Selected publications

(Click here for a full list)

image

SFR-HI relations

Despite being the raw material for forming stars, the general link between HI and SFR is weak, because too many processes and factors lie between them. (Wang et al.2017MNRAS)

image

HI size-mass relation

Massive and dwarf galaxies have very different gas conversion efficiency and history but surprisingly share the same HI size-mass relation (catalog available). (Wang et al.2016MNRAS)

image

HI environment

HI-rich galaxies have more HI in the 500 kpc envrionment which is outside individually detected sources but cumulates to significant mass.. (Wang et al.2015MNRAS)

image

HI in satellites

HI-rich galaxies have HI-rich satellites within a distance of 1 Mpc around them.. (E.Wang et al.2015MNRAS)

image

HI radial distribution

Different kind of galaxies have surprisingly similar outer HI disk after a very simple scaling (catalog and data available)... (Wang et al.2014MNRAS)

image

HI morphology

The extremely HI-rich galaxies have only normal HI morpholgies (catalog and data available).. (Wang et al.2013MNRAS)

image

Bars and central SF

Galaxies hosting bars tend to have significant enhanced central star formation but also tend to have suppressed central star formation.. (Wang et al.2012MNRAS)

image

Outer disk and HI gas

Stellar population in galactic outer disks are only determined by HI gas content.. (Wang et al.2011MNRAS)

image

BGCs

Brightest cluster galaxies are on average old and dead, despite the cooling flow of gas in some really massive clusters.. (Wang et al.2010MNRAS)

View All