<p>From <a href="https://arxiv.org/abs/1807.09287" rel="nofollow noreferrer">Martini et al. 2018</a>:</p>
<blockquote>
<p>The Dark Energy Spectroscopic Instrument (DESI) to measure the expansion history of the Universe using the Baryon Acoustic Oscillation technique. The spectra of 35 million galaxies and quasars over 14000 sqdeg is measured during the life of the experiment. A new prime focus corrector for the KPNO Mayall telescope delivers light to 5000 fiber optic positioners. The fibers in turn feed ten broad-band spectrographs.</p>
</blockquote>
<p>A large amount of images was recorded, from 1,000 to 3,000 depending on the spectrograph during the performance series phase, and about 23,000 in total. Not all these data have been analyzed, among them there is a lot of dark images.
Most images have been acquired for a specific purpose, but could be used later on for another. For instance this has proven useful to understand an issue found with the collimator coating.</p>

CC BY-SA 4.0
2021-07-30T16:32:19.693Z
But this answer doesn't address the question, which has been asked: "How the data collected during 5 year DESI operation will be analyzed with regards to finding out what dark energy really is?"
Alex
CC BY-SA 4.0
2021-07-30T16:03:06.583Z
2021-08-03T20:25:02.120Z
2021-08-03T20:25:02.120Z
Lariliss
<p>Please have a look at this forecast paper: <a href="https://arxiv.org/abs/1611.00036" rel="nofollow noreferrer">1611.00036</a>. I will cite some important figures.</p>
<p>There are two important observables in the large-scale structures: Baryon Acoustic Oscillations(<a href="https://en.wikipedia.org/wiki/Baryon_acoustic_oscillations" rel="nofollow noreferrer">BAO</a>) and Redshift-space Distortions(<a href="https://en.wikipedia.org/wiki/Redshift-space_distortions" rel="nofollow noreferrer">RSD</a>). BAO tells us the expansion history of the universe, so measuring BAO puts constraints on the equation of state(EoS) of dark energy.</p>
<p>For example, if the EoS is parameterized like <span class="math-container">$w=w_0+w_a(1-a)$</span>. DESI expects to see such a contour plot(<span class="math-container">$68\%$</span> limit) if the &quot;true&quot; value is <span class="math-container">$w_0=-1$</span> and <span class="math-container">$w_a=0$</span>:
<a href="https://i.sstatic.net/ClYJv.jpg" rel="nofollow noreferrer"><img src="https://i.sstatic.net/ClYJv.jpg" alt="eos of dark energy" /></a>
Here &quot;P&quot; means Planck prior and &quot;BB&quot; means the case when board band information (the shape of measured density power spectrum) is used. Blue line is previous result obtained by <a href="https://en.wikipedia.org/wiki/Sloan_Digital_Sky_Survey#Baryon_Oscillation_Spectroscopic_Survey_(BOSS)" rel="nofollow noreferrer">BOSS project</a>, so we see huge improvements.</p>
<p>Similarly, RSD tells us how structures are clustered and grow, while different gravity theories predict different growth rate. Therefore DESI will give stronger constraints on gravity theory (modified gravity is an alternative explanation of the acceleration of the universe):
<a href="https://i.sstatic.net/xKvai.jpg" rel="nofollow noreferrer"><img src="https://i.sstatic.net/xKvai.jpg" alt="growth rate" /></a></p>
<p>And of course DESI will have better measurement of the total amount of dark energy:
<a href="https://i.sstatic.net/QfCW6.jpg" rel="nofollow noreferrer"><img src="https://i.sstatic.net/QfCW6.jpg" alt="total amount of DE" /></a></p>
<p>update:</p>
<p>It is a long story from raw data to cosmological parameters, but the procedure can be briefly but not precisely summarized:</p>
<p>The raw data is the positions (RA, DEC, redshift) of many galaxies/quasars. These positions will be transformed into statistics, e.g. power spectrum and correlation function.</p>
<p>And then people adopt one kind of parameterization/model to establish the likelihood <span class="math-container">$\mathcal{L}(d|\boldsymbol{\theta})$</span>, here <span class="math-container">$d$</span> means data and <span class="math-container">$\boldsymbol{\theta}$</span> means parameters.</p>
<p>With the aid of Bayes theorem <span class="math-container">$p(\boldsymbol{\theta}|d)\propto\mathcal{L}(d|\boldsymbol{\theta})p_{\mathrm{prior}}(\boldsymbol{\theta})$</span>, we will obtain the constraints/measurements on these parameters.</p>

