Molecular clouds and gamma rays

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Molecular clouds and gamma rays   Yasuo Fukui Nagoya University   H. Sano, S. Yosiike, T. Fukuda, H. Matsumoto T. Inoue, S. Inutsuka, R. Yamazaki, T. Tanaka, F. Aharonian, G, Rowell, M. Tavani, A. Guliani, N.McClure-Griffiths+ March 2-4, 2013 Physics with GAMMA 400, Trieste

Molecular clouds and gamma-rays The origin of the cosmic rays is SNR?- Yes. Interstellar Medium ISM Molecular clouds: dense neutral gas H2 (2.6mm CO) - density 10^3 cm-3 or higher, Tk=10-20K Atomic clouds: dense atomic gas HI (21cm HI) - density 1-100 cm-3, Ts=30-100K Gamma-rays produced by 1) Hadronic scenario: This has been verified in 2012-13 - cosmic ray CR proton - ISM proton reaction, neutral pions decay into gamma rays 2) Leptonic scenario - CR electrons, Inverse Compton (IC) process, CMB etc. Gamma-rays (0.1GeV-100TeV) observed by HESS, MAGIC, VERITAS, Fermi, AGILE and CTA[2016-]

Hadronic Cosmic-ray Interactions  (CMB)  (Cosmic Microwave Background)  Compton scattering e+e– p π0  (CMB) π± → µ± →e± p p (Inter stellar medium) Target ISM protons No real test yet for the targets By H. Tajima 2006

SNRs emitting gamma-rays By courtesy of H. Tajima

CO transitions to probe molecular hydrogen Hydrogen molecules are not observable in radio. Too high energy levels. Only in absorption. Carbon monoxide CO and others can be observed in rotational transitions. Sub-mm transitions from generally higher excited states ratio between J and J’ gives density/temperature.

NANTEN & NANTEN2 @Las Campanas, alt.2400m @Atacama, alt.4800m

TeV γ vs. CO(J=1-0) Left: NANTEN 12CO(1-0) image (beam size : 2.7’) of the W 28 region for VLSR=0 to 10 km/s with VHE γ ray significance contours overlaid (green) -levels 4,5,6σ. The radio boundary of W 28, the 68% and 95% location contours of GRO J1801-2320 and the location of the HII region W 28A2 (white stars) are indicated. Right: NANTEN 12CO(1-0) image for VLSR=10 to 20 km/s. (Aharonian et al. 2007)

Comparison of 12CO(J=1-0) with X-rays -11 km/s < VLSR < -3 km/s D A B C Fukui et al. 2003

SNR G347.3-0.5 (RX J1713.7-3946) Aharonian et al. 2005 Shell-like structure: similar with X-rays - No significant variation of spectrum index across the regions spatial correlation with surrounding molecular gas Aharonian et al. 2005

RX J1713.7-3946 Fukui et al. 2012, ApJ, 746, 82

Dark HI SE Cloud (Self-Absorption)

HI becomes dark at higher density Goldsmith et al. 2007

ISM protons in RX J1713.7-3946 HI + 2H2 Fukui et al. 2012 先行研究として、星間物質の観測により、TeVガンマ線の強度と星間陽子数の相関を示した例として Fukui et al. 2012を紹介します。 左側の図は超新星残骸RXJ1713.7-3946の図です。 カラーは観測により明らかになった星間陽子の個数密度、黒のコントアがTeVガンマ線の放射強度を示します。 右の図はTeVガンマ線強度と星間陽子数の角度分布を表しています。 左の白い楕円で囲まれた領域の0度、90°、-90°とそれぞれの領域で 黒がガンマ線の強度、そして赤が、全ての星間陽子の個数を表します。 Fukui et alでは、このように、Tevガンマ線と、星間陽子の数が強く相関している事がを示しました。 この研究により, 超新星残骸で宇宙線陽子が加速されている事を世界で初めて観測的に支持しました。 また、この研究の重要な点として、分子雲観測により計算された水素分子として存在する 陽子の個数だけではなく、中性水素21cm輝線の観測で明らかになった水素原子として存在する 陽子の数も合わせて計算したことがあげられます。 私は、このように宇宙線陽子が加速されていることを示すことのできる天体の2例目を探しました。 HI + 2H2 Fukui et al. 2012

