INTERNATIONAL   EARTH   ROTATION   SERVICE   (IERS)

SERVICE   INTERNATIONAL   DE   LA   ROTATION   TERRESTRE

           

SERVICE DE LA ROTATION TERRESTRE                                                             RAPID SERVICE/PREDICTION CENTRE

OBSERVATOIRE DE PARIS                                                                                      U.S. NAVAL OBSERVATORY

61  Av. de l'Observatoire                                                                                               3450 Massachusetts Avenue, NW

75014 PARIS (France)                                                                                                  WASHINGTON, DC  20392-5420 (USA)

Tél.          : 33 (0) 1 40 51 22 26                                                                                    1 202 762 0060

FAX        : 33 (0) 1 40 51 22 91                                                                                    1 202 762 1563

Internet    : iers@obspm.fr                                                                                             ser7@maia.usno.navy.mil

 

 

August 2004

 

 

 

EXPLANATORY SUPPLEMENT

 

TO IERS BULLETINS A AND B

 

 

 

     IERS Bulletins A and B provide current information on the Earth's orientation in the IERS Reference System.  This includes Universal Time, coordinates of the terrestrial pole, and celestial pole offsets.  Bulletin A gives an advanced solution updated weekly by e-mail subscription or daily by anonymous ftp; the standard solution is given monthly in Bulletin B. The Annual Report contains information on the data used, the models, the algorithms, and the reference frames, as well as revised solutions for the past years. All solutions are continuous within their respective uncertainties.  Bulletin A is issued by the IERS Rapid Service/Prediction Centre at the U.S. Naval Observatory, Washington, DC and Bulletin B is issued by the IERS Earth Orientation Centre at the Paris Observatory.

 

     Bulletin A is intended for users who need accurate information before the Bulletin B “finals” series is available, i.e., those who reduce data in the very recent past (require rapid service) or those who operate in real-time (require predictions).  Bulletin B is intended for standard use.  For scientific and long-term analyses of the Earth's orientation, users are advised to request the long-term continuous series maintained by the Earth Orientation Centre from 1846 (pole components), 1962 (UT), and 1981 (dPsi, dEpsilon) to the current date.  All solutions are available electronically (see Section VIII).

 

    Resolutions adopted at the 24th General Assembly of the International Astronomical Union (IAU) recommend the implementation of new procedures concerning the transformation between the celestial and terrestrial reference systems: adoption of a new precession/nutation model (IAU 2000), a new celestial pole (the Celestial Intermediate Pole), and a new transformation between the terrestrial and celestial systems defining UT1 as directly proportional to the Earth rotation angle. These resolutions were implemented in Bulletins A and B on January 1, 2003 and are discussed below. 

   

 

 

 

I.  THE IERS CONVENTIONS

 

     The IERS uses the following conventions:

 

   A. The International Celestial and Terrestrial Reference Systems

 

   The International Celestial and Terrestrial Reference Systems (respectively ICRS, ITRS) are defined by their origins, directions of axes and, in the case of the ITRS, length unit.  The ICRS is described by Arias et al. (1995).  Its origin is at the barycenter of the solar system.  The directions of its axes are fixed with respect to the quasars to better than +/- 20 micro-arcseconds; they are aligned with those of the FK5 within the consistency of the latter (+/- 80 milliarcseconds at epoch J1991.25 (van Leeuwen et al., 1997).  The ICRS is realized by estimates of the coordinates of a set of extragalactic sources:  the International Celestial Reference Frame (ICRF) (Ma and Feissel, 1997; Ma et al., 1998).  According to Resolution B2 of the International Astronomical Union (IAU)  23rd General Assembly (Kyoto, 1998), after 1 January 1998 the IAU celestial reference system is the International Celestial Reference System (ICRS) as defined by the International Earth Rotation Service (IERS) and the corresponding fundamental reference frame is the ICRF constructed by the IAU Working Group on Reference Frames.  The IERS was asked to monitor the maintenance of the ICRS and its ties to the reference frames at other wavelengths.  In the present IERS structure, two groups share this task: the International VLBI Service for Geodesy and Astrometry (IVS) and the IERS ICRS Centre, which is jointly operated by the Paris Observatory and the U.S. Naval Observatory.

