HI-rich, ultra-diffuse galaxies lie way above the baryonic Tully-Fisher relation Kyle Oman (Kapteyn Institute → Durham ICC)
HI-rich, ultra-diffuse galaxies lie way above the baryonic Tully-Fisher relation Kyle Oman (Kapteyn Institute → Durham ICC)
Pavel Mancera Piña HI-rich, Filippo Fraternali, Betsey Adams, Antonino Marasco, Tom Osterloo Lucas Leisman ultra-diffuse Michael Battipaglia, John Cannon, Lexi Gault, Martha Haynes, Steven Janowiecki, Elizabeth McAllan, Hannah Pagel, Kameron Reiter, Katherine Rhode, John Salzer, Nicolas Smith galaxies lie way above the baryonic Tully-Fisher relation Kyle Oman (Kapteyn Institute → Durham ICC)
Sample & Method • Parent sample from Leisman et al. (2017), 30 objects • UDGs : from SDSS, and h µ r ( R e ) i � 24 mag / arcsec 2 8 R e > 1 . 5 kpc ALFALFA outliers • Gas rich : from ALFALFA, M HI ∼ 10 9 M � HUDS with Synthesis 7 • Isolated : any ALFALFA detections within has UDGs (vD+15; RT16) 500 km / s D > 350 kpc DwIrr (HE06) • Observed with Karl G. Jansky Very Large Array (C configuration), or Westerbork 6 h µ r i e > 24 . - HUDS-B Sythesis Radio Telecope µ g, 0 > 24 . - HUDS-R 5 • 6 objects with useable data, kinematic modelling using 3D-BAROLO AGC229385 r e ff (kpc) 4 3 2 1 0 � 12 � 13 � 14 � 15 � 16 � 17 26 25 24 23 22 µ V, 0 (mag asec � 2 ) M V (mags)
Sample & Method • Parent sample from Leisman et al. (2017), 30 objects • UDGs : from SDSS, and h µ r ( R e ) i � 24 mag / arcsec 2 R e > 1 . 5 kpc • Gas rich : from ALFALFA, M HI ∼ 10 9 M � • Isolated : any ALFALFA detections within has 500 km / s D > 350 kpc • Observed with Karl G. Jansky Very Large Array (C configuration), or Westerbork Sythesis Radio Telecope • 6 objects with useable data, kinematic modelling using 3D-BAROLO
<latexit sha1_base64="F09t79rXOIdwyqIQD6tMLyQS8k=">AB8nicbZC7SgNBFIZn4y3GW9TSZjAIqcJuLQM2FhGyQ02IcxOZpMhMzvLzFkhLHkMGwtFbK1T+QhWdpa+gY/g5FJo4g8DH/9/DnPOCWLBDbjup5NZW9/Y3Mpu53Z29/YP8odHDaMSTVmdKqF0KyCGCR6xOnAQrBVrRmQgWDMYXk3z5h3ThquoBqOYdSTpRzklIC1/Ntu2tYSqwTG3XzBLbkz4VXwFlCoFN/fvieTr2o3/9HuKZpIFgEVxBjfc2PopEQDp4KNc+3EsJjQIekz32JEJDOdDbyGJ9Zp4dDpe2LAM/c3x0pkcaMZGArJYGBWc6m5n+Zn0B42Ul5FCfAIjr/KEwEBoWn+Me14yCGFkgVHM7K6YDogkFe6WcPYK3vPIqNMol7xUvEKlRqaK4tO0CkqIg9doAq6RlVURxQpdI8e0ZMDzoPz7LzMSzPOoucY/ZHz+gNMEpaE</latexit> Baryon-dominated within R out (van Dokkum et al. 2019) (Danieli et al. 2019) (Trujillo et al. 2019) (Iorio et al. 2017)
