Towards the ICRF3: Comparing USNO 2016A VLBI Global Solution to Gaia and ICRF2 Megan Johnson in collaboration with Julien Frouard, Alan Fey, Valeri Makarov,

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Towards the ICRF3: Comparing USNO 2016A VLBI Global Solution to Gaia and ICRF2 Megan Johnson in collaboration with Julien Frouard, Alan Fey, Valeri Makarov, and Bryan Dorland 6 January 2018

Johnson - URSI - January 2018 Outline Introduction USNO 2016A Global Solution Comparison to ICRF2 Comparison to GAIA DR1 Results Future Prospects Conclusions Johnson - URSI - January 2018 2

International Celestial Reference Frame (ICRF) A brief history… The first realization (ICRF1) adopted by IAU on 1 January 1998 as the fundamental celestial reference frame replacing FK5 optical frame (Fricke+ 1988) ICRF1 contained Very Long Baseline Interferometry (VLBI) positions of a total of 608 compact radio sources Geodetic/astrometric data obtained from August 1979 through July 1995 Simultaneous observations made at S- and X-bands using a dichroic 212 “defining” compact radio sources independent of equator, equinox, ecliptic, and epoch 2 extensions added another 109 sources (Fey+ 2004) Some sources from the VLBA Calibrator Survey (VCS) (Beasley+ 2002) Johnson - URSI - January 2018

Spatial distribution of ICRF1 Beasley+ 2002 Johnson - URSI - January 2018

Johnson - URSI - January 2018 Introduction Current International Celestial Reference Frame, ICRF2 (Fey et al. 2015) Radio Astrometry catalog of 3414 radio loud quasars, Active Galactic Nuclei (AGN) 295 Defining Sources 2197 VLBA Calibrator Survey (VCS) sources 922 non-VCS sources Accuracy floor of ~40 μas for the whole dataset Not all sources have same astrometric quality! VCS sources only observed 1 time! Wide range of accuracies Johnson - URSI - January 2018

Johnson - URSI - January 2018 USNO 2016A (U16A) Solution Global solution includes data from the onset of VLBI in August 1979 through the present VLBI observations at 13 and 3.6 cm simultaneously Accurate calibration of Earth’s ionosphere Least-squares analysis over multiple channels in each band for precise group delay CALC/SOLVE software used for source position derivation (see Ma et al. 1986) U16A solution contains 4129 sources 295 defining sources 2195 VCS sources 921 non-VCS sources 718 new sources Johnson - URSI - January 2018

Johnson - URSI - January 2018 U16A Compared to ICRF2 Improved astrometric accuracy over ICRF2 Increased number of observations for VCS sources Offsets of 0.1 mas Johnson - URSI - January 2018

Johnson - URSI - January 2018 U16A Compared to ICRF2 Johnson - URSI - January 2018

Johnson - URSI - January 2018 U16A Compared to ICRF2 Johnson - URSI - January 2018

Johnson - URSI - January 2018 U16A Compared to Gaia Using Gaia Auxiliary Quasar Solution (AQS; Mignard+ 2016) to understand offset between U16A and ICRF2 U16A Johnson - URSI - January 2018

Johnson - URSI - January 2018 U16A Compared to Gaia Using Gaia AQS to understand offset between U16A and ICRF2 Johnson - URSI - January 2018

Johnson - URSI - January 2018 Results Johnson - URSI - January 2018

Johnson - URSI - January 2018 Results Johnson - URSI - January 2018

Johnson - URSI - January 2018 Results Johnson - URSI - January 2018

Johnson - URSI - January 2018 Results Johnson - URSI - January 2018

Johnson - URSI - January 2018 Results Johnson - URSI - January 2018

New Sources Compared to Gaia Out of 718 new sources in U16A, 415 matches within 150 mas of Gaia sources 22 outliers Johnson - URSI - January 2018

New Sources Compared to Gaia PanSTARRS DR1 images can help explain offset sources Extended Source Offset = 948 mas No Discernable Feature Offset = 309 mas Double Source Offset = 27 mas Johnson - URSI - January 2018

Johnson - URSI - January 2018 Future Prospects ICRF3 will debut at upcoming IAU general assembly Going forward with VLBA… Radio astrometry measurements key to maintaining ICRF Source structure studies currently underway Higher frequencies, i.e., Ka-band, allow for more compact source structure detections Wide bandwidth capabilities could transition to more accurate phase delay measurements Johnson - URSI - January 2018

Johnson - URSI - January 2018 Conclusions U16A has source position offsets of ~0.1 mas when compared to ICRF2 U16A global solutions are statistically more inline with Gaia than ICRF2 Systematic differences between ICRF2 and U16A? Those might be caused by observations from some of the AUST stations, from 2010 onwards 718 new radio sources in U16A Gaia contains 415 matches within 150 mas; 22 of these are outliers 10 out of 22 optical-radio offset sources can be explained when compared to PanSTARRS optically resolved images Future prospects for potentially higher frequencies and wide bandwidth capabilities on VLBA Johnson - URSI - January 2018