 

    The ITRS origin is at the center of mass of the entire Earth system, including the oceans and the atmosphere.  Its length unit is the meter (SI), consistent with the TCG time coordinate for a geocentric local frame.  The orientation of its axes is consistent with that of the BIH System at 1984.0 within +/- 3 milli-arcseconds.  The International Reference Meridian (IRM) is implicitly defined through the adoption of the set of coordinates of stations realizing the ITRF.

    Its time evolution in orientation is such that it has no residual rotation relative to the Earth's crust.  The ITRS is realized by estimates of the coordinates and velocities of a set of observing stations, the International Terrestrial Reference Frame (ITRF).  For more details, see Boucher et al. (1996) and the IERS Conventions (2003) (McCarthy and Petit, 2004). A new ITRF realization (ITRF2000) is now available (http://lareg.ensg.ign.fr/ITRF/).

 

   B. IERS constants and models

 

   The IERS Conventions (2003) (McCarthy and Petit, 2004) are a set of constants and models used by the IERS Technique and Analysis Centres for Very Long Baseline Interferometry (VLBI), Global Positioning System (GPS), satellite radio positioning (DORIS), Satellite Laser Ranging (SLR), and by the IERS Product Centres in the combination of results.

 

     The values of the constants are adopted from recent analyses.  In some cases, they differ from the current IAU and International Association of Geodesy conventional ones.  The models are, in general, the best estimates of the specialists in the field.   Observations have shown that there are deficiencies in the IAU 1976 Theory of Precession and the IAU 1980 Theory of Nutation.  As a result the IAU has adopted the IAU 2000 precession-nutation model (see IERS Conventions (2003) [McCarthy and Petit, 2004]).  This model was implemented by the IERS as of 1 January 2003.

 

II.  TIMESCALES USED IN BULLETINS a AND b

 

    TAI is the atomic time scale calculated by the BIPM.  Its unit interval is exactly one SI second at mean sea level.  The origin of TAI is such that UT1-TAI was approximately 0 on 1 January 1958.  The instability of TAI is about six orders of magnitude smaller than that of UT1.

 

    UTC is defined by the International Radio Consultative Committee (CCIR) Recommendation 460-4 (CCIR, 1986).  It differs from TAI by an integral number of seconds in such a way that UT1-UTC remains smaller than 0.9s in absolute value.  The decision to introduce a leap second in UTC to meet this condition is the responsibility of the IERS; it is announced in Bulletin C.  According to the CCIR Recommendation, first preference is given to opportunities at the end of June and December and second preference to those at the end of March and September.  Since the system was introduced in 1972, only dates in June and December have been used.

    

    A new definition of UTC is under discussion by the IAU and the International Telecommunication Union, but no action is anticipated before 2006. 

 

 

 

III.  THE EARTH ORIENTATION PARAMETERS, DEFINITION BEFORE JANUARY 1, 2003

 

 

     The IERS Earth Orientation Parameters (EOP) describe the rotation of the ITRS relative to the ICRS, in conjunction with the conventional Precession-Nutation model.

 

A. The coordinates of the Celestial Ephemeris Pole (CEP) relative to the International Reference Pole (IRP) are defined as x and y.  The CEP differs from the instantaneous rotation axis by quasi-diurnal terms with amplitudes under 0.01" (see Seidelmann, 1982).  The x-axis is in the direction of the IERS Reference Meridian (IRM), the y-axis is in the direction 90 degrees West longitude.

 

B.  UT1 is the rotation angle about the pole.  It is defined by a conventional relationship between the origins of the terrestrial and celestial reference frames (Capitaine et al., 2000, Capitaine et al., 2003, McCarthy and Petit, 2004).  This relationship was developed to maintain consistency with the previous defining relationship (Aoki et al., 1982).  It gives access to the direction of the International Reference Meridian (IRM) in the ICRS, reckoned around the CEP axis.  It is expressed as the difference UT1-TAI or UT1-UTC.

