###
Max Tegmark's cosmology library: 2dF

We've done an independent analysis of the the
2dF galaxy redshift survey.
Below you can get the
power spectra,
survey mask,
and
uniform galaxy sample
described in the paper as well as some software,
as a starting point for your own analysis.
*Figure 26: Our 2dFGRS power spectrum measurements
compared with theoretical models.
*
The astro-ph version,
has low-res figures (1 and 6)
because of the size limit, so please
click here to download
a PDF file with the final MNRAS
published version of the paper.
Click
if you are interested in other research of mine.

##
The power spectrum of galaxies in the 2dF 100k redshift survey

###
Authors:

Max Tegmark,
Andrew Hamilton &
Yongzhong Xu
### Abstract:

We compute the real-space power spectrum and the redshift-space distortions of
galaxies in the 2dF 100k galaxy redshift survey using pseudo-Karhunen-Loeve
eigenmodes and the stochastic bias formalism. Our results agree well with those
published by the 2dFGRS team, and have the added advantage of producing
easy-to-interpret uncorrelated minimum-variance measurements of the
galaxy-galaxy, galaxy-velocity and velocity-velocity power spectra in 27
k-bands, with narrow and well-behaved window functions in the range 0.01h/Mpc <
k < 0.8h/Mpc. We find no significant detection of baryonic wiggles, although
our results are consistent with a standard flat Omega_Lambda=0.7
``concordance'' model and previous tantalizing hints of baryonic oscillations.
We measure the galaxy-matter correlation coefficient r > 0.4 and the
redshift-distortion parameter beta=0.49+/-0.16 for r=1 (beta=0.47+/- 0.16
without finger-of-god compression). Since this is an apparent-magnitude limited
sample, luminosity-dependent bias may cause a slight red-tilt in the power
spectum. A battery of systematic error tests indicate that the survey is not
only impressive in size, but also unusually clean, free of systematic errors at
the level to which our tests are sensitive. Our measurements and window
functions are available at http://www.hep.upenn.edu/~max/2df.html together with
the survey mask, radial selection function and uniform subsample of the survey
that we have constructed.
### Reference info:

astro-ph/0111575,
*MNRAS*, **335**, 887-908
### Power spectrum

If you simply want to plot up the 13 band powers shown above
for a chi-by-eye analysis or the like, use
this table (from Figure 26 in the paper).
The 5 columns are (k_eff,k_low,k_high,P,dP).
If you want to do a quantitative analysis comparing to models, then
use this table instead, which contains
the 27 points from Figure 17 without unneccesary binning.
The corresponding 27 window functions are the rows of
this file.
To compute chi2 as in the paper, evaluate *p_i = P(k_i)*,
where *P(k)* is your own model power spectrum and
*k_i* are the 49 k-values from
this file.
Then compute

*chi2 = sum_i [P_i-(Wp)_i]^2/dP_i^2,*

where P_i and dP_i are the measurements and error bars you loaded above
and W is the 27 x 49 window matrix.
Note that if you want the window functions to look like
in Figure 11 of the paper, which shows windows on the
*relative* power (power relative to the prior),
you need to multiply each window by the prior power spectrum we used,
available in this file - the columns give (k,P).
The resulting 27 window functions are plotted here,
normalized to unit area.
### Uniform galaxy sample

You'll find the uniform galaxy sample described in the paper in
this file.
The 5 columns are (ra,dec,cz,b_j,eta_type).
If you'd like a file with additional fields, say the 2dFGRS team ID numbers,
just let me know and I'll be happy to send it.
This sample is strictly magnitude limited at b_j=19.27, so it's
very easy to interpret and work with.
Our fit for its radial selection function nbar(r) is in
this file, where the columns
are (r,nbar) and r is comoving distance.
It's only valid for 10-650 Mpc/h.
The only additional thing you need before you run off and compute
your own power spectrum, trispectrum, genus curve or whatever
is the angular mask below.

### Angular mask

As the cutout to the left illustrates, the angular mask is pretty complicated.
As described in the paper, it consists of 3614 spherical polygons.
All the info you need is in this file.
To help you along, I've put some demo software in
tarball.tar.gz - the easiest way
to figure out how it works is probably to run
the enclosed code completeness_demo.f.
If you have questions, please don't hesitate to ask.

If you'd like additional stuff that you can't find here, please drop me
an email! And, needless to say, don't forget to visit the
site of the
2dF galaxy redshift survey
itself - it's terrific that the 2dFGRS team has made their data public, thereby
making analyses like ours possible.

Return to my home page

This page was last modified October 7, 2002.
max@physics.upenn.edu