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arxiv: 0805.2366 · v5 · pith:2P54TG2Cnew · submitted 2008-05-15 · 🌌 astro-ph

LSST: from Science Drivers to Reference Design and Anticipated Data Products

\v{Z}eljko Ivezi\'c , Steven M. Kahn , J. Anthony Tyson , Bob Abel , Emily Acosta , Robyn Allsman , David Alonso , Yusra AlSayyad
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Scott F. Anderson John Andrew James Roger P. Angel George Z. Angeli Reza Ansari Pierre Antilogus Constanza Araujo Robert Armstrong Kirk T. Arndt Pierre Astier \'Eric Aubourg Nicole Auza Tim S. Axelrod Deborah J. Bard Jeff D. Barr Aurelian Barrau James G. Bartlett Amanda E. Bauer Brian J. Bauman Sylvain Baumont Andrew C. Becker Jacek Becla Cristina Beldica Steve Bellavia Federica B. Bianco Rahul Biswas Guillaume Blanc Jonathan Blazek Roger D. Blandford Josh S. Bloom Joanne Bogart Tim W. Bond Anders W. Borgland Kirk Borne James F. Bosch Dominique Boutigny Craig A. Brackett Andrew Bradshaw William Nielsen Brandt Michael E. Brown James S. Bullock Patricia Burchat David L. Burke Gianpietro Cagnoli Daniel Calabrese Shawn Callahan Alice L. Callen Srinivasan Chandrasekharan Glenaver Charles-Emerson Steve Chesley Elliott C. Cheu Hsin-Fang Chiang James Chiang Carol Chirino Derek Chow David R. Ciardi Charles F. Claver Johann Cohen-Tanugi Joseph J. Cockrum Rebecca Coles Andrew J. Connolly Kem H. Cook Asantha Cooray Kevin R. Covey Chris Cribbs Wei Cui Roc Cutri Philip N. Daly Scott F. Daniel Felipe Daruich Guillaume Daubard Greg Daues William Dawson Francisco Delgado Alfred Dellapenna Robert de Peyster Miguel de Val-Borro Seth W. Digel Peter Doherty Richard Dubois Gregory P. Dubois-Felsmann Josef Durech Frossie Economou Michael Eracleous Henry Ferguson Enrique Figueroa Merlin Fisher-Levine Warren Focke Michael D. Foss James Frank Michael D. Freemon Emmanuel Gangler Eric Gawiser John C. Geary Perry Gee Marla Geha Charles J. B. Gessner Robert R. Gibson D. Kirk Gilmore Thomas Glanzman William Glick Tatiana Goldina Daniel A. Goldstein Iain Goodenow Melissa L. Graham William J. Gressler Philippe Gris Leanne P. Guy Augustin Guyonnet Gunther Haller Ron Harris Patrick A. Hascall Justine Haupt Fabio Hernandez Sven Herrmann Edward Hileman Joshua Hoblitt John A. Hodgson Craig Hogan Dajun Huang Michael E. Huffer Patrick Ingraham Walter R. Innes Suzanne H. Jacoby Bhuvnesh Jain Fabrice Jammes James Jee Tim Jenness Garrett Jernigan Darko Jevremovi\'c Kenneth Johns Anthony S. Johnson Margaret W.G. Johnson R. Lynne Jones Claire Juramy-Gilles Mario Juri\'c Jason S. Kalirai Nitya J. Kallivayalil Bryce Kalmbach Jeffrey P. Kantor