Comparison of Photometric And Spectroscopic Redshifts

SCUBA beam (850  m) Atacama beam (350  m) Atacama FOV The Atacama Telescope bolometer camera’s large FOV and high angular resolution provide a powerful tool in measuring magnetic fields, by observing the polarization of FIR dust emission. NGC2024 [Image: Mathews et al. 2002] The FIR emission Of dust is polarized At the level between A few and several % (Hildebrand, Dragovan & Novak 1984).

Most PMS stars of < 3—4 solarm are thought to have circumstellar disks Disks last a few Myr, until they dissipate Planets form during that phase Disks’ sizes are thought to vary widely, between a few 10’s and few 100 AU Disks’ masses also vary widely, about on average a few % of the stellar mass Disks’ temperatures are consistent with irradiation by the star, hence they exhibit strong thermal gradients Inner disk morphology can be studied via scattered radiation in the NIR Understanding of disks’ physics requires measurements of dust mass, which radiates in the FIR Outer disk structure is tidally disrupted by the presence of planets Circumstellar Disks Flux (Jy) Wavelength (  m) Heinrichsen et al.1998 SED of Disk around Vega go

SOFIA at 38  m Atacama at 200  m SIRTF at 38  m LMT at 1100  m

Vega  Eri. Scuba beam at 850 mm Atacama beam at 200 mm

SCUBA 5-sigma 10,000sec PWV 1.5mm JCMT Confusion Limit Atacama 5-sigma 10,000sec PWV 0.3mm Atacama Confusion Limit

LMT 5-sigma 10,000sec PWV 1.5mm LMT Confusion Limit

Atacama 5-sigma 10,000sec Atacama Confusion Limit

Atacama 5-sigma 10,000sec PWV 0.3mm Atacama Confusion Limit

Surface error budget (micron) and pointing Error (arcsec) for the LMT, ALMA and the Proposed Atacama FIR/submm Telescope Both LMT and ALMA telescope Will operate without dome/windscreen Protection. Their surface error Budgets are designed for operation In up to 10 m/s winds.