ETC Teaching Session Instructor: Swara Ravindranath JWST Proposal - PowerPoint PPT Presentation

The Canadian NIRISS Unbiased Cluster Survey (CANUCS) ETC Teaching Session Instructor: Swara Ravindranath JWST Proposal Planning Workshop May 15 – 18, 2017 STScI

The Canadian NIRISS Unbiased Cluster Survey (CANUCS) • Slitless spectroscopy and Imaging of 5 massive galaxy clusters and 10 parallel fields using NIRISS WFSS, NIRCam imaging, and NIRSpec MOS modes • Primary science goals: 1. DetecJon and CharacterizaJon of galaxies within the reionizaJon epoch 2. EvoluJon of low-mass galaxies across cosmic Jme 3. Resolved emission-line maps and line raJos for galaxies in the cosmic noon

The Canadian NIRISS Unbiased Cluster Survey (CANUCS) Cluster SelecDon: • 1. High mass and large area with high magnificaJon 2. CriJcal curves fit within the 2.2’ x 2.2’ FOV of NIRISS 3. More than 10 degrees away from zodiacal plane 4. Minimal area lost to bright stars 5. At z>0.35 to avoid contaminaJon from ICL and cluster galaxies 6. High quality data available at other wavelengths

The Canadian NIRISS Unbiased Cluster Survey (CANUCS) NIRISS Wide Field Slitless Spectroscopy IdenJcal grisms (GR150R and GR150C) with R=150 • Grisms disperse along Orthogonal direcJons • Grisms mounted on Filter wheel • Blocking filters in the Pupil wheel • Can use 6 short wavelength filters for WFSS •

The Canadian NIRISS Unbiased Cluster Survey (CANUCS) NIRISS Prime ObservaDons (137/199 hrs) • CANUCS GTO also includes: NIRISS direct imaging in F115W, F150W, F200W – 4 exposures of NIS Ng=13 (4x558s = 2232s) NIRCam Imaging NIRISS GR150R grism in F115W, F150W, F200W – NIRSpec MOS 8 exposures of NIS Ng=33 (8x1417.3s = 11338s) NIRCam Imaging parallels NIRISS WFSS parallels NIRISS GR150C grism in F115W, F150W, F200W – 8 exposures of NIS Ng=33 (8x1417.3s = 11338s) NIRISS WFSS Observing sequence • Direct image --- GR150C --- Direct image Direct image --- GR150R --- Direct image

JWST ETC - Topics being covered • Re-useability of scenes in mulDple calculaDons (point src sensiJviJes) • Batch expansion (deciding on integraJons, exposure Jmes) • Adding Emission Lines to source spectra (grism exposure sensiJviJes) • Sky Background with posiDon (effect of background on SNR)

JWST ETC -Topics being covered • Complex scenes (eg; lensed galaxies) • Spectral overlap from close targets (esJmate contaminaJon for the 2 grisms) • Aperture Size (choosing aperture radius for strategy) • Upload Source Spectrum (user-supplied spectra for special targets)

JWST ETC - Downloads Direct image GR150R+200W GR150C+200W • FITS files of 2D SNR, Detector image, SaturaJon Maps • FITS file of 3D data cube • Tables of the lineplots for SNR, extracted source flux, background flux, and contaminaJon

Scene 1 has mulJple sources to examine Adding emission lines to the SNR in direct & grism exposures source spectrum Examine the source Examine the sources, overlap, spectrum and flux levels orientaJon

Complex scenes and sources Reusability of sources can be created in 2D Galaxy spectra templates Examine the source spectrum and flux Examine the sources, overlap, levels, adjust wavelength range in plots orientaJon

GR150R: Overlap along dispersion direcJon GR150C: Overlap minimal along orthogonal dispersion direcJon

Over-subtracJng the background from within the scene

GR150C GR150R Line spread funcJon depends on morphology of source. In GR150C, lensed arc is along the dispersion direcJon and results in lower spectralresoluJon relaJve to GR150R.

CalculaKons for z=8.79 starburst galaxy near bright cluster galaxy at z=0.45 Ly-α CIII] Plot results for 3 filters for full λ coverage