<?xml version="1.0" encoding="UTF-8" standalone="no"?>
<adc:VO_Catalog_ADC xmlns:adc="http://adc.astro.umd.edu/dataset_054" xmlns:au="http://adc.astro.umd.edu/Units" xmlns:dc="http://purl.org/dc/elements/1.1/" xmlns:cat="http://www.ivoa.net/Catalog" xmlns:cha="http://www.ivoa.net/Characterization" xmlns:col="http://www.ivoa.net/Collection" xmlns:stc="http://www.ivoa.net/xml/STC/stc-v1.20" xmlns:r="http://www.ivoa.net/xml/STC/STCregion/v1.20" xmlns:crd="http://www.ivoa.net/xml/STC/STCcoords/v1.20" xmlns:h="http://www.ivoa.net/Provenance" xmlns:p="http://www.ivoa.net/Publications" xmlns:ppl="http://www.ivoa.net/People" xmlns:ucd="http://www.ivoa.net/UCD1+" xmlns:u="http://www.ivoa.net/Units" xmlns:q="http://www.ivoa.net/Quantity" xmlns:xlink="http://www.w3.org/1999/xlink" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" cid="adc_1251" name="Definition and Realization of the International Celestial Reference System by VLBI Astrometry of Extragalactic Objects" xsi:schemaLocation="http://adc.astro.umd.edu/dataset_054 dataset_054.xsd">
  <dc:identifier>1251</dc:identifier>
  <h:provenance provenanceId="history_1251">
    <h:creation>
      <h:creator>
        <ppl:person>
          <ppl:firstName>Julie</ppl:firstName>
          <ppl:middleName>Anne</ppl:middleName>
          <ppl:lastName>Watko</ppl:lastName>
          <ppl:institution>
            <ppl:name>SSDOO/ADC</ppl:name>
          </ppl:institution>
        </ppl:person>
      </h:creator>
      <h:creator>
        <ppl:person>
          <ppl:firstName>James</ppl:firstName>
          <ppl:initial>E</ppl:initial>
          <ppl:lastName>Gass</ppl:lastName>
          <ppl:institution>
            <ppl:name>SSDOO/ADC</ppl:name>
          </ppl:institution>
        </ppl:person>
      </h:creator>
      <stc:date>1998-07-17</stc:date>
    </h:creation>
    <h:revisions>
      <h:revision>
        <h:revisor>
          <ppl:person>
            <ppl:firstName>James</ppl:firstName>
            <ppl:initial>E</ppl:initial>
            <ppl:lastName>Gass</ppl:lastName>
            <ppl:institution>
              <ppl:name>SSDOO/ADC</ppl:name>
            </ppl:institution>
          </ppl:person>
        </h:revisor>
        <h:revisor>
          <ppl:person>
            <ppl:firstName>Julie</ppl:firstName>
            <ppl:initial>A</ppl:initial>
            <ppl:lastName>Watko</ppl:lastName>
            <ppl:institution>
              <ppl:name>SSDOO/ADC</ppl:name>
            </ppl:institution>
          </ppl:person>
        </h:revisor>
        <stc:date>1998-07-17</stc:date>
        <p:note><![CDATA[The RSC(WGRF) 95 R 01 files were provided by the author. ADC has added the table of RSC(WGRF) 95 R 02 as found on the IERS Web site as a convenience to users.]]></p:note>
      </h:revision>
      <h:revision>
        <h:revisor>
          <ppl:person>
            <ppl:firstName>Francois</ppl:firstName>
            <ppl:lastName>Ochsenbein</ppl:lastName>
            <ppl:institution>
              <ppl:name>CDS</ppl:name>
            </ppl:institution>
          </ppl:person>
        </h:revisor>
        <h:revisor>
          <ppl:person>
            <ppl:firstName>Patricia</ppl:firstName>
            <ppl:lastName>Bauer</ppl:lastName>
            <ppl:institution>
              <ppl:name>CDS</ppl:name>
            </ppl:institution>
          </ppl:person>
        </h:revisor>
        <stc:date>1998-12-04</stc:date>
        <p:note><![CDATA[Added in this ReadMe extracts from the 1998AJ....116..516M paper.]]></p:note>
      </h:revision>
      <h:revision>
        <h:revisor>
          <ppl:team>
            <ppl:name>ADC staff</ppl:name>
            <ppl:institution>
              <ppl:name>ADC</ppl:name>
              <ppl:address>
