A&A 452, 1099-1106 (2006)
DOI: 10.1051/0004-6361:20053021
N. Pradel^{1} - P. Charlot^{1} - J.-F. Lestrade^{2}
1 - Observatoire de Bordeaux (OASU) - CNRS/UMR
5804, BP 89, 33270 Floirac, France
2 - Observatoire de Paris - CNRS/UMR 8112, 61 avenue de
l'Observatoire, 75014 Paris, France
Received 8 March 2005 / Accepted 4 January 2006
Abstract
Astrometric accuracy of complex modern VLBI arrays cannot
be calculated analytically. We study the astrometric accuracy of
phase-referenced VLBI observations for the VLBA, EVN and global VLBI
array by simulating VLBI data for targets at declinations
,
,
,
,
and
.
The systematic
error components considered in this study are calibrator position,
station coordinate, Earth orientation and troposphere parameter
uncertainties. We provide complete tables of the astrometric
accuracies of these arrays for a source separation of
either
along the right ascension axis or along the declination
axis. Astrometric accuracy is as at mid declination and is
as at low (
)
and high (
)
declinations
for the VLBA and EVN. In extending our simulations to source
separations of
and
,
we establish the formula for
the astrometric accuracy of the VLBA:
(as) where
is the astrometric accuracy for a separation
provided in our tables for various declinations and
conditions of the wet troposphere. We argue that this formula is also
valid for the astrometric accuracy of the EVN and global VLBI array.
Key words: astrometry - techniques: high angular resolution - techniques: interferometric
Very Long Baseline Interferometry (VLBI) narrow-angle astrometry pioneered by Shapiro et al. (1979) makes use of observations of pairs of angularly close sources to cancel atmospheric phase fluctuations between the two close lines of sight. In this initial approach, the relative coordinates between the two strong quasars 3C 345 and NRAO512 and other ancilliary parameters were adjusted by a least-squares fit of the differenced phases after connecting the VLBI phases for both sources over a multi-hour experiment. Then, Marcaide & Shapiro (1984,1983) made the first phase-referenced map where structure and astrometry were disentangled for the double quasar 1038+528 A and B. Both of these experiments demonstrated formal errors at the level of a few tens of microarcseconds or less in the relative angular separation between the two sources.
Another approach was designed to tackle faint target sources by
observing a strong reference source (quasar) to increase the
integration time of VLBI from a few minutes to a few hours
(Lestrade et al. 1990). This approach improves the sensitivity by the factor
In the approach above, the VLBI phases of the strong reference source are connected, interpolated in time and differenced with the VLBI phases of the faint source that do not need to be connected. The differenced visibilities are then inverted to produce the map of the brightness distribution of the faint target source and its position is determined by reading directly the coordinates of the map peak which are relative to the a priori reference source coordinates. The map is usually highly undersampled but suffices for astrometry. This mapping astrometry technique is implemented in the SPRINT software (Lestrade et al. 1990) and a similar procedure is also used within the NRAO AIPS package to produce phase-referenced VLBI maps with absolute source coordinates on the sky.
While phase-referencing in this way is efficient, it still provides no direct positional uncertainty as does least-squares fitting of differenced phases (Shapiro et al. 1979). In order to circumvent this problem, we have developed simulations to evaluate the impact of systematic errors in the derived astrometric results. Such simulations have been carried out for of a pair of sources observed with the Very Long Baseline Array (VLBA) and the European VLBI Network (EVN) at various declinations and angular separations. Systematic errors in station coordinates, Earth rotation parameters, reference source coordinates and tropospheric zenith delays were studied in turn. The results of the simulations are summarized below in tables that indicate positional uncertainties when considering these systematic errors either separately or altogether. Such tables can be further interpolated to determine the accuracy of any full-track experiment with the VLBA and EVN.
Our study includes atmospheric fluctuations caused by the turbulent atmosphere above all stations. These fluctuations have been considered uniform and equivalent to a delay rate noise of 0.1 ps/s for all stations. The impact of these fluctuations is limited if the antenna switching cycle between the two sources is fast enough. The phase structure function measured at 22 GHz above the VLA by Carilli & Holdaway (1999) provides prescriptions on this switching time. At high frequency, it can be as short as 10 s, as e.g. in Reid et al. (2003) who carried out precise 43 GHz VLBA astrometric observations of Sgr A^{*} at a declination of . Switching time in more clement conditions is typically a few minutes at 8.4 GHz for northern sources.
