Max Tegmark's SDSS page  download power spectra, windows etc. here
Together with my fellow members of the
Sloan Digital Sky Survey
(SDSS)
largescale structure working group, I've had lots of fun thinking about
ways to test, validate and analyze galaxy clustering data since 1996.
I'll keep updating this page with publications and
downloadable data products that I've worked on as they become available.
Cosmological Constraints from the SDSS Luminous Red Galaxies
This packages up the largescale clustering information from the SDSS LRGs as a useful starting point for cosmological model fitting.
These SDSS luminous red galaxies are a great cosmological probe,
providing much smaller error bars on large scales than
any other currently available galaxy sample, including the
main sample galaxies discussed further down on this page.
Figure 22:
Measured power spectra for the LRG and main galaxy samples.
The solid curves correspond to
the linear theory LCDM fits to WMAP3 alone
normalized to galaxy bias b=1.9 (top) and b=1.1 (bottom)
relative to the z=0 matter power.
The dashed curves include the nonlinear correction of Cole et al (2005) for A=1.4,
with Q=30 for the LRGs and Q=4.6 for the main galaxies.
The onset of nonlinear corrections is clearly visible for k>0.09 h/Mpc (vertical line).
Click here to download a PDF version of the paper.
The measurements and their window functions are further down on this page.
Downloadable P(k) data and software
 Monte Carlo Markov Chains:
here.
The 15 columns in each file contain
(step, exp(2*tau), Theta_s, Omega_Lambda, omega_d, omega_b, omega_nu, n_s, 1+n_t, A_s, r, b, w, Q_nl, lnL)
as defined by Table 2 of astroph/0608632.
Files mentioning "lrg" are WMAP+LRG, the rest are WMAPonly.
If you'd like me to post additional chains, or ones including all the dependent parameters in Table 2, please let me know.
 Measurements and error bars from Table 1 in the paper:
sdss_lrg_measurements.txt
 Window functions:
sdss_lrg_windows.txt
 kbands at which window functions are defined:
sdss_lrg_kbands.txt
 Sample f77 code that computes SDSS LRG likelihood given some P(k) model:
compute_lrg_likelihood.f,
lrg_likelihood_common.f
 All of the above combined into a single gzipped tar file:
lrg_likelihood_code.tar.gz
This code is described in Appendix A.4 of the paper.
If you're a CosmoMC user, you'll be pleased to know that the guts of this code have already been converted to a CosmoMC plugin
by Anthony Lewis, Hiranya Peiris and Licia Verde, and is available
here.
Slides for a talk?
Here's a tarball with ps and gif images of all the figures
in the LRG+WMAP3 paper.
If you type "xv *.gif" after unpacking it, hitting "[TAB]" will overlay the constraints
one by one.
Here's the same plots in
in the powerpoint.
Authors:
Max Tegmark, Daniel Eisenstein, Michael Strauss, David Weinberg, Michael Blanton, Joshua Frieman,
Masataka Fukugita, James Gunn, Andrew Hamilton, Gillian Knapp, Robert Nichol, Jeremiah Ostriker,
Nikhil Padmanabhan, Will Percival, David Schlegel, Donald Schneider, Roman Scoccimarro, Uros Seljak,
HeeJong Seo, Molly Swanson, Alexander Szalay, Michael Vogeley, Jaiyul Yoo, Idit Zehavi, Kevork
Abazajian, Scott Anderson, James Annis, Neta Bahcall, Bruce Bassett, Andreas Berlind, Jon Brinkmann,
Tamas Budavari, Francisco Castander, Andrew Connolly, Istvan Csabai, Mamoru Doi, Douglas Finkbeiner,
Bruce Gillespie, Karl Glazebrook, Gregory Hennessy, David Hogg, Zeljko Ivezic, Bhuvnesh Jain, David
Johnston, Stephen Kent, Donald Lamb, Brian Lee, Huan Lin, Jon Loveday, Robert Lupton, Jeffrey Munn,
Kaike Pan, Changbom Park, John Peoples, Jeffrey Pier, Adrian Pope, Michael Richmond, Constance
Rockosi, Ryan Scranton, Ravi Sheth, Albert Stebbins, Christopher Stoughton, Istvan Szapudi, Douglas
Tucker, Daniel Vanden Berk, Brian Yanny, Donald York
Abstract:
We measure the largescale realspace power spectrum P(k) using luminous red galaxies
(LRGs) in the Sloan Digital Sky Survey (SDSS) and use this measurement to sharpen
constraints on cosmological parameters from the Wilkinson Microwave Anisotropy Probe (WMAP).
We employ a matrixbased power spectrum estimation method using PseudoKarhunenLoeve
eigenmodes, producing uncorrelated minimumvariance measurements in 20 kbands of both the
clustering power and its anisotropy due to redshiftspace distortions, with narrow and
wellbehaved window functions in the range 0.01h/Mpc < k < 0.2h/Mpc. Results from the LRG
and main galaxy samples are consistent, with the former providing higher signaltonoise.
Our results are robust to omitting angular and radial density fluctuations and are
consistent between different parts of the sky. They provide a striking confirmation of the
