1. 1 AUI Cooperative Agreement — NSF Panel Review August 25 – 28, 2008 National Radio Astronomy Observatory Science enabled by NRAO facilities into the next decade Chris Carilli Process: radio astronomy science priorities, and the NRAO Decadal Survey 2010 working group Five exemplary science programs that demonstrate the synergy between NRAO instruments, and their key roles in modern, multi- wavelength astrophysics.

2. 2 AUI Cooperative Agreement Proposal NSF Panel Review August 25 – 28, 2008 Gauging the community NRAO/AUI has co-sponsored an extensive series of meetings, advisory committees, and internal discussions, to consider the main science priorities for (radio) astronomy into the next decade: Chicago I, II, III: open meetings with broad, multiwavelength input NRAO 50th anniversary science meeting NRAO scientific staff retreats NRAO strategic planning retreats GBT, ALMA science workshops AAS townhall discussions McCray committee

3. 3 AUI Cooperative Agreement Proposal NSF Panel Review August 25 – 28, 2008 Decade Survey 2010 Working Group Review reports and produce set of key science programs for radio astronomy in the next decade, delineating the role of NRAO facilities in enabling these programs. Generate flow-down from science requirements to technical improvements to NRAO facilities, or new facilities, including assessment of technical readiness, (rational) costing, global context (OTC, OSC…) Goal: Report on role of NRAO in DS2010 for review by user community Guiding principles Attract the broad community: multi-wavelength approach to tackling the key problems in modern astronomy NRAO as a ‘single facility’: complementary use of NRAO facilities to produce non-linear gains in scientific discovery

4. 4 AUI Cooperative Agreement Proposal NSF Panel Review August 25 – 28, 2008 DS2010 Working Group: Initial deliberations Science priorities expressed in various venues are generally consistent with the Key Science Projects proposed by the SKA science working group in 2004. [Even SKA project office admits full SKA is not realizable in next decade.] Near term: Narrow focus to quantify how NRAO facilities will make major strides in addressing the SKA KSP goals, as well as delineate the requisite upgrades, or development work on plausible new facilities. Naturally places NRAO DS2010 science planning into global context, with firm-footing based on broad community input.

5. 5 AUI Cooperative Agreement Proposal NSF Panel Review August 25 – 28, 2008 Key Science Projects: (i) Address critical questions, (ii) Unique role of radio, or complementary but fundamental, (iii) Excites broad community I. Cosmic reionization and first (new) light: (i) HI 21cm tomography of IGM, (ii) gas, dust, star formation in first galaxies II. Galaxy evolution and cosmology (BAO): all-sky HI + continuum survey III. Cosmic magnetism -- origin and evolution: all sky RM survey IV. Strong field tests of GR using pulsars V. Cradle of Life: star and planet formation, astrochemistry/biology, SETI JWST primary science goals: The end of the dark ages: first light and reionization The assembly of galaxies and SMBH The birth of stars and proto-planetary systems Planets and the origins of life

6. 6 AUI Cooperative Agreement Proposal NSF Panel Review August 25 – 28, 2008 Multi-wavelength approach to addressing key questions in modern astrophysics

7. 7 AUI Cooperative Agreement Proposal NSF Panel Review August 25 – 28, 2008 Power of radio astronomy Seeing through dust: earliest phases of star and galaxy formation Cool universe: thermal emission from gas, dust = fuel for star and galaxy formation  as astrometry sub-mas imaging m/s velocity resolution Accurate polarimetry -- magnetic fields on all scales Chemistry and bio-tracers HST + OVRO CO VLA polarization

8. 8 HST SMA 350 GHz detection of proplyds in Orion Derive dust mass (>0.01M o ), temperature KSP V: Protoplanetary disks and planet formation Williams et al.

9. 9 TW Hya Disk: VLA observations of planet formation Calvet et al. 2002 mid-IR “gap” cm slope ”pebbles” Pre-solar nebula analog 50pc distance star mass = 0.8M o Age = 5 -- 10 Myr mid IR deficit => disk gap caused by large planet formation at ~ 4AU?

