CryoNIRSP Performance Summary Sept. 20, 2014

CryoNIRSP Wavelength and

Angular Resolution

0

0.1

0.2

0.3

0.4

0.5

0.6

0 1000 2000 3000 4000 5000 6000 7000

Sp

ati

al R

eso

luti

on

[arc

sec]

Wavelength [nm]

C DL V

VBI

VISP DLNIRSP

CryoNIRSP

VTF

CryoNIRSP Overview

• Standalone instrument: no AO or beam sharing,

integrated context imaging and spectropolarimetry

• Diffraction limited at long-wavelengths without AO

• Big FOV

• Broad wavelength range

• “Coronal Instrument”

– Reflective optics, Optimized scattered light control

– Core and wing PSF calibration

– Wide dynamic range photometry

• Flux sensitivity allows full-aperture stellar polarization

calibration

CryoNIRSP Modes

• Science operations modes (imaging and

spectroscopy)

– Solar Disk

– Off-limb corona

– Near-limb corona

• Calibration modes

– Geometry registration (context, spectral, beamsplitter)

– Wavelength

– Polarimetric crosstalk

– Photometric/scattered light

CryoNIRSP Optical Summary:

A cryogenic instrument

Table 4.6. Representative CryoNIRSP

Optical Specifications

CryoNIRSP

Grating (primary) Echelle: 32 line/mm

Grating size 408 154 mm

Relay, focal ratio 18

Coll/Cam. Focal Ratio 18/8

Plate scale 0.16 mm/arcsec

Slit Width, multi-slits 52/175µm

Pixel scale (at 1 μm) 165 mÅ

Pixel scale (arcsec) 0.12“ (18μm pix) Design/Diffraction

limited FOV 240/90”

Hawaii-2RG FOV 240" Cold blocking filter

BW 1%

System QE 5% Max spectral

resolution at 4μm 100000

CryoNIRSP FOV

4’ slit

3’ scan

90s

CryoNIRSP Single Slit Data Sample: Si IX 3.93μm

3.94μm

3.92μm

240 arcsec = 0.25 R☺

I+P

I-P

ATST and CryoNIRSP will

measure B>5G at this resolution

in about 1hr

Kuhn, IAS, 2008

Si IX: v, B Sensitivity Estimates

• Estimate Si IX 3.9μm line measurements 1arcsec, 1min

• At edge of field, r = 0.25R from limb

– S =102 phot/s/pix(1μS) x (n=40) x (9pix=1”) x (60s) = 2x106 phot

– B ≈ S k=10-3

– σv = 60km/s x k = 60 m/s

– σB = 60 x 0.24 = 15G

• Near limb

– S =103 phot/s/pix (10μS) x (n=40) x (9pix=1”) x (60s) = 2x107 phot

– B ≈ S k=3x10-4

– σv = 60km/s x k = 20 m/s

– σB = 60 x 0.24 = 5G

• 3x4’ region, 1” samples, 5G max. sensitivity, 3hr (1hr w/

triple slit)

Exposed CryoNIRSP 77K

Cold Optics

Spectrograph

Context

Imager

Helium closed-cycle coolers

Mechanism feed-thrus

Warm coude

optics

CN Wavelengths and benchmark

coronal magnetic sensitivity

Wavelength (μm) Line

0.53 FeXIV

0.637 FeX

0.789 FeXI

1.075 FeXIII

1.083 HeI

1.25 S IX

1.43 Si X

2.218 FeIX

2.326 CO

2.58 SiX

3.028 MgVIII

3.93 Si IX

4.651 CO

Sky and Corona at 0.1R

Temperature sensitivity from 3000K to 3MK

(2R)

DKIST and CryoNIRSP: emergent

science frontiers

• The molecular photosphere

– Ambipolar dynamics in sunspots

• Observing the heliosphere from the ground

– A dusty plasma, “inner source”

• Our dark energy problem

– Seeing coronal magnetism

– Permitted + Forbidden line Hanle Vector coronal

magnetometry

• Night-time solar physics

– Imaging magnetism in other stellar atmospheres

and learning from solar magnetism

– Circumstellar science (imbedded stars…)