predicted largescale LCDM power spectrum.
Combining only SDSS LRG and WMAP data places robust constraints on many cosmological
parameters that complement prior analyses of multiple data sets. The LRGs provide
independent crosschecks on Omega_m and the baryon fraction in good agreement with WMAP. Within
the context of flat LCDM models, our LRG measurements complement WMAP by sharpening
the constraints on the matter density, the neutrino density and the tensor amplitude by
about a factor of two, giving Omega_m=0.24+0.02 (1 sigma), sum m_nu < 0.9 eV (95%) and
r<0.3 (95%). Baryon oscillations are clearly detected and provide a robust measurement of
the comoving distance to the median survey redshift z=0.35 independent of curvature and dark
energy properties. Within the LCDM framework, our power spectrum measurement improves
the evidence for spatial flatness, sharpening the curvature constraint Omega_tot=1.05+0.05
from WMAP alone to Omega_tot=1.003+0.010. Assuming Omega_tot=1, the equation of state
parameter is constrained to w=0.94+0.09, indicating the potential for more ambitious
future LRG measurements to provide precision tests of the nature of dark energy. All these
constraints are essentially independent of scales k>0.1h/Mpc and associated nonlinear
complications, yet agree well with more aggressive published analyses where nonlinear
modeling is crucial.
.
Publication info
astroph/0608632,
Phys. Rev. D, in press (36 PRD pages, 25 figures, 3 tables)
Download: pdf
LUMINOUS RED GALAXY PICS
Luminous Red Galaxies (red dots) provide six times more cosmological information than typical
ones, because they can be seen further away and therefore map a large volume.
Galaxies have their distance determined from their spectrum to create
the 5 billion lightyears deep 3D map (right) where each galaxy is shown as a single
point whose color represents its luminosity.
This image shows only the small fraction of the
galaxies in the map that lie near the plane of Earth's equator.
(Click for high resolution jpg)
Same as previous figure, but showing only the upper slice.
(Click for high resolution jpg)
The 3D power spectrum of galaxies from the SDSS
This packages up the largescale clustering information from the 2004 SDSS data release 2 as a useful starting point for cosmological model fitting.
Figure 22:
Our measured power spectrum of L* galaxies. The errors are uncorrelated
except for an overall calibration uncertainty of order 4%
not included in the error bars.
The red curve is the best fit linear concordance model.
Click here to download the paper: (pdf, ps).
The measurements and their window functions are
further down on this page.
Authors:
Max Tegmark, Michael R. Blanton, Michael A. Strauss, Fiona S. Hoyle, David Schlegel, Roman Scoccimarro, Michael S. Vogeley, David H. Weinberg, Idit Zehavi, Andreas Berlind, Tamas
Budavari, Andrew Connolly, Daniel J. Eisenstein, Douglas Finkbeiner, Joshua A. Frieman, James E. Gunn, Andrew J. S. Hamilton, Lam Hui, Bhuvnesh Jain, David Johnston, Stephen Kent, Huan Lin, Reiko
Nakajima, Robert C. Nichol, Jeremiah P. Ostriker, Adrian Pope, Ryan Scranton, Uros Seljak, Ravi K. Sheth, Albert Stebbins, Alexander S. Szalay, Istvan Szapudi, Licia Verde, Yongzhong Xu, James Annis, Neta A.
Bahcall, J. Brinkmann, Istvan Csabai, Jon Loveday, Mamoru Doi, Masataka Fukugita, Richard Gott III, Greg Hennessy, David Hogg, Zeljko Ivezic, Gillian R. Knapp, Don Q. Lamb, Brian C. Lee, Robert
H. Lupton. Timothy A. McKay. Peter Kunszt. Jeffrey A. Munn. Liam O'Connell, John Peoples, Jeffrey R. Pier, Michael Richmond, Constance Rockosi,
Christopher Stoughton, Douglas L. Tucker, Brian Yanny and Donald G. York, for the SDSS Collaboration
Abstract:
We measure the largescale realspace power spectrum P(k) using a sample of 205,443 galaxies
from the Sloan Digital Sky Survey, covering 2417 effective square degrees with mean redshift
z~0.1.
We employ a matrixbased method using pseudoKarhunenLoeve eigenmodes,
producing
uncorrelated minimumvariance measurements in 22 kbands of
both the clustering power and its anisotropy due to redshiftspace distortions,
with narrow and wellbehaved window functions in the range
0.02h/Mpc < k < 0.3h/Mpc.
We pay particular attention to modeling, quantifying and correcting for
potential systematic errors,
nonlinear redshift distortions and
the artificial redtilt caused by
luminositydependent bias. Our results are robust to omitting angular and
radial density fluctuations and are consistent between different
parts of the sky.
Our final result is a measurement of the realspace matter power spectrum P(k)
up to an unknown overall multiplicative bias factor.
Our calculations suggest that this bias factor
