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1. Online Scientific Data Curation, Publication, and Archiving

Author

Gray, Jim, Szalay, Alexander S., Thakar, Ani R., Stoughton, Christopher, and vandenBerg, Jan

Subjects
Computer Science - Digital Libraries, H.3.7, I.7.4, J.2, J.3, J.7
Abstract

Science projects are data publishers. The scale and complexity of current and future science data changes the nature of the publication process. Publication is becoming a major project component. At a minimum, a project must preserve the ephemeral data it gathers. Derived data can be reconstructed from metadata, but metadata is ephemeral. Longer term, a project should expect some archive to preserve the data. We observe that pub-lished scientific data needs to be available forever ? this gives rise to the data pyramid of versions and to data inflation where the derived data volumes explode. As an example, this article describes the Sloan Digital Sky Survey (SDSS) strategies for data publication, data access, curation, and preservation., Comment: original at http://research.microsoft.com/scripts/pubs/view.asp?TR_ID=MSR-TR-2002-74

Published
2002
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2. Data Mining the SDSS SkyServer Database

Author

Gray, Jim, Szalay, Alex S., Thakar, Ani R., Kunszt, Peter Z., Stoughton, Christopher, Slutz, Don, and vandenBerg, Jan

Subjects
Computer Science - Databases, Computer Science - Digital Libraries, H.2.8, H.3.3, H.3.5, h.3.7, H.4.2
Abstract

An earlier paper (Szalay et. al. "Designing and Mining MultiTerabyte Astronomy Archives: The Sloan Digital Sky Survey," ACM SIGMOD 2000) described the Sloan Digital Sky Survey's (SDSS) data management needs by defining twenty database queries and twelve data visualization tasks that a good data management system should support. We built a database and interfaces to support both the query load and also a website for ad-hoc access. This paper reports on the database design, describes the data loading pipeline, and reports on the query implementation and performance. The queries typically translated to a single SQL statement. Most queries run in less than 20 seconds, allowing scientists to interactively explore the database. This paper is an in-depth tour of those queries. Readers should first have studied the companion overview paper Szalay et. al. "The SDSS SkyServer, Public Access to the Sloan Digital Sky Server Data" ACM SIGMOND 2002., Comment: 40 pages, Original source is at http://research.microsoft.com/~gray/Papers/MSR_TR_O2_01_20_queries.doc

Published
2002

3. The SDSS SkyServer: Public Access to the Sloan Digital Sky Server Data

Author

Szalay, Alexander S., Gray, Jim, Thakar, Ani R., Kunszt, Peter Z., Malik, Tanu, Raddick, Jordan, Stoughton, Christopher, and vandenBerg, Jan

Subjects
Computer Science - Digital Libraries, Computer Science - Databases, H.3.7, H.3.5, H.2, H.3, H.4, H.5
Abstract

The SkyServer provides Internet access to the public Sloan Digi-tal Sky Survey (SDSS) data for both astronomers and for science education. This paper describes the SkyServer goals and archi-tecture. It also describes our experience operating the SkyServer on the Internet. The SDSS data is public and well-documented so it makes a good test platform for research on database algorithms and performance., Comment: 12 pages, original word document at http://research.microsoft.com/~gray/Papers/MSR_TR_01_104_SkyServer.doc

Published
2002

4. The SDSS SkyServer, Public Access to the Sloan Digital Sky Server Data

Author

Szalay, Alexander, Gray, Jim, Thakar, Ani, Kunszt, Peter Z., Malik, Tanu, Raddick, Jordan, Stoughton, Christopher, and vandenBerg, Jan

Subjects
Computer Science - Digital Libraries, Computer Science - Databases, H.3.5, H.4, J.2, H.2.8
Abstract

The SkyServer provides Internet access to the public Sloan Digital Sky Survey (SDSS) data for both astronomers and for science education. This paper describes the SkyServer goals and architecture. It also describes our experience operating the SkyServer on the Internet. The SDSS data is public and well-documented so it makes a good test platform for research on database algorithms and performance., Comment: submitted for publication, original at http://research.microsoft.com/scripts/pubs/view.asp?TR_ID=MSR-TR-2001-104

Published
2001

5. The Tragedy of Climate Change

Author

Stoughton, Christopher Stephen

Subjects
Climate change, climate change, climate change policy, global warming, public policy, realism, theory
Abstract

This Dissertation develops a Neorealism theory of climate change to provide a deeper, power-based, explanation for why global efforts have largely failed to limit climate change over the last thirty years. Nearly all of the literature on climate change is based within a Neoliberalism framework. No published study to date has provided a comprehensive examination of climate change from a Neorealism perspective. This Dissertation begins to fill this gap in the literature by examining efforts to limit climate change from a number of different angles while using both quantitative and qualitative methods. The analysis finds that the interaction of the underlying structural dynamic at both the global and state levels largely explains why efforts have failed to limit climate change. The interaction of the global anarchic political structure, dominant Liberalism ideology, and fossil fuel dependence among leading state and nonstate actors has led to a business-as-usual pathway to persist. The findings imply that it is highly unlikely global efforts will be able to limit climate change to under two degrees Celsius above pre-industrial levels, the stated target of the latest international agreement, the 2015 Paris Agreement. Achieving such a target would require a transformation of the global structural dynamic which is unlikely in the foreseeable future. The Dissertation concludes by offering a few recommendations for scholars and policymakers.

Published
2020

6. The 3D Power Spectrum from Angular Clustering of Galaxies in Early SDSS Data

Author

Dodelson, Scott, Narayanan, Vijay K., Tegmark, Max, Scranton, Ryan, Budavari, Tamas, Connolly, Andrew, Csabai, Istvan, Eisenstein, Daniel, Frieman, Joshua A., Gunn, James E., Hui, Lam, Jain, Bhuvnesh, Johnston, David, Kent, Stephen M., Loveday, Jon, Nichol, Robert C., O'Connell, Liam, Scoccimarro, Roman, Sheth, Ravi K., Stebbins, Albert, Strauss, Michael A., Szalay, Alexander S., Szapudi, Istvan, Vogeley, Michael S., Zehavi, Idit, Annis, James, Bahcall, Neta A., Brinkman, Jon, Doi, Mamoru, Fukugita, Masataka, Hennessy, Greg, Ivezic, Zeljko, Knapp, Gillian R., Kunszt, Peter, Lamb, Don Q., Lee, Brian C., Lupton, Robert H., Munn, Jeffrey A., Peoples, John, Pier, Jeffrey R., Rockosi, Constance, Schlegel, David, Stoughton, Christopher, Tucker, Douglas L., Yanny, Brian, and York, Donald G.

