Abstract
We describe here the most ambitious survey currently planned in the optical, the Large Synoptic Survey Telescope (LSST). The LSST design is driven by four main science themes: probing dark energy and dark matter, taking an inventory of the solar system, exploring the transient optical sky, and mapping the Milky Way. LSST will be a large, wide-field ground-based system designed to obtain repeated images covering the sky visible from Cerro Pachón in northern Chile. The telescope will have an 8.4 m (6.5 m effective) primary mirror, a 9.6 deg 2 field of view, a 3.2-gigapixel camera, and six filters (ugrizy) covering the wavelength range 320-1050 nm. The project is in the construction phase and will begin regular survey operations by 2022. About 90% of the observing time will be devoted to a deep-wide-fast survey mode that will uniformly observe a 18,000 deg 2 region about 800 times (summed over all six bands) during the anticipated 10 yr of operations and will yield a co-added map to r ∼27.5. These data will result in databases including about 32 trillion observations of 20 billion galaxies and a similar number of stars, and they will serve the majority of the primary science programs. The remaining 10% of the observing time will be allocated to special projects such as Very Deep and Very Fast time domain surveys, whose details are currently under discussion. We illustrate how the LSST science drivers led to these choices of system parameters, and we describe the expected data products and their characteristics.
| Original language | English (US) |
|---|---|
| Article number | 111 |
| Journal | Astrophysical Journal |
| Volume | 873 |
| Issue number | 2 |
| DOIs | |
| State | Published - Mar 10 2019 |
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
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In: Astrophysical Journal, Vol. 873, No. 2, 111, 10.03.2019.
Research output: Contribution to journal › Article › peer-review
TY - JOUR
T1 - LSST
T2 - From Science Drivers to Reference Design and Anticipated Data Products
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AU - Tyson, J. Anthony
AU - Abel, Bob
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AU - Araujo, Constanza
AU - Armstrong, Robert
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AU - Burke, David L.
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AU - Charles-Emerson, Glenaver
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AU - Chow, Derek
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AU - Peyster, Robert De
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AU - Digel, Seth W.
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AU - Dubois, Richard
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AU - Durech, Josef
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AU - Moeyens, Joachim
AU - Moolekamp, Fred E.
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AU - Nief, Jean Yves
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AU - O'Mullane, William
AU - Ortiz, Sandra
AU - Osier, Shawn
AU - Owen, Russell E.
AU - Pain, Reynald
AU - Palecek, Paul E.
AU - Parejko, John K.
AU - Parsons, James B.
AU - Pease, Nathan M.
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AU - Petravick, Donald L.
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AU - Petry, Cathy E.
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AU - Ridgway, Stephen T.
AU - Riot, Vincent J.
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AU - Robinson, Sean
AU - Roby, William
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AU - Rosing, Wayne
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AU - Russo, Stefano
AU - Saha, Abhijit
AU - Sassolas, Benoit
AU - Schalk, Terry L.
AU - Schellart, Pim
AU - Schindler, Rafe H.
AU - Schmidt, Samuel
AU - Schneider, Donald P.
AU - Schneider, Michael D.
AU - Schoening, William
AU - Schumacher, German
AU - Schwamb, Megan E.
AU - Sebag, Jacques
AU - Selvy, Brian
AU - Sembroski, Glenn H.
AU - Seppala, Lynn G.
AU - Serio, Andrew
AU - Serrano, Eduardo
AU - Shaw, Richard A.
AU - Shipsey, Ian
AU - Sick, Jonathan
AU - Silvestri, Nicole
AU - Slater, Colin T.
AU - Smith, J. Allyn
AU - Smith, R. Chris
AU - Sobhani, Shahram
AU - Soldahl, Christine
AU - Storrie-Lombardi, Lisa
AU - Stover, Edward
AU - Strauss, Michael A.
AU - Street, Rachel A.
AU - Stubbs, Christopher W.
