Science data sets available to scientists in Sweden
On this page we present SST data sets, that are released for scientists based in Sweden but outside the Institute for Solar Physics.
Please contact us at sst-data-request@astro.su.se.
CRISP and CHROMIS
CRISP is an imaging spectropolarimeter and CHROMIS is an imaging spectrometer, both are based on dual etalon Fabry-Pérot interferometers. CHROMIS operates at wavelengths between 390 and 490 nm, whereas CRISP operates between 500 and 860 nm.
These instruments allow acquiring narrow band images over a relatively large field of view. By tuning the instrument over the spectral dimension, we can sample a full spectral line profile in a few seconds.
At the moment only CRISP allows for polarimetric observations. The main diagnostics that can be observed with CHROMIS are the Ca II H&K and H I Beta lines. The main diagnostics that can be observed with CRISP are the Ca II 8542, H I Alpha, Na I D1, Mg I 517, He I D3 and Fe I 525, 617.3, 630.1, 630.2 nm lines.
Videos
There are temporal videos, illustrating the seeing variations affecting the quality of the data. There are also spectral videos, illustrating the wavelength coverage of the scans. The image next to each table is a CHROMIS Ca II continuum image illustrating what is in the field of view.
The actual data are stored as 5-dimensional datacubes in FITS files. There is metadata in the FITS file headers and extensions as described by Löfdahl et al. (in prep.), including spatial, spectral, temporal, and polarimetric coordinates in the World Coordinate System (WCS).
Because the two instruments are scanning independently, the cadences in the data cubes are not the same. Therefore some frames are repeated in the CRISP cubes (and videos below), to make them the same length. Each frame in the CRISP cubes is the nearest neighbor in time to the frame with the same number in the corresponding CHROMIS cube.
Flux emergence
This datasets was acquired 09:28:36 UT on 2016.09.19 at heliocentric angle mu=1.0. The target is an active region where new horizontal magnetic flux is emerging into the surface, partly changing the properties of the granulation pattern.
In this case the emerging flux is confined between two sunspots, one of which is included in the FOV. This dataset is interesting to study small scale magnetic reconnection events and chromospheric heating. The latter was analyzed by Leenaarts et al. (2018).
107 Ca II K scans collected with CHROMIS. Quasi-simultaneous spectro-polarimetric data were collected with CRISP in the following wavebands: 6563, 6301/6302, 8542 Å.
Scans are defined by the following spectral distances in mÅ from line center:
- Ca II K 3934: -1331, -704, -665, -626, -587, -548, -509, -470, -430, -391, -352, -313, -274, -235, -196, -157, -117, -78, -39, +0, +39, +78, +117, +157, +196, +235, +274, +313, +352, +391, +430, +470, +509, +548, +587, +626, +665, +704, +1331 (plus continuum near 4000 Å)
- Fe I 6302: -1180, -1120, -1070, -1030, -990, -950, -910, -860, -800, -290, -120, -80, -40, +0, +40, +80
- Hα 6563: -1950, -1550, -750, -600, -450, -300, -150, +0, +150, +300, +450, +600, +750, +900, +1050, +1550
- Ca II 8542: -1700, -765, -680, -595, -510, -425, -340, -255, -170, -85, +0, +85, +170, +255, +340, +425, +510, +595, +680, +765, +1700
| Instrument | Waveband | Video type |
|---|---|---|
| CHROMIS | Ca II K 3934 Å | temporal, core |
| CHROMIS | Ca II K 3933 Å | temporal, continuum |
| CHROMIS | Ca II K 3933 Å | spectral |
| CRISP | Hα 6563 Å | temporal, core |
| CRISP | Hα 6563 Å | spectral |
| CRISP | Fe I 6301/6302 Å | temporal, Stokes I, 6301 core |
| CRISP | Fe I 6301/6302 Å | temporal, Stokes V, 6301 core |
| CRISP | Fe I 6301/6302 Å | spectral |
| CRISP | Ca II 8542 Å | temporal, Stokes I, core |
| CRISP | Ca II 8542 Å | temporal, Stokes V, core |
| CRISP | Ca II 8542 Å | spectral |
Quiet Sun
This dataset was acquired 10:46:37 UT on 2016.10.12, very close to disk center, avoiding strong magnetic concentrations. The datasets is well suited to study dynamics in quiet-Sun and quiet-Sun fibrils that originate from photospheric network field concentrations.
