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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0153


plan term


@ @


 name : Judge
Lin, Jaeggli, Pietarila, Tritschler, Centeno
@  e-mail : judge[at]ucar.edu

contact person in HINODE team

 name : Berger @  e-mail : berger[at]lmsal.com

 abstract of observational proposal
This is a coordinated observing program with the Dunn Solar Telescope at Sac Peak operating in somewhat of a Service mode. Phil Judge aims to capture a multi-instrument spectropolarimetric dataset for "a wide variety of purposes" that will be immediately opened to sharing by anyone.  The DST will be attempting to obtain vector field measurements from the photosphere to the base of the corona.  Hinode support is requested primarily as a larger FOV context in which the DST datasets will be embedded. The datasets will be particularly useful for comparison to magnetic field extrapolation models.

 request to SOT
- AT LEAST ONE NFI Na I D LONGITUDINAL MAGNETOGRAM centered on the active region, covering 264"x164"

This is needed to capture magnetic sources/sinks at the photosphere over a large surface area, into which the DST data can be embedded.

- AT LEAST ONE SP 225"X164" FAST MAP. For telemetry purposes it could be compressed (spatially or spectrally).  (40 minutes).

- this would be very useful again for additional magnetic constraints outside the DST FOV.

 request to XRT
SEVERAL XRT IMAGES of the active region encompassing a FOV sufficient to see the connectivity of the brightest features, and some aspects of evolution over say 2 hours. The FOV should be about 260"x260".

 request to EIS
EIS data spanning the FIRS FOV. Since these are some of the first efforts to combine vector fields at the coronal base with coronal spectral imaging, a rastered 1" slit may optimize the scientific return (Doppler information).  This would mean something like 230"x180" FOV for telemetry to the ground. This would mean 230 E-W steps for a 1" slit.  With an exposure time of 10s, this is a 38 minute raster.

Only some of the strongest lines would really be needed, but should include He II.

 other participating instruments
DST: At the DST we will attempt to obtain vector field measurements from photosphere to the base of the corona using IBIS and FIRS.

FIRS will be used in a configuration where four long slits raster across the Sun.  For each pointing with the DST, the following can be obtained:
      x"    y"     Time for raster or image
FIRS   75   172     18 min
IBIS   40    80     20-70s
Thus, with the DST we would point 2-3x for each active region to get

2x... FIRS 150" x 175"   36 min
    IBIS  80" x 80"

3x... FIRS 225" x 175"    54 min
    IBIS 120" x 80"

- IBIS fibril kinematics in Ca II will be used as tracers of field lines, so a 20s cadence is needed. This is in addition to spectropolarimetric measurements of magnetic field.

Hinode support is requested during the prime DST observing window of 15:00 -- 17:30 UT. For example, SOT full FOV magnetic field maps at 15:00, 16:15, and 17:30 would be ideal.

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