Planck satellite unveils the Universe -- now and then (w/ Video)

Jul 05, 2010
This multi-frequency all-sky image of the microwave sky has been composed using data from Planck covering the electromagnetic spectrum from 30 GHz to 857 GHz. Credits: ESA/ LFI & HFI Consortia

(PhysOrg.com) -- ESA's Planck mission has delivered its first all-sky image. It not only provides new insight into the way stars and galaxies form but also tells us how the Universe itself came to life after the Big Bang.

“This is the moment that Planck was conceived for,” says ESA Director of Science and , David Southwood. “We’re not giving the answer. We are opening the door to an Eldorado where scientists can seek the nuggets that will lead to deeper understanding of how our Universe came to be and how it works now. The image itself and its remarkable quality is a tribute to the engineers who built and have operated Planck. Now the scientific harvest must begin.”

From the closest portions of the Milky Way to the furthest reaches of space and time, the new all-sky Planck image is an extraordinary treasure chest of new data for astronomers.

The main disc of our Galaxy runs across the centre of the image. Immediately striking are the streamers of cold dust reaching above and below the Milky Way. This galactic web is where are being formed, and Planck has found many locations where individual stars are edging toward birth or just beginning their cycle of development.

Less spectacular but perhaps more intriguing is the mottled backdrop at the top and bottom. This is the ‘’ (CMBR). It is the oldest light in the Universe, the remains of the fireball out of which our Universe sprang into existence 13.7 billion years ago.

This video is not supported by your browser at this time.
Credits: ESA, C. Carreau

While the Milky Way shows us what the local Universe looks like now, those microwaves show us what the Universe looked like close to its time of creation, before there were stars or galaxies. Here we come to the heart of Planck’s mission to decode what happened in that primordial Universe from the pattern of the mottled backdrop.

The microwave pattern is the cosmic blueprint from which today’s clusters and superclusters of galaxies were built. The different colours represent minute differences in the temperature and density of matter across the sky. Somehow these small irregularities evolved into denser regions that became the galaxies of today.

The CMBR covers the entire sky but most of it is hidden in this image by the ’s emission, which must be digitally removed from the final data in order to see the microwave background in its entirety.

When this work is completed, Planck will show us the most precise picture of the microwave background ever obtained. The big question will be whether the data will reveal the cosmic signature of the primordial period called inflation. This era is postulated to have taken place just after the and resulted in the Universe expanding enormously in size over an extremely short period.

Credits: ESA/ LFI & HFI Consortia

Planck continues to map the . By the end of its mission in 2012, it will have completed four all-sky scans. The first full data release of the CMBR is planned for 2012. Before then, the catalogue containing individual objects in our Galaxy and whole distant galaxies will be released in January 2011.

“This image is just a glimpse of what Planck will ultimately see,” says Jan Tauber, ESA’s Planck Project Scientist.

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omatumr
1.4 / 5 (10) Jul 05, 2010
If CMBR represents a primordial event, then the data may "reveal the cosmic signature of the primordial period called inflation."

There is evidence even now of great inflation on the atomic scale, as nuclear matter dissociates in the compact cores of stars and galaxies because of neutron repulsion:

a.) Neutron star =(neutron emission)=> Free neutron

b.) Neutron =(neutron decay)=> H+ + e-

In this last step, the atomic volume increases by a factor of 1,000,000,000,000,000 = Volume(H atom)/Volume(Neutron)

Expansion may not have been limited to the period after the hypothetical Big Bang.

See: Physics of Atomic Nuclei 69 (2006) 1847-1856.

With kind regards,
Oliver K. Manuel
shavera
5 / 5 (8) Jul 05, 2010
if a neutron decays into a proton and an electron, those particles MUST be emitted back to back to conserve momentum (in the neutron's rest frame). If those particles are back to back then they can't form a hydrogen atom.

Furthermore, you're mistaken as to what inflation means. Inflation increases the scale of measurement in our universe, not the volume of stuff inside it. If your argument was correct, we could count the expansion of ice cubes as inflation. (Volume(Ice)/Volume(water)).
omatumr
1.4 / 5 (11) Jul 05, 2010
Sorry, shavera, I should have been more specific:

A free neutron spontaneously decays into a proton, and electron and an anti-neutrino in about 10 minutes with the release of 0.782 MeV of energy.

The volume increases by 1,000,000,000,000,000 in this decay.

With kind regards,
Oliver K. Manuel

daywalk3r
3.8 / 5 (16) Jul 06, 2010
A free neutron spontaneously decays into a proton, and electron and an anti-neutrino in about 10 minutes with the release of 0.782 MeV of energy.

The volume increases by 1,000,000,000,000,000 in this decay.
So I wonder..

When I take a tennis ball out of my pocket, bind a 2 metre long rope to it, grab the loose end of the rope and start to swing it wildly around me in a random manner..

Does my effective volume increase to 4/3*pi*2m^3 just by doing this?

Though I can see your point - but it is somewhat hard to spot a direct analogy with the expansion of (the visible part of) the Universe.
omatumr
1 / 5 (4) Jul 06, 2010
"Does my effective volume increase to 4/3*pi*2m^3 just by doing this?"

Yes.

The volume that excludes the presence of another object becomes 4/3*pi*2m^3.

With kind regards,
Oliver K. Manuel
omatumr
1 / 5 (4) Jul 06, 2010
The product from step b.) above

Neutron =(neutron decay)=> H+ + e-

Where, the volume suddenly increases by a factor of 1,000,000,000,000,000 = Volume(H atom)/Volume(Neutron)

Departs in the solar wind (or stellar wind) of stars to fill interstellar space with Hydrogen.

Thus, stars are evaporating to fill interstellar space. That is an expansion.

Hydrogen is a waste product emitted from the stellar engines. It is not the fuel.

With kind regards,
Oliver K. Manuel

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