Holography far-side images with HMI

Irene Gonzalez HernandezCharlie LindseyRichard BogartPhil Scherrer

Sebastian Couvidat, and the calibration team !

Quick solution (I)

High resolution Dopplergrams

Low resolution Dopplergrams

Binning Algorithm

Stanford

Low resolution Dopplergrams

Tucson

Farside maps

Farside maps

NetDRMS GONG farside pipeline

Tucson Web Publication

StanfordWeb Publication

First attempts to calculate far-side maps

Apr. 4 2010

May 7 2010

May 13 2010

First attempts to calculate far-side mapsHMI cuts of the central region of the “far-side map”

First attempts to calculate far-side mapsGONG cuts of the central region of the “far-side map”

The input dataHMI (binned) postel projected Doppler images

The input data

HMI (binned) postel projected Doppler images

Temporal series of a single pixel

The input dataHMI averaged postel-projected Dopplergram

The input dataAcoustic power map

The input dataDoppler Parameters

The input dataSensitivity of the Doppler signature to the radial velocity of the Spacecraft

The input dataSensitivity of the Doppler signature to the radial velocity of the Spacecraft

Quick solution (II)

FS Preprocessor

Fourier transformeddata cube

Tucson

Farside maps

NetDRMSModified GONG farside pipeline

Tucson Web Publication

StanfordWeb Publication

High resolution Dopplergrams

Fourier transformed data cube

Stanford

H. Farside maps

T-D. Farside maps+

Time-distance pipeline

The FS Preprocessor

•Postel Projection of Dopplergrams•Quality control:• Frame rejection (based on NaN values)• Glitch/cosmic-ray recognition and removal (deviation from

temporal trends)• Conformation to appropriate rotational profile

•Spatial filtering/condensation (what is this?)•Spectral filtering: extraction of the 2.5-4.5 mHz band

•** Possibility of binning down to 90sec. Cadence (Nyquist frequency of 5.6mHz)

The FS Preprocessor

Possibility of binning down to 90sec. Cadence (Nyquist frequency of 5.6mHz)