1. Future AO Legacy HI line surveys: Synergies with other surveys Martha Haynes Cornell University Frontiers of Astronomy with the World’s Largest Radio Telescope September 12-13, 2007 Thanks to many people whose slides/diagrams/ideas have been borrowed for this presentation

2. Topics in this talk What are the main questions in cosmology and galaxy evolution that HI science can address? What is the current state of extragalactic HI science of relevance to those topics? How do Exgal/Cosmo HI surveys fit in with surveys at other wavelengths? What other radio facilities are/will be available? How might AO contribute uniquely to advancing the field?

3. 2nd+ generation HI surveys 2nd+ generation HI surveys In comparison with opt/IR, the HI view is largely immature HIMF based only only few thousand objects (HIPASS; SFI++), whereas O/IR LF is based on hundreds of thousands to millions of objects! “Missing Satellite Problem”: HIMF at low masses Halo occupation number Clustering of gas-rich galaxies: Correlation functions: HI-HI, HI-opt, HI-IR Bias parameter “Void problem” Dark energy constraints from baryon acoustic oscillation peaks determined with redshifts Mass assembly history of galaxies: HIMF across the masses

4. Four published results 1. Eisenstein et al 2005 3D map from SDSS 46,000 galaxies in 0.72 (h -1 Gpc) 3 2. Cole et al 2005 3D map from 2dFGRS at AAO 221,000 galaxies in 0.2 (h -1 Gpc) 3 3. Padmanabhan et al 2007 Set of 2D maps from SDSS 600,000 galaxies in 1.5 (h -1 Gpc) 3 4. Blake et al 2007 (Same data as above) Current State of the Art in Baryon Acoustic Oscillations (BAO) Thanks to Pat McDonald (CITA) AAO 4-m telescope at Siding Spring, Australia SDSS 2.5-m telescope, Apache Point, NM (spectro-z) 5% (spectro-z) 3% (photo-z) 5% HI surveys are woefully behind in numbers of detections

5. a.k.a.: SDSS-3

6. JDEM: ADEPT concept Warren Moos: presentation to BEPAC

7. OIR Spectroscopic BAO surveys Warren Moos: presentation to BEPAC

8. How and when do galaxies form? Numerical simulations are used to trace the gravitational collapse of matter (dark+luminous) across cosmic time

9. The “Missing Satellite Problem” Models/simulations predict large numbers of satellites => Logarithmic slope of the faint end of the CDM mass function ~ -1.8 (Press-Schechter value) Kauffmann et al. (1993) Klypin et al. (1999) But the current census does not count them (light not mass): Faint end slope of the optical LF Faint end slope of the HIMF But, is there anything we can detect? Baryon loss during reionization ( e.g., Efstathiou 1992; Barkana & Loeb 1999; Shaviv & Dekel 2003) Can they (ever) form stars? (Verde et al. 2002)

10. The HI Mass Function N=1000 ? Parkes HIPASS survey: Zwaan et al. 2003 Previous surveys have included few (if any) objects with HI masses less than 10 8 M . At lowest masses, differ by 10X: Rosenberg & Schneider (2000) versus Zwaan et al. (1997) Statistics Systematics

11. Challenges HIMF @ z=0 Challenges Need better statistics: larger, more sensitive surveys At the faint end, all the galaxies are nearby Redshift distances are highly unreliable LSS affects accuracy of flow models Masters, H & G 2004, ApJ 607 L115 Need a “fair sample” to overcome (and allow study of) cosmic variance Σ(1/V max ) corrections must account for LSS Not just that space density varies with distance Fractional volume of space occupied by regions of a particular density do too Springob, H & G 2005, ApJ 621, 215 Other methods (e.g. 2DSWML) do not give normalization

12. Statistics, statistics, statistics Springob et al. 2005 (optically selected) N=2800 N= 265 Rosenberg & Schneider 2002

13. Cosmic variance Must sample enough volume to acquire a “fair sample” If we covered a similar slice in the opposite part of the sky (coming….) we would see a very DIFFERENT redshift distribution => LSS!!! At these distances, 540 square degrees is not enough.