Subjects
Astrophysics and Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Early photometric data from the Sloan Digital Sky Survey (SDSS) contain angular positions for 1.5 million galaxies. In companion papers, the angular correlation function $w(\theta)$ and 2D power spectrum $C_l$ of these galaxies are presented. Here we invert Limber's equation to extract the 3D power spectrum from the angular results. We accomplish this using an estimate of $dn/dz$, the redshift distribution of galaxies in four different magnitude slices in the SDSS photometric catalog. The resulting 3D power spectrum estimates from $w(\theta)$ and $C_l$ agree with each other and with previous estimates over a range in wavenumbers $0.03 < k/{\rm h Mpc}^{-1} < 1$. The galaxies in the faintest magnitude bin ($21 < \rstar < 22$, which have median redshift $z_m=0.43$) are less clustered than the galaxies in the brightest magnitude bin ($18 < \rstar < 19$ with $z_m=0.17$), especially on scales where nonlinearities are important. The derived power spectrum agrees with that of Szalay et al. (2001) who go directly from the raw data to a parametric estimate of the power spectrum. The strongest constraints on the shape parameter $\Gamma$ come from the faintest galaxies (in the magnitude bin $21 < \rstar < 22$), from which we infer $\Gamma = 0.14^{+0.11}_{-0.06}$ (95% C.L.). Early photometric data from the Sloan Digital Sky Survey (SDSS) contain angular positions for 1.5 million galaxies. In companion papers, the angular correlation functionw(θ) and two-dimensional power spectrumClof these galaxies are presented. Here we invert Limber's equation to extract the three-dimensional power spectrum from the angular results. We accomplish this using an estimate ofdn/dz, the redshift distribution of galaxies in four different magnitude slices in the SDSS photometric catalog. The resulting three-dimensional power spectrum estimates fromw(θ) andClagree with each other and with previous estimates over a range in wavenumbers 0.03

Published
2001

7. Galaxy Clustering in Early SDSS Redshift Data

Author

Zehavi, I., Blanton, Michael R., Frieman, Joshua A., Weinberg, David H., Mo, Houjun J., Anderson, Scott F., Strauss, Michael A., Annis, James, Bahcall, Neta A., Bernardi, Mariangela, Briggs, John W., Brinkmann, Jon, Burles, Scott, Carey, Larry, Castander, Francisco J., Connolly, J., Csabai, Istvan, Dalcanton, Julianne J., Dodelson,Scott, Doi,Mamoru, Eisenstein, Daniel, Evans, Michael L., Finkbeiner, Douglas P., Friedman, Scott, Fukugita, Masataka, Gunn, James E., Hennessy, Greg S., Hindsley, Robert B., Ivezic, Zeljko, Kent,Stephen, Knapp, Gillian R., Kron, Richard, Kunszt, Peter, Lamb, Donald, French Leger, R., Long, Daniel C., Loveday, Jon., Lupton, Robert H., McKay, Timothy, Meiksin, Avery, Merrelli, Aronne, Munn, Jeffrey A., Narayanan, Vijay, Newcomb, Matt, Nichol, Robert C., Owen, Russell, Peoples, John, Pope, Adrian, Rockosi, Constance M., Schlegel, David, Schneider, Donald P., Scoccimarro, Roman, Sheth, Ravi K., Siegmund, Walter, Smee, Stephen, Snir, Yehuda, Stebbins, Albert, Stoughton, Christopher, SubbaRao, Mark, Szalay, Alexander S., Szapudi, Istvan, Tegmark, Max, Tucker, Douglas L., Uomoto, Alan, Vanden Berk, Dan, Vogeley, Michael S., Waddell,Patrick, Yanny, Brian, and York, Donald G.

Subjects
Astrophysics and Astronomy
Abstract

We present the first measurements of clustering in the Sloan Digital Sky Survey (SDSS) galaxy redshift survey. Our sample consists of 29,300 galaxies with redshifts 5,700 km/s < cz < 39,000 km/s, distributed in several long but narrow (2.5-5 degree) segments, covering 690 square degrees. For the full, flux-limited sample, the redshift-space correlation length is approximately 8 Mpc/h. The two-dimensional correlation function \xi(r_p,\pi) shows clear signatures of both the small-scale, ``fingers-of-God'' distortion caused by velocity dispersions in collapsed objects and the large-scale compression caused by coherent flows, though the latter cannot be measured with high precision in the present sample. The inferred real-space correlation function is well described by a power law, \xi(r)=(r/6.1+/-0.2 Mpc/h)^{-1.75+/-0.03}, for 0.1 Mpc/h < r < 16 Mpc/h. The galaxy pairwise velocity dispersion is \sigma_{12} ~ 600+/-100 km/s for projected separations 0.15 Mpc/h < r_p < 5 Mpc/h. When we divide the sample by color, the red galaxies exhibit a stronger and steeper real-space correlation function and a higher pairwise velocity dispersion than do the blue galaxies. The relative behavior of subsamples defined by high/low profile concentration or high/low surface brightness is qualitatively similar to that of the red/blue subsamples. Our most striking result is a clear measurement of scale-independent luminosity bias at r < 10 Mpc/h: subsamples with absolute magnitude ranges centered on M_*-1.5, M_*, and M_*+1.5 have real-space correlation functions that are parallel power laws of slope ~ -1.8 with correlation lengths of approximately 7.4 Mpc/h, 6.3 Mpc/h, and 4.7 Mpc/h, respectively. We present the first measurements of clustering in the Sloan Digital Sky Survey (SDSS) galaxy redshift survey. Our sample consists of 29,300 galaxies with redshifts 5700 km s-1≤cz≤ 39,000 km s-1, distributed in several long but narrow (25-5°) segments, covering 690 deg2. For the full, flux-limited sample, the redshift-space correlation length is approximately 8h-1Mpc. The two-dimensional correlation function ξ(rp,π) shows clear signatures of both the small-scale, "fingers-of-God" distortion caused by velocity dispersions in collapsed objects and the large-scale compression caused by coherent flows, though the latter cannot be measured with high precision in the present sample. The inferred real-space correlation function is well described by a power law, ξ(r) = (r/6.1 ± 0.2h-1Mpc)-1.75±0.03, for 0.1h-1Mpc ≤r≤ 16h-1Mpc. The galaxy pairwise velocity dispersion is σ12≈ 600 ± 100 km s-1for projected separations 0.15h-1Mpc ≤rp≤ 5h-1Mpc. When we divide the sample by color, the red galaxies exhibit a stronger and steeper real-space correlation function and a higher pairwise velocity dispersion than do the blue galaxies. The relative behavior of subsamples defined by high/low profile concentration or high/low surface brightness is qualitatively similar to that of the red/blue subsamples. Our most striking result is a clear measurement of scale-independent luminosity bias atr10h-1Mpc: subsamples with absolute magnitude ranges centered onM*- 1.5,M*, andM*+ 1.5 have real-space correlation functions that are parallel power laws of slope ≈-1.8 with correlation lengths of approximately 7.4, 6.3, and 4.7h-1Mpc, respectively.

