X-raying Galaxy Ecosystems of Disk Galaxies. Q. Daniel Wang IoA/Cambridge University University of Massachusetts

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1 X-raying Galaxy Ecosystems of Disk Galaxies Q. Daniel Wang IoA/Cambridge University University of Massachusetts

2 Hot Gaseous Corona Wang et al. (2001)

3 Key questions to be addressed: 1. How do diffuse X-ray properties vary among galaxies? 2. Does the diffuse X-ray emission trace the accretion or feedback of galaxies? 3. What is the nature of the X-ray emission? 4. How hot is our own Galaxy? X-ray observations I. A Chandra survey of hot gas around galactic disks. II. High-res emission spectroscopy of starforming galaxies, using XMM-Newton RGS data. III. X-ray absorption line spectroscopy.

4 I. Chandra survey of disk galaxies: imaging the CGM X-ray emission Galaxy sample: Highly-inclination angles (i > 60 o ) D < 30 Mpc Each with Chandra ACIS exposure > 10 kses Size: 53, compared to < 10 in previous studies Allowing for statistical analysis and comparison with cosmological simulations. Li & Wang 2013a,b

5 Diffuse X-ray Emission: Examples

6 Lx vs. energy C feedback rate Adding Type Ia SNe to the total energy input improves the E SN -L X correlation for normal galaxies; Type Ia SNe contribute 3%-93% of the input for our sample galaxies.

7 X-ray emission efficiency (η=l X /Ė SN ) vs. galaxy properties η < a few %! What determines the X-ray radiation efficiency? η is roughly proportional to the mean surface density of the galaxy mass (M TF /M * ).

8 Enhanced soft X-ray emission: NGC 4438 as an example An interacting system within the Virgo cluster. Good spatial correlation of the X-ray and Hα emissions. Color: Chandra kev Contour: Hα+[NII] Machacek, Jones & Forman (2004)

9 Comparison with elliptical/s0 galaxies SF disk galaxies tend to have higher Lx and T than expected for elliptical or S0 galaxies.

10 Fe/O abundance ratio vs. galaxy type Hot gas is Oxygen enriched in latetype galaxies, especially for starburst ones. Early type Later type

11 Q1: How does the X-ray emission depend on galaxy properties? Lx is correlated primarily with the total mechanical energy input rate and secondarily with the compactness of galaxy mass. Lx accounts for < a few % of the rate; the bulk of the energy is most likely gone with galactic outflows. Both Lx and T of the hot gas are typically higher than expected for elliptical/s0 galaxies. O is strongly enriched (relative to Fe) in late-type galaxies.

12 Comparison with simulations Simulations by Crain et al. (2010) Caveats of the comparison: The simulations predict large-scale, low-surface brightness emission, which is so far hard to detect. Simulated Lx is calculated over a much larger regions than those covered in the observations. Galaxy mass selection of the simulated sample: M * > 2 x M.

13 Comparison with simulations Li et al. (2013 in prep) Elliptical galaxies only Kim & Fabbiano (2013) The halo mass is obtained from the stellar-masshalo-mass-relation (Behroozi et al. 2010) The total masses are from optical kinematics of globular clusters and planetary nebulae (Deason et al. 2012). The total mass of a galaxy plays a key role in determining Lx.

14 Q2: Does the X-ray emission trace the accretion or feedback of the galaxies? The simulations greatly under-predict the X- ray emission in the vicinity of galactic disks and still seem to miss important X-ray-emitting processes in disk/halo interaction regions. The X-ray-emitting gas near the disks is apparently enriched by the stellar feedback and thus most likely traces the feedback. The emission is also observed from low-mass galaxies for which little hot gas is expected from the accretion.

15 II. X-ray Emission Line Spectroscopy The resonance line is found to be weaker than the forbidden + interrecommbination lines, which is not expected for thermal emission. Liu, Mao, & Wang 2011 Photons cm 2 s 1 Å Si XIII Mg XII Mg XI Ne X Ne X Ne IX Fe XVII O VIII Fe XVII O VIII O VII O VII N VII C VI r i f Wavelength (Å) Composite of optical (HST), infrared (Spitzer), and X-ray (Chandra) images Soft X-ray arises primarily from the interplay between the superwind and entrained cool gas clouds.

16 Charge exchange contribution to soft X-ray line emission Charge exchange (CX) nature of comet X-ray emission is confirmed, spectroscopically and temporally. CX has a cross-section of ~10-15 cm -2 and occurs on scales of the mean free path of hot ions at the interface. P CX /P th propto 1/n e 2 Peter Beiersdorfer Color: Chandra kev Contour: Hα+[NII] r i f Machacek, Jones & Forman (2004)

17 RGS Survey of nearby active star forming galaxies: examples Liu, Wang, Mao (2012) M83 M51 r i f r i f Soria & Wu (2002) (Credit: NASA/CXC/SAO/R.DiStefano et al.) Little evidence for significant AGN activities; foviii/fovii ratios are similar to star bursts than AGNs Soft X-ray are spatially correlated with star forming regions

18 Antennae galaxy Liu, Wang, & Mao (2012) r i f Optical (Yellow), X-ray (Blue), Infrared (Red)

19 Thermal plasma+charge exchange model fit of the spectrum of M82 Photons cm 2 s 1 Å Si XIII Mg XII Mg XI Ne X Ne X Ne IX Fe XVII O VIII Fe XVII O VIII O VII O VII N VII C VI Wavelength (Å) Zhang, Wang, Smith, & Foster (2013)

