Projects on the cosmic distance scale and stellar populations based on pulsating variables

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1 Projects on the cosmic distance scale and stellar populations based on pulsating variables Gisella Clementini INAF - Osservatorio Astronomico, Bologna Coordination Unit 7 - Gaia DPAC Bologna, Giornate di Osservatorio, Feb. 2016

2 RR Lyrae & Cepheids Easily recognizable thanks to the light variations Periods and amplitudes unaffected by distance and reddening, and related to Mass, Luminosity, Teff (Y,Z) constraints on intrinsic stellar parameters Trace populations with different age and chemical composition: t <100 Myr - Classical Cepheids t~1-5 Gyr -Anomalous Cepheids t >10 Gyr (RR Lyrae, Type II Cepheids) Map 3D structures, radial trends, streams hints on how galaxies have formed Most important standard candles in the Local Group (RR Lyrae stars, M V -[Fe/H], PL K Z) and beyond, up to 20 Mpc (Cepheids, PL, PLC, Weseneiht) calibration of secondary indicators measure of H0 OABo Days, Bologna Feb. 2016

3 The team ( over time) F. Cusano (TD-LBT), A. Garofalo (PhD), T. Muraveva (Postdoc), M.I. Moretti, M. Cignoni, M. Palmer V. Ripepi, M. Marconi, S. Leccia, I. Musella (OACn) L. Di Fabrizio (TNG), A. Mercurio, G. Coppola, V. Testa, L. Federici, M. Dall Ora, E. Held, E. Poretti, M. Tosi, C. Cacciari, F. Fusi Pecci L. Baldacci, C. Greco, R. Contreras, G. Fiorentino and several more.

4 RR Lyrae & Cepheids in the MW, M31 and their satellites MW UFDs Gaia M31 satellites

5 RR Lyrae & Cepheids in the MW, M31 and their satellites MW UFDs Gaia M31 satellites

6 RR Lyrae & Cepheids with Gaia Census of Galactic Cepheids: ~ 9000 Classical Cepheids ~ 2000 Type II Cepheids Census of Galactic RR Lyrae: ~70,000 in the MW halo ~ 15-40,000 in the bulge Parallaxes e.o.m. parallax accuracy: 10 μas for V < mag trigonometric distances and absolute calibration via parallax of MV-[Fe/H], PLKZ relations for RRLs and PL, PLC, PW relations for Cepheids DISTANCE SCALE H0 Positions + proper motions RVS metallicities: metallicity distributions of young and old populations Parallaxes + photometry + RVS radial velocities: physics of the census of the RRLs down to G~20.7 mag, spatial distribution, identification and tracement of structures, overdensities, streams, new satellites. MW formation and assembling star, tests of pulsation models, improvement of model input Physics..

7 Gaia variability processing (CU 7) DPAC Coordination Unit 7 (CU7) DPCG (Geneva) L. Eyer (manager) Cepheid & RRLyrae pipeline - G. Clementini (manager) Team: V. Ripepi, S. Leccia, M. Marconi, I. Musella (INAFOACn), L. Szabados (Konkoly Observatory) affiliated contributors & developers + support staff at DPCG (6-7 units) + T. Muraveva OABo postdoc + A. Garofalo PhD at UniBO Support from ASI (grants: ASI I/058/10/0 and ASI R ). but not for science exploitation!!

8 RR Lyrae stars in the LMC as seen by Gaia Gaia OGLE IV Gaia s IoW March 5 th, 2015 Credits: ESA/Gaia/DPAC/CU5/CU7/INAF-OABo Gisella Clementini, Dafydd Evans, Laurent Eyer, Krzysztof Nienartowicz, Lorenzo Rimoldini and the Geneva CU7/DPCG and CU7/INAF-OACN teams. Left panels: G-band light curves of RR Lyrae stars in the Large Magellanic Cloud observed by Gaia during the EPSL scanning. Right panels: I-band light curves obtained for the same stars by the OGLE IV survey.

9 Short period/faint magnitude Cepheids in the LMC observed by Gaia Gaia s IoW May 28 th, 2015 Credits: ESA/Gaia/DPAC/CU5/DPCI/CU7/INAF-OABo/INAF-OACn Gisella Clementini, VincenzooRipepi, Silvio Leccia, Laurent Eyer, Lorenzo Rimoldini, Isabelle Lecoeur-Taibi, Nami Mowlavi, Dafydd Evans, Geneva CU7/DPCG and the whole CU7 team. The photometric data reduction was done with the PhotPipe pipeline at DPCI; processing data were received from the IDT pipeline at DPCE.

