HOP 0357

HINODE Operation Plan (HOP)

accepted on

22-mar-2018

HOP No.

HOP title

HOP 0357

Joint observation of a quiescent filament with ALMA and IRIS

plan term

2018/04/22-2018/04/22
2018/05/04-2018/05/04

proposer

name :

Rodger, Wedemeyer, Labrosse, Szydlarski, Simoes, Fletcher

e-mail :

a.rodger.1[at]research.gla.ac.uk, sven.wedemeyer[at]astro.uio.no, nicolas.labrosse[at]glasgow.ac.uk, mikolaj.szydlarski[at]astro.uio.no, paulo.simoes[at]glasgow.ac.uk, lyndsay.fletcher[at]glasgow.ac.uk

contact person in HINODE team

name :

Savage, Watanabe, De Pontieu

e-mail :

sabrina.savage[at]nasa.gov, watanabe[at]uvlab.mtk.nao.ac.jp, bdp[at]lmsal.com

abstract of observational proposal

Main Objective:
To determine the temperature distribution across a solar filament using ALMA and coordinated observations.

Scientific Justification:
Solar filaments, also known as prominences when viewed off-limb, present some of the most complex and intriguing mysteries still facing solar physics to this day. Believed to be confined magnetically by the coronal magnetic field, filaments consist of a cool dense plasma core surrounded on all sides by one of the solar systems most energetic yet sparse environments, the million K coronal plasma. How then does the structure of the boundary between these so very contrasting regimes appear? How is this environment sustained with such large density and temperature gradients? We have been granted a category B observing proposal to investigate these questions using the new solar capability of the Atacama Large Millimetre/sub-millimetre telescope in its cycle 5. In this proposal we would like to take advantage of the planned coordination between ALMA and instruments such as HINODE. By co-ordinating our ALMA observation with HINODE we will be able to vastly increase the scientific significance and scope of this project through the ability to probe the filament structure at different formation layers defining each observing band.

request to SOT

SP -Fast map (cycle 2), cadence=repeat
FOV=100"x82", sum=2x2

FOV may be adjusted depending on the size of the filament and available telemetry.

request to XRT

As HOP 0328 e.g.
-AR: Al-poly & thin-Be, better than 3 mins cadence, FoV: 128"x128" (512"x512", if telemetry available)
-QR: Al-mesh & thin-Be, better than 3 mins cadence, FoV: 128"x128" (512"x512", if telemetry available)

request to EIS

As HOP 0328 e.g.
60"x60" wide Maps with the 2" slit of low coronal lines. Input from EIS team about appropriate support observation encouraged.

other participating instruments

ALMA: #734
IRIS:
3620107469 | Large dense 128-step raster 42.2x120 128s Si IV Mg II h/k Deep x4 | 665.86 | 507.25 | 0.5 | 5.2+/-0.1 | 666+/-0 | 0.0+/-0.0 | 10.4+/-0.0 |10.4+/-0.0 | 0.0+/- 0.0

SST?

remarks

Dates: ToO. Observation is likely to occur during one day whilst ALMA is in the correct array configuration; 30 March -15 May, and 15-30 August.

Time window: ALMA observation consists of 3 2-hour duration science goals leading to a total observation duration of approximately 6 hours. Exact time of day is not currently known.

Target(s) of interest: A (quiescent) Solar Filament (TOO)