                <ppl:street>Code 630, Goddard Space Flight Center/NASA</ppl:street>
                <ppl:postcode>20771</ppl:postcode>
                <ppl:city>Greenbelt</ppl:city>
                <ppl:state>Maryland</ppl:state>
                <ppl:country>United States of America</ppl:country>
              </ppl:address>
            </ppl:institution>
          </ppl:team>
          <p:note><![CDATA[Revision using version 1.36 of ADC's legacy conversion pipeline]]></p:note>
        </h:revisor>
        <stc:date>2002-03-14</stc:date>
        <p:note><![CDATA[XML generated from CDS/ADC ReadMe document and associated data files using txt2ML Rules Set: 1.56]]></p:note>
      </h:revision>
      <h:revision>
        <h:revisor>
          <ppl:team>
            <ppl:name>UMd-ADC staff</ppl:name>
            <ppl:institution>
              <ppl:name>UMd Astronomical Data Center</ppl:name>
              <ppl:address>
                <ppl:street>Department of Astronomy, University of Maryland</ppl:street>
                <ppl:postcode>20742</ppl:postcode>
                <ppl:city>College Park</ppl:city>
                <ppl:state>Maryland</ppl:state>
                <ppl:country>United States of America</ppl:country>
              </ppl:address>
              <ppl:email>thomas@astro.umd.edu</ppl:email>
              <ppl:url>http://archive.astro.umd.edu/archive</ppl:url>
            </ppl:institution>
          </ppl:team>
          <p:note><![CDATA[Revision using version 0.16 of the quantity/dataset transform pipeline.]]></p:note>
        </h:revisor>
        <stc:date>2005-09-30T05:03:48-04:00</stc:date>
        <p:note><![CDATA[This version of the document has unverified coordinate system information. Use at your ownrisk!]]></p:note>
      </h:revision>
    </h:revisions>
  </h:provenance>
  <p:references referencesId="ref_1251">
    <p:reference referenceId="srf1" type="source">
      <dc:title>Definition and Realization of the International Celestial Reference System by VLBI Astrometry of Extragalactic Objects</dc:title>
      <p:abstract>
        <p:para><![CDATA[
    of the 1998AJ....116..516M paper
    A quasi-inertial reference frame is defined based on the radio
    positions of 212 extragalactic sources distributed over the entire
    sky. The positional accuracy of these sources is better than about
    1mas in both coordinates. The radio positions are based upon a general
    solution for all applicable dual-frequency 2.3 and 8.4GHz Mark III
    very long baseline interferometry data available through the middle of
    1995, consisting of 1.6 million pairs of group delay and phase delay
    rate observations. Positions and details are also given for an
    additional 396 objects that either need further observation or are
    currently unsuitable for the definition of a high-accuracy reference
    frame. The final orientation of the frame axes has been obtained by a
    rotation of the positions into the system of the International
    Celestial Reference System and is consistent with the FK5 J2000.0
    optical system, within the limits of the link accuracy. The resulting
    International Celestial Reference Frame has been adopted by the
    International Astronomical Union as the fundamental celestial
    reference frame, replacing the FK5 optical frame as of 1998 January 1.]]></p:para>
      </p:abstract>
      <p:description>
        <p:para type="section"><![CDATA[General Description]]></p:para>
        <p:para><![CDATA[
    The International Celestial Reference Frame (ICRF), is intended for
    adoption be the International Astronomical Union (IAU) as the
    conventional celestial system, under the name International Celestial
    Reference System (ICRS).
