Giada's Intro Talk ISM@ST

Transcript

1. Giada Pastorelli Intro Talk ISM group @ STScI March 16, 2020
2. Research background Department of Physics and Astronomy University of Padova, Italy B.S. Astronomy (2013) M.S. Astronomy (2015) Ph.D. Astronomy (2019) Post-doc (2019) Supervisors: Prof. Paola Marigo & Dr. Léo Girardi Post-doc ISM @ STScI → Evolved stars models, nearby galaxies Supervisor: Dr. Martha Boyer • Resolved Stellar Populations in nearby galaxies • Calibration of AGB models in the Magellanic Clouds • Magellanic Clouds star formation history
3. TP-AGB stars
4. TP-AGB stars • Uncertainties of all previous evolutionary phases • Treatment of convection → HBB and 3DUP • Formation and growth of dust grains • No satisfactory theory for mass loss • Interplay between mass loss, 3DUP, HBB
5. STARKEY Project @ Padova University PI: Paola Marigo Solving the TP-AGB STAR Conundrum: a KEY to Galaxy Evolution • Accurate SFH • Detailed TP-AGB models • Synthetic photometry • Reliable identification of AGB stars Global calibration method of key uncertain processes (mass-loss, 3DUP) as a function of initial mass and metallicity in nearby galaxies Calibration of TP-AGB models
6. Calibrating TP-AGB models in the SMC
7. SMC resolved stars in the infrared VMC Survey Cioni+11 SAGE-SMC Survey Gordon+11
8. SMC resolved stars in the infrared Rubele S., Pastorelli G., et al. 2018, MNRAS, 478, 5017 VMC Survey Cioni+11 SAGE-SMC Survey Gordon+11
9. SMC resolved stars in the infrared VMC Survey Cioni+11 SAGE-SMC Survey Gordon+11 SFR(t) - Z(t) - DM - Av Rubele+18 o Robust age estimate down to old MSTO o No TP-AGB contribution o PARSEC v1.2s o VMC-SAGE overlap ~ 87 % 147 sub-fields → 21 deg2 Rubele S., Pastorelli G., et al. 2018, MNRAS, 478, 5017
10. SMC resolved stars in the infrared VMC Survey Cioni+11 SAGE-SMC Survey Gordon+11 SFR(t) - Z(t) - DM - Av Rubele+18 o Robust age estimate down to old MSTO o No TP-AGB contribution o PARSEC v1.2s o VMC-SAGE overlap ~ 87 % 147 sub-fields → 21 deg2 AGB catalogs Boyer+11, Srinivasan+16 AGB = 5 792 C-rich = 2 340 O-rich = 3 109 X-AGB = 343
11. Calibration Strategy
12. Varying mass-loss prescriptions: - Pre-dust regime Cranmer & Saar 2011, starting in early-AGB - Dust-driven regime O-rich: Blöcker 1995 Ṁ ~ η dust x L2.7 x R x M-3 C-rich: Dynamical atmospheres models (CDYN) Eriksson+14 , Mattsson+10 Fixed 3DUP from Karakas+02 (very efficient 3DU for massive stars) TP-AGB model grid (1)
13. AGB + 0.2 % O-rich + 1.0 % C-rich - 1.5 % X-AGB + 4.6 % Pre-dust: Cranmer & Saar 2011 η = 3 Dust Driven M-stars : BL95 η = 0.06 C-stars : CDYN Best-Fit 1 • Efficient 3DUP (K02) • Extreme mass-loss efficiency for M-stars 8/19 Giada Pastorelli - January 5, 2020 – 235th AAS meeting - Honolulu, Hawai’i Best-fitting model 1
14. Fixed mass-loss prescription: → M-stars: BL95 η = 0.01-0.03 Ventura+10 → C-stars: CDYN f ( C-O) Varying 3DUP parameters: → Onset → Efficiency 9/19 Giada Pastorelli - January 5, 2020 – 235th AAS meeting - Honolulu, Hawai’i TP-AGB model grid (2)
15. AGB +2.6% O-rich + 5.1 % C-rich - 4.3 % X-AGB + 28 % Best-Fit 2 Best-fitting model 2
16. Sptizer IRAC 2MASS 3.6 μm 4.5 μm 5.8 μm 8.0 μm J H Ks Best-Fit 2 Best-Fit 1 AGB O-rich C-rich X-AGB AGB O-rich C-rich X-AGB NIR and MIR LFs
17. Best-Fit 2 Moderate 3DUP efficiency ( M i > 3 M ☉ , λ < 0.5) → better agreement with the empirical IFMR BF 2 BF 1 Zi = 0.014 Initial-to-final mass relation
