Interstellar shocks:! The contribution of SOFIA/GREAT!
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1 1! Interstellar shocks:! The contribution of SOFIA/GREAT! Antoine Gusdorf,!!!!!! LERMA, Paris, France! Claudio Codella,!!!!!!!!!!INAF Firenze, Italy! Rolf Güsten,!!!!!!!!! MPIfR, Bonn, Germany! Sibylle Anderl,!!!!!!!!!! IPAG, Grenoble, France! Maryvonne Gerin,!!!!!!!!! LERMA, Paris, France! Bertrand Lefloch,!!!!!!!!! IPAG, Grenoble, France! Pierre Lesaffre,!!!!!!!!!! LERMA, Paris, France! Silvia Leurini,!!!!!!!!! MPIfR, Bonn, Germany! Alexandre Marcowith,!!!!!!! LUPM, Montpellier, France! Frédérique Motte,!!!!!!!!! IPAG, Grenoble, France! 25/11/15! 1! SOFIA community tele-talk series!
2 Outline! 2! The importance of shocks in the interstellar medium of galaxies! From low-mass star formation! To higher-mass star formation! Filaments and ridges! Supernova remnants! 25/11/15! 2! SOFIA community tele-talk series!
3 The importance of shocks in the ISM of galaxies! 3! BHR71! 0.1 pc! archive image! Spitzer/IRAC 8 "m! adapted from! Gusdorf et al. 2015!
4 The importance of shocks in the ISM of galaxies! 4! BHR71! 0.1 pc! archive image! Spitzer/IRAC 8 "m! adapted from! Gusdorf et al. 2015!
5 The importance of shocks in the ISM of galaxies! 5! BHR71! 0.1 pc! archive image! Spitzer/IRAC 8 "m! adapted from! Gusdorf et al. 2015!
6 The importance of shocks in the ISM of galaxies! 6! BHR71! 0.1 pc! archive image! Spitzer/IRAC 8 "m! adapted from! Gusdorf et al. 2015!
7 The importance of shocks in the ISM of galaxies! 7! BHR71! 0.1 pc! CO (3-2)! archive image! Spitzer/IRAC 8 "m! adapted from! Gusdorf et al. 2015!
8 The importance of shocks in the ISM of galaxies! 8! BHR71! 0.1 pc! CO (3-2)! archive image! Spitzer/IRAC 8 "m! adapted from! Gusdorf et al. 2015!
9 The importance of shocks in the ISM of galaxies! 9! BHR71! 0.1 pc! physical processes! chemical! enrichment! CO (3-2)! archive image! Spitzer/IRAC 8 "m! adapted from! Gusdorf et al. 2015!
10 The importance of shocks in the ISM of galaxies! 10! BHR71! 0.1 pc! physical processes! chemical! enrichment! energetic impacts! star formation:!! scenarios!! triggered! cosmic rays! CO (3-2)! archive image! Spitzer/IRAC 8 "m! adapted from! Gusdorf et al. 2015!
11 11! From low-mass star formation! 25/11/15! 11! SOFIA community tele-talk series!
12 Low-mass star formation: the BHR71 example! 12! BHR71! CO (3-2)! CO (6-5)! SiO (5-4)! H 2! 0-0 S(5)!
13 Low-mass star formation: the BHR71 example! 13! BHR71! H 2 : Giannini et al. 2010! SiO : Gusdorf et al. 2011! CO : Gusdorf et al. 2015!
14 1D shock models! 14! n H = 10 4 cm -3 ; v s = 30 km/s! J shock (Jump) ;! B = 10 "G! v s > v critical! impulse heating ;! single fluid! pré-choc! post-choc!
15 1D shock models! 15! n H = 10 4 cm -3 ; v s = 30 km/s! J shock (Jump) ;! B = 10 "G! v s > v critical! impulse heating ;! single fluid! pré-choc! post-choc!
16 1D shock models! 16! n H = 10 4 cm -3 ; v s = 30 km/s! J shock (Jump) ;! B = 10 "G! v s > v critical! impulse heating ;! single fluid! C shock (Continuous) ;! B = 100 "G! pré-choc! post-choc! v s < v critical! ion-neutral friction ;! multi-fluid!
17 1D shock models! 17! n H = 10 4 cm -3 ; v s = 30 km/s! J shock (Jump) ;! B = 10 "G! v s > v critical! impulse heating ;! single fluid! C shock (Continuous) ;! B = 100 "G! pré-choc! post-choc! v s < v critical! ion-neutral friction ;! multi-fluid!
18 1D shock models! 18! n H = 10 4 cm -3! v s = 30 km/s! âge 2000 ans! CJ shock! pré-choc! post-choc!
