Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.atnf.csiro.au/whats_on/workshops/mm_science2001/talks/Blake.pdf Дата изменения: Tue Apr 23 11:34:11 2002 Дата индексирования: Wed Dec 26 08:10:13 2007 Кодировка: Поисковые слова: dust disk

Millimetre Science with the AT
Astrochemistry with mm-Wave Arrays G.A. Blake, Caltech
29Nov 2001


mm-Arrays: Important Features

- Spatial Filtering - Transform to image plane - Cross Correlation


(Sub)Millimeter Astrophysics
- Thermal emission from cool dust, gas - High frequency non- thermal tail - Uniquely high spectral resolution possible Orion KL, CSO


Late Type Stars and mm -Arrays
IRC+10216 Plateau de Bure (6 15 m's)

2 µ m AO image


Young Stars & Arrays
What size ranges are present?


Absorption Spectroscopy w/mm-Arrays
IRAM 30m Oph

PKS1830 High z features

Arrays filter out extended cloud!


SIRTF
- IRAC (mid - IR cameras, 3.6 4.5, 5.8, 8.0 µ m) - MIPS (far- IR cameras, 24, 70 160 µ m, R=20 SED mode) - IRS (5-40 µ m long slit,R=150, 10-38 µ m echelle , R=600) 01 Dec 2002 launch

- GTO observations - Legacy program - General observations


SIRTF ­ Mapping Large Clouds

Evans et al. Legacy Team Perseus , Cha, Lupus, Oph, Serpens + Isolated cores


Large Scale Structure? Single dish or...
Ideally, single dish should be ~twice array dish diameter for good (u,v) overlap... Use Mopra to start, good single dish pointing essential. SEST 15m
M ax- Planck- Institut f Эr Radioastronomie European S outhern Observatory Onsala Space Observatory

Atacama Pathfinder EXperiment


Heterogeneous Arrays:
CARMA = BIMA + OVRO + SZ Array (8 3.5m telescopes) SUP submitted Juniper 2002 road Flat 2003 move OVRO 2004 move BIMA 2005 full operations


Chemistry and Massive Stars:
- Embedded at main sequence
- Large area heated, shocked - Extensive chemistry


Orion as a Hot Core Test Case:
Bright lines, complex spatial structure!


The Dynamic Envelopes Around YSOs
- Dust + Gas = n(R),T(R),f(R) - Polarization (B field support)?


The Dynamic Envelopes Around YSOs. II


Complementary IR Envelope/Disk Studies
CO M-band, infall to ~0.1 AU in L1489.
NIRSPEC R=25000

Keck

VLT


Molecules in the Outflows from Young Stars
mm- arrays can be used to study all outflow phases, even those that are highly extincted. Velocity resolution critical!


Chemistry in YSO Accretion Disks. I
- Line shapes constrain disk orientation, size - T Tauri, HAe disks well isolated - Line ratios constrain n,T,chemistry (1 map+spectra)

DM Tau, PdBI


Chemistry in YSO Accretion Disks. II
LkCa 15 Disk, OVRO Photochemistry near the disk surface?

Disk transport timescales?


Complementary IR Envelope/Disk Studies
CO emission at 4.7 µ m, 0.1-10 Keck AU gaps? Other species?
NIRSPEC R=25000

VLT


Planetary Science with Millimeter Arrays. I.

Planetary Science with mmArrays I
BIMA LkCa 15 Disk

OVRO


Planetary Science with Millimeter Arrays. II.

Planetary Science with mmArrays II
BIMA LkCa 15 Disk

OVRO


Comets with mm-Arrays
HaleBopp Jets, OVRO

Comae are LARGE, so good zero spacing flux or models mandatory! Jets, however, are compact.


Future Submm Arrays - ALMA
64 12m's SIS, 8 GHz IF Construction FY02 approved.

2011


ALMA Receiver Bands/Atmosphere

ASTE telescope: Ship to Chile '01 Operational in '02 SIS receivers Superconducting submm camera


Future Submm Arrays ­ ALMA. II
ALMA will be incredibly sensitive ­ Disk images will be possible in continuum to a resolution of <1 AU! Little is known about the Southern sky at high angular resolution...


Conclusions
-Wealth of opportunities for the ATCA, start with small sources that exploit the excellent sensitivity (disks, absorption line studies...), then move toward mosaics as the system improves. - Make aggressive use of public datasets on nearby clouds and galaxy (2MASS, SIRTF) and on the new submillimeter single dish capabilities in Chile. - ATCA not just an ALMA pathfinder, excellent complementary science even after 2011.