English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Recent studies have proposed that GRAVITY+ instrument is able to trace thecircular orbit of the subparsec close-binary supermassive black holes(CB-SMBHs) by measuring the photocentre variation of the hot dust emission.However, the CB-SMBHs orbit may become highly eccentric throughout theevolution of these objects, and the orbital period may be far longer than theobservational time baseline. We investigate the problem of detecting theCB-SMBH with hot dust emission and high eccentricity (eCBSMBH, e=0.5) when theobserved time baselines of their astrometric data and radial velocities areconsiderably shorter than the orbital period. The parameter space of theKeplerian model of the eCBSMBH is large for exploratory purposes. We thereforeapplied the Bayesian method to fit orbital elements of the eCBSMBH to combinedradial velocity and astrometric data covering a small fraction of the orbitalperiod. We estimate that a number of potential eCBSMBH systems within reach ofGRAVITY + will be similar to the number of the planned circular targets. Weshow that using observational time baselines that cover ~ 10% of the orbitincreases the possibility of determining the period, eccentricity, and totalmass of an eCBSMBH. When the observational time baseline becomes too short (~5%), the quality of the retrieved eCBSMBH parameters degrades. We alsoillustrate how interferometry may be used to estimate the photo-centre at theeCBSMBH emission line, which could be relevant for GRAVITY+ successors. Even ifthe astrometric signal for eCBSMBH systems is reduced by a factor ofsqrt{1-e^{2}} compared to circular ones, we find that the hot dust emission ofeCBSMBHs can be traced by GRAVITY+ at the elementary level.

Detection of eccentric close-binary supermassive black holes with incomplete interferometric data