Frank H. ShuNational Tsing Hua University

Hsinchu, Taiwan15 June 2005

Bridge to Tomorrow• Mm and submm interferometer

s– Transition from blobology to re

solved structures– Warm dusty universe– Warm neutral (molecular) univ

erse• Largest radio investments by u

niversities and university consortia– Local control of research agen

da– 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

ProtogalaxiesArt Wolfe

Definition of Damped Lya System (DLA): N(HI) > 2*10**20 cm-2

Distinguishing characteristic of DLAs : Gas is Neutral

Bolocam Candidates—CSO

Pixel Sensitivity Histogram

Jackknife Histogram

17 GalaxyCandidates

324 square arcminutes(0.25 sq Jason Glenn. deg. survey of COSMOS underway)

= 1.1 mm

(Laurent et al., ApJ, 623, 742)

M82 from ISO, Beelen and Cox, in prep.

Galaxies at High Redshift

• 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

Christine Wilson

CO(7-6) and [CI] from NGC 4038/4039

[Spitzer Space Telescope, IRAC; NASA/JPL-Caltech/ Z. Wang (Harvard Smithsonian CfA)] (Isaak, in preparation)

• [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

T. Nikola

SPIFI at JCMT

Results• Arp 220 CO(6-5) Velocity Map

SMA CO(6-5)SMA CO(6-5)

Sakamoto et al. 1999Sakamoto et al. 1999

Satoki Matsushita

3C48

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)

1.2mm & 3.5mm continuum

3C48: Evidence for two merger nuclei? Melanie Krips

Sakamoto, Matsushita, Peck, Wiedner, & Iono 2004Sakamoto, Matsushita, Peck, Wiedner, & Iono 2004

fender benders

Jean Turner

fender benders

Jean Turner SMASMA

CO(3-2)CO(3-2)Off-center nucleus: Mdyn ~ 3 x 108 Mo within r=40 pcOff-center nucleus: Mdyn ~ 3 x 108 Mo within r=40 pc

CO(2-1)CO(2-1)

Double Rings and Central SpiralsChi Yuan

Sgr A* Polarization at 340 GHzI Q

VU

Dan Marrone

183 GHz 1015 kms-1 Feature 7- detection

Originates from nuclear region

Associated with disk/ outflow/ both ?

Mass arguments do not determine if thermal/maser

Linewidth arguments emission likely maser in origin

150 pc

CO

& 2

2 G

Hz

H2O

dis

k

rela

tivist

ic

outfl

ow

NGC 3079 – Liz Humphreys

= 22 GHz water maser position

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

GMCs in LMC – Yasuo Fukui

Thermal Emission + Extinction: Thermal Emission + Extinction: PerseusPerseus

Kirk, Johnstone, & Di Francesco (2005, in prep.)Kirk, Johnstone, & Di Francesco (2005, in prep.)

NGC 1333 IRAS4A - B vectors

•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

R. Rao

• time unit tg=1.9 Myrs

• sound speed Cs=0.2 km/s

• red plus=star 0.5 M each

• total mass 302 M

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%

Zhi-Yun Li

HCN (4-3) Velocity Structure

Extended Envelope with 2 Vel. Grad. + High-Velocity Compact Disk at A with Vel. Grad.

NW-SE Gradientin the Circumbi. Envaround the bin. axis

+NE-SW Gradientperpendicularly

NE-SW Gradient in the compact disk at A

Note: HCN avoids B..

(a) (b)

2.5 - 3.4 km s-1 3.6 - 5.8 km s-1

Low-Velocity

(c) (d)

-2.6 - +2.4 km s-1 6.0 - 9.1 km s-1

High-Velocity

a

outflow

b

~ Parallel to outflow---> Infall

Shigehasa Takukuwa

Spiral Structure and Episodic Accretion

Vorobyov & Basu (2005)

FU Ori events

integrated gravitational torque

Spiral arms create a strong centrifugal disbalance bursts of mass accretion; 0.01 to 0.05 solar masses are accreted.

Shantanu Basu

L1489 IRS: An infalling, rotating, psedodiskBr

inch

, Hog

erhe

ijde,

& J

oerg

ense

n (in

pre

p)Michiel Hogerheide

Cf. Allen, Li, & Shu (2003)

Luis Rodriguez

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

n=4

M=6

Hsien Shang

HCO+ (1-0) outflow emission: outflow chemical impact

Class 0

Class I

Class II

HH114mms RNO43

HH300 L1228 RNO129

TTAU

IRAS3282

Other HCO+ outflow studies:• Hogerheijde et al. 1998; 1999• Girart et al. 1999

Consistent with chemical models:• Rawlings et al. 2000; 2004• Viti et al. 2002

Hector Arce

The Mass Spectrum of the clumps

Motte et al. (1998) Williams et al. (2004)Johnstone et al. (2000)

Prestellar and protostellar dust clumps in Ophiuchi

High-mass protostellar clumps

0.5 MO

0.1 MO 3 MO

0.6 MO

2.4 - 6.3 MO

800 MO

100 MO

10 MO

Maite Beltran

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

Orion proplypids: bremsstrahlung + greybody (ionized gas + dust)

Submillimeter wavelengths essential to get the dust

Average mass~ 8x10-4 M

18 nondetections

This size distribution gives opacity varying approximately as 1 in submm, once grain growth reaches amax > 1mm.

(submm) amax-0.5

Bruce Draine

Blue: Canonical Model (Calvet et al. 2002, Qi et al. 2004 )Black: SMA dataRed: Model with X ray heating

CO 2-1 CO 3-2 Chunhua Qi

CO 6-5

If depletion is extensive, what species might be able to probe the disk midplane? One possible route involves deuterated ions such as H2D+:

The abundances of these ions may be difficult to quantify, however, and so SOFIA/Herschel studies of HD J=1-0 at 112 m are eagerly awaited!

Are there gas probes of the disk midplane? Geoff Blake

Ceccarelli et al. 2004, ApJ 607, L51

TW Hya

vLSR (km/s)

TMB (K)

Van Dishoeck et al. 2003, A&A 400, L1

Ring Rotation in Epsilon Eridani

• Debris disk: proper motion plus rotation leads to characteristic shifts

– tentative!!!!

• but systematic, ~2’’ counter-clockwise

– if ok, planet at ~40 AU

Jane Greaves

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 Structures of the gaseous disk seems to be very different from those around other Herbig Ae/T Tauri stars.from those around other Herbig Ae/T Tauri stars.

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Driven Spiral Density and Bending Waves in Saturn’s Rings

Shu, Cuzzi, & Lissauer (1983)

Implications for planet migration due to planet-disk interaction

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)

Glenn Orton

Pluto & Charon Resolved!

08h-16h 21 May 2005

Mark Gurwell

Detached shell: Vexp ~ 15 km/s

Present day wind: Vexp ~ 10 km/s

Dynamical age ~ 1700 yr

Helium flash ?

CO J=21

Protoplanetary nebula: Dinh Van Trung

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.

Thanks to the Organizers• 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

Poster Paper Prizes