate mass black hole (IMBH) with a mass between 10,000 and 300,000 solar.
The image also reveals three faint galaxies in the remote background, and a modest quasar (QSO) lying at a distance of 3.56 billion ly.
Image Details:
Remote Takahashi TOA 150 x 1105 mm
OSC 27 x 300 sec exposures, 9 discarded
2x drizzle, 55% linear crop
Software: DSS, StarNet++ v2, XnView, StarTools
The @redshiftsports Dual-Position seatpost in my @jguillem Orient endurance bike.
I have just posted my impressions and aero position musings on my blog. Find the link here: torstenfrank.wordpress.com/2017/10/27/aero-position-probl...
--
Die Redshift Sports Dual-Position Sattelstütze in meinem J.Guillem Orient Endurance Rad.
Ich habe soeben meine Eindrücke und Zeitfahr-Positions-Überlegungen in meinem Blog publiziert. Anbei der Link: torstenfrank.wordpress.com/2017/10/27/aero-position-probl...
Sundays early autumn tour at Gimborn near Marienheide. Can you spot the two pieces I'm currently testing?
--
Sonntags Frühherbst Tour bei Gimborn nahe Marienheide. Könnt ihr die zwei Teile ausmachen, die ich gerade teste?
Mountain due east of Las Vegas on the border of Lake Mead draws in the early red shifted light of morning.
Draco is a constellation in the far northern sky. Its name is Latin for dragon. It was one of the 48 constellations listed by the 2nd century astronomer Ptolemy, and remains one of the 88 modern constellations today. The north pole of the ecliptic is in Draco. Draco is circumpolar (that is, never setting), and can be seen all year from northern latitudes.
Thuban (α Draconis) was the northern pole star from 3942 BC, when it moved farther north than Theta Boötis, until 1793 BC. The Egyptian Pyramids were designed to have one side facing north, with an entrance passage geometrically aligned so that Thuban would be visible at night. Due to the effects of precession, it will again be the pole star around the year AD 21000. It is a blue-white giant star of magnitude 3.7, 309 light-years from Earth. The traditional name of Alpha Draconis, Thuban, means "head of the serpent".
There are three stars under magnitude 3 in Draco. The brighter of the three, and the brightest star in Draco, is Gamma Draconis, traditionally called Etamin or Eltanin. It is an orange giant star of magnitude 2.2, 148 light-years from Earth. The aberration of starlight was discovered in 1728 when James Bradley observed Gamma Draconis. Nearby Beta Draconis, traditionally called Rastaban, is a yellow giant star of magnitude 2.8, 362 light-years from Earth. Its name shares a meaning with Thuban, "head of the serpent".[1]Draco also features several interacting galaxies and galaxy clusters. One such massive cluster is Abell 2218, located at a distance of 3 billion light-years (redshift 0.171).
Draco is home to several double stars and binary stars. Eta Draconis (the proper name is Athebyne) is a double star with a yellow-hued primary of magnitude 2.8 and a white-hued secondary of magnitude 8.2 located south of the primary. The two are separated by 4.8 arcseconds. Mu Draconis, traditionally called Alrakis, is a binary star with two white components. Magnitude 5.6 and 5.7, the two components orbit each other every 670 years. The Alrakis system is 88 light-years from Earth. Nu Draconis is a similar binary star with two white components, 100 light-years from Earth. Both components are of magnitude 4.9 and can be distinguished in a small amateur telescope or a pair of binoculars. Omicron Draconis is a double star divisible in small telescopes. The primary is an orange giant of magnitude 4.6, 322 light-years from Earth. The secondary is of magnitude 7.8. Psi Draconis (the proper name is Dziban ) is a binary star divisible in binoculars and small amateur telescopes, 72 light-years from Earth. The primary is a yellow-white star of magnitude 4.6 and the secondary is a yellow star of magnitude 5.8. 16 Draconis and 17 Draconis are part of a triple star 400 light-years from Earth, divisible in medium-sized amateur telescopes. The primary, a blue-white star of magnitude 5.1, is itself a binary with components of magnitude 5.4 and 6.5. The secondary is of magnitude 5.5 and the system is 400 light-years away.[1] 20 Draconis is a binary star with a white-hued primary of magnitude 7.1 and a yellow-hued secondary of magnitude 7.3 located east-northeast of the primary. The two are separated by 1.2 arcseconds at their maximum and have an orbital period of 420 years. As of 2012, the two components are approaching their maximum separation.[4] 39 Draconis is a triple star 188 light-years from Earth, divisible in small amateur telescopes. The primary is a blue star of magnitude 5.0, the secondary is a yellow star of magnitude 7.4, and the tertiary is a star of magnitude 8.0; the tertiary appears to be a close companion to the primary. 40 Draconis and 41 Draconis are a binary star divisible in small telescopes. The two orange dwarf stars are 170 light-years from Earth and are of magnitude 5.7 and 6.1.