19 Tracing the propagation of shocks: SiO emission! 19! pre-shock medium:! Si **! cores! SiO *! mantles!
20 Tracing the propagation of shocks: SiO emission! 20! pre-shock medium:! Si **! cores! SiO *! mantles! Grain charge! (Flower & Pineau des Forêts 2003)!
21 Tracing the propagation of shocks: SiO emission! 21! pre-shock medium:! Si **! cores! SiO *! mantles! Grain charge! (Flower & Pineau des Forêts 2003)! mantle sputtering (Flower & Pineau des Forêts 1994, semi-classical prescriptions) :! SiO * + (H, He, H 2 ) " SiO + (H, He, H 2 )! core erosion (May et al. 2000, Monte-Carlo simulations) :! Si ** + (He, C, N, O, H 2 O, N 2, CO, O 2 ) " Si + (He, C, N, O, H 2 O, N 2, CO, O 2 )!
22 Tracing the propagation of shocks: SiO emission! 22! pre-shock medium:! Si **! cores! SiO *! mantles! grain charge! core erosion! mantles sputtering! SiO formation in the gas phase, from grain-core silicium:! Si + O 2 " SiO + O! (Le Picard et al. 2001, CRESU experiment)! Si + OH " SiO + H! (Rivero-Santamaria, Dayou et al. 2014, quantum calculations)!
23 Tracing the propagation of shocks: SiO emission! 23! pre-shock medium:! Si **! cores! SiO *! mantles! grain charge! core erosion! mantles sputtering! gas phase formation! gas phase, chemical destruction of SiO:! SiO + OH " SiO 2 + H! (prescription E. Herbst)! adsorption (freeze-out) on to grains :! SiO + grain " SiO * + grain!
24 Tracing the propagation of shocks: SiO emission! 24! pre-shock medium:! grain charge! core erosion! mantles sputtering! gas phase formation! gas phase destruction! adsorption! Si **! cores! SiO *! mantles! level populations and transition emissivities calculations:!! statistical equilibrium equations!! Large Velocity Gradient (LVG) assumption!! collisional excitation rate coefficients of SiO by H 2, H, He! (calculated by Dayou & Balança 2006)!
25 Comparing observations with models! 25! H 2 observations! SiO observations! CO observations!
26 Comparing observations with models! 26! H 2 observations! SiO observations! CO observations! CJ model, n H = 10 4 cm -3, v s = 22 km/s, B = 150 "G ; 1% of Si! SiO * (pre-shock)!! physical conditions are constrained! (shock age, magnetic field strength)!! silicon chemistry constrained (initial distribution, processes)!! ejection rate (precise) measure: M " /an!! pure shock diagnosis! Gusdorf et al. 2015a!
27 Comparing observations with models! 27! H 2 observations! SiO observations! CO observations! CJ model, n H = 10 4 cm -3, v s = 22 km/s, B = 150 "G ; 1% of Si! SiO * (pre-shock)!! physical conditions are constrained! (shock age, magnetic field strength)!! silicon chemistry constrained (initial distribution, processes)!! ejection rate (precise) measure: M " /an!! pure shock diagnosis! Gusdorf et al. 2015a!
28 BHR71: the latest news! 28! H 2 observations! CO observations! SiO observations! New PACS & HIFI observations of CO, OH and OI lines! CJ model, n H = 10 4 cm -3, v s = 22 km/s, B = 150 "G ; 1% of Si! SiO * (pre-shock)!
29 BHR71: the latest news! 29! H 2 observations! CO observations! SiO observations! New PACS & HIFI observations of CO, OH and OI lines! CJ model, n H = 10 4 cm -3, v s = 22 km/s, B = 150 "G ; 1% of Si! SiO * (pre-shock)! OI observations! OI: models ~1% of observations! # we are missing something! # irradiated shocks! # some kind of jet component?! Benedettini et al., in prep.!
30 BHR71: the latest news! 30! Gusdorf et al., in prep.!
31 BHR71: the latest news! 31! Gusdorf et al., in prep.!
32 BHR71: the latest news! 32! Gusdorf et al., in prep.!
33 BHR71: the latest news! 33! Gusdorf et al., in prep.!
34 34! To higher-mass star formation! 25/11/15! 34! SOFIA community tele-talk series!
35 Intermediate-mass star formation: Cepheus E! 35! 0.07 pc! The Cep E outflow at 4.5 "m by Spitzer/IRAC!
36 Intermediate-mass star formation: Cepheus E! 36! 0.07 pc! IRAM-30m! CO (2-1)! SOFIA! CO (12-11)! SOFIA! CO (13-12)! The Cep E outflow at 4.5 "m by Spitzer/IRAC! Gomez-Ruiz et al. 2012!
37 Intermediate-mass star formation: Cepheus E! 37! 0.07 pc! The Cep E outflow at 4.5 "m by Spitzer/IRAC! Lefloch et al. 2015!
