# Presentation: 053477

## Paul M. Harveya
George H. Riekeb
Daniel F. Lestera
Dominic J. Benfordc

aUniversity of Texas
bUniversity of Arizona
cGoddard Space Flight Center

***George H. Rieke******b***
***Daniel F. Lester******a***
***Dominic J. Benford******c***
- aUniversity of Texas
- bUniversity of Arizona
- cGoddard Space Flight Center

## SAFIRSingle Aperture Far-Infrared Observatory

- Basic observatory parameters
- 10-m Class
- Operating temperature ~ 4K
- Wavelength range 20 – 500+ m
- Lifetime > 5 years
- SAFIR concept embraces FAIR and DART mission goals as well
- Decadal Survey Recommendation

## Context of the SAFIR MissionA Far-IR mission with sensitivity and resolution to complement and enhance the investments in neighbouring spectral regions

- 2000-2010 Decade
- SIRTF launch and mission completion
- SOFIA operating
- Herschel Space Observatory launched
- NGST near completion
- ALMA begins operations
- Rapid progress possible due to slow start for Far-IR

## SAFIR Science Drivers The Ubiquity of Far-IR/Submm Radiation

- Dust is an extremely efficient reprocessor of short wavelength radiation into IR/Submm
- The young distant universe is redshifted from the visible/NIR to Far-IR/Submm
- Young objects are cool both line and continuum emission occur at long 

## Early Galaxies and the Birth of AGNWhen and How Do Black Holes Form

- X-Ray background indicates most AGN’s at high redshift are heavily absorbed
- AGN/Starburst separation can be done with IR fine structure lines, e.g. Ne
- Far-IR/Submm background and low-res imaging shows many high luminosity, dust enshrouded galaxies

## The Youngest Gas CloudsThe Birth of Stars and Galaxies

- H2  lines at 17, 28m (redshifted) will be emitted by very young, metal-poor gas clouds
- As soon as metal production starts:
- C+ line at 158m, N+ lines at 122 and 205m
- Will be redshifted into 200 - 700m where observations from the ground are very difficult

## Star and Planetary System BirthPhysical Structure of Circumstellar Disks

- Imaging and spectroscopy with < 100 AU spatial resolution for nearby protostars
- CO, H2O, [O I] lines probe different physical and spatial regimes.
- The combination of spatial and spectral resolution means that the collapse process can be dissected and compared among stars of different masses and environments.

## Planetary System EvolutionDebris Disks and Their Interaction With Planets

- KBO’s in our Solar System enable primitive Solar Nebula conditions to be studied.
- Debris disks around other stars provide a similar laboratory, and many will be found by SIRTF in the next few years.
- Spatial resolution and spectroscopic capability can help us understand how planetary systems form and evolve.

## Telescope Requirements

| Parameter | Requirement | Driving Science |
| --- | --- | --- |
| Aperture | > 8m | High z Galaxies; Debris Disks |
| Temperature | ~ 4K | Spectroscopy; L* Galaxy@ z ~ 5 |
| Wavelength Range | 20-800m | NGST Overlap; Gas Cooling Lines |
| Diffraction Limit | 40m | Debris Disks; Distant Galaxies |
| Pointing Accuracy | 0.5 – 1” | Driven by 40m  diffraction limit |
| Pointing Stability | ~ 0.1” | Driven by 40m  diffraction limit |
| Lifetime | > 5 years | Productivity |

## Strawman Instrumentation

| Instrument | range | Spectral 
Resolution | FOV | Driving Science |
| --- | --- | --- | --- | --- |
| Camera | 20 - 600m | ~ 5 | 1-4’ | High z reddening
KBO’s |
| Spectrometer | 20 - 100m | ~ 100 | ~10”
Img Slicer | Debris Disks; YSO’s |
| Spectrometer
 | 20 - 800m | ~ 2000 | ~ 1’ | C+;  N+; Chemical Evolution |
| Spectrometer
 | 25 - 520m | ~105 | > 1 beam | Dynamics; Gas Cooling |

## Sensitivity DriversThe Natural Sky Confusion Limit

- Fig 3 from paper

## Comparison With Other Facilities

- Fig 4 from paper

## Observatory Concepts – NGST-likeSmaller Aperture – Relaxed Surface Tolerance

## Observatory Concepts – New TechMembrane Mirror

## Near-Term GoalsTechnology Studies/Development

- Detector technology advancing rapidly but needs continued support
- Bolometers
- Photoconductors
- Heterodyne detectors and local oscillators
- Telescope technology tradeoffs
- NGST-like with less stringent performance
- New, e.g. membrane telescope technology
- NASA has just begun an initial technology study
- Most significant issue likely to be telescope cooling

## Summary

*     “**The combination of its size, low temperature, and detector capability makes its astronomical capability about 100,000 times that of other missions and gives it tremendous potential to uncover new phenomena in the universe.  SAFIR will complement ALMA, NGST, and TPF by providing sensitive coverage of the wavelengths that lie between the capabilities of these missions.”*