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Whither UVO Space Science?

Whither UVO Space Science?. HST. John Huchra, Center for Astrophysics. What have we learned?. (Highpoints from HST ++) Planetary Science Stellar Astrophysics ISM + IGM Stellar Populations Galaxies & their Evolution Cosmology

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Whither UVO Space Science?

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  1. Whither UVO Space Science? HST John Huchra, Center for Astrophysics

  2. What have we learned? (Highpoints from HST ++) Planetary Science Stellar Astrophysics ISM + IGM Stellar Populations Galaxies & their Evolution Cosmology --- ask not what you can do for HST but what HST has done for you ---

  3. Jupiter Aurora in the UV

  4. PlanetaryTransits Transit of Venus 1882 USNO

  5. HST Transit HD 209458 Brown et al.

  6. Deuterium in the UV or“Better Astronomy through Chemistry”

  7. Truran

  8. Eta Carinae Treasury ProgramR~109,000 & 0.03” Spatial Wind Structure Eta Carinae 0.3” -146 km/s (Little Homunculus) -513 Component (Homunculus) Weigelt C (emission) Ted Gull

  9. Propylids

  10. High Velocity Clouds

  11. Rich et al. 2004 Stellar Populations in Andromeda

  12. The Power of Comparison

  13. AM0644-741

  14. NGC5548UVabsorptionfeatures

  15. HubbleUltraDeepField(2004)

  16. Hubble UDF

  17. Galaxy Size versus Redshift Half Light Radius Ferguson et al 2004 HST H**-1(z) H**-2/3(z) No evolution

  18. SFR versus z

  19. Strong & Weak Lensing Omega matter ~ 0.25

  20. HST H0 Key Project

  21. Ho =72+/-7 km/s/Mpc

  22. ESSENCE + ACS 2004 Riess et al. + Tonry et al 2004

  23. JT’s note: Systematics will get you! TABLE 1. FLUX DATA FOR VEGA WAVE MAG LOG FNU FNU FLAM LOG MAG DELTA 2900. 1.140 -19.912 1.225D-20 4.364D-09 -8.360 0.460 3300. 1.137 -19.911 1.228D-20 3.379D-09 -8.471 0.738 0.03 3350. 1.145 -19.914 1.219D-20 3.255D-09 -8.487 0.779 3400. 1.129 -19.908 1.237D-20 3.207D-09 -8.494 0.795 0.06 3450. 1.115 -19.902 1.253D-20 3.155D-09 -8.501 0.812 3500. 1.097 -19.895 1.274D-20 3.117D-09 -8.506 0.826 0.04 3571. 1.077 -19.887 1.298D-20 3.050D-09 -8.516 0.849 3600. 1.070 -19.884 1.306D-20 3.020D-09 -8.520 0.860 0.03 3636. 1.059 -19.880 1.319D-20 2.991D-09 -8.524 0.871 3680. 1.050 -19.876 1.330D-20 2.944D-09 -8.531 0.888 0.03 3704. 1.040 -19.872 1.343D-20 2.933D-09 -8.533 0.892 3730. 0.700 -19.736 1.837D-20 3.956D-09 -8.403 0.567 3835. 0.400 -19.616 2.421D-20 4.933D-09 -8.307 0.327 3940. 0.100 -19.496 3.192D-20 6.161D-09 -8.210 0.086 4036. -0.299 -19.336 4.609D-20 8.479D-09 -8.072 -0.261 -0.016 4167. -0.278 -19.345 4.521D-20 7.802D-09 -8.108 -0.170 -0.015 4255. -0.263 -19.351 4.459D-20 7.380D-09 -8.132 -0.110 -0.013 4460. -0.238 -19.361 4.357D-20 6.564D-09 -8.183 0.017 -0.032 4464. -0.238 -19.361 4.357D-20 6.552D-09 -8.184 0.019 -0.023 4566. -0.199 -19.376 4.203D-20 6.042D-09 -8.219 0.107 -0.014 4780. -0.153 -19.395 4.029D-20 5.284D-09 -8.277 0.253 -0.012 4785. -0.153 -19.395 4.029D-20 5.273D-09 -8.278 0.255 -0.012 5000. -0.103 -19.415 3.848D-20 4.612D-09 -8.336 0.400 -0.002 5263. -0.050 -19.436 3.664D-20 3.964D-09 -8.402 0.565 -0.011 5556. 0.000 -19.456 3.499D-20 3.397D-09 -8.469 0.732 -0.025 5840. 0.062 -19.481 3.305D-20 2.904D-09 -8.537 0.902 -0.017 6056. 0.111 -19.500 3.159D-20 2.581D-09 -8.588 1.030 6370. 0.160 -19.520 3.020D-20 2.230D-09 -8.652 1.189 -0.030 6436. 0.167 -19.523 3.001D-20 2.171D-09 -8.663 1.218 6790. 0.217 -19.543 2.866D-20 1.863D-09 -8.730 1.385 6800. 0.219 -19.544 2.860D-20 1.854D-09 -8.732 1.390 -0.05 7100. 0.272 -19.565 2.724D-20 1.619D-09 -8.791 1.537 7550. 0.361 -19.600 2.510D-20 1.319D-09 -8.880 1.759 • Calibration uncertainty Gotta Fly a BB!