14. Environment & the HIMF Previous studies based only on Virgo have suggested that the HIMF in Virgo is flatter than in the field Only a single cluster Very small number statistics/systematics vs comparison Is this just HI deficiency? Watch out for morphological biases Kovač, Oosterloo & van der Hulst (2005): CanVen Similar to Virgo (low mass slow flatter) BUT…….. Zwaan et al. (2005): HIPASS Higher density regions => more low masses Inconsistency: Symptom of inadequate volume?

15. Springob, Haynes & Giovanelli (2005) Much larger sample, optically targeted HI flux and diameter limited subsample (N = 2200 objects) PSCz density field out to 6000 km/s Low mass end of HIMF in high density regions flatter and M* lower Cannot be just morphology or HI deficiency Environment & the HIMF Agreement between optically selected and HI blind HIMFs no worse than internal agreement among HI blind surveys Need larger sample to discriminate whether HIMF shape is dependent on morphology and environment separately (as done for 2dFGRS LF, e.g. Croton et al 2006) Springob et al 2005 ApJ 621 215

16. HI and the “missing satellite” problem result: no cosmologically significant population of HI- rich dark galaxies: agrees… but M HI > 10 8 M  HIPASS result: no cosmologically significant population of HI- rich dark galaxies: ALFALFA agrees… but HIPASS M HI > 10 8 M  is specifically designed (wide area, high velocity resolution) to detect hundreds of objects with M HI < 10 7.5 M  ALFALFA is specifically designed (wide area, high velocity resolution) to detect hundreds of objects with M HI < 10 7.5 M  Low HI massLow HI mass Narrow HI line width + exclude face-on objectsNarrow HI line width + exclude face-on objects Will be detected nearby => need to sampleWill only be detected nearby => need to sample cosmologically significant volume Future studies will focus on extending Deeper in HI Mass than ALFALFA in Local Supercluster Much larger volume than AGES ALFALFA has already detected more objects with log M HI < 7.5 than all other previous blind HI surveys combined

17. Lowest HI mass objects log M HI < 7.2 ALFALFA has already detected more objects with log M HI < 7.5 than all other previous blind HI surveys combined

18. The “Void Problem” Peebles (2000) ApJ 597, 495 Cosmic voids are filled with low mass dark matter haloes Mare Nostrum simulation v rot >55km/s ~1000 haloes with M < 10 9 M  and v rot < 20 km/s in a 20 h -1 Mpc void are predicted Halo mass function in voids Gottlöber et al (2003)

19. Luminosity function of void galaxies Void LF has a faint M* but a similar faint-end slope, compared to the overall LF Void galaxies are blue, disk-like and have high H  equivalent width => good HI targets Void galaxies in the SDSS: Hoyle et al (2005) 1000 galaxies in lowest density cells of total 155,000 galaxies (SDSS 2005)

20. Clustering of HI galaxies ξ(r) for HIPASS Meyer et al (2007): HI rich galaxies extremely weakly clustered Clustering scale depends on V rot Basilakos et al (2007): Massive HIPASS galaxies show same clustering as optically-selected sample Low mass systems (M HI < 10 9 M  ) show nearly uniform distribution Inconsistency: Symptom of inadequate volume?

21. (Very) preliminary ALFALFA result 460 Mpc -3 in PPS foreground void at v~2200 km/s Simulations of Gottlöber et al. (2003) with dark:HI = 10:1 predict 38 HI sources ALFALFA finds no objects This makes Jim Peebles very excited… But only 2% of ALFALFA volume STAY TUNED….. Amélie Saintonge, Ph.D. thesis, Cornell U. Saintonge et al. 2007, submitted

22. ALFALFA: HI Cosmology at z=0 HI Mass function sampled over a fair volume Low mass slope Highest masses Variation with environment Halo occupation number The “void problem” Correlation function over a fair volume HI-HI HI-optical/IR selected Bias parameter (do galaxies trace mass) TF relation => peculiar velocities 3 rd generation surveys need to improve by ~10X in mass sensitivity on ALFALFA in local universe. 3 rd generation surveys must probe deeper in z and still cover cosmologically significant volume

