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  • NAM2019
    • Registration
    • Key Dates & Outline Schedule
    • Practical Information
    • Exhibitors
    • Grants & Bursaries
    • Contacts
  • Science
    • Science Programme
    • Parallel Sessions
    • Plenary Talks
    • Community Session
    • Special Lunches
    • Posters
    • Presenter Guidelines
  • Social
    • What's On
    • Welcome Reception
    • RAS Awards Dinner
  • Media
  • Outreach
    • Outreach and Education Day
    • Fringe Event
    • School Visit Day
  • Lancaster
    • Travel
    • Accommodation
    • Childcare
    • Campus Map
    • About Lancaster
    • Code of Conduct

Wednesday

Schedule

id
date time
PM2
16:30
Abstract
The Galaxy Stellar Mass Function & Low Surface Brightness Galaxies from Core-Collapse Supernovae
Wednesday

Abstract details

id
The Galaxy Stellar Mass Function & Low Surface Brightness Galaxies from Core-Collapse Supernovae
Date Submitted
2019-03-11 17:15:54
Tom
Sedgwick
Astrophysics Research Institute (LJMU)
Studying galaxy evolution from reionization to cosmic noon with the latest-generation multiwavelength facilities
Talk
T. M. Sedgwick (ARI), I. K. Baldry (ARI), P. A. James (ARI) & L. S. Kelvin (ARI)
I will introduce a galaxy sample selection method using core-collapse supernovae (CCSNe). Using a complete sample of ~900 z0.2 CCSNe, identified from the SDSS-II Supernova Survey, as pointers towards their host galaxies, we find 140 ‘new’ low surface brightness galaxies whilst identifying the hosts. Selecting star-forming galaxies using CCSNe leads to the removal of surface brightness and mass biases. I will demonstrate how CCSN-rates as a function of galaxy stellar mass can be used to trace both star-formation rates and the form of the galaxy stellar mass function. Resultant number densities are well-constrained deep into the dwarf regime and are found to increase following a power-law with decreasing mass down to the low mass limit of ~10^6.4 M⊙, well represented by a single Schechter function with a faint-end slope of α = -1.41. This lack of downturn to galaxy number densities down to the low mass limit implies that overcoming surface brightness and stellar mass biases is important for an assessment of the sub-structure problem.

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