View allAll Photos Tagged Redshift
#19. The Millennium Simulation, announced 2005.06.02 by the Virgo consortium, used the largest supercomputer in Europe, at the German Astrophysical Virtual Observatory, for over a month to model the history of the Universe in a cube over 2 billion light years on a side, holding 20 million galaxies.
static.flickr.com/13/18135102_07a58fd89d_o.jpg
This image is a closeup of the results at redshift z = 0, showing a 15 MPC/h thick slice, showing the visible light distribution, which closely follows the mass distribution. The view is four times wider than in #18, so that the width of the image is 1628 MLy. The length of the central large and dense galaxy cluster is about 60 MLy.
1024 X 768 pixels jpg 0.970950 MB
The distance measure Mpc/h has been used for decades to adjust to the fact that the Hubble constant = H has not been exactly determined. Mpc is megaparsecs.
A parsec is 3.26 light years. The Millennium Simulation used the value 0.73 for the Hubble constant H.
To get the distance in Mpc, we multiply their value by 100/H = 100/0.73 = 1.37 .
The huge, densely packed galaxy cluster, holding thousands of galaxies, for the greenish central region, has a length of about 60 MLy. In contrast, the nearest large neighbor to our Milky Way galaxy is Andromeda galaxy at 2.2 MLy distance.
The distribution of mass in the Universe is very fractile -- it looks just as complex and very much the same at a very wide range of distance scales.
So, even though I do not know how wide this image would be in terms of angular measures (degrees, minutes, seconds), it is probably justified to compare it to the Capodimonte Deep Field subtle background visible light images.
Many features are the same: complex 3D fractile network, with bright boundaries around both brighter (more dense) and dimmer (more empty) regions, and both brighter and thicker and thinner and dimmer lines, marked by myriad tiny dense features. I don't believe that the MS image includes gravitational lensing, which must be a complex factor in the CDF images.
Click on All Sizes to view Original.
www.pparc.ac.uk/Nw/millennium_sim.asp The Virgo consortium
www.mpa-garching.mpg.de/galform/millennium/
www.mpa-garching.mpg.de/galform/millennium/galseq_D_063.jpg
arxiv.org/abs/astro-ph/0504097
Simulating the joint evolution of quasars, galaxies and their large-scale distribution
pil.phys.uniroma1.it/debate3.html
On the fractile structure of the universe
Sylos Labini, Montuori & Pietronero
Canon Canonet
Fuji Velvia 100F
cross-processed in Tetenal C41 AND bleach bypassed
The latest experiment in bleach bypassing: xpro'd slide film that's also bleach bypassed. Conclusion: there's definitely a little bit of Velvia's characteristic redshift (more like a pinkshift), but mostly it just looks bleach bypassed. Not worth wasting a roll of Velvia on.
By pushing NASA's Hubble Space Telescope to its limits, an international team of astronomers has shattered the cosmic distance record by measuring the farthest galaxy ever seen in the universe. This surprisingly bright, infant galaxy, named GN-z11, is seen as it was 13.4 billion years in the past, just 400 million years after the big bang. GN-z11 is located in the direction of the constellation of Ursa Major.
"We've taken a major step back in time, beyond what we'd ever expected to be able to do with Hubble. We see GN-z11 at a time when the universe was only three percent of its current age," explained principal investigator Pascal Oesch of Yale University in New Haven, Connecticut. The team includes scientists from Yale University, the Space Telescope Science Institute (STScI) in Baltimore, Maryland, and the University of California in Santa Cruz, California.
Astronomers are closing in on the first galaxies that formed in the universe. The new Hubble observations take astronomers into a realm that was once thought to be only reachable with NASA's upcoming James Webb Space Telescope.
This measurement provides strong evidence that some unusual and unexpectedly bright galaxies found earlier in Hubble images are really at extraordinary distances. Previously, the team had estimated GN-z11's distance by determining its color through imaging with Hubble and NASA's Spitzer Space Telescope. Now, for the first time for a galaxy at such an extreme distance, the team used Hubble's Wide Field Camera 3 to precisely measure the distance to GN-z11 spectroscopically by splitting the light into its component colors.
Astronomers measure large distances by determining the "redshift" of a galaxy. This phenomenon is a result of the expansion of the universe; every distant object in the universe appears to be receding from us because its light is stretched to longer, redder wavelengths as it travels through expanding space to reach our telescopes. The greater the redshift, the farther the galaxy.