    (See http://maia.usno.navy.mil/iauc19/iaures.html#B5).]]></p:para>
        <p:para><![CDATA[    A Working Group on Reference Frames (WGRF), with the participation of
    International Earth Rotation Service (IERS), was appointed by the IAU
    to accomplish the task of constructing the ICRF. The WGRF set up a
    list of 608 extragalactic radio sources uniformly distributed on the
    sky and evaluated their J2000.0 Very Long Baseline Interferometry
    (VLBI) coordinates in the ICRS by applying a no rotation constraint
    with respect to an earlier realization of the IERS Celestial reference
    system, RSC(IERS) 95 C 02 .]]></p:para>
        <p:para><![CDATA[    The first realization of the ICRF has J2000.0 coordinates of 608
    objects and is named RSC(WGRF)95 R 01. Radio sources in RSC(WGRF)95 R
    01 are divided into three categories (see file "guide.txt"): defining,
    candidate and other sources.]]></p:para>
        <p:para><![CDATA[    In order to provide radio source coordinates to link to the Hipparcos
    stellar reference frame to the ICRS, the WGRF issued a shorter version
    of the ICRF, RSC(WGRF) 95 R 02. It is a subset of RSC(WGRF) 95 R 01
    that contains J2000.0 coordinates of 253 radio sources covering the
    declination range -81 degrees to +85 degrees. The 212 defining sources
    of RSC(WGRF)95 R 01 included 17 Hipparcos link objects. An additional
    41 other radio sources had to be added RSC(WGRF) 95 R 02 for the link.
    The median positional accuracy of RSC(WGRF) 95 R 02 is 0.4 mas. The
    other 357 sources of RSC(WGRF) 95 R 01 have coordinates with lower
    precision (median= 0.8 mas) but they are still consistent with the
    ICRS.]]></p:para>
        <p:para><![CDATA[    The direction of the axes of the ICRF are consistent with those of the
    FK5 system within the uncertainties of the latter. On the basis of
    Fricke's (1982A&A...107L..13F) and Schwan (1988) considerations, the
    uncertainty of the pole position relative to the mean pole at J2000.0
    is +/-50 mas. Studies by Morrison et al. (1990A&A...240..173M) and
    Lindegren et al. (1995A&A...304...44L) have shown that the FK5 origin
    of right ascensions has an uncertainty of the order of +/-100 mas.]]></p:para>
        <p:para><![CDATA[    The accuracy of the tie of the Hipparcos stellar frame to ICRS is
    +/-0.6 mas at the Hipparcos mean epoch of observation (1991.25) and
    +/-0.25 mas/year for the time evolution. The tie between the dynamical
    planetary frame and ICRS is known within +/-3 mas (Folkner et al.
    1994A&A...287..279F).]]></p:para>
        <p:para xml:space="preserve"><![CDATA[
    Table 1: Summary of catalog differences (from 1998AJ....116..516M)
    --------------------------------------------------------------------------------
                       Rotation angles         RMS residuals       Internal trends
      Catalog pair       A1   A2   A3  ki2  RAcosDE DE Arc Length   Dmax  Dmax/sigma
                            (mas)                 (mas)           mas/100deg
    --------------------------------------------------------------------------------
    WGRF vs. IERS95    0.1 -0.4  0.0  2.92  0.23  0.39  0.55       0.32     14
    WGRF vs. RORF     -0.2 -0.5  0.0  2.77  0.10  0.38  0.42       0.32     15
    IERS95 vs. IERS94  0.0  0.0  0.0  2.85  0.30  0.31  0.52       0.29     12
    WGRF vs. GSFC     -0.1 -0.1 -0.0  1.68  0.09  0.29  0.39       0.15      7
    WGRF vs. JPL       0.1 -0.3 -0.2  2.84  0.26  0.44  0.51       0.66     15
    GSFC vs. JPL       0.2 -0.3  0.2  3.42  0.30  0.36  0.58       0.38     14
    WGRF vs. WGRFna    0.2  0.0  0.0  0.18  0.05  0.06  0.12       0.07      2
    WGRF vs. WGRFel    0.0  0.0  0.0  0.04  0.01  0.02  0.04       0.02      2
    WGRF vs. WGRFng    0.0 -0.1  0.0  0.99  0.03  0.12  0.22       0.19      8
    --------------------------------------------------------------------------------]]></p:para>
        <p:para xml:space="preserve"><![CDATA[
    Table 2: Alignment of the ICRF axes with the ICRS (from 1998AJ....116..516M)
    ----------------------------------------------------
     Parameter                   Value
    ----------------------------------------------------