A few applications of mapping astrometry are the search for extra-solar planets around radio-emitting stars (Lestrade et al. 1994), the determination of the Gravity Probe B guide star proper motion (Lebach et al. 1999), the determination of absolute motions of VLBI components in extragalactic sources, e.g. in compact symetric objects (Charlot et al. 2005) or core-jet sources (Ros et al. 1999), probing the jet collimation region in extragalactic nuclei (Ly et al. 2004), pulsar parallax and proper motion measurements (Brisken et al. 2002) and the determination of parallaxes and proper motions of maser sources in the whole Galaxy as planned with the VERA project (Honma et al. 2000; Kawaguchi et al. 2000).
As indicated in e.g. Thompson et al. (1986), the theoretical precision of
astrometry with the interferometer phase is
(1) |
While the theoretical precision above might be regarded as the potential accuracy attainable for the VLBI, systematic errors in the model of the phase limit narrow-angle astrometry precision to roughly ten times this level in practice (Fomalont et al. 1999). An analytical study of systematic errors in phase-referenced VLBI astrometry over a single baseline is given in Shapiro et al. (1979) and it shows that all systematic errors are scaled by the source separation. Another error analysis in such differential VLBI measurements can be found in Morabito (1984). However, for modern VLBI arrays with 10 or more antennae, the complex geometry makes the analytical approach intractable. For this reason, we have estimated such systematic errors by simulating VLBI visibilities and inverting them for a range of model parameters (station coordinates, reference source coordinates, Earth Orientation parameters, and tropospheric dry and wet zenith delays) corresponding to the expected errors in these parameters.
The visibilities were simulated for a pair of sources at declinations , , , , , and with angular separations , and 2 for the VLBA, EVN and global VLBI array (VLBA+EVN). For each of these cases, we simulated visibilities every 2.5 min from source rise to set (full track) with a lower limit on elevation of 7 . The adopted flux for each source (calibrator and target) was 1 Jy to make the phase thermal noise negligeable in our simulations. For applications to faint target sources, one should combine the corresponding thermal astrometric uncertainty (Eq. (1)) with the systematic errors derived below. The simulated visibilities were then inverted using uniform weighting to produce a phase-referenced map of the target source and estimate its position. This operation was repeated 100 times in a Monte Carlo analysis after varying slightly the parameters of the model based on errors drawn from a Gaussian distribution with zero-mean and plausible standard deviation. We report the rms of the differences found between the known a priori position of the target source and the resulting estimated positions as a measure of the corresponding systematic errors for each of the above cases. We have adopted the usual astrometric frequency of 8.4 GHz for this analysis.
The phase delay and group delay in VLBI are described in
Sovers et al. (1998). The phase
at frequency
is
related to the interferometer delay
The model above is that implemented in the SPRINT software used for our simulations. It is thought to be complete for narrow-angle astrometry and additional refinements, such as ocean loading, atmospheric loading, etc., would not make difference into our results. We have not studied the ionosphere contribution to systematic errors. The unpredictible nature of the ionosphere makes this task difficult. Calibration of the ionosphere by dual-frequency observations, or over a wide bandwidth at low frequency (Brisken et al. 2002), or simply by observing at high frequency (>10 GHz) where the effect is small, offers solutions to this problem.
Table 1: Adopted rms errors for the source coordinates, VLBA station coordinates and Earth Orientation Parameters in our Monte Carlo simulations.
Table 2: Dry and wet tropospheric zenith path delays ( and ) at the VLBA stations along with the adopted rms errors and in our Monte Carlo simulations.
The parameter rms errors adopted as plausible for the VLBA phase model are listed in Tables 1 and 2. The reference source coordinate uncertainties ( , ) of 1 mas are typical of those in the VLBA Calibrator Survey (Beasley et al. 2002), from which most of the reference sources originate. However, ICRF extragalactic sources have better position accuracies down to 0.25 mas (Ma et al. 1998). We have thus carried out the calculations for both of these cases (1 mas and 0.25 mas) and both and have been perturbed by these uncertainties in our simulations. The uncertainties for the station coordinates are from the ITRF2000 frame (Boucher et al. 2004) while those for the Earth Orientation Parameters are from the IERS web site^{}. The adopted dry tropospheric rms error of 0.5 cm corresponds to 2.5 millibars in atmospheric pressure uncertainty at sea level. Although barometer reading is usually better, the absolute calibration of station barometers is at this level. Uncertainties in the wet tropospheric zenith delay derived from temperature and humidity are known to be large (Saastamoinen 1973). Experience makes us believe that a 30% error is likely on and thus we took 1/3 of as the plausible rms error with a minimum value of 2 cm. We carried out simulations for both mean and maximum values of wet zenith path delays based on estimates of recently derived from multiple VLBA geodetic and astrometric sessions (Sovers 2003). The maximum wet zenith delays and corresponding errors were used to investigate the impact of extreme weather conditions on observations. These values are listed for each VLBA station in Table 2.