is independent of scale to better than a few percent for k < 0.1h/Mpc,
thereby making our results useful for precision measurements of
cosmological parameters in conjunction with data from other experiments such as
the WMAP satellite. The power spectrum is not wellcharacterized by a
single power law, but unambiguously shows curvature.
As a simple characterization of the data,
our measurements are well fit by a flat scaleinvariant adiabatic cosmological model with
h Omega_m = 0.213 +/ 0.023
and sigma_8 = 0.89 +/ 0.02 for L* galaxies,
when fixing the baryon fraction
Omega_b/Omega_m=0.17
and the Hubble parameter h=0.72;
cosmological interpretation is given in a
companion paper.
Publication info
astroph/0310725,
submitted to ApJ
6/18/03, report received 9/21/03,
resubmitted 10/27/03, accepted 12/4/03
(41 ApJ pages, 40 figures, 3 tables)
Download: pdf, ps
Downloadable P(k) data
 Measurements and error bars from Table 3 in the paper:
sdss_measurements.txt
 Window functions:
sdss_windows.txt
 kbands at which window functions are defined:
sdss_kbands.txt
 Sample f77 code that computes SDSS likelihood given some P(k) model:
compute_sdss_likelihood.f,
sdss_likelihood_common.f
 All of the above combined into a single gzipped tar file:
tarball.tar.gz
We recommend that you cut at kmax or 0.15h/Mpc (using 17 bands)
or 0.20h/Mpc (using 19 bands)
and fit to a nonlinear P(k) model.
Cosmological parameters from SDSS and WMAP
This is the companion paper to the "here's a measurement" paper above,
discussing what it means.
Figure 10:
Constraints on inflation models at 95% confidence.
The phi^4 model (star) and the phi^2 model (a.k.a. eternal stochastic inflation; line segment)
are seen to be emminently testable.
Click here to download the paper: (pdf, ps).
Authors:
Max Tegmark, Michael Strauss, Michael R. Blanton, Kev Abazajian, Scott Dodelson, Havard Sandvik, Xiaomin
Wang, David H. Weinberg, Idit Zehavi, Neta A. Bahcall, Fiona Hoyle, David Schlegel, Roman Scoccimarro,
Michael S. Vogeley, Andreas Berlind, Tamas Budavari, Andrew Connolly Daniel J. Eisenstein, Douglas
Finkbeiner, Joshua A. Frieman, James E. Gunn, Lam Hui, Bhuvnesh Jain, David Johnston,
Stephen Kent, Huan Lin, Reiko Nakajima, Robert C. Nichol, Jeremiah P. Ostriker, Adrian Pope, Ryan Scranton, Uros Seljak, Ravi K.
Sheth, Albert Stebbins, Alexander S. Szalay, Istvan Szapudi, Yongzhong Xu, James Annis, J. Brinkmann, Scott
Burles, Francisco J. Castander, Istvan Csabai, Jon Loveday, Mamoru Doi, Masataka Fukugita, Greg Hennessy,
David W. Hogg, Zeljko Ivezic, Gillian R. Knapp, Don Q. Lamb, Brian C. Lee, Robert H. Lupton, Timothy A.
McKay, Peter Kunszt, Jeffrey A. Munn, Liam O'Connell, John Peoples, Jeffrey R. Pier,
Michael Richmond, Constance Rockosi, Donald P. Schneider, Christopher Stoughton, Douglas L. Tucker, Daniel E.
Vanden Berk, Brian Yanny and Donald G. York
Abstract:
We measure cosmological parameters using the threedimensional power spectrum P(k)
from over 200,000 galaxies in the Sloan Digital Sky Survey (SDSS) in combination with WMAP and other data.
Our results are consistent with a
``vanilla'' flat adiabatic LambdaCDM model without
tilt (n=1), running tilt, tensor modes or massive neutrinos.
Adding SDSS information more than halves the WMAPonly error bars on some parameters,
tightening 1 sigma constraints on the Hubble parameter from
h~0.74+0.180.07
to
h~0.70+0.040.03,
on the matter density from
Omega_m~0.25+/0.10
to
Omega_m~0.30+/0.04 (1 sigma)
and on neutrino masses from <11 eV to <0.6 eV (95%).
SDSS helps even more when dropping prior assumptions about curvature, neutrinos, tensor modes
and the equation of state.
Our results are in
substantial agreement with the joint analysis of WMAP and the 2dF
Galaxy Redshift Survey, which is an impressive consistency check with
independent redshift survey data and analysis techniques.
In this paper,
we place particular emphasis on clarifying the physical origin of the constraints,
i.e., what we do and do not know when using different data sets and
prior assumptions.
For instance, dropping the assumption that space is perfectly flat,
the WMAPonly constraint on
the measured age of the Universe tightens from
t0~16.3+2.31.8 Gyr
to
t0~14.1+1.00.9 Gyr by adding SDSS and SN Ia data.
Including tensors, running tilt, neutrino mass and equation of state in
the list of free parameters, many constraints are still quite weak,
but future cosmological measurements from SDSS and other sources
should allow these to be substantially tightened.
Publication info
astroph/0310723,
submitted to Physical Review D (26 PRD pages, 18 figures, 8 tables)
10/27/03.
Download: pdf, ps
POWER SPECTRUM PICS
(This was astronomy picture of the day
October 28 2003.)
