Synergy between MOSAIC, MICADO, and MUSE: resolved stellar populations in nearby galaxies Martin M. Roth (P.I.) Andreas Kelz Leibniz-Institute for Astrophysics Potsdam (AIP) University of Potsdam Toledo, 19.10.2107 1
ELT-MOS-white paper Evans et al., arxiv150104726e MOSAIC Science Case: with contributions from more than 100 scientists from all over Europe SC1: First galaxies, reionisation SC2: Large scale structure SC3: Galaxies mass assembly SC4: AGN/Galaxy coevolution SC5: Resolved stars beyond the LG SC6: Galactic archaeology SC7: Galactic centre SC8: Planet formation in clusters
Outline 1. Introduction: PSF-fitting 3D spectroscopy 2. Globular Clusters: NGC 6397 3. Nearby Galaxies: NGC 300 4. Application to MOSAIC 5. Conclusions 4
1. Introduction: PSF-fitting crowded field 3D spectroscopy 5
PSF-fitting crowded field 3D spectroscopy Modelling the Point Spread Function (PSF): Kamann (thesis, 2013) important input data: star positions from HST images
PSF-fitting crowded field 3D spectroscopy Global Model: important input data: star positions from HST images observed datacube: model datacube: minimization: Kamann (thesis, 2013) SMFNS2015, Varadero, 15-05-2015
2. Globular Clusters NGC 6397 9
NGC 6397 (m M) 0 = 11.90 D = 2.4 kpc credit: ESO (WFI) 10
NGC6397 A mosaic of MUSE pointings (each 1 sqrarcmin) Total 127 exposures of <60s Husser et al. 2016 A&A 588, A148 Kamann et al. 2016 A&A 588, A149 Chemical Odd-Balls, AG Kiel, 15-09-2015 Total exposure time: 95min seeing 0.6 1.0.
NGC6397 deblending spectra with PampelMuse MUSE-VLT ACS-HST late G star A star 12
NGC6397 18932 spectra for 12307 stars in total 10521 with S/N>10. 894 stars above turnoff (15.7 mag) 6248 fainter than turnoff 13
3. Resolved stellar populations in nearby Galaxies NGC300 14
credit: ESO (WFI) NGC 300 (m M) 0 = 26.36 D = 1.87 Mpc
0.75 Overlays of 7 re-constructed images from MUSE pointings (1x1 arcmin) 0.7 1.2 1.0 0.8 credit: ESO 0.85 0.6
0.75 0.7 1.2 1.0 0.8 credit: ESO 0.85 0.6 Field with best seeing
Data Analysis HST photometry catalogue (ANGST) VRI images from HST archive MUSE images extracted from datacubes Extraction of spectra using PampelMuse Fields not covered by HST with DAOPHOT FIND Stars: Spectral template fitting with ULYSS Spectral library: MIUSCAT (MILES+CAT+indoU.S.) Fitting with Göttingen Library GLIB Photometry of MIUSCAT stars (SIMBAD) Visual inspection Teff, log g, vrad Emission line objects: classification, flux,fwhm,vrad (p3d) Catalogue Atlas 18
Example spectra: 19
B3 III R = 22.34 v rad = 186 11 km/s 20
A1 Ib A5 II R = 20.64 v rad = 149 18 km/s 21
K3 Iab M1 Ia R = 21.38 v rad = 171 17 km/s 22
Test: deblending M4.5 III M6 III R = 23.26 v rad = 138 10 km/s 23
B9p A2 Ia R = 21.84 v rad = 178 26 km/s 24
M6 III R = 24.79 v rad = 174 7 km/s 25
Carbon stars Van Loon et al. 2005
Carbon stars 23 carbon stars in field (i) 27
Radial velocities of resolved stars 28
Radial velocities of unresolved stars 29
Emission line objects (e) 0.75 (a) 0.7 (b) 1.2 (c) 1.0 (d) 0.8 (j) 0.85 (i) 0.6 Deharveng+ (1988) Blair & Long (1997) 30
Summary (from 9 hrs total exposure time) a b c d12 e1 i j Seeing 0.7 1.2 1.0 0.8 0.75 0.6 0.85 PN 4 1 3 3 13 3 3 30 PN candidates 5 2 4 2 7 0 4 24 HII regions 11 18 12 24 12 26 11 114 chii regions 1) 7 29 3 14 11 3 3 70 SNR candidates 12 18 9 11 1 4 18 73 emstars 2) 18 2 5 10 27 11 6 79 bgr. Galaxies 3) 2 TBD TBD 3 3 8 4 >20 Stars 4) 445 77 152 265 299 427 91 1756 1) compact HII regions 2) emission line stars 3) background galaxies 4) stars with spectral type 31
4. Application to MOSAIC 32
MUSE + AOF
NGC 6563 non AO 120 s exposure Airmass 1.3 Dimm 0.9 arcsec measured FWHM (Moffat) 1.02 arcsec @ 5100 A 0.81 arcsec @ 9000 A
NGC 6563 with GLAO 120 s exposure Airmass 1.3 Dimm 0.9 arcsec measured FWHM (Moffat) 0.78 arcsec @ 5100 A 0.57 arcsec @ 9000 A
deployable mini-ifus for crowded-field multiobject spectroscopy Left: PMAS-IFU 16x16 spaxels (FoV: 8 ) Right: MUSE 300x300 spaxels (FoV: 60 ) Above: Parameters for deployable IFUs of MOSAIC & synergy with MICADO to provide imaging data for precise astrometry
Conclusions (1) Crowded field 3D spectroscopy with MUSE + HST works extremely well in globular clusters, even out to distances of nearby galaxies (2) MUSE + HST very efficient in discovering faint continuum and emission line objects (3) Classical sequence of imaging follow-up spectroscopy no longer necessary (4) MUSE target seletion for MOSAIC (5) Crowded field 3D spectroscopy is a powerful tool also for deployable IFUs MOSAIC 37
Acknowledgements BMBF Verbundforschung Astrophysik Projektträger PT-DESY: various grants: PMAS ULTROS MUSE ERASMUS-F ELT-MOS Projektträger Jülich: innofspec Potsdam Deutsche Forschungsgemeinschaft: Calar Alto travel grants Chemical Odd-Balls, AG Kiel, 15-09-2015