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Frank H. Shu National Tsing Hua University Hsinchu, Taiwan 15 June 2005

Frank H. Shu National Tsing Hua University Hsinchu, Taiwan 15 June 2005. Bridge to Tomorrow. Mm and submm interferometers Transition from blobology to resolved structures Warm dusty universe Warm neutral (molecular) universe

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Frank H. Shu National Tsing Hua University Hsinchu, Taiwan 15 June 2005

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  1. Frank H. Shu National Tsing Hua University Hsinchu, Taiwan 15 June 2005

  2. Bridge to Tomorrow • Mm and submm interferometers • Transition from blobology to resolved structures • Warm dusty universe • Warm neutral (molecular) universe • Largest radio investments by universities and university consortia • Local control of research agenda • Training of generation of radio interferometrists • Next step: ALMA • Billion dollar investment – Large international consortium • Drawbacks of big science? • Story: structure and evolution of complex objects

  3. Protogalaxies Art Wolfe Definition of Damped Lya System (DLA): N(HI) > 2*10**20 cm-2 Distinguishing characteristic of DLAs : Gas is Neutral

  4. Bolocam Candidates—CSO 324 square arcminutes (0.25 sq Jason Glenn. deg. survey of COSMOS underway) Pixel Sensitivity Histogram 17 Galaxy Candidates Jackknife Histogram  = 1.1 mm (Laurent et al., ApJ, 623, 742)

  5. Galaxies at High Redshift Christine Wilson • For distant galaxies, dimming due to distance is offset by the brighter part of the spectrum redshifting into an ALMA band • Result is galaxies have relatively similar brightness out to large distances M82 from ISO, Beelen and Cox, in prep.

  6. CO(7-6) and [CI] from NGC 4038/4039 T. Nikola • [CI] Line intensity essentially constant • CO(7  6) greatly enhanced at the starburst interaction zone reflecting the high gas excitation there • Strong mid-J CO emission reflects influence of OB stars SPIFI at JCMT [Spitzer Space Telescope, IRAC; NASA/JPL-Caltech/ Z. Wang (Harvard Smithsonian CfA)] (Isaak, in preparation)

  7. Results Satoki Matsushita • Arp 220 CO(6-5) Velocity Map SMA CO(6-5) Sakamoto et al. 1999

  8. 3C48 3C48: Evidence for two merger nuclei? Melanie Krips 1.2mm & 3.5mm continuum • New IRAM PdBI Observations (~1-2"):(Krips et al., accept. at A&A) • continumm: 3.5 & 1.2mm • line: 12CO(1-0) • (merged with Wink et al. 1997)

  9. fender bendersJean Turner SMA CO(2-1) Sakamoto, Matsushita, Peck, Wiedner, & Iono 2004 CO(3-2) Off-center nucleus: Mdyn ~ 3 x 108 Mo within r=40 pc

  10. Double Rings and Central Spirals Chi Yuan

  11. Sgr A* Polarization at 340 GHz Q Dan Marrone I U V

  12. 183 GHz 1015 kms-1 Feature NGC 3079 – Liz Humphreys 7- detection Originates from nuclear region Associated with disk/ outflow/ both ? Mass arguments donot determine if thermal/maser Linewidth arguments  emission likely maser in origin CO & 22 GHz H2O disk 150 pc relativistic outflow = 22 GHz water maser position

  13. GMCs in LMC – Yasuo Fukui CO distribution 259 CO clouds (Mvir > 104 Msun) Total molecular mass ~ 7×107 Msun Total ~ 27,000 points Contours; from 1.2Kkm/s intervals 2.4Kkm/s

  14. Thermal Emission + Extinction: Perseus Kirk, Johnstone, & Di Francesco (2005, in prep.)

  15. NGC 1333 IRAS4A - B vectors R. Rao • Polarization hole • Polarization peak is offset • Hour glass shape of the magnetic field structure in the circumbinary envelope • The large scale field is well aligned with the minor axis • We will need some higher angular resolution observations to map the structure of the field between the two cores

  16. Zhi-Yun Li • time unit • tg=1.9Myrs • sound speed • Cs=0.2km/s • redplus=star • 0.5Meach • total mass • 302M 3.7pc star formation efficiency (SFE) = mass of stars/total mass of cloud e.g., SFE at t=2.0 tg or 3.8 Myrs: 15 x 0.5/302 = 2.5%

  17. HCN (4-3) Velocity Structure + NE-SW Gradient perpendicularly Shigehasa Takukuwa NW-SE Gradient in the Circumbi. Env around the bin. axis NE-SW Gradient in the compact disk at A ~ Parallel to outflow ---> Infall Note: HCN avoids B.. Extended Envelope with 2 Vel. Grad. + High-Velocity Compact Disk at A with Vel. Grad.

