Gas kinematics and morphology of low-mass galaxies Kareem El-Badry (UC Berkeley) Eliot Quataert, Andrew Wetzel, Dan Weisz, Phil Hopkins, Shea Garrison-Kimmel, TK Chan, Mike Boylan-Kolchin, Alex Fitts, ++
Feedback drives gas outflows, leads to bursty SF El-Badry+16 M star ~ 3e8 M ⊙ Kareem El-Badry (UC Berkeley)
Feedback drives gas outflows, leads to bursty SF El-Badry+16 M star ~ 3e8 M ⊙ Kareem El-Badry (UC Berkeley)
<latexit sha1_base64="oiwtz2SVO/+cWtuTLe6RPjZasho=">ACnicbVA9SwNBEN2LXzF+RS1tVoNgY7iLYmyEoI2NEMF8QHKGvc0mWbJ3e+zOCeG42sa/YmOhiK2/wM5/4ya5QhMfDzem2FmnhcKrsG2v63MwuLS8kp2Nbe2vrG5ld/eqWsZKcpqVAqpmh7RTPCA1YCDYM1QMeJ7gjW84dXYbzwpbkM7mAUMtcn/YD3OCVgpE5+/6YTt5WPNRCV4Avs2Pfx2XE5wWNdiUknXzBLtoT4HnipKSAUlQ7+a92V9LIZwFQbRuOXYIbkwUcCpYkmtHmoWEDkmftQwNiM+0G09eSfChUbq4J5WpAPBE/T0RE1/rke+ZTp/AQM96Y/E/rxVB79yNeRBGwAI6XdSLBAaJx7ngLleMghgZQqji5lZMB0QRCia9nAnBmX15ntRLRekWLo9LVQu0ziyaA8doCPkoDKqoGtURTVE0SN6Rq/ozXqyXqx362PamrHSmV30B9bnDzkqmVY=</latexit> <latexit sha1_base64="LcGKEzXPibTHaNvBQ1dNKOFLZ5g=">ACnicbVA9SwNBEN2LXzF+RS1tVoNgY7iLQtIQRsbIYL5gOQMe5tNsmTv9tidE8JxtY1/xcZCEVt/gZ3/xk1yhSY+GHi8N8PMPC8UXINtf1uZpeWV1bXsem5jc2t7J7+719AyUpTVqRStTyimeABqwMHwVqhYsT3BGt6o6uJ3xgSnMZ3ME4ZK5PBgHvc0rASN384U037igfayAqwRfYse/j8mklwRNd9iQk3XzBLtpT4EXipKSAUtS6+a9OT9LIZwFQbRuO3YIbkwUcCpYkutEmoWEjsiAtQ0NiM+0G09fSfCxUXq4L5WpAPBU/T0RE1/rse+ZTp/AUM97E/E/rx1Bv+LGPAgjYAGdLepHAoPEk1xwjytGQYwNIVRxcyumQ6IBZNezoTgzL+8SBqlonNWLN2eF6qXaRxZdICO0AlyUBlV0TWqoTqi6BE9o1f0Zj1ZL9a79TFrzVjpzD76A+vzBzxKmVg=</latexit> <latexit sha1_base64="h8Nu6ygFApmxYkRc9+Tc7oqfC6w=">ACnicbVA9SwNBEN2LXzF+RS1tVoNgY7iLgrEQgjY2QgTzAckZ9jabZMne7bE7J4Tjahv/io2FIrb+Ajv/jZvkCk18MPB4b4aZeV4ouAb/rYyC4tLyvZ1dza+sbmVn57p65lpCirUSmkanpEM8EDVgMOgjVDxYjvCdbwhldjv/HAlOYyuINRyFyf9APe45SAkTr5/ZtO3FY+1kBUgi+wY9/H5ePzBI912ZWQdPIFu2hPgOeJk5ICSlHt5L/aXUkjnwVABdG65dghuDFRwKlgSa4daRYSOiR91jI0ID7Tbjx5JcGHRuninlSmAsAT9fdETHytR75nOn0CAz3rjcX/vFYEvbIb8yCMgAV0uqgXCQwSj3PBXa4YBTEyhFDFza2YDogiFEx6OROCM/vyPKmXis5JsXR7WqhcpnFk0R46QEfIQWeogq5RFdUQRY/oGb2iN+vJerHerY9pa8ZKZ3bRH1ifPz9qmVo=</latexit> <latexit sha1_base64="UITFMH2ed/Vb/DGCzhSanh3Jsk=">AC3icbVA9SwNBEN3zM8avU0ubJUGwMdxFQS2EoI2NEMF8QHKGvc0mWbJ3e+zOCeG43sa/YmOhiK1/wM5/416SQhMfDzem2Fmnh8JrsFxvq2FxaXldXcWn59Y3Nr297ZrWsZK8pqVAqpmj7RTPCQ1YCDYM1IMRL4gjX84VXmNx6Y0lyGdzCKmBeQfsh7nBIwUscu3HStgqwBqJSfIFd5z45P3LdFGeG7EpIO3bRKTlj4HniTkRTVHt2F/trqRxwEKgmjdcp0IvIQo4FSwN+ONYsIHZI+axkakoBpLxn/kuIDo3RxTypTIeCx+nsiIYHWo8A3nQGBgZ71MvE/rxVD78xLeBjFwEI6WdSLBQaJs2BwlytGQYwMIVRxcyumA6IBRNf3oTgzr48T+rlkntcKt+eFCuX0zhyaB8V0CFy0SmqoGtURTVE0SN6Rq/ozXqyXqx362PSumBNZ/bQH1ifP60smY4=</latexit> HI mock observations M star = 10 6 � 7 M � M star = 10 7 � 8 M � M star = 10 8 � 9 M � M star = 10 9 � 11 M � all galaxies viewed “edge-on” Kareem El-Badry (UC Berkeley)
Kareem El-Badry (UC Berkeley)
Kareem El-Badry (UC Berkeley)
LITTLE THINGs; Oh+2015 Kareem El-Badry (UC Berkeley)
