ngvla The Next Generation Very Large Array

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1 NATIONAL RADIO ASTRONOMY OBSERVATORY Extremely Large Telescopes ngvla The Next Generation Very Large Array

2 Extremely Large (Optical) Telescopes in the Era of ngvla Stefi Baum and Chris O Dea University of Manitoba Slides from Michele Cirasuolo (E-ELT), Warren Skidmore (TMT), Pat McCarthy (GMT), David Silva (LSST). The Next Generation Very Large Array

Heart of Glass The next generation optical telescopes will likely consist of: Thirty Meter Telescope (TMT, northern hemisphere) Giant Magellan Telescope (GMT, Chile) European Extremely Large

3 Heart of Glass The next generation optical telescopes will likely consist of: Thirty Meter Telescope (TMT, northern hemisphere) Giant Magellan Telescope (GMT, Chile) European Extremely Large Telescope (E-ELT, Chile) Large Synoptic Survey Telescope (LSST, Chile) There will be all sky coverage by the combination of large optical telescopes. The TMT, GMT, and E-ELT will be general purpose observatories with a wide suite of instrumentation. The Next Generation Very Large Array

4 An ELT Instrumentation Equivalence Table Type of Instrument GMT TMT E-ELT Near-IR, AO-assisted Imager + IFU GMTIFS IRIS HARMONI Wide-Field, Optical Multi-Object Spectrometer GMACS WFOS MOSAIC-HMM Near-IR Multislit Spectrometer NIRMOS IRMS MOSAIC-HMM Deployable, Multi-IFU Imaging Spectrometer IRMOS MOSAIC-HDM Mid-IR, AO-assisted Echelle Spectrometer MIRES METIS High-Contrast Exoplanet Imager TIGER PFI ELT-PCS Near-IR, AO-assisted Echelle Spectrometer GMTNIRS NIRES HIRES High-Resolution Optical Spectrometer G-CLEF HROS HIRES Wide -Field AO-assisted Imager IRIS MICADO 4

5 Features of the ELTs High resolution diffraction limited imaging (~7 mas at 1μm) Quick response time to ToOs (~10 min). Time domain science (1 ms photometry). Sensitivity to new classes of objects. The Next Generation Very Large Array

$Diffraction limited$ TMT TMT resolution at 1µm

6 Diffraction limited observations with AO on TMT TMT resolution at 1µm (λ/d) is 7 mas, 4 mas pixels 7 mas = 200m at 5Mkm, 25 km at 5 AU (Jupiter) AU at 5 pc (nearby stars), pc at 1 Mpc, 300 pc at z~2.5! 6

7 Imaging the Galactic Center Black Hole Current GMT Technology GMT AAS OPEN HOUSE - JAN 5,

8 Simulated AO Images Globular Cluster around Cen A 3.8Mpc 3pc core radius H-band Gemini 8m GMT 25m GMT Overview Sept 23, 2016 Ohio University 0.5 8

9 GMT Image Simulations Current Telescopes Hubble Space Telescope GMT with Adaptive Optics James Webb GMT w/adaptive Optics 9

10 10 ToO programs and Time Critical or Coordinated Observing Programs TMT policies for ToO and Time Critical Observations (TCO) are the most mature of the ELTs. But incomplete! Have not yet defined policies for multi-facility cooperation TMT policies for ToO and TCO are in-line with those considered for E-ELT and GMT All future ELTs will be capable of; Changing to a new science target on a timescale of a few minutes Changing and configuring an instrument and acquiring a new target within 10 to 30 minutes or faster All regularly offered observing modes can be expected to be available on these timescales All ELTs are being designed to support ToO interrupts within any observing mode

11 ToO programs and Time Critical or Coordinated Observing Programs Queue scheduled observations will be a major operating mode for all ELTS (may be the dominant mode) Pre-approved ToO overrides will usually be implemented during queue scheduled observations Up to 1 hour per night for ToO during PI directed observations (at the discretion of the observer) ToO PIs will be notified of a trigger and encouraged to eavesdrop on and participate in the observations The overall impact of ToO observations on a partner s time will be limited to 2 to 5% (TBD) per semester 11

