Presentation is loading. Please wait.

Presentation is loading. Please wait.

Science with a Next Generation Very Large Array Notional Specifications Physical area 6 x VLA, but higher efficiency > 30 GHz Frequency range: 1 – 50,

Similar presentations


Presentation on theme: "Science with a Next Generation Very Large Array Notional Specifications Physical area 6 x VLA, but higher efficiency > 30 GHz Frequency range: 1 – 50,"— Presentation transcript:

1 Science with a Next Generation Very Large Array Notional Specifications Physical area 6 x VLA, but higher efficiency > 30 GHz Frequency range: 1 – 50, 70 – 115 GHz Configuration: 50% to few km; 40% to 200km; 10% to 3000km

2 Process to date Jan 2015: AAS Jan community discussion https://science.nrao.edu/science/meetings/2015/aas225/next-gen-vla/ngvla March 2015: Science working group white papers  Cradle of Life (Isella, Moullet, Hull)  Galaxy ecosystems (Murphy, Leroy)  Galaxy assembly (Lacy, Casey, Hodge)  Time domain, Cosmology, Physics (Bower, Demorest) April 2015: Pasadena technology meeting

3 Resolution ~ 1cm (180km) Killer Gap Thermal imaging on mas scales at λ ~ 0.3cm to 3cm 140pc B. Kent

4 Sensitivity ~ 1cm, 10hr, 8GHz T B ~ 1cm, 15mas Real line science begins at 15GHz Killer Gap Thermal imaging on mas scales at λ ~ 0.3cm to 3cm

5 Many other parameters: FoV, Bandwidth, T sys, RFI occupation, UV coverage (dynamic range, surface brightness), Atmospheric opacity and Phase stability, Pointing… Relative metrics depend on science application Killer Gap Thermal imaging on mas scales at λ ~ 0.3cm to 3cm

6 Cradle of life: Terrestrial planet formation imager (Isella et al. SWG1) See through dust to pebbles: inner few AU disk optically thick in mm/submm Grain size stratification at 0.3cm to 3cm:  Poorly understood transition from dust to planetesimals  Annual changes τ = 1 at λ < 1mm τ = 1 at λ > 1cm ngVLA zone 100AU

7 Terrestrial planet formation imager Circumplanetary disks: imaging accretion on to planets? Imaging Earth-like planets in habitable zone is top priority in OIR in the next decade: “The vision outlined in this report is for a 10–12 m segmented space telescope with exquisite sensitivity from the UV through the NIR, and superb image and wavefront quality. This observatory would allow direct detection of Earth-like planets and characterization of their atmospheres, along with a rich program of astrophysics covering every stage of the pathway from cosmic birth to living earths.” AURA report ‘Future of UVOIR Space Astronomy’

8 Cradle of Life: origin stars, planets, life Star formation  Origin of stellar multiplicity  High mass star formation: resolving accretion in dust-obscured early phases Peer deep into planetary atmospheres, comets, asteroids, sub-surface radar Chemistry in PP disks on AU- scales  Complex organics: ice chemistry in cold regions  Pre-biotic molecules: rich spectra in 0.3cm to 3cm regime  Ammonia and water Glycine; Codella ea SKA ngVLA

9 SF Law Galaxy assembly (Casey + SWG3): Dense gas history of Universe Missing half of galaxy formation SFR Gas mass (L CO 1-0 )

10 Gas mass calibrated w. CO 1-0  Total gas mass w/o excitation uncertainty  Dense gas tracers associated w. SF cores: HCN, HCO+ Low order CO: key total cool gas mass tracer ngVLA ‘sweet spot’ SKA 10x uncertainty

11 Galaxy assembly CO emission from typical star forming, ‘main sequence’ galaxies at high z z=5, 30 M o /yr, 1hr, 300 km/s Number of CO detections per hour JVLA ~ 1, M gas > M o ngVLA: tens to hundreds, M gas > M o JVLA ngVLA

12 CO 1-0 CO 3-2 z ~ 3 Galaxy assembly: Imaging on 1 kpc-scales Low order: distributed gas dynamics, not just dense cores w. ALMA dust imaging: resolved star formation laws (gas – SFR surface density) Narayanan n cr > 10 4 cm -3 n cr ~ 10 3 cm -3

13 Galaxy eco-systems (Murphy + SWG2) Milky Way and the nearby Universe Broad-Band Continuum Imaging Simultaneously capture multiple radio emission mechanisms: synchrotron, free-free, cold (spinning?) dust, SZ effect Independent estimates of SFR Physics of cosmic rays, ionized gas, dust, and hot gas around galaxies ngVLA

14 Spectral Line 10GHz to 100GHz on pc-scales Map cool ISM 10x faster than ALMA First order transitions of major astrochemical tracers Baryon cycle: following life cycle of gas to stars to gas Snell ea Schinerer ea.

15 Galaxy eco-systems: Milky Way and the nearby Universe VLBI uas astrometry Complete view of the large scale structure of MW 3D imaging of dynamics of local group: dark matter, real-time cosmology Not strongly dynamic range limited: 10% on long baselines?

16 Physics, cosmology, time domain ( Bower et al. SWG4) Time domain: phenomena 0.3cm to 3cm  FRBs, TDEs  Solar bursts  Radio photospheres Novae: ‘peeling onion’  Radio counterparts to GW events 10GHz 1GHz GBR/TDE: late time jet shock 15GHz

17 The plasma Universe: solar flares to galaxy clusters Magnetic reconnection vs. shock acceleration: broad band phenomena Stellar photospheres, winds, mass loss Stellar-exoplanet magnetospheric interactions Physics, cosmology, time domain 100ms solar flares Mpc-scale cluster emission

18 Physics, cosmology, time domain Megamasers and H o : double precision cosmology Evolution of fundamental constants using radio absorption lines: best lines in K through Q band CO intensity mapping: BAO in matter dominated era (z>2) Galactic center pulsars

19 Killer gap: where ngVLA excels wrt SKA1 and ALMA Imaging terrestrial zone planet formation Dense gas history of Universe Pre-biotic molecules Maser, CO cosmology Next steps  Quantify! physical modeling + configurations + simulations  Focused workshop on science case, calculations  Call for community white papers?


Download ppt "Science with a Next Generation Very Large Array Notional Specifications Physical area 6 x VLA, but higher efficiency > 30 GHz Frequency range: 1 – 50,"

Similar presentations


Ads by Google