"Our spectroscopic observations reveal the galaxy to be even farther away than we had originally thought, right at the distance limit of what Hubble can observe," said Gabriel Brammer of STScI, second author of the study.
Before astronomers determined the distance for GN-z11, the most distant galaxy measured spectroscopically had a redshift of 8.68 (13.2 billion years in the past). Now, the team has confirmed GN-z11 to be at a redshift of 11.1, nearly 200 million years closer to the time of the big bang. "This is an extraordinary accomplishment for Hubble. It managed to beat all the previous distance records held for years by much larger ground-based telescopes," said investigator Pieter van Dokkum of Yale University. "This new record will likely stand until the launch of the James Webb Space Telescope."
The combination of Hubble's and Spitzer's imaging reveals that GN-z11 is 25 times smaller than the Milky Way and has just one percent of our galaxy's mass in stars. However, the newborn GN-z11 is growing fast, forming stars at a rate about 20 times greater than our galaxy does today. This makes such an extremely remote galaxy bright enough for astronomers to find and perform detailed observations with both Hubble and Spitzer.
The results reveal surprising new clues about the nature of the very early universe. "It's amazing that a galaxy so massive existed only 200 million to 300 million years after the very first stars started to form. It takes really fast growth, producing stars at a huge rate, to have formed a galaxy that is a billion solar masses so soon," explained investigator Garth Illingworth of the University of California, Santa Cruz.
These findings provide a tantalizing preview of the observations that the James Webb Space Telescope will perform after it is launched into space in 2018. "Hubble and Spitzer are already reaching into Webb territory," Oesch said. "This new discovery shows that the Webb telescope will surely find many such young galaxies reaching back to when the first galaxies were forming," added Illingworth.
This discovery also has important consequences for NASA's planned Wide-Field Infrared Survey Telescope (WFIRST), which will have the ability to find thousands of such bright, very distant galaxies.
The team's findings will appear in the March 8, 2016, edition of The Astrophysical Journal.
#18. The Millennium Simulation, announced 2005.06.02 by the Virgo consortium, used the largest supercomputer in Europe, at the German Astrophysical Virtual Observatory, for over a month to model the history of the Universe in a cube over 2 billion light years on a side, holding 20 million galaxies.
static.flickr.com/12/18135101_1ef7723b85_o.jpg
This image is a closeup of the results at redshift z = 0, showing a 15 MPC/h thick slice, showing the mass distribution, not the visible light.
2048 X 1536 pixels jpg 2.07411 MB
You can magnify this image 8X to see pixels of 1 mm size on a 17" monitor.
The distance measure Mpc/h has been used for decades to adjust to the fact that the Hubble constant = H has not been exactly determined. Mpc is megaparsecs.
A parsec is 3.26 light years. The Millennium Simulation used the value 0.73 for the Hubble constant H.
To get the distance in Mpc, we multiply their value by 100/H = 100/0.73 = 1.37 , which for the scale bar of 31.25 Mpc/h becomes 42.8 Mpc = 139.6 MLy.
This image has a width, directly measured on my monitor, of 91.1 Mpc/h =
124.8 Mpc = 406.9 MLy.
The huge, densely packed galaxy cluster, holding thousands of galaxies, for the greenish central region, has a length of about 2/13.6 = 14.7 % of the image width = 60 MLy. In contrast, the nearest large neighbor to our Milky Way galaxy is Andromeda galaxy at 2.2 MLy distance.
The distribution of mass in the Universe is very fractile -- it looks just as complex and very much the same at a very wide range of distance scales.
So, even though I do not know how wide this image would be in terms of angular measures (degrees, minutes, seconds), it is probably justified to compare it to the Capodimonte Deep Field subtle background visible light images.
Many features are the same: complex 3D fractile network, with bright boundaries around both brighter (more dense) and dimmer (more empty) regions, and both brighter and thicker and thinner and dimmer lines, marked by myriad tiny dense features. I don't believe that the MS image includes gravitational lensing, which must be a complex factor in the CDF images.