23. How and when do galaxies acquire their gas? Kereš et al. (2005)

24. How and when do galaxies acquire their gas? Kereš et al. (2005)

25. AUDS: Arecibo Ultra-Deep Survey Results (as reported by M. Zwaan) 53 hours during commissioning 50 microJy rms 14 HI detections + 9 candidates 0.07 < z < 0.15 N=23

26. Highest mass objects: future SKA A prime science driver of the SKA is a HI “billion galaxy” survey. (Abdalla & Rawlings 2004) Previous HI surveys detect very few objects with M HI > 10 10 M  ; HIMF not well constrained at highest masses either. No theoretical expectation for massive galaxies with no stellar counterpart => targeted surveys ALFALFA has already detected more than twice as many objects with log M HI > 10.4 than all other previous blind HI surveys combined

27. Highest mass objects: future SKA ALFALFA has already detected more than twice as many objects with log M HI > 10.4 than all other previous blind HI surveys combined

28. SDSS color distribution Ivan Baldry et al.

29. SDSS color distribution Ivan Baldry et al.

30. Blue and red sequence LF’s Baldry et al. (2004)

32. AGN: The Missing Link? Di Matteo, Springel & Hernquist 2005 Tight observed relation between M bulge and M BH Many of the transition objects in the so-called “green valley” with 3 < (NUV- r) < 5 appear to have AGN HI provides measure of cool gas, potential for star formation, unavailable otherwise => key clue to models of galaxy assembly

33. Highest HI mass ALFALFA detections show a range of morphologies/optical surface brightnesses (Most) appear to be luminous disk systems Some have M HI /L > 2 => M gas ~ M * Some have M * > 3 x 10 10 M  (“transition mass”) Fraction of AGN (TBD) Direct measure of gas content in z ~ 0 “transition objects” High mass objects Many in “green valley” (NUV-r: (3-5)) have AGN GASS (GALEX-Arecibo-SDSS survey: Schminovich et al.) 1000 galaxies, chosen by (NUV-r) colors, spectra 0.025 < z < 0.06 (matches ALFALFA range) Low gas mass fraction M gas /M * ~ 0.01 Mass assembly: cool gas content

34. Probing HI galaxies at z ~ 0.2 There current are NO constraints on the HIMF at cosmological z’s SDSS-selected sample of spirals at z ~ 0.2+ Demonstrator of AO capability for HI studies over cosmic timescales => evolution of Tully-Fisher relation, evolution of HI disks, constraints on evolution of HI Mass function Future: development of focal/phased array for 900-1200 MHz Redshifted HI emission Barbara Catinella, NAIC (now MPA) SDSS image

35. SKA precursor science with AO

36. Lister Staveley-Smith (Spineto, 2007)

38. But mapping may not be the right approach for Arecibo at intermediate z!

39. Legacy applications of extragalactic HI line surveys pre-SKA Deeper local blind HI surveys to explore faint end of HIMF over adequate volume for cosmology => wide area Deeper targeted HI surveys to explore the astrophysics of mass assembly of galaxies=> push as far in z as practical Absorption line studies (not discussed here) For redshifted HI line, need capability in 900-1200 MHz range Phase I: 3-beam array, low noise (1 beam on target; 2 RFI) Phase II: Phased array RFI issues must be tackled head-on! Future HI line surveys with AO

40. Need well defined survey science requirements What surveys are needed to do what science? Design surveys to optimize science Mechanisms to prioritize/coordinate Need to understand resource requirements of surveys Survey results must be delivered on optimal schedule Observing team support & software development Automation + quality assurance Data management, archiving, data products, access Data volumes are huge! R&D for RFI mitigation/identification/excision Timely and convenient delivery of data products to public archive Permanent curation/delivery Public access tools; visualization tools How to engage and energize the community at large?! Practical challenges to “US”