Table 3: VLBA rms astrometric errors (in as) for a relative source separation . Individual astrometric error contributions from calibrator position, Earth orientation parameter, station coordinate, and dry and wet troposphere uncertainties are given separately, while the last two lines indicate the total astrometric errors when all model parameters are perturbed together.
Table 4: VLBA rms astrometric errors (in as) for a relative source separation . Individual astrometric error contributions from calibrator position, Earth orientation parameter, station coordinate, and dry and wet troposphere uncertainties are given separately, while the last two lines indicate the total astrometric errors when all model parameters are perturbed together.
We simulated the visibilities of a full u-v track experiment with the VLBA for six declinations between and with a relative source separation (either oriented in right ascension or in declination). Uniform weighting was applied to the visibilities, resulting in a synthesized beam mainly shaped by the longest baselines. As a test, we have also removed the 9 baselines smaller than 1500 km in length out of the 45 baseline array and noted a decrease in systematic errors of in a few test cases. Conservatively, we have retained these "short'' baselines in our final simulations. This is motivated by the fact that all possible baselines must be kept for sensitivity when observing weak sources. The antenna switching cycle between target and reference sources was set to 2.5 min. The results, however, do not depend critically on this value. It was chosen so that the automatic phase connection routine for the reference source does not discard too much data in the presence of a delay rate error of 0.1 ps/s (adopted uniformly for all the stations in the simulation). As mentioned previously, we analysed these data simulated with SPRINT using the a priori parameter values perturbed by some errors. We carried out this analysis 100 times for each systematic error component with perturbation errors drawn from Gaussian distributions with zero mean and standard deviations according to the rms errors in Tables 1 and 2. The resulting position of the target was estimated by reading the peak position in each of the 100 phase-referenced maps. The pixel size in the maps was 0.05 mas. This size is small compared to the synthesized beam (1 mas at 8.4 GHz on 8000 km baseline) and, hence, the uncertainty in the peak position due to the pixel size is negligeable. This position was determined by fitting a parabola over the full half beam width. This procedure was used in the Hipparcos/VLBI work of Lestrade et al. (1999) and was found to be appropriate. As expected, each position was slightly offset from the map phase center, reflecting the corresponding systematic errors. After substracting the initial perturbation in the calibrator position, we calculated the rms of these 100 relative coordinate offsets and for the adopted source separation in right ascension or declination. Note that the mean of these 100 coordinate offsets was close to zero in all cases. In Tables 3 and 4, we report the rms astrometric errors for each individual error component along with the total astrometric errors when all model parameters are perturbed together in the simulation. The total errors were derived by considering a 1 mas error in the calibration position.
The wet troposphere systematic error clearly dominates over all the
other error components for
but the calibrator
error dominates at higher declinations if its position is not known
to better than 1 mas.
This behavior was first noted by Shapiro et al. (1979) who derived analytical
formulae providing the astrometric errors caused by the calibrator coordinate
uncertainties in the case of a single VLBI baseline. A detailed analysis
comparing our simulated errors with those obtained from these formulae
is given in Appendix A. Other systematic errors,
in particular the Earth orientation parameter and the station
coordinate errors, are small. In Tables 3 and 4,
we note that astrometric errors originating from mean and maximum wet
troposphere uncertainties are not drastically different (a ratio of 1.5
at most).
Figure 1: Distribution of total astrometric errors for a relative source separation along declination at declination . All perturbating errors (calibrator position, Earth orientation parameters, station coordinates, dry and wet troposphere parameters) are considered together in thissimulation. | |
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Finally, we have plotted in Fig 1 the distribution of all coordinate offsets and for the declination target when all perturbation errors are present. For this specific case we have carried out 1000 simulations to refine the binning of the distribution. We have also performed the Pearson test on all distributions and provide the reduced chi-square and probability p that such distributions are Gaussian in Table 5. The results of this test show that most of the distributions are not Gaussian with p generally smaller than 0.4.
We have carried out a similar study for the EVN by simulating full track observations for the 10 stations of the array at 8.4 GHz. The adopted errors for the reference source coordinates and Earth orientation parameters were identical to those used in the VLBA simulations. Station coordinate errors were similar to the VLBA ones (1-6 mm), with the exception of those for Westerbork which are at the level of 50 mm (Charlot et al. 2002). The same scheme as that adopted for the VLBA was used to define zenith dry and wet tropospheric delay errors at each EVN station and the corresponding values are given in Table 6.