 

   

    DUT1 is the difference UT1-UTC expressed with a precision of +/- 0.1s; it is broadcast with the time signals and announced in Bulletin D.  The changes in DUT1 are decided by the IERS.

 

    The difference between the astronomically determined duration of the day (D) and 86400s of TAI, is called length of day (LOD).  Its relationship with the angular velocity of the Earth, Omega, is:

 

            Omega = 72 921 151.467064 - 0.843994803 D, where Omega is in picoradians/s and D in ms.

 

    UT1, hence D and Omega, are subject to variations due to zonal tides.  The model, which is a part of the IERS Conventions, includes 62 periodic components with periods ranging from 5.6 days to 18.6 years. UT1R, DR, and OmegaR are the values of UT1, D, and Omega corrected for the short-term part of the model by Yoder et al. (1981), i.e., the 41 components with periods under 35 days.  In absolute value UT1R-UT1 is smaller than 2.5 ms, LODR-LOD is smaller than 1 ms.  As recommended in IERS Gazette #13 (McCarthy and Gambis, 1997), IERS Earth orientation data are produced at daily intervals and do not include the effects of semidiurnal and diurnal variations; Ray's model has been adopted for interpolation.  The corresponding numerical program is available from either Centre’s ftp site, see McCarthy and Gambis (1997) for details.

 

C.  The IERS continues to provide the offset in longitude dDy1980 and in obliquity dDe1980 with respect to the IAU 1976 Theory of Precession and the IAU 1980 Theory of Nutation. Following the implementation of the IAU 2000 precession-nutation model in 2003, however, the IERS also provides offsets with respect to this model.  The offsets dDy1980 and dDe1980 are labeled dpsi and deps in the released IERS EOP Bulletin A, and Bulletin B.

 

IV.  THE EARTH ORIENTATION PARAMETERS, DEFINITION AFTER JANUARY 1, 2003

 

 

A.  New parameterization of the Earth orientation

 

     The most important changes are those introduced by IAU Resolutions B1.6 (IAU 2000 Precession-Nutation Model), B1.7 (Definition of Celestial Intermediate Pole), and B1.8 (Definition and Use of Celestial and Terrestrial Ephemeris Origins).  The new precession-nutation model is accompanied by a new formulation for the transformation between the celestial (CRS) and terrestrial (TRS) reference systems in the form recommended in the IERS Conventions (2003) (McCarthy and Petit, 2004):

 

,

 

in which , and  are time-dependent transformation matrices to account for the precession-nutation, proper rotation of the Earth about the axis corresponding to CIP, and polar motion, respectively:

 

, and

 

.

 

The Earth rotation angle between the CEO and TEO is given as function of UT1 by a simple linear relation:

 

q(Tu) = 2p(0.779 057 273 264 0 + 1.002 737 811 911 354 48 Tu)

 

where  .

 

Here  and  describe the position of the Celestial Intermediate Pole (CIP) and the Celestial/Terrestrial Ephemeris Origins (CEO, TEO) in the Geocentric Celestial Reference System (GCRS) and International Terrestrial Reference System (ITRS), respectively (see http://maia.usno.navy.mil/ch5tables.html). The developments of X, Y, and s into Poisson series, based on the IAU 2000A precession/nutation model, are published by Capitaine et al. (2003) and are available in the IERS Conventions (2003). Expressions for the classical transformation based on the new IAU 2000 model have been developed to be equivalent in the new transformation (IERS Conventions (2003)).