CC BY-SA 4.0
2021-08-08T18:23:11.247Z
I think this answer could be improved if you addressed the question of how one goes from the DESI data to the cosmological parameters you discuss. (E.g., how will the DESI data produce "a better measurement of the total amount of dark energy"?)
Peter Erwin
CC BY-SA 4.0
2021-08-08T18:25:13.053Z
Thanks for answering, but isn't what you have cited, still relates to studying the effects of the dark energy, rather then addresses the question what are the internals of the dark energy?
Alex
CC BY-SA 4.0
2021-08-09T04:26:10.750Z
@Alex We can only observe the effects of dark energy. There are many theories aiming to explain what dark energy is. It maybe scalar field, modified gravity and etc. Better measurement, e.g. DESI, provides more precise information of the properties of dark energy to help us understand it. Some theories will be excluded and some will survive.
R.Y. Zhao
CC BY-SA 4.0
2021-08-08T17:34:30.817Z
2021-08-09T05:01:20.127Z
2021-08-09T05:01:20.127Z
R.Y. Zhao
<p>Dark Energy Spectroscopic Instrument, or DESI at the end of it's 5 years operation will create the largest 3-D spectroscopic map of the universe.</p>
<p>How the data collected during 5 year DESI operation will be analyzed with regards to finding out what dark energy really is?</p>
<hr />
<ul>
<li><a href="https://www.desi.lbl.gov/" rel="nofollow noreferrer">https://www.desi.lbl.gov/</a></li>
<li><a href="https://en.wikipedia.org/wiki/Dark_Energy_Spectroscopic_Instrument" rel="nofollow noreferrer">https://en.wikipedia.org/wiki/Dark_Energy_Spectroscopic_Instrument</a></li>
</ul>

CC BY-SA 4.0
2021-08-03T21:31:49.380Z
I suspect the best we can hope for is to understand what dark energy does, rather than to understand what it is.
James K
CC BY-SA 4.0
2021-08-03T23:52:26.660Z
@James K So dark energy is what it is :-)
Alex
<observational-astronomy><data-analysis><dark-energy>
How the data collected during 5 year DESI operation will be analyzed with regards to finding what dark energy really is?
Alex
# How the data collected during 5 year DESI operation will be analyzed with regards to finding what dark energy really is?

(Asked by: username_0 on 2021-07-28)

Dark Energy Spectroscopic Instrument, or DESI at the end of it's 5 years operation will create the largest 3-D spectroscopic map of the universe.

How the data collected during 5 year DESI operation will be analyzed with regards to finding out what dark energy really is?

---

* <https://www.desi.lbl.gov/>
* <https://en.wikipedia.org/wiki/Dark_Energy_Spectroscopic_Instrument>

**Tags:** observational-astronomy, data-analysis, dark-energy
> **Comments:**
> **username_1**: I suspect the best we can hope for is to understand what dark energy does, rather than to understand what it is.  
> **username_0**: @James K So dark energy is what it is :-)  

---

## 2 answers

### Answer by username_2 on 2021-07-30. Score: 0 | Accepted answer

From [Martini et al. 2018](https://arxiv.org/abs/1807.09287):

> The Dark Energy Spectroscopic Instrument (DESI) to measure the expansion history of the Universe using the Baryon Acoustic Oscillation technique. The spectra of 35 million galaxies and quasars over 14000 sqdeg is measured during the life of the experiment. A new prime focus corrector for the KPNO Mayall telescope delivers light to 5000 fiber optic positioners. The fibers in turn feed ten broad-band spectrographs.

