Large Synoptic Survey Telescope: Overview

Tyson, J. Anthony

doi:10.1117/12.456772

Cited by 244 publications

(99 citation statements)

References 11 publications

(11 reference statements)

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“…The success of SDSS provides encouragement that even more ambitious surveys, such as LSST (Tyson 2002), which is expected to produce and immediately process 20 TB of data per observing night, may also be successful endeavors.…”

Section: Discussionmentioning

confidence: 99%

SDSS data management and photometric quality assessment

et al. 2004

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Abstract. We summarize the Sloan Digital Sky Survey data acquisition and processing steps, and describe runQA, a pipeline designed for automated data quality assessment. In particular, we show how the position of the stellar locus in color-color diagrams can be used to estimate the accuracy of photometric zeropoint calibration to better than 0.01 mag in 0.03 deg 2 patches. Using this method, we estimate that typical photometric zeropoint calibration errors for SDSS imaging data are not larger than ∼ 0.01 mag in the g, r, and i bands, 0.02 mag in the z band, and 0.03 mag in the u band (root-mean-scatter for zeropoint offsets).

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Section: Discussionmentioning

confidence: 99%

SDSS data management and photometric quality assessment

et al. 2004

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“…We also look forward to larger data sets with eBOSS (Zhao et al 2016), the Subaru Prime Focus Spectrograph (PFS; Takada et al 2014), DESI (Levi et al 2013), Euclid (Laureijs 2009;Laureijs et al 2011), LSST (Tyson 2002), and WFIRST (Spergel et al 2013a,b) that can be matched up to deeper imaging.…”

Section: Discussionmentioning

confidence: 99%

The Color and Stellar Mass Dependence of Small-scale Galaxy Clustering in SDSS-III BOSS

Law-Smith

Eisenstein

2017

ApJ

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We measure the color and stellar mass dependence of clustering in spectroscopic galaxies at 0.6 < z < 0.65 using data from the Baryon Oscillation Spectroscopic Survey component of the Sloan Digital Sky Survey. We greatly increase the statistical precision of our clustering measurements by using the cross-correlation of 66,657 spectroscopic galaxies to a sample of 6.6 million fainter photometric galaxies. The clustering amplitude w(R) is measured as the ratio of the mean excess number of photometric galaxies found within a specified radius annulus around a spectroscopic galaxy to that from a random photometric galaxy distribution. We recover many of the familiar trends at high signal-to-noise ratio. We find the ratio of the clustering amplitudes of red and blue massive galaxies to be w red /w blue = 1.92 ± 0.11 in our smallest annulus of 75-125 kpc. At our largest radii (2-4 Mpc), we find w red /w blue = 1.24 ± 0.05. Red galaxies therefore have denser environments than their blue counterparts at z ∼ 0.625, and this effect increases with decreasing radius. Irrespective of color, we find that w(R) does not obey a simple power-law relation with radius, showing a dip around 1 Mpc. Holding stellar mass fixed, we find a clear differentiation between clustering in red and blue galaxies, showing that clustering is not solely determined by stellar mass. Holding color fixed, we find that clustering increases with stellar mass, especially for red galaxies at small scales (more than a factor of 2 effect over 0.75 dex in stellar mass).

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“…The revolutionary progress in studies of the Milky Way kinematics enabled by the SDSS-POSS proper motion database will be maintained by the upcoming next-generation surveys, such as Pan-STARRS (Kaiser 2002) and LSST (Tyson 2002). The expected performance by Pan-STARRS is described by E. Magnier in these Proceedings.…”

Section: The Proper Motion and Parallax Accuracy Expected From Lsstmentioning

confidence: 99%

Astrometry with digital sky surveys: from SDSS to LSST

et al. 2007

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Abstract. Major advances in our understanding of the Universe have historically come from dramatic improvements in our ability to accurately measure astronomical quantities. The astrometric observations obtained by modern digital sky surveys are enabling unprecedentedly massive and robust studies of the kinematics of the Milky Way. For example, the astrometric data from the Sloan Digital Sky Survey (SDSS), together with half a century old astrometry from the Palomar Observatory Sky Survey (POSS), have enabled the construction of a catalog that includes absolute proper motions as accurate as 3 mas/year for about 20 million stars brighter than V=20, and for 80,000 spectroscopically confirmed quasars which provide exquisite error assessment. We discuss here several ongoing studies of Milky Way kinematics based on this catalog. The upcoming next-generation surveys will maintain this revolutionary progress. For example, we show using realistic simulations that the Large Synoptic Survey Telescope (LSST) will measure proper motions accurate to 1 mas/year to a limit 4 magnitude fainter than possible with SDSS and POSS catalogs, or with the Gaia survey. LSST will also obtain geometric parallaxes with accuracy similar to Gaia's at its faint end (0.3 mas at V=20), and extend them to V=24 with an accuracy of 3 mas. We discuss the impact that these LSST measurements will have on studies of the Milky Way kinematics, and potential synergies with the Gaia survey.

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Large Synoptic Survey Telescope: Overview

Cited by 244 publications

References 11 publications

SDSS data management and photometric quality assessment

SDSS data management and photometric quality assessment

The Color and Stellar Mass Dependence of Small-scale Galaxy Clustering in SDSS-III BOSS

Astrometry with digital sky surveys: from SDSS to LSST

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