Schedule and Abstract book
Schedule in brief
Twelfth IVS General Meeting
Oral sessions in Zoom, poster sessions via Wonder.me
All times in UT
Monday, March 28, 2022
09:00–11:00 Opening and Oral Session 1
11:15–13:00 Oral Session 1
13:15–14:45 Poster Block A (Sessions 1+5)
Tuesday, March 29, 2022
09:00–11:00 Oral Session 2
11:15–12:30 Oral Session 2
12:45–14:15 Poster Block B (Sessions 2+4)
Wednesday, March 30, 2022
09:00–11:00 Oral Session 3
11:15–13:00 Oral Session 3
13:15–14:30 Poster Block C (Session 3)
Thursday, March 31, 2022
09:00–11:00 Oral Session 4
11:15–12:30 Oral Session 4
12:45–14:30 Oral Session 5 and Closing
Friday, April 1, 2022
09:00–10:45 IVS Analysis Workshop
11:00–12:45 IVS Analysis Workshop
13:00–14:30 Correlator Workshop on Polconvert
Information for oral presentations
- All contributed talks are 12 minutes plus 3 minutes of discussion.
- The oral program will be held via Zoom. The corresponding Zoom invite will be distributed in mid-March.
Information for poster and recorded (movies) presentations
- The poster/movie program will be held via Wonder.me in three blocks on Monday, Tuesday, and Wednesday.
- Posters should be prepared as a PDF. You have free choice of portrait vs. landscape orientation as well as equivalent paper size (like A0, A1).
- Movies should be prepared as MP4 or QuickTime (MOV). The length of each movie should not be longer than 15 min. The file size limit is 400 MB.
- Please use the following file name convention:
[Poster|Movie number]_[lastname of first author].[pdf|mp4]
- Both poster PDF and movie MP4 (or MOV) files should be sent to the local host by March 25. Please send an email to Nataliya Zubko <email@example.com>. You can send a file as an attachment in the email when the file size is below 10 MB. For larger files, please provide a link from where to download the file (e.g., using Google Drive or Dropbox).
- The files will be made available for download for all participants via a shared Google Drive link:
- Attendants are encouraged to access the files prior to each poster block.
Session 1: Technical Developments at the Stations
Conveners: Nataliya Zubko, Stuart Weston, José A. López-Pérez
The goals of this decade for the global VLBI network are to provide unprecedented accuracies for geodetic results including station positions and velocities (1 mm and 0.1 mm/yr) and Earth orientation parameters. Therefore, the IVS is introducing the VLBI Global Observing System (VGOS).
For the past two decades, the operational products of the IVS have been based on observations made by the legacy S/X network stations which still form the backbone of today’s product generation. In 2019, the evolving VGOS network has matured enough that initial operational products could be derived. It is anticipated that the maturation of the VGOS system and the build-out of the VGOS network will advance in 2020 and subsequent years until VGOS can replace S/X as the production system of the IVS.
In this session we seek contributions which demonstrate the efforts of improving the VLBI systems. We request contributions covering aspects on station activities, recent developments, simulations, studies on how to improve the network, status and progress reports for VGOS and legacy systems. The technical developments may cover all signal chain components at the stations (feeds, backends, recording systems) but also reference frequency generation and distribution, timing systems, e-transfer, and RFI excision techniques, among others.
Session 2: Observations, Operation and Correlation
Conveners: Fengchun Shu, Chet Ruszczyk, Phillip Haftings
This session focuses on the present and near-term future activities at VLBI network stations and correlators. This includes reports from the stations and correlators as well as reports about mixed-mode observations and legacy-to-VGOS local ties. We also encourage performance reports for the various IVS observing series (e.g., R1/R4, T2, VO) and any suggested actions to improve quality. In addition, we solicit presentations about issues that relate to improving VLBI data quality product. The near-term future topics could cover presentations about strategies for the transition from the current network to the VGOS network, such as network compatibilities, and investigations of the effect of station and correlation centers conversion to VGOS broadband. In particular, we welcome contributions that deal with improving the efficiency of VLBI data processing such as automation of correlation or post-correlation processing. Furthermore, we welcome submissions concerning the GGOS project's contributions to local surveys to determine the spatial vectors from the radio telescopes to co-located geodetic instruments.