<latexit sha1_base64="Oac4dGsEYlLZ4n5xIbufy0LXT4c=">AB+nicbVC7TsMwFHUKLaW8UhZLCokFqkDBGYmEsEn1ITagc12mt2k5kO6AqdOUrYGEAIRj5EjY+hB3MUDLka50dM69uveMGFUacf5snIrq/nCWnG9tLG5tb1jl3ebKk4lJg0cs1i2Q6QIo4I0NWMtBNJEA8ZaYXD84nfuiFS0Vhc6VFCAo76gkYUI2krl2mvqIcus5xzbn2MZW4a1ecqjMFXCbunFS8wsO3eL/P17v2p9+LcqJ0JghpTquk+gQ1JTzMi45KeKJAgPUZ90DBWIExVk09PH8NAoPRjF0pTQcKr+nsgQV2rEQ9PJkR6oRW8i/ud1Uh2dBRkVSaqJwLNFUcqgjuEkB9ijkmDNRoYgLKm5FeIBkghrk1bJhOAuvrxMmrWqe1KtXboVzwMzFME+OABHwAWnwAMXoA4aAINb8AiewYt1Zz1Zr9brDVnzWf2wB9YHz8e7pZJ</latexit> <latexit sha1_base64="dptTNAOHYn9LlFwYaf31VZubr+k=">AB/3icbVDLSsNAFJ3UV62vaMGNm8EiuJCS1IUuA27qolDBPqAJYTKdtENnkjAzEUrsQj/FjQtF3PobLgT/wG9w5fSx0NYDFw7n3Mu9wQJo1JZ1qeRW1peWV3Lrxc2Nre2d8zdvaMU4FJA8csFu0AScJoRBqKkbaiSCIB4y0gsHF2G/dECFpHF2rYUI8jnoRDSlGSku+uV/zXamQgC5jsOZnruCwejnyzZJVtiaAi8SekZJT/Pi+/xqd1H3z3e3GOUkUpghKTu2lSgvQ0JRzMio4KaSJAgPUI90NI0QJ9LJveP4JFWujCMha5IwYn6eyJDXMohD3QnR6ov572x+J/XSV47mU0SlJFIjxdFKYMqhiOw4BdKghWbKgJwoLqWyHuI4Gw0pEVdAj2/MuLpFkp26flypVdchwR4cgENwDGxwBhxQBXQABjcgfwBJ6NO+PReDFep605YzZTBH9gvP0AdzGZg=</latexit> Systematic errors, biases • Distance At 70-90 Mpc Hubble flow is robust. • HI mass ALFALFA & VLA/WSRT fluxes agree. • Stellar mass M ? ⌧ M HI • Outer radius 7-18 kpc should reach flat part of rotation curve. • Beam smearing 3D-BAROLO convolves beam with model to compare with data. • Inclination All 6 galaxies would need . i ∼ 10 − 20 �
Systematic errors, biases Radius [kpc] Oman et al. (2015)
<latexit sha1_base64="Oac4dGsEYlLZ4n5xIbufy0LXT4c=">AB+nicbVC7TsMwFHUKLaW8UhZLCokFqkDBGYmEsEn1ITagc12mt2k5kO6AqdOUrYGEAIRj5EjY+hB3MUDLka50dM69uveMGFUacf5snIrq/nCWnG9tLG5tb1jl3ebKk4lJg0cs1i2Q6QIo4I0NWMtBNJEA8ZaYXD84nfuiFS0Vhc6VFCAo76gkYUI2krl2mvqIcus5xzbn2MZW4a1ecqjMFXCbunFS8wsO3eL/P17v2p9+LcqJ0JghpTquk+gQ1JTzMi45KeKJAgPUZ90DBWIExVk09PH8NAoPRjF0pTQcKr+nsgQV2rEQ9PJkR6oRW8i/ud1Uh2dBRkVSaqJwLNFUcqgjuEkB9ijkmDNRoYgLKm5FeIBkghrk1bJhOAuvrxMmrWqe1KtXboVzwMzFME+OABHwAWnwAMXoA4aAINb8AiewYt1Zz1Zr9brDVnzWf2wB9YHz8e7pZJ</latexit> <latexit