Antlia 2 The hidden giant Vasily Belokurov Institute of Astronomy, - PowerPoint PPT Presentation

Jan 10, 2023 •231 likes •561 views

Antlia 2 The hidden giant Vasily Belokurov Institute of Astronomy, Cambridge based on Torrealba et al. 2019 What controls the size of a (dwarf) galaxy? based on: size-luminosity + abundance matching (both highly non-linear) Kravtsov 2013

Antlia 2 The hidden giant Vasily Belokurov Institute of Astronomy, Cambridge based on Torrealba et al. 2019
What controls the size of a (dwarf) galaxy? based on: size-luminosity + abundance matching (both highly non-linear) Kravtsov 2013
Stellar feedback? Navarro et al 1996 Mashchenko et al 2008 Pontzen & Governato 2012 Zolotov et al 2012 Madau et al 2014 Di Cintio et al 2014 Brooks & Zolotov 2014 Read, Agertz & Collins 2016 … Bullock & Boylan-Kolchin 2017
Gaia, the halo explorer • relatively bright magnitude limit, but • no weather • perfect star/galaxy separation • artifact rejection • whole sky • uniform(ish) quality • astrometry
Prediction • “Our experiments suggest that Gaia will be able to detect UFDGs that are similar to some of the known UFDGs even if the limit of Gaia is around 2 mag brighter than that of SDSS, with the advantage of having a full-sky catalogue. We also see that Gaia could even find some UFDGs that have lower surface brightness than the SDSS limit”
Gaia DR2
Galactic latitude Galactic longitude
Galactic latitude Galactic longitude
Galactic latitude Galactic longitude
Gaia’s magic
New satellite revealed by RR Lyrae - RR Lyrae with distances D > 70 kpc
Archival deeper DECam imaging
Distance to Antlia 2 Archival deeper DECam imaging Blue Horizontal Branch - distant RR Lyrae “standard candle” D=130 kpc
Size and luminosity super mega ultra diffuse!
Spectroscopic Follow-up confirmed members Antlia 2 dwarf Galactic foreground line-of-sight velocity
3D motion + metallicity
Kinematics PM expected if Ant 2 moves in the direction of elongation
Kinematics
Metallicity distribution
Mass-luminosity
Luminosity-density
Fluffy dwarfs NFW cored NFW truncated NFW Efficient Feedback Kravtsov relation
Can tidal stripping play a role? Cuspy and cored haloes   react to tides differently Errani & Peñarrubia 2019
(predicted) Tidal debris
Stellar mass - metallicity not too much tidal stripping? a-la Kirby et al 2013
Antlia 2 and the LMC
LMC changes Ant 2 orbit Peri-centre shifts from 37 kpc to 27 kpc if massive LMC is included (Erkal & Belokurov 2019) future orbit, past orbit, LMC orbit
Formation pathways? • Strong feedback - clues in SFH/MDF? • Dwarf merging - clues in SFH/MDF? • Born cored - clues anywhere?
Conclusions • Gaia can detect super mega ultra diffuse galaxies • There may be a (much) larger scatter in luminosity at fixed size than previously assumed • Ant 2 is difficult to stuff into a cuspy halo • Even a cored halo requires plenty of tidal stripping • Giant clouds of tidal debris predicted • Unclear if the cored halo is consistent with feedback- induced conditions
Low surface brightness Universe • Are And XIX , Cra 2 and Ant 2 the tip of the iceberg? • If yes, our predictions for LSST detection efficiency (with resolved stelar pops) at large distances are   too pessimistic • Last week Gaia finished its 5 year-long mission… and started its second life, also 5 years long
The END

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