The SDSS is two separate surveys in one: galaxies are identified in 2D images (right),
then have their distance determined from their spectrum to create
a 2 billion lightyears deep 3D map (left) where each galaxy is shown as a single
point, the color representing the luminosity  this shows only
those 66,976 our of 205,443 galaxies in the map that lie
near the plane of Earth's equator.
(Click for
high resolution jpg,
version without lines.)
The new SDSS results (black dots) are the most accurate
measurements to date of how the density of the Universe
fluctuates from place to place on scales of millions of lightyears.
These and other cosmological measurements agree with the
theoretical prediction (blue curve) for a Universe composed of
5% atoms, 25% dark matter and 70% dark energy.
The larger the scales we average over, the more uniform the Universe appears.
(Click for
high resolution jpg,
no frills version.)
Slides for a talk?
Here's a tarball with gif images of all the figures
in the 2003 SDSS+WMAP paper.
If you type "xv *.gif" after unpacking it, hitting "[TAB]" will overlay the constraints
one by one.
Here's a powerpoint file with the highlights from
in the SDSS+WMAP paper.
Here's a tarball with gif images of the figures
in the P(k) paper.
SDSS in the news
Here is a 2006 article about our SDSS power spectrum work in
Sky & Telescope.
Here are some popular articles from 2003 that covered our SDSS power spectrum work in
Astronomy picture of the day,
Science,
Sky & Telescope,
Science News,
New Scientist,
Japanese 1,
Japanese 2,
Japanese 3,
Japanese 4,
Dutch and
Science Magazine's
Breakthrough of the Year 2003.
This angular power spectrum,
packages up the largescale clustering information from the SDSS early data release
as a useful starting point for cosmological model fitting.
It's one of a suite of five simultaneous papers:
Scranton et al,
Connolly et al,
Tegmark et al,
Szalay et al &
Dodelson et al.
Figure 2:
Uncorrelated measurements of
the angular power spectrum for four magnitude bins.
The curves show a standard ``concordance'' model
with (solid) and without (dashed) nonlinear evolution using
four separate bias factors of order unity as.
Please click here
to download the paper. The measurements and their window functions are
further down on this page.
Authors:
Max Tegmark,
Scott Dodelson,
Daniel Eisenstein,
Vijay Narayanan,
Roman Scoccimarro,
Ryan Scranton,
Michael A. Strauss, et al. (41 more)
Abstract:
We compute the angular power spectrum C_l from
1.5 million galaxies in early SDSS data
on large angular scales, l<600.
The data set covers about 160 square degrees, with a characteristic
depth of order
1 Gpc/h
in the faintest (21 < r' < 22) of our four
magnitude bins.
Cosmological interpretations of these results are
presented in a companion paper by Dodelson et al (2001).
The data in all four magnitude bins are consistent with a
simple flat ``concordance'' model with nonlinear evolution
and linear bias factors of order unity. Nonlinear evolution
is particularly evident for the brightest galaxies.
A series of tests suggest that systematic errors related to
seeing, reddening, etc., are negligible,
which bodes well for the sixtyfold larger
sample that the SDSS is currently collecting.
Uncorrelated error bars and wellbehaved window functions
make our measurements a convenient starting point for
cosmological model fitting.
Figure 7:
The same band power measurements as in Figure 2 above,
but plotted in kspace assuming a radial selection function.
The solid curve is a
``concordance'' model with (solid) and without (dashed) nonlinear evolution.
Mean depth misestimates would shift
the points along the dotted lines of slope 3.
Publication
astroph/0107418, ApJ, 571, 191
Downloadable C_l data
 C_l measurements and error bars from Table 1 in the paper
for magnitude bins
1819,
1920,
2021 &
2122
 lspace window functions from Figure 3 in the paper
for magnitude bins
1819,
1920,
2021 &
2122
 kspace window functions from Figure 5 in the paper
for magnitude bins
1819,
1920,
2021 &
2122
 A readme file
describing the contents of the files and their relation to
the notation in the paper
 All of the above stuff in a single
gzipped tar file
1 and 2 are measured from the data alone  see Scranton et al (2001),
astroph/0107416
for a systematic error budget.
3 assumes the radial selection functions of
Dodelson et al,
astroph/0107421.
The error bars are uncorrelated, so no the covariance matrix is simply
the diagonal matrix with the above variances on the diagonal.
Note that 1 + 3 combined is all you need to generate figure 7 above
and to do your own fits cosmological models that predict P(k).
Other SDSSrelated papers I've been involved with

