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

In the paper

“The effective étendue for LSST will be greater than 300 m 2 deg 2 , which is more than an order of magnitude larger than that of any existing facility.”

In the paper

“Detailed simulations of WL techniques show that imaging over ∼ 20,000 deg 2 to a 5 σ pointsource depth of r AB ∼ 27.5 gives adequate signal to measure shapes for of order 2 billion galaxies for WL.”

In the paper

“The constants Cm depend on the overall throughput of the instrument and are computed using our current best throughput estimates for optical elements and sensors.”

In the paper

“Systematic and random errors become similar at about r = 22, and there are about 100 stars per LSST sensor ( 0.05 deg 2 ) to this depth ( and fainter than the LSST saturation limit at r ∼ 16 ) even at the Galactic poles.”

In the paper

“If these fi elds were selected at Galactic latitudes of b 30 ~ ∣ ∣ ° , they would include about 10 million stars with r < 21 observed with S / N above 100 in each visit.”

In the paper

“Each 15 s exposure in a sequence would have an equivalent 5 σ depth of r ∼ 24, and each fi lter subsequence when co-added would be 2 mag deeper than the main survey visits ( r ∼ 26.5 ) .”

In the paper

“Again, this effect is only substantial in the u band, as demonstrated by the values of C 2 m t D = ( ) listed in Table 2.”

In the paper

“Blue stars ( e.g., F / G stars ) fainter than r ∼ 23 will have about 50% larger proper-motion and parallax errors than given in the table, due to decreased numbers of z - and y -band detections.”

In the paper

“The anticipated total number of visits for a 10 yr LSST survey is about 2.45 million ( ∼ 4.9 million 15 s long exposures, summing over the six fi lters ) .”

In the paper

“Considering this ' extended ' LSST in the context of existing / ongoing surveys would result in a system-wide cumulative completeness of 86% for PHAs ( 77% for NEOs ) , approaching the 90% required by the congressional mandate ( see bottom panels of Figure 20 ) .”

In the paper

“By improving MOPS and increasing the MOPS linking window from 15 to 30 days, we can boost completeness by about 3%.”

In the paper

“In all six bands they imply single-visit depths m 5 ( also listed in Table 2 ) that lie between the minimum and design speci fi cation values from the SRD listed in Table 1.”

In the paper

“Taking weather into account, the selected fi elds would each have on average about 40 hr long sequences of 200 exposures each.”

In the paper

“The impact on red stars is smaller, due to a relatively small number of observations in the u and g bands, but extremely red objects, such as L and T dwarfs, will de fi nitely have larger errors, depending on details of their SEDs.”

In the paper

“Realistic MOPS simulations show > 99% linking ef fi ciency across all classes of solar system objects ( Denneau et al. 2013 ) , and at least 93% ef fi ciency for NEOs ( Vere š & Chesley 2017a, 2017b ) .”

What the sources say

• Not checked yetcites Denneau et al. 2013 source
• Not checked yetcites Vereš & Chesley 2017a, 2017b

In the paper

“After the fi rst 3 yr of the survey, the proper-motion errors will be about fi ve times as large, and parallax errors will be about twice as large, as the values given in Table 3; the errors scale as t -3 / 2 and t -1 / 2 , respectively.”

In the paper

“When all 40 sequences and the main survey visits are co-added, they would extend the depth to r ∼ 28.”

In the paper

“These fi gures are likely to be uncertain at the level of ± 5%, due to uncertainties in the orbital distribution of the true population, the size distribution, uncertain distributions of shape ( and thus light-curve variations ) , and surface properties ( thus colors and albedo ) , plus variations in survey cadence due to weather, etc.”

In the paper

“Accounting for readout time and fi lter changes, it could obtain about 50 consecutive 15 s exposures in each of four fi lters in an hour.”

In the paper

“This cadence spends 6% of the total observing time on NEO-optimized observations north of δ = + 5 ° , and MOPS links objects with windows of 15 days.”

In the paper

“For the nominal exposure time of 30 s and θ = 0 7, the loss of limiting magnitude is 0.04 mag for v = 0 ° . 25 day -1 , typical for objects in the main asteroid belt, and 0.46 mag for v = 1 ° . 0 day -1 , typical of PHAs passing near Earth.”

In the paper

“The overwhelming majority of the almost 8000 refereed papers based on SDSS data to date have been written by scientists from outside the project”

In the paper

“As of 2017, 34 institutions from 23 countries have signed Memoranda of Agreement to contribute signi fi cantly to the LSST operating costs, in exchange for participation in the science collaborations and data access.”

In the paper

“The LSST science collaborations in particular have helped develop the LSST science case and continue to provide advice on how to optimize their science”

In the paper

“there are over 800 participants in these collaborations.”

In the paper

“The project is in the construction phase and will begin regular survey operations by 2022.”

• Also stated in: § 1. Introduction · p. 3

  “the 10 yr sky survey is projected to begin in 2022.”

In the paper

“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.”

What the sources say

• Not checked yetcites Science Working Group of the LSST & Strauss 2004

In the paper

“LSST will be a large, wide- fi eld ground-based system designed to obtain repeated images covering the sky visible from Cerro Pachón in northern Chile.”

• Also stated in: § 1. Introduction · p. 3

  “Located on Cerro Pachón in northern Chile, the LSST will be a large, widefi eld, ground-based telescope designed to obtain multiband images over a substantial fraction of the sky every few nights.”

In the paper

“The telescope will have an 8.4 m ( 6.5 m effective ) primary mirror, a 9.6 deg 2 fi eld of view, a 3.2-gigapixel camera, and six fi lters ( ugrizy ) covering the wavelength range 320 -1050 nm.”

In the paper

“Distinguishing competing models for the physical nature of dark energy, or alternative explanations involving modi fi cations of the general theory of relativity, will require percent-level measurements of both the cosmic expansion and the growth of dark matter structure as a function of redshift.”

In the paper

“and will yield a co-added map to r ∼ 27.5.”

In the paper

“Photometric repeatability should achieve 5 mmag precision at the bright end, with zero-point stability across the sky of 10 mmag and band-to-band calibration errors not larger than 5 mmag.”

In the paper

“SNe Ia provided the fi rst robust evidence that the expansion of the universe is accelerating”

What the sources say

• Not checked yetcites Riess et al. 1998 source
• Not checked yetcites Perlmutter et al. 1999 source

In the paper

“Unlike other cosmological probes, even a single object gives information on the relationship between redshift and distance.”

In the paper

“Thus, a large number of SNe across the sky allows one to search for any dependence of dark energy properties on direction, which would be an indicator of new physics.”