 

1) Celestial pole offsets

Precession-nutation is referred to the CIP that exhibits, by definition, only long-periodic motions with periods of two days and longer in space.  The IERS provides the celestial pole offsets dX2000 and dY2000 referred to the new model IAU 2000 following the new formalism and the quantity s.  Classical nutation angles, the celestial pole offsets in longitude and obliquity (dDy2000 , dDe2000), respectively, referred to the new model can be easily derived from (dX2000 , dY2000) using equations 23 in Chapter 5 of the IERS Conventions (2003) or the relative Fortran subroutine dXdY_dpsideps included in the package, uai2000.package (see next paragraph for its availability).  These values dX and dY are now smaller than 1 mas, reflecting mostly the effect of the Free Core Nutation (FCN) that is not predictable and therefore not incorporated into the new model.  The position of the CEO, given by s, is insensitive to any small change of the precession-nutation at the level of one mas, so only its model values are to be used (http://maia.usno.navy.mil/ch5tables.html).  In parallel with these values, the values of the ‘classical’ celestial pole offsets dDy1980 and dDe1980 referred to the old IAU 1976 Precession and 1980 Nutation model are also being published in Bulletin A and Bulletin B.

 

2) Polar motion

Polar motion is not affected by adopting the IAU 2000 resolutions.  Polar motion contains (relatively small) diurnal and sub-diurnal terms, due to ocean tides and high-frequency nutation terms.  These are not part of the polar motion values published by the IERS at daily intervals; they are represented by a model (IERS Conventions (2003), Chapters 5 and 8) and should be added after interpolation.  The Earth Orientation Centre makes available a Fortran subroutine for such an interpolation (ftp://hpiers.obspm.fr/eop-pc/models/interp.f).  The position of the TEO, given by s’, depends on the actual polar motion but the value of s’ is so small that a simple linear approximation (Lambert and Bizouard, 2002) is sufficient:

 

s' = - 47 mas (t - 51544.5) / 36525   where t is expressed in modified Julian days (MJD).

 

3) Universal Time

UT1-UTC is theoretically not affected by the resolutions.  Although UT1 is now directly linked to the Earth rotation angle through the linear relation above, the positioning of CEO (represented by the quantity s) and IAU2000 expressions between sidereal time and universal time UT1 are such that continuity in UT1 is ensured at the epoch of change from the old system.

There are short-periodic (diurnal, semi-diurnal) variations in UT1 due to ocean tides that are treated similarly to polar motion (the IERS publishes the daily values from which these terms have been removed, and they are to be added back after the interpolation).

B.  Availability of new products and models

Since January 2003, the IERS Rapid Service/Prediction Centre and IERS Earth Orientation Centre have been publishing Bulletin A and Bulletin B containing dX and dY with respect to IAU 2000A precession/nutation model in parallel to the current issue containing (dDy, dDe)1980.

The new Bulletin A files are available at the following ftp sites:

- anonymous ftp: maia.usno.navy.mil

   files : /ser7/finals2000A.daily

      /ser7/finals2000A.data

The new Bulletin B files are available at the following Web/ftp sites:

- Web:

   http://hpiers.obspm.fr/eoppc/bul/bulb/

 

- anonymous ftp:  hpiers.obspm.fr         

   files : / eoppc/bul/bulb/          

          

C.  Fortran subroutines

1) Transformation of (dX, dY)2000 to (dDy, dDe)1980 or (dDy, dDe)2000 and inversely are available in Fortran 77/90 at :

- Web page:

 http://hpiers.obspm.fr/eop-pc/models/models.html#software

Files:  

            - ftp://hpiers.obspm.fr/eop-pc/models/uai2000.package

            - ftp://hpiers.obspm.fr/eop-pc/models/uai2000.package.readme

 

- anonymous ftp:  hpiers.obspm.fr

   files : /eop-pc/models/uai2000.package

            /eop-pc/models/uai2000.package.readme         

 

2) Interpolation of Polar Motion at hourly scale

- Web:  http://hpiers.obspm.fr/eop-pc/models/models.html#software

 Files:  

            - ftp://hpiers.obspm.fr/eop-pc/models/interp.f

- ftp://hpiers.obspm.fr/eop-pc/models/interp.readme

 

 

 

V.  THE DATA ANALYSIS

 

 

The data analysis that yields the values of the EOP published in Bulletins A and B includes several steps that are summarized below.

