The New EXor Outburst of ESO-H-alpha~99 observed by Gaia ATLAS and TESS

TL;DR

This paper documents a detailed multi-wavelength observational study of the recent outburst of the young stellar object ESO-H-alpha 99, revealing its outburst characteristics, outflow activity, and spectral changes, suggesting it may be an intermediate-mass EXor-type star.

Contribution

It provides the first comprehensive multi-epoch, multi-wavelength analysis of ESO-H-alpha 99's outburst, including light curves, spectroscopy, and outflow imaging, highlighting its potential intermediate-mass status.

Findings

The outburst showed brightness fluctuations on timescales of days and hours.

Detection of a collimated outflow with a knot of H2 emission indicating recent activity.

Spectral analysis reveals increased continuum and decreased shock-excited lines during outburst.

Abstract

We report photometry and spectroscopy of the outburst of the young stellar object ESO-Halpha 99. The outburst was first noticed in Gaia alert Gaia18dvc and later by ATLAS. We have established the outburst light curve with archival ATLAS ``Orange'' filter photometry, Gaia data, new V-band photometry, and J, H, and K_s photometry from IRIS and UKIRT. The brightness has fluctuated several times near the light curve maximum. The TESS satellite observed ESO-Halpha 99 with high cadence during one of these minor minima and found brightness fluctuations on timescales of days and hours. Imaging with UKIRT shows the outline of an outflow cavity, and we find one knot of H_2 1-0 S(1) emission, now named MHO 1520, on the symmetry axis of this nebula, indicating recent collimated outflow activity from ESO-Halpha 99. Its pre-outburst SED shows a flat FIR spectrum, confirming its early evolutionary state and its similarity to other deeply embedded objects in the broader EXor class. The pre-outburst luminosity is 34 L_sun, a much higher luminosity than typical EXors, indicating that ESO-Halpha 99 may be a star of intermediate mass. Infrared and optical spectroscopy show a rich emission line spectrum, including HI lines, strong red CaII emission, as well as infrared CO bandhead emission, all characteristic EXors in the broadest sense. Comparison of the present spectra with an optical spectrum obtained in 1993, presumably in the quiescent state of the object, shows that during the present outburst the continuum component of the spectrum has increased notably more than the emission lines. The Halpha equivalent width during the outburst is down to one half of its 1993 level, and shock-excited emission lines are much less prominent.