1. 1 National Radio Astronomy Observatory NRAO Operations Review ~ February 29 – March 1, 2008 Current and Future Science with NRAO Instruments Chris Carilli Four exemplary science programs that demonstrate the synergy between NRAO instruments, and their key roles in modern, multiwavelength astrophysics. a.First galaxies: gas, dust, star formation into cosmic reionization b.Cosmic geometry: Megamasers and a 3% measure of H o c.Protoplanetary disks: imaging planet formation d.At the extremes of physics: strong field GR, TeV sources explained!

2. 2 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 I.Radio studies of the first galaxies: gas, dust, star formation, into cosmic reionization

3. 3 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)

4. 4 Dust mass ~ 7e8 M o Gas mass ~ 2e10 M o CO size ~ 6 kpc Note: low order molecular lines redshift to cm bands 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? AGB Winds take > 1.4e9yr > age Universe => dust formation associated with high mass star formation? L FIR = 1.2e13 L o MAMBO/IRAM 30m

5. 5  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

6. 6 [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

7. 7 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

8. 8 (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

9. 9 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

10. 10 II. Cosmic geometry: H o to few % with 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

11. 11 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

12. 12 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

13. 13 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!

14. 14 HST SMA 350 GHz detection of proplyds in Orion Derive dust mass (>0.01M o ), temperature III. Protoplanetary disks and planet formation Williams et al.

15. 15 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?

16. 16 TW Hya Disk: VLA observations of planet formation Hughes, Wilner + VLA imaging on AU-scales: consistent with disk gap model cm probes grains sizes between ISM dust and planetesimals (~1cm) Dec= -34

17. 17 ALMA 850 GHz, 20mas res. 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 EVLA: AU-scale imaging of large dust grain emission JWST: image dust shadow on scales 10’s mas Herschel: dust spectroscopy

18. 18 TW Hya -- Molecular gas SMA: Gas mass, rotation ALMA: dynamics at sub-AU, sub- km/s resolution SMA ALMA simulation Wilner

19. Credit: Bill Saxton, NRAO IV. At the extremes of physics Extreme gravity: using pulsars to detect nHz gravity waves TeV sources: explained by VLBI!

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

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

22. 22 ●Discovered 1976 @ 100 MeV; variable 5 GHz emission. ●High mass binary: 12 M סּ Be *, 1–3M סּ NS or BH. ●Eccentric orbit e=0.7, period 26.5 days. ●X-rays peak @ periastron, radio 0.5 cycle later. ●TeV detected by Magic ●MODELS: (A)Accretion powered relativistic jet (microQuasar?) (B)Compact pulsar wind nebula LS I +61 303: Solving the TeV mystery > 400 GeV Xray Radio Albert+ 2006 Harrison + 2000

23. VLBA Images vs. Orbital Phase (orbit exaggerated) VLBA movie shows 'cometary' morphology => a Pulsar Wind Nebula shaped by the Be star envi- ronment, not a relativistic jet. Dhawan + VLBA resolution ~ 2AU BeBe

24. 24 Gamma-Rays from AGN Jets GLAST launch scheduled for May 2008 VLBA jet imaging on pc-scales during flares required to understand gamma ray production Prelaunch survey: VIPS project to image 1100 objects (Taylor et al.) Planned: 43 GHz + GLAST monitoring of gamma ray blazars Marscher et al.

25. 25 NRAO in the modern context Golden age of astrophysics: NRAO telescopes play a fundamental role in topical areas of modern astrophysics Precision cosmology: setting the baseline (Planck ++) Galaxy evolution and first (new) light: gas, dust, star formation (JWST, TMT) Birth of stars and planets: dust and gas on AU scales (JWST, Herschel) Testing basic physics: GR, fundamental constants, … (LIGO, LISA) Resolving high energy phenomena: a  ray source primer (GLAST, CONX) Capabilities into next decade keep NRAO on the cutting edge ALMA -- biggest single step ever in ground based astronomy EVLA -- the premier cm telescope on the planet, and a major step to the SKA GBT -- just hitting its stride, with pending FPA revolution VLBA -- Mankind’s highest resolution instrument

26. 26 END

27. 27 Current large programs: VLA, VLBA, GBT AUI Operations Review February 29 – March 1, 2008 Radio interferometric planet search -- VLBA, VLA, GBT Coordinated radio and infrared survey for high mass star formation -- VLA Definitive test of star formation theory -- GBT Legacy survey of prebiotic molecules toward Sgr B2 and TMC-1 -- GBT Detecting nHz gravitational radiation using pulsar timing array -- GBT Star Formation History and ISM Feedback in Nearby Galaxies -- VLA LITTLE THINGS survey: HI in dwarf galaxies -- VLA Megamaser cosmology project -- GBT, VLBA, VLA Probing blazars through multi-waveband variability of flux, polarization, and structure -- VLBA MOJAVE/GLAST program: mas imaging of gamma ray sources -- VLBA VLA low frequency sky survey -- VLA Deep 1.4 GHz observations of extended CDFS -- VLA

28. GR tests: Timing of the Double Pulsar J0737-3039 GBT provides the best timing precision for this system 6 post-Keplerian orbital terms give neutron star masses strong-field tests of GR to 0.05% accuracy Measure relativistic spin precession: Obs = 5.11+/- 0.4 deg/yr GR = 5.07 deg/yr Kramer et al., 2006, Science, 314, 97