Detection of the Baryon Acoustic Peak in the LargeScale Correlation Function of SDSS Luminous Red
Galaxies,
D. J. Eisenstein, I. Zehavi, D. W. Hogg, R. Scoccimarro, M. R. Blanton, R. C. Nichol,
R. Scranton, H. Seo, M. Tegmark, Z. Zheng, S. Anderson, J. Annis, N. Bahcall, J. Brinkmann,
S. Burles, F. J. Castander, A. Connolly, I. Csabai, M. Doi, M. Fukugita, J. A. Frieman,
K. Glazebrook, J. E. Gunn, J. S. Hendry, G. Hennessy, Z. Ivezic, S. Kent, G. R. Knapp, H.
Lin, Y. Loh, R. H. Lupton, B. Margon, T. McKay, A. Meiksin,
J. A. Munn, A. Pope, M. Richmond, D. Schlegel, D. Schneider, K. Shimasaku, C. Stoughton, M. Strauss,
M. SubbaRao, A. S. Szalay, I. Szapudi, D. Tucker, B. Yanny & D. York 2005,
astroph/0501171, ApJ

The IntermediateScale Clustering of Luminous Red Galaxies,
Idit Zehavi, Daniel J. Eisenstein, Robert C. Nichol, Michael R. Blanton, David W. Hogg,
Jon Brinkmann, Jon Loveday, Avery Meiksin, Donald P. Schneider, Max Tegmark 2004,
astroph/0411557, ApJ, 621, 22

