federica bianco PRO
astro | data science | data for good
Vera C. Rubin Observatory:
Federica Bianco
University of Delaware
Department of Physics and Astronomy
Biden School of Public Policy and Administration
Data Science Institute
Rubin Legacy Survey of Space and Time
Deputy Project Scientist, Rubin Construction
Interim Head of Science, Rubin Operation
Rubin Observatory
Site: Cerro Pachon, Chile
Funding: US NSF + DOE
Status: final phases of construction - completion expected 2025
federica bianco - fbianco@udel.edu
LSST Science Drivers
Probing Dark Energy and Dark Matter
federica bianco - fbianco@udel.edu
image credit ESO-Gaia
LSST Science Drivers
Mapping the Milky Way and Local Volume
via resolved stellar population
federica bianco - fbianco@udel.edu
An unprecedented inventory of the Solar System from threatening NEO to the distant Oort Cloud
LSST Science Drivers
LSST Science Drivers
image credit: ESA-Justyn R. Maund
Exploring the Transients and Variable Universe
10M alerts every night shared with the world
60 seconds after observation
federica bianco - fbianco@udel.edu
To accomplish this, we need:
1) a large telescope mirror to be sensitive - 8m (6.7m)
2) a large field-of-view for sky-scanning speed - 10 deg2
3) high spatial resolution, high quality images - 0.2''/pixels
4) process images in realtime and offline to produce live alerts and catalogs of all 37B objects
2M 3,200 Megapixel images in 10 years -about 60 PB of data
Objective: provide a science-ready dataset to transform the 4 key science area
federica bianco - fbianco@udel.edu
2026
federica bianco - fbianco@udel.edu
@fedhere
At this level of precision,everything is variable, everything is blended, everything is moving.
SDSS
LSST-like HSC composite
|
Field of View' Image resolution' DDFs' Standard visit' Photometric precision' Photometric accuracy' Astrometric precision' Astrometric accuracy' |
9.6 sq deg 0.2'' (seeing limited) 5 DDF 30 sec 5 mmag 10 mmag 10 mas 50 mas |
' requirement: ls.st/srd
SDSS 2x4 arcmin sq griz
MYSUC (Gawiser 2014) 1 mag shallower than LSST coadds
federica bianco - fbianco@udel.edu
| u,g,r,i,z,y | |
|---|---|
|
Photometric filters' saturation limit' # visits* mag single image* mag coadd* Nominal cadence |
u, g, r, i, z, y ~15, 16, 16, 16, 15, 14 53, 70, 185, 192, 168, 165 23.34, 23.2, 24.05, 23.55 22.03 25.4, 26.9, 27.0, 26.5, 25.8, 24.9 2-3 visits per night |
At this level of precision,everything is variable, everything is blended, everything is moving.
' requirement: ls.st/srd
NOMINAL LSST REQUIREMENT:
≤10 mas rms relative astrometric accuracy per axis
NOMINAL LSST REQUIREMENT:
≤10 mas rms relative astrometric accuracy per axis
Improve on requirement by x10 (depending on stellar density)
Rubin Observatory Status
@fedhere
September 2016
@fedhere
Fabruary 2020
@fedhere
May 2022
@fedhere
November 2022
@fedhere
May 2022
The DOE LSST Camera - 3.2 Gigapixel
3024 science raft amplifier channels
Camera and Cryostat integration completed at SLAC in May 2022,
Shutter and filter auto-changer integrated into camera body
LSSTCam undergoing final stages of testing at SLAC
May 2022 - Telescope Mount Assembly
weight 2e5 kg, max slew rate 0.2 rad/s
Most of the weight in a 10m disk
Angular momentum
5,000,000 ~kg~m^2 s^{-1}
ok but when????????????
late 2024-
early 2025
mid 2025
~2 years
from now
First data release ~3y from now
alerts build up
LSST
data products
federica bianco - fbianco@udel.edu
Time
Domain
Science
Static
Science
Alerts based
Catalog based
Deep stack
based
Deep stack
based
Data Products
federica bianco - fbianco@udel.edu
federica bianco - fbianco@udel.edu
world public!
ls.st/LDM-612
Rubin Observatory LSST
federica bianco - fbianco@udel.edu
federica bianco - fbianco@udel.edu
world public!