Pierre Karst Mansi M. Kasliwal Heather Kelly Richard Kessler Veronica Kinnison David Kirkby Lloyd Knox Ivan V. Kotov Victor L. Krabbendam K. Simon Krughoff Petr Kub\'anek John Kuczewski Shri Kulkarni John Ku Nadine R. Kurita Craig S. Lage Ron Lambert Travis Lange J. Brian Langton Laurent Le Guillou Deborah Levine Ming Liang Kian-Tat Lim Chris J. Lintott Kevin E. Long Margaux Lopez Paul J. Lotz Robert H. Lupton Nate B. Lust Lauren A. MacArthur Ashish Mahabal Rachel Mandelbaum Darren S. Marsh Philip J. Marshall Stuart Marshall Morgan May Robert McKercher Michelle McQueen Joshua Meyers Myriam Migliore Michelle Miller David J. Mills Connor Miraval Joachim Moeyens David G. Monet Marc Moniez Serge Monkewitz Christopher Montgomery Fritz Mueller Gary P. Muller Freddy Mu\~noz Arancibia Douglas R. Neill Scott P. Newbry Jean-Yves Nief Andrei Nomerotski Martin Nordby Paul O'Connor John Oliver Scot S. Olivier Knut Olsen William O'Mullane Sandra Ortiz Shawn Osier Russell E. Owen Reynald Pain Paul E. Palecek John K. Parejko James B. Parsons Nathan M. Pease J. Matt Peterson John R. Peterson Donald L. Petravick M.E. Libby Petrick Cathy E. Petry Francesco Pierfederici Stephen Pietrowicz Rob Pike Philip A. Pinto Raymond Plante Stephen Plate Paul A. Price Michael Prouza Veljko Radeka Jayadev Rajagopal Andrew P. Rasmussen Nicolas Regnault Kevin A. Reil David J. Reiss Michael A. Reuter Stephen T. Ridgway Vincent J. Riot Steve Ritz Sean Robinson William Roby Aaron Roodman Wayne Rosing Cecille Roucelle Matthew R. Rumore Stefano Russo Abhijit Saha Benoit Sassolas Terry L. Schalk Pim Schellart Rafe H. Schindler Samuel Schmidt Donald P. Schneider Michael D. Schneider William Schoening German Schumacher Megan E. Schwamb Jacques Sebag Brian Selvy Glenn H. Sembroski Lynn G. Seppala Andrew Serio Eduardo Serrano Richard A. Shaw Ian Shipsey Jonathan Sick Nicole Silvestri Colin T. Slater J. Allyn Smith R. Chris Smith Shahram Sobhani Christine Soldahl Lisa Storrie-Lombardi Edward Stover Michael A. Strauss Rachel A. Street Christopher W. Stubbs Ian S. Sullivan Donald Sweeney John D. Swinbank Alexander Szalay Peter Takacs Stephen A. Tether Jon J. Thaler John Gregg Thayer Sandrine Thomas Vaikunth Thukral Jeffrey Tice David E. Trilling Max Turri Richard Van Berg Daniel Vanden Berk Kurt Vetter Francoise Virieux Tomislav Vucina William Wahl Lucianne Walkowicz Brian Walsh Christopher W. Walter Daniel L. Wang Shin-Yawn Wang Michael Warner Oliver Wiecha Beth Willman Scott E. Winters David Wittman Sidney C. Wolff W. Michael Wood-Vasey Xiuqin Wu Bo Xin Peter Yoachim Hu Zhan (for the LSST Collaboration)
This is my paper

