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HINODE Operation Plan (HOP)

accepted on

22-mar-2018

 HOP No.

  HOP title

HOP 0356
The temperature structure of the chromospheric network: coordination with ALMA cycle 5 observations

plan term

2018/04/18-2018/04/18
2018/04/21-2018/04/21

 　 　

proposer

  name : Cauzzi, Reardon, Molnar, Uitenbroek, Chen, Cranmer, Chai, Mathioudakis 　  e-mail : gcauzzi[at]NSO.edu

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:
ALMA-Hinode-IRIS-GBO coordination to assess spatio-temporal structure of the temperature of the chromospheric network

Scientific Justification:
We will study the spatial and temporal distribution of chromospheric heating in around quiet Sun magnetic network, both on-disk and near the limb. We aim at recovering the chromospheric plasma temperature via the calibrated continuum observations in ALMA Bands 3 and 6, to compare and contrast with results obtained from concomitant observation of chromospheric spectral lines, Halpha in particular (Cauzzi et al. 2009). Coordinated, high cadence observations with Hinode (SP, XRT and EIS, if available) and IRIS will allow us to relate the dynamics of the photospheric magnetic field with the chromospheric heating (events), as well as to gauge the response of the outer solar atmosphere. A total of ~2-3hr of observations is requested (see below).

 request to SOT
SP: fast scan, 3.2 s exposure, 0.32" sampling along slit; 0.32" slit step. 20" (raster) x 82" (slit), ~4 minute cadence, repeated. ~19 Mb/scan

 request to XRT
Continuous high cadence time series
Al-poly+Open or similar filter 1x1 pixel, FOV 128"x128" or 64"x 64"(384"x384", if telemetry available with high cadence)
Highest possible time cadence (shorter than 8 sec). See HOP 327

 request to EIS
If EIS is available, we would like to request the standard observations of HOP 328 "Support for ALMA" (60"x60" wide Maps with the 2" slit of low coronal lines)

 other participating instruments
ALMA: #1197
BBSO/NST; NSO/DST Best observing window is 14-19 UT
IRIS:
We'd like to run OBSID 3624505432 as in our ALMA run of 2017. Medium coarse 8-step raster; 14"x 60"; 3s exposure, line list v36_01. We'll discuss further details with IRIS PI (in particular for
near-limb observations)

 remarks
Dates: A total of 2 hrs of ALMA observations for this program have been granted for cycle 5, to be run in April 2018. Exact dates are not yet defined, but plausibly this program will run in the second half of the month. Support has been secured from both the Dunn Solar Telescope and the Goode Solar Telescope.

Time window: We will coordinate with both DST (New Mexico) and GST (Big Bear). Best observing conditions at the ground based sites are within the ~14-19 UT window. ALMA planners are aware of the constraints and willing to run within this window (weather permitting).

Target(s) of interest: Quiet Sun magnetic network.

Additional Remarks:
Per past experience, ALMA might delay start of observations due to weather/technical issues; it will be safer to extend the coordinated observations to ~ 1 hr after nominal end of period.

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