frank h. shu national tsing hua university hsinchu, taiwan 15 june 2005
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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