A search for the near-infrared counterpart of the eclipsing millisecond X-ray pulsar Swift J1749.4-2807

TL;DR

This study conducted deep near-infrared imaging of the field around Swift J1749.4-2807 during quiescence to search for its counterpart, aiming to enable future dynamical mass measurements of the neutron star.

Contribution

First deep NIR imaging campaign targeting Swift J1749.4-2807's quiescent counterpart, providing constraints on the companion star and guiding future phase-resolved observations.

Findings

Detected 41 sources within the X-ray error circle.

Identified potential variable sources consistent with expectations.

Provided constraints on the companion star's nature.

Abstract

Swift J1749.4-2807 is a transient accreting millisecond X-ray pulsars, the first that displayed X-ray eclipses. Therefore it holds a great potential for accurate mass measurements in a low mass X-ray binary system. The determination of the companion star radial velocity would make it possible to fully resolve the system and to accurately measure the mass of the neutron star based on dynamical measurements. Unfortunately, no optical/NIR counterpart has been identified to date for this system, either in outburst or in quiescence. We performed a photometric study of the field of Swift J1749.4-2807 during quiescence in order to search for the presence of a variable counterpart. The source direction lies on the Galactic plane, making any search for its optical/NIR counterpart challenging. To minimize the effects of field crowding and interstellar extinction, we carried out our observations using the adaptive optics near-infrared imager NACO mounted at the ESO Very Large Telescope. From the analysis of Swift X-ray data obtained during outburst, we derived the most precise (1.6" radius) position for this source. Due to the extreme stellar crowding of the field, 41 sources are detected in our VLT images within the X-ray error circle, with some of them possibly showing variability consistent with the expectations. We carried out the first deep imaging campaign devoted to the search of the quiescent NIR counterpart of Swift J1749.4-2807. Our results allow to provide constraints on the nature of the companion star of this system. Furthermore, they suggest that future phase-resolved NIR observations (performed with large aperture telescopes and adaptive optics) covering the full orbital period of the system are likely to identify the quiescent counterpart of Swift J1749.4-2807, through the measure of its orbital variability, opening the possibility of dynamical studies of this unique source.