Table 5: Reduced chi-square and probability p of Gaussian distribution for the astrometric errors and using the Pearson test.
Since the EVN comprises antennas with different sensitivities, each baseline has been weighted by the reciprocal of their noise power equivalent with System Equivalent Flux Densities (SEFD_{i}) for each station according to Table 2 of the EVN Status Table^{} (as available in May 2003). The Effelsberg-Westerbork baseline is the most sensitive baseline of the array but also the shortest one and so unfavorable for high-accuracy astrometry. For this reason, we decided to perform the simulations without this baseline, hence using an array of 44 baselines only. We have applied uniform weighting to the visibilities similarly to the VLBA. We have tested that in removing the 12 baselines shorter than 1500 km in this 44 baseline array, systematic errors decrease by but, conservatively, we have kept them in our simulations. In order to reduce the number of simulations, calculations were carried out for only mean values of the wet zenith tropospheric delays since the results when using mean or maximum values were not found to be drasticaly different. We also did not calculate individual contributions from calibrator position, dry tropospheric zenith delay and Earth orientation parameter errors since these were found to be very small for the VLBA (see Tables 3 and 4). One should keep in mind, however, that calibrator error dominates at high declination. The results of the EVN simulations are reported in Tables 7 and 8 for a source separation in right ascension or declination.
At declination , many SPRINT maps were found to be ambiguous, i.e. the main lobe of the point spread function of the EVN could not be identified because secondary lobes were too high. This is essentially caused by the relatively high latitude of the array and hence to the difficulty of observing such low declination sources due to very limited visibility periods. For this reason, we do not provide EVN results for this declination. For other declinations, EVN astrometric errors (Tables 7 and 8) are similar to those found for the VLBA (Tables 3 and 4) and the Westerbork position error is not a limiting factor. Declination accuracies are somewhat better for the EVN than for the VLBA at low declination ( and ), a consequence of the participation of Hartebeeshoek (South Africa) in such observations.
Table 6: Dry and wet tropospheric zenith path delays ( and ) at the EVN stations along with the adopted rms errors and in our Monte Carlo simulations.
Table 7: EVN rms astrometric errors (in as) for a relative source separation . Individual astrometric error contributions from station coordinate and wet troposphere uncertainties are given separately along with the total astrometric errors when all model parameters are perturbed together.
Table 8: EVN rms astrometric errors (in as) for a relative source separation . Individual astrometric error contributions from station coordinate and wet troposphere uncertainties are given separately along with the total astrometric errors when all model parameters are perturbed together.
Table 9: Global VLBI array rms astrometric errors (in as) for a relative source separation . The individual astrometric error contribution from wet troposphere uncertainties is given separately along with the total astrometric errors when all model parameters are perturbed together.
Table 10: Global VLBI array rms astrometric errors (in as) for a relative source separation . The individual astrometric error contribution from wet troposphere uncertainties is given separately along with the total astrometric errors when all model parameters are perturbed together.
Table 11: VLBA without Saint Croix rms astrometric errors (in as) for a relative source separation . The individual astrometric error contribution from wet troposphere uncertainties is given separately along with the total astrometric errors when all model parameters are perturbed together.
We have carried out a similar study for the global VLBI array which is the combination of the VLBA and EVN. It includes 20 stations, with 190 possible baselines. As discussed above, the Effelsberg-Westerbork baseline was ignored and the calculations were thus carried out for 189 baselines only. The adopted systematic error values for the simulations with this array were the same as those adopted for the individual VLBA and EVN (Tables 1, 2 and 6) and calculations were performed for full track observations as previously. The results of these simulations (Tables 9 and 10) indicate that the astrometric errors for the global VLBI array are consistent with those found for the VLBA and the EVN. As expected, these errors are generally slightly better than the ones derived for each individual array.
Our simulations show that the astrometric accuracy of the VLBI phase-referencing technique (defined as ) is as for mid declinations and is as at low and high declinations for point sources with a relative separation of . The major systematic error components are the wet tropospheric delay and the calibrator astrometric position, the latter only at high declination. Station coordinate, Earth orientation parameter and dry tropospheric zenith delay errors contribute generally to less than as in the error budget.
Table 12: VLBA without Saint Croix rms astrometric errors (in as) for a relative source separation . The individual astrometric error contribution from wet troposphere uncertainties is given separately along with the total astrometric errors when all model parameters are perturbed together.
