SDSS

(Sloan Digital Sky Survey)

Other Web pages: Spires

References

  1 - Reviews

  2 - Articles

  3 - Type Ia Supernovae - Conference Proceedings

  4 - Detector

  5 - Conference Proceedings

The references in each group are listed in approximate inverted chronological order.
Click on the reference label to search it in inSPIRE.

1 - Reviews

[1-1]
Clusters of Galaxies in the SDSS, Robert C. Nichol, arXiv:astro-ph/0305041, 2003.
[2-23]
The Sloan Digital Sky Survey, Loveday, Jon (SDSS), Contemp. Phys. 43 (2002) 437-449, arXiv:astro-ph/0207189.

2 - Articles

[2-1]
The Sixth Data Release of the Sloan Digital Sky Survey, Adelman-McCarthy, Jennifer K. et al. (SDSS), Astrophys. J. Suppl. 175 (2008) 297-313, arXiv:0707.3413.
[2-2]
The Fifth Data Release of the Sloan Digital Sky Survey, Adelman-McCarthy, Jennifer K. (SDSS), Astrophys. J. Suppl. 172 (2007) 634-644, arXiv:0707.3380.
[2-3]
Cosmological Constraints from the SDSS Luminous Red Galaxies, Tegmark, M et al. (SDSS), Phys. Rev. D74 (2006) 123507, arXiv:astro-ph/0608632.
[2-4]
The Fourth Data Release of the Sloan Digital Sky Survey, Adelman-McCarthy, J.K. et al. (SDSS), Astrophys. J. Suppl. 162 (2006) 38, arXiv:astro-ph/0507711.
[2-5]
Detection of Cosmic Magnification with the Sloan Digital Sky Survey, Ryan Scranton et al. (SDSS), Astrophys. J. 633 (2005) 589, arXiv:astro-ph/0504510. SDSS News Release.
[2-6]
The Sloan Digital Sky Survey Quasar Catalog III. Third Data Release, Schneider, D. P. et al. (The SDSS), Astron. J. 130 (2005) 367-380, arXiv:astro-ph/0503679.
[2-7]
Detection of the Baryon Acoustic Peak in the Large-Scale Correlation Function of SDSS Luminous Red Galaxies, Eisenstein, Daniel J. et al. (SDSS), Astrophys. J. 633 (2005) 560, arXiv:astro-ph/0501171.
From the abstract: We find a well-detected peak in the correlation function at 100 h^{-1} <b>Mpc</b> separation that is an excellent match to the predicted shape and location of the imprint of the recombination-epoch acoustic oscillations on the low-redshift clustering of matter. This detection demonstrates the linear growth of structure by gravitational instability between z =~ 1000 and the present and confirms a firm prediction of the standard cosmological theory. The acoustic peak provides a standard ruler by which we can measure the ratio of the distances to z=0.35 and z=1089 to 4% fractional accuracy and the absolute distance to z=0.35 to 5% accuracy. From the overall shape of the correlation function, we measure the matter density \Omega_mh^2 to 8% and find agreement with the value from cosmic microwave background (CMB) anisotropies. Independent of the constraints provided by the CMB acoustic scale, we find \Omega_m=0.273 +- 0.025+0.123(1+w_0)+0.137\Omega_K. Including the CMB acoustic scale, we find that the spatial curvature is \Omega_K=-0.010 +- 0.009 if the dark energy is a cosmological constant.
[2-8]
The Third Data Release of the Sloan Digital Sky Survey, K. Abazajian et al. (SDSS), Astron. J. 129 (2005) 1755, arXiv:astro-ph/0410239.
[2-9]
Cosmological parameter analysis including SDSS Ly-alpha forest and galaxy bias: Constraints on the primordial spectrum of fluctuations, neutrino mass, and dark energy, Seljak, Uros et al. (SDSS), Phys. Rev. D71 (2005) 103515, arXiv:astro-ph/0407372.
From the abstract: We find no evidence of neutrino mass: for the case of 3 massive neutrino families with an inflationary prior, \sum m_{\nu}<0.42eV and the mass of lightest neutrino is m_1<0.13eV at 95% c.l. For the 3 massless + 1 massive neutrino case we find m_{\nu}<0.79eV for the massive neutrino, excluding at 95% c.l. all neutrino mass solutions compatible with the LSND results.
[2-10]
The Lyman-alpha Forest Power Spectrum from the Sloan Digital Sky Survey, Patrick McDonald et al. (SDSS), Astrophys. J. Suppl. 163 (2006) 80, arXiv:astro-ph/0405013.
[2-11]
The Second Data Release of the Sloan Digital Sky Survey, K. Abazajian et al. (SDSS), Astron. J. 128 (2004) 502, arXiv:astro-ph/0403325.