R Draconis is a red Mira-type variable star with a period of about 8 months. Its average minimum magnitude is approximately 12.4, and its average maximum magnitude is approximately 7.6. It was discovered to be a variable star by Hans Geelmuyden in 1876.
The constellation contains the star recently named Kepler-10, which has been confirmed to be orbited by Kepler-10b, the smallest rocky Earth-sized planet yet detected outside of the Solar System.
One of deep-sky objects in Draco is the Cat's Eye Nebula (NGC 6543), a planetary nebula approximately 3,000 light-years away that was discovered by English astronomer William Herschel in 1786. It is 9th magnitude and was named for its appearance in the Hubble Space Telescope, though it appears as a fuzzy blue-green disk in an amateur telescope.[1] NGC 6543 has a very complex shape due to gravitational interactions between the components of the multiple star at its center, the progenitor of the nebula approximately 1,000 years ago.[6] It is located 9.6 arcminutes away from the north ecliptic pole to the west-northwest. It is also related to IC 4677, a nebula that appears as a bar 1.8 arcminutes to the west of the Cat's Eye nebula. In long-term exposures, IC 4677 appears as a portion of a ring surrounding the planetary nebula.
There are several faint galaxies in Draco, one of which is the lenticular galaxy NGC 5866 (sometimes considered to be Messier Object 102) that bears its name to a small group that also includes the spiral galaxies NGC 5879 and NGC 5907. Another is the Draco Dwarf Galaxy, one of the least luminous galaxies with an absolute magnitude of −8.6 and a diameter of only about 3,500 light years, discovered by Albert G. Wilson of Lowell Observatory in 1954. Another dwarf galaxy found in this constellation is PGC 39058.
PGC 39058, a dwarf galaxy found within the Draco constellation – picture taken by ESA/Hubble & NASA.
Draco also features several interacting galaxies and galaxy clusters. One such massive cluster is Abell 2218, located at a distance of 3 billion light-years (redshift 0.171). It acts as a gravitational lens for even more distant background galaxies, allowing astronomers to study those galaxies as well as Abell 2218 itself; more specifically, the lensing effect allows astronomers to confirm the cluster's mass as determined by x-ray emissions. One of the most well-known interacting galaxies is Arp 188, also called the "Tadpole Galaxy". Named for its appearance, which features a "tail" of stars 280,000 light-years long, the Tadpole Galaxy is at a distance of 420 million light-years (redshift 0.0314). The tail of stars drawn off the Tadpole Galaxy appears blue because the gravitational interaction disturbed clouds of gas and sparked star formation.
Q1634+706 is a quasar that holds the distinction of being the most distant object usually visible in an amateur telescope. At magnitude 14.4, it appears star-like, though it is at a distance of 12.9 billion light-years. The light of Q1634+706 has taken 8.6 billion years to reach Earth, a discrepancy attributable to the expansion of the universe.
