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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0276

Joint Observations of ALMA, Hinode and IRIS for the scientific verification of ALMA data

plan term


@ @


 name : Shimojo, Bastian, Brajsa, NA&EU-ALMA @  e-mail : masumi.shimojo[at]nao.ac.jp

contact person in HINODE team

 name : Shimojo @  e-mail : masumi.shimojo[at]nao.ac.jp

 abstract of observational proposal
Objective: To verify the quality of solar data obtained with ALMA, we wish to compare the ALMA data with the data observed with Hinode. The scope of the scientific achievements from ALMA solar observations will be clarified by these simultaneous observations.

The Atacama Large Millimeter/sub-millimeter Array (ALMA) is a millimeter/sub-millimeter interferometer of revolutionary design, composed of 66 high precision antennas located on the Chajnantor plateau, 5000 meters altitude in northern Chile. The Sun is one of the observing targets of ALMA, and ALMA data will contribute significantly to the understanding of not only flare science but also chromospheric science.

ALMA solar observations are still in the commissioning phase now. We will hold a observing campaign for commissioning of solar observations from December 9 to December 16, 2014. The principal goals of the campaign are; 1) to establish the observing sequences and calibration methods for solar observations in public use, 2) to verify the quality of solar data obtained with ALMA, to fix the specifications for ALMA solar public-use observations, 3) to provide data needed for assessing the scientific achievements to be obtained from general use of ALMA observations. To verify the quality of ALMA data and assess the scientific achievements, a comparison between ALMA data and Hinode data is important. Especially, CaII images obtained with SOT show us the atmospheric layers close to those seen in the continuum with ALMA data, and the spatial resolution of SOT is similar to the predicted spatial resolution of solar synthesized image made from ALMA data with the planned antenna configuration of the early phase of public use. Hence, the SOT data are essential for the scientific verification of ALMA solar observations. To achieve the goals of this first campaign, we propose joint observations of ALMA and Hinode.

 request to SOT
- Ca II
 ! Time cadence: better than 5mins cadence (1 mins cadence is good)
 ! Binning: 1x1
 ! FoV: 100h x 100h
- G-band (used for co-alignment)
 ! Time cadence: one image per one hour.
 ! Binning: 1x1
 ! FoV 100h x 100h

SP: (Please obtain SP data only when the target is the structure on disk.)
! One map for one observing period
! FoV 100h x 100h
! Fast-Deep Mode

 request to XRT
We will use XRT data to identify weak coronal activity.
- AR: Al-poly & thin-Be, better than 3 mins cadence, FoV: 128h x128h
- QR: Al-mesh & Ti-poly, better than 3 mins cadence, FoV: 128h x128h
- Limb: Al-mesh & Ti-poly, better than 3 mins cadence, FoV: 128h x128h
- Please enter one White Light image every one hour

 request to EIS

 other participating instruments

We are discussing the plans for the solar campaign now. We will provide a detailed schedule of the campaign to the Hinode team at an appropriate time prior to the actual observations.

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