Spectral imaging of the Central Molecular Zone in multiple 7-mm molecular lines

TL;DR

This study maps 24 molecular spectral lines in the Central Molecular Zone using the Mopra telescope, analyzing their distribution, excitation conditions, and line ratios to understand the molecular environment near the Galactic Centre.

Contribution

First comprehensive 7-mm spectral line imaging of the CMZ, including principal component analysis and excitation modeling across multiple molecules.

Findings

Line ratios vary across the CMZ, higher near Sgr B2 and Sgr A.

Lines are sub-thermally excited under non-LTE conditions.

Densities are around 10^4 cm^{-3} based on RADEX modeling.

Abstract

We have imaged 24 spectral lines in the Central Molecular Zone (CMZ) around the Galactic Centre, in the range 42 to 50 GHz. The lines include emission from the CS, CH3OH, HC3N, SiO, HNCO, HOCO+, NH2CHO, OCS, HCS+, CCS, C34S, 13CS, 29SiO, H13CCCN, HCC13CN and HC5}N molecules, and three hydrogen recombination lines. The area covered is Galactic longitude -0.7 to 1.8 deg. and latitude -0.3 to 0.2 deg., including the bright cores around Sgr A, SgrB2, SgrC and G1.6-0.025. This work used the 22-m Mopra radio telescope in Australia, obtaining ~ 1.8 km/s spectral and ~ 65 arcsec spatial resolution. We present peak images from this study and conduct a principal component analysis on the integrated emission from the brightest 10 lines, to study similarities and differences in the line distribution. We examine the integrated line intensities and line ratios in selected apertures around the bright cores, as well as for the complete mapped region of the CMZ. We compare these 7-mm lines to the corresponding lines in the 3-mm band, for five molecules, to study the excitation. There is a variation in 3-mm to 7-mm line ratio across the CMZ, with relatively higher ratio in the centre around Sgr B2 and Sgr A. We find that the lines are sub-thermally excited, and from modelling with RADEX find that non-LTE conditions apply, with densities of order 10^4 cm^{-3}.