Published
2001

8. Cosmological constraints from the SDSS luminous red galaxies

Author

Tegmark, Max, Eisenstein, Daniel J., Strauss, Michael A., Weinberg, David H., Blanton, Michael R., Frieman, Joshua A., Fukugita, Masataka, Gunn, James E., Hamilton, Andrew J. S., Knapp, Gillian R., Nichol, Robert C., Ostriker, Jeremiah P., Padmanabhan, Jeremiah, Percival, Will J., Schlegel, David J., Schneider, Donald P., Scoccimarro, Roman, Seljak, Uroš, Seo, Hee-Jong, Swanson, Molly, Szalay, Alexander S., Vogeley, Michael S., Yoo, Jaiyul, Zehavi, Kevork, Abazajian, Kevork, Anderson, Scott F., Annis, James, Bahcall, Neta A., Bassett, Bruce, Berlind, Andreas, Brinkmann, Jon, Budavari, Tamás, Castander, Francisco, Connolly, Andrew, Csabai, Douglas, Doi, Mamoru, Finkbeiner, Douglas P., Gillespie, Bruce, Glazebrook, Karl, Hennessey, Gregory S., Hogg, David W., Ivezić, Željko, Jain, Bhuvnesh, Johnston, David, Kent, Stephen, Lamb, Donald Q., Lee, Brian C., Lin, Huan, Loveday, Jon, Lupton, Robert H., Munn, Jeffrey A., Park, Changbom, Peoples, John, Pier, Jeffrey R., Pope, Adrian, Richmond, Michael, Rockosi, Constance, Scranton, Ryan, Sheth, Ravi K., Stebbins, Albert, Stoughton, Christopher, Szapudi, István, Tucker, Douglas L., Vanden Berk, Daniel E., Yanny, Brian, York, Donald G., Tegmark, Max, Eisenstein, Daniel J., Strauss, Michael A., Weinberg, David H., Blanton, Michael R., Frieman, Joshua A., Fukugita, Masataka, Gunn, James E., Hamilton, Andrew J. S., Knapp, Gillian R., Nichol, Robert C., Ostriker, Jeremiah P., Padmanabhan, Jeremiah, Percival, Will J., Schlegel, David J., Schneider, Donald P., Scoccimarro, Roman, Seljak, Uroš, Seo, Hee-Jong, Swanson, Molly, Szalay, Alexander S., Vogeley, Michael S., Yoo, Jaiyul, Zehavi, Kevork, Abazajian, Kevork, Anderson, Scott F., Annis, James, Bahcall, Neta A., Bassett, Bruce, Berlind, Andreas, Brinkmann, Jon, Budavari, Tamás, Castander, Francisco, Connolly, Andrew, Csabai, Douglas, Doi, Mamoru, Finkbeiner, Douglas P., Gillespie, Bruce, Glazebrook, Karl, Hennessey, Gregory S., Hogg, David W., Ivezić, Željko, Jain, Bhuvnesh, Johnston, David, Kent, Stephen, Lamb, Donald Q., Lee, Brian C., Lin, Huan, Loveday, Jon, Lupton, Robert H., Munn, Jeffrey A., Park, Changbom, Peoples, John, Pier, Jeffrey R., Pope, Adrian, Richmond, Michael, Rockosi, Constance, Scranton, Ryan, Sheth, Ravi K., Stebbins, Albert, Stoughton, Christopher, Szapudi, István, Tucker, Douglas L., Vanden Berk, Daniel E., Yanny, Brian, and York, Donald G.

Abstract

We measure the large-scale real-space 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 matrix-based power spectrum estimation method using Pseudo-Karhunen-Loève eigenmodes, producing uncorrelated minimum-variance measurements in 20 k-bands of both the clustering power and its anisotropy due to redshift-space distortions, with narrow and well-behaved window functions in the range 0.01h/Mpc