A large amount of images was recorded, from 1,000 to 3,000 depending on the spectrograph during the performance series phase, and about 23,000 in total. Not all these data have been analyzed, among them there is a lot of dark images.
Most images have been acquired for a specific purpose, but could be used later on for another. For instance this has proven useful to understand an issue found with the collimator coating.

> **Comments:**
> **username_0**: But this answer doesn't address the question, which has been asked: "How the data collected during 5 year DESI operation will be analyzed with regards to finding out what dark energy really is?"  

---

### Answer by username_3 on 2021-08-08. Score: 1

Please have a look at this forecast paper: [1611.00036](https://arxiv.org/abs/1611.00036). I will cite some important figures.

There are two important observables in the large-scale structures: Baryon Acoustic Oscillations([BAO](https://en.wikipedia.org/wiki/Baryon_acoustic_oscillations)) and Redshift-space Distortions([RSD](https://en.wikipedia.org/wiki/Redshift-space_distortions)). BAO tells us the expansion history of the universe, so measuring BAO puts constraints on the equation of state(EoS) of dark energy.

For example, if the EoS is parameterized like $w=w\_0+w\_a(1-a)$. DESI expects to see such a contour plot($68\%$ limit) if the "true" value is $w\_0=-1$ and $w\_a=0$:
[![eos of dark energy](https://i.sstatic.net/ClYJv.jpg)](https://i.sstatic.net/ClYJv.jpg)
Here "P" means Planck prior and "BB" means the case when board band information (the shape of measured density power spectrum) is used. Blue line is previous result obtained by [BOSS project](https://en.wikipedia.org/wiki/Sloan_Digital_Sky_Survey#Baryon_Oscillation_Spectroscopic_Survey_(BOSS)), so we see huge improvements.

Similarly, RSD tells us how structures are clustered and grow, while different gravity theories predict different growth rate. Therefore DESI will give stronger constraints on gravity theory (modified gravity is an alternative explanation of the acceleration of the universe):
[![growth rate](https://i.sstatic.net/xKvai.jpg)](https://i.sstatic.net/xKvai.jpg)

And of course DESI will have better measurement of the total amount of dark energy:
[![total amount of DE](https://i.sstatic.net/QfCW6.jpg)](https://i.sstatic.net/QfCW6.jpg)

update:

It is a long story from raw data to cosmological parameters, but the procedure can be briefly but not precisely summarized:

The raw data is the positions (RA, DEC, redshift) of many galaxies/quasars. These positions will be transformed into statistics, e.g. power spectrum and correlation function.

And then people adopt one kind of parameterization/model to establish the likelihood $\mathcal{L}(d|\boldsymbol{\theta})$, here $d$ means data and $\boldsymbol{\theta}$ means parameters.

With the aid of Bayes theorem $p(\boldsymbol{\theta}|d)\propto\mathcal{L}(d|\boldsymbol{\theta})p\_{\mathrm{prior}}(\boldsymbol{\theta})$, we will obtain the constraints/measurements on these parameters.

> **Comments:**
> **username_4**: I think this answer could be improved if you addressed the question of how one goes from the DESI data to the cosmological parameters you discuss. (E.g., how will the DESI data produce "a better measurement of the total amount of dark energy"?)  
> **username_0**: Thanks for answering, but isn't what you have cited, still relates to studying the effects of the dark energy, rather then addresses the question what are the internals of the dark energy?  
> **username_3**: @Alex We can only observe the effects of dark energy. There are many theories aiming to explain what dark energy is. It maybe scalar field, modified gravity and etc. Better measurement, e.g. DESI, provides more precise information of the properties of dark energy to help us understand it. Some theories will be excluded and some will survive.  

---