In the paper

“We illustrate how the LSST science drivers led to these choices of system parameters”

• Also stated in: § 1. Introduction · p. 4

  “The purpose of this paper is to provide an overall summary of the main LSST science drivers and how they led to the current system design parameters”

In the paper

“WL techniques can be used to map the distribution of mass as a function of redshift and thereby trace the history of both the expansion of the universe and the growth of structure”

What the sources say

• Not checked yetcites Hu & Tegmark 1999
• Not checked yetcites Kilbinger 2015 source
• Not checked yetcites Mandelbaum 2018 source

In the paper

“Current models of cosmology require the existence of both dark matter and dark energy to match observational constraints”

What the sources say

• Not checked yetcites Riess et al. 2007 source
• Not checked yetcites Komatsu et al. 2009 source
• Not checked yetcites Percival et al. 2010 source

In the paper

“The results from this method can be compared with similar measures of anisotropy from the combination of WL and LSS ( Zhan et al. 2009 ) .”

What the sources say

• Not checked yetcites Zhan et al. 2009 source

In the paper

“Given the expected SN fl ux distribution at the redshifts where dark energy is important, the single-visit depth should be at least r ∼ 24.”

In the paper

“Image quality should maintain the limit set by the atmosphere ( the median free-air seeing is 0 65 in the r band at the chosen site; see Figure 1 ) and not be degraded appreciably by the hardware.”

In the paper

“We note that the Pan-STARRS project ( Kaiser et al. 2002, 2010 ) , with similar science goals to LSST, envisions a distributed aperture design, where the total system étendue is a sum of étendue values for an array of small 1.8 m telescopes.”

What the sources say

• Not checked yetcites Kaiser et al. 2002 source
• Not checked yetcites Kaiser et al. 2010 source

In the paper

“The challenge is to turn this available precision into accuracy, by careful modeling and marginalization over a variety of systematic effects”

What the sources say

• Not checked yetcites Krause & Eifler 2017

In the paper

“The Milky Way and its environment provide a unique data set for understanding the detailed processes that shape galaxy formation and for testing the smallscale predictions of our standard cosmological model.”

In the paper

“Recent surveys have shown the power of measuring variability of celestial sources for studying gravitational lensing, searching for SNe, determining the physical properties of gamma-ray burst sources, discovering gravitational wave counterparts, probing the structure of active galactic nuclei ( AGNs ) , studying variable star populations, discovering exoplanets, and many other subjects at the fore”

What the sources say

• Not checked yetcites SciBook, Chap. 8
• Not checked yetcites Law et al. 2009 source
• Not checked yetcites Djorgovski et al. 2012

In the paper

“This depth, as well as the corresponding deep surface brightness limit, optimizes the number of galaxies with measured shapes in ground-based seeing and allows their detection in signi fi cant numbers to beyond a redshift of two.”

In the paper

“To fully exploit the SN science potential, light curves sampled in multiple bands every few days over the course of a few months are required.”

In the paper

“The cross-correlation of the three-dimensional mass distribution -as probed by neutral hydrogen in CHIME ( Newburgh et al. 2014 ) , HIRAX ( Newburgh et al. 2016 ) , or SKA, or galaxies in DESI and PFS -with the gravitational growth probed by tomographic shear in LSST will be a complementary way to constrain dark energy properties beyond simply characterizing its equation of state and to test the”

In the paper

“Carrying out these K -corrections requires that the calibration of the relative offsets in photometric zero-points between fi lters and the system response functions, especially near the edges of bandpasses, be accurate to about 1% ( Wood-Vasey et al. 2007 )”

What the sources say

• Not checked yetcites Wood-Vasey et al. 2007 source

In the paper

“Large survey volumes are key to probing dynamical dark energy models ( with subhorizon dark energy clustering or anisotropic stresses ) .”

In the paper

“Therefore, the most robust cosmological constraints are the result of using interlocking combinations of probes.”

In the paper

“In order to control systematic errors in shear measurement, the desired depth must be achieved with many short exposures”

In the paper

“Deeper data ( r > 26 ) for small areas of the sky can extend the discovery of SNe to a mean redshift of 0.7 ( from ∼ 0.5 for the main survey ) , with some objects beyond z ∼ 1 ( Garnavich et al. 2004; Pinto et al. 2004; SciBook, Chap. 11 ) .”

What the sources say

• Not checked yetcites Garnavich et al. 2004
• Not checked yetcites Pinto et al. 2004
• Not checked yetcites SciBook, Chap. 11

In the paper

“rather than simply co-adding all images in a given region of sky, the individual exposures, each with their own PSF and noise characteristics, should be analyzed simultaneously to optimally measure the shapes of galaxies”

What the sources say

• Not checked yetcites Tyson et al. 2008
• Not checked yetcites Jee & Tyson 2011

In the paper

“The single-visit depth should reach r ∼ 24.5.”

• Also stated in: § 2.1.2. Taking an Inventory of the Solar System · p. 6

  “The images should reach a depth of at least 24.5 ( 5 σ for point sources ) in the r band to reach high completeness down to the 140 m mandate for NEOs.”

• Also stated in: § 2.2.1. The Aperture Size · p. 9

  “the depth of a single visit, r ∼ 24.5”

In the paper

“Three of the primary dark energy probes, WL, LSS, and SN, provide unique and independent constraints on the LSST system design ( SciBook, Chaps. 11 -15 ) .”

What the sources say

• Not checked yetcites SciBook, Chaps. 11-15

In the paper

“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”

In the paper

“Analyzing these data will require sophisticated data processing techniques.”

In the paper

“A major challenge in extragalactic cosmology today concerns the formation of structure on subgalactic scales, where baryon physics becomes important, and the nature of dark matter may manifest itself in observable ways ( e.g., Weinberg et al. 2015 ) .”

What the sources say

• Not checked yetcites Weinberg et al. 2015 source

In the paper

“This is essential to search for systematic differences in SN populations ( e.g., due to differing progenitor channels ) , which may masquerade as cosmological effects, as well as to determine photometric redshifts from the SNe themselves.”

In the paper

“The strongest constraints on the LSST image quality arise from this science program.”

In the paper

“Observations in at least fi ve photometric bands will allow proper K -corrected light curves to be measured over a range of redshift.”

In the paper

“Measurements of cosmic shear as a function of redshift allow determination of angular distances versus cosmic time, providing multiple independent constraints on the nature of dark energy.”

In the paper

“About 90% of the observing time will be devoted to a deep-wide-fast survey mode”

• Also stated in: § 2. From Science Drivers to Reference Design · p. 4

  “About 90% of the observing time will be devoted to a deep-wide-fast ( main ) survey mode.”

In the paper

“Good image quality is required to separate SN photometrically from their host galaxies.”

In the paper

“These investigations require deep wide-area multicolor imaging with stringent requirements on shear systematics in at least two bands, and excellent photometry in at least fi ve bands to measure photometric redshifts”

In the paper

“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.”

