Variable stars with LSST

Wednesday, 13 June 2018

Laurent Eyer University of Geneva, Switzerland

LSST@Europe3, Lyon, France

LBV

Stars

AGN

Stars

Asteroids

RotationEclipse

Microlensing CataclysmicEruptive PulsationSecular

Novae

(DAV) H-WDs

Variability Tree

Extrinsic Intrinsic

NSupernovae

SN

Symbiotic

ZAND

Dwarf novae

UG

Eclipse

Asteroid occultation

Eclipsing binary

Planetary transits

EA

EB

EW

Rotation

ZZ CetiPG 1159

Solar-like

(PG1716+426 / Betsy)long period sdB

V1093 Her

(W Vir / BL Her)Type II Ceph.

δ Cepheids

RR Lyrae

CWCredit: Eyer et al. (2018)Adapted from: Eyer & Mowlavi (2009)

δ Scuti

γ Doradus

Slowlypulsating B stars

α Cygni

β Cephei

λ Eri

SX Phoenicis

SXPHE

Hot OB Supergiants

ACYG

BCEP

SPB

SPBe

GDOR

DST

PMSδ Scuti

roAp

MirasIrregulars

Semi-regulars

M

SR

L

Small ampl.red var.

(DO,V GW Vir)He/C/O-WDs

PV TelHe star

Be stars

RCB

GCASFU

UV Ceti

Binary red giants

α2 Canes VenaticorumMS (B8-A7) withstrong B fields

SX ArietisMS (B0-A7) withstrong B fields

Red dwarfs(K-M stars)

ACV

BY Dra

ELL

FKCOMSingle red giants

WR

SXA

β Per / α Vir

RS CVn

PMS

S Dor

Eclipse

(DBV) He-WDs

V777 Her

(EC14026)short period sdB

V361 Hya

RV Tau

Photom. PeriodFG SgeSakurai

V605 Aql

R Hya (Mira-type)δ Cep (Cepheid)

DY Per BLAP

LPV

OSARGSARV

CEPRR

RV

The variability tree: A temptative to organise variable phenomena in the Universe

2Dmap

ChemistryAstroph.parametersRadialVelocity

Colour-ColourDiag.HRdiagramsofclustersAstroph.parameters

Singleepoch

Luminosi?esHRDiagram

Parallax3DmapPropermo?on

Mul?-epoch

Variability:-Standardcandles-VariablestarsastracersofPop.-Probing“invisible”(microlensing)-Asteroseismology(masse,age,lum.)-Astroph.parameters(binaries,Baade-Wesselinkmethod,etc.)

Variablestars

Variablestars:Binaries,exoplanets,…Dopplerimaging

+neutrinos,cosmicrays,gravita?onalwaves,…. Astrometry

Photometry Spectroscopy

Eyer 2018

The multi-epoch LSST photometry

Time allocation:

u: 8%; g: 10%

r: 22%; i: 22%

z: 19%; y: 19%

One visit corresponds to one photometric band observation

(non-simultaneous, filter are non-sequential for a given field)

Courtesy of Z.IvezicThis for 20 billion stars!

>800 visits over 10 years

LSST/Gaia photometry and astrometry

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

Complementarity of the Gaia and LSST surveys: photometric, proper motion and trigonometric parallax errors are similar around r=20

LSST: Two exposures of 15 seconds (or maybe one of 30 seconds) 3-5 days back on the same field

Chapitres chosis de physique stellaire: photométrie et variabilité des étoiles (L. Eyer et N. Mowlavi)

50,000 stars 396,000 measurements

Geneva photometry: colour-colour diagramme

Chapitres chosis de physique stellaire: photométrie et variabilité des étoiles (L. Eyer et N. Mowlavi)

