Transcript Submillimeter Astronomy In the Era of the SMA

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
• 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
Protogalaxies
Art Wolfe
Definition of Damped Lya System (DLA): N(HI) > 2*10**20 cm-2
Distinguishing characteristic of DLAs : Gas is Neutral
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)
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.
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
SPIFI at JCMT
[Spitzer Space Telescope, IRAC; NASA/JPLCaltech/ Z. Wang (Harvard Smithsonian CfA)]
• Strong mid-J CO
emission reflects
influence of OB stars
(Isaak, in preparation)
Results
Satoki Matsushita
• Arp 220 CO(6-5) Velocity Map
SMA CO(6-5)
Sakamoto et al. 1999
3C48: Evidence for two merger nuclei?
1.2mm & 3.5mm continuum
3C48
Melanie Krips
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)
fender benders
Jean Turner
SMA
CO(2-1)
Sakamoto, Matsushita, Peck, Wiedner, & Iono 2004
Off-center nucleus: Mdyn ~ 3 x 108 Mo within r=40 pc
CO(3-2)
Double Rings and Central Spirals
Chi Yuan
Sgr A* Polarization at 340 GHz
I
Q
U
V
Dan Marrone
183 GHz 1015 kms-1 Feature
NGC 3079 – Liz Humphreys
150 pc
7- detection
Originates from
nuclear region
Associated with
disk/ outflow/
both ?
Mass arguments
do not determine
if thermal/maser
= 22 GHz water maser position
Linewidth
arguments 
emission likely
maser in origin
GMCs in LMC – Yasuo Fukui
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
Thermal Emission + Extinction: Perseus
Kirk, Johnstone, & Di Francesco (2005, in prep.)
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
Zhi-Yun Li
3.7pc
• time unit
tg=1.9 Myrs
• sound speed
Cs=0.2 km/s
• red plus=star
0.5 M each
• total mass
302 M
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%
HCN (4-3) Velocity Structure
L o w - V e lo c it y
( a)
2 . 5 - 3 . 4 k m s- 1
Hig h - V e lo c it y
Shigehasa Takukuwa
(b )
NW-SE Gradient
in the Circumbi. Env
around the bin. axis
+
NE-SW Gradient
perpendicularly
( d)
NE-SW Gradient in
the compact disk at A
~ Parallel to outflow
---> Infall
3 . 6 - 5 . 8 k m s -1
(c)
a
o u t f lo w
b
-2 .6 - + 2 .4 km s - 1
6 . 0 - 9 . 1 km s -1
Note: HCN avoids B..
Extended Envelope with 2 Vel. Grad. + High-Velocity Compact Disk at A with Vel. Grad.
Spiral Structure and Episodic Accretion
Shantanu Basu
FU Ori events
Spiral arms create a strong centrifugal
disbalance  bursts of mass accretion;
0.01 to 0.05 solar masses are accreted.
  integrated gravitational torque
Vorobyov & Basu (2005)
L1489 IRS: An infalling, rotating, psedodisk
Brinch, Hogerheijde, & Joergensen (in prep)
Michiel Hogerheide
Cf. Allen, Li, & Shu (2003)
Luis Rodriguez
Chin-Fei Lee
12CO
J=2-1(Contours) + H2 (Image)
sien Shang
n=4
M=6
HCO+ (1-0) outflow emission:
outflow chemical impact
HH114mms
RNO43
IRAS3282
Hector Arce
Class 0
HH300
L1228
RNO129
Class I
TTAU
Class II
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
The Mass Spectrum of the clumps
Maite Beltran
Prestellar and protostellar
dust clumps in r Ophiuchi
High-mass
protostellar clumps
100 MO
0.5 MO
0.6 MO
800 MO
0.1 MO
Motte et al. (1998)
3 MO
Johnstone et al. (2000)
2.4 - 6.3
MO
10 MO
Williams et al. (2004)
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)
Average mas
~ 8x10-4 M
18
nondetections
Submillimeter wavelengths essential to get the dust
Bruce Draine
This size distribution gives
opacity varying
approximately as 1 in
submm, once grain growth
reaches amax > 1mm.
(submm)  amax-0.5
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
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+:
Van Dishoeck et al. 2003, A&A 400, L1
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!
Ceccarelli et al. 2004,
ApJ 607, L51
TW Hya
TMB (K)
vLSR (km/s)
Ring Rotation in Epsilon Eridani
• Debris disk: proper motion
plus rotation leads to
characteristic shifts
– tentative!!!!
• but systematic, ~2’’ counterclockwise
– 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
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• 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.
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
Glenn Orton
•
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)
Pluto & Charon Resolved!
Mark Gurwell
08h-16h 21 May 2005
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
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
•
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Pierre Cox
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•
LOC
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Jennifer Barnett
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Ramiro Franco-Hernandez
Mark Gurwell
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Chin-Fei Lee
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Chunhua Qi
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Poster Paper Prizes