Alerts Images
Meta Data &
Catalog Visits
80
Pitt-Google
Broker
BABAMUL
data right holders only
federica bianco - fbianco@udel.edu
LSST survey strategy optimization
Rubin LSST survey design
federica bianco - fbianco@udel.edu
Rubin LSST survey design
federica bianco - fbianco@udel.edu
KN
Rubin LSST survey design
Rubin has involved the community to an unprecedented level in survey design this is a uniquely "democratic" process!
Survey Cadence Optimization Committee
Operation Simulator (OpSim)
simulates the catalog of LSST observations + observation properties
Metric Analysi Framwork (MAF)
Python API to interact with OpSims specifying science performance on a science case with a metric
Lynne Jones
Peter Yoachim
~100s simulations
~1000s MAFs
Rubin LSST survey design
Rubin LSST survey design
20+ peer review papers accepted several more under review and in preparation https://iopscience.iop.org/journal/0067-0049/page/rubin_cadence
Rubin LSST survey design
Rubin has involved the community to an unprecedented level in survey design this is a uniquely "democratic" process!
2017
Rubin LSST survey design
Rubin has involved the community to an unprecedented level in survey design this is a uniquely "democratic" process!
2019
Rubin LSST survey design
Rubin has involved the community to an unprecedented level in survey design this is a uniquely "democratic" process!
2023
Rubin LSST survey design
Rubin has involved the community to an unprecedented level in survey design this is a uniquely "democratic" process!
2024
Marshall et al. 2017
Mortersen et al. 2019
Kilonovae in LSST Wide Fast Deep
Smith +2019
Ragosta+ et al. 2023
Kilonovae in LSST Wide Fast Deep
Presto-Color, Bianco+ 2019
Identified an issue with the original survey plan:
2 intranight obs in same filer +
2 intranight obs in another filter ~5 day later
Proposed 3 intranight obs
2 within 1 hour in different filters
1 at 4-8 hours separation w repeat filter
Kilonovae in LSST Wide Fast Deep
Presto-Color, Bianco+ 2019
Identified an issue with the original survey plan:
2 intranight obs in same filer +
2 intranight obs in another filter ~5 day later
Proposed 3 intranight obs
2 within 1 hour in different filters
1 at 4-8 hours separation w repeat filter
Ofek+ 2024
cepheid
- Kilonovae
- SN-GRB breakout
- Fast Radio Bursts
- X-ray binary stars,
- cataclysmic variable stars,
- blazars
- stellar flares
- solar system occultations
- technosignatures
Željko Ivezić et al 2019 ApJ 873 111
LSST: From Science Drivers to Reference Design and Anticipated Data Products
# pairs of observations (1e5)
time gaps (days)
based on 2017 LSST simulations
With a naive survey strategy the 2-14 hours time scales where significantly undersamples
Kilonovae in LSST Wide Fast Deep
Give me a few hours, Bellm+ 2019
Assuming:
a rate of 800/Gpc^3/y
uniform luminosity function
=> ~350 GW170817-like kilonovae are expected to be present in Rubin data,
=> 3 – 32 might be identified using ZTFReST-like algorithms on pre 2018 simulations
Kilonovae in LSST Wide Fast Deep
Andreoni+ 2022a
newer simulations ->
<-bad good ->
2023 simulations: 62% improvement
newer simulations ->
4 – 24 hour gaps between epochs will enable kilonova parameter estimation
Kilonovae in LSST Wide Fast Deep
Andreoni+ 2022a
2017
2024
Rubin LSST survey design
(~current plan: the Wide Fast Deep 75-90% of the sky time)
The LSST@europe series
has been exploring synergies with European missions and surveys
LSST@Europe6 - 2024 La Palma- Spain
Synergy and Survey coordination
Guy et al. https://arxiv.org/pdf/2201.03862.pdf
Synergy and Survey coordination
In preparation for Roman’s launch and operations, our analysis suggests to (i) make available a rapid (∼ 1 week) Target of Opportunity mode for GW follow-up; (ii) include observations of the High Latitude Time-Domain survey footprint in at least two filters [...]; (iii) operate in synergy with Rubin Observatory.