18. Conclusions Reliable calibration of TP-AGB models in the SMC • Pre-dust mass-loss important for low-mass O-rich stars • Mass-loss based on C-star dynamical models • SMC photometry reproduced with 2 different set of models 1) Efficient 3DUP + Extreme mass-loss efficiency for M-stars 2) Less efficient 3DUP (M i > 3 M ☉ ) + lower mass-loss efficiency → better agreement with empirical IFMR → effects on the chemical yields WORK in PROGRESS Calibrated stellar isochrones → stev.oapd.inaf.it/cmd Pastorelli et al. 2019, MNRAS, 485, 5666
19. A method to distinguish evolutionary stage, initial mass, and chemical type of AGB stars: Gaia + 2MASS diagram
20. LPVs in Gaia DR2 GAIA + 2MASS photometry → Discriminate initial stellar masses evolutionary phase & chemical type Lebzelter T., Mowlavi N., Marigo P., Pastorelli G. et al. 2018, A&A Letter 616, L13
21. Simulations of the LSST stellar content LSST stars Milky Way and Local Volume Science Collaboration PI L. Girardi TRILEGAL Working Group & STARKEY Team @ UniPd L. Girardi, Y. Chen, G. Pastorelli, P. dal Tio, M. Trabucchi K. Olsen @ NOAO Data Lab LSST-Brazil team @ LinEA M. Barbieri @ LSST-Chile MW working group, Z. Ivezic & M. Juric @ University of Washington PARSEC Team, P. Marigo, A. Bressan @ UniPD & SISSA
22. LMC SMC SMC LMC Complete simulation • 19 billions stars • Disk space ~ 3 Tby • SMC ~ 1.6 x 10 8 stars • LMC ~ 6 x 108 stars • Simulations are done @ NCSA HEALPix nested scheme • Complete down to r = 27.5 mag • NEW! Variable resolution & interacting binaries 39/45 LSST stellar content
23. 27 26 25 24 23 22 21 20 crowding limit r mag Crowding limit (Olsen+2003): • seeing=0.6 arcsec & 10% photometric errors . . . on-going estimation . . . MCs central regions → r lim ~ 20 mag SMC 1.6 ⋅ 10 8 → 2 ⋅ 10 7 stars LMC 6.0 ⋅ 10 8 → 4 ⋅ 10 7 stars 40/45 Crowding Limit
24. Crowding limit in central regions TP-AGB TRILEGAL catalogs are being used to optimize the LSST observing strategy LSST White Paper: Mapping the Periphery and Variability of the Magellanic Clouds K. Olsen, P. Szkody, M.-R- Cioni, M. Di Criscienzo, I. Musella, V. Ripepi, F. Borsa, M. Marconi, L. Girardi, G. Pastorelli, M. Trabucchi, P. Ventura, M. Moniiez - eprint arXiv:1812.03139 AGBs as seen by LSST
25. Modeling Local Group Dwarf Galaxies
26. Follow-up with WFC3/IR on HST (Boyer+17) Medium-band filters F127M, F139M, F153M → to separate C- and O-rich stars (Boyer+17) AGB candidates in nearby dwarf galaxies : DUSTiNGS survey (Boyer+15) Most of them are very metal poor (Z ∼0.008Z ☉ ) Local Group Dwarf galaxies
27. Local Group Dwarf galaxies DATA MODEL M(1766) C(534) C/M = 0.3 M(9) C(65) C/M = 7.2 M(22) C(14) C/M = 0.6 M(724) C(540) C/M = 0.7 IC10 IC10 Sex A Sex A (Boyer+17) Simulations based on SFH from HST photometry (Weisz+14, Boyer priv. comm.) Work in progress Good agreement with observed C/M separation More accurate simulations, i.e. phot. err., completeness Data-model comparison
28. 2. Long Period Variables in GAIA DR2 4. Modelling of Local Group Dwarf galaxies 3. Simulations of the LSST stellar content Extending the calibration to the LMC (Pastorelli et al., in prep.) Metallicity dependence & additional filters combinations to apply the diagram to more distant objects (Pastorelli et al., in prep.) Constraining models of TP-AGB and Core He-burning stars (Pastorelli et al., in prep.) Including calibrated TP-AGB models & variability information 1. Calibration of TP-AGB models in the SMC Summary