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The Dark Energy Science
Collaboration
Andy Connolly (DESC Computing Coordinator),
Rachel Bean (DESC Spokesperson)
Science to test L and beyond
Origins of cosmic acceleration could come from varied modifications to
Einstein’s equations
Deviations
from GR?
L?
Dark Energy evolving with z?
Dark sector interactions?
Anisotropic clustering?
LSST, DESI, Euclid, WFIRST, CMB-S4 others designed to test these using
both spatial and time-domain data through revealing different facets both
individually and in combination
Andy Connolly/Rachel Bean, LSST@Europe2, June 2016
Observational Probes
Probe
Physical
Measurement
Effect of dark energy
Weak Gravitational
Lensing
Correlated distortions
in galaxy shapes
• Geometric distance
Project growth of structure
Large Scale
Structure
Galaxy power spectrum
•
•
•
Galaxy Clusters
Type 1a Supernovae
Strong Lensing
Cluster abundance as •
function of mass and
redshift
Fluxes and redshift
Time Delays of Multiply •
Lensed Sources
Andy Connolly/Rachel Bean, LSST@Europe2, June 2016
Geometry/ distance-redshift (z)
relation: BAO Standard Ruler
Structure growth with redshift
(clustering & peculiar motion)
Structure growth with redshift
(clustering & peculiar motion)
•
Geometry/ distance-z relation:
luminosity distance standard
candle
Geometry/ distance-z relation
LSST Dark Energy Science
Collaboration (DESC)
Formed in June 2012 to bring together scientists to prepare for and carry
out cosmological analyses with LSST data
DESC whitepaper arXiv:1211.0310 set out initial goals
HEP style structure with democratic, member-based governance
Members with astrophysics and particle physics backgrounds
Expertise in instrumentation, computing, observing & theory
Rapidly evolved since inception to become active international collaboration
Over 490 members, 156 “full members”
Full member locations
DOE is the lead agency:
• Six DOE Labs, 1/3 of full members, playing key roles.
• ~20 DOE HEP supported university members
Public website: http://www.lsst-desc.org/
Andy Connolly/Rachel Bean, LSST@Europe2, June 2016
Collaboration Structure
Andy Connolly/Rachel Bean, LSST@Europe2, June 2016
DESC work organized in 12
Working Groups
Collaboration Council Chair
Spokesperson
Deputy Spokesperson
Phil Marshall (SLAC)
Rachel Bean
Jeff Newman
DOE Lab researcher
DOE HEP PI grant support
Non-US member
Conveners
Computing and Software Infrastructure Team
Coordinator: Andrew Connolly
Working Group
Conveners
Clusters
Anya von der Linden
Ian Dell'Antonio
Cosmological Simulations Katrin Heitman (ANL)
Simon Krughoff
Large Scale Structure
Eric Gawiser
Anze Slosar (BNL)
Survey Simulation
Photometric Redshifts
Ofer Lahav
Sam Schmidt
Computing Infrastructure Scott Dodelson (FNAL)
Richard Dubois (SLAC)
Strong Lensing
Chris Fassnacht
Phil Marshall (SLAC)
Analysis Team
Coordinator: Rachel Mandelbaum
Working Group
Supernovae
Saurabh Jha
Michael Wood Vasey
Theory/ Joint Probes
Elisabeth Krause
Andrew Zentner
Weak Lensing
Joe Zuntz
Michael Schneider (LLNL)
Andy Connolly/Rachel Bean, LSST@Europe2, June 2016
John Peterson
Chris Walter
Technical Team
Coordinator: Aaron Roodman
Working Group
Conveners
Sensor Anomaly
Pierre Astier
Andrei Nomerotski (BNL)
Photometric Calibration
Eli Rykoff (SLAC)
Nicolas Regnault
DESC Planning: 2015 DESC
Science Roadmap (SRM)
Find at http://lsst-desc.org/sites/default/files/DESC_SRM_V1.pdf
Lays out essential tasks across the working groups to be ready for LSST
commissioning
Focused on tasks to build and rigorously test the analysis pipeline to ensure
meets requirements to analyze LSST-level data
3 sequential Data Challenges (DC1-3) of increasing complexity & integration
DC3: End-to-end analyses at LSST data complexity for all science areas
Scope of the 2015 Science Roadmap
LSST
Commissioning
FY2016
FY 2017
FY 2018
FY 2019
FY 2020
FY 2021
Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4
DC1
DC2
DC3
LSST Project
Verification
Verification & ComCam
Commissioning Mini-surveys
DESC Data
Challenges
Andy Connolly/Rachel Bean, LSST@Europe2, June 2016
DESC Planning: 2015 DESC Science Roadmap
(SRM)
Lays out WG key projects, deliverables and individual tasks to meet them
Andy Connolly/Rachel Bean, LSST@Europe2, June 2016
DESC Operations
Well-planned research and operations effort crucial to enable delivery of the
dark energy science
Ensure DOE ROI on camera investment.
