# Searching for the Donor Stars of ULX Pulsars

## TL;DR

This study searches for optical counterparts of two ultraluminous X-ray pulsars using HST data, aiming to identify their donor stars and understand their nature, with mixed results and some candidate identifications.

## Contribution

First detailed optical counterpart search for ULX pulsars M82 X-2 and NGC 5907 X-1, providing candidate donor stars and insights into their properties.

## Key findings

- Detected potential donor star candidates for M82 X-2.
- Did not find the expected red giant donor for NGC 5907 X-1.
- Identified possible AGB star counterparts for NGC 5907 ULX-2.

## Abstract

We report on our search for the optical counterparts of two ultraluminous X-ray pulsars with known orbital periods, M82 X-2 and NGC 5907 X-1, in new and archival HST observations, in an effort to characterize the donor stars in these systems. We detect five near-infrared sources consistent with the position of M82 X-2 that are too bright to be single stars. We also detect seven sources in the WFC3/UVIS F336W image whose photometry matches that of 10-15 M$_\odot$ stars turning off the main sequence. Such stars have densities consistent with the properties of the donor star of M82 X-2 as inferred from X-ray timing analysis, although it is also possible that the donor is a lower mass star below our detection limit or that there is a significant contribution from the accretion disc to the optical emission. We detect three candidate counterparts to NGC 5907 X-1 in the near-infrared. All of these are too bright to be the donor star of the ULX, which based on its orbital period is a red giant. The high background at the location of NGC 5907 X-1 precludes us from detecting this expected donor star. The recently discovered NGC 5907 ULX-2 also falls within the field of view of the near-infrared imaging; we detect four sources in the error circle, with photometry that matches AGB stars. The star suggested to be the counterpart of NGC 5907 ULX-2 by Pintore et al. (2018) falls outside our 2-$\sigma$ error circle.