In the paper

“The most powerful probes include weak gravitational lens cosmic shear ( weak lensing ( WL )) , galaxy clustering and baryon acoustic oscillations ( large-scale structure, LSS ) , the mass function and clustering of clusters of galaxies, time delays in lensed quasar and supernova ( SN ) systems, and photometry of Type Ia SNe -all as functions of redshift.”

In the paper

“The LSST fi lter complement ( ugrizy ; see Figure 4 ) is modeled after the SDSS system ( Fukugita et al. 1996 ) because of its demonstrated success in a wide variety of applications, including photometric redshifts of galaxies ( Budavári et al. 2003 ) , separation of stellar populations ( Lenz et al. 1998; Helmi et al. 2003 ) , and photometric selection of quasars ( Richards et al. 2002; Ross et”

What the sources say

• Not checked yetcites Fukugita et al. 1996 source
• Not checked yetcites Budavári et al. 2003 source
• Not checked yetcites Lenz et al. 1998 source

In the paper

“In times of good seeing and at low air mass, preference is given to r - and i -band observations.”

In the paper

“The single-visit exposure time should be less than about a minute to prevent trailing of fast-moving objects and to aid control of various systematic effects induced by the atmosphere. It should be longer than ∼ 20 s to avoid signi fi cant ef fi ciency losses due to fi nite readout, slew time, and read noise.”

In the paper

“The total number of visits of any given area of sky, when accounting for all fi lters, should be of the order of 1000, as mandated by WL science, the search for NEOs, and proper-motion and trigonometric parallax measurements.”

In the paper

“The distribution of visits per filter should enable accurate photometric redshifts, separation of stellar populations, and suf fi cient depth to enable detection of faint extremely red sources ( e.g., brown dwarfs and high-redshift quasars ) .”

In the paper

“The remaining 10% of the observing time will be used to obtain improved coverage of parameter space such as very deep ( r ∼ 26 ) observations, observations with very short revisit times ( ∼ 1 minute ) , and observations of ' special ' regions such as the ecliptic plane, Galactic plane, and the Large and Small Magellanic Clouds.”

In the paper

“To maintain ef fi ciency losses below ∼ 30% ( i.e., at least below the limit set by the weather patterns ) , and to minimize the read noise impact, t vis > 20 s is required.”

In the paper

“A primary mirror effective diameter of ∼ 6.5 m. With the adopted optical design, described below, this effective diameter corresponds to a geometrical diameter of ∼ 8 m. Motivated by characteristics of the existing equipment at the Steward Mirror Laboratory, which fabricated the primary mirror, the adopted geometrical diameter is set to 8.4 m.”

In the paper

“Additional coverage of a crescent within 10 degrees of the northern ecliptic plane would sample the full azimuthal distribution of KBOs, crucial for understanding the different dynamical families in which they fall.”

In the paper

“The ranking criteria also ensure that the visits to each fi eld are widely distributed in position angle on the sky and rotation angle of the camera in order to minimize systematic effects in galaxy shape determination.”

In the paper

“In addition, the LSST system will explicitly measure the atmospheric transmission spectrum associated with each image acquired.”

In the paper

“Extensive precursor data including the SDSS data set and our own data obtained using telescopes close to the LSST site of Cerro Pachón ( e.g., the SOAR and Gemini South telescopes ) , as well as telescopes of similar aperture ( e.g., Subaru ) , indicate that the photometric and astrometric accuracy will be limited not by our instrumentation or software, but rather by atmospheric effects.”

In the paper

“In order to measure the tangential velocity of stars at a distance of 10 kpc, where the halo dominates over the disk, to within 10 km s -1 ( comparable to the accuracy of large-scale radial velocity surveys ) , the proper-motion accuracy should be 0.2 mas yr -1 or better.”

In the paper

“For this reason, the sky area for the main survey is maximized to its practical limit, 18,000 deg 2 , determined by the requirement to avoid air masses less than 1.5, which would substantially deteriorate the image quality and the survey depth ( see Equation ( 6 )) .”

In the paper

“The overall photometric calibration philosophy ( Stubbs & Tonry 2006 ) is to measure explicitly, at 1 nm resolution, the instrumental sensitivity as a function of wavelength using light from a monochromatic source injected into the telescope pupil.”

What the sources say

• Not checked yetcites Stubbs & Tonry 2006

In the paper

“The data collected by the LSST system will be automatically reduced to scienti fi cally useful catalogs and images by the LSST Data Management ( DM; Juri ć et al. 2017a ) system.”

What the sources say

• Not checked yetcites Jurić et al. 2017a

In the paper

“Data processing, data products, and data access should result in data products that approach the statistical uncertainties in the raw data, i.e., the processing must be close to optimal. To enable fast and ef fi cient response to transient sources, the processing latency for variable sources should be less than a minute, with a robust and accurate preliminary characterization of all reported vari”

In the paper

“The chosen fi lter complement corresponds to a design ' sweet spot. '”

In the paper

“A visit exposure time of 30 s ( using two 15 s exposures to ef fi ciently reject cosmic rays; the possibility of a single exposure per visit, to improve observing ef fi ciency, will be investigated during the commissioning phase ) , yielding ò = 77%.”

In the paper

“Thus, we plan to extend the universal cadence to this region using the r and i fi lters only, along with more relaxed limits on air mass and seeing.”

In the paper

“We present here a speci fi c realization, the so-called ' universal cadence, ' which yields the main deep-wide-fast survey and meets our core science goals.”

In the paper

“Such an instrument would probe the ∼ 100 m size range at main belt distances and discover rare distant TNOs such as Sedna ( Brown et al. 2004 ) and 2012 VP113 ( Trujillo & Sheppard 2014 ) .”

What the sources say

• Not checked yetcites Brown et al. 2004 source
• Not checked yetcites Trujillo & Sheppard 2014 source

In the paper

“A system with a smaller étendue would require separate specialized surveys to address the science goals, which results in a loss of surveying ef fi ciency.”

In the paper

“As often as possible, each fi eld will be observed twice, with visits separated by 15 -60 minutes.”

In the paper

“Placing the red edge of the u band blueward of the Balmer break allows optimal separation of stars and quasars, and the telluric water absorption feature at 9500 Å effectively de fi nes the blue edge of the y band.”

In the paper

“Mapping the Galaxy requires large-area coverage; excellent image quality to maximize photometric and astrometric accuracy, especially in crowded fi elds; photometric precision of at least 1% to separate main-sequence and giant stars ( e.g., Helmi et al. 2003 ) , as well as to identify variable stars such as RR Lyrae ( Sesar et al. 2010; Sharma et al. 2011 ) ; and systematic astrometric errors not”

What the sources say

• Not checked yetcites Helmi et al. 2003 source
• Not checked yetcites Sesar et al. 2010 source
• Not checked yetcites Sharma et al. 2011 source

In the paper

“The adopted survey lifetime of 10 yr is a compromise between a shorter time, which leads to an excessively large and expensive mirror ( 15 m for a 3 yr survey and 12 m for a 5 yr survey ) and not as effective proper-motion measurements, and a smaller telescope, which would require more time to complete the survey, with the associated increase in operations cost.”