[2-12]
Cosmological Parameters from Eigenmode Analysis of Sloan Digital Sky Survey Galaxy Redshifts, Pope, Adrian C. et al. (SDSS), Astrophys. J. 607 (2004) 655, arXiv:astro-ph/0401249.
[2-13]
Sloan Digital Sky Survey Spectroscopic Lens Search: I. Discovery of Intermediate-Redshift Star-Forming Galaxies Behind Foreground Luminous Red Galaxies, A. S. Bolton et al. (SDSS), Astron. J. 127 (2004) 1860, arXiv:astro-ph/0311055.
[2-14]
The 3D power spectrum of galaxies from the SDSS, M. Tegmark et al. (SDSS), Astrophys. J. 606 (2004) 702, arXiv:astro-ph/0310725.
[2-15]
Cosmological parameters from SDSS and WMAP, M. Tegmark et al. (SDSS), Phys. Rev. D69 (2004) 103501, arXiv:astro-ph/0310723.
From the abstract: We measure cosmological parameters using the three-dimensional 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 \Lambda<b>CDM</b> model without tilt (n_s=1), running tilt, tensor modes or massive neutrinos. Adding SDSS information more than halves the WMAP-only error bars on some parameters, tightening 1\sigma constraints on the Hubble parameter from h =~ 0.74^{+0.18}_{-0.07} to h =~ 0.70^{+0.04}_{-0.03}, 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\text{eV} to <0.6<b>eV</b> (95%).
From the article: The most favored value is \sum_k m_{\nu_k}=0, and obtain a 95% upper limit \sum_k m_{\nu_k}<1.7<b>eV</b>.
...
The WMAP team obtains the constraint \sum_k m_{\nu_k}<0.7\text{eV} [astro-ph/0302209] by combining WMAP with the 2dFGRS. This limit is a factor of three lower than ours because of their stronger priors, most importantly that on galaxy bias b determined using a bispectrum analysis of the 2dF galaxy clustering data [astro-ph/0112161].... Since the bias is marginalized over, our SDSS neutrino constraints come not from the amplitude of the power spectrum, only from its shape.
[2-16]
SDSS J0903+5028: A New Gravitational Lens, Johnston, D. E. et al. (SDSS), Astron. J. 126 (2003) 2281, arXiv:astro-ph/0307371.
[2-17]
Physical Evidence for Dark Energy, Scranton, R. et al. (SDSS), arXiv:astro-ph/0307335, 2003.
[2-18]
The First Data Release of the Sloan Digital Sky Survey, Abazajian, Kevork et al. (SDSS), Astron. J. 126 (2003) 2081, arXiv:astro-ph/0305492.
[2-19]
The size distribution of galaxies in the Sloan Digital Sky Survey, S. Shen et al. (SDSS), Mon. Not. Roy. Astron. Soc. 343 (2003) 978, arXiv:astro-ph/0301527.
[2-20]
SDSS Catalog of Stars in the Draco Dwarf Spheroidal Galaxy, H. A. Rave et al. (SDSS), Astrophys. J. Suppl. 145 (2003) 245, arXiv:astro-ph/0301185. To appear in ApJS 14 pages, 6 figures.
[2-21]
A Survey of z>5.7 Quasars in the Sloan Digital Sky Survey II: Discovery of Three Additional Quasars at z>6, X. Fan et al. (SDSS), Astron. J. 125 (2003) 1649, arXiv:astro-ph/0301135.
[2-22]
Astrometric Calibration of the Sloan Digital Sky Survey, Pier, J. R. et al., Astron. J. 125 (2003) 1559, arXiv:astro-ph/0211375.
[2-23]
The Sloan Digital Sky Survey, Loveday, J. (SDSS), Contemp. Phys. 43 (2002) 437-449, arXiv:astro-ph/0207189.
[2-24]
The 3D Power Spectrum from Angular Clustering of Galaxies in Early SDSS Data, Dodelson, S. et al. (SDSS), Astrophys. J. 572 (2001) 140-156, arXiv:astro-ph/0107421.

3 - Type Ia Supernovae - Conference Proceedings

[3-1]
The Fall 2004 SDSS Supernova Survey, Masao Sako et al. (The SDSS), eConf C041213 (2005) 1424, arXiv:astro-ph/0504455. 22nd Texas Symposium on Relativistic Astrophysics.

4 - Detector

[4-1]
The 2.5 m Telescope of the Sloan Digital Sky Survey, James E. Gunn, Walter A. Siegmund, Edward J. Mannery et al. (SDSS), Astron. J. 131 (2006) 2332, arXiv:astro-ph/0602326.

5 - Conference Proceedings

Useful Links

Max Tegmark's SDSS page

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Authors:
Carlo Giunti / giunti@to.infn.it
Marco Laveder / marco.laveder@pd.infn.it
Last Update: Tue 15 May 2012, day 136 of the year 2012, 09:42:20 UTC