LOFAR-MKSP workshop Robert Benjamin (U of Wisconsin) Apr 6, 2011 Models and Observations of the Warm Ionized ^ Magnetised Medium (WIMM) of the Galaxy Talk Outline 1.WHAM update 2.Modeling WHAM 3.Magnetised HVCs! Dame & Thaddeus 2011 submitted

LOFAR-MKSP workshop Robert Benjamin (U of Wisconsin) Apr 6, 2011 Galactic Diffuse Ionized Gas (DIG) Layers Milky Way (Reynolds 1989): Pulsar DM in globular clusters [at known distance] External galaxies NGC 891 (1990): H  emission from edge-on spirals Dettmar 1990Rand et al Low frequency free-free absorption of radio synchrotron halo (Hoyle & Ellis 1963)

LOFAR-MKSP workshop Robert Benjamin (U of Wisconsin) Apr 6, 2011 Wisconsin H  Mapper goes to Chile Ground-based high throughput velocity resolved survey 15 cm aperature dual-etalon Fabry-P é rot spectrometer — largest used in astronomy — attached to 0.6m aperature sidereostat Velocity resolution: 12 km/s Spectral window: 4800 to 7300 Å Angular resolution: 1 o 3  sensitivity: 0.15 Rayleigh (10 6 /4  ph cm -2 s -1 sr -1 = 2.4 x ergs cm -2 s -1 sr -1 at H  )

LOFAR-MKSP workshop Robert Benjamin (U of Wisconsin) Apr 6, 2011 [SII] 6716 Galactic plane observations (Gostisha et al 2011) 330 o 320 o Ionizing source: two late-type O stars near the center of the bubble HD =  Cir (l=319.69, b=-2.91, O8.5 V, m V =5.07) and HD (l=320.13, b=-2.6, O8 IIIp, m V =5.43). Log L LC = and 49.22, consistent with H  emission. Distance greater than 430 pc.

LOFAR-MKSP workshop Robert Benjamin (U of Wisconsin) Apr 6, 2011 Mysteries of the WiMM Q: What powers it? A: Ionizing photons from O stars that apparently leak from disk … — Puts constraints on spatial organization of ISM, but attempts to “ photoionize ” Joung & MacLow (JM06) simulations don ’ t create our WIM (Wood et al. 2010, ApJ, 721, 1379). Q: What stirs it? A: High latitude EM distribution very well fit by log-normal function (Berkhuijsen & Fletcher 2008, MNRAS, 390, L19; Hill et al 2008, ApJ, 686, 363). Idealized models of (M)HD turbulence that is mildly supersonic (M s ~2) but sub-Alfv é nic (M A ~0.6) can match (1) EM distribution, (2) H  line widths, and (3) pulsar DM|sin b| distribution. Q: What supports it? A: Scaleheight of 1-2 kpc much thicker than the scaleheight of 10 4 K gas in the gravitational potential. Cox (2005, ARAA, 43, 337) shows that the observed vertical distribution is consistent with hydrostatic equilibrium given observational estimates of magnetic, CR, turbulent pressures. But what is the physics that establishes this equilibrium and how would it change with SFR,  gas,  stars ? Q: What temperature is it? A: A mixture? Dong & Draine, 2011, ApJ 727:35 address question of discrepancy of optical (8000 K) vs. free-free (3000 K) by appealing to mix of components/mechanisms.

LOFAR-MKSP workshop Robert Benjamin (U of Wisconsin) Apr 6, 2011 Can we create a numerical WImM (and then photoionize it?) A: We will see … Previous results: Hydrodynamic simulations (JM06) + Monte Carlo photoionization (Wood et al 2010) show photons escape clumpy ISM, but do not produce an extended thick ionized layer and produce much broader distributions of EM than observed. Hypothesis: Addition of magnetic field will provide additional pressure support, producing a more vertically extended layer with less compression (and narrower EM distribution). Simulations: FLASH v2.5 adaptive-mesh hydrodynamic model of a turbulent, supernova-driven ISM (Joung & MacLow 2006,2009). A. Hill has added the MHD solver of Waagan, Federath & Klingenberg (2011, astro-ph/ ). Basic characteristics: 1 kpc x 1 kpc x [2 x 20 kpc],  x res (z)=2-30 pc, B x, ini =0, 6.5, 13  G evolved for 400 Myr. Galactic g z,  gas, SNe rate fixed. Found sensitivity to (a) grid size, (b) T halo, i, (c)  x res.

