Introtalk_EDT.pdf

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1. Enrico Di Teodoro Johns Hopkins University Space Telescope Science Institute Intro talk: Galaxy dynamics and outflows STScI – March 30th
2. Who Am I? Who Am I? TERAMO TORINO BOLOGNA University of Bologna: BSc, MSc and PhD in Astrophysics
3. Who Am I? Who Am I? Australian National University Canberra, Australia Johns Hopkins University Space Telescope Science Institute Baltimore, US
4. My Research My Research Gas accretion Scaling relations Galaxy dynamics Strong gravitational lensing Galactic outflows Protoplanetary disks High Velocity Clouds Star formation Bars and circumnuclear rings Code development Galaxy mass assembly Gas
5. PART I. Kinematics of local and high- Kinematics of local and high-z z disk galaxies disk galaxies through 3D modeling of emission-line datacubes through 3D modeling of emission-line datacubes Collaborators: - Filippo Fraternali (University of Bologna) - Giuliano Iorio (University of Bologna) - Antonino Marasco (Kapteyn Institute) - Sarah Miller (UCI)
6. Tracing the mass distribution: DM Stars Gas c Mass Decomposition And Scaling Relations Mass Decomposition And Scaling Relations Tully-Fisher relations: McGaugh 2005 Stellar mass Stellar mass + gas L or M * or M b = β V α with α ~ 4
7. 0th 1st 2nd Moment maps Moment maps Velocity dispersion Column density Velocity Global profile Flux (Jy/beam) Velocity (km/s) VEL RA DEC HI Emission-line Datacubes In A Nutshell Emission-line Datacubes In A Nutshell
8. SAME SAME galaxy at different resolutions! galaxy at different resolutions! VLA interferometer PSF Effelsberg single dish PSF Radius [kpc] 0 20 40 Radius [kpc] 0 20 40 Velocity elds Dispersion elds Gentile et al., 13 Winkel et al., 12 VLOS σOBS High res. Low res. 2D Beam Smearing: NGC3198 Example Beam Smearing: NGC3198 Example
9. - 2D velocity fields (e.g., Rogstad et al. 1974, Begeman 1987, Schoenmakers 2001, Spekkens 2007) - 6 free parameters - 6 free parameters + 3 (Z0, Σgas and σ) - No analytical expression 2-D 3-D Tilted Ring Model: Fitting Strategies Tilted Ring Model: Fitting Strategies Di Teodoro & Fraternali, 2015
10. NGC 3198 (Effelsberg) Beam area Beam Smearing: 3D Vs 2D Beam Smearing: 3D Vs 2D
11. Glazebrook 2013 σ ↑ and v/σ ↓ with z? Wisnioski et al., 2015 Glazebrook, 2013 Deriving reliable Vrot and σgas is essential (breaking degeneracy!) z = 2 z = 0 σHα ~ 50-80 km/s h ~ 1500 pc σHI ~ 8 km/s, σHα ~ 25 km/s h ~ 50-100 pc Tully-Fisher Relation evolution Evolving vs not evolving? Resolved kinematics at high-z through emission-lines (Hα, O[III], ...) IFS surveys Kinematics Of High Redshift Galaxies Kinematics Of High Redshift Galaxies
12. Hα F814 VLOS σOBS Hα F814 VLOS σOBS 18 galaxies in Hα with KMOS (KROSS and KMOS-3D surveys) 0.85 < z < 1 9.5 < Log(M * /Mʘ ) < 10.5 Normal SF (SFR < 40 Mʘ /yr) High-z Galaxies: KMOS Sample High-z Galaxies: KMOS Sample
13. zcos_z1_202 zcos_z1_692 Data Model 0 0 1.3 1.3 -1.3 -1.3 -150 150 0 Offset from center (arcsec) VLOS (km/s) 0 0 1.1 1.1 -1.1 -1.1 -200 200 0 Offset from center (arcsec) VLOS (km/s) Major axis Major axis Minor axis Minor axis major axis major axis minor axis minor axis High-z Galaxies: Models Vs Data High-z Galaxies: Models Vs Data
14. Steeply rising + Flat until last point Shape similar to local SF galaxies with ~ M * 10 km/s < σHα < 40 km/s Comparable to local galaxies Rotation curves Velocity dispersions High-z Galaxies: Rotation & Velocity Dispersion High-z Galaxies: Rotation & Velocity Dispersion Di Teodoro et al. 2016
15. No significant evolution to z~1 Good agreement with local TF Local TF (Reyes+11) Tully-Fisher relation High-z galaxies: σ evolution & TFR High-z galaxies: σ evolution & TFR Di Teodoro et al. 2016
16. Many published papers have made use of 3D-Barolo Detailed structure of local disk galaxies (HI, CO) Low mass systems (dwarf and ultra-diffuse galaxies) High redshift disks, up to z~6! (rec lines, C+) Nuclear molecular rings and accretion disks Cosmological simulations Circum-stellar disks Local and high-z outflows Gravitational lensed galaxies (mass+kinematic) 3D-Barolo So Far 3D-Barolo So Far
17. PART II. The cold nuclear outflow of the Milky Way The cold nuclear outflow of the Milky Way Collaborators: - Naomi McClure-Griffiths (RSAA-ANU) - Felix J. Lockman (NRAO-GBT) - Lucia Armillotta (Princeton)
18. Galactic Winds Galactic Winds What is an outflow (or galactic wind)? Galactic disk (gas + stars + dust) Gas gets pushed out BO O M !
