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Check out the huge version :) An optical follow-up of the SpARCS fields. Color images from the z,r and g-bands corresponding to the R, G and B channels. www.faculty.ucr.edu/~gillianw/SpARCS/
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
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.
Taken with my Pentax 67 with 200mm lens and Ilford HP5 Plus film. Scanned with my Plustek OpticFilm 120
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)
This image shows the Hubble Ultra Deep Field 2012, an improved version of the Hubble Ultra Deep Field image featuring additional observation time. The new data have revealed for the first time a population of distant galaxies at redshifts between 9 and 12, including the most distant object observed to date. These galaxies will require confirmation using spectroscopy by the forthcoming NASA/ESA/CSA James Webb Space Telescope before they are considered to be fully confirmed.
More information and download-options:
www.spacetelescope.org/images/heic1219b/
Credit:
NASA, ESA, R. Ellis (Caltech), and the HUDF 2012 Team
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/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.
#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/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:
NGC 5545 (UGC 9143, PGC 51023, VV 210a and others) – the oblong spiral. Redshift puts this one approximately 158 million light-years away in Bootes.
Luminance – 24x600s – 240 minutes – binned 1x1
RGB – 8x300s – 40 minutes each – binned 2x2
360 minutes total exposure – 6 hours
Imaged June 9th and 11th and July 6th, 2024 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.
#62. astrodeep200407 a g HUDF heic0611aa
Click on All Sizes button and select Original to see highest resolution image.
In the full HUDF view, saturating the colors reveals huge regions with very different overall colors -- this deserves research.
www.spacetelescope.org/images/html/zoomable/heic0611a.html Zoomable
The boxes are 3 arcsec wide, 100x100 pixels, with 0.03 arc-second per pixel. They are in order of apparent brightness, from 1 to 28.
The half-light galaxy diameters are about 1.6 kpc = 5220 Ly, as 1 kpc = 1000 parsecs = 3262 Ly. Our Milky Way galaxy is about 100,000 Ly wide.
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
www.flickr.com/photos/rmforall/1363979470/in/photostream/
Double click on photo and click on All Sizes button and select Original to see highest resolution image, as well as some smaller images.
www.spacetelescope.org/images/html/zoomable/heic0611a.html Zoomable
The boxes are 3 arcsec wide, 100x100 pixels, with 0.03 arc-second per pixel. They are in order of apparent brightness, from 1 to 28.
The HUDF is made of 0.03 arc-second pixels, 6200X6200, 186X186 arc-seconds, 3.1X3.1 arc-minutes, about a tenth of the width of the Moon or Sun, 0.5X0.5 degrees.
'In this image, blue and green correspond to colors that can be seen by the human eye, such as hot, young, blue stars and the glow of Sun-like stars in the disks of galaxies.
Red represents near-infrared light, which is invisible to the human eye, such as the red glow of dust-enshrouded galaxies.'
Four wavelength filters collected the B435, V606, i775, z850 wavelength images for the observed blue, violet, near infrared, infrared images -- combined in this vast image with tiny 0.03 arc-second pixels.
'Galaxy sizes: Typical i-dropouts at z850,AB about 27 (from the HUDF-Ps and HUDF) have PSF-corrected half-light radii of about 0.8 kpc [2610 Ly] or about 0.14 arc-second (Figure 6: §3.7). [ So diameter is 1.6 kpc = 5220 Ly, as 1 kpc = 1000 parsecs = 3262 Ly. Our Milky Way galaxy is about 100,000 Ly wide. ]'
'The reheating, driven by the galaxies ultraviolet starlight, transformed the gas between galaxies from a cold, dark hydrogen soup to a hot, transparent plasma over only a few hundred million years.
With Hubble's help, astronomers are now beginning to see the kinds of galaxies that brought about the reheating.'
'The first 900 million years (Myr) to redshift z about 6 (the first seven per cent of the age of the Universe) remains largely unexplored for the formation of galaxies.'
