Closing the gap: Follow-up observations of peculiar dusty objects close to Sgr A* using ERIS

TL;DR

This study uses the upgraded ERIS instrument to observe and analyze the trajectories and properties of dusty objects near Sgr A*, aiming to understand their evolution and nature through high-resolution spectroscopy.

Contribution

It provides new observations of G objects near Sgr A* with ERIS, extending the data baseline and analyzing their Keplerian orbits and emission properties to clarify their nature.

Findings

Extended data on G2/DSO's orbit and luminosity changes

Insights into the evolution of dusty G objects near Sgr A*

Refined understanding of the environment around Sgr A*

Abstract

Context. In addition to the supermassive black hole Sgr A*, the inner parsec of our Galactic center is home to numerous fruitful scientific habitats. One of these environments is the S cluster, which consists of two distinct populations: the main-sequence S stars and the dusty G objects. While the majority of the brightest S stars can be classified as young B stars, the G sources can be described as dusty objects whose nature is still under debate. Aims. In this work, we focus on the most prominent G objects in the S cluster and follow their Keplerian trajectory around Sgr A*. With this, we test the predictions based on almost two decades of monitoring of the direct vicinity of our central supermassive black hole using NACO and SINFONI, formerly mounted at the Very Large Telescope (VLT). The goal is to increase the existing data baseline for G2/DSO, D9, and X7 to get insights into their evolution on their Keplerian trajectories. In addition, we revisit the massive Young Stellar Object (YSO) X3 and scrutinize the potential impact of its environment on this highly dynamic source. Methods. The successor to the two instruments is called ERIS and offers upgraded optics and improved properties, including an enhanced spectral resolution. We utilize the IFU mode of ERIS, called SPIFFIER. We search for the Doppler-shifted Br{\gamma} emission line to rediscover peculiar objects in the S cluster using SPIFFIER with the highest available spatial plate scale of 12.5 mas. Furthermore, we will derive the Br{\gamma} luminosity of G2/DSO to inspect the degree of its change more than ten years after the pericenter passage. If present, a decrease in the Br{\gamma} luminosity of G2/DSO on its descending part of the orbit would directly impact the direction of the debate about its nature.