Make or Break: HI & Optical Views of Galaxy Disks

1. Make or Break: HI & Optical Views of Galaxy Disks • Dissecting and tracking disk galaxies • Connecting optical and HI views back to First Light (EoR) • Matching HI telescopes with counterpart optical survey engines Matthew Bershady U. Wisconsin

2. Disk Galaxy Assembly …didn’t happen this way: 1<z<2 ??? today UDF • Disks are fragile destroyed in major mergers; heated in minor mergers • Dry vs wet mergers Wet mergers can make new disks; must happen early to yield old, cold disks today • Large disks today - stirred, not shaken streams not train-wrecks

3. Blue Cloud andRed Sequence growth and destruction • Some galaxies evolve from blue cloud to form the red sequence. • Most stars are made in the blue cloud but end up in the red sequence. • Identify which are stirred, which are shaken: • Tag environment • For those that are stirred: • Monitor smooth & continuous… • accretion growth • star-formation gas consumption Red sequence e.g., Bell et al.’03,’07 Blue cloud

4. Connect Optical and HI Views • Are these two trends self-consistent? • Confirm SFR with a single, direct measure from z=0 to z=1 and higher (Ha) • Measure WHI(z) and HI mass-function directly • Determine SFR as function of both dynamical and HI mass • Identify the individual galaxies, e.g., at the knee of the HI mass-function SDSS M* Ha, OII, LUV Heavens et al’04 Baugh’04

5. Go beyond the co-moving integral • Are these two trends self-consistent? • Confirm SFR with a single, direct measure from z=0 to z=1 and higher (Ha) • Measure WHI(z) and HI mass-function directly • Determine SFR as function of both dynamical and HI mass • Identify the individual galaxies, e.g., at the knee of the HI mass-function Heavens et al’04 large disks Baugh’04

6. Trace Key Observables in the Blue Cloud • Dynamical mass • HI mass (+molecular) • Star-formation rate (SFR) • Stellar mass (dynamically calibrated) • Abundances • Dynamical mass - baryonic mass - metallicity correlations baryons processing Efficiency of processing baryons in gravitational wells

7. The Nearby Universe (z<0.1) Dissecting disk galaxies and establishing a stellar mass zeropoint • Ha velocity fields • Stellar velocity dispersions • Optical-mid-IR SEDs • HI synthesis maps The DiskMass Project Marc Verheijen - Kapteyn / Groningen Kyle Westfall - U. Wisconsin Rob Swaters - U. Maryland David Andersen - HIA / Victoria Thomas Martinsson - Kapetyn/Groningen

8. The DiskMass Project Breaking the Disk-Halo Degeneracy • What are the shapes of dark halos? • How massive are spiral disks? • Are they maximal? • What’s the stellar mass-to-light ratio (M/L) in disks? Maximum disk M/LK = 0.75 Sub-maxium disk M/LK = 0.22 UGC 6918 high surface-brightness disk degenerate solutions

9. Sample Properties: Normal Face-on Spirals from UGC 50x50 kpc: SDSS A wide range of physical size and disk morphology

10. Large range in SF histories: Factors of 60 in LK 10 in mR 6 in LB/LK

11. SparsePak FFU 82 fibers, 4.’’7 diameter 72’’ FOV l/Dl = 11,000 WIYN 3.5m (Bershady et al.’04,’05) PPak IFU 331 fibers, 2.’’7 diam. 75’’ FOV l/Dl = 8000 Calar Alto 3.5m (Verheijen et al.’05) Optical Survey Engines Customized integral field units… gas stars

12. Connecting mass and fuel to consumption Radio synthesis maps (Westerbork + VLA) Baryon reservoir Halo mass at large radii

13. Connecting mass and fuel to consumption High-resolution 2D optical kinematics: stars + gas SFR: Ha + Spitzer

14. Mapping the Cosmic History of Disks • Track blue cloud in a range of environments across look-back time • Clusters are nodes in the cosmic web • Large volumes around clusters probe the largest dynamic range in environments • Find the primeval disks at “First Light” – driving part of the Epoch of Re-ionization (EoR) 0<z<1.5 7<z<12 globular clusters

15. At z=0.5, the red sequence is well-formed MS0451: z=0.54, s=1354 km/s, Lx=40e44 ergs/s WIYN Long-Term Variability Survey Crawford et al. 2006, 2008

16. At z=0.9, the blue cloud dominates. . . even in rich clusters CL1604: z=0.9, s=982 km/s, Lx=2e44 ergs/s WIYN Long-Term Variability Survey Crawford et al. 2006, 2008