'It is not at all clear how galaxies built up from the first stars when the Universe was about 300Myr old (z about 12-15) to z about 6, just 600Myr later.'
'The nearest galaxies -- the larger, brighter, well-defined spirals and ellipticals -- thrived about 1 billion years ago, when the cosmos was 13 billion years old.'
'The image required 800 exposures taken over the course of 400 Hubble orbits around Earth. The total amount of exposure time was 11.3 days, taken between Sept. 24, 2003 and Jan. 16, 2004.'
www.spacetelescope.org/images/html/heic0611a.html
Probing the distant Universe for young galaxies
This Hubble Space Telescope image shows 28 of the brightest of 506 young galaxies that existed when the universe was less than 1 billion years old.
The galaxies were uncovered in a study of two of the most distant surveys of the cosmos, the Hubble Ultra Deep Field (HUDF), completed in 2004, and the Great Observatories Origins Deep Survey (GOODS), made in 2003.
Just a few years ago, astronomers had not spotted any galaxies that existed significantly less than 1 billion years after the Big Bang.
The galaxies spied in the HUDF and GOODS surveys are blue galaxies brimming with star birth.
The large image at left shows the Hubble Ultra Deep Field, taken by the Hubble telescope.
The numbers next to the small blue boxes correspond to close-up views of 28 of the newly found galaxies at right. [ arranged by apparent brightness from 1 to 28 ]
The galaxies in the postage-stamp size images appear red because of their tremendous distance from Earth. The blue light from their young stars took nearly 13 billion years to arrive at Earth. During the journey, the blue light was shifted to red light due to the expansion of space.
Credit: NASA, ESA, R. Bouwens and G. Illingworth (University of California, Santa Cruz, USA)
www.spacetelescope.org/news/html/heic0611.html
News Release -- heic0611: Hubble finds hundreds of young galaxies in the early Universe
21-Sep-2006: Astronomers analyzing two of the deepest views of the cosmos made with the NASA/ESA Hubble Space Telescope have uncovered a gold mine of galaxies, more than 500 that existed less than a billion years after the Big Bang.
These galaxies thrived when the cosmos was less than 7 percent of its present age of 13.7 billion years.
This sample represents the most comprehensive compilation of galaxies in the early Universe, researchers said.
The discovery is scientifically invaluable for understanding the origin of galaxies, considering that just a decade ago early galaxy formation was largely uncharted territory.
Astronomers had not seen even one galaxy that existed when the Universe was a billion years old, so finding 500 in a Hubble survey is a significant leap forward for cosmologists.
The galaxies unveiled by Hubble are smaller than today's giant galaxies and very bluish in colour, indicating they are ablaze with star birth.
The images appear red because of the galaxies' tremendous distance from Earth.
The blue light from their young stars took nearly 13 billion years to arrive at Earth.
During the journey, the blue light was shifted to red light due to the expansion of space.
'Finding so many of these dwarf galaxies, but so few bright ones, is evidence for galaxies building up from small pieces -- merging together as predicted by the hierarchical theory of galaxy formation,' said astronomer Rychard Bouwens of the University of California, Santa Cruz, USA who led the Hubble study.
Bouwens and his team spied these galaxies in an analysis of the Hubble Ultra Deep Field (HUDF), completed in 2004, and the Great Observatories Origins Deep Survey (GOODS), made in 2003.
The results were presented on August 17 at the 2006 General Assembly of the International Astronomical Union, and will be published in the November 20 issue of the Astrophysical Journal.
The findings also show that these dwarf galaxies were producing stars at a furious rate, about ten times faster than is happening now in nearby galaxies.
Astronomers have long debated whether the hottest stars in early star-forming galaxies, such as those in this study, may have provided enough radiation to reheat the cold hydrogen gas that existed between galaxies in the early Universe.
The gas had been cooling since the Big Bang.
'Seeing all of these starburst galaxies provides evidence that there were enough galaxies 1 billion years after the Big Bang to finish reheating the Universe,' explained team member Garth Illingworth of the University of California, Santa Cruz. 'It highlights a period of fundamental change in the Universe, and we are seeing the galaxy population that brought about that change.'