Published
2006

9. Cosmological constraints from the SDSS luminous red galaxies

Author

Tegmark, Max, primary, Eisenstein, Daniel J., additional, Strauss, Michael A., additional, Weinberg, David H., additional, Blanton, Michael R., additional, Frieman, Joshua A., additional, Fukugita, Masataka, additional, Gunn, James E., additional, Hamilton, Andrew J. S., additional, Knapp, Gillian R., additional, Nichol, Robert C., additional, Ostriker, Jeremiah P., additional, Padmanabhan, Nikhil, additional, Percival, Will J., additional, Schlegel, David J., additional, Schneider, Donald P., additional, Scoccimarro, Roman, additional, Seljak, Uroš, additional, Seo, Hee-Jong, additional, Swanson, Molly, additional, Szalay, Alexander S., additional, Vogeley, Michael S., additional, Yoo, Jaiyul, additional, Zehavi, Idit, additional, Abazajian, Kevork, additional, Anderson, Scott F., additional, Annis, James, additional, Bahcall, Neta A., additional, Bassett, Bruce, additional, Berlind, Andreas, additional, Brinkmann, Jon, additional, Budavari, Tamás, additional, Castander, Francisco, additional, Connolly, Andrew, additional, Csabai, Istvan, additional, Doi, Mamoru, additional, Finkbeiner, Douglas P., additional, Gillespie, Bruce, additional, Glazebrook, Karl, additional, Hennessy, Gregory S., additional, Hogg, David W., additional, Ivezić, Željko, additional, Jain, Bhuvnesh, additional, Johnston, David, additional, Kent, Stephen, additional, Lamb, Donald Q., additional, Lee, Brian C., additional, Lin, Huan, additional, Loveday, Jon, additional, Lupton, Robert H., additional, Munn, Jeffrey A., additional, Pan, Kaike, additional, Park, Changbom, additional, Peoples, John, additional, Pier, Jeffrey R., additional, Pope, Adrian, additional, Richmond, Michael, additional, Rockosi, Constance, additional, Scranton, Ryan, additional, Sheth, Ravi K., additional, Stebbins, Albert, additional, Stoughton, Christopher, additional, Szapudi, István, additional, Tucker, Douglas L., additional, Berk, Daniel E. Vanden, additional, Yanny, Brian, additional, and York, Donald G., additional

Published
2006
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10. Detection of the Baryon Acoustic Peak in the Large‐Scale Correlation Function of SDSS Luminous Red Galaxies

Author

Eisenstein, Daniel J., primary, Zehavi, Idit, additional, Hogg, David W., additional, Scoccimarro, Roman, additional, Blanton, Michael R., additional, Nichol, Robert C., additional, Scranton, Ryan, additional, Seo, Hee‐Jong, additional, Tegmark, Max, additional, Zheng, Zheng, additional, Anderson, Scott F., additional, Annis, Jim, additional, Bahcall, Neta, additional, Brinkmann, Jon, additional, Burles, Scott, additional, Castander, Francisco J., additional, Connolly, Andrew, additional, Csabai, Istvan, additional, Doi, Mamoru, additional, Fukugita, Masataka, additional, Frieman, Joshua A., additional, Glazebrook, Karl, additional, Gunn, James E., additional, Hendry, John S., additional, Hennessy, Gregory, additional, Ivezić, Zeljko, additional, Kent, Stephen, additional, Knapp, Gillian R., additional, Lin, Huan, additional, Loh, Yeong‐Shang, additional, Lupton, Robert H., additional, Margon, Bruce, additional, McKay, Timothy A., additional, Meiksin, Avery, additional, Munn, Jeffery A., additional, Pope, Adrian, additional, Richmond, Michael W., additional, Schlegel, David, additional, Schneider, Donald P., additional, Shimasaku, Kazuhiro, additional, Stoughton, Christopher, additional, Strauss, Michael A., additional, SubbaRao, Mark, additional, Szalay, Alexander S., additional, Szapudi, Istvan, additional, Tucker, Douglas L., additional, Yanny, Brian, additional, and York, Donald G., additional

Published
2005
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11. Cosmological parameters from SDSS and WMAP

Author

Tegmark, Max, primary, Strauss, Michael A., additional, Blanton, Michael R., additional, Abazajian, Kevork, additional, Dodelson, Scott, additional, Sandvik, Havard, additional, Wang, Xiaomin, additional, Weinberg, David H., additional, Zehavi, Idit, additional, Bahcall, Neta A., additional, Hoyle, Fiona, additional, Schlegel, David, additional, Scoccimarro, Roman, additional, Vogeley, Michael S., additional, Berlind, Andreas, additional, Budavari, Tamás, additional, Connolly, Andrew, additional, Eisenstein, Daniel J., additional, Finkbeiner, Douglas, additional, Frieman, Joshua A., additional, Gunn, James E., additional, Hui, Lam, additional, Jain, Bhuvnesh, additional, Johnston, David, additional, Kent, Stephen, additional, Lin, Huan, additional, Nakajima, Reiko, additional, Nichol, Robert C., additional, Ostriker, Jeremiah P., additional, Pope, Adrian, additional, Scranton, Ryan, additional, Seljak, Uroš, additional, Sheth, Ravi K., additional, Stebbins, Albert, additional, Szalay, Alexander S., additional, Szapudi, István, additional, Xu, Yongzhong, additional, Annis, James, additional, Brinkmann, J., additional, Burles, Scott, additional, Castander, Francisco J., additional, Csabai, Istvan, additional, Loveday, Jon, additional, Doi, Mamoru, additional, Fukugita, Masataka, additional, Gillespie, Bruce, additional, Hennessy, Greg, additional, Hogg, David W., additional, Ivezić, Željko, additional, Knapp, Gillian R., additional, Lamb, Don Q., additional, Lee, Brian C., additional, Lupton, Robert H., additional, McKay, Timothy A., additional, Kunszt, Peter, additional, Munn, Jeffrey A., additional, O’Connell, Liam, additional, Peoples, John, additional, Pier, Jeffrey R., additional, Richmond, Michael, additional, Rockosi, Constance, additional, Schneider, Donald P., additional, Stoughton, Christopher, additional, Tucker, Douglas L., additional, Vanden Berk, Daniel E., additional, Yanny, Brian, additional, and York, Donald G., additional

Published
2004
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12. PRIME: probing the very early universe

Author

Zheng, Wei, primary, Ford, Holland C., additional, Kruk, Jeffrey W., additional, Tsvetanov, Zlatan I., additional, Szalay, Alexander, additional, Hartig, George F., additional, Stockman, Hervey S., additional, Postman, Marc, additional, Voit, G. M., additional, Shu, Peter K., additional, Greenhouse, Matthew A., additional, Rix, Hans-Walter, additional, Lenzen, Rainer, additional, Kent, Steven M., additional, Stoughton, Christopher, additional, Omont, Alain, additional, and Mellier, Yannick, additional

Published
2003
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13. Data Processing Factory for the Sloan Digital Sky Survey