 

1. The individual Technique Centres coordinated the observations made using the VLBI, SLR, GPS, and DORIS networks.

 

2. Analyses (operational and refined) are done by the Analysis Centres of the Technique Centres.  The operational results are transmitted in parallel to the IERS Rapid Service/Prediction Centre to contribute to Bulletin A and to the IERS Earth Orientation Centre to contribute to Bulletin B.  The operational results are also archived at each centre.  The refined results are computed yearly. 

 

3. The IERS Rapid Service/Prediction Centre performs additional processing of operational results.  The IGS GPS satellite orbit data are used to estimate a GPS UT1-like quantity, and atmospheric angular momentum (AAM) analysis and forecast data from NOAA and the IERS Global Geophysical Fluid Center’s Special Bureau of the Atmosphere are used to estimate an AAM UT1-like quantity.

 

4. General adjustment of ICRF, ITRF, and EOP by the IERS Product Centres are based on the refined annual results.  This adjustment, described in the IERS Annual Report provides the basis for determining the systematic corrections to be added to the individual series in order to bring them into the IERS Reference System.  These corrections are used in step 6.  The general results are published in the IERS Annual Report and long-term monitoring results were given by Gambis (2000).

 

5.  Determination of EOP by the IERS Rapid Service/Prediction Centre is in the form of slightly smoothed solutions at one-day intervals.  This involves the application of systematic corrections and statistical weighting.  The accuracy of this solution is given in Table 1.  The results are published in Bulletin A with a delay of about 18-hours between the date of publication and the last available date with estimated EOP.  The details of the procedure are outlined in McCarthy and Luzum (1991a).

 

6.  Determination of EOP by the IERS Earth Orientation Centre is in the form of combined solutions derived from the individual series.  Various solutions are computed: normal values at five-day intervals and slightly smoothed solutions at one-day and five-day intervals.  In the procedure systematic corrections determined in step 4 and statistical weighting is applied.  The accuracy of these solutions is given in Table 1.  The results are published in Bulletin B with a delay of thirty days between the date of publication and the last date of the standard solution.

7.  Bulletins A provides predictions of the EOP while Bulletin B gives an extrapolation of the standard solution. Details of the procedure used for Bulletin A are given in McCarthy and Luzum (1991b) .  Their performances are given in Table 1.

 

 

 

 

Table 1: Precision of the current solutions.  The accuracy which includes the uncertainty of the tie to the IERS System can be estimated by adding quadratically 0.0002" in terrestrial pole, 0.00003s in UT1, and 0.0002" in celestial pole.

 

 

 

Solutions

 

 

Terrestrial Pole

 

UT1

 

Celestial Pole

 

 

0.001"

0.0001s

0.001"

Bulletin A daily

 

Prediction

 

 

1d

5d

10d

20d

40d

90d

0.1

 

0.6

2.6

4.8

9.0

16.1

25.6

0.2

 

1.1

4.2

8.8

20.3

49.9

125.0

 

0.3

 

0.3

0.3

0.3

 

0.3

 

 

 

 

 

 

Bulletin B

daily

 

  0.1

 0.2

0.3

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

VI.  CONTENTS OF BULLETINS A AND B

 

 

A.  BULLETIN A (weekly and daily)

 

General information including key definitions and the most recently adopted values of DUT1 and TAI-UTC.

 

Quick-look daily (finals.daily) and weekly (finals.all and finals.data) estimates of the EOP are determined by combining the most recently available observed and modeled data (including VLBI 24-hour and intensive, GPS, and AAM).  The combination process involves applying systematic corrections and slightly smoothing in order to remove the high frequency noise.  The SLR data type is updated for the weekly estimates.