The Third Data Release of the Sloan Digital Sky Survey,
K. Abazajian et al. (SDSS collaboration; I'm one of 154 alphabetized authors) 2005,
astroph/0410239, Astron. J, 129, 1755

NYUVAGC: a galaxy catalog based on new public surveys,
Michael R. Blanton, David J. Schlegel, Michael A. Strauss, J. Brinkmann, Douglas Finkbeiner, Masataka Fukugita, James E. Gunn,
David W. Hogg, Zeljko Ivezic, G. R. Knapp, Robert H. Lupton, Jeffrey A. Munn, Donald P. Schneider, Max Tegmark \& Idit Zehavi 2004,
astroph/0410166, Astron. J, 129, 2562

The Luminosity and Color Dependence of the Galaxy Correlation Function,
I Zehavi, Z Zheng, DH Weinberg, JA Frieman, AA Berlind, MR Blanton, R Scoccimarro, RK
Sheth, MA Strauss, I Kayo, Y Suto, M Fukugita, O Nakamura, NA Bahcall, J Brinkmann, JE
Gunn, GS Hennessy, Z Ivezic, GR Knapp, J Loveday, A Meiksin, DJ Schlegel, DP Schneider, I
Szapudi, M Tegmark, MS Vogeley & DG York 2004,
astroph/0408569

Cosmology and the Halo Occupation Distribution from SmallScale Galaxy
Clustering in the Sloan Digital Sky Survey,
Kevork Abazajian, Zheng Zheng, Idit Zehavi, David H. Weinberg, Joshua A. Frieman, Andreas A. Berlind,
Michael R. Blanton, Neta A. Bahcall, J. Brinkmann, Donald P. Schneider & Max Tegmark 2005,
astroph/0408003, ApJ, 625, 613

Cosmological parameter analysis including SDSS Lyalpha forest and galaxy bias:
constraints on the primordial spectrum of fluctuations, neutrino mass, and dark energy,
U Seljak, A Makarov, P McDonald, S Anderson, N Bahcall, J Brinkmann, S Burles, R Cen, M Doi,
J Gunn, Z Ivezic, S Kent, R Lupton, J Munn, R Nichol, J Ostriker, D Schlegel,
M Tegmark, D Van den Berk, D Weinberg & D York 2005,
astroph/0407372, PRD, 71, 103515

