Kiruna Atmospheric- and GeophysicalObservatory (KAGO)ALIS 4D — status, possibilities and future plansUrban Brändström1 Asta Pellinen-Wannberg,2Maria Hamrin2 Peter Dalin1 Nickolay Ivchenko3
Jan Karlsson1 Johan Kero1
Natuschka Lee21
1
Thomas Leyser
Anders Lejon
Mats Luspa1
Rick McGregor1 Daria Mikhaylova1 Peje Nilsson1
Uwe Raffalski1 Fredrik Rutqvist1 Ulf Stenmark1
Csilla Szasz1 Tima Sergienko1 Peter Sköld2
Lars-Göran Vanhainen1 Masatoshi Yamauchi1 . . .
1 Swedish Institute of Space Physics (KAGO, STAR)
2 University of Umeå (Physics, EMG, ArcUm)
3 KTH Royal Institute of Technology

Swedish Space Plasma meeting, 2018

Swedish Institute of Space Physics
New organisation from 2018

I PAF + STP ⇒ STAR, Solar Terrestrial and AtmosphericResearch (Head: Johan Kero)I KGO ⇒ KAGO Kiruna Atmospheric and GeophysicalObservatory: Urban Brändström (head), Daria Mikhaylova,
Lars-Göran Vanhainen and Uwe Raffalski
I Uwe Raffalski is responsible for atmospheric measurements

within KAGOI Ozone radiometer (KIMRA) became observatory instrument

2018.

KAGO
Kiruna Atmospheric and Geophysical Observatory

I Magnetometers, 1950–
I Allsky cameras, 1956–
I Ionosondes, 1952–
I Riometers, 1958–
I Infrasound, 1973– (In observatory since 2015)
I Ozone radiometer (KIMRA), 2001– (In observatory since 2018)
I ALIS 4D (Observatory measurements from fall 2019)
I (Weather station, ALIS, guest instr.)

Geomagnetic observations
Kiruna, Lycksele and Tormestorp
I PI: Masatoshi Yamauchi
I Kiruna: timeseries 1950–

2 Variometers (DMI-FGE91) and EDA (backup)
2 Proton magnetometers (Gemsys)
I 2 DI-flux teodolites
I Plans for 2018II

Solve baseline issuesSolve noise issues with new proton magnetometer
I Upgrade observatory to INTERMAGNET 1 s standard.
I Replace at least one variometer with a more moderninstrumentII

I Lycksele (in cooperation with SGU): timeseries 1957–

2 Variometers
Proton (Gemsys) I DI-flux teodolite
II

I Tormestorp (Hässleholm): variometer (DTU-FGE) 2018–
I Abisko and Uppsala PI Gerhard Schwarz (Owned andoperated by SGU)

Geomagnetic observatory
KirunaGeomagnetic observations
Hosted Nordic Comparision meeting 2017

Geomagnetic observations
FGE-91 cal. in Nurmijärvi

Riometers
Kiruna and Lycksele

I PI/Project leader: Tima Sergienko/Daria Mikhaylova
I IRFs first scientific publication on polar cap absorption.
I Instruments: La Jolla Sciences (“blue box”)
I Kiruna: timeseries since 1958
II

30 MHz and 38 MHz
New SDR-riometer during 2018 (RF-Shamaanit)

I Lycksele: timeseries since 1958
I

38 MHzI GloRiA http://spears.lancs.ac.uk/gloria/
I Delivers data to Aviation Civile, France, ICAO 24/7 service(2018–)

Ionosondes
Kiruna, Lycksele and Uppsala

I PI: Thomas Leyser
I Kiruna: timeseries since 1957 (first ionograms 1948!)
I

Vertical Incidence Pulsed Ionospheric Radar, (VIPR) delivered
fall 2016. Running since December 2016.

I Lycksele: timeseries since 1957
I

Old ionosonde 4 ionograms/hour.

I Uppsala: timeseries: since 1952

Old ionosonde 4 ionograms/hour. Urgent need for new
instruments
I New ionosonde procured during 2018
I

Ionosondes
KirunaInfrasoundKiruna, Jämtön, Lycksele and Sodankylä

I PI: Johan KeroI Objective: Infrasound detection and triangulation
I Kiruna: Timeseries since 1973II

Kiruna: microphones (old and new)Four microbarographs from CEA, France

I Jämtön:
I

Microphones (old and new)

I Lycksele:
I

Microphones (old and new)

I Sodankylä (moved from Uppsala)I

Microphones (old to be upgraded)InfrasoundAll-sky cameras
Kiruna and Abisko

I PI: Urban Brändström
I Objective: Sky overview during dark hours. (Colour imaging

each minute during dark periods).
I Kiruna: timeseries 1956–2004 (film) 2001– (digital)
II