In the paper

“This strategy will provide motion vectors to link detections of moving objects in the solar system and fi ne-time sampling for measuring short-period variability.”

In the paper

“The extension of the SDSS system to longer wavelengths ( the y band at ∼ 1 μ m ) is driven by the increased effective redshift range achievable with the LSST, due to deeper imaging; the desire to study substellar objects, high-redshift quasars, and regions of the Galaxy that are obscured by interstellar dust; and the scienti fi c opportunity enabled by modern CCDs with high quantum ef fi ciency in”

In the paper

“The vast majority ( about 90% ) of the observing time will be devoted to a deepwide-fast survey mode of the sort we have just described, with the remaining 10% allocated to special programs that will also address multiple science goals.”

In the paper

“Indeed, any one of the four main science drivers could be removed, and the remaining three would still yield very similar requirements for most system parameters.”

In the paper

“The co-added survey depth should reach r ∼ 27.5, with suf fi cient signal-to-noise ratio ( S / N ) in other bands to address both extragalactic and Galactic science drivers.”

In the paper

“Astrometric calibration will be based on the results from the Gaia mission ( Lindegren et al. 2018 ) , which will provide numerous high-accuracy astrometric standards in every LSST fi eld.”

What the sources say

• Not checked yetcites Lindegren et al. 2018 source

In the paper

“Remarkably, even with these joint requirements, none of the individual science programs are severely overdesigned, i.e., despite their signi fi cant scienti fi c diversity, these programs are highly compatible in terms of desired data characteristics.”

In the paper

“The filter complement should include at least six fi lters in the wavelength range limited by atmospheric absorption and silicon detection ef fi ciency ( 320 -1050 nm ) , with roughly rectangular fi lters and no large gaps in the coverage, in order to enable robust and accurate photometric redshifts and stellar typing.”

In the paper

“The images must be well sampled to enable accurate astrometry, with absolute accuracy of at least 0 1 in order to measure orbital parameters of TNOs with enough precision to constrain theoretical models and enable prediction of occultations.”

In the paper

“In summary, given the science requirements as stated here, there is a minimum étendue of ∼ 300 deg 2 m 2 , which enables our seemingly disparate science goals to be addressed with a single data set.”

In the paper

“Individual exposures should be shorter than about 30 s to minimize the effects of trailing for the majority of moving objects.”

In the paper

“A dedicated 1.2 m auxiliary calibration telescope will obtain spectra of standard stars in LSST fi elds, calibrating the atmospheric throughput as a function of wavelength ( Stubbs et al. 2007; see Figures 5 and 6 ) .”

What the sources say

• Not checked yetcites Stubbs et al. 2007 source

In the paper

“These three requirements place a fi rm upper limit on the optimal visit exposure time of t vis < 40 s.”

In the paper

“Precise determination of the PSF across each image, accurate photometric and astrometric calibration, and continuous monitoring of system performance and observing conditions will be needed to reach the full potential of the LSST mission.”

In the paper

“The congressional mandate can be ful fi lled with a 10 m class telescope equipped with a multi-gigapixel camera and a sophisticated and robust data processing system ( Ivezi ć et al. 2007b ) .”

What the sources say

• Not checked yetcites Ivezić et al. 2007b

In the paper

“The main deep-wide-fast survey will use about 90% of the observing time.”

In the paper

“We have investigated the possibility of replacing the ugrizy system with a fi lter complement that includes only fi ve fi lters. For example, each fi lter width could be increased by 20% over the same wavelength range ( neither a shorter wavelength range nor gaps in the wavelength coverage are desirable options ) , but this option is not satisfactory.”

In the paper

“The LSST observing strategy is designed to maximize the scienti fi c throughput by minimizing slew and other downtime and by making appropriate choices of the fi lter bands given the realtime weather conditions.”

In the paper

“A revisit time of 3 days on average for 10,000 deg 2 of sky, with two visits per night.”

In the paper

“The observing strategy for the main survey will be optimized for the homogeneity of depth and number of visits.”

In the paper

“The photometric calibration should be better than 1% -2% to measure asteroids ' colors and thus determine their types.”

In the paper

“To summarize, the chosen primary mirror diameter is the minimum diameter that simultaneously satis fi es the depth ( r ∼ 24.5 for single visit and r ∼ 27.5 for co-added depth ) and cadence ( revisit time of 3 -4 days, with 30 s per visit ) constraints described above.”

In the paper

“The universal cadence provides most of LSST ' s power for detecting NEOs and Kuiper Belt objects ( KBOs ) and naturally incorporates the southern half of the ecliptic within its 18,000 square degrees, with a decl. cut of about δ = + 2 ° .”

In the paper

“The planned calibration process decouples the establishment of a stable and uniform internal relative calibration from the task of assigning absolute optical fl ux to celestial objects.”

In the paper

“The required co-added survey depth provides a direct constraint, independent of the details of survey execution such as the exposure time per visit, on the minimum effective primary mirror diameter of 6.4 m, as illustrated in Figure 2.”

In the paper

“A larger fi eld of view would lead to unacceptable deterioration of the image quality.”

In the paper

“The revisit time distribution should enable determination of orbits of solar system objects and sample SN light curves every few days, while accommodating constraints set by proper-motion and trigonometric parallax measurements.”

In the paper

“As a last option, the riz bands could be redesigned as two wider bands. However, this option is also undesirable because the r and i bands are the primary bands for WL studies and for star / galaxy separation, and atmospheric dispersion would worsen the PSF for a wider bandpass ( e.g., at air mass of 1.3, the typical dispersion in the u , g , and r bands is 0 55, 0 46, and 0 19, respectively; if”

In the paper

“These surveys aim to extend the parameter space accessible to the main survey by going deeper or by employing different time / fi lter sampling.”

In the paper

“This error behavior is a strong independent argument for a survey lifetime of at least 10 yr ( see Section 2 ) .”

In the paper

“For example, the SN sample would be extended to redshifts of z ∼ 1.2, with more densely sampled light curves than obtained from the universal cadence.”

In the paper

“In addition to transient science, the prompt products will support discovery and follow-up of objects in the solar system.”

In the paper

“Based on SDSS experience ( Sesar et al. 2007 ) , the random photometric error for point sources, as a function of magnitude, is well described 98 by”

What the sources say

• Not checked yetcites Sesar et al. 2007 source

In the paper

“The calibration system and procedures are designed to maintain σ sys < 0.005 mag.”

In the paper

“Although the uniform treatment of the sky provided by the universal cadence proposal can satisfy the majority of LSST scienti fi c goals, roughly 10% of the time will be allocated to other strategies that signi fi cantly enhance the scienti fi c return.”