Pith reviewed 2026-05-17 08:58 UTC · model grok-4.3

classification 🌌 astro-ph
keywords willsurveylssttimeobservingsciencesinglesystem
0
0 comments X

The pith

LSST will image 18,000 square degrees of sky about 800 times across six bands over 10 years to a coadded depth of r~27.5, producing a public database of 40 billion objects and 32 trillion observations.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The LSST uses an 8.4 meter primary mirror and a 3.2 gigapixel camera with a 9.6 square degree field of view. It takes pairs of 15-second exposures and can cover 10,000 square degrees in one filter every three nights. The main science goals are probing dark energy and dark matter, cataloging solar system bodies, finding changing objects like exploding stars, and mapping our galaxy. Most time goes to a deep wide fast survey mode, with the rest for special projects. All data will be released publicly as a huge relational database.

Core claim

The LSST system is capable of imaging about 10,000 square degrees of sky in a single filter in three nights. The typical 5 sigma point-source depth in a single visit in r will be ~24.5 (AB). The survey will yield a coadded map to r~27.5.

Load-bearing premise

The design assumes that the 8.4m telescope, 3.2 gigapixel camera, and site conditions at Cerro Pachon will deliver the stated image quality, depth, and operational efficiency starting in 2022.

read the original abstract

(Abridged) We describe here the most ambitious survey currently planned in the optical, the Large Synoptic Survey Telescope (LSST). A vast array of science will be enabled by a single wide-deep-fast sky survey, and LSST will have unique survey capability in the faint time domain. 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 wide-field ground-based system sited at Cerro Pach\'{o}n 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, and a 3.2 Gigapixel camera. The standard observing sequence will consist of pairs of 15-second exposures in a given field, with two such visits in each pointing in a given night. With these repeats, the LSST system is capable of imaging about 10,000 square degrees of sky in a single filter in three nights. The typical 5$\sigma$ point-source depth in a single visit in $r$ will be $\sim 24.5$ (AB). The project is in the construction phase and will begin regular survey operations by 2022. The survey area will be contained within 30,000 deg$^2$ with $\delta<+34.5^\circ$, and will be imaged multiple times in six bands, $ugrizy$, covering the wavelength range 320--1050 nm. About 90\% of the observing time will be devoted to a deep-wide-fast survey mode which will uniformly observe a 18,000 deg$^2$ region about 800 times (summed over all six bands) during the anticipated 10 years of operations, and yield a coadded map to $r\sim27.5$. The remaining 10\% of the observing time will be allocated to projects such as a Very Deep and Fast time domain survey. The goal is to make LSST data products, including a relational database of about 32 trillion observations of 40 billion objects, available to the public and scientists around the world.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 2 minor

Summary. The paper claims to describe the science drivers, reference design, and anticipated data products for the LSST, a wide-field optical survey telescope. It links four science themes to specific technical specifications including an 8.4 m primary mirror, 9.6 deg² field of view, 3.2 Gigapixel camera, and a survey plan with 15 s exposures in pairs, achieving coverage of 10,000 square degrees in three nights per filter, single-visit depth ~24.5 in r, and coadded depth ~27.5 over 18,000 deg² with 800 visits in 10 years, producing a database of 32 trillion observations.

Significance. If realized, the LSST will provide transformative data for dark energy studies, solar system science, transient detection, and galactic structure. The paper's value lies in its comprehensive mapping of science requirements to engineering targets and quantitative performance predictions, serving as a key planning document for the project.

major comments (1)
  1. [Abstract] The assertion that the LSST system can image about 10,000 square degrees of sky in a single filter in three nights is central to the survey strategy but is stated without reference to the underlying calculation of visit times, slew times, or efficiency factors; including a brief derivation or table of time budget in the main text would substantiate this claim.
minor comments (2)
  1. The abstract mentions 'the project is in the construction phase' but the paper date is 2008; update any timeline references if this is a revised version.
  2. [Abstract] Clarify the distinction between the total survey area of 30,000 deg² and the main deep-wide-fast survey area of 18,000 deg² early in the text for better readability.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful review and positive recommendation for minor revision. We address the single major comment below.

read point-by-point responses

  1. Referee: [Abstract] The assertion that the LSST system can image about 10,000 square degrees of sky in a single filter in three nights is central to the survey strategy but is stated without reference to the underlying calculation of visit times, slew times, or efficiency factors; including a brief derivation or table of time budget in the main text would substantiate this claim.

    Authors: We agree that a brief time budget would strengthen the presentation of this key performance metric. Although the observing sequence, exposure times, and overall survey efficiency are described in the body of the manuscript, we will add a concise derivation or summary table in the revised main text (near the description of the standard observing sequence) that accounts for the 15 s exposure pairs, slew and settle times, camera readout overhead, and net efficiency. This addition will directly support the stated capability of covering approximately 10,000 square degrees in three nights per filter. revision: yes

Circularity Check

0 steps flagged

No significant circularity; design parameters follow from external requirements

full rationale

The paper is a 2008 reference design document that consolidates independent science drivers (dark energy, Solar System inventory, transients, Milky Way mapping) and technical constraints (8.4 m aperture, 9.6 deg² FOV, 15 s exposures, Cerro Pachón site) into concrete survey specifications. Quantities such as 10,000 deg² coverage in three nights, single-visit 5σ depth ~24.5 in r, and coadded depth r~27.5 are direct arithmetic consequences of those stated inputs plus operational efficiency assumptions; they are not fitted to or defined in terms of the survey's own future data products. No equations, self-citations, or ansatzes create definitional loops or rename known results as novel derivations. The chain is self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The design rests on standard assumptions about telescope performance and site quality drawn from prior engineering studies; no new entities are postulated.

free parameters (2)
  • Number of summed visits
    Design choice of approximately 800 visits across bands to meet depth and time-domain requirements for the main science themes.
  • Coadded depth target
    Target of r~27.5 set by science requirements for faint-object detection rather than derived from first principles.
axioms (1)
  • domain assumption The 8.4 m primary mirror and 3.2 gigapixel camera will achieve the stated single-visit depth and image quality under Cerro Pachon conditions.
    Invoked when stating the 5-sigma depth of ~24.5 in r and overall survey performance.

pith-pipeline@v0.9.0 · 7229 in / 1259 out tokens · 63698 ms · 2026-05-17T08:58:01.567908+00:00 · methodology

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