Looking back seems strange to me and that if one is to take such a position then evidence must exist in this very moment?
This may seem like a stupid question to some, but for me it is really about looking at where I exist in the universe and what exists right next to us in the same space. I am not sure if that makes any sense but hopefully somebody out there can help me focus better.
The mission's main goal is to study the cosmic microwave background –
the relic radiation left over from the Big Bang – across the whole sky
at greater sensitivity and resolution than ever before.
The cosmic microwave background (CMB) is the furthest back in time we can explore using light.
The cosmic microwave background (CMB) is detected in all directions of
the sky and appears to microwave telescopes as an almost uniform
background. Planck’s predecessors (NASA's COBE and WMAP missions) measured the temperature of the CMB to be 2.726 Kelvin (approximately -270 degrees Celsius) almost everywhere on the sky.
So with parsing some of these points from the link associated above with picture, I am not sure if my question has been properly asked.
A discussion about the definition of nothing.
For me then too, I would always wonder about "what nothing is" as that to relates to the question about what can exist right next to me. It was meant to be logical and not metaphysical question, so as to be reduced
to those first moments.
***
If BICEP2′s recent result is correct:
” -as big as a large fraction of a percent of the Planck
temperature (where the universe would have been hot enough to make black
holes just from its own heat) or
– as small as the temperature corresponding to about the energy of
the Large Hadron Collider (where it would barely have been hot enough
to make Higgs particles)”
History of the Universe-
“not of the whole universe but rather just the part of the universe
(called, on this website, “the observable patch of the universe“) that
we can observe today,”
Why is this “observable patch” important and where in the CMB map is
this located? As strange a question as this might be, can this
“observable patch” be right next to us?
So I am constructing a method here to help us see the universe as if I am on a location within this CMB map.
"The cosmic microwave background (CMB) is detected in all directions of the sky and appears to microwave telescopes as an almost uniform background. " -See: ESA and Planck Collaboration
So of course you look at the map, and for me, I wonder where we are located on that map. So with regard to that particular patch what does the background look like?-
"The contents point to a Euclidean flat geometry, with curvature (\Omega_{k}) of −0.0027+0.0039 −0.0038. The WMAP measurements also support the cosmic inflation paradigm in several ways, including the flatness measurement."- WMAP
So such a illustration and my question about our location and where we are in that "all sky map(CoBE, WMAP, and PLanck)" tells us something about the region we are in? Right next to us, in this map while seeking our placement, I am curious as to what this region looks like in relation to say another point on that map.
Cosmological parameters from 2013 Planck results[23][24][25]
Parameter |
Age of the universe (Gy) |
Hubble's constant
( km⁄Mpc·s ) |
Physical baryon density |
Physical cold dark matter density |
Dark energy density |
Density fluctuations at 8h−1 Mpc |
Scalar spectral index |
Reionization optical depth |
Symbol |
|
|
|
|
|
|
|
|
Planck
Best fit |
13.819 |
67.11 |
0.022068 |
0.12029 |
0.6825 |
0.8344 |
0.9624 |
0.0925 |
Planck
68% limits |
13.813±0.058 |
67.4±1.4 |
0.02207±0.00033 |
0.1196±0.0031 |
0.686±0.020 |
0.834±0.027 |
0.9616±0.0094 |
0.097±0.038 |
Planck+lensing
Best fit |
13.784 |
68.14 |
0.022242 |
0.11805 |
0.6964 |
0.8285 |
0.9675 |
0.0949 |
Planck+lensing
68% limits |
13.796±0.058 |
67.9±1.5 |
0.02217±0.00033 |
0.1186±0.0031 |
0.693±0.019 |
0.823±0.018 |
0.9635±0.0094 |
0.089±0.032 |
Planck+WP
Best fit |
13.8242 |
67.04 |
0.022032 |
0.12038 |
0.6817 |
0.8347 |
0.9619 |
0.0925 |
Planck+WP
68% limits |
13.817±0.048 |
67.3±1.2 |
0.02205±0.00028 |
0.1199±0.0027 |
0.685+0.018
−0.016 |
0.829±0.012 |
0.9603±0.0073 |
0.089+0.012
−0.014 |
Planck+WP
+HighL
Best fit |
13.8170 |
67.15 |
0.022069 |
0.12025 |
0.6830 |
0.8322 |
0.9582 |
0.0927 |
Planck+WP
+HighL
68% limits |
13.813±0.047 |
67.3±1.2 |
0.02207±0.00027 |
0.1198±0.0026 |
0.685+0.017
−0.016 |
0.828±0.012 |
0.9585±0.0070 |
0.091+0.013
−0.014 |
Planck+lensing
+WP+highL
Best fit |
13.7914 |
67.94 |
0.022199 |
0.11847 |
0.6939 |
0.8271 |
0.9624 |
0.0943 |
Planck+lensing
+WP+highL
68% limits |
13.794±0.044 |
67.9±1.0 |
0.02218±0.00026 |
0.1186±0.0022 |
0.693±0.013 |
0.8233±0.0097 |
0.9614±0.0063 |
0.090+0.013
−0.014 |
Planck+WP
+highL+BAO
Best fit |
13.7965 |
67.77 |
0.022161 |
0.11889 |
0.6914 |
0.8288 |
0.9611 |
0.0952 |
Planck+WP
+highL+BAO
68% limits |
13.798±0.037 |
67.80±0.77 |
0.02214±0.00024 |
0.1187±0.0017 |
0.692±0.010 |
0.826±0.012 |
0.9608±0.0054 |
0.092±0.013 |
So as we look at this map much is told to us about the Cosmological Parameters and what can be defined in this location we occupy.
Parameter |
Value |
Description |
Ωtot |
|
Total density |
w |
|
Equation of state of dark energy |
r |
, k0 = 0.002Mpc−1 (2σ) |
Tensor-to-scalar ratio |
d ns / d ln k |
, k0 = 0.002Mpc−1 |
Running of the spectral index |
Ωvh2 |
|
Physical neutrino density |
Σmν |
eV (2σ) |
Sum of three neutrino masses |
See:
***
See Also: