Interstellar shocks:! The contribution of SOFIA/GREAT!
|
|
|
- Dwain Patrick
- 5 years ago
- Views:
Transcription
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!
Far-IR cooling in massive star-forming regions: a case study of G
Far-IR cooling in massive star-forming regions: a case study of G5.89-0.39 Silvia Leurini (MPIfR, Bonn) F. Wyrowski, R. Güsten, H. Wiesemeyer, K. Menten (MPIfR, Bonn) A. Gusdorf, M. Gerin, F. Levrier (LERMA,
arxiv: v1 [astro-ph.ga] 23 Mar 2015
![arxiv: v1 [astro-ph.ga] 23 Mar 2015](/thumbs/78/78222523.jpg "arxiv: v1 [astro-ph.ga] 23 Mar 2015")
APEX observations of non-stationary magneto-hydrodynamical shocks in W44 arxiv:1503.06586v1 [astro-ph.ga] 23 Mar 2015 Univ. Grenoble Alpes, IPAG, F-38000 Grenoble, France CNRS, IPAG, F-38000 Grenoble,
SOFIA observations of far-infrared hydroxyl emission toward classical ultracompact HII/OH maser regions
SOFIA observations of far-infrared hydroxyl emission toward classical ultracompact HII/OH maser regions T. Csengeri, K. Menten, M. A. Requena-Torres, F. Wyrowski, R. Güsten, H. Wiesemeyer, H.-W. Hübers,
arxiv: v1 [astro-ph.ga] 30 Nov 2015
![arxiv: v1 [astro-ph.ga] 30 Nov 2015](/thumbs/96/126610941.jpg "arxiv: v1 [astro-ph.ga] 30 Nov 2015")
Astronomy in Focus, Volume 15 XXIXth IAU General Assembly, August 2015 Kwok & Bergin, eds. c 2015 International Astronomical Union DOI: 00.0000/X000000000000000X Water in the interstellar media of galaxies
The Effect of FUV Radiation and Grain Surface Chemistry on Hydride Emission from Dense Shocks
The Effect of FUV Radiation and Grain Surface Chemistry on Hydride Emission from Dense Shocks with collaboration of Gary Melnick (CfA), Agata Karska (Torun), Michael Turner (SJSU) with support from NASA/ADAP
The Interstellar Medium
The Interstellar Medium Fall 2014 Lecturer: Dr. Paul van der Werf Oortgebouw 565, ext 5883 pvdwerf@strw.leidenuniv.nl Assistant: Kirstin Doney Huygenslaboratorium 528 doney@strw.leidenuniv.nl Class Schedule
arxiv: v2 [astro-ph.ga] 24 Aug 2016
![arxiv: v2 [astro-ph.ga] 24 Aug 2016](/thumbs/92/111015901.jpg "arxiv: v2 [astro-ph.ga] 24 Aug 2016")
Astronomy & Astrophysics manuscript no. 29077_PUBLISHER-ArXiv c ESO 2018 September 6, 2018 Tracing extended low-velocity shocks through SiO emission Case study of the W43-MM1 ridge F. Louvet 1, 2, F. Motte
The Excited and Exciting ISM in Galaxies: PDRs, XDRs and Shocks as Probes and Triggers
The Excited and Exciting ISM in Galaxies: PDRs, XDRs and Shocks as Probes and Triggers Marco Spaans (Groningen) Rowin Meijerink (Groningen), Paul van der Werf (Leiden), Juan Pablo Pérez Beaupuits (Bonn),
Sounding the diffuse ISM with Herschel/HIFI
PRISMAS PRobing InterStellar Molecules with Absorption line Studies Sounding the diffuse ISM with Herschel/HIFI.. W3 Maryvonne Gerin on behalf of the PRISMAS team PRISMAS PRobing InterStellar Molecules
MOLECULES IN THE CIRCUMNUCLEAR DISK OF THE GALACTIC CENTER
MOLECULES IN THE CIRCUMNUCLEAR DISK OF THE GALACTIC CENTER Implications from Chemical Modeling Nanase Harada 1, Denise Riquelme 1, Serena Viti 2, Karl Menten 1, Miguel Requena-Torres 1, Rolf Güsten 1,
Sunbathing around low-mass protostars: new insights from hydrides
Sunbathing around low-mass protostars: new insights from hydrides Agata Karska (N. Copernicus Univ., Toruń, Poland) L. Kristensen, M. Kaufman & WISH, DIGIT, WILL teams (Univ. of Copenhagen, San Jose St.
The Physics of the Interstellar Medium
The Physics of the Interstellar Medium Ulrike Heiter Contact: 471 5970 ulrike@astro.uu.se www.astro.uu.se Matter between stars Average distance between stars in solar neighbourhood: 1 pc = 3 x 1013 km,
Origin of the stellar Initial Mass Function (IMF) in the W43-MM1 ridge
Origin of the stellar Initial Mass Function (IMF) in the W43-MM1 ridge Fabien Louvet (Universidad de Chile & IPAG Grenoble) Special credits to: F. Motte, T. Nony, S. Bontemps, A. Gusdorf, P. Didelon, P.
Absorption spectroscopy with Herschel/HIFI and IRAM-PdBI : Promises for ALMA
PRISMAS PRobing InterStellar Molecules with Absorption line Studies Absorption spectroscopy with Herschel/HIFI and IRAM-PdBI : Promises for ALMA Maryvonne Gerin Why Absorption Spectroscopy? Sensitivity
The dynamics of photon-dominated regions (PDRs)
The dynamics of photon-dominated regions (PDRs) V. Ossenkopf, M. Röllig, N. Schneider, B. Mookerjea, Z. Makai, O. Ricken, P. Pilleri, Y. Okada, M. Gerin Page 1 Main question: What happens here? Impact
Frédérique Motte (AIM Paris-Saclay)
Clusters of high-mass protostars: From extreme clouds to minibursts of star formation Frédérique Motte (AIM Paris-Saclay) Special thanks to S. Bontemps, T. Csengeri, P. Didelon, M. Hennemann, T. Hill,
Interstellar Medium and Star Birth
Interstellar Medium and Star Birth Interstellar dust Lagoon nebula: dust + gas Interstellar Dust Extinction and scattering responsible for localized patches of darkness (dark clouds), as well as widespread
Cosmic Rays in the Interstellar Medium. Nick Indriolo University of Illinois at Urbana- Champaign
Cosmic Rays in the Interstellar Medium Nick Indriolo University of Illinois at Urbana- Champaign November 3, 2010 Stormy Cosmos Cosmic Ray Basics Energetic charged particles and nuclei protons, alpha particles,
The Unbearable Lightness of Chemistry
Z H IG C G N I OM H T A P U The Unbearable Lightness of Chemistry The Unbearable Lightness of Chemistry ~ 0.5 % Molecular (H 2 ) ~ 0.002 % CO ~ 0.000002 % any other molecule A total of 46 molecular species
Maria Cunningham, UNSW. CO, CS or other molecules?
