– & (2.9$^{+0.4}_{-0.3}$) $\times$ 10$^{-5}$ & (3.0$^{+0.4}_{-0.4}$) $\times$ 10$^{-13}$ & 36.89/32\
*diskbb* & 0.02$^{+0.02}_{-0.02}$ & 2.1$^{+0.3}_{-0.4}$ & – & – & – & –& (8$^{+7}_{-3}$) $\times$ 10$^{-4}$ & (3.0$^{+0.4}_{-0.3}$) $\times$ 10$^{-13}$ & 39.97/34\
*comptt* & 0.02$^{+0.03}_{-0.02}$ & – & – & 0.03$^{+0.1}_{-0.03}$ & 1.2$^{+0.2}_{-0.2}$ & 17$^{+3}_{-3}$ & (1.3$^{+1.0}_{-0.5}$) $\times$ 10$^{-4}$ & (2.9$^{+0.3}_{-0.3}$) $\times$ 10$^{-13}$ & 35.01/32\

![Fit to a power-law (top) and a thermal Comptonization model (bottom) to the *Swift* XRT combined spectrum of N4088–X1. \[figSwift\]](powplot3.pdf "fig:") ![Fit to a power-law (top) and a thermal Comptonization model (bottom) to the *Swift* XRT combined spectrum of N4088–X1. \[figSwift\]](comptt.pdf "fig:")

Radio counterpart of the ULX {#radiocounterpart}
----------------------------

A 1.6 GHz radio counterpart to N4088–X1 consistent with the *ROSAT* X-ray detection was reported by [@2011AN....332..379M]. The *Chandra* position of N4088–X1 obtained here reveals an offset of 6 arcsec between the X-ray position and the 1.6 GHz EVN radio source of [@2011AN....332..379M], which can now be ruled out as a candidate counterpart of the ULX.

The reanalysis of the 1.6 GHz using a FOV of 1 arcsec around the *Chandra* position yields the detection of compact radio emission consistent, within 0.3 arcsec, with the *Chandra* positional error (component A in Fig. \[radio\]). This compact 