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TRANSCRIPT
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Organizational issues
Start in 226/228, move up to 427 at lunch Wireless connection on floor 4 + 5, especially Oort
building User: guest6, passwd: work#shop2007 Lunch in HL 427, sandwiches Travel support: see Kirsten Groen during lunch Dinner tonight at Anak Bandung
10 Euro/per person: pay Sandrine Need headcount by coffee break Taxi’s at 6:30 pm from lab => restaurant
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February 1, 2007 eSMA workshop, Leiden
Some thoughts about eSMA science
Ewine van DishoeckLeiden Observatory
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Radiation at mm/submm wavelengths
Continuum: cold dust at 10-100 K; steep spectrum with 3-4
Lines: pure rotational transitions of molecules
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Different lines probe different conditions
ncrit~23
Higher frequencytransitions probe higherdensities and temperatures
CO principle tracerof H2 gas
Cold tenuous gas vs warm dense gas
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eSMA vs other facilities
Higher frequency Stronger dust emission: factor 3.5-5 gain at
345 GHz vs 230 GHz Higher excitation lines: warmer or denser
gas => qualitatively different
Higher (or comparable) spatial resolution Higher (or comparable) sensitivity
Programs need to exploit these unique eSMA strengths!
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CO excitation Milky Way galaxies different from starbursts
Milky Way galaxy
Starburst nucleus
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Nearby Galaxy: NGC6090
HST: Dinshaw et a. 1999HST: Dinshaw et a. 1999 SMA: J. WangSMA: J. Wang
CO 2-1CO 2-1
CO 3-2CO 3-2
Note: CO 3-2 qualitatively different from 2-1
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eSMA vs SMA
Go for fainter point/small sources Resolve/image bright sources
Larger samples?
Recall sensitivity Trms ~-2 => time ~4
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Continuum: fainter sources
eSMAVLT
Herschel
BDDisk
Natta & Testi 2001
Brown dwarf disks
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Blobs in large beams break up in individual sources
MIPS-24 image.
9 objects within 90” (0.1 pc).
Rebull et al. 2007
IRAS beam
Example IRAS => Spitzer
Stellar aggregate in Perseus
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High-mass star formation
Image Credit: Cormac Purcell
Observed as cold, dense cores• Infrared-dark clouds •“mm-only” cores
•Hyper-compact HII regions (eg Kurtz et al. 2005)•Ultra-compact HII regions - well studied (see Churchwell and co.)
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Orion-KL: 690 GHz spectra SMA
Beuther et al. in prepBlake et al. 1987, Ohishi et al. 1995, Wright et al. 1996,Schilke et al. 1997, 2001,White et al. 2003, Comito et al. 2005, ….
Hot cores: complex chemistry
G327 with APEX
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Chemical differentiation in Cep A East
resolution 0.”6
SMA 875 m VLA 3.6 cm
nprotostars = 8 x 105 pc-3
C. Brogan
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1.5” 0.4” resolution at PdBDynamical age 1000 yr
Gueth et al. (in prep)
Unexpected results at subarcsec resolution
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Objects that need subarcsec resolution
Image jets in cometary atmospheres
Minor planets/moons
Titan 0.8’’
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High-redshift galaxies CO at z=6.4
VLA
- Need high spatial resolution to image CO and dust at high-z: typical sizes 0.2-0.3’’ - Need intererometry to pinpoint sources for comparison with IR and optical data
Walter et al. 2004VLA and IRAM PdB
Walter et al. 2003
CO 3-2 map, SDSS J1148+5251
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Starting to study them…
CO 3-2 at z=2.80 CO rotation curve
Genzel et al. 2003SMM J020399-0136
M>4x1011 Msun within 8 kpc => challenge for standardhierarchical galaxy merger scenarios
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Detached shells around AGB stars
Olofsson et al. 2000
TT Cyg
20’’
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M. HogerheijdeEnvelope overwhelms disks except on longest baselines
: the problem of extended resolved emission
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How and when do disks form?
Hueso & Guillot (2005)
Disk
Star
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Even disks can show structure….
VLT VISIR image
8.6 PAH 11.3 PAH 19.8 m large grains
Geers et al. 2007
IRS48
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Scenario for star- and planet formation
Cloud collapse Protostar with disk
infall
outflow
Formation planets Solar system
Factor 1000 smaller
Fig. by McCaughrean
t=0 t=105 yr
t=106-107 yr t>108 yr
Single isolated low-mass star
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Class III
Disk evolutionThere are multiple paths from massive gas-rich disks to tenuous debris disks
Class II Star
Disk
Class II
Class II
Merin et al. in prep
Grain growth?
Gap opening?
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Possible interpretations
Grain growth:Planetesimals
Jupiter-type planets Supra Jupiter-type planets (5-10 MJ)
Photoevaporation Grain growth to large particles Jupiter-type planets
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Gas in holes in transitional disks?
Augereau, Dutrey et al. 2004, in prep
IRAM PdB12CO 2-1
Superposed onHST-STIS
Massive gas-rich disk
Debris disk
HD141569
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Large fraction of T Tauri disks shows evidence for grain growth
Models
Data
Kessler-Silacci et al. 2006
10 m band 20 m band
Obs
Model
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Cold Disks can be modeled with very large gaps
Model outer radii of dust gap are >20 AUAt least 3 out of 4 have gas inside 1 AU (from CO IR lines)
Brown, et al. (in prep)
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More cold disks in c2d sample
Cycle 3 IRS Follow up of c2d candidates Merin et al. (in prep)
We have found 30 objects with signs of having inner holes in their disks in the c2d mapped clouds (few % of disks => fast or rare?)