LOFAR-MKSP workshop Robert Benjamin (U of Wisconsin) Apr 6, 2011 Medium resolution results:  x res =8-64 pc Initial conditions that definitely (or may) matter ? T halo,i  x range ≥ 1 kpc  y range ≥ 1 kpc  z range ≥ 20 kpc  t max ≥400 Myr  f SN ? B x,i

LOFAR-MKSP workshop Robert Benjamin (U of Wisconsin) Apr 6, 2011 Vertical profiles (after 100 Myr) Dickey-Lockman HI + Reynolds WIM

LOFAR-MKSP workshop Robert Benjamin (U of Wisconsin) Apr 6, 2011 Midplane slices Will definitely change with higher resolution runs …

LOFAR-MKSP workshop Robert Benjamin (U of Wisconsin) Apr 6, 2011 An oscillatory surprise! Similar to that predicted by Walters & Cox (2001, ApJ 549, 353) Models of Vertical Disturbances in the Interstellar Medium

LOFAR-MKSP workshop Robert Benjamin (U of Wisconsin) Apr 6, 2011 Magnetized HVCs? McClure-Griffiths et al (2010, ApJ, 725,275) Measurement of Magnetic Field in a [Magellanic Stream] Leading Arm High-Velocity Cloud RM reversal coincident with HI HVC (from Taylor et al 2009 RM catalog from NVSS MHz/ MHz) Using an estimate of n e L: P B comparable to estimated ram pressure. Ordered field higher than in SMC/LMC. Unsolved Mysteries of High Velocity Clouds — Benjamin (2004)

LOFAR-MKSP workshop Robert Benjamin (U of Wisconsin) Apr 6, 2011 Smith Cloud (Smith 1963) Lockman et al 2008, ApJL 679, L21 d= kpc; 12.4±1.3 kpc z=-3 kpc Projected size=3x1 kpc Main body has two kinematic components v space =296±20/ 271±6 km/s v ISM =130±14/130±5 km/s N HI (cloud)=1-5 x cm -2 Assuming cloud moves as a coherent linear object projection on our line of sight--> L

LOFAR-MKSP workshop Robert Benjamin (U of Wisconsin) Apr 6, 2011 Ionized component of Smith Cloud Hill et al. 2009, ApJ 703, 1832 Brightest region of H  at the tip of HI cloud, but an almost equally bright H  cloud with low N(HI).

LOFAR-MKSP workshop Robert Benjamin (U of Wisconsin) Apr 6, 2011 An extended search? Another clump of RM reversal suggests a deeper search for high velocity gas.

LOFAR-MKSP workshop Robert Benjamin (U of Wisconsin) Apr 6, 2011 Conclusions — M. Haffner, A. Hill, K. Barger, R. Reynold, M. Gostisha, R. Benjamin Evidence for a second magnetized high velocity cloud where key parameters (position, velocity, neutral/ionized mass) are known. Significance? — R. Benjamin, A. Hill, ? 3D adaptive mesh MHD simulations underway to explore the vertical structure, porosity/ionization, and dynamics of warm ionized medium. First two papers by this summer. Questions on B field evolution/topology welcomed! Magnetic fields definitely provide additional vertical support, narrow range in PDF than hydro-only models. Match to our galaxy not yet clear. Under certain conditions, simulations result in a damped oscillatory motion, with a period predicted by Walters & Cox (2001). — A. Hill, R. Joung, M. Mac Low, K. Wood, K. Waggan, C. Federath, C. Klingenberg, R. Benjamin WHAM all-sky velocity-resolved H  survey almost complete. Data reduction should be done by end of the spring. Several surprises include a nearby off-plane HII region and increased depth through the Galaxy.

LOFAR-MKSP workshop Robert Benjamin (U of Wisconsin) Apr 6, 2011 Please Remove All Slides After This

LOFAR-MKSP workshop Robert Benjamin (U of Wisconsin) Apr 6, 2011 The problems with averages Volume vs. mass weighted? Very resolution dependent  x res =8-64 pc Very height dependent Black <125 pc Red kpc Green kpc