In the paper

“Another meaning of Cm D ¥ is the loss of depth at the nominal value of t vis due to fi nite readout noise.”

In the paper

“Rather, it represents a proof of concept that it is indeed possible to design a observing strategy that addresses a wide variety of science goals in a nearly optimal way.”

In the paper

“The alerts to such events will be published within 60 s of observation; we expect several million alerts per night ( Ridgway et al. 2014 ) .”

What the sources say

• Not checked yetcites Ridgway et al. 2014 source

In the paper

“When this assumption is not correct ( e.g., in the u band ) , the coef fi cients Cm do slightly depend on t vis .”

In the paper

“We have already discussed three examples of such mini-surveys: the northern ecliptic spur to improve completeness of the asteroid and KBO population, the southern celestial cap to extend the survey footprint to the South Pole ( thus providing coverage of the Magellanic Clouds ) , and the Galactic plane survey to include low Galactic latitude fi elds.”

In the paper

“Due to very red V - u colors and the relatively bright limiting magnitude in the y band, the smallest objects are preferentially detected in the griz bands.”

In the paper

“When subsequences from a given night were co-added, they would provide dense time sampling to a faint limit of r ∼ 26.5 and would enable deep searches for SNe, TNOs, and other faint transient, moving, and variable sources.”

In the paper

“Furthermore, there are close to 1000 galaxies per sensor with r < 22, which will provide exquisite control of systematic astrometric errors as a function of magnitude, color, and other parameters and thus enable absolute proper-motion measurements.”

In the paper

“After accounting for differences in their input assumptions and models, each of these independent works calculates a completeness value that is consistent within a few percent.”

What the sources say

• Not checked yetcites Jones et al. 2018 source
• Not checked yetcites Vereš & Chesley 2017a, 2017b
• Not checked yetcites Grav et al. 2016 source

In the paper

“However, this decoupling between the system sensitivity expressed via Cm and observing conditions is only correct in the limit that the instrumental noise ( dominated by the readout noise ) is negligible compared to the background noise.”

In the paper

“The differences in performance between LSST and, for example, SDSS follow directly from these relations.”

In the paper

“These four fi elds are only the fi rst chosen for deep-drilling observations.”

In the paper

“They will include alerts to objects that were newly discovered or have changed brightness or position at a statistically signi fi cant level.”

In the paper

“Within this region, the Galactic plane proposal provides 30 observations in each of the six fi lters, distributed roughly logarithmically in time ( it may not be necessary to use the u and g fi lters for this heavily extincted region ) .”

In the paper

“These will be generated continuously every observing night, by detecting and characterizing sources in images differenced against deep templates.”

In the paper

“The structure of Equation ( 6 ) nicely illustrates decoupling between the system sensitivity that is fully absorbed into Cm and observing conditions speci fi ed by m sky , θ , t vis , km , and X .”

In the paper

“Finally, the universal cadence proposal excludes observations at low Galactic latitudes, where the high stellar density leads to a confusion limit at much brighter magnitudes than those attained in the rest of the survey.”

In the paper

“Data collected by the LSST telescope and camera will be automatically processed to data products -catalogs, alerts, and reduced images -by the LSST Data Management system ( Section 2.6.3 ) .”

In the paper

“Hence, LSST will smoothly extend Gaia ' s error versus magnitude curve about 4 mag fainter ( for illustration, see Figure 21 in Ivezi ć et al. 2012 ) .”

What the sources say

• Not checked yetcites Ivezić et al. 2012 source

In the paper

“The values of Cm listed in Table 2 assume instrumental noise of 9 e -per pixel and per readout ( whose effect on m 5 is signi fi cant only in the u band ) .”

In the paper

“Such sequences would also serve as excellent tests of our photometric calibration procedures.”

In the paper

“Even a drift-scanning survey such as SDSS delivers uncorrelated systematic errors ( dominated by seeing effects ) at the level of 20 -30 mas ( measured from repeated scans; Pier et al. 2003 ) ; the expected image quality for LSST will be twice as good as for SDSS.”

What the sources say

• Not checked yetcites Pier et al. 2003 source

In the paper

“Prompt products, 101 designed to support the discovery, characterization, and rapid follow-up of time-dependent phenomena ( ' transient science ' ) .”

In the paper

“The individual sequences would be sensitive to 1% variability on subminute timescales, allowing discovery of planetary eclipses and of interstellar scintillation effects, expected when the light of a background star propagates through a turbulent gas medium ( Moniez 2003; Habibi et al. 2011 ) .”

What the sources say

• Not checked yetcites Moniez 2003 source
• Not checked yetcites Habibi et al. 2011 source

In the paper

“The MOPS software system and its algorithms are signi fi cantly more advanced than anything previously fi elded for this purpose to date.”

In the paper

“In both examples, the conclusions crucially depend on the assumed accuracy of the photometry and astrometry, as we now describe.”

In the paper

“For a given albedo and spherical asteroids, H depends only on the asteroid diameter.”

In the paper

“The LSST has already selected four distant extragalactic survey fi elds 97 that the project guarantees to observe as Deep Drilling Fields with deeper coverage and more frequent temporal sampling than provided by the standard LSST observing pattern.”

In the paper

“Objects with motions suf fi cient to cause trailing in a single exposure will be identi fi ed and fl agged as such when the alerts are broadcast.”

In the paper

“These products are designed to enable a large majority of LSST science cases, without the need to work directly with the raw pixels.”

In the paper

“For comparison with Table 3, the SDSS-POSS propermotion measurements have an accuracy of ∼ 5 mas yr -1 per coordinate at r = 20 ( Munn et al. 2004 ) , and Gaia DR 2 has delivered a median uncertainty in parallax of 0.7 mas and in proper motion of 1.2 mas yr -1 at its faint end, approximately corresponding to r = 20 ( Gaia Collaboration et al. 2018; Lindegren et al. 2018 ) .”

What the sources say

• Not checked yetcites Munn et al. 2004 source
• Not checked yetcites Gaia Collaboration et al. 2018 source
• Not checked yetcites Lindegren et al. 2018 source

In the paper

“The user experience will be nearly identical to working with Jupyter notebooks locally, except that computation and analysis will occur with resources provided at the LSST Data Access Center.”

In the paper

“The JupyterLab aspect, which will provide a Jupyter 106 Notebook-like interface and is geared toward enabling next-to-the-data remote analysis. A large suite of commonly used astronomical software, including the LSST software stack ( Section 2.6.4 ) , will be made available through this interface.”

In the paper

“Each sky position within the main survey area will be observed close to 1000 times, with timescales spanning seven orders of magnitude ( from 30 s to 10 yr ) , and produce roughly 30 trillion photometric measures of celestial sources.”