sha1_base64="dptTNAOHYn9LlFwYaf31VZubr+k=">AB/3icbVDLSsNAFJ3UV62vaMGNm8EiuJCS1IUuA27qolDBPqAJYTKdtENnkjAzEUrsQj/FjQtF3PobLgT/wG9w5fSx0NYDFw7n3Mu9wQJo1JZ1qeRW1peWV3Lrxc2Nre2d8zdvaMU4FJA8csFu0AScJoRBqKkbaiSCIB4y0gsHF2G/dECFpHF2rYUI8jnoRDSlGSku+uV/zXamQgC5jsOZnruCwejnyzZJVtiaAi8SekZJT/Pi+/xqd1H3z3e3GOUkUpghKTu2lSgvQ0JRzMio4KaSJAgPUI90NI0QJ9LJveP4JFWujCMha5IwYn6eyJDXMohD3QnR6ov572x+J/XSV47mU0SlJFIjxdFKYMqhiOw4BdKghWbKgJwoLqWyHuI4Gw0pEVdAj2/MuLpFkp26flypVdchwR4cgENwDGxwBhxQBXQABjcgfwBJ6NO+PReDFep605YzZTBH9gvP0AdzGZg=</latexit> Systematic errors, biases • Distance At 70-90 Mpc Hubble flow is robust. • HI mass ALFALFA & VLA/WSRT fluxes agree. • Stellar mass M ? ⌧ M HI • Outer radius 7-18 kpc should reach flat part of rotation curve. • Beam smearing 3D-BAROLO convolves beam with model to compare with data. • Inclination All 6 galaxies would need . i ∼ 10 − 20 �
Inclination tests • Sample of 4 simulated galaxies from the APOSTLE suite. • Similar HI masses to HI-rich UDG sample, but lie on BTFR. • “Observed” at several inclinations using MARTINI code. • Matched beam, S/N, distance, channel width, etc. • Construct models at different inclinations and compare to “observations”.
Inclination tests • Sample of 4 simulated galaxies from the APOSTLE suite. • Similar HI masses to HI-rich UDG sample, but lie on BTFR. • “Observed” at several inclinations using MARTINI code. • Matched beam, S/N, distance, channel width, etc. • Construct models at different inclinations and compare to “observations”.
Inclination tests • Sample of 4 simulated galaxies from the APOSTLE suite. • Similar HI masses to HI-rich UDG sample, but lie on BTFR. • “Observed” at several inclinations using MARTINI code. • Matched beam, S/N, distance, channel width, etc. • Construct models at different inclinations and compare to “observations”.
<latexit sha1_base64="Nir1yrqWA2e0CzioK73a2OPG7sY=">AB8nicbZDLSgMxFIYz9VZHq1WXboKl4KrM1IVdFgRxWcFeYFpKJs20oclkSM6IZehjuHGhiODKp/AR3Pk2peFtv4Q+Pj/c8g5J0wEN+B5305uY3Nreye/6+7tFw4Oi0fHLaNSTVmTKqF0JySGCR6zJnAQrJNoRmQoWDscX83y9j3Thqv4DiYJ60kyjHnEKQFrBa1+1tUS/Iw7RdLXsWbC6+Dv4RSvfCZlq/d90a/+NUdKJpKFgMVxJjA9xLoZUQDp4JN3W5qWELomAxZYDEmkpleNh95isvWGeBIaftiwHP3d0dGpDETGdpKSWBkVrOZ+V8WpBDVehmPkxRYTBcfRanAoPBsfzgmlEQEwuEam5nxXRENKFgr+TaI/irK69Dq1rxLyrVW79Ur6GF8ugUnaFz5KNLVEc3qIGaiCKFHtEzenHAeXJenbdFac5Z9pygP3I+fgDBLZPM</latexit> Kinematic modelling tests • Same mock-observed sample from APOSTLE. • Fully blind analysis. • Reliably recover within estimated V max error.