SDSS galaxy bias from halo massbias relation and its cosmological implications,
U Seljak, A Makarov, R Mandelbaum, C Hirata, N Padmanabhan, P McDonald, M Blanton, M Tegmark,
N Bahcall & J Brinkmann 2005, astroph/0406594, PRD, 71, 043511

The Sloan Digital Sky Survey Commissioning Data: Orion,
Douglas Finkbeiner et al 2004,
Astron. J., in press

The Second Data Release of the Sloan Digital Sky Survey,
Kev Abazajian et al 2004 (144 authors :),
astroph/0403325,
Astron. J., 128, 502

Cosmological Parameters from Eigenmode Analysis of Sloan Digital Sky Survey Galaxy Redshifts,
A. Pope et al 2004,
astroph/0401249, ApJ, 607, 655660

A Map of the Universe,
J. Richard Gott III, Mario Juric, David Schlegel, Fiona Hoyle, Michael Vogeley,
Max Tegmark, Neta Bahcall, Jon Brinkmann 2005, astroph/0310571, ApJ, 624, 463

Physical evidence for dark energy,
R. Scranton, A. J. Connolly, R. C. Nichol, A. Stebbins,
I. Szapudi, D. J. Eisenstein, N. Afshordi, T. Budavari, I. Csabai,
J. A. Frieman, J. E. Gunn, D. Johnson, Y. Loh, R. H. Lupton,
C. J. Miller, E. S. Sheldon, R. S. Sheth, A. S. Szalay,
M. Tegmark, Y. Xu, et al 2003,
astroph/0307335

A scheme to deal accurately and efficiently with
complex angular masks in galaxy surveys,
Andrew J. S. Hamilton & Max Tegmark 2003,
astroph/0306324, MNRAS, 349, 115

Angular Clustering with Photometric Redshifts in the Sloan Digital Sky Survey:
Bimodality in the Clustering Properties of Galaxies,
Tamas Budavari, Andrew J. Connolly, Alexander S. Szalay, Istvan Szapudi, Istvan Csabai,
Ryan Scranton, Neta A. Bahcall, Jon Brinkmann, Daniel J. Eisenstein, Joshua A. Frieman,
Masataka Fukugita, James E. Gunn, David Johnston, Stephen Kent, Jon N. Loveday,
Robert H. Lupton, Max Tegmark, Aniruddha R. Thakar, Brian Yanny, Donald G. York,
Idit Zehavi 2003,
astroph/0305603,
ApJ, 595, 59

The First Data Release of the Sloan Digital Sky Survey,
Kev Abazajian et al 2003 (I'm out of 162nd out of 189 alphabetized authors :),
astroph/0305492,
Astron. J., 126, 2081

On Departures From a Power Law in the Galaxy Correlation Function,
Idit Zehavi, David H. Weinberg, Zheng Zheng, Andreas A. Berlind,
Joshua A. Frieman, Roman Scoccimarro, Ravi K. Sheth, Michael R. Blanton,
Max Tegmark, Houjun J. Mo, et al. 2004,
astroph/0301280,
ApJ, 608, 16

The Galaxy Luminosity Function and Luminosity Density at Redshift z=0.1
Michael R. Blanton, David W. Hogg, J. Brinkmann, Andrew J. Connolly, Istvan Csabai, Neta A. Bahcall, Masataka Fukugita,
Jon Loveday, Avery Meiksin, Jeffrey A. Munn, R. C. Nichol, Sadanori Okamura, Thomas Quinn, Donald P. Schneider,
Kazuhiro Shimasaku, Michael A. Strauss, Max Tegmark, Michael S. Vogeley & David H. Weinberg 2003,
astroph/0210215, ApJ, 592, 819

TwoDimensional Topology of the Sloan Digital Sky Survey
Fiona Hoyle, Michael S. Vogeley, J. Richard Gott III, Michael Blanton,
Max Tegmark, David H. Weinberg, J. Brinkmann, N. Bahcall 2002,
astroph/0206146, ApJ, 580, 663671

