Variable stars with LSSTindico.in2p3.fr/event/16341/contributions/... · Variable stars with LSST...
31
Variable stars with LSST Wednesday, 13 June 2018 Laurent Eyer University of Geneva, Switzerland LSST@Europe3, Lyon, France
Transcript of Variable stars with LSSTindico.in2p3.fr/event/16341/contributions/... · Variable stars with LSST...
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
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vm
RR Cet RR Lyrae
50,000 stars
Geneva photometry
u
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−0.3 −0.1 0.1 0.3
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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