Maria Cunningham, UNSW CO, CS or other molecules? Wide field Surveys at mm wavelengths: pu8ng the whole picture together Follow chemical abundances through the whole ISM. Follow energy transfer through
AGN-driven turbulence revealed by extreme [CII]158µm line cooling in radio-galaxies
![AGN-driven turbulence revealed by extreme [CII]158µm line cooling in radio-galaxies](/thumbs/81/83115490.jpg "AGN-driven turbulence revealed by extreme [CII]158µm line cooling in radio-galaxies")
AGN-driven turbulence revealed by extreme [CII]158µm line cooling in radio-galaxies Pierre Guillard CNES Fellow Intitut d Astrophysique Spatiale, Orsay, France The Universe Explored by Herschel, ESTEC,
C+ and Methylidyne CH+ Mapping with HIFI
C and H Reactives in Orion KL C+ and Methylidyne CH+ Mapping with HIFI Pat Morris, NHSC (IPAC/Caltech) J. Pearson, D. Lis, T. Phillips and the HEXOS team and HIFI Calibration team Outline Orion KL nebula
Interstellar Medium and Plasmas (IMP; pole 2)
Interstellar Medium and Plasmas (IMP; pole 2) December 1, 2017: 40 members; 4 sites (Denfert, Meudon, ENS, Jussieu) Permanent members (26): 19 staff scientists, 5 emeriti, 2 engineers Non permanent members
A shocking group! Turbulent dissipation and star formation in Stephan s Quintet
Physics of Groups, IAP, Dec 12-15 A shocking group! Turbulent dissipation and star formation in Stephan s Quintet Pierre Guillard, P. Appleton, F. Boulanger, M. Cluver, P. Lesaffre, G. Pineau des Forêts,
NEARBY GALAXIES AND ALMA
NEARBY GALAXIES AND ALMA Jean Turner, UCLA nearby galaxies close-up views of star formation & nuclear fueling on scales of GMCs and star clusters - where & how do galaxies form stars? - where does gas
Water in the diffuse interstellar medium
Water in the diffuse interstellar medium David Neufeld Johns Hopkins University Main collaborators on this subject: Paule Sonnentrucker, Mark Wolfire, Nicholas Flagey, Paul Goldsmith, Darek Lis, Maryvonne
Astrophysical Quantities
Astr 8300 Resources Web page: http://www.astro.gsu.edu/~crenshaw/astr8300.html Electronic papers: http://adsabs.harvard.edu/abstract_service.html (ApJ, AJ, MNRAS, A&A, PASP, ARAA, etc.) General astronomy-type
The O budget in lowmass protostars:
The O budget in lowmass protostars: The NGC1333-IRAS4A R1 shock observed in [O I] 63 μm with SOFIA-GREAT Lars E. Kristensen Center for Star & Planet Formation, Niels Bohr Institute, University of Copenhagen
R. D. Gehrz a E. E. Becklin b, and Göran Sandell b
Infrared Spectroscopic Studies with the Stratospheric Observatory for Infrared Astronomy (SOFIA) a E. E. Becklin b, and Göran Sandell b a University of Minnesota b Universities Space Research Association
Astrochemistry the summary
Astrochemistry the summary Astro 736 Nienke van der Marel April 27th 2017 Astrochemistry When the first interstellar molecules were discovered, chemists were very surprised. Why? Conditions in space are
Radio spectroscopy. Annoying question at a NSF Science and Technology Center Review
Radio spectroscopy A. Harris Image: part of an H-ATLAS field as seen in the Herschel-SPIRE 250/350/500 m bands H-ATLAS: Eales et al., PASP 2010 Annoying question at a NSF Science and Technology Center
SOFIA/GREAT [CII] observations in nearby clouds near the lines of
![SOFIA/GREAT [CII] observations in nearby clouds near the lines of](/thumbs/72/66797387.jpg "SOFIA/GREAT [CII] observations in nearby clouds near the lines of")
Page 1/24 SOFIA/GREAT [CII] observations in nearby clouds near the lines of sight towards B0355+508 and B0212+735 Jürgen Stutzki I. Physikalisches Institut, SFB 956 (Coordinated Research Center 956) Conditions
Probing the embedded phase of star formation with JWST spectroscopy
Probing the embedded phase of star formation with JWST spectroscopy NIRSPEC Spitzer NGC 1333 Low mass Herschel Cygnus X High mass Jorgensen et al. Gutermuth et al. 10 10 Motte, Henneman et al. E.F. van