19. Galactic Winds Galactic Winds OBSERVATIONS THEORY Melioli et al., 2013 Tanner et al., 2016 - Outflows commonly observed in the local and high universe - Different gas phases co-exist: ionized, neutral and molecular Westmoquette et al., 2005 Bolatto et al., 2013 M82 NGC253 Cold and dense gas can survive in filaments Lifetimes depends on - mach number - density contrast - wind temperature Zhang et al., 2015
20. Galactic Wind In The Milky Way Galactic Wind In The Milky Way Our Galaxy has its own wind! Giant lobes extending to 8-10 kpc and detected in: - γ-rays (Fermi Bubbles, Su+10) - X-rays (e.g., Kataoka+13) - Mid-infrared (Bland-Hawthorn+13) - Polarised radio (Carretti+13) Ackermann et al., 2014 Credits to NASA Bi-conical outflow generated a few 106 years ago by either SF (Crocker+11) or SMBH (Yang+12)
21. H HI I Tracing The MW Wind Tracing The MW Wind HI evacuated by wind? or Pre-evacuated cavity? Evidence for a cavity in the HI gas that anti- correlates with γ-ray Lockman & McClure-Griffiths, 2016 Finding the relics of HI swept up by the wind 5 kpc -10 -5 0 5 10 Galactic Longitude (deg) Galactic Latitude (deg) -10 -5 0 5 10 High sensitivity survey above and below the Galactic Centre with the GBT ATCA Di Teodoro et al. 2018a
22. VLSR = 200 km/s -20 -10 0 10 20 Galactic Longitude (degree) Galactic Latitude (degree) -20 -10 0 10 20 -20 -10 0 10 20 Galactic Longitude (degree) Galactic Latitude (degree) -20 -10 0 10 20 VLSR = -130 km/s Masking the MW disk emission Masking the MW disk emission GALACTIC DISK ROTATION GALACTIC DISK ROTATION ANOMALOUS CLOUDS ANOMALOUS CLOUDS GOAL: detecting and studying anomalous clouds above and below the GC Clouds not in the disk Masking the MW disk by modelling it!
23. Results: source detection Results: source detection 100+ anomalous clouds covering ~ 130 deg2 GC GC
24. Wind kinematic model Wind kinematic model Describing observed cloud kinematic with a simple a galactic wind model SUN GC R z θ l b R0 D d r CLOUD ϕ x y Vw ≡ Vw (r) Simplest model defined by 2 parameters: - wind velocity Vw = const - opening angle α = π – 2φ + acceleration term A cloud in (R, z, θ) with V = V(r) can be easily mapped into the (l, b, VLSR ) system:
25. Wind best model Wind best model Simulating winds with different velocities and opening angles ` Best model: A wind accelerating from the Galactic Centre to a velocity of about 330 km/s at ~2 kpc. Opening angle: 140 deg Di Teodoro+18, Lockman & Di Teodoro 20
26. Derived wind properties Derived wind properties Model-dependent derived properties for a wind with Vw = 330 km/s and α = 140º ` - Total HI mass in clouds: - Cloud lifetimes: ~ few x 106 years Challenge for theory. Destruction timescales are generally lower Clouds likely represent the cold gas component entrained in a hot, starburst-driven nuclear wind - Wind kinetic power: > 3 x 1039 erg/s Can be supplied by GC with SFR~0.1 Ms/yr (Crocker12) Di Teodoro+18 - Cold mass loading rate: < 0.1 Msun/yr Similar to SFR in the CMZ 5 x 105 Msun
27. Currently on-going projects Currently on-going projects - Kinetic Tomography of the Milky Way at high latitudes (with Josh) - Full characterization of the Milky Way cold wind with APEX + GBT (with N. McClure-Griffiths, J. Lockman, L. Armillotta, A. Fox, R. Bordoloi) - Galaxy assembly in early SF galaxies at z~5-6 with ALMA (TRICEPS survey) (with F. Lelli, F. Fraternali, C. DeBreuck, R. Maiolino) - Dynamics of super-massive spiral galaxies (with L. Posti, P. Ogle, M. Fall) - Deviations from Newtonian fall in proto-planetary disks (with F. Fraternali et al.) Good intentions for 2020: Thank you for your kind attention Thank you for your kind attention