Standard candles in the Gaia perspective

Standard candles in the Gaia perspective Laurent Eyer, L. Palaversa, N. Mowlavi, P.Dubath Geneva Observatory and S.Leccia, G.Clementini, et al., T.Lebzelter et al., Gaia CU7 DPAC Naples, May 6 2011

Plan of the talk Quick reminder on Gaia Standard Candles measured by Gaia Gaia Data Processing and Analysis Consortium activities Location: L2

The Gaia mission Satellite of the European Space Agency Observations of all the objets between than ~6 < V < ~20, about 1 billion objects Astrometry, photometry, spectrophotometry, and spectroscopy (radial velocities) Length: 5 (+1) years (70 times all sky) Launch (Soyuz rocket, French Guyana) 2013 Final Results: 2021 Location: L2

The astrometric performance: Mission Critical Design Review (April 2011):

The astrometric performance: Mission Critical Design Review (April 2011): Mean parallax error end of mission Position error ( as):... x ~0.7 Proper motion error ( as/year):... x ~0.5

10 micro arcsec is very,

10 micro arcsec is very, very,

10 micro arcsec is very, very, very,

10 micro arcsec is very, very, very, very small

Plan of the talk Quick reminder on Gaia Standard Candles measured by Gaia Gaia Data Processing and Analysis Consortium activities Location: L2

Standard candles in the perspective of Gaia Cepheids/RR Lyrae stars Long Period Variables, Mira, SR, OSARG Eclipsing binaries Others... (Supernovae, Novae,..., etc...)

General impact of Gaia Astrometry Calibration star luminosity Astrometric binary stars Calibration of primary distance indicators Photometry/Spectrophot. Detection of new cepheids, new RR Lyrae, new eclipsing systems... etc... Test of universality of standard candles RVS Physical parameters: Wilson-Devinney Baade Weselink method Detection of new standard candles such as OSARG in OGLE

Few numbers: RR Lyrae stars Galactic Observed 186 Hipparcos 1997 1,635 ASAS catalogue, as in 2011 Pojmanski ~4,000 LINEAR, Sesar, inprogress 16,836 OGLE, bulge, Soszynski 2011

Few numbers: RR Lyrae stars Galactic Observed 186 Hipparcos 1997 1,635 ASAS catalogue, as in 2011 Pojmanski ~4,000 LINEAR, Sesar, inprogress Estimated for Gaia 16,836 15,000-40,000 70,000 OGLE, bulge, Soszynski 2011 bulge Eyer & halo Cuypers (2000) optimist: Gaia will multiply by nearly 5 the Galactic RR Lyrae number

Few numbers: Cepheids Galactic Observed 273 509 Hipparcos 1997 Fernie et al. 1995 455 Berdnikov et al 2000 872 ASAS catalogue, as in 2011 Pojmanski

Few numbers: Cepheids Galactic Observed 273 509 Hipparcos 1997 Fernie et al. 1995 455 Berdnikov et al 2000 872 ASAS catalogue, as in 2011 Pojmanski Estimated for Gaia 2,000-8,000 Eyer & Cuypers (2000) 9,000 Windmark (2011) optimist: Gaia will multiply by 10 the Galactic Cepheid number

Few numbers: Long Period Variables (M, SR, OSARG)

Few numbers: Long Period Variables (M, SR, OSARG) Galactic Observed 1,238 2,793 (Mira) 2,691 Hipparcos 1997 ASAS catalogue, as in 2011 Pojmanski Bulge, OGLE-II Groenewegen et al. 2005

Few numbers: Long Period Variables (M, SR, OSARG) Galactic Observed 1,238 2,793 (Mira) 2,691 Hipparcos 1997 ASAS catalogue, as in 2011 Pojmanski Bulge, OGLE-II Groenewegen et al. 2005 Estimated for Gaia 200,000 Eyer & Cuypers (2000) Mira? optimist: Gaia will multiply by nearly 40 the Galactic LPVs

Few numbers: Eclipsing binaries Galactic Observed 917 5,911 Hipparcos 1997 ASAS catalogue, as in 2011 Pojmanski

Few numbers: Eclipsing binaries Galactic Observed 917 5,911 Hipparcos 1997 ASAS catalogue, as in 2011 Pojmanski Estimated for Gaia 500,000 Söderhjelm 2004 6,000,000 Zwitter 2002

Few numbers: Eclipsing binaries Galactic Observed 917 5,911 Hipparcos 1997 ASAS catalogue, as in 2011 Pojmanski Estimated for Gaia 500,000 Söderhjelm 2004 6,000,000 Zwitter 2002 3,000,000 Eyer & Cuypers 2000 optimist: Gaia will multiply by nearly 1000 the Galactic eclipsing binaries

Plan of the talk Quick reminder on Gaia Standard Candles measured by Gaia Gaia Data Processing and Analysis Consortium activities Location: L2

The DPAConsortium: the global view Two main concepts:

The DPAConsortium: the global view Two main concepts: 1. Coordination Units CU1 Architecture CU3 Astrometry CU2 Simulation CU4 Objects CU5 Photometry CU6 Spectroscopy CU7 Variability CU8 A.P.

