Vera C. Rubin Observatory and the

Rubin LSST Science Collaborations

Federica Bianco

University of Delaware

Department of Physics and Astronomy

Biden School of Public Policy and Administration

Data  Science Institute

Rubin Deputy Project Scientist

Transients & Variable Stars SC CoChair

https://bit.ly/NAM22Rubinintro

slides available at

https://slides.com/federicabianco/GaiaTransients22

This is a living land acknowledgement developed in consultation with tribal leadership of Poutaxet, what is now known as the “Delaware Bay,” including: the Lenape Indian Tribe of Delaware, the Nanticoke Indian Tribe, and the Nanticoke Lenni-Lenape Tribal Nation in 2021. We thank these leaders for their generosity.

The University of Delaware occupies lands vital to the web of life for Lenni Lenape and Nanticoke, who share their ancestry, history, and future in this region. UD has financially benefited from this regional occupation as well as from Indigenous territories that were expropriated through the United States land grant system. European colonizers and later the United States forced Nanticoke and Lenni Lenape westward and northward, where they formed nations in present-day Oklahoma, Wisconsin, and Ontario, Canada. Others never left their homelands or returned from exile when they could. We express our appreciation for ongoing Indigenous stewardship of the ecologies and traditions of this region. While the harms to Indigenous people and their homelands are beyond repair, we commit to building right relationships going forward by collaborating with tribal leadership on actionable institutional steps.

LSST Science Drivers

Probing Dark Energy and Dark Matter

An unprecedented inventory of the Solar System from threatening NEO to the distant Oort Cloud

LSST Science Drivers

LSST Science Drivers

Exploring the Transients and Variable Universe

10M astrophysical alerts per night

picked up and distributed worldwide by brokers like Lasair

image credit ESO-Gaia

LSST Science Drivers

Mapping the Milky Way and Local Volume

via resolved stellar population

17B stars characterized in color, variability, position

Rubin Observatory

Site: Cerro Pachon, Chile

Funding: US NSF + DOE

Status: final phases of construction - completion expected 2023

September 2016

Fabruary 2020

May 2022

May 2022

what's in a name?

Rubin Obs is the first ground-based US National Observatory named after a woman astrophysicist, Dr. 

Vera Florence Cooper Rubin  

pioneered studies of Dark Matter through rotational curves

VRO

8m Telescope

9.6 deg.sq. field of view

maximizes survey entendue

Observatory

May 2022 - Telescope Mount Assembly

Status: ongoing demonstration of the Camera/Secondary Mirror (M2) removal procedures, and  ComCam installation expected in  August.

The DOE LSST Camera - 3.2 Gigapixel

3.2 Gigapixel camera 

378 4K ultra-high-definition TV

The DOE LSST Camera - 3.2 Gigapixel

Camera and Cryostat integration completed at SLAC in May,

Shutter and filter auto-changer integrated into camera body

3024 science raft amplifier channels, only 3 are substandard.

Rubin ugrizy filters

Summer 2021

AuxTel:

latest run June 28-July 1 2022

LOVE: LSST Operations Visualization Environment

Telescope Mount Assembly complete 

October 2022

3-mirror Optical System Ready for Testing

July 2023

ComCam: Engineering First Light

September  2023

LSSTCam: System First Light

February  2024

Operations Readiness Review completed

June  2024

The Rubin Observatory Construction Project

Current

Forecast

Rubin LSST

https://www.lsst.org/about/project-status

Rubin Montly Updates page

Current

Forecast

the Rubin LSST

Science Collaborations

The Rubin Organization is almost as complex as the Universe it will explore!

Rubin LSST Science Collaborations

8 SCs - 6 continents - 2000 people - 25 countries

Rubin LSST Science Collaborations

A direct line to Project through dedicated Rubin liaisons, 

responsibility and right to participate in decision making committees, benefitting from the expert knowledge and develop new LSST-based collaborations

Why should I join?

https://www.youtube.com/watch?v=MXQQzbC5HxY&t=69s

If you are a transient fan, from variable stars to kilonovae... TVS is for you!

https://lsst-tvssc.github.io/

If you are a transient fan, from variable stars to kilonovae... TVS is for you!