LITTLE THINGs; Oh+2015 Selection function? Quantitative comparison is hard. Kareem El-Badry (UC Berkeley)
Unresolved HI Kareem El-Badry (UC Berkeley)
Unresolved HI Kareem El-Badry (UC Berkeley)
Unresolved HI ~50 kpc Kareem El-Badry (UC Berkeley)
Unresolved HI ~50 kpc flux density available for ~50,000 galaxies; morphologically blind velocity Kareem El-Badry (UC Berkeley)
Unresolved observations contain kinematic information Kareem El-Badry (UC Berkeley)
El-Badry+18 Kareem El-Badry (UC Berkeley)
El-Badry+18 Kareem El-Badry (UC Berkeley)
El-Badry+18 Kareem El-Badry (UC Berkeley)
El-Badry+18 k=-0.5 k=-0.9 k=-1.4 Kareem El-Badry (UC Berkeley)
HI line kurtosis is sensitive to V/ σ El-Badry+18 Kareem El-Badry (UC Berkeley)
comparison to observations El-Badry+18 Kareem El-Badry (UC Berkeley)
agreement at MW-masses El-Badry+18 Kareem El-Badry (UC Berkeley)
overly dispersion-supported at low/intermediate masses El-Badry+18 Kareem El-Badry (UC Berkeley)
overly dispersion-supported at low/intermediate masses El-Badry+18 Kareem El-Badry (UC Berkeley)
overly dispersion-supported at low/intermediate masses Line shape problem El-Badry+18 Kareem El-Badry (UC Berkeley)
Non-cosmological simulations • Idealized setup: NFW halo + gas in hydrostatic equilibrium • “normal” angular momentum; λ = 0.03 • run for 10 Gyr with same physics as cosmological sims. Kareem El-Badry (UC Berkeley)
Non-cosmological simulations • Disks form and survive! M star ~ 1e8 M ⊙ green: T ~ 1e4 K purple: T < 1e3 K red: T > 1e5 K Kareem El-Badry (UC Berkeley)
Non-cosmological sims: better agreement with observations FIRE NC Kareem El-Badry (UC Berkeley)
MW-mass galaxies accrete until z=0 M star ~10 7 M ⊙ M star ~10 10.5 M ⊙ gas accretion rate gas accretion rate Kareem El-Badry (UC Berkeley)
Dwarfs accrete mostly at early times M star ~10 7 M ⊙ M star ~10 10.5 M ⊙ gas accretion rate Kareem El-Badry (UC Berkeley)
Gas accreted late has higher angular momentum M star ~10 7 M ⊙ M star ~10 10.5 M ⊙ gas accretion rate log(j gas, accreted ) see also Brook+11; Übler+14 Kareem El-Badry (UC Berkeley)
irregular disky Both galaxies have: Kareem El-Badry (UC Berkeley)
irregular disky Both galaxies have: Kareem El-Badry (UC Berkeley)
Summary • FIRE cosmological simulations produce a diversity of dwarf galaxy morphologies and kinematics. • On average, simulated galaxies are more dispersion supported and less disky than observed. • Idealized non-cosmological simulations with the same ingredients make diskier dwarfs on average. • In cosmological simulations, feedback & UV background prevent dwarfs from accreting high-angular momentum gas at late times. Kareem El-Badry (UC Berkeley)
Kareem El-Badry Kurtosis is insensitivity to SNR KE, Bradford, Geha+18
Kareem El-Badry Kurtosis is insensitivity to SNR …but sensitive to inclination. KE, Bradford, Geha+18
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