# Searching for Faint X-ray Emission from Galactic Stellar Wind Bow Shocks

## TL;DR

This study uses archival Chandra data to set upper limits on X-ray emissions from stellar wind bow shocks, compares properties of bow shock stars to other OB stars, and evaluates Lynx observatory's detection prospects.

## Contribution

It provides the most stringent X-ray luminosity upper limits for bow shocks and assesses future detection capabilities with Lynx.

## Key findings

- Upper limit on X-ray luminosity of bow shocks is <2×10^{29} erg/s.
- No high L_X/L_bol ratios indicative of magnetic stars in the sample.
- Lynx could detect the nearest bow shocks with ~100 ks exposure.

## Abstract

We present a stacking analysis of 2.61 Msec of archival Chandra observations of stellar wind bow shocks. We place an upper limit on the X-ray luminosity of IR-detected bow shocks of $<2\times10^{29}$ erg s$^{-1}$, a more stringent constraint than has been found in previous archival studies and dedicated observing campaigns of nearby bow shocks. We compare the X-ray luminosities and $L_X/L_{\rm bol}$ ratios of bow shock driving stars to those of other OB stars within the Chandra field of view. Driving stars are, on average, of later spectral type than the "field of view" OB stars, and we do not observe any unambiguously high $L_X/L_{\rm bol}$ ratios indicative of magnetic stars in our sample. We additionally asses the feasibility of detecting X-rays from stellar wind bow shocks with the proposed Lynx X-ray Observatory. If the X-ray flux originating from the bow shocks is just below our Chandra detection limit, the nearest bow shock in our sample (at $\sim$0.4 kpc with an absorbing column of $\sim10^{21}$ cm$^{-2}$) should be observable with Lynx in exposure times on the order of $\sim$100 kiloseconds.