Proplyds around a B1 star - 42 Orionis in NGC 1977

TL;DR

This paper reports the discovery of seven new proplyds around a B1 star in NGC 1977, the first such finding around a B star, and analyzes their properties and the effects of FUV radiation on their ionization fronts.

Contribution

It presents the first identification of proplyds around a B star and provides detailed observations and modeling of their ionization fronts and disks under weaker FUV radiation.

Findings

Seven new proplyds discovered around 42 Orionis in NGC 1977.

Proplyd ionization fronts point toward the B star, with tails pointing away.

Proplyd sizes are consistent with FUV photoevaporation models in weak radiation fields.

Abstract

We present the discovery of seven new proplyds (i.e. sources surrounded by cometary Halpha emission characteristic of offset ionization fronts) in NGC 1977, located about 30' north of the Orion Nebula Cluster at a distance of ~400 pc. Each of these proplyds are situated at projected distances 0.04-0.27 pc from the B1V star 42 Orionis (c Ori), which is the main source of UV photons in the region. In all cases the ionization fronts of the proplyds are clearly pointing toward the common ionizing source, 42 Ori, and 6 of the 7 proplyds clearly show tails pointing away from it. These are the first proplyds to be found around a B star, with previously known examples instead being located around O stars, including those in the Orion Nebula Cluster around $\theta^1$ Ori C. The radii of the offset ionization fronts in our proplyds are between ~200 and 550 AU; two objects also contain clearly resolved central sources that we associate with disks of radii 50-70 AU. The estimated strength of the FUV radiation field impinging on the proplyds is around 10-30 times less than that incident on the classic proplyds in the Orion Nebula Cluster. We show that the observed proplyd sizes are however consistent with recent models for FUV photoevaporation in relatively weak FUV radiation fields.