The DPAConsortium: the global view Two main concepts: 1. Coordination Units 2. Data Processing Centres CU1 Architecture CU3 Astrometry CU2 Simulation ESAC/BPC/OAOT BPC/CNES CU4 Objects CU5 Photometry CU6 Spectroscopy CU7 Variability CU8 A.P. CNES Cambridge CNES ObsGE/ISDC CNES

The goal of the consortium Produce a catalogue Data products that are useful for scientific community Help and maximise the scientific exploitation No proprietary data, ESA has the data rights, until public release New Coordination Unit CU9: data access, archive

The schedule: more than 25 years of work! 1993 1994 1995 1996 1997 1998 1999 2000 2005 2010 2015 2020 2021 Figure courtesy Michael Perryman and François Mignard Proposal Definition Implementation Operation Data Processing 2004 2003 2002 2001 Concept & Technology Study Mission Selection Re-Assessment Study Studies Phase B1 2009 2008 2007 2006 Selection of Prime Contractor (EADS Astrium) Phase B2 Phase C/D 2014 2013 2012 2011 Launch 2013 Software Development 2019 2018 2017 2016 Scientific operation Mission Data Processing Mission Products Intermediate Final Now 17

Operation scenario: The van Leeuwen chart Days of Data 0 30 60 90 120 150 180 210 240 270 300 330 360 390 420 450 480 510 540 570 600 630 660 690 720 750 780 810 840 870 900 930 960 990 Launch End of Segment 03 End of Segment 02 End of Segment 01 End of Segment 00 L2 MDB-INIT First Data CDM-INIT-00 IOCR IDT FL AIM BAM CU6-Daily SCI Alerts IDT-00 re-runs PHOTPIPE PHOT-CAT-00 MDB-INT-00 MDB-00 End of Cycle 00 AGIS trials IDU trials IDU-XM-01 PHOT-CAT-01 AGIS-01 MDB-INT-01 IDT-02 Catalogue rev. MDB-01 End of Cycle 01 IDU-CAL-02 IDU-MAIN-02 AGIS-02 PHOTU-02 IDU-XM-02 PHOT-CAT-02 MDB-INT-02 MDB-02 End of Cycle 02 AGIS-03 End of AGIS-03 End of IDU-CAL-03 IDU-CAL-03 IDU-MAIN-03 PHOTU-03 IDU-XM-03 PHOT-CAT-03 0 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 32 33 34 35 36 3 Main Dates: Launch: 13/12/12 L2: Launch + 1 mo First Data: Launch + 3 mo IOCR: Launch + 4 mo Segment 00: 180 days Segment 01: 180 days Segment 02: 180 days Segment 03: 360 days Cycle 00: 225 days Cycle 01: 195 days Cycle 02: 165 days Cycle 03: 360 days Changes since previous issue : Cycle 00 IOCR = Launch + 4mo Insertion L2 = Launch + 1mo Insertion IDT-00 re-runs x 3 : 5 days, 5 days, 20 days CDM-INIT-00: beginning at (First Data + 45 days), duration = 30 days Cycle 01 Insertion IDU trials: 100 days in parallel of AGIS trials Move of AGIS-02 to AGIS-01: after PHOT-CAT-01 and before MDB-INT-01 AGIS-01 = 15 days IDT Catalogue revision during MDB-INT-01 Cycle 01 is extended by 15 days Cycle02 Insertion of PHOT-U-02 Cycle03 Segment 03 duration extended from 180 days to 360 days Assumptions/Constraints: CDM-INIT-00 succesfully calibrated by Cycle 00 IDT reruns at 6 times speed AGIS trials and IDU trials are successfull in Cycle 01 AGIS-01 converges with 12 mo of data IDU processes 360 days of data in 70 days in Cycle 02 DPCI facilities allow to process PhotPipe and Phot-U in parallel in Cycle 02 (Not all CU3 and CU5 SW products are included in this diagram) Limitation: astrometry needs 18 month solution MDB-INT-03 MDB-03 End of Cycle 03

