The VSOP Survey: Final Individual Results R

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arXiv:astro-ph/0612373v2 20 Dec 2006 d E-mail: h g e b a c Toru´n, Poland 2006 26-29, September Symposium Network VLBI European 8th The Hirabayashi .Dodson R. results individual Final Survey: VSOP The

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a) Contribution from all antennae Survey b) 120 Code abcdefghji k lm nopq r s tuvwxyz 01 S 5.5 Jy Combined Mopra 100 02 3.3 Jy S 5.2 Jy Paper V 03 2.7 Jy S 3.3 Jy

Paper III HaRAO 04 2.2 Jy S 2.6 Jy Sheshan 80 Hobart 05 1.9 Jy S 2.2 Jy 06 1.7 Jy S 1.9 Jy 07 1.5 Jy S 1.7 Jy 60 08 1.3 Jy S 1.5 Jy

Mauna Kea 09 1.2 Jy S 1.3 Jy Kashima St. Croix 10 1.1 Jy S 1.2 Jy

Number of experiments 40 11 1.0 Jy S 1.1 Jy Usuda 12 S = 1.0 Jy Ceduna N. Liberty Hancock Noto Kalyazin Brewster Pie Town 13 20 Green Bank Los Alamos ATCA Effelsburg Fort Davis Kitt Peak Arecibo

Owens Valley Paper III Torun Onsala Jodrell Bank VLA Medicina 0 Paper V 0 5 10 15 20 25 30 No Space fringes Not observed Failed Rank

Figure 1: a) A histogram of the contribution of all 28 antennae used to make the VSOP survey images, for Paper III, V and both. b) The ﬁnal status of all the VSOP survey targets.

1. Introduction

The VLBI Space Observing Program (VSOP) satellite HALCA provided the space baseline for the observation of a complete sample of bright compact Active Galactic Nuclei (AGNs) at 5 GHz; the VSOP survey [2]. Of this set of 294 AGNs: 102 were presented in [4] (hereafter P-III), 140 will be presented in [1] (hereafter P-V), and 29 were not observed. The remaining 23 did not produce space fringes, where we expected to find them. These maybe the true result, however we have erred on the side of caution and consider them to be failures. Figure 1a) plots the contribution of all the antennae to the published, or to be published, experiments, and Figure 1b) plots the final status of all the survey experiments. The images produced are compared, where possible, to both the General Observing Time (GOT), and any other available, images. We confirmed, as reported in [3], that the Survey data reproduces that of the more completely sampled images. See Figure 2 which plots all the images from P-V.

2. Conclusions

We have completed the VSOP survey imaging data reduction. The paper covering 140 sources is in preparation, and when it is published the imaging portion of the VSOP Survey Project will be completed. All the images from the ﬁnal paper are shown in a montage.

Acknowledgments

The contributions of very many people have been essential to the success of the VSOP Survey project. Many more than can be included in the list of authors. We wish to recognise and thank them for their contributions.

References

[1] Dodson, R., et al., 2007, in preparation, P-V [2] Hirabayashi H., et al., 2000, PASJ, 52, 997 , P-I [3] Lister M. L., Piner B. G., Tingay S. J., 2000, Astrophysical Phenomena Revealed by SVLBI, Proceedings of the VSOP Symposium, eds: H. Hirabayashi, P. G. Edwards, & D. W. Murphy, p. 189 [4] Scott W. K., et al., 2004, ApJS, 155, 33, P-III

2 The VSOP Survey: Final individual results R. Dodson

Figure 2: A montage of all the images which will appear in the VSOP Survey Paper V.

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a) Number of GRTs for paper III, V and combined b) Tb distrubtion for sources in PV 120 35

Combined 30 100 Paper V

Paper III 25 80

Number of experiments 40 10

20 5

0 0 0 1 2 3 4 5 6 7 0 1 2 3 4 5 6 7 8 Number of antennae Tb in units of 10^12 K Figure 1. a) A histogram of the number of antennae for experiments in P-III, V and both. b) A histogram of the upper limits to the source rest frame brightness temperatures from the imaged data in P-V, in logarithmic bins.

One of the core goals of the VSOP Survey imaging program was to measure lower limits to the brightness temperatures (Tb) directly from the data (c.f. Horiuchi et al. 2004). The determined Tb (from VLBI) depends only on the physical baseline length, independent of frequency, so space baselines will always provide the highest possible limits. Figure 1b) plots the lower limits to Tb for the sources in P-V, binned logarithmically. These are the source frame Tb values, unless the redshift is unknown. In which case the observer frame values are used, as a lower limit. Lower limits were estimated from the lowest brightness temperature model compatible with the data.

2. Conclusions We have completed the VSOP survey imaging data reduction. The paper covering 140 sources is in preparation, and when it is published the imaging portion of the VSOP Survey Project will be completed. We have directly measured the source brightness temperatures, and produce a distribution of the lower limits to directly measured Tb.

Acknowledgements RD, KJW and JEJL acknowledge support from the Japan Society for the Promo- tion of Science. WKS wishes to acknowledge support from the Canadian Space Agency. SH acknowledges support through an NRC/NASA-JPL Research Associateship. SF acknowledges the Bolyai Scholarship received from the Hungarian Academy of Sciences. RD wishes to thank S. Lorenzo. The NRAO is a facility of the National Science Foundation, operated under cooperative agreement by Associated Universities, Inc. The Australia Telescope Compact Array is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO.

References Dodson, R., et al., 2007, in preparation, P-V Hirabayashi H., et al., 2000,PASJ, 52, 997, P-I Horiuchi S., et al., 2004, ApJ, 616, 110, P-IV Scott W. K., et al., 2004, ApJS, 155, 33, P-III