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--- courses:ast403:redshift-surveys [2026/04/06 10:23] – [DESI BAO Survey] shuvo
+++ courses:ast403:redshift-surveys [2026/04/06 22:27] (current) – [DESI BAO Survey] shuvo
@@ Line 52: / Line 52: @@
 For graduate students studying large-scale structure, understanding the progression of SDSS is crucial, as its distinct phases introduced new observational techniques and targeted different cosmic epochs.
+About SDSS: https://www.youtube.com/watch?v=UD6cOMpJlZU
 **The First Detection: SDSS-I and II (2000–2008):**
@@ Line 111: / Line 113: @@
 These automated micromotors can reconfigure the arrangement of the 5,000 fibers in a matter of minutes, aligning them with new target galaxies to an accuracy of a few microns. The light from these fibers is fed into ten spectrographs, each split into three spectral bands (blue, red, and near-infrared). This allows DESI to capture the spectra of 5,000 targets simultaneously, enabling it to map tens of millions of galaxies in just five years.
+DESI focal plane: https://www.youtube.com/watch?v=g1LVMox0KNc&t=50s
 **The Tracers: A Multi-Target Strategy:**\\
@@ Line 141: / Line 145: @@
 $$w(a) = w_0 + w_a (1 - a)$$
-Here:
+Here:\\
-* $w_0$ is the current value of the dark energy equation of state at $z = 0$.
+* $w_0$ is the current value of the dark energy equation of state at $z = 0$.\\
-* $w_a$ dictates how quickly $w$ evolves with time.
+* $w_a$ dictates how quickly $w$ evolves with time.\\
-* *(Note: $\Lambda$CDM strictly requires $w_0 = -1$ and $w_a = 0$)*.
+* (Note: $\Lambda$CDM strictly requires $w_0 = -1$ and $w_a = 0$).\\
 When the DESI collaboration combined their Y1 BAO measurements with CMB data and Type Ia Supernova data, the statistical fit preferred a parameter space where **$w_0 > -1$ and $w_a < 0$**.