1. Low Energy measurements of Cosmic Rays suggested by the HE group 1 1Tracing the distribution of matter in order to understand HE data Measurements of NH and 3D location of MC within GC CMZ H2O maser of the type of Sgr B2 MC for LOS location Herschel measurements of ions at the GC (HF) Herschel measurements of dust distribution and correlation to MC 2.Testing the past Sgr A* outburst hypothesis at other wavelengths Variable X-ray induced chemistry ? Eg. SiO IR echoes in MC ? => Do not seem viable !

2. LE measurements of CR suggested by the HE group 1 (2) 3 CR Ionization measurements at specific locations were there are HE indications of local CR particle acceleration – The case of the Arches cluster in the GC – Cases 4. and 5. 4LE measurements for the Fermi bubble 5Variable CR ionization in nebulae close to powerful variable microquasars 6Radio polarization measurements at the SN Shock environment

3. 1.a Localisation of MC with masers Further measurements of maser sources in Molecular Clouds could allow the LOS-localization of other MCs in CMZ In W28 there are maser sources in both the MC interacting wit the SNR and those closeby => relative localisation through parallax measurements ? VLBA observations of H 2 O masers in Sgr B2 have led to parallax measurements of the cloud (Reid+ 09) and proper motion respect to Sgr A*

4. 1b. Molecule Ions and dust Surveys of the CMZ region Most results (eg those based on 6.4 keV line measures) are based on CS (0-1) surveys Further molecular line surveys, sensitive to dense MC can reduce uncertainties in the estimated parameters HCO+ and HF may be the best tracers (Gerin’s talk)? Herschel (HEXGAL program) shall provide soon mol-gas distribution with measurements in 500GHz – 2THz range, and possibly dust distribution

5. 2.a X-ray induced chemistry Further SiO (and other molecules) surveys somehow correlated with 6.4 keV can show if MC chemistry is related to X- ray variations X-rays able to evaporate grains => increase Silicate abundance Part of this program already proposed with IRAM and APEX, by J. Martin-Pintado +. Measurements of SiO (2-1, 86,8 GHz) in CMZ and comparison with CS show that SiO /CS is correlated to Fe 6.4 keV line (Amo Baladron+ 09)

6. SiO vs CS (Amo Baladron+ 09)

7. 3. CR ionization rate close to the Arches cluster It has been proposed that the 6.4 keV line emission associated with the Arches cluster is produced by a high density of LECR protons  any evidence for a high CR ionization rate from H 3 + ? XMM-Newton - Ponti et al. (2010)

8. 4. Fermi Bubbles LOFAR; associated radio signatures; see low-energy cutoff depending on B spectral evolution with height Molecular lines to identify bubble edge High-resolution absorption spectroscopy of Na lines to measure outflow speeds H 3 + not feasible due to lack of OB stars at high latitudes Leptonic Model Pros: No energetics problem; correlation with WMAP haze Cons: Requires reacceleration; low-energy cutoff in  -ray spectrum Hadronic Model Pros: No cooling or energetics problem Cons: Long collision time; Confinement and collimation; No intensity gradient  B > 6  G to account for WMAP haze; low-energy cutoff in  -ray spectrum Origin: AGN vs. star formation activity Radiation mechanism: hadronic or leptonic If AGN powers the bubble, coincidence that it is transverse to plane of Galaxy

9. 5. Transient X-ray/CR ionization in galactic XRBs

10. X-rays filaments => Small scale high-energy processes associated with shock acceleration: Chandra micro-arcsecond resolution. In future possible X-ray polarization. Radio: high angular resolution+polarization: ALMA. Important to have such high resolution in radio + possibility polarization measurements: extension of lower energy particles wrt shock AND magnetic field configurations. Infra-red: Probe of non-linear back-reaction (E. van Dishoeck) Infra-red point in the MW spectrum: Probing non-linear back- reaction (eg Jones et al 2003 for CasA) 6. Radio-Infrared high resolution observations of SNRs