20 Thermal plasma+charge exchange model fit of the spectrum of M82 Photons cm 2 s 1 Å Si XIII Mg XII Mg XI Ne X Ne X Ne IX Fe XVII O VIII Fe XVII O VIII O VII O VII N VII C VI Without considering CX, X-ray spectral modeling leads to wrong metal abundances and underestimate of temperature. CX is proportional to the ion flux to hot/ cold gas interfaces; e.g., the size of the interfaces is ~ 20x larger that the crosssection of the superwind in M82. Wavelength (Å) Zhang, Wang, Smith, & Foster (2013)

21 Q3: What is the soft X-ray emission mechanism? A good fraction of the diffuse soft X-ray emission appears to arise from the CX. This interface mechanism naturally explains the spatial correlation between X-ray and cool gas tracers and the enhancement of X-ray emission in the immediate vicinity of galactic disks. CX measurements can potentially provide a powerful tool to probe the thermal, chemical, and kinematical properties of the hot plasma and its interplay with cool gas.

22 CX contributes to the soft X-ray background! 4U AGN X-ray binary ROSAT all-sky survey in the ¾-keV band

23 normalized counts s 1 kev 1 cm 2 Suzaku/XIS Spectrum of the Galactic Center field OVII -- OVIII -- FeXVII -- Ne IX -- FeXVII? -- MgXI -- SiXIII -- SiXIV -- SXV -- ArXVII -- Fe I-XVII -- FeXXVI -- FeXXV OVII OVIII Energy (kev) Wang, Roberts, et al 2013 in prep.

24 X-ray Absorption Line Spectroscopy: the Tomography of the Hot Gas 4U AGN X-ray binary ROSAT all-sky survey in the ¾-keV band

25 X-ray absorption line spectroscopy is powerful! Mrk 421 Tracing all K transitions of metals à all three phases of the ISM. Not affected by photo-electric absorptionà unbiased measurements of the global ISM. Multiple lines à velocity dispersion, gas temperature, and/ or relative metal abundance. Multiple sightlines --> differential hot plasma properties Joint-fit of absorption and emission data --> pathlength and density Wang et al. 05, Yao & Wang 05/06, Yao et al. 06/07/08/09/10

26 LMC X-3 Sightline as an example of X-ray absorption line spectroscopy BH X-ray binary undergoing Roche lobe accretion Away from the LMC main body 50 kpc away and V s = +310 km/s The line centroids of the OVI and OVII lines are consistent with their Galactic origin. N OVII ~ 1.9 x atoms/cm 2, similar to those seen in AGN spectra! b ~ 79 km/s T ~ 1.3 x 10 6 K, lower than that inferred from the emission spectrum of the X-ray background Wang et al. 2005

27 Q4: How hot is our own Galaxy? Thermal property: mean T ~ K toward the inner region ~ K at solar neighborhood Velocity dispersion from ~200 km/s to 80 km/s Abundance ratios ~ solar Structure: A thick Galactic disk with a scale height of ~ a few kpc, ~ the values of OVI absorbers and free electrons Enhanced hot gas around the Galactic bulge 95% upper limit: N OVII ~ 3 x10 15 cm -2 for r > 10 kpc ~ 1 x10 15 cm -2 for r > 50 kpc No evidence for a large-scale X-ray-emitting/absorbing halo!

28 Bonus Q: How hot are other galaxies? Sightline toward PKS with a total exposure of 1 Ms. Selected galaxies are in the kpc projected distances. Blue lines: Galactic absorption Vertical red bars: expected group absorption line positions Yao, QDW, Tripp, et al. (2010)

29 No evidence for large-scale massive hot gaseous halos around other galaxies like our own Stacking of absorption line spectra according to intervening galaxy/group redshifts à an effective exposure: ~ 10 Ms. But no absorption is detected! N OVII < cm -2, or < 1/10 of the column density observed around the Milky Way. Groups typically contain little gas at T~ K, unless the Oxygen abundance is << 1/10 solar.

30 Take-away Points 1. Diffuse Lx accounts for ~1% of the stellar feedback energy -> outflows. 2. Galaxy formation simulations under-predict X-ray emission around galactic disks. 3. Charge exchange appears to be an important mechanism for soft X-ray emission. 4. Detectable hot gas is located primarily in and around galactic disks. 5. The missing baryon matter of galaxies is likely dispersed on scales greater than galaxy groups (> 1 Mpc).

31 How to make progress? Need to detect the X-ray emission on large scales ß staking of existing data; erosita all sky survey; and more sensitive X-ray absorption line observations. Better spectral data ß deeper observations with Chandra/XMM-Newton, as well as Astro-H. Need complete samples for comparison with simulations ß erosita and dedicated large surveys with existing X-ray telescopes. Theory/simulations should predict the absorption column of various key lines, temperature, kinematics, and morphology, as well as Lx; dedicated modeling of the interfaces; spectral models of CX. Multi-wavelengths: e.g., radio.

32 Continuum HAlos in Nearby Galaxies an EVLA Survey (CHANG-ES; PI: Judy Irwin)pes Selec0on of 35 edge- on galaxies with inclina0on > 75 δ > GHz fluxes > 20 mjy 4 D25 15, All (> 400 hrs) data have been taken: two wide bands centered at 1.5 and 6 GHz and in B, C & D arrays, all 4 Stokes. 153 hours of GBT 0me in the upcoming cycle.

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