     A_1_ (mas)               -0.006+/-0.018
     A_2_ (mas)                0.007+/-0.018
     A_3_ (mas)                0.005+/-0.021
     D_DE_ (mas/100{deg})      0.0
     D_DE_ (mas/100{deg})      0.2
     B_DE_ (mas/100{deg})     -0.28 +/-0.02
     wrms_RAcosDE_ (mas)       0.14
     wrms_DE_ (mas)            0.20
    ----------------------------------------------------]]></p:para>
      </p:description>
      <p:author>
        <ppl:person>
          <ppl:initial>C</ppl:initial>
          <ppl:lastName>Ma</ppl:lastName>
        </ppl:person>
      </p:author>
      <p:author>
        <ppl:person>
          <ppl:initial>M</ppl:initial>
          <ppl:lastName>Feissel</ppl:lastName>
        </ppl:person>
      </p:author>
      <p:other>
        <p:name>IERS Tech. Note 23</p:name>
        <stc:date>1997-??-??</stc:date>
      </p:other>
    </p:reference>
    <p:reference referenceId="srf2" type="source">
      <dc:title>Realization of the International Celestial Reference Frame from VLBI Astrometry</dc:title>
      <p:abstract>
        <p:para><![CDATA[
    of the 1998AJ....116..516M paper
    A quasi-inertial reference frame is defined based on the radio
    positions of 212 extragalactic sources distributed over the entire
    sky. The positional accuracy of these sources is better than about
    1mas in both coordinates. The radio positions are based upon a general
    solution for all applicable dual-frequency 2.3 and 8.4GHz Mark III
    very long baseline interferometry data available through the middle of
    1995, consisting of 1.6 million pairs of group delay and phase delay
    rate observations. Positions and details are also given for an
    additional 396 objects that either need further observation or are
    currently unsuitable for the definition of a high-accuracy reference
    frame. The final orientation of the frame axes has been obtained by a
    rotation of the positions into the system of the International
    Celestial Reference System and is consistent with the FK5 J2000.0
    optical system, within the limits of the link accuracy. The resulting
    International Celestial Reference Frame has been adopted by the
    International Astronomical Union as the fundamental celestial
    reference frame, replacing the FK5 optical frame as of 1998 January 1.]]></p:para>
      </p:abstract>
      <p:description>
        <p:para type="section"><![CDATA[General Description]]></p:para>
        <p:para><![CDATA[
    The International Celestial Reference Frame (ICRF), is intended for
    adoption be the International Astronomical Union (IAU) as the
    conventional celestial system, under the name International Celestial
    Reference System (ICRS).
    (See http://maia.usno.navy.mil/iauc19/iaures.html#B5).]]></p:para>
        <p:para><![CDATA[    A Working Group on Reference Frames (WGRF), with the participation of
    International Earth Rotation Service (IERS), was appointed by the IAU
    to accomplish the task of constructing the ICRF. The WGRF set up a
    list of 608 extragalactic radio sources uniformly distributed on the
    sky and evaluated their J2000.0 Very Long Baseline Interferometry
    (VLBI) coordinates in the ICRS by applying a no rotation constraint
    with respect to an earlier realization of the IERS Celestial reference
    system, RSC(IERS) 95 C 02 .]]></p:para>
        <p:para><![CDATA[    The first realization of the ICRF has J2000.0 coordinates of 608
    objects and is named RSC(WGRF)95 R 01. Radio sources in RSC(WGRF)95 R
    01 are divided into three categories (see file "guide.txt"): defining,
    candidate and other sources.]]></p:para>
        <p:para><![CDATA[    In order to provide radio source coordinates to link to the Hipparcos
    stellar reference frame to the ICRS, the WGRF issued a shorter version
    of the ICRF, RSC(WGRF) 95 R 02. It is a subset of RSC(WGRF) 95 R 01
    that contains J2000.0 coordinates of 253 radio sources covering the
    declination range -81 degrees to +85 degrees. The 212 defining sources
    of RSC(WGRF)95 R 01 included 17 Hipparcos link objects. An additional
    41 other radio sources had to be added RSC(WGRF) 95 R 02 for the link.