We speculated that if the VLBA station at Saint Croix in the Virgin Islands that suffers from dampness were withdrawn from the array, it should improve the astrometric accuracy of the VLBA. We thus repeated our VLBA simulations without that station. The results of this test are given in Tables 11 and 12. In contrast to our intuition, the astrometric accuracy is actually degraded when the target-calibrator direction is oriented along declination. In fact, the addition of Saint Croix strengthens the geometry of the array and improves the astrometric accuracy despite severe weather conditions. In order to further explore this question, we ran simulations without Pie Town in the middle of the array and without Mauna Kea at the far West of the array. Withdrawing Pie Town does not change the astrometric accuracy but the absence of Mauna Kea degrades the accuracy in a similar way to Saint Croix.
An important question is whether the astrometric accuracy scales linearly as a function of the source separation. To study this matter, we repeated all the previous simulations but with source separations of and . Then, we performed a linear fit to the astrometric errors for the three values of the calibrator-target separation ( , and ), considering separately each systematic error component of the tables above. Figure 2 shows an example of such results for the VLBA in the case of a target at declination. Overall, our plots show that the astrometric accuracy generally scales fairly linearly as a function of the source separation.
Figure 2: Astrometric accuracy as a function of the relative source separation for a target-calibrator pair observed with the VLBA at a declination of . Each error component is represented with a different symbol and the total contributing error is also plotted. | |
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To obtain a quantitative measure of the likehood of the
linearity, we determined the regression coefficients for each of the 107 linear fits. Such coefficients should be close to 1 for a linear
behavior while they should decrease as the behavior becomes less
linear. This analysis reveals that 80% of the coefficients are larger
than 0.95, indicating that the astrometric errors behave
linearly. Among all errors, calibrator position systematics are those
that were found to behave the least linearly. An empirical formula for
the astrometric accuracy
has been further
estimated by averaging the parameters of all the fits:
As a verification of this empirical formula, we computed the astrometric accuracy for eight target-calibrator pairs observed with the global VLBI array as part of a project to monitor absolute lobe motions in compact symmetric objects (Charlot et al. 2005). For the source pair J2212+0152/J2217+0220 with a separation of along the right ascension direction, we obtained simulated accuracies as and as, versus as and as when derived from Eq. (2) and Table 9. In the worst case (target-calibrator J0754+5324/J0753+5352 with a separation of along declination), simulated accuracies were as and as while Eq. (2) and Table 10 give as and as. Thus, overall we found a discrepancy of a factor of 2 at most between our simple formula (Eq. (2)) and real simulation of the case considered.
We have performed extensive simulations of VLBI data with the VLBA, EVN and global VLBI array to study the dependence of the astrometric accuracy on systematic errors in the phase model of phase-referenced VLBI observations. Systematic errors considered in this study are calibrator position uncertainties, station coordinate uncertainties, Earth orientation parameters uncertainties and dry and wet troposphere errors. We have adopted state of the art VLBI values for these errors.
Our simulations show that the astrometric accuracy of a full track phase-referenced VLBI experiment is as at mid declination and is as at low ( ) and high ( ) declinations for point sources angularly separated by . Not surprinsingly, the major systematic error originates from wet tropospheric zenith delay uncertainties except at high declination where calibrator position uncertainties dominate. We show that the astrometric accuracy depends linearly on the source separation and we established the simple formula where is the astrometric error provided by our tables for the various arrays and configurations and is the source separation in degrees. Our study has been carried out for point sources but variable source structure is likely to degrade the accuracy derived from this formula.
Figure A.1: Astrometric errors and (respectively left and right) as a function of declination. The two upper plots are for the case and while the two lower plots are for the case and . The continuous dotted lines show the errors derived from the Shapiro et al. (1979) formulae. The stars show the errors from our simulations at six declinations from to . |
The analytical formulae in the Appendix A of Shapiro et al. (1979) provide
the astrometric errors caused by the inaccuracy of the calibrator
coordinates in the case of a single VLBI baseline. Adopting our
notation, these formulae become:
Adopting the same parameters as in our simulations ( mas, mas, or , or ), we obtain the astrometric errors plotted as a function of declination in Fig. A.1 (dotted lines). The results of our simulations for declinations of , , , , and in the case of the VLBA (first lines of Tables 3 and 4) are also superimposed on these plots.
The right ascension errors obtained from the simulations match perfectly those derived analytically, while the declination errors show a strong discrepancy near declination (although they agree at high declinations). This discrepancy originates from a singularity in the formula at (term in ), inherent to the approximation used to establish the formula (baseline declination of ). For a more complex and realistic network, such a singularity does not exist, as also demonstrated by the results of our simulations.