The dataset can also be used to study properties of average spectra in quiet-Sun. 45 Ca II K scans collected with CHROMIS. Quasi-simultaneous spectro-polarimetric data were collected with CRISP in the following wavebands: 6563, 6301/6302, 8542 Å.
Disk center/quiet Sun (x = 2, y = -38)
Scans are defined by the following spectral distances in mÅ from line center:
- Ca II K 3934: -1409, -1291, -1174, -1057, -939, -822, -704, -587, -528, -470, -411, -352, -294, -235, -176, -117, -59, +0, +59, +117, +176, +235, +294, +352, +411, +470, +528, +587, +704, +822, +939, +1057, +1174, +1291, +1409 (plus continuum near 4000 Å)
- Fe I 6302: -1180, -1120, -1070, -1030, -990, -950, -910, -860, -800, -290, -120, -80, -40, +0, +40, +80
- Hα 6563: -1550, -1050, -900, -750, -600, -450, -300, -150, +0, +150, +300, +450, +600, +750, +900, +1050, +1550
- Ca II 8542: -1700, -765, -680, -595, -510, -425, -340, -255, -170, -85, +0, +85, +170, +255, +340, +425, +510, +595, +680, +765, +1700
| Instrument | Waveband | Video type |
|---|---|---|
| CHROMIS | Ca II K 3933 Å | temporal, core |
| CHROMIS | Ca II K 3933 Å | temporal, continuum |
| CHROMIS | Ca II K 3933 Å | spectral |
| CRISP | Hα 6563 Å | temporal, core |
| CRISP | Hα 6563 Å | spectral |
| CRISP | Fe I 6301/6302 Å | temporal, Stokes I, 6301 core |
| CRISP | Fe I 6301/6302 Å | temporal, Stokes V, 6301 core |
| CRISP | Fe I 6301/6302 Å | spectral |
| CRISP | Ca II 8542 Å | temporal, Stokes I, core |
| CRISP | Ca II 8542 Å | temporal, Stokes V, core |
| CRISP | Ca II 8542 Å | spectral |
Sunspot
This dataset, collected 10:57:58 on 2016.10.12, contains a vigorously active sunspot, showing strong magnetic reconnection events in its lightbridge in the form of surges.
Besides umbral shockwave propagation, and magnetic reconnection events, the observation has allowed for the study of penumbral microjets (Bühler et al. in prep.), and active region filament physics (Bühler et al. in prep.). These data include the sunspot in AR 12599 at coordinates (x=596, y = -310), viewing angle μ=0.688.
134 Ca II K scans collected with CHROMIS between 10:57 UT and 11:27 UT. Quasi-simultaneous spectro-polarimetric data were collected with CRISP in the following wavebands: 6563, 6301/6302, 8542 Å.
Scans are defined by the following spectral distances in mÅ from line center:
- Ca II K 3934: -1409, -1291, -1174, -1057, -939, -822, -704, -587, -528, -470, -411, -352, -294, -235, -176, -117, -59, +0, +59, +117, +176, +235, +294, +352, +411, +470, +528, +587, +704, +822, +939, +1057, +1174, +1291, +1409 (plus continuum near 4000 Å)
- Fe I 6302: -1180, -1120, -1070, -1030, -990, -950, -910, -860, -800, -290, -120, -80, -40, +0, +40, +80
- Hα 6563: -1550, -1050, -900, -750, -600, -450, -300, -150, +0, +150, +300, +450, +600, +750, +900, +1050, +1550
- Ca II 8542: -1700, -765, -680, -595, -510, -425, -340, -255, -170, -85, +0, +85, +170, +255, +340, +425, +510, +595, +680, +765, +1700
| Instrument | Waveband | Video type |
|---|---|---|
| CHROMIS | Ca II K 3933 Å | temporal, core |
| CHROMIS | Ca II K 3933 Å | temporal, continuum |
| CHROMIS | Ca II K 3933 Å | spectral |
| CRISP | Hα 6563 Å | temporal, core |
| CRISP | Hα 6563 Å | spectral |
| CRISP | Fe I 6301/6302 Å | temporal, Stokes I, 6301 core |
| CRISP | Fe I 6301/6302 Å | temporal, Stokes V, 6301 core |
| CRISP | Fe I 6301/6302 Å | spectral |
| CRISP | Ca II 8542 Å | temporal, Stokes I, core |
| CRISP | Ca II 8542 Å | temporal, Stokes V, core |
| CRISP | Ca II 8542 Å | spectral |
Contact
Please contact us at sst-data-request@astro.su.se
Last updated: December 14, 2022
Source: Institute for Solar Physics