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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0231

Sunrise 2013 Co-Observations

plan term


@ @


 name : Lagg, Riethmueller, Solanki, and the Sunrise team
@  e-mail : lagg[at]mps.mpg.de

contact person in HINODE team

 name : Katsukawa @  e-mail : yukio.katsukawa[at]nao.ac.jp

 abstract of observational proposal
The flight of the balloon-borne Sunrise observatory in 2009 demonstrated the high performance of the telescope and its post focus instrumentation in retrieving data with unprecedented resolution. The obtained data sets resulted in numerous publications (see, e.g., Astrophysical Journal Letters, Volume 723, Issue 2, Nov. 2010) and are still being analyzed by solar physics groups world-wide.
Already in 2009 we attempted to obtain co-observations with Hinode. Unfortunately, the problems with the direct communication link to Sunrise, resulting in the lack of knowledge of the exact pointing, made the coordinated observations almost impossible. Additionally, the lack of active regions on the solar surface did not allow for feature-oriented pointing information.

Although great efforts have been undertaken from the Hinode team, no dataset with a common field-of-view(FOV) could be recorded. This was a very unfortunate situation, especially since we know how much additional work the Hinode team put into the support of Sunrise, e.g. by changing tracking curves on Hinode on a daily basis.

With this experience in mind, we plan to change the observing strategy for the re-flight in 2013. The improved communication link between the ground station in Kiruna and the Sunrise observatory should allow for almost real-time control of the Sunrise pointing, and to obtain real-time thumbnail images of the observed region. Therefore, it should be rather straightforward to operate Sunrise as a slave instrument to Hinode.

The most promising strategy to obtain datasets of a common FOV is therefore to define Hinode as the master observatory. We ask the Hinode team to control the pointing in the usual manner by defining tracking curves for a two-day period in advance. These tracking curves are, as usual, displayed on the Hinode operations website, from where the Sunrise team can access the Hinode pointing for every given moment in time. Sunrise attempts to follow the Hinode coordinates. This strategy minimizes the efforts for the Hinode team in performing the co-observations and at the same time maximizes the chances of obtaining joint data sets.

The reflight of Sunrise in 2013 will concentrate on the observations of active regions. The scientific questions address all topics regarding the temporal evolution of the magnetic and velocity field in sunspot umbrae and penumbrae, the surrounding plage fields and pores at the highest achievable spatial resolution. New filters in the Sunrise Filtergraph (SuFi) will also allow to observe the chromosphere above these regions with unprecedented spatial resolution. These topics were already addressed in the scientific proposal for the Sunrise flight in2009 and could not be completed due to the lack of active regions in June 2009. The Sunrise science proposal for the reflight is currently under revision and will be made available for the co-observers as soon as possible.
The high spectral resolution of the SOT/SP telescope ideally complements the Sunrise data from the Imaging Magnetograph eXperiment (IMaX). IMaX will be operated in similar modes as during the 2009 flight, with some adjustments to allow for more sophisticated analysis techniques (i.e. height-dependent inversions applied to Stokes spectra sampled at 8 wavelength positions). In order to maximize the chances for overlapping FOV we propose to perform normal mode scans over active regions (as large as possible during the eclipse season, FOV ≈100~160arcsec2 ).

Albeit the FOV of the normal mode scans is smaller than of the fast mode scans, we prefer the normal mode scans. A newly developed, spatially coupled inversion technique applied to the Hinode SOT/SP data is optimized for the superior quality of the normal mode map data. Additionally, comparing the high spatial resolution data of Sunrise with Hinode data at the maximum possible resolution will simplify the analysis of the joint dataset.

The chromospheric capabilities of Sunrise have been extended by adding new filters to SuFi. The SuFi filters are:

1. The CaIIH filterfrom2009(396.80/0.18 nm),
2. a more narrow CaIIH filter (396.84/0.11 nm),
3. a 300/4.4 nm filter for the lower photosphere,
4. a Mg II filter (279.62/0.48),
5. 214/22 nm for the mid photosphere.

We ask to use a standard mode at highest possible spatial resolution (nobinning) for chromospheric observations for Hinode NFI and BFI as the baseline for the co-observations.

 request to SOT
EActive regions(sunspots with surrounding plage and pores). Various heliocentric angles desirable, starting at positions close to disk center.
E3-4limb observations above regions with various activity levels (on day4 of the Sunrise flight or later).

The start date of the observations should be as soon as possible after the launch of Sunrise. A total of three hours per day preferably during the prime observing time of the ground based facilities on the Canary islands (08:00 –11:00UT) would be highly appreciated.

Normal mode maps, unbinned, 4.8s cadence, over largest FOV possible (constrained by eclipse period and data volume). Estimated data volume: Normal map, 1 side, FOV: 102h~164h (640~1024, ≈52 min), 725 Mbits

A mode optimized for chromospheric dynamics is desired (similarto HOP171). Large FOV preferable over high cadence to maximize chance of overlapping FOV with Sunrise. The duration should be the same as for SOT/SP observation (≈52 min).

1. BFI: sequence of images in the filters Ca IIH and G-band 111h~111h FOV, 2x2 binning (0.108hpix, 1024~1024), at a cadence of32 s(data volume148Mbits)

2. BFI: sequence of images in all BFI filters 111h~111h FOV, 2x2 binning (0.108hpix, 1024~1024), at a cadence of60 s(data volume300Mbits)

3. NFI H-alpha, 3WL (same FOV as SP): 102h~164h, 2~2 binned, at a cadence of 30 s (data volume 317 Mbits)

If data rate permits we would appreciate to obtain at least two SOT scans per day. For each of these scans one of the BFI filter sequences 1 and 2 should be used (alternating for every scan).

 request to XRT

 request to EIS

 other participating instruments
Canary Islands observatories

Time Period for Observations:
We ask for Hinode support during the entire flight of the Sunrise balloon. The flight duration is estimated to be up to 6 days. The exact date of the flight is not known. The sunrise launch window opens on June 1 (earliest possible launch date) and closes on July 18 (latest possible landing date). During this period the procedure for the Sunrise flight is as follows (all times are MESZ = UTC +2h):

1. Day before launch, 14:00: Weather briefing, if predictions are good, fgo-aheadf for launch preparations.

2. Launch day, 01:00: start of payload launch preparations (instrument functional checkout, instrument roll-out in front of integration hall, mounting of solar panels, wind shields, antennas, ballast hoppers etc.).

3. Continuous weather monitoring regarding surface and mid altitude winds throughout the night and early morning, 2 -3 sounding balloon launches.

4. Launch day, 04:00: instrument switch-on in stand-by, instrument check-out.

5. Launch day, 05:00: roll-out to launch pad, antenna check-out.

6. Wait for optimum weather conditions.

7. L-2,5 hours: Roll-out of balloon film and helium filling. decision to launch.

8. Launch (unusually approx. 07:30-10:00).

9. L+2,5hours: balloon is at float, instrument commissioning, and telescope and LISS co-alignment, pointing system parameter tuning.

10. L+ ~5 hours: start of observations.

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