Photodissociation Regions Radiative Transfer. Dr. Thomas G. Bisbas
Photodissociation Regions Radiative Transfer Dr. Thomas G. Bisbas tbisbas@ufl.edu Interstellar Radiation Field In the solar neighbourhood, the ISRF is dominated by six components Schematic sketch of the
Galaxy Ecosystems Adam Leroy (OSU), Eric Murphy (NRAO/IPAC) on behalf of ngvla Working Group 2
Next Generation Very Large Array Working Group 2 HI in M74: Walter+ 08 CO in M51: Schinnerer+ 13 Continuum in M82: Marvil & Owen Galaxy Ecosystems Adam Leroy (OSU), Eric Murphy (NRAO/IPAC) on behalf of
SOFIA follow-ups of high-mass clumps from the ATLASGAL galactic plane survey
SOFIA follow-ups of high-mass clumps from the ATLASGAL galactic plane survey Friedrich Wyrowski, Rolf Güsten, Karl Menten, Helmut Wiesemeyer, Timea Csengeri, Carsten König, Silvia Leurini & James Urquhart
New Observational Views on the Chemistry of Diffuse Interstellar Clouds
New Observational Views on the Chemistry of Diffuse Interstellar Clouds Helmut Wiesemeyer MPIfR Bonn SOFIA Community Tele Talk 2018 June 27 Collaborators: R. Güsten, K.M. Menten, J. Stutzki, T. Csengeri,
Galaxies of Many Colours: Star Formation Across Cosmic Time. z=0, t= /-0.037x10 9 years (Now)
Galaxies of Many Colours: Star Formation Across Cosmic Time z=0, t=13.798+/-0.037x10 9 years (Now) And if you want to study the initial conditions for star formation the colour is black Dense Gas SDC335:
Radio Continuum: Cosmic Rays & Magnetic Fields. Rainer Beck MPIfR Bonn
Radio Continuum: Cosmic Rays & Magnetic Fields Rainer Beck MPIfR Bonn Synchrotron emission Beam angle: Ψ/2=1/γ=E o /E Radio continuum tools to study GeV Cosmic ray electrons (CRE) Synchrotron spectrum:
Challenges for the Study of Hot Cores with ALMA: NGC 6334I
Challenges for the Study of Hot Cores with ALMA: NGC 6334I Crystal Brogan (NRAO/North American ALMA Science Center) Collaborators: Todd Hunter (NRAO) Remy Indebetouw (UVa/NRAO), Ken (Taco) Young (CfA),
Supernova Remnants and Cosmic. Rays
Stars: Their Life and Afterlife Supernova Remnants and Cosmic 68 th Rays Brian Humensky Series, Compton Lecture #5 November 8, 2008 th Series, Compton Lecture #5 Outline Evolution of Supernova Remnants
Probing the Chemistry of Luminous IR Galaxies
Probing the Chemistry of Luminous IR Galaxies, Susanne Aalto Onsala Space Observatory, Sweden Talk Outline Luminous IR galaxies Chemistry as a tool Observations in NGC 4418 Conclusions Luminous IR Galaxies
Detection of cyanopolyynes in the protostellar shock L1157-B1
Detection of cyanopolyynes in the protostellar shock L1157-B1 Edgar Mendoza IAG/USP, S~ao Paulo B. Lefloch, C. Ceccarelli, A. Al-Edhari, J. Lepine, C. Codella, L. Podio, S. Viti, H. M. Boechat-Roberty,
Warm Molecular Hydrogen at high redshift with JWST
Warm Molecular Hydrogen at high redshift with JWST Pierre Guillard Institut d Astrophysique de Paris Université Pierre et Marie Curie he Warm H 2 with JWST Outline and take-home messages 1. Observations
Midterm Results. The Milky Way in the Infrared. The Milk Way from Above (artist conception) 3/2/10
Lecture 13 : The Interstellar Medium and Cosmic Recycling Midterm Results A2020 Prof. Tom Megeath The Milky Way in the Infrared View from the Earth: Edge On Infrared light penetrates the clouds and shows
Lecture 18 - Photon Dominated Regions
Lecture 18 - Photon Dominated Regions 1. What is a PDR? 2. Physical and Chemical Concepts 3. Molecules in Diffuse Clouds 4. Galactic and Extragalactic PDRs References Tielens, Ch. 9 Hollenbach & Tielens,
Discovery of Terahertz Water Masers with SOFIA/GREAT
Discovery of Terahertz Water Masers with SOFIA/GREAT 1 Outline Motivation for studying water masers Physics of maser amplification Discovery of Terahertz masers with SOFIA 2 Water masers First detection