ISM protons in RX J1713.7-3946 Support hadronic scenario 先行研究として、星間物質の観測により、TeVガンマ線の強度と星間陽子数の相関を示した例として Fukui et al. 2012を紹介します。 左側の図は超新星残骸RXJ1713.7-3946の図です。 カラーは観測により明らかになった星間陽子の個数密度、黒のコントアがTeVガンマ線の放射強度を示します。 右の図はTeVガンマ線強度と星間陽子数の角度分布を表しています。 左の白い楕円で囲まれた領域の0度、90°、-90°とそれぞれの領域で 黒がガンマ線の強度、そして赤が、全ての星間陽子の個数を表します。 Fukui et alでは、このように、Tevガンマ線と、星間陽子の数が強く相関している事がを示しました。 この研究により, 超新星残骸で宇宙線陽子が加速されている事を世界で初めて観測的に支持しました。 また、この研究の重要な点として、分子雲観測により計算された水素分子として存在する 陽子の個数だけではなく、中性水素21cm輝線の観測で明らかになった水素原子として存在する 陽子の数も合わせて計算したことがあげられます。 私は、このように宇宙線陽子が加速されていることを示すことのできる天体の2例目を探しました。 HI + 2H2 Fukui et al. 2012

Ellison et al. 2010 paper Uniform model, to account for gamma rays we need high proton density like 10 cm-3 Then we have too strong thermal X rays, contradicting no thermal X rays (Suzaku) This is not a problem if the ISM is highly clumpy; cavity (0.1 cm-3) and dense clumps (1000 cm-3) Cavity is the site of particle acceleration and clumps are the target

Inoue, Yamazaki, Inutsuka, Fukui 2012, ApJ, 744, 71

MHD simulations of shock-cloud interaction density vs. magnetic field Inoue+ 2010

density vs. magnetic field [sub-pc scale]

Shock propagation into dense gas n : density of clump n0 : ambient density (=1 cm-3) 10^4 cm-3, t〜1000yrs Penetrating Depth = 0.03 pc Sano et al. 2010

SNR RXJ1713 summary Gamma-rays corresponds well with interstellar H nuclei, CO+HI, allowing detailed identification of target protons in a density range from 100 to 103 cm-3. The gas is highly clumpy. Wp ~ 1048erg for 100cm-3: gamma rays ~ Wp x ISM Hadronic origin is consistent with the spatial correspondence Careful analysis of dense atomic and molecular gas, HI and CO, yields total ISM protons Shock-cloud interaction causes gas turbulence and strong B field up to mG (e.g., Uchiyama+ 2007)

TeV gamma-ray SNR RX J0852.0-4622 Color TeV gamma rays contour X rays

RX J0852: CO distribution (interact with the SNR) CO vs. X-rays good spatial corresp-ondence between the CO and X-rays Interacting with the SNR image: CO(1-0) I.I. (Vlsr: 24-33 km/s) contours: X-ray (1-5 keV)

RX J0852: HI distribution (interact with the SNR) HI vs. X-rays HI wind bubble at same velocity in CO ISM cavity created by the progenitor Image: HI I. I. (Vlsr: 28-34 km/s) contours: X-ray (1-5 keV)

TeV gamma-ray SNR RX J0852 ISM Proton Column Density Distributions Fukui et al. 2013, in prep. Color: HI+2H2 Contour : TeV g rays

TeV gamma-ray SNR RX J0852 ISM Proton and TeV gamma-ray Distributions ISM protons good correspondence as targets for cosmic ray protons

RXJ0852 Fermi LAT

Gamma-ray spectrum of RXJ1713 Abdo et al. 2011 The hard spectrum is not unique to the leptonic scenario The hard spectrum is explained by energy dependent penetration of CR protons into dense molecular gas.

Hadronic g-ray spectrum for dense cloud cores Gabici 2007, Zirakasivili Aharonian 2010, Inoue, Inutsuka, Yamazaki, Fukui 2012 accelerated particles in the cavity diffuse into clouds and pions are created diffusion length: - mass of the cloud penetrated by CR particles (∝ number of gamma rays) Dense cloud cores [ r ∝ r -2 ] Photon spectrum: N(E) ∝ M(E) E -p ∝ E 1/2-p = E -1.5 for p = 2 The same with the leptonic spectrum by IC Hadronic scenario is consistent with the Fermi spectrum

ISM/gamma-ray comparison RXJ1713.7-3946 -Dense molecular rich/clumpy M(H2)=104Mo, M(HI)=104Mo -Hard gamma-ray spectrum RXJ0852.0-4622 -Diffuse atomic rich/uniform M(H2)=103Mo, M(HI)=104Mo -Soft gamma-ray spectrum

X rays vs. CO pc-scale correlation

SNRs emitting gamma-rays By courtesy of H. Tajima

W44 new Fermi/AGILE results

W44 CO 2-1/1-0 Yoshiike+2013 ApJ

W44

W44 CO

W44 Uchida+ 2012

W44

Summary ISM plays a key role in production of the gamma-rays and X-rays. ISM target protons showing good spatial correspondence with gamma rays In RX J1713 and RX J0852, gamma rays are hadronic,   CR proton acceleration has been verified -Their total CR proton energy is 10^48 erg Dense clumps amplify B field via shock-cloud interaction, leading to enhanced X-rays X-ray photon index becomes small toward dense clumps. This may suggest additional acceleration in turbulent magnetic field Middle-aged SNRs W44 etc. GAMMA400/CTA will provide future steps forward