Sesar et al. 2007

GeneraldescripFonofvariabilityFracFonofVariableswithSDSS

Hertzsprung-Russelldiagramme

GaiaCollaboration, Babusiaux et al. 2018

LSST

Fraction of variable stars with Gaia in HR diagramme

GaiaCollaboration, Eyer et al. 2018

Variability types in the HR diagram

GaiaCollaboration, Eyer et al. 2018

Motion in colour-colour diagramme

2yearsappart

Ivezic et al. 2007

3hoursappart

with SDSS data

https://www.youtube.com/watch?v=Pcy4U5uvL8I

Motions in the Colour-Absolute Magnitude Diagram

“Pollock” diagram

GaiaCollabora?on,Eyeretal.2018

With LSST filters system will be remarkable

source_id: 4660498360447427840 period: 10.441275 d

mag

nitu

de

13.5

14.0

14.5

15.0

15.5

16.01700 1800 1900 2000 2100 2200 2300

G: 108 (5)14.314.414.514.614.714.814.915.015.115.215.3

0 0.5 1.0 1.5

GBP: 106 (0)14.714.814.915.015.115.215.315.415.515.615.7

0 0.5 1.0 1.5

GRP: 106 (0)13.713.813.914.014.114.214.314.414.514.614.7

0 0.5 1.0 1.5

Classification & SOS: CEP

BJD - 2455197.5 (TCB) phase phase phase

source_id: 4660498360447427840 period: 10.441275 d

mag

nitu

de

13.5

14.0

14.5

15.0

15.5

16.01700 1800 1900 2000 2100 2200 2300

G: 108 (5)14.314.414.514.614.714.814.915.015.115.215.3

0 0.5 1.0 1.5

GBP: 106 (0)14.714.814.915.015.115.215.315.415.515.615.7

0 0.5 1.0 1.5

GRP: 106 (0)13.713.813.914.014.114.214.314.414.514.614.7

0 0.5 1.0 1.5

Classification & SOS: CEP

BJD - 2455197.5 (TCB) phase phase phase

Extracted scientific information: • Variability type: Classical Cepheid • Period: 10.44 days • Amplitude, absolute brightness,

effective temperature, etc…

Variability Processing and Analysis

source_id: 4660498360447427840 period: 10.441275 d

mag

nitu

de

13.5

14.0

14.5

15.0

15.5

16.01700 1800 1900 2000 2100 2200 2300

G: 108 (5)14.314.414.514.614.714.814.915.015.115.215.3

0 0.5 1.0 1.5

GBP: 106 (0)14.714.814.915.015.115.215.315.415.515.615.7

0 0.5 1.0 1.5

GRP: 106 (0)13.713.813.914.014.114.214.314.414.514.614.7

0 0.5 1.0 1.5

Classification & SOS: CEP

BJD - 2455197.5 (TCB) phase phase phase

Time series of 3 colour bands for Gaia: • G(aia) = most visible light • R(ed) • B(blue) • + position, parallax (distance), motion

source_id: 4660498360447427840 period: 10.441275 d

mag

nitu

de

13.5

14.0

14.5

15.0

15.5

16.01700 1800 1900 2000 2100 2200 2300

G: 108 (5)14.314.414.514.614.714.814.915.015.115.215.3

0 0.5 1.0 1.5

GBP: 106 (0)14.714.814.915.015.115.215.315.415.515.615.7

0 0.5 1.0 1.5

GRP: 106 (0)13.713.813.914.014.114.214.314.414.514.614.7

0 0.5 1.0 1.5

Classification & SOS: CEP

BJD - 2455197.5 (TCB) phase phase phase

Variability Processing and Analysis

Courtesy of B.Holl

LSST: 6 bands!

LSSTwillhaveaveryimportantimpactonperiodobjects

Inthephasespaceobserva?onsoverlaps

However,thespectralwindowofthecadenceiscurrentlynotop?mal

VanderplasandIvezic2015developedaperiodsearchthatusesallbands

Manydiscussionsonthecadence…

MichaelJonhsonshoweditworksremarkablywell

Spectralwindowsfromvarioussurveys

Eyer et al. 2009

SpectralwindowsfromLSST

IcontactedZeljko

LynneJonesefficientlytransmiYedmefewfiles

Principal component analysis

• Idea:

• Proposed by Paul Bartholdi 2005

• Applied to the Geneva constant stars (results: some are variable!)

• Perform the period search on the “new magnitude” (first component)

• Characterize the physical properties of stars

• Tests on Geneva Photometry, and on SDSS stripe 82

u

−0.5 0.0 0.5

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vm

RR Cet RR Lyrae

50,000 stars

Geneva photometry

u

−3 −2 −1 0 1 2 3

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vm

3 C 273 AGN

PrincipalcomponentanalysisonSDSSstripe82data

Süveges et al. 2012

LSST should not have difficulties to determine the physical origin of variability

LSST will be able to compare population of variables in different systems

OGLE-II SMCOGLE-II LMC

Eyer 2002

FocusonEclipsingbinariesthankstoKepler

Kepleris``game-changer”,unprecedentedsampling/photometricprecision

Onesurprise:18%arenotregular(witheclipseschanging/disappearing)

70%shouldbedetectedbyLSST-rbanddetec?on-(Wellsetal.2017)

80%whenotherbandsaretakenintoaccount(Pršaprivatecom.)

Keplerallowstostudyperformanceforotherprojects

Foreclipsingbinaries:

Kepleriscompleteto10daysfortheselectedsampleofF,G,Kstars(Kirketal2016)

1, 30 minutes

LSST will detect 24 million eclipsing binaries (Prša et al. 2011)

DetecFonofbinaries:specialeclipsingbinariesDoubleWhiteDwarf

Study by Korol et al. 2017

Ultra compact detached white dwarfs

LSSTandstandardcandlesstars

LSSTwillprobeverylargedistances

Discovery of distant RR Lyrae stars in the Milky Way using DECam

Medinaetal.2018

completetoover350kpc!

LSSTandstandardcandlesstarsRRLyraestarsinthehalowithPS1datafromSesaretal2017

up to 130 kpc

Thank you for your attention