Nikon D700, Nikkor 8mm.
To be replaced with a Sony α7s

I Abisko (STF tourist station)
I

Guest instrument from Hiroshima University, (Nishi-san)All-sky cameras
KirunaIRF MagnetokeogramMeteor cameras
Abisko, Kiruna, Sodankylä and UmeåI PI: Eric Stempels (UU) (IRF: Johan/Urban)
I Objective: Sky overview. (B/W video imaging 24/7) meteor

detection
I Kiruna and Abisko part of Swedish Meteor Imaging network
I Abisko:
I Kiruna:
I Sodankylä:I Umeå: (UmU)
I Time-series: 2015–
I More cameras planned

ISEE/NIPR cameras
100 Hz EMCCD and four channel auroral imagers

ISEE/NIPR

Optical absolute calibration

ALIS 4DA Swedish contribution to complementary instruments for EISCAT 3D

ALIS 4D
A Swedish contribution to complementary instruments for EISCAT 3D

I High-speed narrow-band imaging of aurora, RIOE, meteor

trails, . . .
I Observatory modes (long-time monitoring)
I The string “optic” occurs 46 times in 122 pages
I Table 1 “EISCAT 3D radar performance requirements” p.

107–109: Optics required in 70 % (16 of 23) science topics .
Optical measurements are a requirement for EISCAT 3D!
new-moon periods are popular! (Gustavsson, present EISCAT)
There are many clear solid scientific objectives for optical
instruments!

AILS 4D
A Swedish contribution to complementary instruments for EISCAT 3D
I High-rime resolution (> 25 FPS)
I Continuous operation (observatory modes)
I Status

2016: (summer) Funding application (granted in November)
2017: Procurement procedures, four imagers delivered, optics
orderedI 2018: Optics delivery (April) Main development work. Tests infall.
I 2019: Continuous operations from fall. Ground support forSPIDER2 rocket.
II

I Funded by Kempestiftelserna, Department of Physics at UmUand IRF.
I PIs Urban Brändström (IRF), Asta Pellinen-Wannberg (UmU)

ALIS 4D sites

ALIS/ALIS 4D
Comparision

FoVResTime
Mode

Sort of an Àttje

ALIS
4 CCD ≈ 60◦
1 EMCCD ≈ 30◦(1 EMCCD ≈ 15◦ )10242 ≈ 100m
2562 ≈ 500m
12 FPM
Campaign only

ALIS 4D phase II
4 EMCCD ≈ 150◦
1 EMCCD ≈ 30◦(1 EMCCD ≈ 15◦ )10242 ≈ 750m
5122 ≈ 1.5km> 25 FPS
monitoring/campaign

ALIS/ALIS 4D
Available filters

λ [Å]
3950
4227
4340.54278
4861.3
5100
5577
5893
6230
6300
6562
6562.8
6750
8000
8446

∆λ [Å]92280
255025404020040407025200
100040Line
Ca, FeCa, Fe, H2 O, . . .
Hγ , Balmer series
N+2 1Neg.
Hβ , Balmer seriesO(1 S)
Na, . . .
O(1 D)
HαHα , Balmer series
N2 1P
OH MeinelO(3p3 P)

Remarks
Meteors
Meteors
Meteors
Aurora/Airglow
Meteors
Background
Aurora/Airglow
Meteors
Background
Aurora/Airglow
SPIDER
Meteors
SPIDER/LEEWAVES
Airglow LEEWAVES
Aurora/Airglow (O(3p3 P))#111614614641444ALIS 4D
Sensitivity and speed

ALIS (CCD)
ALIS (CCD)
ALIS (CCD)
ALIS 4D (EMCCD)ALIS 4D (EMCCD)

Res.
10242
2562
2562
10242
10242

Hz
0.04
0.2
0.2
16.5
25

R/count
13.4
0.78
1.74
60.5

λc
5577Å
5577Å
4278Å
5577Å
5577Å

Data production“Harddisks are either new or full” Gustavsson

Hz
0.1
0.1
0.1
111
25
25
25

resolution
2562
5122
10242
2562
5122
10242
2562
5122
10242

GiB/h
0.02
0.09
0.35
0.22
0.9
3.5
1144176

total GiB/h
0.09
0.4
14.1
0.88
3.51
14.06
44176
703

GiB/night1
622
1456
225
352
1406
5625

Summary

I ALIS 4D will be a powerful swedish contribution tocomplementary instruments for EISCAT 3D.
I Extensive upgrades of the observatory instrumentation

underway at IRF. New Ionosonde (Uppsala), Riometer andvariometer Kiruna (Also including atmospheric measurements)
I We have a very nice collaboration with Umeå University!
I . . . and of course also with KTH, SPIDER2 coming up!