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Origin of Star-Forming Rings around Massive Centres in Massive Galaxies at $z!<!4$ | | Avishai Dekel
; Sharon Lapiner
; Omri Ginzburg
; Jonathan Freundlich
; Fangzhou Jiang
; Doug Lin
; Daniel Ceverino
; Joel Primack
; Mauro Giavalisco
; Zhiyuan Ji
; | | Date: |
19 Mar 2020 | | Abstract: | Using analytic modeling and simulations, we address the origin of an
abundance of star-forming, clumpy, extended gas rings about massive central
bodies in massive galaxies at $z! <! 4$. Rings form by high-angular-momentum
streams and may survive in galaxies of $M_{
m star} !>! 10^{9.5}, M_odot$
where merger-driven spin flips and supernova feedback are ineffective. The
rings survive above this threshold mass after events of compaction to central
nuggets. Ring longevity seemed to conflict with the expected inward mass
transport driven by torques from violent disc instability. However, by
evaluating the torques from a tightly wound spiral structure, we find that the
timescale for transport per orbital time is $propto! delta_{
m d}^{-3}$,
with $delta_{
m d}$ the cold-to-total mass ratio interior to the ring. A
long-lived ring forms when the ring transport is slower than its replenishment
by accretion and the interior depletion by SFR, both valid for $delta_{
m d}
!<! 0.3$. The central mass that lowers $delta_{
m d}$ and maintains the
ring is made of compaction-driven bulge and/or dark-matter, aided by the lower
gas fraction at lower $z$. The ring could be Toomre unstable for clump and star
formation. Mock images of simulated rings through dust indicate qualitative
consistency with observed rings about bulges in massive $z!sim!0.5!-!3$
galaxies, in $H_{alpha}$ and in deep HST imaging. ALMA mock images indicate
that $z!sim!0.5!-!1$ rings should be detectable. We quote expected
observable properties and abundances of rings and their central blue or red
nuggets for comparison to observations. | | Source: | arXiv, 2003.8984 | | Services: | Forum | Review | PDF | Favorites | |
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