Gas 1: Molecular clouds
Gas 1: Molecular clouds > 4000 known with masses ~ 10 3 to 10 5 M T ~ 10 to 25 K (cold!); number density n > 10 9 gas particles m 3 Emission bands in IR, mm, radio regions from molecules comprising H,
SCIENTIFIC CASES FOR RECEIVERS UNDER DEVELOPMENT (OR UNDER EVALUATION)
SCIENTIFIC CASES FOR RECEIVERS UNDER DEVELOPMENT (OR UNDER EVALUATION) C.STANGHELLINI (INAF-IRA) Part I Infrastructure 1 Main characteristics and status of the Italian radio telescopes 2 Back-ends, opacity
The formation of high-mass stars: new insights from Herschel, IRAM, and ALMA imaging
The formation of high-mass stars: new insights from Herschel, IRAM, and ALMA imaging Frédérique Motte (IPAG Grenoble & AIM Paris-Saclay) Special credits to S. Bontemps, T. Csengeri, P. Didelon, A. Gusdorf,
Galactic Observations of Terahertz C+ (GOT C+): CII Detection of Hidden H2 in the ISM
Galactic Observations of Terahertz C+ (GOT C+): CII Detection of Hidden H2 in the ISM Bill Langer GOT C+ Team: P. Goldsmith, D. Li, J. Pineda, T. Velusamy, & H. Yorke Jet Propulsion Laboratory, California
Interstellar Medium. Alain Abergel. IAS, Université Paris-Sud, Orsay Cedex, France
Interstellar Medium Alain Abergel IAS, Université Paris-Sud, 91405 Orsay Cedex, France ISO Legacy Colloquium, Dec 13, 2006 Main Topics Elemental abundances in the ionised gas of HII regions Interstellar
Gamma rays from supernova remnants in clumpy environments.! Stefano Gabici APC, Paris
Gamma rays from supernova remnants in clumpy environments!! Stefano Gabici APC, Paris Overview of the talk Galactic cosmic rays Gamma rays from supernova remnants Hadronic or leptonic? The role of gas
HerCULES. Paul van der Werf. Leiden Observatory. Lorentz Centre February 28, 2012
Paul van der Werf Leiden Observatory Lorentz Centre February 28, 2012 Introducing Herschel Comprehensive (U)LIRG Emission Survey Open Time Key Program on the Herschel satellite 2 Who is? Paul van der Werf
Nearby Universe: Rapporteur
Nearby Universe: Rapporteur Margaret Meixner (STScI) SAGE: Tracing the Lifecycle of Baryonic Matter: Intermediate mass stars High mass stars credit: http://hea-www.cfa.harvard.edu/champ/education/public/icons/
S-PASS and Giant Magnetised outflows from the Centre of the Milky Way
S-PASS and Giant Magnetised outflows from the Centre of the Milky Way Ettore Carretti The Universe as seen by Planck Noordwijk - 4 April 2013 CSIRO ASTRONOMY AND SPACE SCIENCE Outline S-PASS: S-band Polarization
Diffuse Interstellar Medium
Diffuse Interstellar Medium Basics, velocity widths H I 21-cm radiation (emission) Interstellar absorption lines Radiative transfer Resolved Lines, column densities Unresolved lines, curve of growth Abundances,
Understanding Submillimetre Galaxies: Lessons from Low Redshifts
#SMG20 Durham 2017 Understanding Submillimetre Galaxies: Lessons from Low Redshifts Paul van der Werf Leiden: Marissa Rosenberg Rowin Meijerink Saskia van den Broek Edo Loenen Kirsty Butler Cardiff/ESO:Padelis
The Superbubble Power Problem: Overview and Recent Developments. S. Oey
The Superbubble Power Problem: Overview and Recent Developments S. Oey It has been known for decades that superbubbles generated by massive star winds and supernovae are smaller than expected based on
The FIR-Radio Correlation & Implications for GLAST Observations of Starburst Galaxies Eliot Quataert (UC Berkeley)
The FIR-Radio Correlation & Implications for GLAST Observations of Starburst Galaxies Eliot Quataert (UC Berkeley) w/ Todd Thompson & Eli Waxman Thompson, Quataert, & Waxman 2007, ApJ, 654, 219 Thompson,
Massive Star Formation in the LMC Resolved at Clump Scales
Massive Star Formation in the LMC Resolved at Clump Scales N44 NT80 N159 Rosie Chen (MPIfR) R. Indebetouw, A. Hughes, C. Henkel, R. Güsten, K. Menten, Z. Zhang, G. Li, J. Urquhart, M. Requena Torres, L.
