Identifying Compact Object Candidates using Gaia DR3 Astrometric Accelerations and Jerks
Abstract
Gaia Data Release 3 (DR3) provides astrometric measurements for more than a billion sources, hundreds of thousands of which have non-single-star astrometric solutions that indicate deviations from linear proper motion. Although sources with orbital solutions have been extensively inspected for compact objects via the astrometric mass function, two other solution types--the 7-parameter constant-acceleration solutions characterized by μ̇, and the 9-parameter variable-acceleration solutions characterized by μ̇ and μ̈--have not been as carefully explored. In this work, we develop a methodology for selecting sources within the Gaia DR3 9-parameter non-single-star astrometric solutions that are most likely to host massive compact companions. We assume that a source is the luminous star in a binary orbit around a dark object and derive analytic expressions for the sky-projected accelerations and jerks for three binary populations with different orbit approximations: inclined eccentric, face-on eccentric, and face-on circular. Using POSYDON, we develop a fourth, more realistic population of binaries, each consisting of a luminous star and a black hole. For each population, we address observational biases using gaiamock and select only the systems it fits with a 9-parameter solution. We find that binaries likely to host massive compact companions can be identified from the characteristic joint astrometric accelerations and jerks exhibited by the luminous stars, despite 9-parameter fits under-constraining full orbits. Finally, to illustrate the utility of our approach, we analyze a historical object of interest, HD 12871, and examine 9-parameter fits of Gaia BH3-like binaries.
Related
- Beyond what's observed: hierarchical inference of Gaia astrometric compact-object binaries
- High-Priority Compact-Object Candidates in Young Clusters from the \textit{Gaia} DR3 Non-Single-Star Catalog
- A Sample of Long-Period Binaries with Dormant Compact-Object Candidates from LAMOST DR13 MRS and Gaia DR3
- A Sample of Long-period Binaries with Dormant Compact-object Candidates from LAMOST DR13 MRS and Gaia DR3
- Spectroscopic follow-up of compact object binary candidates from Gaia DR3: White dwarfs, neutron stars, black holes, and the parallax zeropoint
BibTeX
@misc{kinnion2026identifying,
title = {{Identifying Compact Object Candidates using Gaia DR3 Astrometric Accelerations and Jerks}},
author = {Andrew Kinnion and Jeff J. Andrews and Eirini Kasdagli},
howpublished = {arXiv},
year = {2026},
month = nov,
doi = {10.48550/arxiv.2611.05536},
eprint = {2611.05536},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2611.05536},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Identifying Compact Object Candidates using Gaia DR3 Astrometric Accelerations and Jerks
AU - Andrew Kinnion
AU - Jeff J. Andrews
AU - Eirini Kasdagli
PY - 2026
DA - 2026/11/03
PB - arXiv
DO - 10.48550/arxiv.2611.05536
UR - https://arxiv.org/abs/2611.05536
AB - Gaia Data Release 3 (DR3) provides astrometric measurements for more than a billion sources, hundreds of thousands of which have non-single-star astrometric solutions that indicate deviations from linear proper motion. Although sources with orbital solutions have been extensively inspected for compact objects via the astrometric mass function, two other solution types--the 7-parameter constant-acceleration solutions characterized by μ̇, and the 9-parameter variable-acceleration solutions characterized by μ̇ and μ̈--have not been as carefully explored. In this work, we develop a methodology for selecting sources within the Gaia DR3 9-parameter non-single-star astrometric solutions that are most likely to host massive compact companions. We assume that a source is the luminous star in a binary orbit around a dark object and derive analytic expressions for the sky-projected accelerations and jerks for three binary populations with different orbit approximations: inclined eccentric, face-on eccentric, and face-on circular. Using POSYDON, we develop a fourth, more realistic population of binaries, each consisting of a luminous star and a black hole. For each population, we address observational biases using gaiamock and select only the systems it fits with a 9-parameter solution. We find that binaries likely to host massive compact companions can be identified from the characteristic joint astrometric accelerations and jerks exhibited by the luminous stars, despite 9-parameter fits under-constraining full orbits. Finally, to illustrate the utility of our approach, we analyze a historical object of interest, HD 12871, and examine 9-parameter fits of Gaia BH3-like binaries.
ER -