Interacting Galaxies NGC 3718 and NGC 3729, Hickson 56, Ursa Major
NGC 3718 is an intermediate barred spiral galaxy whose spiral arms have been dramatically warped and stretched through gravitational interaction with a nearby neighbor to the ENE. The near-collision resulted in rapid displacement of galactic gas and dust triggering an outburst of new star formation. This is revealed in the form of several OB associations, or immense clusters of young, blue stars. The full extent of the spiral arms is about 13 arcmin, which corresponds to 173,000 light years. The luminous central portion is about 68,000 light years in diameter, and half as bright as the Milky Way. It consists of a large galactic bulge composed of ancient, yellow stars, surrounded by a light blue region of new star formation. The bulge is bisected by dark equatorial dust lanes, which also appear to be warped. NGC 3718 has a very bright active galactic nucleus of the Seyfert type powered by a central supermassive black hole.
The interacting galaxy, NGC 3729, which lies about 12 arcmin to the ENE, is also a barred spiral galaxy warped by gravitational interaction. Its spiral arms have beed dispersed into a featureless faint nebulosity. Its barred nucleus is surrounded by a prominent ring mottled with starburst activity. Based on the K_s band luminosity of the nucleus, the galaxy is thought to have a central intermediate-mass black hole. The oval cloud NE of the ncleus may be a tidal tail extending along the line of sight, or a disturbed satellite galaxy.
Measured and derived properties of the two galaxies are listed in the chart below. Although they appear to be very near to each other, their redshifts suggest the two galaxies are now about 1.1 million light years apart in 3 dimensions, NGC 3729 being the more distant. Eventually, the two galaxies are expected to merge into a giant elliptical galaxy.
On a larger scale, the pair belong to the Ursa Major Galaxy Cluster, which is itself a component of the Virgo Supercluster.
South of NGC 3718, around 370 million light years distant, lies Hickson Compact Group 56, a cluster of five tightly interacting galaxies, which is the subject for a separate post.
A number of remote galaxies and two quasars are identified in the annotated image, and listed in the chart below. The most remote is SDSS J113228.23+525328.8, located at light travel distance of 11.1 billion light years, or proper distance of 19.5 billion LY (in the present epoch). When the photons were emitted, the quasar was receding at 256,102 km/s, while at the present time it is estimated to be receding at superluminal 422,004 km/s. With absolute magnitude of -29.63, it is about 3,400 times brighter than the Milky Way galaxy. 99.38% of its light is extincted, or literally diluted by the expansion of the intervening space.
Image Details:
Meade 8'' ACF, AP 0.7x compressor, 200 x 1400 mm
iEQ30pro mount, Orion 60mm f/4 SSAGpro autoguider
Canon T3i modified camera, Astronomik L3 filter
29 x 300 sec subs (7 discarded), iso 1600, 30 darks, 30 bias, 2x drizzle, 40% linear crop
Software: PHD2, DSS, XnView, StarNet++, StarTools.
NGC 7479, Caldwell 44, Pegasus, Propeller Galaxy
NGC7479 is a distorted barred spiral galaxy in the constellation of Pegasus, discovered by W. Herschel in 1784. With apparent diameter of 4.4 arcmin, and apparent magnitude of 10.85 (V), visual observation calls for large apertures. However, its basic structures are evident photographically with modest telescopes. From its measurable properties we can derive light travel distance (lookback time) of 110 million light years, redshift recession velocity of 2,379 km/s, actual diameter of 140,000 ly, and absolute magnitude of -21.83 (V), approximately 1.5 times as bright as the Milky Way. NGC7479 has an active galactic nucleus (AGN) which is 8.5 times brighter in the near IR (z filter) than in the visible band, and which emits narrow spectral lines of weakly ionized elements. These characteristics classify it as a Seyfert 2 and a LINER galaxy. It is powered by an actively accreting central supermassive black hole (SMBH) obscured by a large, dense cloud of light-absobing gas and dust. The nucleus is also active at radio frequencies, suggesting the SMBH has polar jets emitting synchrotron radiation. Bright blue floccules in the spiral arms and even within the bar are OB Associations, or vast clusters of recently formed blue giant stars which emit most of their energy in the ultraviolet band. NGC7479 is an isolated field galaxy with no nearby neighbors. Starburst activity, several stellar streams, and gravitational distortion in the W spiral arm are thought to have been caused by a merger with one or more dwarf satellite galaxies between 300 and 100 million years ago.