Click on All Sizes to view Large and Original.
www.pparc.ac.uk/Nw/millennium_sim.asp The Virgo consortium
www.mpa-garching.mpg.de/galform/millennium/
www.mpa-garching.mpg.de/galform/millennium/seqF_063a.jpg
arxiv.org/abs/astro-ph/0504097
Simulating the joint evolution of quasars, galaxies and their large-scale distribution
pil.phys.uniroma1.it/debate3.html
On the fractile structure of the universe
Sylos Labini, Montuori & Pietronero
www.space.com/scienceastronomy/first_star_011115.html popular article by Robert Roy Britt 2001.11.15 on www.space.com re Tom Abel simulation of the first start in our Universe www.tomabel.com/
www.solstation.com/x-objects/first.htm excellent general introduction to many recent simulations of the first stars -- many links
www.astro.psu.edu/users/tabel/GB/gb.html many awesome images and movies of simulations of the first structures and stars in our Universe by Tom Abel, Greg Bryan, and Mike Norman in 2001
www.astro.psu.edu/users/tabel/GB/gb.html frame by frame tour of the simulation with commentary
www.mpia-hd.mpg.de/GALAXIES/CADIS/irsee2003/PROCEEDINGS/A...
the first stars, a slideshow review by Tom Abel
Compare #21 Closeup of many tiny bright sources on background mesh in HUDF.
NGC 3521 is a flocculent[4] intermediate spiral galaxy located in the constellation Leo. Its velocity with respect to the cosmic microwave background is 1167 ± 26 km/s, which corresponds to a Hubble distance of 56.1 ± 4.1 Mly (17.21 ± 1.26 Mpc).[1] However, 26 non-redshift measurements give a much closer distance of 37.17 ± 1.83 Mly (11.395 ± 0.56 Mpc).[5] It was discovered by German-British astronomer William Herschel on 22 February 1784.[6] Source:Wikipedia
NGC 4151 est une galaxie spirale intermédiaire relativement rapprochée et située dans la constellation des Chiens de chasse.
À ce jour, une quinzaine de mesures non basées sur le décalage vers le rouge (redshift) donnent une distance de 31 millions d'al !
NGC 4145 est une galaxie spirale intermédiaire relativement rapprochée et située dans la constellation des Chiens de chasse.
À ce jour, 18 mesures non basées sur le décalage vers le rouge (redshift) donnent une distance de 51,1 millions d'al !
Lunette ASKAR APO120
Caméra ASI2600MC
Monture Ioptron CEM120
Traitement Pixinsight & Photoshop
95 x 240s soit 6H24
Hoover Dam as seen from the bypass bridge pedestrian walkway.
Moskva 5 6x9 folding rangefinder on expired TMax 100 film developed in caffenol CL, semi-stand 47 minutes at 72 F. To get the color shift, I scanned these as color negatives and post processed them in LR. Still working on the overall effect/look and for images that lend themselves to this type of treatment. Appreciate any feedback.
Arp 128 - part of Arp’s ‘E and E-like galaxies – close to and perturbing spirals’ – consists of:
PGC 4645 (UGC 827a) – the spiral on the right (west)
PGC 200189 (UGC 827b) – the elliptical on the left
Located about four degrees from M74 in Pisces, redshift shows that these are between 500 and 560 million light-years away.
Luminance – 25x600s – 250 minutes – binned 1x1
RGB – 12:9:8x300s – 60:45:40 minutes each – binned 2x2
395 minutes total exposure – 6 hours 35 minutes
Imaged October 7th, 8th, 10th and 13th, 2023 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.
"...I used to think it didn’t. Now I think it does. And I think that mine is this: a morbid longing for the picturesque at all costs.”
Donna Tartt, The Secret History
Diana F+, Fuji Tungsten T64, cross-processed
ARP 140, NGC 274 and NGC 275 Interacting Galaxies, Cetus
In 1966, American astronomer Halton Arp published a catalog of 338 peculiar galaxies under the assumption that the distorted shapes were due to large galactic ejections. It was soon demonstrated that the majority of the objects are in fact interacting galaxies, deforming each other by tidal forces. Entry number 140 is an example of two such galaxies, NGC 274 and NGC 275 in the constellation of Cetus, which appear to be in the early stages of merging. NGC 274 is a lenticular galaxy discovered by William Herschel in 1785. Although NGC 275 is in the same field of view, and of nearly the same brightness and identical contrast index, there is no mention of it in any of his observation notes. It is not unlikely that he mistook the pair for a single object. NGC 275 was first identified as a separate galaxy by his son, John Herschel in 1828.
Distance measurements of extragalactic objects are essential in estimating their physical properties, and are usually based on the redshift for very distant objects. However, redshift is dependent on two velocity components. One is due to the expansion of space, and the second to the object's "peculiar velocity" through space relative to the observer. It is generally accepted that "redshift-independent distances" are more accurate for redshifts lower than 0.01. In the case of ARP 140, redshift-independent distances are questionable on several levels. As listed in the NED database, the number of measurements is statistically too low. The range of results is too large, and varies by several hundred percent between low and high values. Distance calculations are based on outdated Hubble parameter (Ho) values. And, mean distance estimates for the two galaxies place them very widely apart, though they convincingly appear to be interacting in close contact. For these reasons, galaxy properties in the attached chart are calculated on the basis of their redshift derived distances.
