Deep HI Mapping of M 106 Group with FAST

TL;DR

This study used FAST to perform deep HI imaging of the M 106 group, discovering new HI structures, identifying satellite galaxies, and analyzing their properties and interactions, providing insights into galaxy evolution and quenching mechanisms.

Contribution

First deep HI mapping of the M 106 group with FAST, revealing new HI filaments, clouds, and satellite galaxy properties, and analyzing their interactions and star formation activity.

Findings

Discovered new HI filaments and clouds connecting DDO 120 and NGC 4288.

Identified 11 satellite galaxies of M 106 with M_B < -10.

Satellite galaxies with lower stellar masses deviate more from the star-forming main sequence.

Abstract

We used FAST to conduct deep HI imaging of the entire M 106 group region, and have discovered a few new HI filaments and clouds. Three HI clouds/filaments are found in a region connecting DDO 120 and NGC 4288, indicating an interaction between these two galaxies. The HI features in this region suggest that DDO 120 is probably the origin of the HI stream extending from the northern end of NGC 4288 to M 106. This structure is similar to the SMC-LMC stream, but much longer, about 190 kpc. Furthermore, based on the distance measurements, we have determined the satellite galaxy members of M 106. With an absolute magnitude cutoff of M_B=-10, we obtained a sample of 11 member satellite galaxies for M 106. Using the observed HI mass with FAST, we studied the properties of satellite galaxies in M 106 and found that satellite galaxies with lower stellar masses exhibit more significant deviations from the star-forming main sequence (SFMS) in their specific star formation rates. Furthermore, the relationship between the HI mass of satellite galaxies and optical diameter generally follows the field galaxies relation. We discuss the possible mechanisms leading to the quenching in the M 106 group based on the new data from FAST