As the annotated image illustrates, different spectral bands reveal different details within a galaxy. In the ultraviolet band (GALEX), the most prominent features are OB associations, starburst regions, and reflection nebulae. The compact, round UV signal overlapping the N arm of the bar may be the remnant nucleus of a merged dwarf galaxy. The NGC7479 nucleus is not prominent because it is surrounded by a thick layer of gas and dust which absorb and scatter predominantly UV light. However, the brightest feature on the infrared (2MASS) image of the galaxy is precisely the main galactic nucleus with a central SMBH, because longer wavelengths are less obsured. The bulge and the bar are also distinctive due to the presence of ancient cool and red Population II stars. Radio frequency imaging of the galaxy reveals the presence of a bright jet-like feature, centered on the nucleus, and extending through the bar about 20,000 light years in the N and in the S direction. The jet's spiral morphology mildly curves in the direction opposite to that of the stellar and gaseous spiral arms, suggesting that the two structures may be counter-rotating. Jet bending can be caused by precession of the central SMBH accretion disk, by the presence of a binary central SMBH, and/or an off center merger with another galaxy. Based on the rate of expansion and the maximum distance from the nucleus, the jet is felt to be less than 10 million years old.
A large galaxy cluster is visible in the remote background at an estimated light travel distance of 1.5 to 2 billion light years. Only two of these have assigned identifiers. Their measurable and derived properties are listed in the chart on the annotated image.
Image details:
-Remote Takahashi TOA 150 x 1105 mm, Paramount GT GEM,
-OSC 34 x 300 sec, 2x drizzle, 50% linear crop,
-Software: DSS, XnView, StarNet++ v2, StarTools v1.3 and 1.7, Cosmological Calculator v3
it might be hard for people these days to imagine that the was a time before editing tools of the digital kind all around us... this is me as a youngling a picture taken of me holding my own head in my hand which I used as a Christmas card and sent to fiends and friends alike...
this is the original photo without the Christmas greetings... well the original photo of my hand since the pic of my mug is another photo taken by me, a kind of double-self-portrait...
Peace and Noise!
My J.Guillem Orient in front of the Junior University in Wuppertal.
Current spec:
J.Guillem Orient frame, J.Guillem Titanium seat post, SRAM red eTap HRD group, Quarq DZero Powermeter, Brooks Cambium C15 carved saddle, redshift sports Shockstop Stem, Profile Design T1+ aerobars, DT Swiss ERC 1400 Spline 47 wheels, Vittoria Corsa G+ tires.
--
Mein J.Guillem Orient vor der Junior Uni in Wuppertal.
Aktuelle Konfiguration:
J.Guillem Orient frame, J.Guillem Titan-Sattelstütze, SRAM red eTap HRD Gruppe, Quarq DZero Leistungsmesser, Brooks Cambium C15 carved Sattel, redshift sports Shockstop Stem, Profile Design T1+ aerobars, DT Swiss ERC 1400 Spline 47 Laufräder, Vittoria Corsa G+ Reifen.
A scant dwarf galaxy imaged a few days ago by Hubble. There isn't a whole lot to see here beyond the central smudge and the rather impressive area of star formation along the lower edge of the composition. It is interesting that all of the older, dimmer stars seem to come together in a smooth central region, while brighter, younger, individually resolved stars lie in the outer regions, much like a larger spiral galaxy.
This image marks the first moment I am fully caught up on all of the observations in this proposal. I can now simply process them as they come along instead of madly trying to catch up only to fall behind as each new image comes down.
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 47.02° counter-clockwise from up.
this is a pic from some of my experimenting with my old analog Zenit systematic camera, with long time shutter exposure and a heavy light source you could become impish, goblin-like and monstrous, great fun for a silly young chap like me :) hooked on the role-playing fantasy aesthetics ;)
Peace and Noise!
/ MushroomBrain
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
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/2dDdQq5
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is up.