AU - Sullivan, Ian S.
AU - Sweeney, Donald
AU - Swinbank, John D.
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AU - Tice, Jeffrey
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AU - Turri, Max
AU - Berg, Richard Van
AU - Berk, Daniel Vanden
AU - Vetter, Kurt
AU - Virieux, Francoise
AU - Vucina, Tomislav
AU - Wahl, William
AU - Walkowicz, Lucianne
AU - Walsh, Brian
AU - Walter, Christopher W.
AU - Wang, Daniel L.
AU - Wang, Shin Yawn
AU - Warner, Michael
AU - Wiecha, Oliver
AU - Willman, Beth
AU - Winters, Scott E.
AU - Wittman, David
AU - Wolff, Sidney C.
AU - Wood-Vasey, W. Michael
AU - Wu, Xiuqin
AU - Xin, Bo
AU - Yoachim, Peter
AU - Zhan, Hu
N1 - Publisher Copyright: © 2019. The American Astronomical Society. All rights reserved..
PY - 2019/3/10
Y1 - 2019/3/10
N2 - We describe here the most ambitious survey currently planned in the optical, the Large Synoptic Survey Telescope (LSST). The LSST design is driven by four main science themes: probing dark energy and dark matter, taking an inventory of the solar system, exploring the transient optical sky, and mapping the Milky Way. LSST will be a large, wide-field ground-based system designed to obtain repeated images covering the sky visible from Cerro Pachón in northern Chile. The telescope will have an 8.4 m (6.5 m effective) primary mirror, a 9.6 deg 2 field of view, a 3.2-gigapixel camera, and six filters (ugrizy) covering the wavelength range 320-1050 nm. The project is in the construction phase and will begin regular survey operations by 2022. About 90% of the observing time will be devoted to a deep-wide-fast survey mode that will uniformly observe a 18,000 deg 2 region about 800 times (summed over all six bands) during the anticipated 10 yr of operations and will yield a co-added map to r ∼27.5. These data will result in databases including about 32 trillion observations of 20 billion galaxies and a similar number of stars, and they will serve the majority of the primary science programs. The remaining 10% of the observing time will be allocated to special projects such as Very Deep and Very Fast time domain surveys, whose details are currently under discussion. We illustrate how the LSST science drivers led to these choices of system parameters, and we describe the expected data products and their characteristics.
AB - We describe here the most ambitious survey currently planned in the optical, the Large Synoptic Survey Telescope (LSST). The LSST design is driven by four main science themes: probing dark energy and dark matter, taking an inventory of the solar system, exploring the transient optical sky, and mapping the Milky Way. LSST will be a large, wide-field ground-based system designed to obtain repeated images covering the sky visible from Cerro Pachón in northern Chile. The telescope will have an 8.4 m (6.5 m effective) primary mirror, a 9.6 deg 2 field of view, a 3.2-gigapixel camera, and six filters (ugrizy) covering the wavelength range 320-1050 nm. The project is in the construction phase and will begin regular survey operations by 2022. About 90% of the observing time will be devoted to a deep-wide-fast survey mode that will uniformly observe a 18,000 deg 2 region about 800 times (summed over all six bands) during the anticipated 10 yr of operations and will yield a co-added map to r ∼27.5. These data will result in databases including about 32 trillion observations of 20 billion galaxies and a similar number of stars, and they will serve the majority of the primary science programs. The remaining 10% of the observing time will be allocated to special projects such as Very Deep and Very Fast time domain surveys, whose details are currently under discussion. We illustrate how the LSST science drivers led to these choices of system parameters, and we describe the expected data products and their characteristics.
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UR - http://www.scopus.com/inward/citedby.url?scp=85064450156&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/ab042c
DO - 10.3847/1538-4357/ab042c
M3 - Article
AN - SCOPUS:85064450156
SN - 0004-637X
VL - 873
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 111
ER -