Rubin Observatory's LSST

First ground based US National Observatory named for a woman, Dr. 

Vera Florence Cooper Rubin  

July 23, 1928 – December 25, 2016

LSST: the Legacy Survey of Space and Time

 will be delivered by
Rubin Observatory,
as its first, 10-year, project

survey specification

5 Deep Drilling Fields fields observed to higher cadence and more images (~18k)

Current baseline footprint

Wide Fast Deep survey

single image depth ~24

10-year stack image depth ~27

image resolution 0.2'' (seeing limited)

18,000 sq degrees 

815 images over 10 years in 6 filters

2 images per night

each fields reobserved within ~days

mini and micro-surveys

Targets of Opportunity

survey specification

5 Deep Drilling Fields fields observed to higher cadence and more images (~18k)

Current baseline footprint

Wide Fast Deep survey

single image depth ~24

10-year stack image depth ~27

image resolution 0.2'' (seeing limited)

18,000 sq degrees 

815 images over 10 years in 6 filters

2 images per night

each fields reobserved within ~days

mini and micro-surveys

Targets of Opportunity

survey specification

5 Deep Drilling Fields fields observed to higher cadence and more images (~18k)

Current baseline footprint

Wide Fast Deep survey

single image depth ~24

10-year stack image depth ~27

image resolution 0.2'' (seeing limited)

18,000 sq degrees 

815 images over 10 years in 6 filters

2 images per night

each fields reobserved within ~days

mini and micro-surveys

Targets of Opportunity

survey specification

single image depth ~24

10-year stack image depth ~27

image resolution 0.2'' (seeing limited)

18,000 sq degrees 

815 images over 10 years in 6 filters

2 images per night

each fields reobserved within ~days

5 Deep Drilling Fields fields observed to higher cadence and more images 

additional mini and micro-surveys

 ToO

At this level of precision,everything is variable, everything is blended, everything is moving.

https://ls.st/srd

Bianco et al 2022

PSTN-054

SDSS

LSST

Rubin Data Products

Rubin Data Products

Rubin Data Products

Rubin Data Products

Subsystem scientist for Data Management Leanne Guy

Rubin Data Access

Subsystem scientist for Data Management Leanne Guy

Exploratory analysis through browsing and visualisation of available datasets guided  by science cases. 

Visualization of LSST Images.

Subsetting via forms, ADQL.

Plotting basic scientific graphics with linked data selection across plots and images.

Rubin Data Access

Subsystem scientist for Data Management Leanne Guy

Rubin Data Access

E. Bellm https://project.lsst.org/meetings/rubin2021/content/alert-brokers

Astronomy’s Discovery Chain

Discovery Engine

10M alerts/night

Community Brokers

target observation managers

the astronomy discovery chain

~1000 images per night

10M alerts per night (5sigma changes)

17B stars Ivezic+18

~10 million QSO Mary Loli+21

∼200 quadruply-lensed quasars Minghao+19

~50 kilonovae Setzer+19, Andreoni+19   (+ ToO)

~1000 SNe every night in the LSST sky

(10K/year) LSST SCs 2009

Rubin Transients by the number

~1000 images per night

10M alerts per night (5sigma changes)

17B stars Ivezic+18

~10 million QSO Mary Loli+21

∼200 quadruply-lensed quasars Minghao+19

~50 kilonovae Setzer+19, Andreoni+19   (+ ToO)

~1000 SNe every night in the LSST sky

(10K/year) LSST SCs 2009

Rubin Transients by the number

~1000 images per night

10M alerts per night (5sigma changes)

17B stars Ivezic+18

~10 million QSO Mary Loli+21

∼200 quadruply-lensed quasars Minghao+19

~50 kilonovae Setzer+19, Andreoni+19   (+ ToO)

~1000 SNe every night in the LSST sky

(10K/year) LSST SCs 2009

Rubin Transients by the number

~1000 images per night

10M alerts per night (5sigma changes)

17B stars Ivezic+18

~10 million QSO Mary Loli+21

∼200 quadruply-lensed quasars Minghao+19

~50 kilonovae Setzer+19, Andreoni+19   (+ ToO)

~1000 SNe every night in the LSST sky

(10K/year) LSST SCs 2009

Rubin Transients by the number

~1000 images per night

10M alerts per night (5sigma changes)