<latexit sha1_base64="787oJVuIl5M4KzP7jRWfMIt76SY=">AB/3icbVDLSsNAFJ34rPUVLbhxM1gEF1KSKugy4MaNUME+oIlhMp20QyfJMDMRSsxCP8WNC0Xc+hsuBP/Ab3Dl9LHQ1gMXDufcy73BJxRqSzr05ibX1hcWi6sFfX1jc2za3thkxSgUkdJywRrQBJwmhM6oqRlpcEBQFjDSD/tnQb94QIWkSX6kBJ16EujENKUZKS765c+FnrohgETucpFwlcDG9bFvlq2KNQKcJfaElJ3Sx/f9V35Y813t5PgNCKxwgxJ2bYtrwMCUxI3nRTSXhCPdRl7Q1jVFEpJeN7s/hvlY6MEyErljBkfp7IkORlIMo0J0RUj057Q3F/7x2qsJTL6MxTxWJ8XhRmDKonxyGATtUEKzYQBOEBdW3QtxDAmGlIyvqEOzpl2dJo1qxjyrVS7vsOGCMAtgFe+A2OAEOAc1EAdYHALHsATeDbujEfjxXgdt84Zk5kS+APj7QcwCZn4</latexit> <latexit sha1_base64="ogKYo3Wtv8GcO0GzmpDdOvziA0U=">AB8nicbZC7SgNBFIZn4y3GWzSlzWAQLCTsxkLBRvLCOYCmyXMTmaTIXNZmbFsGzjO9hYKGLr01gIvoHPYOXkUmjiDwMf/38Oc86JEka1cd1Pp7Cyura+UdwsbW3v7O6V9w9aWqYKkyaWTKpOhDRhVJCmoYaRTqI4hEj7Wh0Ocnbt0RpKsWNGSck5GgaEwxMtYKWr2sqzjk6C7vlatuzZ0KLoM3h6pf+fi+/8pPG73ye7cvcqJMJghrQPTUyYIWUoZiQvdVNEoRHaEACiwJxosNsOnIOj63Th7FU9gkDp+7vjgxrc8spUcmaFezCbmf1mQmvgizKhIUkMEn0UpwaCSf7wz5VBs2toCwonZWiIdIWzslUr2CN7iysvQqte8s1r92qv6PpipCA7BETgBHjgHPrgCDdAEGEjwAJ7As2OcR+fFeZ2VFpx5TwX8kfP2A+dAlWs=</latexit> <latexit sha1_base64="u0oMy+ovizQeEow6Kx7ho23nF8Q=">AB7HicbZA7SwNBFIXvxleMr/jobAaDYBV2Y6GdARvLCG4SJYwO5lNhszMLjOzQljyGy0UMTWH2RnYW9nZ+3kUWjigYGPc+5l7r1hwpk2rvu5JaWV1bX8uFjc2t7Z3i7l5dx6ki1Ccxj1UzxJpyJqlvmOG0mSiKRchpIxcjvPGLVWaxfLGDBMaCNyTLGIEG2v5bc6R1ymW3LI7EVoEbwali+/7z4Pa10etU3xrd2OSCioN4VjrlucmJsiwMoxwOiq0U0TAa4R1sWJRZUB9lk2BE6tk4XRbGyTxo0cX93ZFhoPRShrRTY9PV8Njb/y1qpic6DjMkNVS6UdRypGJ0Xhz1GWKEsOHFjBRzM6KSB8rTIy9T8EewZtfeRHqlbJ3Wq5ce6VqFabKwyEcwQl4cAZVuIa+ECAwR08wpMjnQfn2XmZluacWc8+/JHz+gOjp5MQ</latexit> <latexit sha1_base64="NDMIycUBp1xJpuEmp4jEI9DPwF8=">AB9XicbVDLSgMxFL1Tba31VXpJlgEN5aZquiy4MZlBfuAdiyZNG1Dk8yQZJQydOs3uNCFIq4E/8WdH+Le9LHQ1gOXezjnXnJzgogzbVz3y0ktLaczK9nV3Nr6xuZWfnunpsNYEVolIQ9VI8CaciZp1TDaSNSFIuA03owuBj79VuqNAvltRlG1Be4J1mXEWysdNPSTKCTo1PbewK38wW36E6AFok3I4Vy5vFbvt+nK+38Z6sTklhQaQjHWjc9NzJ+gpVhNRrhVrGmEywD3atFRiQbWfTK4eoQOrdFA3VLakQRP190aChdZDEdhJgU1fz3tj8T+vGZvuZ8wGcWGSjJ9qBtzZEI0jgB1mKLE8KElmChmb0WkjxUmxgaVsyF4819eJLVS0Tsulq68QrkMU2RhD/bhEDw4gzJcQgWqQEDBAzDi3PnPDmvzt0NOXMdnbhD5yPHx5zlUk=</latexit> Finally some cosmology • High spin ↔ low concentration DM halos? ‣ drops and occurs further out. V max ‣ Need to be in tail of distribution. ∼ 4 − 5 σ ‣ Given parent survey volume expect such object. ⌧ 1 • MOND? ‣ Fail strong prediction for BTFR: . M bar ∝ V 4
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