The Peculiar Astrometric Behaviour and Radio Structure of the Quasar 1524-136 Revealed with Very Long Baseline Interferometry

@misc{osetrova2026peculiar,
  title = {{The Peculiar Astrometric Behaviour and Radio Structure of the Quasar 1524-136 Revealed with Very Long Baseline Interferometry}},
  author = {Angelina Osetrova and Sándor Frey and Oleg Titov and Alexey Melnikov and Panna Gelle},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2610.39603},
  eprint = {2610.39603},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2610.39603},
}

TY  - UNPB
TI  - The Peculiar Astrometric Behaviour and Radio Structure of the Quasar 1524-136 Revealed with Very Long Baseline Interferometry
AU  - Angelina Osetrova
AU  - Sándor Frey
AU  - Oleg Titov
AU  - Alexey Melnikov
AU  - Panna Gelle
PY  - 2026
DA  - 2026/10/29
PB  - arXiv
DO  - 10.48550/arxiv.2610.39603
UR  - https://arxiv.org/abs/2610.39603
AB  - According to astrometric very long baseline interferometry (VLBI) observations accurate to sub-milliarcsecond levels, the radio quasar 1524-136 (J1526-1351) exhibited an exceptionally large shift, more than 0.1", between the 1990s and 2010s. This luminous quasar is known for its extended (~0.4"), highly asymmetric and non-collinear jet structure. Here we analyse historical VLBI astrometric and imaging data, as well as Gaia optical astrometric information, to find the cause of the sudden apparent change in the position. At the X band (~8.4 GHz frequency), where radio positions are conventionally measured, the core region brightened substantially relative to the hotspot at the end of the northern jet. As a result, the brightness peak shifted from the hotspot to the core, causing the VLBI position to shift accordingly. Similar changes could affect the astrometric positions of other radio sources. A better understanding of the astrophysical reasons behind them is important for maintaining the stability of the VLBI-based celestial reference frame.
ER  -