Author

Stoughton, Christopher, primary, Adelman, Jennifer, additional, Annis, James T., additional, Hendry, John, additional, Inkmann, John, additional, Jester, Sebastian, additional, Kent, Steven M., additional, Kuropatkin, Nickolai, additional, Lee, Brian, additional, Lin, Huan, additional, Peoples, Jr., John, additional, Sparks, Robert, additional, Tucker, Douglas, additional, Vanden Berk, Dan, additional, Yanny, Brian, additional, and Yocum, Dan, additional

Published
2002
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15. The SDSS skyserver

Author

Szalay, Alexander S., primary, Gray, Jim, additional, Thakar, Ani R., additional, Kunszt, Peter Z., additional, Malik, Tanu, additional, Raddick, Jordan, additional, Stoughton, Christopher, additional, and vandenBerg, Jan, additional

Published
2002
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16. Higher Order Moments of the Angular Distribution of Galaxies from Early Sloan Digital Sky Survey Data

Author

Szapudi, Istvan, primary, Frieman, Joshua A., additional, Scoccimarro, Roman, additional, Szalay, Alexander S., additional, Connolly, Andrew J., additional, Dodelson, Scott, additional, Eisenstein, Daniel J., additional, Gunn, James E., additional, Johnston, David, additional, Kent, Stephen, additional, Loveday, Jon, additional, Meiksin, Avery, additional, Nichol, Robert C., additional, Scranton, Ryan, additional, Stebbins, Albert, additional, Vogeley, Michael S., additional, Annis, James, additional, Bahcall, Neta A., additional, Brinkman, J., additional, Csabai, Istvan, additional, Doi, Mamoru, additional, Fukugita, Masataka, additional, Ivezić, Željko, additional, Kim, Rita S. J., additional, Knapp, Gillian R., additional, Lamb, Don Q., additional, Lee, Brian C., additional, Lupton, Robert H., additional, McKay, Timothy A., additional, Munn, Jeff, additional, Peoples, John, additional, Pier, Jeff, additional, Rockosi, Constance, additional, Schlegel, David, additional, Stoughton, Christopher, additional, Tucker, Douglas L., additional, Yanny, Brian, additional, and York, Donald G., additional

Published
2002
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17. PRIME: probing the very early universe.

Author

Zheng, Wei, Ford, Holland C., Kruk, Jeffrey W., Tsvetanov, Zlatan I., Szalay, Alexander, Hartig, George F., Stockman, Hervey S., Postman, Marc, Voit, G. M., Shu, Peter K., Greenhouse, Matthew A., Rix, Hans-Walter, Lenzen, Rainer, Kent, Steven M., Stoughton, Christopher, Omont, Alain, and Mellier, Yannick

Published
2003
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18. Data Processing Factory for the Sloan Digital Sky Survey.

Author

Stoughton, Christopher, Adelman, Jennifer, Annis, James T., Hendry, John, Inkmann, John, Jester, Sebastian, Kent, Steven M., Kuropatkin, Nickolai, Lee, Brian, Lin, Huan, Peoples Jr., John, Sparks, Robert, Tucker, Douglas, Vanden Berk, Dan, Yanny, Brian, and Yocum, Dan

Published
2002
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19. Data acquisition systems for the Sloan Digital Sky Survey

Author

Petravick, Don, primary, Berman, Eileen, additional, Mackinnon, Bryan, additional, Nicinski, Thomas, additional, Pordes, Ruth, additional, Sergey, Gary, additional, Rechenmacher, Ron, additional, Annis, James T., additional, Kent, Steven M., additional, McKay, Timothy, additional, Stoughton, Christopher, additional, and Husby, D., additional

Published
1994
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20. Sloan Digital Sky Survey monitor telescope system

Author

Annis, James T., primary, Berman, Eileen, additional, Kent, Steven M., additional, Loveday, Jonathon, additional, McKay, Timothy, additional, Mackinnon, Bryan, additional, Munn, Jeffrey A., additional, Nicinski, Thomas, additional, Peng, Wei, additional, Petravick, Don, additional, Pordes, Ruth, additional, Rechenmacher, Ron, additional, Sergey, Gary, additional, and Stoughton, Christopher, additional

Published
1994
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21. Sloan Digital Sky Survey monitor telescope system.

Author

Annis, James T., Berman, Eileen, Kent, Steven M., Loveday, Jonathon, McKay, Timothy, Mackinnon, Bryan, Munn, Jeffrey A., Nicinski, Thomas, Peng, Wei, Petravick, Don, Pordes, Ruth, Rechenmacher, Ron, Sergey, Gary, and Stoughton, Christopher

Published
1994
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22. The Three-Dimensional Power Spectrum of Galaxies from the Sloan Digital Sky Survey

Author

Tegmark, Max, Blanton, Michael R., Strauss, Michael A., Hoyle, Fiona, Schlegel, David, Scoccimarro, Roman, Vogeley, Michael S., Weinberg, David H., Zehavi, Idit, Berlind, Andreas, Budavari, Tamas, Connolly, Andrew, Eisenstein, Daniel J., Finkbeiner, Douglas, Frieman, Joshua A., Gunn, James E., S, Andrew J., Hui, Lam, Jain, Bhuvnesh, Johnston, David, Kent, Stephen, Lin, Huan, Nakajima, Reiko, Nichol, Robert C., Ostriker, Jeremiah P., Pope, Adrian, Scranton, Ryan, Seljak, Uros, Sheth, Ravi K., Stebbins, Albert, Szalay, Alexander S., Szapudi, Istvan, Verde, Licia, Xu, Yongzhong, Annis, James, Bahcall, Neta A., Burles, Scott, Castander, Francisco J., Csabai, Istvan, Loveday, Jon, Doi, Mamoru, Fukugita, Masataka, Gott, Richard, Hennessy, Greg, Hogg, David W., Ivezic, Zeljko, Knapp, Gillian R., Lamb, Don Q., Lee, Brian C., Lupton, Robert H., McKay, Timothy A., Kunszt, Peter, Munn, Jeffrey A., O, Liam, Peoples, John, Pier, Jeffrey R., Richmond, Michael, Rockosi, Constance, Schneider, Donald P., Stoughton, Christopher, Tucker, Douglas L., Vanden, Daniel E., Yanny, Brian, York, Donald G., and SDSS, The