Nandini Hazra & Marica's group
Vera Rubin Observatory and Einstein Telescope: kilonova observation strategies to understand ET detector design
federica bianco - fbianco@udel.edu
Rubin ToO program
State of the art in coordination: GW Treasure Map
federica bianco - fbianco@udel.edu
Rubin ToO program
Andreoni+ 2022b
+80 authors!
PROS:
Large FoV (10 sq deg - easly cover 100 sq deg in full)
6 filters (5 available on any given night)
deep observations (r~24 in 30 sec, up to 180 sec)
public data
federica bianco - fbianco@udel.edu
Rubin ToO program
Andreoni+ 2022b
+80 authors!
PROS:
Large FoV (10 sq deg - easly cover 100 sq deg in full)
6 filters (5 available on any given night)
deep observations (r~24 in 30 sec, up to 180 sec)
public data
CONS:
no custom pipelines planned
80 hours delay in image access
limited sky time (not a PI facility)
Rubin ToO program
Andreoni+ 2022b
Rubin ToO program
Andreoni+ 2022b
~3% LSST sky time
Rubin ToO program
The main Rubin assets are the 10 sqdeg FoV + rapid slew + depth
PSTN-055 (2022): The SCOC recommends a ToO program be enabled to respond to Gravitational Waves and MMA triggers with a fraction of ≤ 3% of dedicated survey time, with the possibility of extending it to additional types of targets in the future.
Rubin ToO program
Smith+ 2023
0.25% LSST time 1GLGW/year
Rubin ToO program
Smith+ 2023
The problem with GLGW is depth: it takes 1 visit to get to r~24,
about 40 visits to get to r~26
100 sq deg at r~24 ~10 min
100 sq deg at r~25-6 ~5h
0.25% LSST time 1GLGW/year
Registration for online participation open through March 15th!
federica bianco - fbianco@udel.edu
This is a workshop: the goal of the workshop is to produce a report to be delivered to the SCOC containing recommendations for how to implement ToO responses with Rubin. There are no talks.Time is dedicated to collaboratively working toward the workshop report.
Rubin ToO program
SOC: I. Andreoni (KN), F. Bianco, A. Franckowiak (ν), T. Lister (Solar System),
R. Margutti (KN, GRB), G. Smith (Lensed KN)
LSST has profoundly changed the TDA infrastructure
Discovery Engine
10M alerts/night
Community Brokers
target observation managers
the astronomy discovery chain
Pitt-Google
Broker
BABAMUL
federica bianco - fbianco@udel.edu
Photometric Classification of transients
highest participation of any astronomical Kaggle challenges
federica bianco - fbianco@udel.edu
Rubin will see ~1000 SN every night!
Credit: Alex Gagliano IAIFI fellow MIT/CfA
Deep Drilling Fields
Deep Drilling Fields
Wide Fast Deep
Willow Fox Fortino
UDel grad student
When they go high, we go low
Classification power vs spectral resolution for SNe subtypes
Neural Network
classifier architectures:
- transformers
- CNNs
federica bianco - fbianco@udel.edu
Rubin Operations Research Inclusion team
federica bianco - fbianco@udel.edu
slide: Leanne Guy
how to get involved
join a Rubin LSST Science Collaborations
8 teams
>1500 members
>2000 affiliations
5 continents
federica bianco - fbianco@udel.edu
We aspire to be an inclusive, equitable, and ultimately just group and we are working with renewed vigor in the wake of the recent event that exposed inequity and racism in our society to turning this aspiration into action.
No commitment required for basic membership
No data rights required (being a member of an SC does not confer data rights
join a Rubin LSST Science Collaborations
Will Clarkson
SC coordinator
become a DP0 delegate
Rubin Community Science Team lead: Melissa Graham
federica bianco - fbianco@udel.edu
join the Community forum
Rubin Community Forum (Community.lsst.org) is available to everyone, and the posting of any and all Rubin/LSST-related questions is encouraged.
federica bianco - fbianco@udel.edu
thank you!
University of Delaware
Department of Physics and Astronomy
Biden School of Public Policy and Administration
Data Science Institute
@fedhere
federica bianco
Rubin Construction Deputy Project Scientist
fbianco@udel.edu
RAS MMA GW
By federica bianco
RAS MMA GW
KN perspective detection with the Vera C. Rubin Observatory