CU7 Variability Analysis functional analysis

CU7 Variability Analysis functional analysis Period search algorithms and modelling the light curves (J.Cuypers)

CU7 Variability Analysis functional analysis

CU7 Variability Analysis functional analysis 1) Supervised 2) Extraction 3) Unsupervised

Classification (J. De Ridder) Goal:Classification in variability types with membership probability

Classification (J. De Ridder) Goal:Classification in variability types with membership probability Confusion Matrix for Hipparcos periodic variables (random forest) Dubath et al. 2011

Classification (J. De Ridder) Goal:Classification in variability types with membership probability Confusion Matrix for Hipparcos periodic variables (random forest) Dubath et al. 2011 Richards et al. 2011

CU7 Variability Analysis functional analysis

CU7 Variability Analysis functional analysis SOS

CU7 Variability Analysis functional analysis SOS Specific Object Studies

Specific Object Studies N.Mowlavi (ObsGe/ISDC)

Cepheid/RR Lyrae Clementini WorkPackage 1. Determine the Fourier parameters

Cepheid/RR Lyrae Clementini WorkPackage 1. Determine the Fourier parameters Leccia et al, see poster

Cepheid/RR Lyrae Clementini WorkPackage 1. Determine the Fourier parameters 2. Identify Blazhko RR Lyrae stars and double mode RR Lyrae/Cepheids Leccia et al, see poster

Cepheid/RR Lyrae Clementini WorkPackage 1. Determine the Fourier parameters 2. Identify Blazhko RR Lyrae stars and double mode RR Lyrae/Cepheids 3. Identify pulsation mode Leccia et al, see poster

Cepheid/RR Lyrae Clementini WorkPackage 1. Determine the Fourier parameters 2. Identify Blazhko RR Lyrae stars and double mode RR Lyrae/Cepheids 3. Identify pulsation mode 4. Determine stellar parameters Petersen Diagram Baade-Wesselink analysis Leccia et al, see poster

Cepheid/RR Lyrae Clementini WorkPackage 1. Determine the Fourier parameters 2. Identify Blazhko RR Lyrae stars and double mode RR Lyrae/Cepheids 3. Identify pulsation mode 4. Determine stellar parameters 5. Identify binarity Petersen Diagram Baade-Wesselink analysis Leccia et al, see poster

Cepheid/RR Lyrae Clementini WorkPackage 1. Determine the Fourier parameters 2. Identify Blazhko RR Lyrae stars and double mode RR Lyrae/Cepheids 3. Identify pulsation mode 4. Determine stellar parameters 5. Identify binarity Petersen Diagram Baade-Wesselink analysis Leccia et al, see poster 6. Determine period changes

Long Period Variables T.Lebzelter WorkPackage

Long Period Variables T.Lebzelter WorkPackage 1.Quantify the irregularity of the light curve

Long Period Variables T.Lebzelter WorkPackage 1.Quantify the irregularity of the light curve 2.Determine the star luminosity

Long Period Variables T.Lebzelter WorkPackage 1.Quantify the irregularity of the light curve 2.Determine the star luminosity Bolometric correction

Long Period Variables T.Lebzelter WorkPackage 1.Quantify the irregularity of the light curve 2.Determine the star luminosity Bolometric correction 3.Sub-classify

Long Period Variables T.Lebzelter WorkPackage 1.Quantify the irregularity of the light curve 2.Determine the star luminosity Bolometric correction 3.Sub-classify EROS data, Spano et al., in preparation

Long Period Variables T.Lebzelter WorkPackage 1.Quantify the irregularity of the light curve 2.Determine the star luminosity Bolometric correction 3.Sub-classify Note: astrometric shifts of the photocentre studied by CU4 EROS data, Spano et al., in preparation

Eclipsing binaires Eyer WorkPackage 1.Improve period

Eclipsing binaires Eyer WorkPackage 1.Improve period 2. Sub-classify e.g. Pojmanski: ED, ESD, EC, EOC

Eclipsing binaires Eyer WorkPackage 1.Improve period 2. Sub-classify e.g. Pojmanski: ED, ESD, EC, EOC 3.Determine the light curve geometry Durations Depths Phases of primary and secondary eclipses

Eclipsing binaires Eyer WorkPackage 1.Improve period 2. Sub-classify e.g. Pojmanski: ED, ESD, EC, EOC 3.Determine the light curve geometry Durations Depths Phases of primary and secondary eclipses 4.Update probability of being an eclipsing binary

Conclusion: Probst 1974 pyramid Text

Conclusion: Probst 1974 pyramid Text Gaia is a unique mission putting together: astrometry, photometry, spectroscopy

The end Thank you for your attention!