東北大学におけるデータベースの現状
東北大学観測チーム（八木学、小原隆博、熊本篤志、土屋史紀、鍵谷将人、米田瑞生、三澤浩昭、寺田直樹、笠羽康正、佐藤慎也）、岩井一正（NICT）、大矢浩代（千葉大）
Acknowledgement
This work is supported by Dr. Cecconi (Obspm, France)
to develop Virtual Observatory for planetary radio
observation data.

Radio & Geomagnetic Observations
LF radio wave （Ny-Alesund）

Gemagnetic data (Onagawa)LF radio wave（Athabasca）

IPRT/HF (Iitate Obervatory)
VHF wave (IPRT)

Asia VLF Observation Network(AVON)HF wave

Provided by Dr. Ohya (Chiba Univ.)

Database List
Data FormatIUGONET MDDB
(Granule update)

UDAS

IPRT/AMATERASFITS

AutomaticallyRegistered

Iitate wideband HF

CDF

AutomaticallyRegistered

Iitate narrowband
HF

Printed paper--

LFRTO(LF-STD)

CDF

Automatically

Registered

AVON

CDF

Manually

Registered

Onagawa mag

CDF

Manually --> Stop

Registereds*released by ERG-SC

Metadata(Granule) submission
Check tool for real data and metadata
Detail LOG

…

実データ
作成状況

実データ作成状況

Granule作成ツール

Low Frequency wave observation
Precipitation of high energy electrons(>100keV) into the atmosphere• In-situ particle observation– Near the magnetic equator• loss cone << FOV of the instrument– Low-altitude• Electrons in the loss cone
• Time resolution ～satellite orbital period(1~2hrs)• Ground based radio observation
High-energy electron precipitation→ Ionization in the lower ionosphere– Riometer：Absorption of galactic radio noise• ~30keV electron precipitation(contribution of high altitude absorption)– VLF, LF signal perturbation：Propagation
between the lower edge of the ionosphereand the ground (Reflection height ~ 70km)• sensitive to higher energy electrons
than the riometer observation.
• >100keV electron precipitation

Electron precipitation, ionization, and radio
wave modulation (Chevalier et al. 2007)

Low Frequency wave observation
LFRTO (Low Frequency Radio Transmitter Observation)
URL http://iprt.gp.tohoku.ac.jp/lf/cdf/ath/
・CDF Format
・Automatically submit toIUGONET MDDB・Included in UDAS
Plot by IDL (TDAS/UDAS)> thm_init> timespan,’2011-06-05’> iug_load_lfrto> tplot,[‘power_30sec’,’phase_30sec’]VLF wave observation
AVON (Asia VLF Observation Network) Tweeks dataURL http://iugonet02.gp.tohoku.ac.jp/
・CDF Format
・Included in IUGONET
Database・Included in UDAS
Plot by IDL (TDAS/UDAS)> thm_init> cdf_leap_second_init> cdf2tplot,
file=‘vlf_waveform_tnn_200
81130080000_v01.cdf‘> tplot,[1,2]VLF wave observation
Quick Look page (under development)using opensearch

date

1/25

1/26

1/27

1/28

1/29

1/30

1/31

2/1

2/2

tnn

×××××××

○

○

srb

○

○

×××××××ptk

×

○

○

○

○

○

○

○

○

2011/1/26 11:00-11:022011/2/1 11:00-11:02

2011/2/2 11:00-11:02

ptk

tnn

tnn

srb

ptk

ptk

http://iugonet02.gp.tohoku.ac.jp/avon/qltest/ql.html (公開予定)

IPRT / AMATERAS
The system consists of wide-band polarimeter and high-speed FFT spectrometer installedon the IPRT, Tohoku University. The system enables to observe the solar radio bursts in
100-500MHz with world-eminent specifications; i.e., with the sensitivity of 0.7s.f.u(solar fluxunit) and time resolution of less than 10msec. The observations have been madeeveryday.

X,Y

100-500MHzLNALH:100-500MHz
RH:950-550MHz
LH

WidebandPolarimeter RH

FFT:Spectrometer

Mixer

IPRT
Lo:1050MHz

Δt≦ 10msec
ΔS=0.7s.f.u.

Diagram of the IPRT spectro-polarimeter system

IPRT / AMATERASSPEDAS/UDAS

Type II burst?

Type III burst

GOES
X-ray

IPRT(RH) IPRT(LH)

Solar radio burst event (2015/03/15)

tlimitIitate HF wideband receiver
http://ariel.gp.tohoku.ac.jp/~jupiter/it_hf/cdf/
Location (140.40E, 37.42N)

HYB
Log-periodic
Antenna15-40MHz +28dB

Polarization

R&L

Interval
BW
Step #F range

0.5s
10kHz70015-40 MHz

Sensitivity-200dBWm-2Hz-1Precision
Data Rate
Format12 bit470MB/day
CDFPDPD

DET-6dB
DDS

10.7MHz
BW:10kHz

455kHz~ 10.245MHz

A/D
1.4kSPS
2ChPC

Observation of Jovian decametric radiation (DAM)from the ground stations
Jovian aurora (HST)
PurposeRemote sensing of ionosphere-magnetosphere-satellite
coupling processes in the Jovian magnetosphereMerits (compared to in-situ observations)
Possible to use enough facilities
Large array antenna
Receivers with high frequency & time resolutions
High-speed networks & huge storages

Demerits (compared to in-situ observations)
Artificial noises on the Earth
We need efforts to reduce/avoid them…
Possible only while the Jupiter is above the horizon
Avoidable with multi-station observation→Integrated data archives like VO will be
useful for analysis

http://apod.nasa.gov/apod/image/0012/jupiteraurora_hst_big.jpg

Iitatehttp://ariel.gp.tohoku.ac.
jp/~jupiter/

Nancayhttp://www.obs-nancay.fr/-Lereseau-decametrique-.html

Multi-station data of Jovian DAM

Yoneyama

IitateNancayJan. 3Jan. 4

Event-1
VEA-like?

Jan. 5
Event-3Vertex Late Arc(VLA)

Event-2
Vertex Early Arc(VEA)

AuroralThis
plot shown in thistalk was made by collecting data
Event-2
brightening
fromdifferent servers,and doing cut & paste.
VEA(Hisaki)
Easier way should be provided…
13

VOのRepository検索server
http://voparis-europlanet-new.obspm.fr/

VO提供Data Browser(TOPCAT)※ＤＢとも連動
RadioJove

IitateSummary- LFRTO(CDF), AVON(CDF), IPRT(FITS), andIitate HF(CDF) database are provided.
- We develop a automatic submission system foriugonet metadata(granule).
- Now we are planning to develop a Virtual
Observatory of Jovian HF radiation collaboratingwith Dr. Cecconi.