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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
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:
FileName Lrecl Records Explanations
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
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
Bytes Format Units Label Explanations
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)
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.
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, 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 Solar oscillations as seen in the NaI and KI absorption lines Palle P.L., Fossat E., Regulo C., et al. 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
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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