 

The daily solutions contain predictions of x, y, and UT1-UTC daily up to 90 days following the last day of data in Section 4, while the weekly solutions contain predictions of x, y, UT1-UTC daily up to 360 days following the last day of data and smoothed daily values of celestial pole offsets.  The results are published with a delay of about 18-hours between the date of publication and the last available date with estimated EOP.

 

To bring the Bulletin A (weekly and daily) EOP solutions in compliance with IAU 2000 resolutions, additional files (finals2000A.daily and finals2000A.data) are available which contain dX and dY with respect to IAU 2000A precession/nutation theory.

 

 

 

B.  BULLETIN B (Monthly)

 

Section 1:  Five days sampling of section 2.  Final Bulletin B values over one month and provisional extension over the next three months.

 

Section 2: Smoothed values of x, y, UT1-UTC, UT1-UT1R, dDy, and dDe at one-day intervals and provisional extension from the last Final Bulletin B value based on a combination of the series presented in section 6. What is the degree of smoothing?

 

Section 3:  Five-day normal values of x, y, UT1-UTC, dDy, and dDe (EOP(IERS) C02), and their uncertainties and provisional extension from the last Final Bulletin B value based on a combination of the series of section 6.  New class of robust M-Huber estimators is used in the analysis procedures (Bougeard et al., 2000).

 

Section 4:  Smoothed values of DR and OmegaR, with the same degree of smoothing as UT1R-UTC.

 

Section 5:  Information on the time scales and announcement of the leap seconds.

 

Section 6: Average precision of the individual series contributing to the combination and their agreement with the combination.

 

 

 

 

VII.  INDIVIDUAL SERIES CONTRIBUTING TO IERS BULLETINS A AND B, JANUARY 2004

 

Table 2 gives the estimated accuracy with respect to IERS C04 of these series over 2003-2004 after removal of systematic variations, mainly a bias.  The IERS C04 series is maintained by the IERS Earth Orientation Centre (see EOP Combined Series at http://hpiers.obspm.fr/eop-pc/ for details).

 

 

Table 2: Estimated accuracies of individual solutions entering the combined solutions in 2003-2004.

 

 

 

 

 

 

              Estimated uncertainties

Individual solutions

 

 

 

Time

Terrestrial Pole

 UT1        LOD

Celestial Pole

 

 

 

 

 

0.001"

 0.0001s

0.001"

VLBI - 24 h

 

 

 

 

 

 

 

EOP (AUS)      

01

R

01

  3-4d

0.20

0.05

0.12

EOP (BKG)      

03

R

04

  1-4d

0.22

0.05

0.15

EOP (GSFC)    

03

R

06

  1-4d

0.16

0.04

0.10

EOP (IAA)       

03

R

04

  1-4d

0.14

0.04

0.08

EOP (MAO)    

03

R

01

  1-4d

0.21

0.05

0.17

EOP (SPBU)    

03

R

03

  3-4d

0.22

0.05

0.13

EOP (USNO)    

03

R

04

  1-4d

0.15

0.04

0.13

 

 

 

 

 

 

 

 

VLBI - Intensive

 

 

 

 

 

 

 

EOP (BKG)      

03

R

02

1-3 d

 

0.13

 

EOP (GSFC)    

03

R

05

1-3 d

 

0.12

 

EOP (IAA)       

03

R

03

1-3 d

 

0.13

 

EOP (SPBU)    

02

R

01

1-3 d

 

0.14

 

 

 

 

 

 

 

 

 

Satellite Laser Tracking

king

 

 

 

 

 

 

EOP (ASI)      

03

L

02

   1d

0.30

                  2.33

 

EOP (CSR)     

95

L

01

   3d

0.66

1.15    

 

EOP (DUT)    

98

L

01

   3d

0.56

 

 

EOP (IAA)     

02

L

02

   1d

0.27

0.27 *        0.13

 

EOP (MCC)   

97

L

01

   1d

0.30

                  0.48

 

 

 

 

 

 

 

 

 

GPS

 

 

 

 

 

 

 

EOP (CODE)

98

P

01

   1d

0.06

                   0.26

 