10. 10 TW Hya Disk: VLA observations of planet formation Hughes, Wilner + VLA imaging on AU-scales: cm probes grains sizes between ISM dust and planetesimals (~1cm) Double-peak morphology is consistent with disk gap model Dec= -34

11. 11 ALMA 850 GHz, 20mas Wolfe + Birth of planets: The ALMA/EVLA revolution Radius = 5AU = 0.1” at 50pc Mass ratio = 0.5M Jup /1.0 M sun Wilner ALMA: AU-scale imaging of dust, gas, unhindered by opacity, nor confused by the central star, on 10mas scale -- secular changes on yearly timescales EVLA: AU-scale imaging of large dust grain emission (PT link gives fact 2 improvement in resolution) JWST: image dust shadow on scales 40 mas Herschel: dust spectroscopy

12. 12 Infrared Dark Clouds (IRDCs) 0.5 o  Extinction features seen in silhouette against the Galactic IR background  1,000s seen in the Spitzer GLIMPSE survey (and previous surveys like MSX) Egan et al. (1998); Carey et al. (2000); Smith et al. (2006); Rathborne et al. (2006); Pillai et al. (2006) and many others  Sites of the earliest phases of massive star formation 3.6  m 4.5  m 8.0  m

13. 13 Mapping the Galactic Web of Dense Molecular Gas in IRDCs: Initial Conditions of Massive Star Formation VLA 3-pointing NH 3 mosaic Velocity => distance Dense gas tracer: physical conditions, chemical evolution Many hours observing: not an efficient way to survey Devine et al. in 2’ GBT 1.3 cm heterodyne focal plane arrays  large area mapping of NH 3 ~ GLIMPSE  essential to understand the initial conditions of massive star formation

14. KSP IV: Gravitational wave detection using a ‘pulsar timing array’ (NANOGrav, Demorest +) D. Backer Predicted timing residuals Need ~20-40 MSPs with ~100 ns timing RMS bi-weekly obs for 5-10 years Timing precision depends on - sensitivity (G/T sys ) (i.e. GBT and Arecibo)‏ - optimal instrumentation (GUPPI -- wideband pulsar BE)

15. Credit: D. Manchester, G. Hobbs NanoGrav

16. 16 KSP II: Cosmology -- measure H o to few % with extragalactic water maser disks. Why do we need an accurate measure of H o ? To make full use of 1% measures of cosmological parameters via Planck-CMB studies requires 1% measure of H o -- covariance! with H o constraint

17. 17 Measuring Distances to H 2 O Megamasers Two methods to determine distance: “Acceleration” method D = V r 2 / a  “Proper motion” method D = V r / (d  /dt) NGC 4258 2V r 2  D = r/  a = V r 2 /r D = V r 2 /a  VrVr  Herrnstein et al. (1999) D = 7.2  0.5 Mpc Recalibrate Cepheid distance scale Problem: NGC 4258 is too close

18. 18 The Project (Braatz et al.) 1.Identify maser disk galaxies with GBT into Hubble flow ~ 50 currently 2.Obtain high-fidelity images of the sub-pc disks with the High Sensitivity Array (VLBA+GBT+Eff+eVLA) ~ 10% are useful 3.Measure internal accelerations with GBT monitoring 4.Model maser disk dynamics and determine distance to host galaxy Goal: 3% measure of H o GBT

19. 19 UGC 3789: A Maser Disk in the Hubble Flow Discovery: Braatz & Gugliucci (2008) VLBI imaging: Reid et al. (in prep) Distance/modeling: Braatz et al. (in prep) Acceleration modeling D ~ 51 Mpc H o = 64 (+/-7) Already at HST Key project accuracy with 1 source!

20. 20 Dark Ages Cosmic Reionization Major science driver for all future large area telescopes Last phase of cosmic evolution to be tested Bench-mark in cosmic structure formation indicating the first luminous sources Radio astronomy role Gas, dust, star formation, in first galaxies HI 21cm ‘tomographic imaging’ of neutral IGM KSP I: Cosmic reionization and first (new) light in the Universe

21. 21 Highest redshift SDSS QSO L bol = 1e14 L o Black hole: ~3 x 10 9 M o ( Willot etal. ) Gunn Peterson trough = near edge of reionization (Fan etal.) Pushing into reionization: QSO 1148+52 at z=6.4 (t univ = 0.87Gyr) GP effect => first galaxies/BH are only observable at near IR through radio wavelengths

22. 22 Dust mass ~ 7e8 M o Gas mass ~ 2e10 M o CO size ~ 6 kpc Low order molecular lines redshift to cm bands = ‘fuel for gal formation’ mm/cm: Gas, Dust, Star Form, in host galaxy of J1148+5251 1” ~ 6kpc CO3-2 VLA z=6.42 30% of z>6 SDSS QSO hosts are HyLIRGs Dust formation associated with high mass star formation? L FIR = 1.2e13 L o MAMBO/IRAM 30m Only direct observations of host galaxy properties

