View source for Seminar 2. Viewing galaxies in 2D

* '''Title:''' Viewing Galaxies in 2D
* '''Subtitle:''' Spatially-resolved kinematics and stellar populations with IFS

== Spectroscopy ==
We have incoming light which passes through a slit and then a grating and splits it in different wavelengths. Then the detector detects the continuous electromagnetic spectrum.

* But if we put a cold glass before the slit, we will have an absorption spectrum.
* If we put a cold glass before the slit, we will have an emission spectrum.

What will happen if we point our telescope at a galaxy?

* We will have some emission lines in the spectra.

Now, this depends on the slit and how you place it. If you let a lot of points go through, you're getting information from a big region.

== Integral field spectroscopy ==
* Used first at 1789. But it wasn't until ~2000 that it was largely used.

@TODO: Fill

=== Integral field units ===
* Lenslet array
* Fibre array
* Image slicer
* Micro-slicer

Optimal performance: slicer (anyways, none of them is the best, each of them has advantages and disadvantages)

=== Uses of IFUs ===
* Earth remote sensing
* Weather forecasting
* Monitoring natural disasters and climate change

* Resolved stellar populations (stars, HII regions, planetary nebulae, galactic star formation)
* Extended objects (extragalactic): stellar and gas kinematics, stellar populations, gas content
* Crowded regions: distances of different galaxies at once; deblend AGN from hast galaxy emission
* Distant universe: properties of galaxies at z~2, lensed galaxies, measure many redshifts at once

=== Galaxy evolution with IFS ===

@Note: I stopped taking notes because the seminar was very interesting and I didn't have time to write everything down.