NGC 5364 (NGC 5317) and NGC 5363 Galaxy Group,Virgo
NGC 5364, also catalogued as NGC 5317, is a "grand-design" spiral galaxy discovered by William Herschel in 1786. Its morphological classification of SA(rs)bc pec indicates an incomplete ring structure, loosely wound spiral arms, and a peculiar asymmetry of the galactic bulge and the spiral arms which is probably due to gravitational perturbation by its neighbors. The most likely cause is the nearby lenticular galaxy NGC 5360, although some sources suggest that the more distant NGC 5363 also shows evidence of gravitational interaction. Based on its redshift and apparent size and magnitude, NGC 5364 is about 57.4 million light years distant, and receding at 1,239 km/s due to the expansion of the Universe. It is approximately 93,000 LY in diameter, and half as bright as the Milky Way. Light blue floccules in the spiral arms are OB Associations, or immense clusters of large, very hot young stars. Hubble images of the galaxy also show numerous regions of hydrogen gas partially ionised by ultraviolet light from recently formed stars.
The other major galaxy in the image is NGC 5363, also discovered by William Herschel in 1784. As a fairly featureless lenticular galaxy, with a well developed nuclear bulge and a diffuse galactic disk, it is far less spectacular in the visible band than its grand-design spiral companion. However, in the infrared band, the galaxy displays two prominent lanes of cold dust which still retain evidence of a spiral structure and a central bar. The total mass of interstellar dust is about 100 times greater than expected from the total mass lost by evolved stars, which suggests an external origin. The detection of density shells within the galaxy as evidence of recent mergers confirms the hypothesis that the excess interstellar dust was acquired through accretion. Further, ultraviolet studies reveal the presence of young, hot stars born during star formation activity caused by a recent merger. Spectroscopic studies of the central region show evidence of an active galactic nucleus (AGN) of the LINER type, powered by the accretion disk of a central supermassive black hole (SMBH) with a mass of 375 million solar. The AGN is also a source of radio waves, indicating the precence of polar jets emanating from the central SMBH, generating synchrotron radiation. Thus, when studied throughout the electromagnetic spectrum, this apparently featureless galaxy tells a fascinating story. Based on measurable properties (redshift, apparent magnitude, and angular size), NGC 5363 is about 90,000 LY in diameter, and one third as bright as the Milky Way (much of its visible light is extincted by the dust). It lies at a distance of 57 million LY, receding at 1,129 km/s due to the expansion of the Universe. It is approximately 5 million LY distant from its spiral companion, NGC 5364, so it does not appear likely that either is tidaly deforming the other at present, though they are members of the same gravitationally bound galaxy cluster.
The other members within the photograph belonging to the NGC 5364 galaxy group are marked in light blue color on the annotated image, and their physical properties are described on the attached chart. The group belongs to the Virgo III Galaxy Group, which is itself the E part of the large Virgo Galaxy Cluster.
www.atlasoftheuniverse.com/galgrps/viriii.html
In the backround lie more remote galaxies at distances between 250 million and 1.5 billion LY. These are marked in green and yellow color on the annotated image, depending on their redshift. Included also are four quasars QSOs). The most distant of these is WISEA J135345.93+051305.4. Its redshift of 3.400 indicates that the light we are presently recording travelled for 11.8 billion years to reach us (lookback time, or light travel distance). When the light was emitted, the quasar was about 16,000 times brighter than the Milky Way, and was receding from the future location of our galaxy at 270,343 km/sec (redshift, apparent, or relativistic recession velocity). In the present epoch, its (comoving = proper) distance is around 22.4 billion LY, and it is receding at the superluminal proper recession velocity of 483,700 km/s. The quasar is presently located well beyond the cosmic event horizon, and the photons it is presently emitting can never reach us. It can be calculated that 99.73% of the light originally emitted was lost to "cosmological extinction", or literally diluted by the expansion of space through which it travelled.