17B stars Ivezic+18

~10 million QSO Mary Loli+21

∼200 quadruply-lensed quasars Minghao+19

~50 kilonovae Setzer+19, Andreoni+19   (+ ToO)

~1000 SNe every night in the LSST sky

(10K/year) LSST SCs 2009

Rubin Transients by the number

~1000 images per night

10M alerts per night (5sigma changes)

17B stars Ivezic+18

~10 million QSO Mary Loli+21

∼200 quadruply-lensed quasars Minghao+19

~50 kilonovae Setzer+19, Andreoni+19   (+ ToO)

~1000 SNe every night in the LSST sky

(10K/year) LSST SCs 2009

Rubin Transients by the number

From Marisol Carnero's slides: 

Rare can become common in LSST!

Rubin will see ~1000 SN every night!

Credit: Alex Gagliano

LSST will observe about half of the sky close to 1000 times over 10 years.

Astronomy (re)meets Data Science

Nightly data rates

Rubin Data Products and the DM team

Science Pipeline v 23.0.0 released late 2021 (and v23.0.1 April 2022)

Rubin env rubin-env 4.0.0. deployed May 2022

Migration of accounts from NCSA to SLAC has started

Deployed alert distribution system - testing connection w alert brokers Jan 2022

Rubin Data Products and the DM team

Data Management verification phase:

Faro is a framework for automatically and efficiently computing scientific performance metrics on the LSST data products, a collaborative project between Rubin Data Management (DM) and System Integration, Test and Commissioning (SIT-Com) as part of a single coordinated project-wide science verification effort and with a view to Operations (see https://www.youtube.com/watch?v=XrhNkdK8hiw&list=PLPINAcUH0dXacwsNrhNnQSq0rOTRf0IfU&index=3&t=6s)

distributions of time gaps in 76 OpSims

Rubin LSST survey design

The survey strategy is being refined and will continue to be re-evaluated in Operations

The Survey Cadence Optimization Committee - SCOC

Minisurveys

Rubin LSST survey design

150

1200

Nvisits

SCOC Workshop, November 2-3 2022

https://project.lsst.org/meetings/scoc-sc-workshop3/

Recommendation to the Director due on December 2022

Current baseline footprint

https://www.lsst.org/content/charge-survey-cadence-optimization-committee-scoc

24.6

24.6

26.8

28

26.9

28.1

5s depth

5s depth

coadd 5s depth

coadd 5s depth

source http://astro-lsst-01.astro.washington.edu:8080/?runId=2

23.0

22.5

0.576

0.52

intranight gap

hours

15

internight gap

days

15

internight gap

days

50

5

internight gap

days

source http://astro-lsst-01.astro.washington.edu:8080/?runId=2

3

0.57

0.52

14

4

internight gap

days

hours

0.576

0.52

intranight gap

hours

source http://astro-lsst-01.astro.washington.edu:8080/?runId=2

Gaia - LSST Comparison and Synergies

We argue, based on the experience with SDSS, that surveys should release data as early and often as possible incorporating incremental improvements in each subsequent release, as opposed to holding off for a single, big, final release.

2011

Gaia - LSST Comparison and Synergies

In the context of Gaia, the LSST can be thought of as its deep complement (for a detailed discussion, we refer the reader to IBJ2012). Gaia will provide an all-sky catalog with unsurpassed trigonometric parallax, proper-motion, and photometric measurements to r∼20, for about 1 billion stars. The LSST will extend the static map to r∼27 over half of the sky, detecting about 20 billion stars.

2015

Text

Comparison of SDSS, LSST, Gaia  

Galactic science

The extension of Gaia through 2025 (?) would allow a ~2 years overlap with LSST

Ivezić, Beers, Jurić 2012, ARA&A, 50, 251

Rubin does not have spectroscopy... but you cannot blame us for trying

Because LSST will have exquisite image quality we may be able to measure color from atmospheric diffraction

Astrometric Redshifts for Quasars (SDSS)

Michael C. Kaczmarczik+2009

Quasar Astrometric Redshifts with LSST

Christina M. Peters, Richards, Yu...LSST AGN SC Roadmap

Astrometric offsets (in arcseconds) for combined, multi-epoch observations of 6430 SDSS quasars in stripe 82.