EOP (EMR)

96

P

03

   1d

0.10

                   0.31

 

EOP (ESOC)      

96

P

01

   1d

0.13

                   0.25

 

EOP (GFZ)        

96

P

02

   1d

0.09

                   0.29

 

EOP (IAA)        

01

P

01

   1d

0.24

                   0.37

 

EOP (JPL)         

96

P

03

   1d

0.08

                   0.48

 

EOP (NOAA)    

96

P

01

   1d

0.25

                   0.49

 

EOP (SIO)         

96

P

01

   1d

0.10

                   0.32

 

 

* The satellite techniques provide information on the rate of change of Universal Time contaminated by effects due to unmodelled orbit node motion. VLBI-based results have been used to minimize drifts  in UT estimates

 

 

 

VIII.  DISTRIBUTION OF THE PUBLICATIONS

 

 

 

A.  IERS Rapid Service/Prediction Centre, at U.S. Naval Observatory:

 

BULLETIN A

 

        By 0h UTC of Friday of each week via e-mail distribution:

-          e-mail subscription (contact:  ser7@maia.usno.navy.mil)

-          World Wide Web (http://maia.usno.navy.mil/)

-          Anonymous ftp (ftp://maia.usno.navy.mil/ser7)

 

        By about 17:30h UTC daily via anonymous ftp:

-          World Wide Web (http://maia.usno.navy.mil/)

-           Anonymous ftp (ftp://maia.usno.navy.mil/ser7)

 

 

 

B.  IERS Earth Orientation Centre, at Paris Observatory:

 

-          e-mail (contact:  iers@obspm.fr)

-          World Wide Web (http://hpiers.obspm.fr/eop-pc/)

-          Anonymous ftp (hpiers.obspm.fr or 145.238.100.28)

 

BULLETIN B

 

        Updated at the beginning of each month

-          World Wide Web

-           Anonymous ftp (directory iers/bul/bulb)

-           airmail     

 

 

 

 

 

 

 

 

William Wooden                                                                                             Daniel Gambis

Director                                                                                                         Director

IERS Rapid Service/Prediction Centre                                                             IERS Earth Orientation Centre

wooden.william@usno.navy.mil                                                            daniel.gambis@obspm.fr               

 

GLOSSARY

 

BIH                 Bureau International de l'Heure

BIPM              Bureau International des Poids et Mesures

BKG                Bundesamt fuer kartographie und geodaesie

CEP                 Celestial Ephemeris Pole

CCIR               International Radio Consultative Committee

CIO                 Conventional International Origin

CODE             Center for Orbit Determination in Europe

CGS                 Space Geodesy Center, Matera

CSR                 Center for Space Research, University of Texas

DORIS            Doppler Orbit determination and Radiopositioning Integrate on Satellite

DUT                Delft University of Technology

EMR                See NRCan

EOP                Earth Orientation Parameters

ESOC              European Space Operations Center

GFZ                 GeoForschungsZentrum

GMST              Greenwich Mean Sidereal Time

GPS                 Global Positioning System

GSFC               Goddard Space Flight Center

IAA                 Institute of Applied Astronomy

IAG                 International Association of Geodesy

IAU                 International Astronomical Union

IERS                International Earth Rotation Service

ICRF               IERS Celestial Reference Frame

ICRS               International Celestial Reference System

IGS                  International GPS Service for Geodynamics

IRP                  IERS Reference Pole

IRM                 IERS Reference Meridian

ITRF                IERS Terrestrial Reference Frame

ITRS                International Terrestrial Reference System

IVS                  International VLBI Service

JPL                  Jet Propulsion Laboratory

LLR                 Lunar Laser Ranging

LOD                Length of day

LODR             Length of day corrected from zonal tides effects

MCC               Russian Mission Control Center

MJD                Modified Julian Day

NEOS              National Earth Orientation Service

NOAA             National Oceanic and Atmospheric Administration

NRCan            Natural Resources Canada, formerly EMR

OPA                Observatoire de Paris

SPBU              St Petersburg University

SLR                 Satellite Laser Ranging

SI                    Système International

SIO                  Scripps Institution of Oceanography

TAI                 Temps Atomique International

TCG                Geocentric Coordinate Time

TT                   Terrestrial Time

USNO             United States Naval Observatory

UT1                 Universal time

UT1R              Universal time corrected for zonal tides effects

UTC                Coordinated Universal Time

VLBI               Very Long Baseline Interferometry

REFERENCES

 

