Episodic starbursts in dwarf spheroidal galaxies: a simple model

TL;DR

This paper proposes a simple model explaining episodic star formation in dwarf spheroidal galaxies based on gas cooling variations caused by orbital eccentricity and external ionizing fields, matching some observed burst timings.

Contribution

The model links gas cooling time variations to orbital eccentricity and external UV fields, providing a new explanation for episodic star formation in dwarf spheroidals.

Findings

Predicts episodic star formation mainly in moderately eccentric orbits.

Up to 40% of early infall dwarfs have experienced at least one burst.

Explains burst timing in Carina and constrains Fornax's orbit.

Abstract

Dwarf galaxies in the Local Group appear to be stripped of their gas within 270 kpc of the host galaxy. Color-magnitude diagrams of these dwarfs, however, show clear evidence of episodic star formation (\Delta{}t ~ a few Gyr) over cosmic time. We present a simple model to account for this behaviour. Residual gas within the weak gravity field of the dwarf experiences dramatic variations in the gas cooling time around the eccentric orbit. This variation is due to two main effects. The azimuthal compression along the orbit leads to an increase in the gas cooling rate of ~([1+\epsilon]/[1-\epsilon])^2. The Galaxy's ionizing field declines as 1/R^2 for R>R_disk although this reaches a floor at R~150 kpc due to the extragalactic UV field ionizing intensity. We predict that episodic SF is mostly characteristic of dwarfs on moderately eccentric orbits (\epsilon>0.2) that do not come too close to the centre (R>R_disk) and do not spend their entire orbit far away from the centre (R>200 kpc). Up to 40% of early infall dwarf spheroidals can be expected to have already had at least one burst since the initial epoch of star formation, and 10% of these dwarf spheriodals experiencing a second burst. Such a model can explain the timing of bursts in the Carina dwarf spheroidal and restrict the orbit of the Fornax dwarf spheroidal. However, this model fails to explain why some dwarfs, such as Ursa Minor, experience no burst post-infall.