In the paper

“Each sky position within the main survey area will be observed close to 1000 times, with timescales spanning seven orders of magnitude ( from 30 s to 10 yr ) , and produce roughly 30 trillion photometric measures of celestial sources.”

In the paper

“The main product of the LSST system will be a multicolor ugrizy image of about half the sky to unprecedented depth ( r ∼ 27.5 ) .”

In the paper

“These will include the ( reduced and raw ) singleepoch images, deep co-adds of the observed sky, catalogs of objects detected in LSST data, catalogs of sources ( the detections and measurements of objects on individual visits ) , and catalogs of ' forced sources ' ( measurements of fl ux on individual visits at locations where objects were detected by LSST or other surveys ) .”

In the paper

“The LSST Science Platform ( Juri ć et al. 2017 ) represents LSST ' s vision for a large-scale astronomical data archive that can enable effective research with data sets of LSST size and complexity.”

What the sources say

• Not checked yetcites Juri ć et al. 2017

In the paper

“At i < 25.3 ( S / N > 20 for point sources ) , the photometry of galaxies will be of high enough quality to provide photometric redshifts with an rms accuracy ( σ / ( 1 + z )) of 2% over the range 0.3 < z < 3.0 ( only 10% of the sample will have redshift errors larger than 6% ) .”

In the paper

“That is, while the co-adds will be used to perform object detection , the measurement of their properties will be performed by simultaneously fi tting ( PSF-convolved ) models to all single-epoch observations.”

In the paper

“We will make it possible for the end users to create ( or use ) such user-generated 105 products at the LSST Data Facility, using the services offered within the LSST Science Platform ( Section 3.3.1 ) .”

In the paper

“The data products for these programs will be generated using the same processing system and will be released on the same timescale as the rest of the survey; any specialized processing that these require will be the responsibility of the community.”

In the paper

“An extended source model -a constrained linear combination of two Sérsic pro fi les -and a pointsource model with proper motion -will generally be fi tted to each detected object.”

In the paper

“Based on the current plans and technology projections, these equate to approximately 2400 cores, 4 PB of fi le storage, and 3 PB of database storage at the beginning of LSST operations ( in 2022 ) .”

In the paper

“LSST DRs will also include fully reprocessed prompt products, as well as all metadata and software necessary for the end user to reproduce any aspect of LSST DR processing.”

In the paper

“The Euclid mission ' s planned 6 yr survey should reach a similar galaxy density over 15,000 square degrees of sky ( Laureijs et al. 2011 ) ; its space-based resolution and broadband optical and NIR fi lters should provide a complementary WL survey of comparable constraining power but limited by different systematics.”

What the sources say

• Not checked yetcites Laureijs et al. 2011

In the paper

“The galaxy -shear correlation function probes the growth of dark matter large-scale structure and is a diagnostic of the underlying cosmology.”

In the paper

“Any given probe constrains degenerate combinations of cosmological parameters, and each probe is affected by different systematics; thus, the combination of probes allows systematics to be calibrated and for degeneracies to be broken.”

In the paper

“It will be possible to further improve photometric redshift calibration by crosscorrelating the photometric sample with redshift surveys of galaxies and quasars in the same fi elds ( Newman 2008; Matthews & Newman 2010; Ménard et al. 2013; Davis et al. 2017 ) .”

What the sources say

• Not checked yetcites Newman 2008 source
• Not checked yetcites Matthews & Newman 2010
• Not checked yetcites Ménard et al. 2013

In the paper

“Those that are not trailed will be identi fi ed and linked based on their motion from observation to observation, over a period of a few days.”

In the paper

“The LSST Science Platform will be a set of web applications ( portals ) and services through which the users will access the LSST data products and, if desired, conduct remote analyses or create user-generated products.”

In the paper

“The design and optimization of the LSST system leverage its unique capability to scan a large sky area to a faint fl ux limit in a short amount of time.”

In the paper

“The Web API aspect will expose the LSST DAC services to other software tools and services using commonly accepted formats and protocols.”

In the paper

“At a slightly brighter cut, there will be around 30 galaxies arcmin -2 with shapes measured well enough for WL measurements ( Chang et al. 2013, 2015 ) , with the number realized in practice being dependent on the performance of the deblending and shape measurement algorithms.”

What the sources say

• ?Not matched

  Couldn’t be matched to a paper in Crossref, so it can’t be checked.

  cites Chang et al. 2013, 2015

In the paper

“The web Portal, designed to provide the essential data access and visualization services through a simple-to-use website. It will enable querying and browsing of the available data sets in ways the users are accustomed to at archives such as IRSA, MAST, or the SDSS archive.”

In the paper

“As described in Section 3.1.2, approximately 10% of the observing time will be devoted to mini-surveys that do not follow the LSST baseline cadence.”

In the paper

“This interface will open the possibility for remote access and analysis of the LSST data set using applications that the users are already comfortable with such as TOPCAT ( Taylor 2005 ) , or libraries such as Astropy ( Astropy Collaboration et al. 2013; Jenness et al. 2016 ) . Furthermore, the offered APIs will allow for federation with other astronomical archives, bringing added value to the LS”

What the sources say

• ?Not matched

  Couldn’t be matched to a paper in Crossref, so it can’t be checked.

  cites Taylor 2005
• ?Not matched

  Couldn’t be matched to a paper in Crossref, so it can’t be checked.

  cites Astropy Collaboration et al. 2013; Jenness et al. 2016

In the paper

“By simultaneously measuring the growth of large-scale structure and luminosity and angular distances as functions of redshift ( via WL, LSS, SN, and cluster counting ) , LSST data can reveal whether the recent cosmic acceleration is due to dark energy or modi fi ed gravity”

What the sources say

• Not checked yetcites Lue et al. 2004 source
• Not checked yetcites Ishak et al. 2006 source
• Not checked yetcites Knox et al. 2006 source

In the paper

“A unique aspect of LSST as a probe of dark energy and dark matter is the use of multiple cross-checking probes that reach unprecedented precision ( see Figure 23 ) .”

In the paper

“For a comparison, one of the best analogous contemporary data sets is that of SDSS, which provides ugriz images of about a quarter of the sky to r ∼ 22.5, with twice as large seeing ( see Figures 21 and 22 ) .”

In the paper

“In addition, the presence of BAOs in the galaxy angular correlation functions is a strong cosmological probe on its own.”

In the paper

“These measurements consist of the two-point auto- and cross-correlations of shear and positions for billions of galaxies across ∼ 10 redshift bins.”

In the paper

“The characterization will be accomplished by sampling, with up to ∼ 200 ( independent ) likelihood samples retained for each object.”

In the paper

“For storage cost reasons, these samples may be retained only for those bands of greatest interest for WL studies.”

In the paper

“The WFIRST baseline survey is expected to cover some 2000 square degrees but reach a galaxy density of 45 arcmin -2 ( Spergel et al. 2015 ) .”