23. 23  FIR excess -- follows Radio-FIR correlation: SFR ~ 3000 M o /yr  CO excitation ~ starburst nucleus: T kin ~ 100K, n H2 ~ 1e5 cm -3 Radio-FIR correlation 50K Elvis QSO SED Continuum SED and CO excitation: ISM physics at z=6.42 NGC253 MW

24. 24 [CII] 158um at z=6.4: dominant ISM gas coolant [CII] PdBI Walter et al.  z>4 => FS lines redshift to mm band  L [CII] = 4x10 9 L o (L [NII] < 0.1 L [CII] )  [CII] similar extension as molecular gas ~ 6kpc => distributed star formation  SFR ~ 6.5e-6 L [CII] ~ 3000 M o /yr 1” [CII] + CO 3-2 [CII] [NII] IRAM 30m

25. 25 Building a giant elliptical galaxy + SMBH at t univ < 1Gyr  Multi-scale simulation isolating most massive halo in 3 Gpc^3 (co-mov)  Stellar mass ~ 1e12 M o forms in series (7) of major, gas rich mergers from z~14, with SFR ~ 1e3 - 1e4 M o /yr  SMBH of ~ 2e9 M o forms via Eddington-limited accretion + mergers  Evolves into giant elliptical galaxy in massive cluster (3e15 M o ) by z=0 10.5 8.1 6.5 Li, Hernquist, Roberston.. z=10 Rapid enrichment of metals, dust, molecules Rare, extreme mass objects: ~ 100 SDSS z~6 QSOs on entire sky Integration times of hours to days to detect HyLIGRs

26. 26 (sub)mm: high order molecular lines. fine structure lines -- ISM physics, dynamics cm telescopes: low order molecular transitions -- total gas mass, dense gas tracers Pushing to first normal galaxies: spectral lines  FS lines will be workhorse lines in the study of the first galaxies with ALMA.  Study of molecular gas in first galaxies will be done primarily with cm telescopes SMA ALMA will detect dust, molecular and FS lines in ~ 1 hr in ‘normal’ galaxies (SFR ~ 10 M o /yr = LBGs, LAEs) at z ~ 6, and derive z directly from mm lines., GBT GBT

27. 27 cm: Star formation, AGN (sub)mm Dust, cool gas Near-IR: Stars, ionized gas, AGN Arp 220 vs z Pushing to normal galaxies: continuum A Panchromatic view of galaxy formation SMA GBT eg. GBT = wide field ‘finder’; ALMA = detailed imager

28. 28 AUI Cooperative Agreement Proposal NSF Panel Review August 25 – 28, 2008 END

29. 29 1.4 GHz stacking: 30,000 z~2 ‘normal’ galaxies in COSMOS Current VLA ~ 40 uJy detections; Stacking => 2 +/- 0.2 uJy 2e10 M o 3e11 Radio-derived UV-derived (w/o dust corr.) 100 M o /yr 10 M o /yr 5x Specific star formation rate = SFR/M * vs. stellar mass  Radio: no dust-bias, SSFR ~ constant w. M * => ‘universality of SF in galaxies’  ~ 5x, but strong trend with SFR (or M * ): key to understanding star form history of Universe EVLA will detect (individually) 100’s of normal star forming galaxies at high redshift in every deep field at 1.4 GHz Panella etal

30. 30 HI 21cm Tomography of IGM z=14 7.6  SKA: Direct imaging of evolution of neutral IGM  Pathfinders: statistical detection (power spectrum), largest Stromgren spheres, absorption toward first radio AGN

31. 31 Experiments under-way: pathfinders 1% to 10% SKA MWA (MIT/CfA/ANU) NRAO participates on individual basis in path-finders NRAO has world-leading expertise in low freq H/W and S/W, and is developing critical wide field imaging software for LWA, EVLA -- additional resources could benefit all experiments NRAO has interest in contributing to development of, and potentially operating, next-gen experiment, perhaps parallel mode to FASR project

32. 32 Destination: Moon! Low frequency array on far side of Moon by 2025  No interference  No ionosphere NASA’s top astronomy priority for Presidential initiative to return Man to Moon 2008 NASA Lunar Science Institute: Mission concept study (Colorado, NRL, NRAO, MIT++)

33. 33 RIPL Radio Interferometric Planet Search Detect Jupiter mass planets around nearby low mass stars through astrometric wobble 32 stars –M1 – M8 –D = 2.7 – 9.5 pc –11 are members of known binary or multiple systems 12 epochs/star/3 years –VLBA + GBT –512 Mb/s –1392 hours total Bower et al.

34. 34 TW Hya -- Molecular gas SMA: Gas mass, rotation ALMA: dynamics at sub-AU, sub- km/s resolution SMA ALMA simulation Wilner