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Low Energy measurements of Cosmic Rays suggested by the HE group 1

Low Energy measurements of Cosmic Rays suggested by the HE group 1. Tracing 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)

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Low Energy measurements of Cosmic Rays suggested by the HE group 1

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  1. LowEnergymeasurements of Cosmic Rays suggested by the HE group 1 • Tracing 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 • 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 suggestedby 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. • LE measurements for the Fermi bubble • Variable CR ionization in nebulae close to powerful variable microquasars • Radio polarization measurements at the SN Shock environment

  3. 1.a Localisation of MC with masers • VLBA observations of H2O masers in Sgr B2 have led to parallaxmeasurements of the cloud(Reid+ 09)and proper motion respect to Sgr A* • Furthermeasurements of maser sources in MolecularCloudscouldallow the LOS-localization of otherMCs in CMZ • In W28 there are maser sources in both the MC interactingwit the SNR and thosecloseby => relative localisation throughparallaxmeasurements ?

  4. 1b.Molecule Ions and dustSurveysof the CMZ region • Most results (egthosebased on 6.4 keV line measures) are based on CS (0-1) surveys • Furthermolecular line surveys, sensitive to dense MC canreduceuncertainties in the estimatedparameters • HCO+ and HF maybe the best tracers (Gerin’s talk)? • Herschel (HEXGAL program) shallprovidesoon mol-gas distribution withmeasurements in 500GHz – 2THz range, and possiblydust distribution

  5. 2.a X-ray inducedchemistry • Measurements of SiO (2-1, 86,8 GHz) in CMZ and comparisonwith CS show thatSiO /CS iscorrelated to Fe 6.4 keV line (AmoBaladron+ 09) • FurtherSiO (and othermolecules) surveyssomehowcorrelatedwith 6.4 keVcan show if MC chemistryisrelated to X-ray variations • X-rays able to evaporate grains => increase Silicate abundance • Part of this program alreadyproposedwith IRAM and APEX, by J. Martin-Pintado +.

  6. SiO vs CS (AmoBaladron+ 09)

  7. XMM-Newton - Ponti et al. (2010) 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 H3+?

  8. 4. Fermi Bubbles 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 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 H3+ 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 g-ray spectrum Hadronic Model Pros: No cooling or energetics problem Cons: Long collision time; Confinement and collimation; No intensity gradient  B > 6 mG to account for WMAP haze; low-energy cutoff in g-ray spectrum

  9. 5.Transient X-ray/CR ionizationin galacticXRBs

  10. 6. Radio-Infrared high resolution observations of SNRs 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)

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