Armin Rest NIRCam Deep field overview Sky Background PSF ETC - PowerPoint PPT Presentation

Armin Rest

 NIRCam Deep field  overview  Sky Background  PSF  ETC example for NIRCam and MIRI:  Galaxy @ z=1.5 and z=8  I will start from scratch! You can follow with your own laptop, comment, make requests!  Bonus  Suggestions from audience?  SN Ia at high-z with NIRCam and NIRSpec

 Teledyne HgCdTe H2RG detectors  SW: 0.6 – 2.3 micron (0.032 “/pixel)  LW: 2.4 – 5.0 micron (0.065 “/pixel)  FOV: 2x 2.2’ x 2.2’  5” inter-detector gaps  40” inter-module gaps  Grism Slitless Spectroscopy (R=1200-1500, LW! )  Coronography

 NIRCam (PI: M. Rieke), MIRI (PI: G. Rieke) & NIRSpec (PI: P. Ferruit) GTO programs  Galaxy Evolution  first steps (z>10)  end of the dark ages (7<z<9)  epoch of galaxy assembly (2<z<6)  Deep, multicolor imaging

Spectra from Ryan Endsley

 Background depends on Pointing and Date  Background important for long wavelengths  Background increases at edge of visibility window

 Aperture size  1.5-2 FWHM for aperture photometry  2.5 FWHM for PSF photometry  Caution with very small apertures  Nominally high SNR, however: ▪ Sub-pixel effects ▪ centroiding

 3.0 pixels=0.095”  FWHM  0.6 micron: 0.09” (max 0.12”)  0.9-1.5 micron: 0.07” (max 0.105”)  1.8-2.2 micron: 0.07”

 3.0 pixels=0.19”  FWHM  2.5 micron: 0.10”  3.0 micron: 0.11”  4.0 micron: 0.14”  5.0 micron: 0.16”  I choose 0.15” as aperture radius

Source 1  Scene1 Calculation 1   Background  Input spec  Instrument  (z=0! Detector (Exptime)  Microns!)  Scene N  Normalize ▪ Redshift z1  Calculation N ▪ Mag/flux at that z1  Source 2  Source N

Scolnic+PS1, in prep.  SN Ia cosmology  Push for higher redshifts  Better lever arm Jones+13, SN UDS10Wil, z=1.9, WFC3 F125W,F160W ~ 24.8  w’  SN Evolution?  Different SN population/progenitors ?  Simulating SN Ia  What redshift can we push in the different restframe bands? What exposure times?

 Simulated SN Ia  SNANA  Realistic stretch and color distribution  z from 0.2 to 3.5  Mags for given JWST filter

 Simulated SN Ia  SNANA  Realistic stretch and color F090W F115W F150W F200W F277W F356W distribution  z from 0.2 to 3.5  Mags for given JWST filter  What we really want: Mags for given restframe

F150W F070W F090W F200W F115W F277W Restframe y Restframe g F150W F356W F200W F444W F090W F150W F115W F200W F150W F277W F200W Restframe J Restframe i F356W F277W F444W F356W