Bibcode
Gelly, B.; Khalikov, S.; Pallé, P. L.; IRIS Team
Referencia bibliográfica
Structure and Dynamics of the Interior of the Sun and Sun-like Stars SOHO 6/GONG 98 Workshop Abstract, June 1-4, 1998, Boston, Massachusetts, p. 199
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1998
Número de citas
2
Número de citas referidas
1
Descripción
The IRIS network is now fourteen years old, and has continuously been
taking data since 1989. The data analysis, which produced some
noticeable scientifical results, like the measurement of the ell = 1
rotationnal splitting or the measurement of the solar acoustic cut-off
frequency, was mainly performed with the summer campaigns data of 1989
to 1992. P-mode frequency and width tables were recently published using
the same subset of the IRIS data . We are now finishing the calibration
and the timing of the whole set of IRIS data from 89 to 97, which will
increase by a factor of 4 the amount of available data. The duty cycle
of the IRIS network ranges from about 65% over 3 months of the summer
campaigns to some 23% over one year in the worst case. To improve our
duty cycle we developed several collaborations with other teams running
similar instruments: (1) the Mark I instrument, ran at the IAC for many
years, a potassium resonance single pixel device, also part of the BiSON
network (Elsworth et al., 1988). (2) Alexandro Cacciani's MOF, ran at
the JPL in Pasadena. Although this is a sodium resonance imaging
instrument, it has been used in ``one pixel'' format for several summer
seasons since 1989 (Cacciani et al., 1984). (3) the LOWL instrument is a
Doppler imager also based on a Magneto-Optical Filter (MOF), operated at
the Mauna Loa solar observatory since 1994 (Tomczyk et al., 1995). The
merging of those 'alien' data has been carefully adressed at the
calibration ands timing stages, and we can now present the advantages of
such a-posteriori collaborations. We endeavour to set-up the
corresponding database of 'one-pixel seismological data from
ground-based intruments' in Nice and to open it to the scientific
community of this meeting by the end of 1998. This database will soon
have the potential to trace the spectral features of the solar signal
over one 11-years cycle.