Using the redshift method, NGC 274 lies at a distance of 80.84 Mly, receding at 1,746 km/s. Its actual diameter is about 37,200 ly, and absolute magnitude -19.46. It is approximately one third in size and brightness as our Milky Way galaxy. SIMBAD database classifies it as E/S0, an intermediate between an elliptical and a lenticular galaxy, while the NED database describes it as SAB0(r) pec, which is an intermediate spiral with a ring and a peculiar morphology. On my low magnification image I can barely visualize a full oval ring once my attention is drawn to it. On close examination, a couple of delicate features are present which suggest gravitational interaction. One is slight eccentricity of the galaxy relative to its nucleus. Another one is the presence of three wispy stellar streamers between the two galaxies. These features are better appreciated on Halton Arp's negative, high contrast, embossed original image.
NGC 275 is classified as SB(rs)cd pec, indicating a loosely wound barred spiral galaxy with an incomplete ring and a peculiar morphology. Its redshift based distance is 80.57 Mly, recession velocity 1,740 km/s, actual diameter approximately 37,700 ly, absolute magnitude -19.28, and brightness about one quarter that of the Milky Way. Even at low magnification, this galaxy shows markedly disrupted spiral arms and numerous bright blue floccules of starburst activity. While few references describe ARP 140 as a widely separated line-of-sight pair, it might be difficult to explain away peculiar features in both galaxies consistent with close gravitational interaction.
The attached image also includes a very distant galaxy, LEDA 1026074, lying at a distance of 1.5 billion light years, which is about half the size and brightness of the Milky Way. The background is strewn with numerous remote galaxies marked with letter "G" on the annotated image. Unfortunately, they have neither measurable properties nor identifiers listed in SIMBAD and NED databases. Based on their angular size alone, they would lie at distances between 1.5 and 3 billion light years. Of course, many of them might be dwarf galaxies, in which case they would be much closer. Without redshift information, there is no way to know.
The most remote object is quasar (QSO) SDSS J005134.95-065841.7, which presents barely above the limiting magnitude. Its apparent magnitude is presently about 0.5 mag brighter than listed. Quasars commonly manifest short and long term variability depending on the matter available to them for accretion. Based on its redshift of 1.38400, it lies at a light travel distance (lookback time) of 9.1 billion light years, and is about 70 times brighter than our Galaxy. When the light we are now recording was emitted, the object was receding from our location at 210,080 km/s. In the present cosmological epoch, its "proper recession velocity" is 292,040 km/s - very nearly the speed of light. When its proper recession velocity becomes superluminal, it will have crossed the cosmic event horizon and, over the next 9 billion years, its light will forever fade away into the infrared and radio waves.
Image Details:
-Remote Takahashi TOA 150 x 1105 mm
-OSC 32 x 300 sec, 2x drizzle, 30% linear crop
Software:
DSS, XnView, StarNet++ v2, Star Tools v1.8
Extragalactic Cosmological Calculator v2
www.cloudynights.com/gallery/image/169610-extragalactic-c...
NGC 4618 ( PGC 42575 = IC 3667 = Arp 23)
Discovered (Apr 9, 1787) by William Herschel (and later listed as NGC 4618)
Discovered (Mar 21, 1903) by Max Wolf (and later listed as IC 3667)
An 11th-magnitude spiral galaxy (type SB(rs)m) in Canes Venatici (RA 12 41 33, Dec +41 09 04)
A member of an interacting pair (with NGC 4625, which see for a discussion of the results of that interaction), hence its use as an example of a one-armed spiral galaxy in the Arp Atlas. Its 545 km/sec recessional velocity is too small, in comparison to peculiar (non-Hubble-expansion) velocities, to provide a reliable distance estimate, but is in good agreement with a redshift-independent distance estimate of 25 million light years. Given that and its apparent size of 4.2 by 3.4 arcmin, NGC 4625 is about 30 thousand light years across.