In terms of human lifetimes, cosmic events happen very slowly.
The evolution of galaxies and stars, for example, occurs over billions of years.
Astronomers, therefore, rarely witness dramatic, relatively brief transitions that changed the Universe.
One such event was the Universe is 'reheating'.
The reheating, driven by the galaxies ultraviolet starlight, transformed the gas between galaxies from a cold, dark hydrogen soup to a hot, transparent plasma over only a few hundred million years.
With Hubble's help, astronomers are now beginning to see the kinds of galaxies that brought about the reheating.
Just a few years ago, astronomers did not have the technology to hunt for faraway galaxies in large numbers.
The installation of the Advanced Camera for Surveys (ACS) aboard the Hubble Space Telescope in 2002 allowed astronomers to probe some of the deepest recesses of our Universe.
Astronomers used the ACS to observe distant galaxies in the HUDF and GOODS public surveys.
Another major step in the exploration of the Universe's earliest years will occur if Hubble undergoes its next upgrade with the Wide Field Planetary Camera 3 (WFC3).
The WFC3's infrared sensitivity will allow it to detect galaxies that are so far away their starlight has been stretched to infrared wavelengths by the expanding Universe.
The galaxies uncovered so far promise that many more galaxies at even greater distances are awaiting discovery by the NASA/ESA/CSA James Webb Space Telescope (JWST), scheduled to launch in 2013.
Co-author Marijn Franx, member of the ESA JWST NIRSPEC science team, explains: 'The JWST will be able to see even further back into the early Universe, and glimpse the first objects that formed.
ESA's NIRSPEC instrument, can even measure the exact distances of these objects.'
Notes for editors:
The Hubble Space Telescope is a project of international cooperation between ESA and NASA.
The members of the science team are Rychard Bouwens and Garth Illingworth (University of California, Santa Cruz),
John Blakeslee (Washington State University),
and Marijn Franx (Leiden University).
NASA, ESA, R. Bouwens and G. Illingworth (University of California, Santa Cruz, USA)
NASA's press release
Contacts:
Marijn Franx
Leiden Observatory, Leiden, the Netherlands
Tel: +31-71-5275870
E-mail: franx@strw.leidenuniv;
Rychard Bouwens
University of California, Santa Cruz, California, USA
Tel: +1-831-459-5276
E-mail: bouwens@ucolick.org;
Garth Illingworth
University of California, Santa Cruz, California, USA
Tel: +1-831-459-2843
E-mail: gdi@ucolick.org;
John Blakeslee
Washington State University, Pullman, Washington, USA
Tel: +1-509-335-2414
E-mail: jblakes@wsu.edu;
Lars Lindberg Christensen
Hubble/ESA, Garching, Germany
Tel: +49-89-3200-6306
Cellular: +49-173-3872-621
E-mail: lars@eso.org;
Donna Weaver
Space Telescope Science Institute, Baltimore, Md., USA
Tel: +1-410-338-4493
E-mail: dweaver@stsci.edu;
Copyright-free material (more info).
hubblesite.org/newscenter/archive/releases/2004/07/image/a/
Hubble Ultra Deep Field Image Reveals Galaxies GaloreSTScI-PRC2004-07a
Galaxies, galaxies everywhere -- as far as NASA's Hubble Space Telescope can see. This view of nearly 10,000 galaxies is the deepest visible-light image of the cosmos. Called the Hubble Ultra Deep Field, this galaxy-studded view represents a 'deep' core sample of the universe, cutting across billions of light-years.
The snapshot includes galaxies of various ages, sizes, shapes, and colors.
The smallest, reddest galaxies, about 100, may be among the most distant known, existing when the universe was just 800 million years old.
The nearest galaxies -- the larger, brighter, well-defined spirals and ellipticals -- thrived about 1 billion years ago, when the cosmos was 13 billion years old.
In vibrant contrast to the rich harvest of classic spiral and elliptical galaxies, there is a zoo of oddball galaxies littering the field.