12 ToO programs and Time Critical or Coordinated Observing Programs Pre-planned time-critical observations will be accommodated in the service observing schedule This allows for

12 12 ToO programs and Time Critical or Coordinated Observing Programs Pre-planned time-critical observations will be accommodated in the service observing schedule This allows for executing contemporaneous observations with other facilities Time-critical observations cannot be interrupted for ToO Cadence observing will also be accommodated during queue scheduled observation

13 Summary of observing capabilities ELTs will be general purpose observatories with all major forms of instrumentation mid-late 2020s ~2.5 yr cadence for new TMT instruments and AO Active concepts and development process is defined Flexible on the timescale for NASA Large Mission overlap All sensible levels of ToO and TCO support with the ELTs can be expected ToO will not always be available and there are restrictions on the schedule impacts of ToO programs Details of multi-facility coordination TBD, but queue scheduling allows for TCOs 13

14 Pulsars WD-NS are test-beds for strong-field gravity theories and alternative gravity theories Modeling the optical spectral lines of the white dwarf and high-precision radio pulsar timing yields

14 14 Pulsars WD-NS are test-beds for strong-field gravity theories and alternative gravity theories Modeling the optical spectral lines of the white dwarf and high-precision radio pulsar timing yields the masses of components in WD-NS binary systems independently of gravity theory High sensitivity and spectral resolution of TMT increases the sample of WD-NS systems with precise mass measurements of the binary components Pulsars spin periods range upwards from milliseconds and cyclotron emission ranges from X-ray to radio. Simultaneous optical/ir and radio observations of the spectral dependence of the pulse shape and spin resolved polarimetry provide information about the geometry of the emission region, the magnetic field, the effects of inclination and allow details of the emission mechanism Low resolution (R 100) optical and NIR (to 1.2 µm) time resolved (t samp ~0.1ms) spectroscopy and spectropolarimetry are needed Large numbers of Pulsars will be discovered with SKA and will need intensive follow-up from ngvla and TMT

Gamma Ray Bursts Explosion Studies of the GRB fireball with prompt observations, beginning within a few hundred seconds of the trigger detection The suggested fire ball model is an inhomgenous

15 Gamma Ray Bursts Explosion Studies of the GRB fireball with prompt observations, beginning within a few hundred seconds of the trigger detection The suggested fire ball model is an inhomgenous relativistic outflow with inverse Compton or synchrotron emission, velocity variations causing γ-ray emission, mild internal shocks at larger radii cause optical emission Radio observations provide the physical properties of the jet and surrounding material Telescope response time of <10 minutes for TMT Flux variations of a factor 10 over 1 minute need to be sampled Low resolution spectroscopy (R~100) with 1s sampling is required in passbands in the optical to NIR (400nm to 2.2µm) 100s exposure time high SNR polarimetric imaging to get information on asymetry 15

16 Planets & Stars Stars & Galaxies ELT Science Galaxies & Cosmology

17 ELT Instrumentation Programme First generation instruments (2024) MICADO+MAORY Imager and single slit spectrograph HARMONI Integral Field Spectrograph METIS Mid-IR imager and spectrograph Second generation instruments (now in Phase A) Third generation HIRES High resolution spectrograph MOSAIC Multi-object spectrograph PCS Extreme AO imager and spectrograph

18 Science with MICADO+MAORY 1 st light E-ELT camera (diffraction limited imaging at near-infrared wavelengths) Work-horse instrument Versatile, addresses a wide range of science cases Spatial resolution at diffraction limit, sensitivity, astrometry Ø Galaxy evolution and star formation history across cosmic time Ø Black Holes in Galaxies centres Ø Resolved stellar populations in galaxies (out to Virgo Cluster) Ø High-contrast imaging of exo-planets Ø Solar system Ø Time resolved astronomy 18

Science with HARMONI 1 st light E-ELT Integral Field Spectrograph (optical and near-ir) Work-horse instrument Spatially resolved spectroscopy: Ø The Physics of Galaxies across cosmic time Ø From