 

Aoki, S., Guinot, B., Kaplan, G.H., Kinoshita, H., McCarthy, D.D., Seidelmann, P.K., 1982: Astron. Astrophys., 105, 1.

Arias, F., Charlot, P., Feissel, M. and Lestrade, J.-F., 1995: Astron. Astrophys., 303, 604.

Boucher, C., Altamimi, Z., Feissel, M., Sillard, P., 1996: IERS Technical Note No. 20, Observatoire de Paris.

Bougeard M.L, D. Gambis and R. Ray, 2000: Algorithms for box constrained M-estimation: fitting large data sets with applications to Earth Orientation Parameters series, Physics and Chemistry of the Earth, 25, 9-11, pp 679-685.

Capitaine N., Guinot, B., and McCarthy, D. D., 2000, “Definition of the Celestial Ephemeris origin and of UT1 in the International Reference Frame,” Astron. Astrophys., 355, pp. 398–405.

Capitaine N., Chapront J., Lambert S., and Wallace P.: 2003, Expressions for the Celestial Intermediate Pole and Celestial Ephemeris Origin consistent with the IAU 2000A Precession-Nutation model, Astron. Astrophys., 400, 1145-1154.

CCIR, 1986: Recommendation and Reports of the CCIR, 16th Plenary Assembly (Dubrovnik), Vol 7, p 12, International Telecommunications Union, Geneva.  

Gambis D., 2000: Earth Orientation Monitoring using Various Techniques, Proc. Colloque IAU 178, Cagliari, Italy, Sept 1999.

IAU, 1998: Transactions of the International Astronomical Union, Vol. XXIIIB, Proceedings of the 23rd General Assembly, Kyoto, Japan.

Lambert S. and Bizouard, C., 2002: Positioning the Terrestrial Ephemeris Origin in the International Terrestrial Reference Frame, Astron. Astrophys. 394, 317-321.

Ma C., Arias, E.F., Eubanks, T.M., Fey, A.L., Gontier, A.M. , Jacobs, C.S., Sovers, O.J., Archinal, B.A., Charlot, P., 1998: The International Celestial Reference Frame as realized by Very Long Baseline Interferometry, Astron. J., 116, 516.

Ma, C. and Feissel, M., 1997: Definition and realization of the International Celestial Reference System by VLBI Astrometry of Extragalactic Objects, IERS Technical Note No. 23, Observatoire de Paris.

McCarthy, D.D. and Petit, G. (ed.), 2004: IERS Conventions (2003), IERS Technical Note No. 32,  Verlag des Bundesamts fuer Kartographie and Geodaesie, Frankfurt am Main.

McCarthy, D.D. and Gambis, D., 1997: Interpolating IERS Earth Orientation Data, IERS Gazette No. 13, at http://maia.usno.navy.mil/iers-gaz13.

McCarthy, D.D. and Luzum, B.J., 1991a: Bull. Geod., 65, 22.

McCarthy, D.D. and Luzum, B.J., 1991b: Bull. Geod., 65, 18.

Seidelmann, P.K., 1982: Celest. Mech., 27, 79.

van Leeuwen, F., Lindgren, L., and Mignard, F., 1997:  The Hipparcos and Tycho Catalogues, Volume 3, Construction of the Hipparcos Catalogue, ESA Publications Division, Noordwijk, The Netherlands.

 

Yoder, C.F., Williams, J.G., and Parke, M.E., 1981: J. Geophys. Res., 86, 881.