Some look like toothpicks; others like links on a bracelet.
A few appear to be interacting.
These oddball galaxies chronicle a period when the universe was younger and more chaotic.
Order and structure were just beginning to emerge.
The Ultra Deep Field observations, taken by the Advanced Camera for Surveys, represent a narrow, deep view of the cosmos.
Peering into the Ultra Deep Field is like looking through an eight-foot-long soda straw.
In ground-based photographs, the patch of sky in which the galaxies reside (just one-tenth the diameter of the full Moon) is largely empty.
Located in the constellation Fornax, the region is so empty that only a handful of stars within the Milky Way galaxy can be seen in the image.
In this image, blue and green correspond to colors that can be seen by the human eye, such as hot, young, blue stars and the glow of Sun-like stars in the disks of galaxies.
Red represents near-infrared light, which is invisible to the human eye, such as the red glow of dust-enshrouded galaxies.
The image required 800 exposures taken over the course of 400 Hubble orbits around Earth. The total amount of exposure time was 11.3 days, taken between Sept. 24, 2003 and Jan. 16, 2004.
Object Names: Hubble Ultra Deep Field, HUDF
Image Type: Astronomical
Credit: NASA, ESA, S. Beckwith (STScI) and the HUDF Team
dipastro.pd.astro.it/venice06/oral/Bouwens_Venice06.ppt
RJB, GDI give 40 slide Power Point Import presentation in Venice 2006.03.31
arxiv.org/PS_cache/astro-ph/pdf/0509/0509641v6.pdf 36 page
Draft version February 4, 2008
Preprint typeset using LATEX style emulateapj v. 04/21/05
Galaxies at z about 6: the UV luminosity function and luminosity density from 506 HUDF, HUDF-PS, and GOODS i-dropouts
Rychard J. Bouwens 3, bouwens@ucolick.org;
Garth D. Illingworth 3, www.ucolick.org/~gdi/ gillingw@ucsc.edu;
John P. Blakeslee 4, jblakes@wsu.edu;
Marijn Franx 5 franx@strw.leidenuniv.nl;
1 Based on observations made with the NASA/ESA Hubble Space Telescope, which is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programs #9803.
2 Observations have been carried out using the Very Large Telescope at the European Southern Observatory (ESO) Paranal
Observatory under program ID: LP168.A-0485.
3 Astronomy Department, University of California, Santa Cruz, CA 95064
4 Department of Physics & Astronomy, Washington State University, Pullman, WA 99164-2814 and
5 Leiden Observatory, Postbus 9513, 2300 RA Leiden, Netherlands.
Draft version February 4, 2008
ABSTRACT [ z = redshift due to increasing distance and time from us here and now, where z = 0 ]
We have detected 506 i-dropouts (z about 6 -- galaxies) in deep, wide-area HST ACS fields: HUDF, enhanced GOODS, and HUDF-Parallel ACS fields (HUDF-Ps).
The contamination levels are under 8% (i.e., over 92% are at z about 6).
With these samples, we present the most comprehensive, quantitative analyses of z about 6 -- galaxies yet and provide optimal measures of the UV luminosity function (LF) and luminosity density at z about 6, and their evolution to z about 3.
We redetermine the size and color evolution from z about 6 to z about 3.
Field-to-field variations (cosmic variance), completeness, flux, and contamination corrections are modeled systematically and quantitatively.
After corrections, we derive a rest-frame continuum UV (about 1350 A) LF at z about 6 that extends to M1350,AB about −17.5 (0.04L*, z=3).
There is strong evidence for evolution of the LF between z about 6 and z about 3, most likely through a brightening (0.6+-0.2 mag) of M* (at 99.7% confidence) though the degree depends upon the faint-end slope.
As expected from hierarchical models, the most luminous galaxies are deficient at z about 6.
Density evolution (phi*) is ruled out at over 99.99% confidence.
Despite large changes in the LF, the luminosity density at z about 6 is similar (0.82 ± 0.21x) to that at z about 3.
