The evolutionary sequence of sub-mm galaxies: from diffuse discs to massive compact ellipticals?

TL;DR

This study analyzes the morphologies and sizes of 12 high-redshift sub-mm galaxies, supporting an evolutionary sequence from gas-rich discs to compact ellipticals via mergers, aligning with theoretical models.

Contribution

It provides observational evidence for an evolutionary pathway of SMGs transforming from diffuse discs to compact ellipticals through mergers.

Findings

33% of galaxies show signs of mergers or interactions

42% are diffuse, regular disc-like objects

25% are very compact, spheroidal systems

Abstract

The population of compact massive galaxies observed at z > 1 are hypothesised, both observationally and in simulations, to be merger remnants of gas-rich disc galaxies. To probe such a scenario we analyse a sample of 12 gas-rich and active star forming sub-mm galaxies (SMGs) at 1.8 < z < 3. We present a structural and size measurement analysis for all of these objects using very deep ACS and NICMOS imaging in the GOODS-North field. Our analysis reveals a heterogeneous mix of morphologies and sizes. We find that four galaxies (33% \pm 17%) show clear signs of mergers or interactions, which we classify as early-stage mergers. The remaining galaxies are divided into two categories: five of them (42% \pm 18%) are diffuse and regular disc-like objects, while three (25% \pm 14%) are very compact, spheroidal systems. We argue that these three categories can be accommodated into an evolutionary sequence, showing the transformation from isolated, gas-rich discs with typical sizes of 2-3 kpc, into compact (< 1 kpc) galaxies through violent major merger events, compatible with the scenario depicted by theoretical models. Our findings that some SMGs are already dense and compact provides strong support to the idea that SMGs are the precursors of the compact, massive galaxies found at slightly lower redshift.