Enlarge the sample of cold disks by a factor of 3.
Large range in stellar parameters, hole sizes, dust mass in the hole, dust composition, and presence of gas.
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Even More Extreme: Cold DisksEven More Extreme: Cold Disks
Onset of excess beyond 10 microns, but strong excessAll 4 cold disks show PAH featuresAt least 3 out of 4 have gas inside 1 AU (from CO IR lines)
Brown,Merin et al.in prep
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cTTs: turn-off < 2 m; excess ~ –1
wTTS: turn-off > 2 m; excess –3 to 1
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SMA 850 µm
Young disks: NGC1333-IRAS2A Class 0 protostar SMA resolves the dust in the inner envelope and the circumstellar disk
Envelope (constrained through SCUBA observations; Jørgensen et al. 2002)
Disk (resolved)
Jørgensen et al. 2005Keene & Masson 1991Looney et al. 2000, Harvey et al. 2003
850 m
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More cold disks in c2d sample
Cycle 3 IRS Follow up of c2d candidates Merin et al. (in prep)
We have found 30 objects with signs of having inner holes in their disks in the c2d mapped clouds (few % of disks => fast or rare?)
Enlarge the sample of cold disks by a factor of 3.
Large range in stellar parameters, hole sizes, dust mass in the hole, dust composition, and presence of gas.
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Class 0 protostellar outflows
SMA PROSACsurvey
Jørgensen et al,submitted
CO 3-2
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Mapping evolutionary paths Evolutionary sequence: CTTs -> WTTs -> Debris
Cieza, Merin et al. 2006
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Dust holes in proto-planetary disks
Beam: 0.39 x 0.25 PA230
GM Aur (Wilner et al. 2006): SMA, PdBLkCa15 (Piétu et al. 2006): PdB
Beam: 0.52 x 0.28 PA 220
Inner cavity of 50 AU
See also Strom et al. 1989 Skrutski et al. 1990
Do gas and dust disappear at the same time?
Search for CO inside dust hole/gap
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Summary
Solar system CO in Pluto TOO bright comet, e.g. HNC Io, Titan: TBC, is eSMA needed, science cases needed
Disk evolution Embedded disks: Class 0 + I
Continuum O.K., but lines? Also compact outflows? Classical disks: do TW Hya really well Transitional disks Brown dwarf disks: not now, get SMA first
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Summary (cont’d)
High-mass SFR IMF and multiplicity
CH3OH + dust setting W33A, W3IRS5, NGC6334 I(N), IRAS19410, AGL490
Disks/inner 1000 AU Circumstellar motions HCN and CH3OH settings AFGL 2591, IRAS20126, G10.6, G24, G31/34,IRAS18566
Pre-stellar phases N2H+/H2D+/HNCH2CO setting HIFI/TH/TK settings, e.g. 18223-3, G11.11, G28.28
Magnetic fields: TBC AGB stars
Dust tori: masses Gas kinematics: CO 3-2/13CO 3-2 Magnetic fields: later, but put in summary report
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Summary (cont’d)
Nearby galaxies Starburst/AGN separation
Followup SMA legacy project Targets Mrk231,UGC5101,NGC6240, possibly Mrk273,I10565
Warm dense gas in galaxies with AGN/starburst HCN 4-3 in Arp 220, NGC6240 (possibly)
ULIRGs: do a few of brightest galaxies well in various tracers High-z galaxies
Structure + size of representative SMGs as test of galaxy formation mechanisms Those with matched radio data from MERLIN
Explore FIR/radio correlation on kpc scale at z=2-3 Lensed examples of faint SMGs
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Summary (cont’d) Nearby galaxies
Starburst/AGN separation Followup SMA legacy project Targets Mrk231,UGC5101,NGC6240, possibly Mrk273,I10565
Warm dense gas in galaxies with AGN/starburst HCN 4-3 in Arp 220, NGC6240 (possibly)
Excitation dense vs tenuous gas in nearby galaxies CO and HCN simultaneously NGC 253, NGC1365, IC342, possibly M83, Maffei2
Differentiating Seyferts and starbursts in nearby galaxies Mostly CO, HCN in feasible (e.g. NGC1068)
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Goal of this workshop
Make community aware that eSMA is coming Start thinking about unique eSMA project
Learned a lot! Killer applications Longer term coherent projects
Provide opportunity for community to start organizing itself around various science themes Not exhaustive in terms of themes
Provide summary of workshop to Boards/Directors about eSMA scientific potential in coming years
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Workshop report
Introduction (Ewine, Michiel) Individual science topics (coordinators or
their designates) ~1 page/theme + 1-2 figures
Summary (Ewine, Michiel)
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Workshop report schedule
First draft of science themes Feb. 25 First complete draft to workshop
participants March 20 Comments April 5 Potentially one more iteration with
coordinators Submit late April How to publicize to community?
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Advice on time allocation call + process?
Encourage collaborative projects Encourage coherent projects? Substantial fraction of TAC members should
have interferometry experience Initial call will be for projects to fit in the 42
nights of pilot program Exploratory/killer aps Limit on max number of tracks per project to get
diversity?
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Thanks
Thanks to everyone who makes eSMA possible
Thanks to LOC