38 Intermediate-mass star formation: Cepheus E! 38! The Cep E outflow in CO (2-1) by the PdBI! Lefloch et al. 2015!
39 Intermediate-mass star formation: Cepheus E! 39! Jet, cavity, HH 377:! LVG analysis of CO emission! => (N, T kin ) estimates! Southern lobe:!! jet mass: 0.02 M ", 1.7 M " km/s!! outflow cavity mass: 0.32 M ",! 2.8 M " km/s! => molecular jet driven bowshock! (Non-irradiated) shock models of! the jet hot component! => perspectives: chemistry (SO, SiO,! HCO +, IRAM-30m and PdBI,! Lefloch et al. in prep, I, II, later H 2 O)!
40 Massive star formation: G ! 40! 0.03 pc! Hunter et al. 2008! Su et al. 2012! The Harvey & Forveille 1988 outflow :!! one massive O-type (imaged) star (Feld s star);!! one UC HII region surrounded by a PDR-like cocoon, 5 continuum sources;!! one Br# outflow, 3 molecular outflows (seen in H 2, CO, SiO and HCO + );!! a collection of OH, H 2 O, CH 3 OH, and NH 3 maser spots!
41 Massive star formation: G ! 41! APEX and Herschel (HIFI and PACS) observations of 12 CO and 13 CO! Analysis of CO emission:!! warm component (275 K, 10 7 cm -3 ) or (1200 K, 10 5 cm -3 ); N~ cm -2!! colder component thanks to APEX observations of 13 CO (3-2), (6-5):! (75 K, cm -2 )! Gusdorf et al., accepted by A&A!
42 Massive star formation: G ! 42! CI 3 P 1 3 P 0! CI 3 P 2 3 P 1! CI optically thin and in LTE conditions! T ex ~ 70 +/- 20 K,! N blue ~ N red ~ cm -2! => associated to CO cold component! Also observed: SiO, CH +!
43 Massive star formation: G ! 43! CI 3 P 1 3 P 0! CI 3 P 2 3 P 1! C + 2 P 3/2 2 P 1/2! CO (16 15)! CI optically thin and in LTE conditions! CII LTE assumption! T ex ~ 70 +/- 20 K,! N blue ~ N red ~ cm -2! => associated to CO cold component! Also observed: SiO, CH +! similarity of profile with CO (16-15)! => associated to CO warm component! T ex ~ 250 K,! N blue ~ cm -2 > N (CO)! Gusdorf et al., accepted by A&A!
44 Massive star formation: G ! 44! H 2 O, Herschel! Leurini et al., in press!
45 Massive star formation: G ! 45! OH, SOFIA/GREAT! H 2 O, Herschel! OI 3 P 1 3 P 2! at 63 "m! SOFIA/GREAT! Leurini et al., in press!
46 Massive star formation: G ! 46! OH, SOFIA/GREAT! H 2 O, Herschel! OI 3 P 1 3 P 2! at 63 "m! SOFIA/GREAT! Leurini et al., in press!
47 Massive star formation: Cep A! 47! Gusdorf et al. 2015b!
48 Filaments and ridges! 48!
49 Filaments and ridges! 49! Schneider et al. 2010!
50 Filaments and ridges! 50! Schneider et al. 2010! Hennemann et al. 2012!
51 The W43-MM1 ridge! 51! The W43MM1 filament in SiO (2-1), Louvet et al. 2014! Nguyen-Luong et al. 2013, Motte et al. 2014! DEC. (J2000) 1 pc! R.A. (J2000)
52 The W43-MM1 ridge! 52! The W43MM1 filament in SiO (2-1), Louvet et al. 2014! Nguyen-Luong et al. 2013, Motte et al. 2014! DEC. (J2000) local bipolar outflows! 1 pc! 1 pc! pc! 8 R.A. (J2000) Louvet et al., in prep.!
53 The W43-MM1 ridge! 53! The W43MM1 filament in SiO (2-1), Louvet et al. 2014! Nguyen-Luong et al. 2013, Motte et al. 2014! 1 pc! DEC. (J2000) R.A. (J2000)
54 The W43-MM1 ridge! 54! Models are ready (Louvet et al., in prep.):!! two scenarios: 10% pre-shock Si in the gas phase (Sig) or in the mantle (Sim)!! two values of interstellar radiation field tested: G 0 = 0, 1!
55 The W43-MM1 ridge! 55! APEX! SOFIA! Gusdorf et al., in prep.!
56 The W43-MM1 ridge! 56! APEX! SOFIA! ALMA Cycle 2, 2500 AU, 0.4, preliminary!! PI$: F. Motte! Gusdorf et al., in prep.!