    The median positional accuracy of RSC(WGRF) 95 R 02 is 0.4 mas. The
    other 357 sources of RSC(WGRF) 95 R 01 have coordinates with lower
    precision (median= 0.8 mas) but they are still consistent with the
    ICRS.]]></p:para>
        <p:para><![CDATA[    The direction of the axes of the ICRF are consistent with those of the
    FK5 system within the uncertainties of the latter. On the basis of
    Fricke's (1982A&A...107L..13F) and Schwan (1988) considerations, the
    uncertainty of the pole position relative to the mean pole at J2000.0
    is +/-50 mas. Studies by Morrison et al. (1990A&A...240..173M) and
    Lindegren et al. (1995A&A...304...44L) have shown that the FK5 origin
    of right ascensions has an uncertainty of the order of +/-100 mas.]]></p:para>
        <p:para><![CDATA[    The accuracy of the tie of the Hipparcos stellar frame to ICRS is
    +/-0.6 mas at the Hipparcos mean epoch of observation (1991.25) and
    +/-0.25 mas/year for the time evolution. The tie between the dynamical
    planetary frame and ICRS is known within +/-3 mas (Folkner et al.
    1994A&A...287..279F).]]></p:para>
        <p:para xml:space="preserve"><![CDATA[
    Table 1: Summary of catalog differences (from 1998AJ....116..516M)
    --------------------------------------------------------------------------------
                       Rotation angles         RMS residuals       Internal trends
      Catalog pair       A1   A2   A3  ki2  RAcosDE DE Arc Length   Dmax  Dmax/sigma
                            (mas)                 (mas)           mas/100deg
    --------------------------------------------------------------------------------
    WGRF vs. IERS95    0.1 -0.4  0.0  2.92  0.23  0.39  0.55       0.32     14
    WGRF vs. RORF     -0.2 -0.5  0.0  2.77  0.10  0.38  0.42       0.32     15
    IERS95 vs. IERS94  0.0  0.0  0.0  2.85  0.30  0.31  0.52       0.29     12
    WGRF vs. GSFC     -0.1 -0.1 -0.0  1.68  0.09  0.29  0.39       0.15      7
    WGRF vs. JPL       0.1 -0.3 -0.2  2.84  0.26  0.44  0.51       0.66     15
    GSFC vs. JPL       0.2 -0.3  0.2  3.42  0.30  0.36  0.58       0.38     14
    WGRF vs. WGRFna    0.2  0.0  0.0  0.18  0.05  0.06  0.12       0.07      2
    WGRF vs. WGRFel    0.0  0.0  0.0  0.04  0.01  0.02  0.04       0.02      2
    WGRF vs. WGRFng    0.0 -0.1  0.0  0.99  0.03  0.12  0.22       0.19      8
    --------------------------------------------------------------------------------]]></p:para>
        <p:para xml:space="preserve"><![CDATA[
    Table 2: Alignment of the ICRF axes with the ICRS (from 1998AJ....116..516M)
    ----------------------------------------------------
     Parameter                   Value
    ----------------------------------------------------
     A_1_ (mas)               -0.006+/-0.018
     A_2_ (mas)                0.007+/-0.018
     A_3_ (mas)                0.005+/-0.021
     D_DE_ (mas/100{deg})      0.0
     D_DE_ (mas/100{deg})      0.2
     B_DE_ (mas/100{deg})     -0.28 +/-0.02
     wrms_RAcosDE_ (mas)       0.14
     wrms_DE_ (mas)            0.20
    ----------------------------------------------------]]></p:para>
      </p:description>
      <p:author>
        <ppl:person>
          <ppl:initial>C</ppl:initial>
          <ppl:lastName>Ma</ppl:lastName>
        </ppl:person>
      </p:author>
      <p:other>
        <p:name>Bull. American Astron. Soc., 191, #16.13</p:name>
        <stc:date>1997-??-??</stc:date>