  24. HST in the next years An Economist’s (my wife) view: Optimization Subject to Constraints: Pointing (Gyro Life) Archival Optimization (Legacy/Treasury) Science Optimization (Kolmogorov Spec) UV Spectroscopy High Spatial Resolution Low Background

  25. Short Term Options for HST: • Chaos and Anarchy (a.k.a. the normal TAC process) • Assessment of Major Science • More Optimization JPH’s advice to young astronomers: “always assume **this** is your last clear night on the telescope”

  26. Key Project Process Decide that a fraction of time is to be set aside for that which you’d be embarrassed not to have done. Assemble community input and advice Select areas of research deserving such special attention Solicit proposals for same as part of the normal process. Encourage teaming. ---- Optimize the science! Use as much info as possible to help make the decision.

  27. What happens after Hubble? • We still need • UV Spectroscopy • UVO Imaging, • and the Atmosphere is not our friend.

  28. Drivers The density of astrophysically interesting features in the UV is extremely high. Some elements can only be measured < 3000A. Spatial resolution is inversely proportional to wavelength. An 8-m at 1600A is the same as an 80-m at 1.6 microns. HST in the UV beats JWST (and AO) in the near IR. The background sky in space is, at a minimum, 10 times less than on the ground.

  29. Absorption Line List for Galaxies & AGN Lambda Ion Lambda Ion Lambda Ion 933.38 SVI 1128.01 PV 1393.76 Si IV 944.52 SVI 1144.94 FeII 1402.77 Si IV 963.99 NI 1175.70 CIII 1486.50 N IV 977.02 CIII 1190.42 SiII 1549.05 C IV 990.79 NIII 1193.29 SiII 1640.50 He II 1020.70 SiII 1199.9 NI 2798. Mg II 1031.93 OVI 1206.50 SiIII 2804. Mg II 1037.62 OVI 1215.67 Ly a 2947.7 Fe I 1048.22 ArI 1240.15 N V 2994.4 Fe I 1062.67 SIV 1260. S II 3020.7 Fe I 1073.28 SIV 1263. Si II 3047.6 Fe I 1083.99 NII 1304.35 O I 3100.0 Fe I 1117.98 PV 1335.30 C II 3143.8 Ti II

  30. Science. And there are many **BIG** unanswered questions --- What is the real distribution of baryons? What is Dark Matter? How did the chemical elements form? Can we explain the differences in their distribution and their evolution with time? What’s in the outer Solar system? What drives BH formation and evolution (both big and small)? Do we have the right cosmological model/params? How do galaxies really evolve? What’s the weather on Neptune? What’s the cause of multiple SF epochs in nearby galaxies? ……. ETC ….

  31. The Cosmic Web 80% of the Baryons in the Universe appear to be in the IGM. The only way to trace them is spectroscopically For z < 1.7, we ***require*** the vacuum UV. L. Hernquist

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