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

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

Oct 04, 2023 108 likes •290 views

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

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SLIDE 1

Armin Rest

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SLIDE 2

 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
  • wn laptop, comment, make requests!

 Bonus

  • Suggestions from audience?
  • SN Ia at high-z with NIRCam and NIRSpec
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SLIDE 3

 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

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SLIDE 4
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SLIDE 5

 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

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SLIDE 6

Spectra from Ryan Endsley

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SLIDE 7

 Background

depends on Pointing and Date

 Background

important for long wavelengths

 Background

increases at edge of visibility window

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SLIDE 8

 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

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SLIDE 9

 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”

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SLIDE 10

 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

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SLIDE 11

Source 1

  • Input spec

(z=0! Microns!)

  • Normalize

▪ Redshift z1 ▪ Mag/flux at that z1

 Source 2  Source N

 Scene1

 Scene N

Calculation 1

  • Background
  • Instrument
  • Detector (Exptime)

 Calculation N

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SLIDE 12
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SLIDE 13

 SN Ia cosmology

  • Push for higher

redshifts

  • Better lever arm
  • w’
  • SN Evolution?
  • Different SN

population/progenitors ?

 Simulating SN Ia

  • What redshift can we

push in the different restframe bands? What exposure times?

Scolnic+PS1, in prep.

Jones+13, SN UDS10Wil, z=1.9, WFC3 F125W,F160W ~ 24.8

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SLIDE 14

 Simulated SN Ia

  • SNANA
  • Realistic stretch

and color distribution

  • z from 0.2 to 3.5
  • Mags for given

JWST filter

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SLIDE 15

 Simulated SN Ia

  • SNANA
  • Realistic stretch

and color distribution

  • z from 0.2 to 3.5
  • Mags for given

JWST filter

 What we really

want: Mags for given restframe

F115W F090W F150W F200W F277W F356W

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SLIDE 16

F115W F090W F150W F200W F277W F356W F115W F090W F150W F200W F070W F150W F200W F277W F356W F444W F150W F200W F277W F356W F444W

Restframe g Restframe i Restframe y Restframe J