What the sources say

• Not checked yetcites Spergel et al. 2015

In the paper

“This number represents a requirement on the accuracy of the photometry at delivering photometric redshifts given known templates for the SEDs.”

In the paper

“The galaxy -galaxy correlation function is vital to constrain the galaxy bias impacting the galaxy -shear correlation and is therefore an essential component in the joint analysis of LSS and WL.”

In the paper

“Their orbits as derived by MOPS will be published within 24 hr of identi fi cation.”

In the paper

“The degradation in photometric redshift quality associated with requiring more training data than currently exists to de fi ne the template set increases the expected σ / ( 1 + z ) to ∼ 0.05 ( e.g., Newman et al. 2015; Graham et al. 2018 ) , which is still well within the expected range for a Stage IV dark energy experiment.”

What the sources say

• Not checked yetcites Newman et al. 2015 source
• Not checked yetcites Graham et al. 2018 source

In the paper

“The ef fi ciency of linking ( and thus the completeness of the resulting orbit catalog ) will depend on the fi nal observing cadence chosen for LSST, as well as the performance of the linking algorithm ( Section 3.2.2 ) .”

In the paper

“2. DR products 102 are designed to enable systematics- and fl ux-limited science and will be made available in annual DRs.”

In the paper

“Approximately 10% of the total budget for the LSST Data Facility compute and storage capacity has been reserved for the LSST Science Platform needs, and to be shared by all LSST DAC users.”

In the paper

“A noteworthy aspect of LSST DR processing is that it will largely rely on multi-epoch model fi tting, or MultiFit , to perform near-optimal characterization of object properties.”

In the paper

“WL and LSS are highly complementary probes, and the combination of their autoand cross-correlations will constrain the properties of the late-time accelerated expansion while providing internal cross-checks for marginalizing over systematic uncertainties ( e.g., Mandelbaum 2018 ) .”

What the sources say

• Not checked yetcites Mandelbaum 2018 source

In the paper

“The combination with the galaxy -velocity correlation function estimated from currently planned spectroscopic surveys could test general relativity and its variants at high redshift ( Reyes et al. 2010 ) .”

What the sources say

• Not checked yetcites Reyes et al. 2010 source

In the paper

“This is an implementation of the ' bringing computation to the data ' paradigm: rather than imposing the burden of downloading, storing, and processing ( potentially large ) subsets of LSST data at their home institutions, we make it possible for the users to bring their codes and perform analyses at the LSST DAC. This reduces the barrier to entry and shortens the path to science for the LSST sci”

In the paper

“The median redshift for this sample will be z ∼ 1.2, with the third quartile at z ∼ 2.”

In the paper

“Dark energy manifests itself in two ways. The fi rst is the relationship between redshift and distance ( the Hubble diagram ) , or equivalently the expansion rate of the universe as a function of cosmic time. The second is the rate at which matter clusters with time.”

In the paper

“The platform makes this possible through three user-facing aspects :”

In the paper

“Barnard et al. ( 2008 ) showed that in a high-dimensional dark energy model space, LSST data could lead to a hundred- to thousand-fold increase in precision over its precursor experiments, thereby con fi rming its status as a premier Stage IV experiment in the sense of Albrecht et al. ( 2006 ) .”

What the sources say

• Not checked yetcites Barnard et al. ( 2008 ) source
• Not checked yetcites Albrecht et al. ( 2006 )

In the paper

“Tens of thousands of galaxy -galaxy lenses will provide the needed statistics to probe dark matter halo pro fi les and substructure ( e.g., Mandelbaum et al. 2006; Vegetti et al. 2012 ) .”

What the sources say

• Not checked yetcites Mandelbaum et al. 2006 source
• Not checked yetcites Vegetti et al. 2012 source

In the paper

“In addition to the usual use of SNe Ia to probe the redshift -distance relation to high redshift, the luminosities will be magni fi ed by lensing from foreground structure, a correlation that can be probed with these data.”

In the paper

“This sample of SNe can be used as a tracer of large-scale structure by directly probing the gravitational potential of structure through inferences of their peculiar velocities ( Gordon et al. 2007; Bhattacharya et al. 2011; Howlett et al. 2017 ) , WL of SN brightnesses ( Dodelson & Vallinotto 2006; Quartin et al. 2014; Macaulay et al. 2017; Scovacricchi et al. 2017 ) , and the local bulk fl”

What the sources say

• Not checked yetcites Gordon et al. 2007 source
• Not checked yetcites Bhattacharya et al. 2011 source
• Not checked yetcites Howlett et al. 2017 source

In the paper

“Given the current constraints on neutrino mass mixing, this is at the level to determine whether there is an inverted neutrino mass hierarchy, a fundamental question in particle physics.”

In the paper

“LSST will also discover between 500 and 1000 strongly lensed SNe Ia ( Goldstein & Nugent 2017; Goldstein et al. 2018 ) , which will provide hundreds of additional high-quality time delays.”

What the sources say

• Not checked yetcites Goldstein & Nugent 2017
• Not checked yetcites Goldstein et al. 2018 source

In the paper

“Time delays of galaxy-scale lensed quasars will allow one to measure Hubble ' s constant ( e.g., Suyu et al. 2010; Bonvin et al. 2017 ) in hundreds of systems; subpercentlevel precision in H ( z ) should be achievable ( Coe & Moustakas 2009; Treu & Marshall 2016 ) , providing a further independent dark energy probe.”

What the sources say

• Not checked yetcites Suyu et al. 2010 source
• Not checked yetcites Bonvin et al. 2017 source
• Not checked yetcites Coe & Moustakas 2009

In the paper

“The baseline LSST cadence will result in orbital parameters for several million objects; these will be dominated by main belt asteroids, with light curves and multicolor photometry for a substantial fraction of detected objects.”

In the paper

“Standard sirens are a new cosmological probe, demonstrated by the recent discovery of a binary neutron star merger by the Laser Interferometer Gravitational Wave Observatory ( LIGO ) with an electromagnetic counterpart ( Abbott et al. 2017a ) , which was used to constrain the Hubble parameter to roughly 15% precision ( Abbott et al. 2017b ) .”

What the sources say

• Not checked yetcites Abbott et al. 2017a
• Not checked yetcites Abbott et al. 2017b

In the paper

“The main survey will obtain light curves in six bands and photometric redshifts of about 400,000 photometrically classi fi ed SNe Ia that can be used for cosmological distance measurements, with further spectroscopic follow-up of a subsample of their host galaxies.”

In the paper

“In addition, LSST will identify optical counterparts and provide deep optical imaging for clusters detected in other wavebands ( e.g., Staniszewski et al. 2009 ) .”

What the sources say

• Not checked yetcites Staniszewski et al. 2009 source

In the paper

“Higher-order shear and galaxy statistics and shear peak counts can improve dark energy constraints and provide self-calibration of various systematics ( Takada & Jain 2004; Dolney et al. 2006; Huterer et al. 2006; Petri et al. 2016 ) .”

