Grism Spectroscopy with FLITECAM Erin C. Smith (UCLA) Ian S. McLean (UCLA)

FLITECAM micron NIR camera 1024x1024 InSb Aladdin III detector Optics cooled to ~ 80K with LN2 Detector controlled at 30K

SOFIA

8 arcminute circular FOV.43 arcsec/pixel (SOFIA).48 arcsec/pixel (Lick) Entrance aperture Slit mechanism Collimator Dual Filter Wheel Re-imaging optics Detector

Why spectroscopy? Water Vapor monitor calibration –Resolve 2.5 micron water line (need R~1000) Allows low background, low water vapor spectroscopy in the thermal ( micron IR) –No spectral coverage by Spitzer at these wavelengths

Science PAH features at 3.3  m Water ices  m Pa-a (1.87  m ) Br-  (4.05  m )

Grism Spectroscopy d d pupil X mm =d pupil /cos A A ii dd grism normal T m c = (n – 1) sin A R = (n – 1) d pupil tan A / D tel s arc, (max/min wavelength) = c +/- [(n – 1) d pix cos A / F cam m T] *N pix /2,

KRS-5 N~2.4 Thalium bromo-iodide Manufactured by Zeiss- Jena –Can make grisms with T=651/n, up to 40 degrees

Wavelength coverage

Slit

Lab testing Neon Argon lamps used to calibrate wavelength solutions Slit width found to be slightly larger than designed, narrow slit is 1.3”, wide slit is 2.35” wide R ~1700/900

FLITECAM also mounts to the Shane 3 meter telescope at Lick Observatory Imaging mode commissioned October 2002 Spectroscopy mode was commissioned in June 2004

DifferenceRAW C + K wide C + LM 69 Leo A0V star, for telluric standards High backgrounds at Lick require differences in thermal IR

Gl406- (M5.5) Raw H band spectrum A-B spectrum High-res position B High res position A

Data reduction

NGC 7027

Imaging & spectroscopy Switching between spectroscopy and imaging takes less than 20 seconds Using narrow band filters, we can make maps of spectral features, then use spectroscopy to investigate

Aboard SOFIA