Changes in the mean UV color of galaxies from z about 6 to z about 3 suggest an evolution in dust content, indicating the true evolution is substantially larger: at z about 6 the star formation rate density is just about 30% of the z about 3 value.
Our UV luminosity function is consistent with z about 6 galaxies providing the necessary UV flux to reionize the universe.
Subject headings: galaxies: evolution -- galaxies: high-redshift
2.1. ACS HUDF
The B435V606i775z850 [colors blue, violet, near infrared, infrared] images used for this analysis are the v1.0 reductions of the HUDF (Beckwith et al. 2006), binned on a 0.03′′ pixel scale.
3.2. i-dropouts in the HUDF
Applying the above selection criteria to the HUDF results in a sample of 122 i-dropouts.
Objects range in magnitude from z850,AB = 25.0 to 29.4 (the 8 d limit).
At z about 6, this corresponds to 0.04 - 2.2 times the characteristic rest-frame UV luminosity at z about 3 (Steidel et al. 1999).... V606i775z850 color cutouts are provided in Figure 1 for the brightest 28 i-dropouts from the HUDF.
Fig. 1. -- Postage stamps (V606i775z850 color images) of the brightest 28 i775-dropouts from the HUDF [ from the 122 galaxies found ].
Objects are ordered in terms of their z850-band magnitude. [infrared]
The z850-band magnitudes and object IDs are shown above and below each object, respectively.
Each postage stamp is 3.0′′ in size.
These high S/N images show definitive evidence for assymetries, mergers, and other interactions -- similar to that seen at lower redshifts (z about 2 - 5).
Galaxy sizes: Typical i-dropouts at z850,AB about 27 (from the HUDF-Ps and HUDF) have PSF-corrected half-light radii of about 0.8 kpc [2610 Ly] or about 0.14 arc-second (Figure 6: §3.7). [ So diameter is 1.6 kpc = 5220 Ly, as 1 kpc = 1000 parsecs = 3262 Ly. Our Milky Way galaxy is about 100,000 Ly wide. ]
www.ucolick.org/~gdi/docs/nature_05156.pdf 15 page
LETTERS
Vol 443, 14 September 2006 doi:10.1038/nature05156
Rapid evolution of the most luminous galaxies during the first 900 million years
Rychard J. Bouwens, Garth D. Illingworth
The first 900 million years (Myr) to redshift z about 6 (the first seven per cent of the age of the Universe) remains largely unexplored for the formation of galaxies.
Large samples of galaxies have been found at z about 6 (refs 1-4) but detections at earlier times are uncertain and unreliable.
It is not at all clear how galaxies built up from the first stars when the Universe was about 300Myr old (z about 12-15) to z about 6, just 600Myr later.
Here we report the results of a search for galaxies at z about 7-8, about 700Myr after the Big Bang, using the deepest near-infrared and optical images ever taken.
Under conservative selection criteria we find only one candidate galaxy at z about 7-8, where ten would be expected if there were no evolution in the galaxy population between z about 7-8 and z about 6.
Using less conservative criteria, there are four candidates, where 17 would be expected with no evolution.
This demonstrates that very luminous galaxies are quite rare 700Myr after the Big Bang.
The simplest explanation is that the Universe is just too young to have built up many luminous galaxies at z about 7-8 by the hierarchical merging of small galaxies.
____________________________________________________________
See similar images:
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
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/24eVAda
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 20.29° clockwise from up.
This Picture of the Week shows a huge cloud of gas around the distant quasar SDSS J102009.99+104002.7, taken by the Multi Unit Spectroscopic Explorer (MUSE) instrument on ESO’s Very Large Telescope (VLT) at the Paranal Observatory. Quasars are the luminous centres of active galaxies, which are kept active by material falling onto the central supermassive black hole. This quasar and its surrounding cloud are at a redshift larger than 3, meaning that they are seen as they were only about 2 billion years after the Big Bang.
More information: www.eso.org/public/images/potw1747a/
Credit:
ESO/Arrigoni Battaia et al.