What the sources say

• Not checked yetcites Takada & Jain 2004
• Not checked yetcites Dolney et al. 2006 source
• Not checked yetcites Huterer et al. 2006 source

In the paper

“Such a sample will not only provide larger statistics for the study of the Type Ia population in the universe but also be spread across the full 18,000 deg 2 LSST main survey footprint, allowing different probes of the large-scale structure of the low-redshift universe.”

In the paper

“The clustering properties of those same galaxy clusters will also be used to constrain cosmological parameters ( Mo et al. 1996; Mana et al. 2013 ) , to marginalize over uncertainties in the mass -observable relation and photometric redshift uncertainties ( Oguri & Takada 2011 ) , and to constrain the effects of supersample covariance in the two-point functions of WL and LSS ( Hu & Kravts”

What the sources say

• Not checked yetcites Mo et al. 1996
• Not checked yetcites Mana et al. 2013 source
• Not checked yetcites Oguri & Takada 2011

In the paper

“Cluster mass reconstruction based on the multiple image positions can probe the cluster inner mass pro fi le and can provide a separate test of cosmology, especially in cases with strongly lensed background objects at different redshifts ( Porciani & Madau 2000; Oguri & Kawano 2003 ) .”

What the sources say

• Not checked yetcites Porciani & Madau 2000
• Not checked yetcites Oguri & Kawano 2003

In the paper

“They are also probes of both primordial nonGaussianities and those caused by nonlinear structure.”

In the paper

“The ultimate promise of such SN surveys will be linked to the observing strategy employed by the LSST.”

In the paper

“Constraints from standard sirens are independent of the local distance ladder, with the primary uncertainties being the local velocity fi eld and the inclination angle of the system.”

In the paper

“Primordial non-Gaussianity is also probed by the largescale power of any biased tracer of the matter overdensities ( Dalal et al. 2008 ) .”

What the sources say

• Not checked yetcites Dalal et al. 2008 source

In the paper

“LSST will be capable of detecting objects like Sedna to beyond 100 au, thus enabling in situ exploration far beyond the edge of the Kuiper Belt at ∼ 50 au.”

In the paper

“Understanding these populations, both physically and in their number and size distribution, is a key element in testing various theories of solar system formation and evolution.”

In the paper

“We will be able to identify the progenitors of eruptive transients in the deep LSST stacks and even look for faint precursor eruptions.”

In the paper

“The superb continuum light curves of AGNs will enable economical ' piggyback ' reverberation-mapping efforts using spectroscopy of emission lines”

What the sources say

• Not checked yetcites Chelouche & Daniel 2012
• Not checked yetcites Shen et al. 2015 source
• Not checked yetcites Grier et al. 2017 source

In the paper

“A large, well-characterized sample of superluminous SNe, including objects at redshift as high as z = 2.5, a sample large enough to be leveraged for cosmology improving constraints on w and Ω m ( Scovacricchi et al. 2016 )”

What the sources say

• Not checked yetcites Scovacricchi et al. 2016 source

In the paper

“Because most of these objects will be observed several hundred times, accurate orbital elements, colors, and variability information will also be available.”

In the paper

“at least several hundred strongly lensed core-collapse SNe ( Oguri & Marshall 2010 ) are expected to be discovered by LSST.”

What the sources say

• Not checked yetcites Oguri & Marshall 2010

In the paper

“Optical identi fi cation of transients and variables detected in other electromagnetic wavebands, from gamma-rays to radio.”

In the paper

“Studying the distribution of their orbits ( in particular including any clustering in the argument of perihelion ) will test models predicting the existence of a planetary-mass object beyond Neptune, a proposed Planet 9 ( Trujillo & Sheppard 2014; Batygin & Brown 2016; Brown & Batygin 2016; Sheppard & Trujillo 2016; Brown 2017 ) .”

What the sources say

• Not checked yetcites Trujillo & Sheppard 2014 source
• Not checked yetcites Batygin & Brown 2016 source
• Not checked yetcites Brown & Batygin 2016 source

In the paper

“LSST will extend the extrasolar planet census to larger distances within the Galaxy, thus enabling detailed studies of planet frequency as a function of stellar metallicity and parent population ( e.g., Hartman et al. 2009; Bayliss & Sackett 2011 ) .”

What the sources say

• Not checked yetcites Hartman et al. 2009 source
• Not checked yetcites Bayliss & Sackett 2011

In the paper

“LSST will be some 3 mag more sensitive than current NEO surveys ( like Pan-STARRS1 ) and will cover more sky more often.”

In the paper

“A study of quasar variability using accurate, multicolor light curves for a few million quasars, leading to constraints on the accretion physics and nuclear environments”

What the sources say

• Not checked yetcites de Vries et al. 2003 source
• Not checked yetcites Vanden Berk et al. 2004 source
• Not checked yetcites MacLeod et al. 2010 source

In the paper

“The LSST will map the Galaxy in unprecedented detail, and by doing so revolutionize the fi elds of Galactic astronomy and near- fi eld cosmology.”

In the paper

“Since LSST extends time -volume -color space 50 -100 times over current surveys ( e.g., Djorgovski et al. 2013 ) , it will facilitate new population and statistical studies and also the discovery of new classes of objects.”

What the sources say

• Not checked yetcites Djorgovski et al. 2013 source

In the paper

“LSST will discover an unprecedentedly large number of comets, with typically 50 observations per object spread throughout their orbits during the 10 yr survey, and will help us to constrain models of the origin of comets ( Solontoi 2010; Silsbee & Tremaine 2016 ) .”

What the sources say

• Not checked yetcites Solontoi 2010
• Not checked yetcites Silsbee & Tremaine 2016

In the paper

“We will also constrain the rates of individual eruption subclasses ( Smith 2014 ) by detecting them in galaxies out to tens of megaparsecs.”

What the sources say

• Not checked yetcites Smith 2014 source

In the paper

“Studies of dwarf novae, including their use as probes of stellar populations and structure in the Local Group”

In the paper

“Discovery and characterization of thousands of hot Jupiters in exoplanetary systems via the transit method ( Wright et al. 2012 ) .”

What the sources say

• Not checked yetcites Wright et al. 2012 source

In the paper

“Microlensing events will also be monitored in the ∼ 4000 gravitationally lensed quasars discovered by LSST and used to measure the spatial structure of quasar accretion disks.”

In the paper

“Therefore, LSST is likely to fi nd more interstellar objects, and more frequently.”

In the paper

“This will result in a much larger, well-understood sample of inner Oort Cloud objects like Sedna and 2012 VP113 ( Trujillo & Sheppard 2014 ) .”

What the sources say

• Not checked yetcites Trujillo & Sheppard 2014 source