"Excerpt courtesy of Courtney Seligman" cseligman.com/text/atlas/ngc46.htm#4618
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: ned.ipac.caltech.edu/level5/Arp/Figures/big_arp23.jpeg
ARP 140, NGC 274 and NGC 275 Interacting Galaxies, Cetus
In 1966, American astronomer Halton Arp published a catalog of 338 peculiar galaxies under the assumption that the distorted shapes were due to large galactic ejections. It was soon demonstrated that the majority of the objects are in fact interacting galaxies, deforming each other by tidal forces. Entry number 140 is an example of two such galaxies, NGC 274 and NGC 275 in the constellation of Cetus, which appear to be in the early stages of merging. NGC 274 is a lenticular galaxy discovered by William Herschel in 1785. Although NGC 275 is in the same field of view, and of nearly the same brightness and identical contrast index, there is no mention of it in any of his observation notes. It is not unlikely that he mistook the pair for a single object. NGC 275 was first identified as a separate galaxy by his son, John Herschel in 1828.
Distance measurements of extragalactic objects are essential in estimating their physical properties, and are usually based on the redshift for very distant objects. However, redshift is dependent on two velocity components. One is due to the expansion of space, and the second to the object's "peculiar velocity" through space relative to the observer. It is generally accepted that "redshift-independent distances" are more accurate for redshifts lower than 0.01. In the case of ARP 140, redshift-independent distances are questionable on several levels. As listed in the NED database, the number of measurements is statistically too low. The range of results is too large, and varies by several hundred percent between low and high values. Distance calculations are based on outdated Hubble parameter (Ho) values. And, mean distance estimates for the two galaxies place them very widely apart, though they convincingly appear to be interacting in close contact. For these reasons, galaxy properties in the attached chart are calculated on the basis of their redshift derived distances.
Using the redshift method, NGC 274 lies at a distance of 80.84 Mly, receding at 1,746 km/s. Its actual diameter is about 37,200 ly, and absolute magnitude -19.46. It is approximately one third in size and brightness as our Milky Way galaxy. SIMBAD database classifies it as E/S0, an intermediate between an elliptical and a lenticular galaxy, while the NED database describes it as SAB0(r) pec, which is an intermediate spiral with a ring and a peculiar morphology. On my low magnification image I can barely visualize a full oval ring once my attention is drawn to it. On close examination, a couple of delicate features are present which suggest gravitational interaction. One is slight eccentricity of the galaxy relative to its nucleus. Another one is the presence of three wispy stellar streamers between the two galaxies. These features are better appreciated on Halton Arp's negative, high contrast, embossed original image.
NGC 275 is classified as SB(rs)cd pec, indicating a loosely wound barred spiral galaxy with an incomplete ring and a peculiar morphology. Its redshift based distance is 80.57 Mly, recession velocity 1,740 km/s, actual diameter approximately 37,700 ly, absolute magnitude -19.28, and brightness about one quarter that of the Milky Way. Even at low magnification, this galaxy shows markedly disrupted spiral arms and numerous bright blue floccules of starburst activity. While few references describe ARP 140 as a widely separated line-of-sight pair, it might be difficult to explain away peculiar features in both galaxies consistent with close gravitational interaction.
The attached image also includes a very distant galaxy, LEDA 1026074, lying at a distance of 1.5 billion light years, which is about half the size and brightness of the Milky Way. The background is strewn with numerous remote galaxies marked with letter "G" on the annotated image. Unfortunately, they have neither measurable properties nor identifiers listed in SIMBAD and NED databases. Based on their angular size alone, they would lie at distances between 1.5 and 3 billion light years. Of course, many of them might be dwarf galaxies, in which case they would be much closer. Without redshift information, there is no way to know.
The most remote object is quasar (QSO) SDSS J005134.95-065841.7, which presents barely above the limiting magnitude. Its apparent magnitude is presently about 0.5 mag brighter than listed. Quasars commonly manifest short and long term variability depending on the matter available to them for accretion. Based on its redshift of 1.38400, it lies at a light travel distance (lookback time) of 9.1 billion light years, and is about 70 times brighter than our Galaxy. When the light we are now recording was emitted, the object was receding from our location at 210,080 km/s. In the present cosmological epoch, its "proper recession velocity" is 292,040 km/s - very nearly the speed of light. When its proper recession velocity becomes superluminal, it will have crossed the cosmic event horizon and, over the next 9 billion years, its light will forever fade away into the infrared and radio waves.
Image Details:
-Remote Takahashi TOA 150 x 1105 mm
-OSC 32 x 300 sec, 2x drizzle, 30% linear crop
Software:
DSS, XnView, StarNet++ v2, Star Tools v1.8
Extragalactic Cosmological Calculator v2
www.cloudynights.com/gallery/image/169610-extragalactic-c...
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