Abstract

We measure the large-scale real-space power spectrum P(k) by 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 matrix-based method using pseudo-Karhunen-Loeve eigenmodes, producing uncorrelated minimum-variance measurements in 22 k-bands of both the clustering power and its anisotropy due to redshift-space distortions, with narrow and well-behaved window functions in the range 0.02 h Mpc-1 < k < 0.3 h Mpc-1. We pay particular attention to modeling, quantifying, and correcting for potential systematic errors, nonlinear redshift distortions, and the artificial red-tilt caused by luminosity-dependent 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 real-space 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 < 0.1 h Mpc-1, thereby making our results useful for precision measurements of cosmological parameters in conjunction with data from other experiments such as the Wilkinson Microwave Anisotropy Probe satellite. The power spectrum is not well-characterized by a single power law but unambiguously shows curvature. As a simple characterization of the data, our measurements are well fitted by a flat scale-invariant adiabatic cosmological model with h Om = 0.213 +- 0.023 and s8 = 0.89 +- 0.02 for L* galaxies, when fixing the baryon fraction Ob/Om = 0.17 and the Hubble parameter h = 0.72; cosmological interpretation is given in a companion paper.

Published
2004

23. Karhunen-Loève Estimation of the Power Spectrum Parameters from the Angular Distribution of Galaxies in Early Sloan Digital Sky Survey Data

Author

Szalay, Alexander S., Jain, Bhuvnesh, Matsubara, Takahiko, Scranton, Ryan, Vogeley, Michael S., Connolly, Andrew, Dodelson, Scott, Eisenstein, Daniel, Frieman, Joshua A., Gunn, James E., Hui, Lam, Johnston, David, Kent, Stephen, Kerscher, Martin, Loveday, Jon, Meiksin, Avery, Narayanan, Vijay, Nichol, Robert C., O, Liam, Pope, Adrian, Scoccimarro, Roman, Sheth, Ravi K., Stebbins, Albert, Strauss, Michael A., Szapudi, Istvan, Tegmark, Max, Zehavi, Idit, Annis, James, Bahcall, Neta, Brinkmann, Jon, Csabai, Istvan, Fukugita, Masataka, Hennessy, Greg, Ivezic, Zeljko, Knapp, Gillian R., Kunszt, Peter Z., Lamb, Don Q., Lee, Brian C., Lupton, Robert H., Munn, Jeffrey R., Peoples, John, Pier, Jeffrey R., Rockosi, Constance, Schlegel, David, Stoughton, Christopher, Tucker, Douglas L., Yanny, Brian, York, Donald G., and SDSS, The

Abstract

We present measurements of parameters of the three-dimensional power spectrum of galaxy clustering from 222 square degrees of early imaging data in the Sloan Digital Sky Survey (SDSS). The projected galaxy distribution on the sky is expanded over a set of Karhunen-Loeve (KL) eigenfunctions, which optimize the signal-to-noise ratio in our analysis. A maximum likelihood analysis is used to estimate parameters that set the shape and amplitude of the three-dimensional power spectrum of galaxies in the SDSS magnitude-limited sample with r* < 21. Our best estimates are G = 0.188 +- 0.04 and s8L = 0.915 +- 0.06 (statistical errors only), for a flat universe with a cosmological constant. We demonstrate that our measurements contain signal from scales at or beyond the peak of the three-dimensional power spectrum. We discuss how the results scale with systematic uncertainties, like the radial selection function. We find that the central values satisfy the analytically estimated scaling relation. We have also explored the effects of evolutionary corrections, various truncations of the KL basis, seeing, sample size, and limiting magnitude. We find that the impact of most of these uncertainties stay within the 2 s uncertainties of our fiducial result.

Published
2003

24. The Angular Correlation Function of Galaxies from Early Sloan Digital Sky Survey Data

Author

Connolly, Andrew J., Scranton, Ryan, Johnston, David, Dodelson, Scott, Eisenstein, Daniel J., Frieman, Joshua A., Gunn, James E., Hui, Lam, Jain, Bhuvnesh, Kent, Stephen, Loveday, Jon, Nichol, Robert C., O, Liam, Postman, Marc, Scoccimarro, Roman, Sheth, Ravi K., Stebbins, Albert, Strauss, Michael A., Szalay, Alexander S., Szapudi, Istvan, Tegmark, Max, Vogeley, Michael S., Zehavi, Idit, Annis, James, Bahcall, Neta, Csabai, Istvan, Doi, Mamoru, Fukugita, Masataka, Hindsley, Robert, Ichikawa, Takashi, Ivezic, Zeljko, J, Rita S., Knapp, Gillian R., Kunszt, Peter, Lee, Brian C., Lupton, Robert H., McKay, Timothy A., Munn, Jeff, Peoples, John, Pier, Jeff, Rockosi, Constance, Schlegel, David, Stoughton, Christopher, Tucker, Douglas L., Yanny, Brian, York, Donald G., the, for, and Collaboration, SDSS

Abstract

The Sloan Digital Sky Survey is one of the first multicolor photometric and spectroscopic surveys designed to measure the statistical properties of galaxies within the local universe. In this paper we present some of the initial results on the angular two-point correlation function measured from the early SDSS galaxy data. The form of the correlation function, over the magnitude interval 18 < r* < 22, is shown to be consistent with results from existing wide-field, photographic-based surveys and narrower CCD galaxy surveys. On scales between 1' and 1deg the correlation function is well described by a power law with an exponent of [?]-0.7. The amplitude of the correlation function, within this angular interval, decreases with fainter magnitudes in good agreement with analysis from existing galaxy surveys. There is a characteristic break in the correlation function on scales of approximately 1deg-2deg. On small scales, th < 1', the SDSS correlation function does not appear to be consistent with the power-law form fitted to the 1' < th < 0.deg5 data. With a data set that is less than 2% of the full SDSS survey area, we have obtained high-precision measurements of the power-law angular correlation function on angular scales 1' < th < 1deg, which are robust to systematic uncertainties. Because of the limited area and the highly correlated nature of the error covariance matrix, these initial results do not yet provide a definitive characterization of departures from the power-law form at smaller and larger angles. In the near future, however, the area of the SDSS imaging survey will be sufficient to allow detailed analysis of the small- and large-scale regimes, measurements of higher order correlations, and studies of angular clustering as a function of redshift and galaxy type.

