component A is detected at a 5.2$\sigma$ level and is centered at RA(J2000) = 12$^h$05$^m$32$^s$.3048 $\pm$ 0.0004$^s$, Dec.(J2000) = 50$^{\circ}$3246.140 $\pm$ 0.004. It has an integrated flux density of 49 $\mu$Jy, from which we derive a 1.6 GHz luminosity $L_\mathrm{1.6 GHz}= 1.6 \times 10^{34}$ erg s$^{-1}$. The AIPS task JMFIT is used to fit an elliptical Gaussian to this peak of emission, which yields a lower limit on the brightness temperature T$_\mathrm{B}$ $>$ 3 $\times$ 10$^{4}$ K.

A second component (labeled B in Fig. \[radio\]) is detected at 5.4$\sigma$ level offset 0.6 arcsec from the *Chandra* X-ray position. Component B is centered at RA(J2000) = 12$^h$05$^m$32$^s$.2983 $\pm$ 0.0003$^s$, Dec.(J2000) = 50$^{\circ}$3245.398 $\pm$ 0.003, and has an integrated flux density of 55 $\mu$Jy, from which we derive a 1.6 GHz luminosity $L_\mathrm{1.6 GHz}= 1.8 \times 10^{34}$ erg s$^{-1}$ assuming it is in NGC4088. The fit of an elliptical Gaussian to this peak of emission yields a lower limit on the brightness temperature T$_\mathrm{B}$ $>$ 3 $\times$ 10$^{4}$ K.

![1.6 GHz EVN image at the *Chandra* position of N4088–X1. The contours are (3, 4, 5) times the off-source rms noise of 11 $\mu$Jy beam$^{-1}$. Two compact components labelled A and B are 