The 3D power spectrum from angular clustering of galaxies in early SDSS data
Scott Dodelson, Vijay K. Narayanan, Max Tegmark, Ryan Scranton et al
(42 others) 2002,
astroph/0107421, ApJ, 572, 140

KL estimation of the power spectrum parameters from the angular distribution of
galaxies in early SDSS data
Alexander Szalay, Bhuvnesh Jain, Takahiko Matsubara, Ryan Scranton,
Michael S. Vogeley, et al (I'm 26 out of 49) 2003,
astroph/0107419, ApJ, 591, 1

The angular power spectrum of galaxies from early SDSS data
Max Tegmark, Scott Dodelson, Daniel Eisenstein, Vijay Narayanan,
Roman Scoccimarro, Ryan Scranton, Michael Strauss et al
(41 others) 2002,
astroph/0107418, ApJ, 571, 191

The angular correlation function of galaxies from early SDSS data
Andrew Connolly, Ryan Scranton, David Johnston et al
(I'm 21 out of 49) 2002,
astroph/0107417, ApJ, 579

Analysis of systematic effects and statistical uncertainties in
angular clustering of galaxies from early SDSS data
Ryan Scranton, David Johnston, Scott Dodelson, Joshua Frieman
et al (I'm 21 out of 47 :) 2002,
astroph/0107416, ApJ, 579, 48

Galaxy clustering in early SDSS redshift data
Idit Zehavi, Michael Blanton, Joshua Frieman, David Weinberg,
Houjun Mo, Michael Strauss + 60 alphabetized authors
(I'm the 53rd...:)
2002, astroph/0102476, ApJ, 571, 172

The timeevolution of bias and Bias
and beyond
M Tegmark & P J E Peebles, ApJL, 500, 7982
and a 2nd paper astroph/9809185
Shows how SDSS can produce more realistic and robust matter power
spectra including stochastic bias

Cosmic Complementarity: Joint Parameter Estimation from CMB Experiments
and Redshift Surveys
D J Eisenstein,W Hu & M Tegmark 1998, astroph/9807130,
ApJ, 518, 223
Detailed forecast of the accuracy with which SDSS + CMB can
measure cosmological parameters

Observationally Determining the Properties of Dark Matter
W Hu, D J Eisenstein, M Tegmark & M White 1998, astroph/9806362,
Phys. Rev. D, 59, 023512
Shows how SDSS + CMB can constrain the equation of state and other
properties of the dark matter

Cosmic complementarity: H_0 and Omega_m from combining CMB experiments
and redshift surveys
D J Eisenstein,W Hu & M Tegmark 1998, astroph/9805239,
ApJL, 504, L57
Shows how SDSS + CMB can give an accurate and robust measurement
of the Hubble constant

Cosmic complementarity: probing the acceleration
of the Universe
M Tegmark, D J Eisenstein,W Hu & R Kron 1998, astroph/9805117,
rejected by ApJL
Shows how SDSS galaxy luminosities, sizes and counts can complement
SN Ia and CMB for measuring Omega and Lambda

Weighing
neutrinos with galaxy surveys
W Hu, D J Eisenstein & M Tegmark 1998, Phys. Rev. Lett., 80,
5255
Shows that SDSS can provide interesting neutino mass limits

Measuring the galaxy power spectrum with future
redshift surveys
M Tegmark, A Hamilton, M Strauss, M Vogeley & A Szalay 1998, ApJ,
499, 555576
Describes methods for computing the SDSS galaxy power spectrum and
measuring cosmological parameters

Measuring cosmological parameters with galaxy
surveys
M Tegmark 1997, Phys. Rev. Lett., 79, 3806
Forecasts the accuracy with which SDSS can measure
cosmological parameters
LINKS

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Some other redshift surveys:
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Last modified: October 30, 2006