Published
2002

25. Analysis of Systematic Effects and Statistical Uncertainties in Angular Clustering of Galaxies from Early Sloan Digital Sky Survey Data

Author

Scranton, Ryan, Johnston, David, Dodelson, Scott, Frieman, Joshua A., Connolly, Andy, Eisenstein, Daniel J., Gunn, James E., Hui, Lam, Jain, Bhuvnesh, Kent, Stephen, Loveday, Jon, Narayanan, Vijay, Nichol, Robert C., O, Liam, Scoccimarro, Roman, Sheth, Ravi K., Stebbins, Albert, Strauss, Michael A., Szalay, Alexander S., Szapudi, Istvan, Tegmark, Max, Vogeley, Michael, Zehavi, Idit, Annis, James, Bahcall, Neta A., Brinkman, Jon, Csabai, Istvan, Hindsley, Robert, Ivezic, Zeljko, J, Rita S., Knapp, Gillian R., Lamb, Don Q., Lee, Brian C., Lupton, Robert H., McKay, Timothy, Munn, Jeff, Peoples, John, Pier, Jeff, Richards, Gordon T., Rockosi, Constance, Schlegel, David, Schneider, Donald P., Stoughton, Christopher, Tucker, Douglas L., Yanny, Brian, York, Donald G., the, for, and Collaboration, SDSS

Abstract

The angular distribution of galaxies encodes a wealth of information about large-scale structure. Ultimately, the Sloan Digital Sky Survey (SDSS) will record the angular positions of order of 108 galaxies in five bands, adding significantly to the cosmological constraints. This is the first in a series of papers analyzing a rectangular stripe of 2.deg5 x 90deg from early SDSS data. We present the angular correlation function for galaxies in four separate magnitude bins on angular scales ranging from 0.deg003 to 15deg. Much of the focus of this paper is on potential systematic effects. We show that the final galaxy catalog--with the mask accounting for regions of poor seeing, reddening, bright stars, etc.--is free from external and internal systematic effects for galaxies brighter than r* = 22. Our estimator of the angular correlation function includes the effects of the integral constraint and the mask. The full covariance matrix of errors in these estimates is derived using mock catalogs with further estimates using a number of other methods.

Published
2002

26. The Three-dimensional Power Spectrum from Angular Clustering of Galaxies in Early Sloan Digital Sky Survey Data

Author

Dodelson, Scott, Narayanan, Vijay K., Tegmark, Max, Scranton, Ryan, Budavari, Tamas, Connolly, Andrew, Csabai, Istvan, Eisenstein, Daniel, Frieman, Joshua A., Gunn, James E., Hui, Lam, Jain, Bhuvnesh, Johnston, David, Kent, Stephen, Loveday, Jon, Nichol, Robert C., O, Liam, Scoccimarro, Roman, Sheth, Ravi K., Stebbins, Albert, Strauss, Michael A., Szalay, Alexander S., Szapudi, Istvan, Vogeley, Michael S., Zehavi, Idit, Annis, James, Bahcall, Neta A., Brinkman, Jon, Doi, Mamoru, Fukugita, Masataka, Hennessy, Greg, Ivezic, Zeljko, Knapp, Gillian R., Kunszt, Peter, Lamb, Don Q., Lee, Brian C., Lupton, Robert H., Munn, Jeffrey A., Peoples, John, Pier, Jeffrey R., Rockosi, Constance, Schlegel, David, Stoughton, Christopher, Tucker, Douglas L., Yanny, Brian, and York, Donald G.

Abstract

Early photometric data from the Sloan Digital Sky Survey (SDSS) contain angular positions for 1.5 million galaxies. In companion papers, the angular correlation function w(th) and two-dimensional power spectrum Cl of these galaxies are presented. Here we invert Limber's equation to extract the three-dimensional power spectrum from the angular results. We accomplish this using an estimate of dn/dz, the redshift distribution of galaxies in four different magnitude slices in the SDSS photometric catalog. The resulting three-dimensional power spectrum estimates from w(th) and Cl agree with each other and with previous estimates over a range in wavenumbers 0.03 < k/(h Mpc-1) < 1. The galaxies in the faintest magnitude bin (21 < r* < 22, which have median redshift zm = 0.43) are less clustered than the galaxies in the brightest magnitude bin (18 < r* < 19 with zm = 0.17), especially on scales where nonlinearities are important. The derived power spectrum agrees with that of Szalay et al., who go directly from the raw data to a parametric estimate of the power spectrum. The strongest constraints on the shape parameter G come from the faintest galaxies (in the magnitude bin 21 < r* < 22), from which we infer G = 0.14img1.gif (95% CL).

Published
2002

27. Galaxy Clustering in Early Sloan Digital Sky Survey Redshift Data

Author

Zehavi, Idit, Blanton, Michael R., Frieman, Joshua A., Weinberg, David H., Mo, Houjun J., Strauss, Michael A., Anderson, Scott F., Annis, James, Bahcall, Neta A., Bernardi, Mariangela, Briggs, John W., Brinkmann, Jon, Burles, Scott, Carey, Larry, Castander, Francisco J., Connolly, Andrew J., Csabai, Istvan, Dalcanton, Julianne J., Dodelson, Scott, Doi, Mamoru, Eisenstein, Daniel, Evans, Michael L., Finkbeiner, Douglas P., Friedman, Scott, Fukugita, Masataka, Gunn, James E., Hennessy, Greg S., Hindsley, Robert B., Ivezic, Zeljko, Kent, Stephen, Knapp, Gillian R., Kron, Richard, Kunszt, Peter, Lamb, Donald Q., Leger, French, Long, Daniel C., Loveday, Jon, Lupton, Robert H., McKay, Timothy, Meiksin, Avery, Merrelli, Aronne, Munn, Jeffrey A., Narayanan, Vijay, Newcomb, Matt, Nichol, Robert C., Owen, Russell, Peoples, John, Pope, Adrian, Rockosi, Constance M., Schlegel, David, Schneider, Donald P., Scoccimarro, Roman, Sheth, Ravi K., Siegmund, Walter, Smee, Stephen, Snir, Yehuda, Stebbins, Albert, Stoughton, Christopher, SubbaRao, Mark, Szalay, Alexander S., Szapudi, Istvan, Tegmark, Max, Tucker, Douglas L., Uomoto, Alan, Vanden, Dan, Vogeley, Michael S., Waddell, Patrick, Yanny, Brian, York, Donald G., the, for, and Collaboration, SDSS