        <p:bibcode>1997AAS...191.1613M</p:bibcode>
      </p:other>
    </p:reference>
    <p:reference referenceId="srf3" type="source">
      <dc:title>The international celestial reference frame as realized by very long baseline interferometry.</dc:title>
      <p:abstract>
        <p:para><![CDATA[
    of the 1998AJ....116..516M paper
    A quasi-inertial reference frame is defined based on the radio
    positions of 212 extragalactic sources distributed over the entire
    sky. The positional accuracy of these sources is better than about
    1mas in both coordinates. The radio positions are based upon a general
    solution for all applicable dual-frequency 2.3 and 8.4GHz Mark III
    very long baseline interferometry data available through the middle of
    1995, consisting of 1.6 million pairs of group delay and phase delay
    rate observations. Positions and details are also given for an
    additional 396 objects that either need further observation or are
    currently unsuitable for the definition of a high-accuracy reference
    frame. The final orientation of the frame axes has been obtained by a
    rotation of the positions into the system of the International
    Celestial Reference System and is consistent with the FK5 J2000.0
    optical system, within the limits of the link accuracy. The resulting
    International Celestial Reference Frame has been adopted by the
    International Astronomical Union as the fundamental celestial
    reference frame, replacing the FK5 optical frame as of 1998 January 1.]]></p:para>
      </p:abstract>
      <p:description>
        <p:para type="section"><![CDATA[General Description]]></p:para>
        <p:para><![CDATA[
    The International Celestial Reference Frame (ICRF), is intended for
    adoption be the International Astronomical Union (IAU) as the
    conventional celestial system, under the name International Celestial
    Reference System (ICRS).
    (See http://maia.usno.navy.mil/iauc19/iaures.html#B5).]]></p:para>
        <p:para><![CDATA[    A Working Group on Reference Frames (WGRF), with the participation of
    International Earth Rotation Service (IERS), was appointed by the IAU
    to accomplish the task of constructing the ICRF. The WGRF set up a
    list of 608 extragalactic radio sources uniformly distributed on the
    sky and evaluated their J2000.0 Very Long Baseline Interferometry
    (VLBI) coordinates in the ICRS by applying a no rotation constraint
    with respect to an earlier realization of the IERS Celestial reference
    system, RSC(IERS) 95 C 02 .]]></p:para>
        <p:para><![CDATA[    The first realization of the ICRF has J2000.0 coordinates of 608
    objects and is named RSC(WGRF)95 R 01. Radio sources in RSC(WGRF)95 R
    01 are divided into three categories (see file "guide.txt"): defining,
    candidate and other sources.]]></p:para>
        <p:para><![CDATA[    In order to provide radio source coordinates to link to the Hipparcos
    stellar reference frame to the ICRS, the WGRF issued a shorter version
    of the ICRF, RSC(WGRF) 95 R 02. It is a subset of RSC(WGRF) 95 R 01
    that contains J2000.0 coordinates of 253 radio sources covering the
    declination range -81 degrees to +85 degrees. The 212 defining sources
    of RSC(WGRF)95 R 01 included 17 Hipparcos link objects. An additional
    41 other radio sources had to be added RSC(WGRF) 95 R 02 for the link.