10 Gaia Data Release 1 G-DR1: end of Summer 2016 Positions and G magnitude (~all sky, single stars) RR Lyrae & Cepheids in the Ecliptic pole regions TGAS for 2 millions stars in common between Tycho and Gaia catalogues Preparing the release of the EPSL RRLyrae & Cepheids and 2 accompaning papers - Clementini et al RRL&Cep pipeline; 2. PL of TGAS Cepheids

11 The near-infrared YJKs VISTA ESO Public survey of the Magellanic Clouds system Core: Cioni (PI), Bekki, Clementini, Emerson, Evans, de Grijs,Gibson, Girardi, Groenewegen, Ivanov, Marconi, Miszalski, Moore, Napiwotzki, Oliveira, Ripepi, van Loon, Wilkinson, Wood + CASU and WFAU Postdocs: Anders, For, Guandalini, Moretti, Sturm, Subramanian, Muraveva, Tatton

12 VMC survey 61% complete Filters: Y, J, K s Sampling: 0.34 /pix FOV: 1.65 deg 2 Area: 170 deg 2 Sensitivity: YJK s ~22 (5σ Vega) Saturation: K s ~10 Epochs: 3 (YJ) + 12 (K s ) Allocation: 2000 h Time-scale: Cioni et al., A&A, 2011, 527, A116, Paper I Italian team working on variables in VMC funded through: PRIN-INAF 2008 ( ),national PI M.Marconi, OABo PI G. Clementini FP7 GREAT- ITN ( ) G. Clementini PI for INAF both are now over!

13 Cepheid in the LMC Previous studies on classical Cepheids in the SEP and 30 Dor regions indicate a σ~0.07 mag (Ripepi et al. 2012). For Anomalous Cepheids and type II Cepheids the σ~0.1 mag (Ripepi et al. 2014a,b). ~40% of LMC Cepheids Ripepi et al. 2015

14 PL relation for RR Lyrae stars in the LMC bar: a Bayesian fitting approach Muraveva et al. 2015

15 RR Lyrae stars in the SEP tile RRab stars (filled) and RRc (open) stars 109 confirmed RR Lyrae stars with a VMC counterpart (79 RRab, 23 RRc, 7 RRd) Moretti et al. 2016, in prep

16 PL relation for RR Lyrae stars in the MW: a bayesian approach Muraveva et al. 2015

17 The LMC structure as traced by: RR Lyrae stars Moretti et al. 2014

18 The LMC structure as traced by: Classical Cepheids Moretti et al. 2014

19 The LMC structure as traced by: hot binaries Moretti et al. 2014, Muraveva et al. 2014

20 PI: W. Freedman, 779h G. Clementini (Co-I) PI: K. Johnston, 664h G. Clementini (Co-I) PI: W. Freedman, 132 orbits G. Clementini (Co-I) Wide international collaborations: Wendy Freedman, Barry Madore, G. Preston, E. Persson, V. Scowcroft, J. Kollmeier, I. Thompson, A. Monson, M. Seibert (Carnegie Observatories, Pasadena, USA); van der Marel (Space Telescope Science Insti tute, Baltimore, USA); S. Majewski (University of Virginia, Charlottesville, USA); K. Johnston, G. Besla (Columbia University, New York, USA); D. Nidever (University of Michigan, Ann Arbor, USA); H.A. Smith (Michigan State University, East Lansing, USA); N. Kallivayalil (Yale Center for Astronomy & Astrophysics, New Haven, USA); C. Klein (University of California, Berkeley, USA); M. Marengo (Iowa State University, Ames, USA); M.R. Cioni (Leibnitz-Institut fur Astrophysik, Potsdam, Germany); D. Law (University of Toronto, Canada); A. Udalski, I. Soszynski, G. Pietrzynski (Warsaw University Observatory, Poland); G. Bono. (Univ. of Roma Tor Vergata) Gaia A. Garofalo, T. Muraveva Gaia Gaia EXCALIBUR S PRIN INAF 2014 (2015-early 2017), PI G. Clementini Gaia

21 What s needed next 1. Long term/permanent positions for the youngsters (..) 2. Funds of course (waiting for results from Astrofit2 & other funding requests..)