19 Science with HARMONI 1 st light E-ELT Integral Field Spectrograph (optical and near-ir) Work-horse instrument Spatially resolved spectroscopy: Ø The Physics of Galaxies across cosmic time Ø From first light to the earliest galaxies Ø Black Holes and AGNs Ø Stellar Populations: SF history, chemical & dynamical evolution Ø From giant to terrestrial exo-planets Ø Resolved Spectroscopy of Solar System Objects 19

20 Science with METIS Mid-infrared ELT Imager and Spectrograph: Discovery and Characterization of Exoplanets. Circumstellar Disk Structure and Evolution. Formation and Evolution of Stars and Star Clusters. Physics and Chemistry of the Solar System. Formation and Evolution of Galaxies. 20

21 Science with MOSAIC Multi-object and multi-integral field spectrograph in the visible and near-ir: - First Galaxies - Large scale structures and 3D reconstruction of IGM - Galaxies mass assembly - Dark matter - AGN/Galaxy coevolution - Resolved stars beyond the LG - Galaxy archaeology - Galactic centre - Planet formation in clusters

22 Science with HIRES High Resolution Spectrograph (R ~ 100,000, λ ~ μm): Exoplanets (characterisation of Exoplanets Atmospheres: detection of signatures of life) Stellar Astrophysics (abundances of solar type and cooler dwarfs in galactic disk bulge, halo and nearby dwarfs: tracing chemical enrichment of Pop III stars in nearby universe) Intergalactic Medium (Signatures of reionization and early enrichment of ISM & IGM observed in high-z quasar spectra) Fundamental Physics (variation of fundamental constants - α, mp/me, Sandage Test) Protoplanetary Disks (dynamics, chemistry and physical conditions of the inner regions) Stellar Populations (metal enrichment and dynamics of extragalactic star clusters and resolved stellar populations) Galaxy Evolution (massive early type galaxies during epochs of formation and assembly) Supermassive Black Holes (the low mass end)

23 LSST: A Deep, Wide, Fast, Optical Sky Survey 8.4m telescope deg2 ugrizy 3.2Gpix camera 10mas astrom. r<24.5 (<27.5@10yr) 0.5-1% photometry 30sec exp/4sec rd 15TB/night 37 B objects Imaging the visible sky, once every 3 days, for 10 years (825 revisits) IAU 2015 Honolulu, Hawai i August 4,

24 24 Alert Rate In ten minutes time the LSST transient pipeline is likely to issue ~80,000 alerts at 5σ. While most of these will be moving objects, perhaps several thousand will be flaring objects or bursts. Possibly new kinds of objects! Clearly any followup requires high purity samples. What is needed then is highly trusted event classification. FAST

Milky Way Ø Tidal streams Ø Galactic structure Dark energy and dark matter Ø Gravitational lensing How does one

25 The Science Enabled by LSST Time domain science Ø Novae, supernovae, GRBs Ø Source characterization Ø Instantaneous discovery Finding moving sources Ø Asteroids and comets Ø Proper motions of stars Mapping the Milky Way Ø Tidal streams Ø Galactic structure Dark energy and dark matter Ø Gravitational lensing How does one do research when faced with trillions of catalog entries, and potentially millions of measurements for each class of objects?

26 Summary During the lifetime of the ngvla, the whole sky will be accessed by 30-m class telescopes. These telescopes will be general purpose observatories with a broad suite of instrumentation. The 30-m telescope will be capable of short response ToO and short timescale ~0.1 ms integrations enabling time domain science in the visible and near-ir. There is a lot of complementary science enabled on the ngvla and 30-m class telescopes. The Next Generation Very Large Array

MEGAN DONAHUE MICHIGAN STATE UNIVERSITY SCIENCE OF GSMTS

MEGAN DONAHUE MICHIGAN STATE UNIVERSITY SCIENCE OF GSMTS MICHIGAN STATE UNIVERSITY SCIENCE OF GSMTS 30-M PROJECTS GIANT MAGELLAN TELESCOPE (GMT) 7 mirrors, 8.5 m (24.5M eff. diameter) Chile THIRTY METER TELESCOPE (TMT) 30 m, segmented primary Canary Islands