First firm spectral classification of an early-B pre-main-sequence star: B275 in M17

TL;DR

This study presents the first firm spectral classification of an early-B pre-main-sequence star, B275, using optical to near-infrared spectroscopy, revealing its physical properties and evolutionary status in M17.

Contribution

It provides the first definitive spectral classification of an early-B PMS star and clarifies its position above the main sequence, contributing to understanding massive star formation.

Findings

B275 is classified as B6-B7 spectral type.

The star is likely a bloated pre-main-sequence object.

Position in HR diagram suggests ongoing but moderate accretion.

Abstract

The optical to near-infrared (300 - 2500 nm) spectrum of the candidate massive Young Stellar Object (YSO) B275, embedded in the star forming region M17, has been observed with X-shooter on the ESO Very Large Telescope. The spectrum includes both photospheric absorption lines and emission features (H and Ca triplet emission lines, 1st and 2nd overtone CO bandhead emission), as well as an infrared excess indicating the presence of a (flaring) circumstellar disk. The strongest emission lines are double-peaked with a peak separation ranging between 70 and 105 km s^-1 and provide information on the physical structure of the disk. The underlying photospheric spectrum is classified as B6-B7, significantly cooler than a previous estimate based on modeling of the spectral energy distribution. This discrepancy is solved by allowing for a larger stellar radius (i.e. a bloated star), and thus positioning the star above the main sequence. This constitutes the first firm spectral classification of an early-B pre-main-sequence (PMS) star. We discuss the position of B275 in the Hertzsprung-Russell diagram in terms of PMS evolution. Although the position is consistent with PMS tracks of heavily accreting protostars (Macc > 10^-5 Msun yr^-1), the fact that the photosphere of the object is detectable suggests that the current mass-accretion rate is not very high.