Image Details:
-Remote Takahashi TOA 150 x 1105mm, Paramount GT GEM
-29 x 300 sec OSC, 15% and 25% area crop
-Software:
DSS, XnView, StarNet++, StarTools v 1.3 and 1.7,
Extragalactic Cosmological Calculator 2
Located in the northern celestial hemisphere, Abell 1703 is composed of over one hundred different galaxies that act as a powerful cosmic telescope, or gravitational lens. The gravitational lens produced by the massive galaxy cluster in the foreground (the yellow mostly elliptical galaxies scattered across the image) bends the light rays in a way that can stretch the images and so amplify the brightness of the light rays from more distant galaxies. In the process it distorts their shapes and produces multiple banana-shaped images of the original galaxies. The result is the stunning image seen here - a view deeper into the Universe than possible with current technology alone. Abell 1703 is located at 3 billion light-years from the Earth (redshift 0.26).
United Arab Emirates Air Force, Sikorsky UH-60L Blackhawk, msn 42361, reg 2621. Seen at Dubai Airshow 2021 held at Al Maktoum DWC / OMDW. carrying two Alta Redshift electric motorbikes (one each side) two deploy a Silent Special Ops team or take your cousins for a desert joy trip.
The Redshift Star Fighter is always guarded by a pair of elite green soldiers.
While docked the ship is charged from power harnessed from a subterranean volcanic fissure.
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/T68ekd
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 8.42° clockwise from up.
NGC 3184 (NGC 3180), (Little Pinwheel Galaxy), NGC 3179, Ursa Major
Image Details:
-TSAPO100Q astrograph, Sigma APO 1.4x tele-extender (100 x 812 mm)
- Ioptron IEQ30pro mount, Orion 60mm F/4 SSAGpro autoguider
-Canon T3i camera, no filters
-20 x 240 sec exposures, iso 1600, 30 darks, 30 bias, 2x drizzle, 25% crop
-Software: PHD2, DSS, XnView, StarNet++, StarTools v 1.3 and 1.7
-Limiting magnitude on the original is better than 18.5.
NGC 3184 (NGC 3180), (Little Pinwheel Galaxy), NGC 3179, Ursa Major
NGC 3184 is a face-on mixed barred-nonbarred spiral galaxy with morphological classification SABc. NED database lists its apparent magnitude in the visible band between 13.5 and 11.49, which is the most recent (1977), and will be adopted here, although it appears at least 1 magnitude brighter on my photograph. Its mean redshift-independent distance is 12.268 Mpc, or 40 Mly. Its redshift-based (Hubble Flow) distance calculated in the chart below is 27.35 million light years, and recession velocity 590 km/sec. Based on its angular size of 8.5 arcmin, the galaxy is about 67,500 ly in diameter. Its calculated absolute magnitude of only -18.14 is probably too low, and should be updated with more reliable photometric data. The galaxy has a small, bright nucleus and long spiral arms rendered prominently blue by large numbers of hot, young stars and OB associations. Due to an error in the New General Catalog, this galaxy is also listed as NGC 3180. The galaxy is notable for a high abundance of heavy elements, making it suitable for rocky planets and interesting exobiology. From its perspective, our Galaxy would appear about twice as large in diameter, and much brighter. Photography indicates the presence of several large star-forming HII regions. The most prominent one is designted as NGC 3181. The annotated image below indicates the position of an ultra-luminous X-ray source (ULX), possibly indicating the presence of an intermediate-mass black hole. Such objects can be associated with bright transient optical signals lasting several days.
www.cloudynights.com/articles/cat/articles/transient-opti...
About 25 arcmin to the south is NGC 3179, a magnitude 13.7 (g) galaxy, 2 arcmin in apparent size. It seems to be a giant spiral galaxy, 326 million LY distant, and about 70% larger in diameter and brighter than the Milky Way.
The most remote recorded object is quasar (QSO) [VV96] J101732.7+410722. Based on its redshift and apparent magnitude, it can be calculated that the photons presently reaching us were emitted 6.2 billion years ago, long before the formation of our Solar system. It is about 83 times brighter than the entire Milky Way galaxy, and is receding due to the expansion of the universe at nearly half the speed of light.