The VMC Survey - VI. Quasars behind the Magellanic system

TL;DR

This study develops criteria using VISTA survey data to identify quasars behind the Magellanic Clouds, enhancing their use as astrometric references by cataloging and analyzing their photometric and variability properties.

Contribution

The paper introduces new selection criteria based on YJKs photometry and Ks light-curve slopes to identify high-confidence QSO candidates behind the Magellanic system.

Findings

Approximately 75% of known QSOs show irregular Ks-band variability.

Found 22 and 26 QSO candidates in specific regions, with about 20% contamination.

Projected to find around 1800 QSOs in total across the survey area.

Abstract

The number and spatial distribution of confirmed quasi-stellar objects (QSOs) behind the Magellanic system is limited. This undermines their use as astrometric reference objects for different types of studies. We have searched for criteria to identify candidate QSOs using observations from the VISTA survey of the Magellanic Clouds system (VMC) that provides photometry in the YJKs bands and 12 epochs in the Ks band. The (Y-J) versus (J-Ks) diagram has been used to distinguish QSO candidates from Milky Way stars and stars of the Magellanic Clouds. Then, the slope of variation in the Ks band has been used to identify a sample of high confidence candidates. These criteria were developed based on the properties of 117 known QSOs presently observed by the VMC survey. VMC YJKs magnitudes and Ks light-curves of known QSOs behind the Magellanic system are presented. About 75% of them show a slope of variation in Ks>10^-4 mag/day and the shape of the light-curve is in general irregular and without any clear periodicity. The number of QSO candidates found in tiles including the South Ecliptic Pole and the 30 Doradus regions is 22 and 26, respectively, with a ~20% contamination by young stellar objects, planetary nebulae, stars and normal galaxies. By extrapolating the number of QSO candidates to the entire VMC survey area we expect to find about 1200 QSOs behind the LMC, 400 behind the SMC, 200 behind the Bridge and 30 behind the Stream areas, but not all will be suitable for astrometry. Further, the Ks band light-curves can help support investigations of the mechanism responsible for the variations.