## Observing objects in the High Redshift Universe

Mathematical details will be left to ASTR 328....

### Cosmological Effects on brightness and size

When observing objects at high redshift, simple Euclidian geometry no longer works. We have to take into account the shape and expansion history of the universe, which various in different cosmologies, i.e., as a function of H0, OmegaM, and OmegaL. This means we have to know the cosmology to derive physical properties, or conversely, if we know physical properties we can infer the cosmological parameters.

So how do we measure luminosity, angular size, and surface brightness at cosmological distances? DON'T SIMPLY USE HUBBLE'S LAW!

Luminosity distance

Normally, flux = Luminosity/(4piD2). But what do we mean by D in curved space? Let's define a luminosity distance dL so that we can simply use the normal flux equation, and then work out what dL is in different cosmologies.

First, define a coordinate distance that depends on the scale factor R and the comoving distance r. The energy flux you get from an object at that position is:
• reduced because of normal inverse square law of light: f ~ L/4pi(Rr)2
• reduced again becase the photons are being redshift and therefore reduced in energy: f ~ 1/(1+z)
• reduced yet again because photons arrive more slowly due to cosmological time dilation: f ~ 1/(1+z)
Put them all together and note that we are observing at t=now, so R=1, and we get f ~ L/(4 pi r2 (1+z)2 ). So we can define dL = r(1+z), and solve for r as a function of z for different cosmological parameters.

For OmegaL=0 universes, dL is analytic in form, but for universes with arbitrary OmegaM and OmegaL, it is not. Need to do numerical integration.

But in all cosmologies, for z<<1 this can be done using simple Taylor expansions to get

r(z) ~ (cz/H0)(1-0.5*(1+q0)z)

so

dL(z) ~ (cz/H0)(1+0.5*(1-q0)z)

where q0 is the deceleration parameter (= 0.5*OmegaM - OmegaL), and note that as z --> 0, dL ~ r --> cz/H0, ie we recover Hubble's Law.

Then we just use dL in place of the usual d in the distance modulus equation (from Carroll and Ostlie):

Angular size distance

Normally, the angular size of an object is given by theta=size/distance (using the small angle approximation). Under cosmology, we write

theta = size/(Rr) and then note that R = 1/(1+z), so

theta = size(1+z)/r

If we define the angular size distance as dA=r/(1+z), then we can use

theta = size / dA

like usual. Defined this way, we have

dA = dL / (1+z)2

for any cosmology. From Carroll and Ostlie:

Surface brightness

Notice that things get fainter and fainter and high redshift, but their angular size behaves differently -- so surface bightness will change with redshift!

Since observed surface brightness is flux/(angular size)2, we can combine the two expressions above:

SB ~ f/theta2 ~ (L/size2)(1+z)-4

for any cosmology.

So surface brightness drops as redshift increases. At z=2, SB is down by 3-4 = 1/81 = 4.8 mag/arcsec2.

### Instrumental complications: observing in a fixed filter, bandshifting, and the K-correction

The above discussion about apparent brightnesses and the luminosity distance assumes you are detecting all the flux at all wavelengths -- i.e, measuring the bolometric flux. We never do this. We measure brightness over a range of wavelengths, ie through a filter. In terms of wavelengths, redshift both shifts and stretches light we see from distant objects. How does this complicate things?

1. Redshift changes the emitted wavelength we observe: lambdaobs = lambdaem(1+z)
2. Redshift changes the range of emitted wavelengths we observe. deltalambdaobs = deltalambdaem(1+z)
Example: observing a z=2 galaxy using the V filter:

 at z=0 at z=2 central wavelength (Angstroms) 5500 1833 bandpass (Angstroms) 1000 333

So when we observe high redshift objects, we are seeing them at intrinsically different (bluer) wavelengths. If you know the spectrum of an object you can correct for this, using a so-called "K-correction". If you don't know what the spectrum is, you have to guess or assume a K-correction.

Or, you can observe in redder (infrared) filters as you look at objects at higher reshift.

### Appearance of high redshift galaxies

Put cosmology and bandshifting together and what do you get? Consider the luminosity profile of a spiral galaxy:

### Galaxy Evolution

Finally, how would galaxy evolution change things -- what did today's spiral galaxies look like when they were young? What about giant elliptical galaxies like M87?