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

February 1, 2007 eSMA workshop, Leiden

Some thoughts about eSMA science

Ewine van DishoeckLeiden Observatory

Radiation at mm/submm wavelengths

Continuum: cold dust at 10-100 K; steep spectrum with 3-4

Lines: pure rotational transitions of molecules

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

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!

CO excitation Milky Way galaxies different from starbursts

Milky Way galaxy

Starburst nucleus

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

eSMA vs SMA

Go for fainter point/small sources Resolve/image bright sources

Larger samples?

Recall sensitivity Trms ~-2 => time ~4

Continuum: fainter sources

eSMAVLT

Herschel

BDDisk

Natta & Testi 2001

Brown dwarf disks

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

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.)

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

Chemical differentiation in Cep A East

resolution 0.”6

SMA 875 m VLA 3.6 cm

nprotostars = 8 x 105 pc-3

C. Brogan

1.5” 0.4” resolution at PdBDynamical age 1000 yr

Gueth et al. (in prep)

Unexpected results at subarcsec resolution

Objects that need subarcsec resolution

Image jets in cometary atmospheres

Minor planets/moons

Titan 0.8’’

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

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

Detached shells around AGB stars

Olofsson et al. 2000

TT Cyg

20’’

M. HogerheijdeEnvelope overwhelms disks except on longest baselines

: the problem of extended resolved emission

How and when do disks form?

Hueso & Guillot (2005)

Disk

Star

Even disks can show structure….

VLT VISIR image

8.6 PAH 11.3 PAH 19.8 m large grains

Geers et al. 2007

IRS48

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

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?

Possible interpretations

Grain growth:Planetesimals

Jupiter-type planets Supra Jupiter-type planets (5-10 MJ)

Photoevaporation Grain growth to large particles Jupiter-type planets

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

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

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)

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.

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

cTTs: turn-off < 2 m; excess ~ –1

wTTS: turn-off > 2 m; excess –3 to 1

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

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.

Class 0 protostellar outflows

SMA PROSACsurvey

Jørgensen et al,submitted

CO 3-2

Mapping evolutionary paths Evolutionary sequence: CTTs -> WTTs -> Debris

Cieza, Merin et al. 2006

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

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

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

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

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)

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

Workshop report

Introduction (Ewine, Michiel) Individual science topics (coordinators or

their designates) ~1 page/theme + 1-2 figures

Summary (Ewine, Michiel)

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?

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?

Thanks

Thanks to everyone who makes eSMA possible

Thanks to LOC