Rubin does not have spectroscopy... but you cannot blame us for trying

Riley Clarke, Davenport, Gizis, Bianco, in prep

5,000K flare on dM

40,000K flare on dM

-0.15

Because LSST will have exquisite image quality we may be able to measure color from atmospheric diffraction

from rare to statistical samples

Stephen T. Ridgway+ 2014

THE VARIABLE SKY OF DEEP SYNOPTIC SURVEYS

arXiv:1409.3265

Ivezić, Beers, Jurić 2012, ARA&A, 50, 251

Comparison of SDSS, Gaia and LSST for main sequence stars

Gaia: excellent astrometry and photometry r < 20 (more??)

LSST: photometry (5sigma) to r < 27.5 and time resolved measurements to r < 24.5

LSST proper motion and trigonometric parallax errors are similar around r=20

"The Milky Way disk “belongs” to Gaia, and the halo to LSST (plus very faint and/or very red sources, such as white dwarfs and LT(Y) dwarfs)." Z. Ivezich - 2021

 ZZ Cetis: 1-3% r.m.s. pulsation

(~1000 ZZ Cetis detected if pulsation 3% in r)

Pulsation stars

• The different colors provided by LSST will enable the temperature determinations. When combined with distances, it will be possible to obtain luminosities. Thus LSST will provide the opportunity to generatea pulsational H-R diagram

• Stellar Envelop Tomography of long-period variables to probe probing layers of different atmospheric depths (Alvarez 2001)... in 6 filters. But these methodologies largely rely on NIR filters, can it be done with z and Y?

• with DDF pulsations of ~hour can be constrained: Red Giant pulsators

K. Humbleton

TVS Roadmap - https://lsst-tvssc.github.io/

et al.

Demonstrated synergies in stellar population studies and distance scales thanks to the magnitude overlap of the surveys

Powerful tools to infer individual distance s independently of reddening uncertainty

et al.

Demonstrated synergies in stellar population studies and distance scales thanks to the magnitude overlap of the surveys

Micro- and meso-lensing for stellar physics

-  detect microlensing events where both the lens and source lie in the Magellanic Clouds, and explore stellar and stellar remnant populations in another galaxy.

- LSST will investigate the mass distribution offaint objects in the local neighborhood, such as low mass dwarfs, stellar remnants, andfree-floating planets.

TVS Roadmap - https://lsst-tvssc.github.io/

Rachel Street co-chair of TVS

Somayeh Khakpash, chair of microlensingsubgroup

Abbott+2021

Corral Santana+2016

Thompson et al. 2019, Liu+2020, Shenar+2022
Rivinius+2020, Jayasinghe+2021

Sahu+2022
Lam+2022, Mróz+2022

Micro- and meso-lensing for stellar physics

• detect microlensing events where both the lens and source lie in the Magellanic Clouds, and explore stellar and stellar remnant populations in another galaxy.
• LSST will investigate the mass distribution offaint objects in the local neighborhood, such as low mass dwarfs, stellar remnants, andfree-floating planets.

Survey coordination

Rubin             +                Roman

Street + 2018, arxiv/1812.04445

TVS Roadmap - in preparation

Rachel Street co-chair of TVS

Somayeh Khakpash, chair of microlensingsubgroup

Ivezić, Beers, Jurić 2012, ARA&A, 50, 251

200,000 L / T dwarfs in LSST with proper motion and trigonometric parallax measurements

2400 T dwarfs with >5σ proper motion and parallax measurements

Compared to UKIDSS, 5 times larger sample of T dwarfs, with parallaxes and 10-20 times more accurate proper motions (~100 Y dwarfs)

https://sites.google.com/inaf.it/lssteurope4

A hybrid conference

Tuesday 10/25 12:00PM SYNERGIES WITH GAIA

G. Clementini (25+5 min), Synergies between Rubin-LSST and Gaia variability
E. Pancino (25+5 min), Synergies between Rubin-LSST and Gaia astrometry/spectroscopy

thank you!

University of Delaware

Department of Physics and Astronomy

Biden School of Public Policy and Administration

Data  Science Institute

federica bianco

fbianco@udel.edu