Gavin Rowell High Energy Astrophysics Group, School of Physical - PowerPoint PPT Presentation

http://www.physics.adelaide.edu.au/astrophysics/MopraGam/ Gavin Rowell High Energy Astrophysics Group, School of Physical Sciences University of Adelaide Nanten2 Meeting (UWS, Sydney) Feb. 2015

Gamma-rays (~30 GeV to ~500TeV) Highly effective tracer of high energy particles High impact results – 18 Nature, Science, PhysRevLett papers since 2004 http://tevcat.uchicago.edu/ Great success with HESS, VERITAS, MAGIC etc. but we want & need to do more...... HESS-II, MAGIC-II, CTA

Carrigan et al 2013 TeV Milky-Way (according to HESS)

Carrigan et al 2013 TeV Milky-Way (according to HESS)

HESS TeV horizon 1% & 10% Crab flux > 1 TeV Carrigan et al 2013

Special Issue Vol 43, CTA Science CTA Science Pg 1-356 (Mar 2013) Extragalactic AGN z>0.5, GRBs, Star-bursts, Gal. clusters, AGN haloes.. Astro-particle Dark matter, Lorentz invariance.... Optical Intensity Interferometry

Gamma Rays from multi-TeV particles + CMB Protons: Gamma-rays and gas targets are generally spatially correlated (need to map atomic and molecular ISM) Electrons: Gamma-ray (IC) + X-ray, radio emission (synch.) coupled (Bremss. usually minor)

Gamma Rays from multi-TeV Cosmic-Rays (p, He ...etc) Gamma Rays from multi-TeV Cosmic-Rays (p, He ...etc) CRs deflected by magnetic fields p+p → π o → 2 γ π ± → µ ± → e ± + ( ν µ ν e …. ) GAS CLOUD Gamma-Rays (+ Neutrinos) Observational Signature → Gamma-rays and gas are ~ spatially correlated (need to measure gas in all chemical states) → Intimate connection with mm- radio astronomy (tracing gas) . → Expected gamma-ray flux F γ ~ (cosmic-ray density) x (gas mass) / (distance) 2

Why study cosmic-ray (CRs) and electrons? - Energy density of galactic CRs similar to that in starlight, magnetic fields, and gas kinetic energy → these energy densities are all tightly connected. → CRs carry energy throughout galaxies → CRs intimately linked to evolution of stars and galaxies - CRs are a signpost of massive stellar evolution – death (supernova remnants) – life (winds from massive stars) – birth (perhaps) signalling onset of fusion/stellar winds – initiates astro-chemistry → life! - Where do magnetic fields come? Are they important? – Magnetic fields can greatly inflence star formation! – CRs can create magnetic fields - they ionise atoms - CRs and electrons trace outflows and jets – jets, pulsar winds, accretion, GRBs-hypernovae.....

Gamma-Rays from Cosmic-Rays escaping RXJ1713 SNR Isotropic diffusion Casanova etal 2010 (Gabici etal 2009) t esc ~ (E/E max ) 2.3 (γ esc + γ diffuse ) / γ diffuse Age = 1600 yr, d = 1 kpc Slow diffusion D = 10 26 cm 2 /s → Expect ~degree-scale TeV emission

CR diffusion – not necessarily Isotropic! Malkov etal 2013 Nava & Gabici 2013 → Nearby clouds will CR propagation see different CR along B flux tube densities Isotropic Anisotrpic → Need detailed maps of ISM gas + B-field direction CR overdensity

CR Diffusion Into Molecular Clouds Gabici etal 2007 R = distance CR travels into molecular cloud core 10 TeV proton 1 TeV proton χ= diffusion suppression → Low energy CRs can't reach cloud core. → Expect harder TeV spectra from cores. → Don't expect electrons to penetrate!! (due to sync. losses) mol. cloud core → Need to map dense cloud cores

Galactic Plane TeV Surveys : Major Issue Funk et al 2012 - CTA will provide Galactic Plane TeV Gamma-ray maps on ~1-3 arc-min scales (~0.5 arc-min possible – high quality cuts) - >3 sources per deg 2 |b|<0.2 o |l|<30 o (Dubus etal 2013) - Diffuse TeV components visible? from CR 'sea' – maybe local CR accelerator enhancements – yes Confusion guaranteed (same as for Fermi-LAT at GeV energies!) - Mapping the ISM on arc-min scales over the plane will be essential Mopra (CO, CS ), Nanten2 (CO), ASKAP (HI, OH), THz (CI, C+)

Angular Resolution (HESS, CTA..) Acharyara etal 2013 HESS hi-res cuts >=10 tels e.g. DeNaurois etal 2009 CTA – 2 tels ISM cloud core at few kpc Typical radius X e.g. Cameron et al 2012 CTA MST-SCTs with small pixels and/or hi-res cuts → resolve cloud cores!

