Galactic Neighborhood and (Chandra-enabled) X-ray Astrophysics

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1 Galactic Neighborhood and (Chandra-enabled) X-ray Astrophysics Q. Daniel Wang (University of Massachusetts) Frontier Science Galactic Neighborhood Panel Members: Leo Blitz, Julianne Dalcanton, Bruce Draine, Rob Fesen, Karl Gebhardt, Juna Kollmeier, Crystal Martin, Michael Shull (chair), Jason Tumlinson, Daniel Wang, Dennis Zaritsky, Steve Zepf + Astro2010 Science Liaison: Scott Tremaine

2 Galactic Neighborhood defined as: Milky Way and Local Group (stars, ISM, satellites) Galaxies out to redshifts z 0.1 (distance 420 Mpc, lookback 1.3 Gyr) Enables detailed study of: Resolved stellar populations Complex interconnected processes (stars-smbhs- ISM-CGM-IGM interactions; large/small scales) Local counterparts of distant objects (DM halos, SMBHs, dwarfs, feedback/accretion)

3 Four Science Questions: (Q1) What are the Flows of Matter & Energy in the Circumgalactic Medium (CGM)? (Q2) What controls the Mass-Energy-Chemical Cycles within Galaxies? (Q3) What is the Fossil Record of Galaxy Assembly and Evolution from the First Stars to the Present? (Q4) What are the Connections between Dark and Luminous Matter? Areas of Discovery Potential: Time-Domain Astronomy Astrometry

4 Unique X-ray observing capabilities of Chandra Highest spatial resolution Resolving X-ray structure Detecting faint sources Cleanly exercise sources for diffuse X-ray analysis Highest spectral resolution from LETG and HETG over the kev range. Allowing for real X-ray spectroscopy, with subarcsecond spatial (albeit mostly 1-D) resolution Stable and low non-x-ray background Particularly important for studying large-scale diffuse X-ray emission.

5 Q1, 2, and 4 are closely related to a single question: How does feedback work in and around galaxies? Feedback represents the least understood part of the structure formation and evolution theory: 1) the subgrid physics and 2) the global impact. Hubble, Chandra, Spitzer metal transport out to ~1 Mpc

6 X-raying the fundamental micro and/or interface astrophysics NTF G in the Galactic center Radio: Yusef-Zadeh et al. (1997) galaxy ESO in Abell 3627 X-ray on optical image: M. Sun, et al Particle acceleration Magnetic field reconnection Charge exchange Plasma cooling and heating Mass-loading Thermal evaporation/ condensation A Chandra workshop on feedback astrophysics?

7 How does the Feedback Affect the Global ISM? How does the feedback affect the ISM and the star formation (suppress or induce SF)? How does the feedback drive outflows (via radiation, thermal pressure, and/or cosmicray)? Townsley et al.

8 How does the Feedback Affect the Global CGM or the baryon/dark matter relation? How much mass and energy can escape into the CGM? How does the feedback regulate the IGM accretion of galaxies? Approach 1: X-ray absorption line tomography: More sight-lines and deeper observations. Measure the global mass-energymetal content, transport, thermal/kinematic structures of diffuse hot plasma in and around our Galaxy.

9 How does the Feedback Affect the Global CGM? Approach 2: Deep large-scale X-ray mapping: Individual observations have to be deep to remove enough background sources, which causes the cosmic variance. To check physical properties of hot plasma near outer boundaries if they are present. Mkn 231, 0.5 Ms ACIS kev Veilleux et al NGC 253

10 (Q4) Dark & Luminous Matter Connection What can X-ray observations tell us about the nature of the dark matter (e.g., via particle decay and annihilation, and self-interaction)? (Discovery area) Time-Domain Astronomy Enormous swaths of parameter space of the transient sky remain to be explored. Chandra, with its unique high resolution capability is well positioned for potential major discoveries of transient events and for variability studies of relatively faint X-ray sources in crowded fields.

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