J/A+A/390/717 Solar Velocities of the Sun in 1989-99 (IRIS++) (Salabert+, 2002)
IRIS++ database: Merging of IRIS + Mark-1 + LOWL
Salabert D., Fossat E., Gelly B., Tomczyk S., Palle P.L.,
Jimenez-Reyes S.J., Cacciani A., Corbard T., Ehgamberdiev S., Grec G.,
Hoeksema J.T., Kholikov S., Lazrek M., Schmider F.X.
<Astron. Astrophys. 390, 717 (2002)>
=2002A&A...390..717S 2002A&A...390..717S
ADC_Keywords: Sun ; Radial velocities
Keywords: Sun: instruments - Sun: signal analysis - Sun: database -
Sun: helioseismology
Abstract:
The IRIS (International Research of Interior of the Sun) network has
been operated continuously since July 1st 1989. To date, it has
acquired more than a complete solar cycle of full-disk helioseismic
data which has been used to constrain the structure and rotation of
the deep solar interior. However, the duty cycle of the network data
has never reached initial expectations. To improve this situation,
several cooperations have been developed with teams collecting
observations with similar instruments. This paper demonstrates that
we are able to merge data from these different instruments in a
consistent manner resulting in a very significant improvement in
network duty cycle over more than one solar cycle initiating what
we call the IRIS++ network.
Description:
The precise measurement of the solar seismic properties requires year
long measurements as uninterrupted as possible. The cooperation
between several groups managing instruments all around the world has
produced the one solar cycle long IRIS++ data bank. Integrated radial
velocities from mid-1989 up to end-1999 measured by the ground-based
IRIS++ network are presented. The full-disc integration gives access
to low degree p-modes (l=0, 1, 2 & 3).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
v89f.dat 35 352142 Year 1989 pre-merged
v90f.dat 35 699609 Year 1990 pre-merged
v91f.dat 35 699101 Year 1991 pre-merged
v92f.dat 35 701963 Year 1992 pre-merged
v93f.dat 35 325813 Year 1993 pre-merged
v94f.dat 35 696614 Year 1994 pre-merged
v95f.dat 35 698556 Year 1995 pre-merged
v96f.dat 35 702161 Year 1996 pre-merged
v97f.dat 35 698622 Year 1997 pre-merged
v98f.dat 35 699232 Year 1998 pre-merged
v99f.dat 35 668952 Year 1999 pre-merged
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See also:
http://www-astro.unice.fr/iris : IRIS network web server
http://www-astro.unice.fr/iris/Irisdata/Distri_1.1/page.html :
A documentation to explain the structure and the contain
of IRIS++ database "A short notice on the IRIS++ database"
Byte-by-byte Description of file: v*.dat
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Bytes Format Units Label Explanations
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1 - 12 F12.6 d MJD Modified Julian Date (sampling 45 seconds) (1)
14- 22 F9.6 m/s Res ?=0.000000 Radial velocity (2)
23- 29 F7.2 --- Trans ?=0.00 Transparency coefficient (2)
31- 34 I04 --- Ind ?=0000 Index of information redundancy (3)
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Note (1): The first point in each file corresponds to the first observing
point, and not to the beginning of each year.
Low-frequencies are high-pass filtered, the cutoff frequency being at
1.1 mHz.
The integer part of the value is the number of days elapsed since
Nov 17, 1858 at 0 UT, and the fractional part is the UT fraction of
day. A 64 bits data format allows to store the MJD with a resolution
better than 1 sec which is quite enough for us. MJD is deduced from
the classical Julian Date by subtracting 2400000.5 days to the JD.
Note (2): The missing points have a value of zero.
Note (3): The last column is a synoptic index indicating how many sites
have contributed to the corresponding data points. Each site used in
the merging sets a given bit inside a 16 bits integer word.
The bits meaning is as follow:
Bit # Value Site
1 1 MK = Izana [Tenerife, Spain] Mark-1 instrument
2 2 IZ = Izana [Tenerife, Spain] IRIS instrument
3 4 KU = Kumbel [Uzbekistan] IRIS instrument
4 8 LA = La Silla [Chile] IRIS instrument
5 16 CU = Culgoora [Australia] IRIS instrument
6 32 OU = Oukaimden [Morocco] IRIS instrument
7 64 NI = Nice [France] IRIS instrument
8 128 ST = Stanford [California, USA] IRIS instrument
9 256 JP = Jet Prop Lab [California, USA] Cacciani's MOF instrument
10 512 ML = Mauna Loa [Hawaii] LOWL instrument
11 1024 PK = Parkent [Uzbekistan] IRIS instrument
hence, a data point merged from Izana alone would have a value of 2,
and a data point merged from the Oukaimden IRIS site (OU) and the LOWL
site (ML) would have a value of 544.
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Acknowledgements: David Salabert
The IRIS group is grateful to BiSON, IAC and HAO for sharing the Mark-1 data
(prepared by P. Palle and S.J. Jimenez-Reyes) and LOWL data (prepared by
T. Corbard and S. Tomczyk).
References:
Fossat E., 1992A&A...263..443F 1992A&A...263..443F, IRIS data merging
I. A solution to minimize the low and intermediate frequency noise
Gelly B., 1991, Solar Physics 133, 31, The IRIS data management
Grec G., Fossat E., Gelly B., Schmider F.X., 1991, Solar Physics 133, 13,
The IRIS sodium cell instrument
Isaak G.R., McLeod C.P., Palle P.L., et al., 1989A&A...208..297I 1989A&A...208..297I
Solar oscillations as seen in the NaI and KI absorption lines
Palle P.L., Fossat E., Regulo C., et al. 1993A&A...280..324P 1993A&A...280..324P
Full-disk helioseismic IRIS raw data calibration
Tomczyk S., Cacciani A., Veitzer S.A., 1993, in GONG 1992. Seismic
Investigation of the Sun and Stars. Proceedings of a Conference held in
Boulder, Colorado, August 11-14, 1993. Editor, Timothy M. Brown; Publisher.
LOWL - An instrument to observe low-degree solar oscillations
(End) David Salabert [Univ. Nice-Sophia Antipolis, France] 24-May-2002