57 The extra-galactic perspective! 57! CO ladders observations from external galaxies! Large scale effects from PDR, XDR, and shock contributions! NGC 253 Hailey-Dunsheath et al ; M82 Panuzzo et al ; NGC 891 Nikola et al ; NGC 6240 Meijerink et al. 2013! Herschel/PACS observations of NGC1068, Hailey-Dunsheath et al. 2012! Schinnerer et al. 2000, CO (1-0)!
58 The extra-galactic perspective! 58!
59 The extra-galactic perspective! 59! Kamenetzky et al. 2014!
60 60! Supernova remnants! 25/11/15! 60! SOFIA community tele-talk series!
61 W28! 61! 5 pc! W28! Emission at 327 MHz, by Claussen et al. 1997!
62 W28! 62! 5 pc! CO (6-5) & (3-2)! W28F! Gusdorf et al. 2012! Emission at 327 MHz, by Claussen et al. 1997!
63 W28! 63! 5 pc! CO (6-5) & (3-2)! W28F! Gusdorf et al. 2012! (3-2)! (4-3)! (6-5)! (7-6)! (11-10)!
64 W28! 64! W28! 5 pc CO (6-5) & (3-2)! W28F! 327 MHz emission, Claussen et al. 1997! Gusdorf et al. 2012! CO H 2
65 W28! 65! W28! 5 pc CO (6-5) & (3-2)! W28F! 327 MHz emission, Claussen et al. 1997! Gusdorf et al. 2012! CO H 2
66 W28! 66! 2 C-shocks, n H = 10 4 cm -3, v s = km/s, B = "G constrain:!! the momentum injected by the shock :!! M " km s -1 per position!! the energy injected by the shock:! erg per position!
67 IC 443! 67! IC443! (Gusdorf et al., in prep.)! CO (6-5)! CO (2-1)! 5 ~2.2 pc!
68 IC 443! 68! IC443 : CO (6-5) + H S(5)! IC443G! Gusdorf et al. 2014! (proceedings IAU 296)!
69 IC 443! 69! IC443 : CO (6-5) + H S(5) + YSOs! IC443G! Gusdorf et al. 2014! (proceedings IAU 296)!
70 IC 443! 70! IC443 : CO (6-5) + H S(5) + YSOs + molecular cloud CO (1-0)! Towards the SNR s progenitor IC443G! Gusdorf et al. 2014! (proceedings IAU 296)!
71 IC 443! 71! IC443G! IC443G! Riquelme et al., in prep. :!! Spectral survey IC443G!! compared to hot core G !! X-, #- rays,! and cosmic rays! G !
72 IC 443! 72! IC443G! IC443G! Riquelme et al., in prep. :!! Spectral survey IC443G!! compared to hot core G !! X-, #- rays,! and cosmic rays! G !
73 IC 443! 73! protons MIS :!! % 0 decomposition!! #! leptons MIS :!! Bremsstrahlung!!! #!! Inverse Compton! #!! Synchrotron!!! #!
74 IC 443! 74! protons MIS :!! % 0 decomposition!! #! leptons MIS :!! Bremsstrahlung!!! #!! Inverse Compton! #!! Synchrotron!!! #! Contribution to RCs studies! through ISM studies:! W28F, 3C391! (Gusdorf et al. 2012, Neufeld et al. 2014)! W44E&F (Anderl, Gusdorf & Güsten 2014)! G (Rho et al., in press)! Meyer et al, 2015# H S(5) CO (6-5)
75 IC 443! 75! protons MIS :!! % 0 decomposition!! #! leptons MIS :!! Bremsstrahlung!!! #!! Inverse Compton! #!! Synchrotron!!! #! Contribution to RCs studies! through ISM studies:! W28F, 3C391! (Gusdorf et al. 2012, Neufeld et al. 2014)! W44E&F (Anderl, Gusdorf & Güsten 2014)! G (Rho et al., in press)! Meyer et al, 2015# HESS! H S(5) CO (6-5)
76 IC 443! 76!.
77 IC 443! 77! HESS! IC443! (Gusdorf et al., in prep.)! CTA! CO (6-5)! CO (2-1)! 5 ~2.2 pc! CTA!
78 IC 443! 78! HESS! CTA! ALMA! CO (6-5)! CO (2-1)! 5 ~2.2 pc! CTA!
79 79! Perspectives! 25/11/15! 79! SOFIA community tele-talk series!
80 Perspectives! 80! Importance of studying various environments! All objectives are intricated! Extend shock studies:!! whole objects!! 2-, 3-D geometry (line profiles fitting)!! processes (UV field influence, X-rays, #-rays, cosmic rays)!! chemistry (SiO, H 2 O, tracers, COMs: spectral surveys)!! methods ( big data )! Extend the context!! link with extra-galactic!! link with CRs! 25/11/15! 80! SOFIA community tele-talk series!
81 81! Thanks for your attention!! 25/11/15! 81! SOFIA community tele-talk series!
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