Abstract

We present the first measurements of clustering in the Sloan Digital Sky Survey (SDSS) galaxy redshift survey. Our sample consists of 29,300 galaxies with redshifts 5700 km s-1 [?] cz [?] 39,000 km s-1, distributed in several long but narrow (2.deg5-5deg) segments, covering 690 deg2. For the full, flux-limited sample, the redshift-space correlation length is approximately 8 h-1 Mpc. The two-dimensional correlation function x(rp,p) shows clear signatures of both the small-scale, "fingers-of-God" distortion caused by velocity dispersions in collapsed objects and the large-scale compression caused by coherent flows, though the latter cannot be measured with high precision in the present sample. The inferred real-space correlation function is well described by a power law, x(r) = (r/6.1 +- 0.2 h-1 Mpc)-1.75+-0.03, for 0.1 h-1 Mpc [?] r [?] 16 h-1 Mpc. The galaxy pairwise velocity dispersion is s12 [?] 600 +- 100 km s-1 for projected separations 0.15 h-1 Mpc [?] rp [?] 5 h-1 Mpc. When we divide the sample by color, the red galaxies exhibit a stronger and steeper real-space correlation function and a higher pairwise velocity dispersion than do the blue galaxies. The relative behavior of subsamples defined by high/low profile concentration or high/low surface brightness is qualitatively similar to that of the red/blue subsamples. Our most striking result is a clear measurement of scale-independent luminosity bias at r [?] 10 h-1 Mpc: subsamples with absolute magnitude ranges centered on M* - 1.5, M*, and M* + 1.5 have real-space correlation functions that are parallel power laws of slope [?]-1.8 with correlation lengths of approximately 7.4, 6.3, and 4.7 h-1 Mpc, respectively.

Published
2002

28. The Angular Power Spectrum of Galaxies from Early Sloan Digital Sky Survey Data

Author

Tegmark, Max, Dodelson, Scott, Eisenstein, Daniel J., Narayanan, Vijay, Scoccimarro, Roman, Scranton, Ryan, Strauss, Michael A., Connolly, Andrew, Frieman, Joshua A., Gunn, James E., Hui, Lam, Jain, Bhuvnesh, Johnston, David, Kent, Stephen, Loveday, Jon, Nichol, Robert C., O, Liam, Sheth, Ravi K., Stebbins, Albert, Szalay, Alexander S., Szapudi, Istvan, Vogeley, Michael S., Zehavi, Idit, Annis, James, Bahcall, Neta A., Csabai, Istvan, Doi, Mamoru, Fukugita, Masataka, Hennessy, Greg, Ivezic, Zeljko, Knapp, Gillian R., Lamb, Don Q., Lee, Brian C., Lupton, Robert H., McKay, Timothy A., Kunszt, Peter, Munn, Jeffrey A., Peoples, John, Pier, Jeffrey R., Richmond, Michael, Rockosi, Constance, Schlegel, David, Stoughton, Christopher, Tucker, Douglas L., Yanny, Brian, York, Donald G., the, for, and Collaboration, SDSS

Abstract

We compute the angular power spectrum Cl from 1.5 million galaxies in early Sloan Digital Sky Survey (SDSS) data on large angular scales, l [?] 600. The data set covers about 160 deg2, with a characteristic depth on the order of 1 h-1 Gpc in the faintest (21 < r* < 22) of our four magnitude bins. Cosmological interpretations of these results are presented in a companion paper by Dodelson and coworkers. The data in all four magnitude bins are consistent with a simple flat "concordance" model with nonlinear evolution and linear bias factors on the order of unity. Nonlinear evolution is particularly evident for the brightest galaxies. A series of tests suggests that systematic errors related to seeing, reddening, etc. are negligible, which bodes well for the 60-fold larger sample that the SDSS is currently collecting. Uncorrelated error bars and well-behaved window functions make our measurements a convenient starting point for cosmological model fitting.

Published
2002

29. Cosmological parameters from SDSS and WMAP

Author

Tegmark, Max, Strauss, Michael A., Blanton, Michael R., Abazajian, Kevork, Dodelson, Scott, Sandvik, Havard, Wang, Xiaomin, Weinberg, David H., Zehavi, Idit, Bahcall, Neta A., Hoyle, Fiona, Schlegel, David, Scoccimarro, Roman, Vogeley, Michael S., Berlind, Andreas, Budavari, Tamás, Connolly, Andrew, Eisenstein, Daniel James, Finkbeiner, Douglas, Frieman, Joshua A., Gunn, James E., Hui, Lam, Jain, Bhuvnesh, Johnston, David, Kent, Stephen, Lin, Huan, Nakajima, Reiko, Nichol, Robert C., Ostriker, Jeremiah P., Pope, Adrian, Scranton, Ryan, Seljak, Uroš, Sheth, Ravi K., Stebbins, Albert, Szalay, Alexander S., Szapudi, István, Xu, Yongzhong, Annis, James, Brinkmann, J., Burles, Scott, Castander, Francisco J., Csabai, Istvan, Loveday, Jon, Doi, Mamoru, Fukugita, Masataka, Gillespie, Bruce, Hennessy, Greg, Hogg, David W., Ivezic, Zeljko, Knapp, Gillian R., Lamb, Don Q., Lee, Brian C., Lupton, Robert H., McKay, Timothy A., Kunszt, Peter, Munn, Jeffrey A., O’Connell, Liam, Peoples, John, Pier, Jeffrey R., Richmond, Michael, Rockosi, Constance, Schneider, Donald P., Stoughton, Christopher, Tucker, Douglas L., Vanden Berk, Daniel E., Yanny, Brian, and York, Donald G.

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-CDM model without tilt (n=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 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 WMAP-only constraint on the measured age of the Universe tightens from t0~16.3+2.3-1.8 Gyr to t0~14.1+1.0-0.9 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., Astronomy

Published
2004
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