    The median positional accuracy of RSC(WGRF) 95 R 02 is 0.4 mas. The
    other 357 sources of RSC(WGRF) 95 R 01 have coordinates with lower
    precision (median= 0.8 mas) but they are still consistent with the
    ICRS.]]></p:para>
        <p:para><![CDATA[    The direction of the axes of the ICRF are consistent with those of the
    FK5 system within the uncertainties of the latter. On the basis of
    Fricke's (1982A&A...107L..13F) and Schwan (1988) considerations, the
    uncertainty of the pole position relative to the mean pole at J2000.0
    is +/-50 mas. Studies by Morrison et al. (1990A&A...240..173M) and
    Lindegren et al. (1995A&A...304...44L) have shown that the FK5 origin
    of right ascensions has an uncertainty of the order of +/-100 mas.]]></p:para>
        <p:para><![CDATA[    The accuracy of the tie of the Hipparcos stellar frame to ICRS is
    +/-0.6 mas at the Hipparcos mean epoch of observation (1991.25) and
    +/-0.25 mas/year for the time evolution. The tie between the dynamical
    planetary frame and ICRS is known within +/-3 mas (Folkner et al.
    1994A&A...287..279F).]]></p:para>
        <p:para xml:space="preserve"><![CDATA[
    Table 1: Summary of catalog differences (from 1998AJ....116..516M)
    --------------------------------------------------------------------------------
                       Rotation angles         RMS residuals       Internal trends
      Catalog pair       A1   A2   A3  ki2  RAcosDE DE Arc Length   Dmax  Dmax/sigma
                            (mas)                 (mas)           mas/100deg
    --------------------------------------------------------------------------------
    WGRF vs. IERS95    0.1 -0.4  0.0  2.92  0.23  0.39  0.55       0.32     14
    WGRF vs. RORF     -0.2 -0.5  0.0  2.77  0.10  0.38  0.42       0.32     15
    IERS95 vs. IERS94  0.0  0.0  0.0  2.85  0.30  0.31  0.52       0.29     12
    WGRF vs. GSFC     -0.1 -0.1 -0.0  1.68  0.09  0.29  0.39       0.15      7
    WGRF vs. JPL       0.1 -0.3 -0.2  2.84  0.26  0.44  0.51       0.66     15
    GSFC vs. JPL       0.2 -0.3  0.2  3.42  0.30  0.36  0.58       0.38     14
    WGRF vs. WGRFna    0.2  0.0  0.0  0.18  0.05  0.06  0.12       0.07      2
    WGRF vs. WGRFel    0.0  0.0  0.0  0.04  0.01  0.02  0.04       0.02      2
    WGRF vs. WGRFng    0.0 -0.1  0.0  0.99  0.03  0.12  0.22       0.19      8
    --------------------------------------------------------------------------------]]></p:para>
        <p:para xml:space="preserve"><![CDATA[
    Table 2: Alignment of the ICRF axes with the ICRS (from 1998AJ....116..516M)
    ----------------------------------------------------
     Parameter                   Value
    ----------------------------------------------------
     A_1_ (mas)               -0.006+/-0.018
     A_2_ (mas)                0.007+/-0.018
     A_3_ (mas)                0.005+/-0.021
     D_DE_ (mas/100{deg})      0.0
     D_DE_ (mas/100{deg})      0.2
     B_DE_ (mas/100{deg})     -0.28 +/-0.02
     wrms_RAcosDE_ (mas)       0.14
     wrms_DE_ (mas)            0.20
    ----------------------------------------------------]]></p:para>
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              <q:refQuantity qidRef="rsc95can_RA"/>
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              <q:refQuantity qidRef="rsc95can_DE"/>
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              <q:refQuantity qidRef="rsc95can_e_DEs"/>
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              <q:refQuantity qidRef="rsc95can_Corr"/>
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              <q:refQuantity qidRef="rsc95can_Ep-MJD"/>
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              <q:refQuantity qidRef="rsc95can_O1-MJD"/>
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              <q:refQuantity qidRef="rsc95can_Ol-MJD"/>
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              <q:refQuantity qidRef="rsc95def_RA"/>