We need to map the interstellar gas to discriminate hadronic vs. leptonic gamma-rays! HI (atomic H), OH CO CO, NH 3 , CS, SiO... Gas density ~10 1 to 2 cm -3 ~10 3 cm -3 >10 3 to 4 cm -3 ATCA Parkes HEAT – THz telescope (Antarctica) [CI] + [CII] → tracing the complete C budget! ASKAP

http://www.physics.adelaide.edu.au/astrophysics/MopraGam/ Team Members Gavin Rowell (lead, Adelaide), Michael Burton (UNSW), Yasuo Fukui (Nagoy), Bruce Dawson (Adelaide), Andrew Walsh (Curtin), Felix Aharonian (DIAS/MPIK), Stefan Ohm (Leicester) Adelaide PhD students: Brent Nicholas (now at DSTO), Nigel Maxted (now at Montpellier), Phoebe de Wilt, Jarryd Hawkes, Fabien Voisin, Jame Lau, Rebecca Blackwell, Stephanie Pointon (MPhil student). Targets Since 2012 observed over ~40 TeV gamma and high energy sources, > 1500 hrs. Student Projects Phoebe deWilt – ISM survey of unidentified TeV sources, TeV+HII regions Jarryd Hawkes – Outflow sources (e.g. XRBs) and magnetars Fabien Voisin – Pulsar Wind Nebulae James Lau – SNR/MC associations / G328 filament Rebecca Blackwell – CMZ Stephanie Pointon – Two bright unidentified TeV sources

Dense (>10 4 cm -3 ) Cores of W28 Molecular Clouds (Nicholas etal 2011, 2012) NH 3 (1,1) , CS(1-0) NE Shocked Cloud Mass of dense core ~10 4 M sun → Gamma-rays from CS clumps (~<10 -13 ph/cm 2 /s) → Detectable & maybe resolvable by CTA

χ=10 −3 RXJ1713: Dense Cores CS(1-0) (Mopra) Maxted etal 2012 Core C n > 10 4 cm -3 M ~ 50 – 100 M sun χ=10 −4 Min CR energy penetrating Core C vs. diffusion supression χ → Another way to Core A probe CRs from χ=10 −5 SNR. Core C Core B

Mopra HOPS++ & Unidentified TeV Sources DeWilt etal 2012,2015 HESS J1745-303 NH3 ortho/para ratio studies HOPS Survey of NH 3 , H 2 0 masers, plus other 12mm lines Walsh etal 2011, Purcell etal 2012 http://awalsh.ivec.org/hops/public/ index.php

Where are the ions in pulsar Winds? (Fabien Voisin) - Ions expected in pulsar winds? e.g. Gallant & Arons 1994 - Only indirect evidence X-ray wisps Gaensler etal 2002 → Look at dense mol. gas Best case: HESSJ1825-137 Voisin etal 2014 Nanten CO Mopra CS, NH 3 , SiO Mopra CS, H62a, NH3(1,1)

HESSJ1640-465 & HESSJ1641-463 (James Lau) Nanten CO(1-0) Mopra CO(1-0)

ISM Studies of Magnetars (Jarryd Hawkes)

HESSJ1616-508 & HESSJ1614-518 (Stephanie Pointon)

Westerlund 1 – The Wolf-Rayet Haven Aharonian etal 2012 (Gavin Rowell, Stefan Ohm) Molongolo 848 MHz image >24 WR stars, ~80 blue supergiants ! L wind ~ 10 40 erg/s; Age ~ 5 Myr (Crowther etal 2006) X-rays L x-ra y ~ 10 34 erg/s (Muno etal 2006) L TeV ~ L x-ray PSR J1648-4611 P spindown ~ 10 33 erg/s/kpc 2 Magnetar: AXP CXOU J1647-4552

First Results from H.E.S.S. phase II First Results from H.E.S.S. phase II Gavin Rowell (for the H.E.S.S. collaboration) First “Mono” Results Statistics (17 hr) from New 28metre ~8σ signif (a-priori) Telescope Pulsar period - 89ms N γ = 6059 ± 640 Grey Band Fermi-LAT <E> = 40 GeV ~30 GeV threshold pulsar peak phase - Vela Pulsar - Crab Nebula - Gal. Centre - 2 AGN → Improved 0.1–10 TeV sensitivity

MopraGam – The Next Steps 2008-2014 Adelaide-led 7/12mm targeting now ~ complete 3mm CO survey extensions underway TeV SNR shell surrounds (RXJ1713, VelaJnr, HESSJ1731) 2015 New targets (>~300 hr for 7/12mm?): - LMC 30DorC etc. 3mm CO, CS, SiO - CO survey extensions (CCC, TeV SNRs...) - HESS 'PeVatrons' - HESS Collaboration AO next week! - Other suggestions welcome Already great legacy for HESS-II and CTA 2016-2018 Mopra LIEF submit Apr 2015 - Complete CO survey b<=+-1.0deg.. - CS/NH3 survey of CTA Key Science Project regions?

Thank you..