Upgrade to Pro — share decks privately, control downloads, hide ads and more …

Decoupling star-gas rotation - I: the fundament...

Decoupling star-gas rotation - I: the fundamental links to morphology and halo spin

Avatar for Chris Duckworth

Chris Duckworth

October 07, 2019
Tweet

More Decks by Chris Duckworth

Other Decks in Science

Transcript

  1. Decoupling star-gas rotation - I: the fundamental links to morphology

    and halo spin Chris Duckworth, Rita Tojeiro [email protected] 7th October 2019 SDSS-IV Project 0535: https://trac.sdss.org/wiki/MANGA/Projects/kinematic_misalignment_morphology SDSS-IV Paper 0391: https://internal.sdss.org/collaboration/publications/browse/select/id%3D391
  2. This project in a nutshell… • First in a series

    which uses a combination of MaNGA and IllustrisTNG (TNG) to comprehensively understand why galaxies have decoupled rotation between stars and gas (kinematic misalignment) • Here we focus on: • Morphological dependence of kinematic misalignment (MaNGA & TNG) • Relationship with angular momentum and gas content at z = 0 (MaNGA & TNG) • Identifying galaxies with stellar rotation but ‘messed up’ gas rotation as potential progenitors of misaligned galaxies (MaNGA) • Relationship with the halo spin back to z = 1 (TNG)
  3. Stars Ionized gas 1) Looking at 3 different types of

    galaxies. 1) Galaxies with aligned rotation between stars and gas (usual expectation from basic TTT) i.e. ΔPA = |PAstars – PAgas | < 30° # = 3378 galaxies
  4. Stars Ionized gas 2) Looking at 3 different types of

    galaxies. 2) Kinematically misaligned galaxies with a difference between rotational axes of stars and gas i.e. ΔPA = |PAstars – PAgas | > 30° # = 420 galaxies
  5. Stars Ionized gas 3) Looking at 3 different types of

    galaxies. 3) Coherent stellar rotation but dispersion dominated or depleted gas Will refer to them as NGRs (no gas rotation) # = 742 galaxies
  6. I have classified the velocity fields for every MaNGA MPL-8

    galaxy. The plan is to share the catalogue with the collaboration early next year. Email me if you are interested in using this catalogue before then.
  7. ΔPA > 30°: 28±3% of 301 ETGs 10±1% of 677

    S0-Sas 5.4±0.6% of 1634 Sb-Sds ETG centrals are more likely to be misaligned than ETG satellites! Morphologies from GalaxyZoo; https://www.sdss.org/dr15/data_access/value-added-catalogs/?vac_id=manga-morphologies-from-galaxy-zoo
  8. General properties of decoupled galaxies (MaNGA) Little difference in stellar

    mass when considering population as a whole but individual trends when broken down by morphology Morphologies from GalaxyZoo; https://www.sdss.org/dr15/data_access/value-added-catalogs/?vac_id=manga-morphologies-from-galaxy-zoo
  9. General properties of decoupled galaxies (MaNGA) This holds regardless of

    morphology and cut in ΔPA (i.e. those with ΔPA > 150° have the same angular momentum as those with >30°)
  10. General properties of decoupled galaxies (MaNGA) Gas mass based on

    dust attention from Pipe3D; https://www.sdss.org/dr15/manga/manga-data/manga-pipe3d-value-added-catalog/ Since angular momentum loss and gas loss seem crucial in misalignment are NGRs progenitors of misaligned (i.e before gas is re-accreted)?
  11. 1) For every MPL-8 object, found unique subhalo with most

    similar combination of stellar mass, size and g-r colour 2) Made MaNGA like observation (particle based with co-added noise and PSF of typical MaNGA observations for each subhalo up- to same number of Re as matched MaNGA galaxy 3 Same eyeballing of velocity fields and kinematic classifications IllustrisTNG-100 mock MaNGA sample Example output from a TNG subhalo
  12. Specific angular momentum of all DM particles in subhalo Galaxies

    with decoupled star-gas rotation at z=0 are in haloes of lower spin going back past z=1!
  13. Paper submitted to collaboration, to be submitted to MNRAS ~

    22nd October Paper in late stage however feedback/comments greatly appreciated and co-authorship (as appropriate) welcomed.
  14. Ongoing work in this series • Relationship with black hole

    feedback in TNG • (Preliminary) Correlates with black hole mass • (Preliminary) Correlates with black hole luminosity (with time lag!) • Currently looking at relationship with energy injection and misalignment • Relationship with mergers for ETGs in TNG / MaNGA • Currently looking at relaxation timescales • Currently looking at merger relationship on individual galaxy basis These projects are not SDSS-IV (currently) but if you are interested feel free to get in touch!