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              <q:refQuantity qidRef="rsc95def_DE"/>
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              <q:refQuantity qidRef="rsc95def_e_DEs"/>
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              <q:refQuantity qidRef="rsc95def_Corr"/>
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              <q:refQuantity qidRef="rsc95def_Ep-MJD"/>
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          <col:property name="status" description="*[DL ] Status of source" qid="rsc95r02_status">
            <cha:limits>
              <q:refQuantity qidRef="rsc95r02_status"/>
              <cha:min/>
              <cha:max/>
            </cha:limits>
            <q:axes>
              <q:refQuantity qidRef="obj_rsc95r02"/>
            </q:axes>
            <u:unitless/>
            <q:string width="2" noDataValue="  "/>
            <q:values fromResource="res_rsc95r02"/>
          </col:property>
          <col:property name="RA" description="Right Ascension (Eq: J2000)" qid="rsc95r02_RA">
            <cha:limits>
              <q:refQuantity qidRef="rsc95r02_RA"/>
              <cha:min>00 05 57.175409</cha:min>
              <cha:max>23 54 21.680275</cha:max>
            </cha:limits>
            <ucd:ucd>RAhms</ucd:ucd>
            <stc:CoordSystemRef qidRef="coords_rsc95can_RA_1251"/>
            <q:axes>
              <q:refQuantity qidRef="obj_rsc95r02"/>
            </q:axes>
            <au:units>
              <au:unit>h</au:unit>
              <au:unit>min</au:unit>
              <au:unit>s</au:unit>
            </au:units>
            <q:string width="15" noDataValue="               "/>
            <q:values fromResource="res_rsc95r02"/>
          </col:property>
          <col:property name="DE" description="Declination (Eq: J2000)" qid="rsc95r02_DE">
            <cha:limits>
              <q:refQuantity qidRef="rsc95r02_DE"/>
              <cha:min>-81 01 02.23146</cha:min>
              <cha:max>+84 32 04.54402</cha:max>
            </cha:limits>
            <ucd:ucd>DEdms</ucd:ucd>
            <stc:CoordSystemRef qidRef="coords_rsc95can_RA_1251"/>
            <q:axes>
              <q:refQuantity qidRef="obj_rsc95r02"/>
            </q:axes>
            <au:units>
              <au:unit>deg</au:unit>
              <au:unit>arcmin</au:unit>
              <au:unit>arcsec</au:unit>
            </au:units>
            <q:string width="15" noDataValue="               "/>
            <q:values fromResource="res_rsc95r02"/>
          </col:property>
          <col:property name="e_RAs" description="Uncertainty in Right Ascension" qid="rsc95r02_e_RAs">
            <cha:limits>
              <q:refQuantity qidRef="rsc95r02_e_RAs"/>
              <cha:min>0.000017</cha:min>
              <cha:max>0.035391</cha:max>
            </cha:limits>
            <q:axes>
              <q:refQuantity qidRef="obj_rsc95r02"/>
            </q:axes>
            <au:units name="s">
              <au:unit>s</au:unit>
            </au:units>
            <q:float noDataValue="-9.999999" precision="6" width="9"/>
            <q:values fromResource="res_rsc95r02"/>
          </col:property>
          <col:property name="e_DEs" description="Uncertainty in Declination" qid="rsc95r02_e_DEs">
            <cha:limits>
              <q:refQuantity qidRef="rsc95r02_e_DEs"/>
              <cha:min>0.00026</cha:min>
              <cha:max>0.45061</cha:max>
            </cha:limits>
            <q:axes>
              <q:refQuantity qidRef="obj_rsc95r02"/>
            </q:axes>
            <au:units name="arcsec">
              <au:unit>arcsec</au:unit>
            </au:units>
            <q:float noDataValue="-9.99999" precision="5" width="8"/>
            <q:values fromResource="res_rsc95r02"/>
          </col:property>
        </col:object>
      </cat:data>
    </cat:VOCatalog>
  </adc:data>
</adc:VO_Catalog_ADC>
