1. PFIS Commissioning - SSII
The Prime Focus Imaging Spectrograph - Operations and Commissioning Science K. Nordsieck Univ of Wisconsin
PFIS modes
Commissioning science programs
PI tool demo
Oct 29, 2003
PFIS Commissioning - SSII

2. PFIS Commissioning - SSII
PFIS Modes
Optics configuration
Detector Configuration
Config
Pol
Slit
Normal
Hi Spd
Shuffle
Drift
Imaging No X x
L,C,S
Multislit
VPH Spectro- scopy
Longslit
Fabry- Perot
Commissioned Not Commissioned
Oct 29, 2003
PFIS Commissioning - SSII

3. Commissioning Science Programs
Title
Purpose PI
Program
Imaging
Astrometry, Photometry
PFIS
Some good cluster
VPH Spectroscopy
Longslit
PFIS, C. Kobulnicky
Abundances in PNe in Early-Type Galaxies
Multislit, Shuffle
High-Speed VPH spectroscopy
High Speed
D. O'Donoghue
Magnetic Cataclysmic variables
Imaging Polarimetry
Linear Polarimetry
K. Nordsieck, K. Bjorkman
Circumstellar disks in the LMC and SMC
VPH spectropolarimetry
Fabry-Perot spectroscopy
Fabry-Perot
T. Williams
Population and velocity dispersions of Intermediate-Redshift Galaxy Clusters
Oct 29, 2003
PFIS Commissioning - SSII

4. PNe Early-Type Galaxies
One Prediction for NGC1399
Dwarf Irregulars
Diffuse Ellipticals
Scientific goal: Oxygen abundances in a giant E galaxy to establish star formation history from O/Fe
Method: multislit UV-blue spectroscopy of Planetary Nebulae
Oct 29, 2003
PFIS Commissioning - SSII

5. PFIS Commissioning - SSII
NGC1399 PNe
Suggested target: NGC 1399: E0, distance 16 Mpc (Fornax Cluster)
~70 PNe positions known from narrow-Band imaging (Ciardullo 1989)
Wavelength range 340 – 510 nm. Resolution ~5000 (to overcome stellar background)
S/N ~ 10 for line F > 3x10-18 erg/s/cm2 (1% of OIII5007 in brightest PN)
Byproduct: kinematics in outer part of galaxy
Makes use of PFIS field, UV sensitivity, resolution
Use to demonstrate long – slit, multislit, shuffle, multislit planning and extraction
Oct 29, 2003
PFIS Commissioning - SSII

6. Circumstellar disks in the LMC and SMC
Spectropolarimetry of φ Per
(PBO 0.9m)
Balmer Jump
Paschen Jump
Scientific goal: establish nature of circumstellar disks in Be stars in LMC/ SMC open clusters
Much larger fraction of B stars are Be (~60%) in LMC than MW: different angular momentum evolution?, metallicity?
Method: UV – red multislit spectropolarimetry: Balmer Jump, Paschen Jump + disk models
Oct 29, 2003
PFIS Commissioning - SSII

7. PFIS Commissioning - SSII
LMC, SMC Open Clusters
NGC 1818 (LMC)
Suggested target: NGC 1818 (LMC), NGC 330 (SMC)
40 Be candidates identified from spectroscopic studies in 1818, 33 in NGC 330, V = 13.7 – 17.2
Linear spectropolarimetry wavelength range 320 – 900 nm. Resolution ~1000 using 900 l/mm grating in blue and red setting
Imaging multislit polarimetry to get interstellar polarization from field stars V < 20 - byproduct: magnetic field map
Makes use of PFIS field, UV sensitivity
a subset of candidates have broad band polarimetry, for verification of calibration
imaging polarimetry
spectropol-arimetry
Oct 29, 2003
PFIS Commissioning - SSII

8. Proposal process and the PI tool
I: use Phase I PI tool (telescope + instruments) to model proposed observations, define instrument configuration, generate proposal for local SAC
II: if approved, use Phase II tool to detail the observation, calibrations (output: instrument script) and define slitmask  "Science Database" and queue definition
SALT Astronomer modifies as necessary for reality, data distributed
PFIS to supply IRAF package for basic reductions (bias, dark, flatfield, wavelength, flux)
Oct 29, 2003
PFIS Commissioning - SSII