17. HI View: State of the Art: Verheijen et al. 2007 (van Gorkum) 45’ z=0.2 Red sequence Blue cloud NB: 200h of 1000h total to come! Westerbork

18. HI View: State of the Art A963 - Westerbork • Solid detections for 42 sources in 2 x 0.4 deg2 fields • expect 200 sources in 1000h • Limited spatially-resolved kinematic information • Ha offers detailed kinematic supplement + SFR map • t=80 min, 3.5m telescope (CA) • 16x16 array of 1” fibers (PMAS) A2192 (z=0.19) - VLA MHI=7x109 Msun Verheijen & Dwarakanath ‘08

19. Optical Follow-up at z>0.2 • Scale 4m-class IFU observations to 8m-class telescopes • comparable S/N in t=10h, 10 times angular resolution, twice the luminosity • Stellar kinematics out z=0.2 • Ha out to z=1 w/ NIR and AO • Best example: VLT / Sinfoni • also Keck / OSIRIS and Gemini / NIFS • Multi-object IFU ? • Only example in optical: VLT / FLAMES-GIRAFFE • Fiber+lenslet coupled spectrograph • 15 units + 15 sky fibers, 25’ patrol field • 2” x 3” arcsec units: 20 square microlenses (0.52” sampling) • 11000<l/dl< 39000, 370-950 nm range Eisenhauer et al.’03 Larkin et al.’06 McGregor et al. ‘99 Flores et al.’04

20. Multiplex at high-z: Science: emission-line kinematics of distant galaxies. Flores et al.’06 VLT / GIRAFFE This is a powerful instrument . . . . . . But note: isovels heavily smoothed. Enough sampling?

21. Finding First Light z = 12.1 9 .2 7.6 H I brightness temperature: Reionization • Science Goal: Discover how rapidly the first galaxies form. When is reionization complete? The frontier is z>7. The achievable flux limit for SALT is about z=10 (Ly @1.35 m) • Instrument Requirements: • Fabry-Perot imaging: =2500 • z=8: we expect > 30 sources in 12 hours • z=9-10: expect ~30 sources in 53-1600 hours • Simultaneous optical FP to cull interlopers (redshifted [OII]3727 if NIR-line is H). • Follow-up optical-NIR MOS at >4000: • eliminate remaining interlopers (split [OII]3727 doublet); • determine kinematics to make dynamical mass estimates; • constrain winds and outflows. Furlanetto et al. Simulations Ly In the J band 2’x2’ 8m tel Barton et al. ‘04

22. Robert Stobie Spectrograph (RSS) @ prime focus Wisconsin-Rutgers-SAAOOptical: Nordsieck, Williams, O’Donoghue NIR: Sheinis, Wolf, Bershady & Nordsieck SALT: Southern African Large Telescope

23. SALT: Tilted, rotating Arecibo Payload RSS Tracker Bream Primary Mirror spherical aberration corrector Concrete Pier

24. Vis-gratings gratings filters Vis-Camera F-P Nordsieck Pre-Dewar RSS: Optical + NIR beams Sheinis Dewar Camera Vis F-P’s Pol-BS Williams pupil doublet

25. RSS Optical layout/Components pupil Pre-Dewar F-P gratings filters doublet Detector Dichroic-BS Dewar Camera collimator Slit

26. Emission-line Sensitivies SALT RSS Visibile and NIR beam, 1 arcsec2 aperture Ha from 0<z<1.75 to 0.1 Mo/yr • Star-formation rates • Nebular abundances Ha/[NII], [OIII]/H • Redenning Ha/Hb • Lya from 2.6<z<12 to 1 Mo/yr • First Light / EoR 5s, 1h, l/dl=4000, 1 arcsec2

27. Future Possibilities…toward SKA • HI surveys of disk galaxies • Arecibo, pointed (GASS++): z~0.3 • Westerbork, EVLA, blind: z~0.2-0.4 • MeerKAT, BigKAT, ASKAP, blind: z~0.3-0.6 • EoR ??? • 3D Optical Spectroscopic Follow-up of HI surveys • Spatially resolved ionized-gas kinematics & abundances • z<0.2-0.3: minor investment in existing 4m-class facilities, • z>0.3: major investment in new 8m-class instrumentation • Stellar kinematics • z<0.2-0.3: major investment in new 8m-class instrumentation • z>0.3: 30m-class optical telescope + spectrograph • 2D Optical Discovery of First Light • Redshifts to z=10 $0.5-1M $10-15M same instrument $1G $10M