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The Next Generation Space Telescope Board on Physics & Astronomy Steven Beckwith April 28, 2000 102 1600 1700 1800 104 1900 Hubble ST Photographic & electronic detection Keck, VLT, Gemini ... CCDs Telescopes alone Mount Palomar 200” Soviet 6-m Photography 106 Mount Wilson 100” Rosse’s 72” Herschell’s 48” 108 Short’s 21.5” 0 Huygens eyepiece Slow f ratios Galileo Sensitivity improvement over the unaided eye NGST Telescopes & Discovery 101 2000 Year of observations After Fig. 3.10 in Cosmic Discovery, M. Harwit 2 Galaxy Sizes in the HDF No significant evolution out to z~1 There is a small population of compact high-SB galaxies that do not fit in the normal Hubble Sequence By z ~ 3, the normal Hubble sequence disappears and most galaxies are compact and high SB 3 z=2.5 z=1.5 z=0 Galaxy Sizes HDF galaxies with z~1 Shifted to z=2.5 4 Lyman-break Galaxies 5 Unique Infrared Objects Dickinson et al. 1999 Optical Infrared 0.33 0.44 0.55 0.8 1.25 U B V I J 1.65 mm H 6 Star-Formation Rates • UV luminosity density – Gives unobscured star-formation rate, metalformation rate – Extinction corrections uncertain • Consistent with other measures of global chemical evolution? • Clustering & star formation? Madau et al. 1996, Rowan-Robinson et al. 1996… Calzetti & Heckman 1999, Pei et al. 1999 7 Future Surveys Haiman & Loeb 1998 model counts NGST 106 s ACS + WFC3 106 s NICMOS 106 s z >10 galaxies quasars Ly-break z=3 Ly-break z=4 HDFS phot z>5 8 NGST At a Glance • • • • • • 8m primary mirror 0.6-27 µm wavelength range 5 year mission life (10 year goal) passively cooled to <50K L2 orbit - Logical successor to HST 3 Core instruments - Key part of the Origins Program – 0.6-5 µm camera – 1-5 µm Multiobject Spectrometer – 5-27 µm camera/spectrometer • 2009 launch 9 NGST Concepts: Phase I Lockheed Martin TRW/Ball 10 Discovery Space NGST 2009 2002 11 NGST: Core Science Goals • Origin & Evolution of Galaxies – The Dark Ages • The Creation of the Elements • The Birth of Galaxies – History of the Milky Way & its Neighbors • Cosmology and Structure of the Universe • Birth of Stars and Planetary Systems 12 Origins and Evolution of Galaxies Seeing the “Dark Ages” • When and how do the first stars and galaxies form? – HST and Keck have detected very luminous star forming regions/galaxies that appeared 1 billion years after the Big Bang (to z ~ 5.6) – New stars appear to be forming at roughly a constant rate until very recently (1 < z < 5) – SCUBA may have detected a significant component of dust-hidden star formation at cosmological distances • To see the growth of galaxies such as our Milky Way, we need NGST (0.6-10µm) – Sensitivity to see the first epoch of star formation, (z ~ 10-20, 0.1 nJy sensitivity in 1 week) – Angular resolution and wide field to survey 100,000 protogalaxies and their environments (to z ~ 5) – mid infrared imaging and spectroscopy to pinpoint the nature of the hidden stars and Active Galactic Nuclei 13 Close-up shows little confusion No Noise, AB ~ 35 NGST PSF, AB ~ 30 10” 15 The Epoch of Reionization • Needs high sensitivity, spectroscopy, R ~ 100. • NGST capability ideal if zreion > 7 (Lya > 1µm). • NGST is uniquely capable if Gunn-Peterson trough falls in atmospheric absorption region. zreion = 8 zreion = 7 zreion = 11 16 Mapping Dark Matter • Weak lensing is best method for measuring masses of galaxies and structures for z >1. – HST/NGST PSF ideal for faint, small background galaxies (Mellier, Schneider) – Large scale (linear) structure on scales of arcmin or individual galaxy lensing on scales of ~ 10 arcsec gives polarizations ~ 1%, requires ~ 104 galaxies. – Optical depths 5 x greater for zsource 1-> 5. • NGST images yield ~ 104 galaxies with z > 2 per 4’ x 4’ field of view. • RMS shear > 10% at z ~ 10 means dark matter mapping is crucial component of deep field surveys! 17 NGST Deep Imaging: 0.5–10 mm 4’x4’ deep survey field 5000 galaxies to AB ~ 28, 105 galaxies to AB ~ 34 photometry, morphology & z's Depth: AB ~ 34 in 106 s Redshifts: Lyman a to z = 40 (?) 4000 Å to z = 10 NGST will detect 1 M yr-1 for 106 yrs to z 20 and 108 M at 1 Gyr to z 10 (conservatively assuming W = 0.2) Origins and Evolution of Galaxies: Imaging & Spectra • Multi-Object Spectroscopy – Deep, R ~ 100, KAB~31 (Photometric redshift verification) – Emission line diagnostics, KAB ~33 R ~ 1000, • Star-formation rates • Metallicities/reddening • Kinematics of bound groups/proto Milky Way galaxies NGC 7714 @ z = 6 (Kennicutt 1998) Sensitivity (10 s) ~ 0.2 M yr-1 z ~ 7 ~ 1.0 M yr-1 z ~ 12 19 Hubble’s Law: Wmatter & WL 5.0 1.2 WMatter: 0.3 W : 0.3 WL:Matter0.7 WL: 0.7 Redshift z 1.0 4.0 0.8 3.0 WMatter: 1.0 WL: 0.0 WMatter: 1.0 WL: 0.0 0.6 2.0 0.4 1.0 0.2 HST only 0.0 0 10 50 20 100 30 150 40 200 Luminosity distance (Billion light-years) 20 Star and Planet Formation • NGST will play an important role with its near- and mid-infrared capabilities by: – Determining the physics of star formation: the assembly of stars and proto-planetary disks from cloud cores – Imaging and doing atmospheric studies of Jupiter-sized planets at similar (5 AU) distances around nearby stars (50 candidates within 8 pc, needs a simple MIR Lyot stop) – Inventorying the prebiotic materials in starforming systems Science 21 Evolution of Planetary Systems Vega Disk Detection l (mm) Flux* Contrast (mJy) Star/Disk 11mm 2.4 1.5x107 22mm 400 2x104 33mm 1300 3x103 Reflected & emitted light detected with a simple coronograph. *per Airy disk NGST resolution at 24mm = 5 AU at Vega, > 10 pixels across the inner hole NGST & Extrasolar Planets From Angel & Woolf 1998, in Science with the NGST, ASP, 133, 172 108 Fn (mJy) • Control of primary only: – Jupiter at 10 < l < 20 mm • Active wavefront correction to 30 nm rms – Direct detection of Jupiter l > 0.4 mm “Sun” 106 “Solar System" at 8 pc, 6m primary 104 102 ldiff=1 mm 1 0.01 Jupiter 10s Earth 30nm 0.1 1 10 100 Wavelength (mm) 23 Summary • NGST gives advance in observing capabilities over HST comparable to the advance of HST • NGST can observe – Acceleration/deceleration of expanding universe – Cosmic dark matter – First luminous objects after Big Bang, even if much – – – – – – smaller than galaxies Protogalaxies merging into large galaxies First release of dust from first stars Deep into active galactic nuclei Individual stars in distant galaxies Interstellar gas and dust Recent formation of stars and planets 24