Session 3: Data Structures, Scheduling and Analysis Strategies
Conveners: Anastasiia Girdiuk, John Gipson, Matthias Schartner
IVS Operations Centers are responsible for the scheduling of IVS sessions. IVS Data Centers are responsible for storing and distributing IVS data, and IVS Analysis Centers are responsible for the analysis of IVS sessions, and the production of IVS data products. These functions are interdependent: what happens at one stage of the processing depends on what happens both before and after. In this session, we call for contributions related to the IVS Operations, Data and Analysis Centers' current activities and plans for the future. VLBI data will increase dramatically (a factor of 10-100) in the future because of VGOS. Because of this, we are especially interested in the planned strategies to automate scheduling, data collection, processing and analysis. Presentations related to the comparison and development of analysis strategies are welcomed, as are changes and new strategies that need to be considered due to VGOS and existing or new user requirements.
Session 4: Interpretation of VLBI Results in Geophysics, Geodesy and Astrometry
Conveners: Lucia McCallum, James Anderson, Chris Dieck
The analysis of VLBI observations produces values, time series, and long-term averages & rates of physical parameters. Analysis of particular sessions also produces images of celestial reference frame objects. We seek contributions in topics such as the use of these VLBI products in modeling geophysical fluids from the atmosphere to the core, improvement of the precession-nutation model, investigation of the Earth rotation variations at different time scales, refinement of the terrestrial and celestial reference frames, detection and interpretation of the motions of specific sites and radio sources, atmospheric studies, astrophysical investigations, tests of relativity, and other scientific uses of geodetic and astrometric VLBI data and images. Other important topics are the comparison, validation, and combination of VLBI with other space geodetic techniques where special attention is expected to be given to the assessment of the actual accuracy and systematic errors of the VLBI-derived results. Studies about the VLBI contribution to ITRF2020, in particular the impact of new stations and networks as well as of VGOS and mixed mode observations are welcome. As VGOS operations develop, we are also particularly interested in presentations on the impacts of quasar source structure variability on the ability to meet the precision goals of VGOS and the subsequent implications on the effort required to maintain the celestial reference frame. We further explicitly welcome contributions about effects of the new IAU resolutions on VLBI results.
Session 5: Extending the Use of VLBI to Frame Ties, Deep Space Exploration and other areas
Conveners: Alet de Witt, Megan Johnson, Benedikt Soja
VLBI observations have contributed greatly to astrometric and geodetic studies, including the construction and maintenance of the celestial and terrestrial reference frames (CRF, TRF), as well as the precise determination of the Earth Orientation Parameters (EOP). They also have contributed significantly to geophysical studies such as modeling of tides and the deep Earth structure. Currently, efforts are underway to extend the use of VLBI observations to frame ties and deep space exploration. For instance, VLBI observations of satellites could facilitate the determination of reference frame tie parameters allowing to study and remove possible systematic errors of various frames or improve the reliability and precision of navigation and positioning applications. VLBI observations have already tremendously contributed to the Lunar and Mars exploration efforts both in orbit determination and positioning of deep space probes. VLBI observations of objects of the Gaia frame enable precise frame ties and thus also to improve the determination precision of the EOP. Geophysical and astrophysical studies require contributions from astrometric and geodetic VLBI observations. In this session, we seek contributions to extend VLBI observations to objects of the Gaia frame to enable precise frame ties (see Resolution B3 adopted at the XXXIst IAU General Assembly), multi-wavelength celestial reference frames, deep space exploration, demands of astrometric and geodetic VLBI observations to geophysical and astrophysical studies, and other novel applications. We also welcome contributions on methodology demonstration, technical verification, and observation practice.