  18. Shantanu Basu Spiral Structure and Episodic Accretion FU Ori events Spiral arms create a strong centrifugal disbalance  bursts of mass accretion; 0.01 to 0.05 solar masses are accreted. Vorobyov & Basu (2005)

  19. L1489 IRS: An infalling, rotating, psedodisk Michiel Hogerheide Brinch, Hogerheijde, & Joergensen (in prep) Cf. Allen, Li, & Shu (2003)

  20. Luis Rodriguez

  21. Chin-Fei Lee 12CO J=2-1(Contours) + H2 (Image)

  22. n=4 M=6 Hsien Shang

  23. HCO+ (1-0) outflow emission: outflow chemical impact HH114mms RNO43 IRAS3282 Hector Arce Class 0 HH300 L1228 RNO129 Class I Other HCO+ outflow studies: • Hogerheijde et al. 1998; 1999 • Girart et al. 1999 TTAU Class II Consistent with chemical models: • Rawlings et al. 2000; 2004 • Viti et al. 2002

  24. 100MO 0.5 MO 0.6MO 0.1 MO 10MO 3 MO 2.4 - 6.3MO The Mass Spectrum of the clumps Maite Beltran Prestellar and protostellar dust clumps in r Ophiuchi High-mass protostellar clumps 800MO Johnstone et al. (2000) Williams et al. (2004) Motte et al. (1998)

  25. Summary Crystal Brogan For the first time the SMA allows submm study of HMPOs in exquisite detail • Multiplicity within HMPOs * Both W33A (4 kpc) and CepA-E (0.7 kpc) composed multiple components * G12.89-0.49 (3.6 kpc) strongest component compact • Role and characteristics of HMPO jets and disks * Complex velocity gradients -> disks * Self-absorption complicates interpretation • Evolutionary sequence * Some evidence for evolution • Density and temperature profiles * Rotation diagrams support temperature profile models for W33A -> see Wootten et al. poster

  26. Average mass ~ 8x10-4 M Submillimeter wavelengths essential to get the dust Orion proplypids: bremsstrahlung + greybody (ionized gas + dust) 18 nondetections

  27. Bruce Draine This size distribution gives opacity varying approximately as 1 in submm, once grain growth reaches amax > 1mm. (submm)  amax-0.5

  28. CO 2-1 CO 3-2 Chunhua Qi CO 6-5 Blue: Canonical Model (Calvet et al. 2002, Qi et al. 2004 ) Black: SMA data Red: Model with X ray heating

  29. Are there gas probes of the disk midplane?Geoff Blake If depletion is extensive, what species might be able to probe the disk midplane? One possible route involves deuterated ions such as H2D+: Ceccarelli et al. 2004, ApJ 607, L51 The abundances of these ions may be difficult to quantify, however, and so SOFIA/Herschel studies of HD J=1-0 at 112 mm are eagerly awaited! Van Dishoeck et al. 2003, A&A 400, L1 TW Hya TMB (K) vLSR (km/s)

  30. Ring Rotation in Epsilon Eridani Jane Greaves • Debris disk: proper motion plus rotation leads to characteristic shifts • tentative!!!! • but systematic, ~2’’ counter-clockwise • if ok, planet at ~40 AU

  31. SMA Results on HAeBe: 12CO (3-2) Nagayoshi Ohashi • An elongated disk structure, consistent with other observations. • Overall dimension: ~530  330 AU • Two peaks; one at the stellar position, and the other at the most prominent spiral arm. • A part of the 12CO 3-2 emission seems to trace the spiral arm. • PdBI 12CO 2-1 map shows only one peak at the stellar position. • Additional extended structures. Structures of the gaseous disk seems to be very different from those around other Herbig Ae/T Tauri stars.

  32. Driven Spiral Density and Bending Waves in Saturn’s Rings Shu, Cuzzi, & Lissauer (1983) Implications for planet migration due to planet-disk interaction

  33. Glenn Orton Atmosphere of Saturn • CH4/H2 = 4.3± 1.0 x 10-3(for 88.1% H2) • C/H is 6 ± 2 times solar abundance • This is consistent with an accreting core of 10-12 MEarth (Mizuno 1980; Owen & Encrenaz 2003, 2005)

  34. Pluto & Charon Resolved! Mark Gurwell 08h-16h 21 May 2005

  35. Protoplanetary nebula: Dinh Van Trung CO J=21 Detached shell: Vexp ~ 15 km/s Present day wind: Vexp ~ 10 km/s Helium flash ? Dynamical age ~ 1700 yr

  36. Valentin Bujarrabal • At the end, aged sunlike stars behave as they did as babies, driving collimated outflows. • Possible mechanism: Rapid rotation + magnetic field. • Inverse angular momentum problem. • Story has come full circle.

  37. SOC Paul Ho (Chair) Pierre Cox Masato Ishiguro Jeremy Lim Fred Lo Jim Moran Tom Phillips Anneila Sargent Juergen Stutzki David Wilner Christine Wilson LOC Qizhou Zhang (Chair) Jennifer Barnett Henrik Beuther Maria Montero-Castano Ramiro Franco-Hernandez Mark Gurwell Muriel Hodges Chin-Fei Lee Nimesh Patel Chunhua Qi Catherine Shifferin Margaret Simonini Jeff Wagg Yang Wang Luis Zapata Thanks to the Organizers

  38. Poster Paper Prizes

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