DESC has been working with the DOE over the last year, or more, to put in
place a coherent operations plan and governance structure, to facilitate
operations support, through commissioning.
SLAC serves as the DOE Host Lab. Operations support will be located at
DOE Labs and DESC university groups.
Operations resources include:
• Computing infrastructure personnel
• Pipeline support personnel
• Computing hardware
• Collaboration infrastructure (communications/leadership support)
• Operations management and administration
Andy Connolly/Rachel Bean, LSST@Europe2, June 2016
How do I join and get involved?
If your institute/country is a member:
• Applications for membership are online and are dealt with on a rolling
basis http://www.lsst-desc.org/Membership
• Members have access to DESC communication tools, internal website,
and documents
• Full members have access to DESC computing resources and all DESC
data products. Full membership requires a description of the work you
plan to undertake and a commitment of time to the collaboration
• Tools available include: mailing lists, a confluence wiki, a Github
organization (hosting code and some documents)
• Bi-annual collaboration meetings (including a dark energy school, hack
days, working group meetings). Next meeting: Oxford July 18-22 2016
If your institute/country is not a member:
• Ask your institute to join!
Andy Connolly/Rachel Bean, LSST@Europe2, June 2016
A single analysis/survey can’t
give the full picture
Trade offs/complementarity in
•
•
•
•
•
Probes (SN1a, BAO, RSD, WL, Clusters + lensing, motions, positions)
Photometric speed vs. spectroscopic precision
Survey area vs depth - repeat imaging, dithering, cadence and overlap.
Astrophysical tracers used (LRGs, ELGs, Lya/QSOs, clusters)
Epochs, scales and environs being studied (cluster vs dwarf galaxies)
Complementarity sensitivity to systematic errors
• Atmospheric contamination
• Chromatic PSF effects
Cross-correlation science
• Weak lensing + spectroscopic galaxy clustering => gravitational slip
• CMB +LSS cross-correlations => mitigates lensing bias/contamination and
yields additional cosmological science
Andy Connolly/Rachel Bean, LSST@Europe2, June 2016
LSST one of a number of upcoming surveys:
Different strengths & systematics
Stage IV
DESI
LSST
Euclid
WFIRST
Starts, duration
~2018, 5 yr
2022, 10yr
2020 Q2, 6.25yr
~2025, 5-6 yr
Area (deg2)
14,000 (N)
20,000 (S)
15,000 (N + S)
2,400 (S)
FoV (deg2)
7.9
10
0.53
0.281
Diameter (m)
4 (less 1.8+)
6.7
1.3
2.4
Spectroscopic
Survey
Fibers R=3-4000)
360-980 nm
Grism R=250
1.1-2 mm
Grism R=550-800
1.35-1.95 mm
Sample
LRGs+ELGs z~0.61.7 (20-30m),
QSOs/Lya 1.9<z<4
(1m)
ELGs: z~0.7-2.1
(~20m)
ELGs: z =1-2 (20m),
2–3 (2m)
~30-35, in one broad
optical + IR band
68, in 3 bands into
near IR
Photometric
galaxies
(per sq arcmin)
~30 over 6 bands
(ugrizy)
SN1a
104-105 SN1a/yr
z = 0.–0.7
photometric
2700 SN1a
z = 0.1–1.7
IFU spectroscopy
(based on publicly available data)
Andy Connolly/Rachel Bean, LSST@Europe2, June 2016
To conclude
LSST is a Stage IV survey with first light scheduled for early 2020
It will use multiple probes to discern the properties of dark energy and gravity
on cosmic scales
Varied probes promise to provide rich insights into cosmology through their
complementary sensitivity to the fundamental physics & systematics
In combination, LSST, DESI and CMB-S4 will provide unprecedented insights
into dark energy, dark matter, the neutrino mass and inflation
LSST DESC is actively preparing for the cosmological analysis of LSST data
A concerted, collaborative effort is underway now, prior to commissioning, to
ensure we realize the scientific potential that LSST data will provide and in a
timely fashion
We welcome interested members of the LSST community, please join us!
Andy Connolly/Rachel Bean, LSST@Europe2, June 2016