Molecular properties of (U)LIRGs: CO, HCN, HNC and HCO +
Proceedings Astrophysical Masers and their Environments Proceedings IAU Symposium No. 242, 2007 J.M. Chapman & W.A. Baan, eds. c 2007 International Astronomical Union DOI: 000/X000000000000000X Molecular
Protostellar Jets in the ngvla Era
Protostellar Jets in the ngvla Era Luis F. Rodríguez (IRyA- UNAM, Mexico) In collabora@on with G. Anglada, C. Carrasco- González, L. Zapata, A. Palau, R. Galván- Madrid, C. Rodríguez- Kamenetzky, A. Araudo,
Astrochemical Models. Eric Herbst Departments of Chemistry and Astronomy University of Virginia
Astrochemical Models Eric Herbst Departments of Chemistry and Astronomy University of Virginia Chemical Models Gas-phase reactions 1000 s of reactions Grain-surface reactions Abundances, columns, spectra
Chapter 11 The Formation and Structure of Stars
Chapter 11 The Formation and Structure of Stars Guidepost The last chapter introduced you to the gas and dust between the stars that are raw material for new stars. Here you will begin putting together
Published in: LOW-METALLICITY STAR FORMATION: FROM THE FIRST STARS TO DWARF GALAXIES
University of Groningen Interstellar Chemistry Spaans, Marco Published in: LOW-METALLICITY STAR FORMATION: FROM THE FIRST STARS TO DWARF GALAXIES DOI: 10.1017/S1743921308024885 IMPORTANT NOTE: You are
The Interstellar Medium in Galaxies: SOFIA Science
The Interstellar Medium in Galaxies: SOFIA Science Margaret Meixner (STScI) Xander Tielens (NASA/Ames/Leiden Univ.), Jesse Dotson (NASA/ARC), Bruce Draine (Princeton), Mark Wolfire (U. Maryland), Jackie
Today in Milky Way. Clicker on deductions about Milky Way s s stars. Why spiral arms? ASTR 1040 Accel Astro: Stars & Galaxies
ASTR 1040 Accel Astro: Stars & Galaxies Prof. Juri Toomre TA: Nick Featherstone Lecture 21 Tues 3 Apr 07 zeus.colorado.edu/astr1040-toomre toomre Superbubble NGC 3079 Today in Milky Way Look at why spiral
Pulsar Wind Nebulae: A Multiwavelength Perspective
Pulsar Wind Nebulae: Collaborators: J. D. Gelfand T. Temim D. Castro S. M. LaMassa B. M. Gaensler J. P. Hughes S. Park D. J. Helfand O. C. de Jager A. Lemiere S. P. Reynolds S. Funk Y. Uchiyama A Multiwavelength
A Radio Jet Drives a Molecular & Atomic Gas Outflow in Multiple Regions within 1 kpc 2 of the Nucleus of IC5063
A Radio Jet Drives a Molecular & Atomic Gas Outflow in Multiple Regions within 1 kpc 2 of the Nucleus of IC5063 K. M. Dasyra (University of Athens) F. Combes (College de France; Observatoire de Paris)
Astrofysikaliska Dynamiska Processer
Astrofysikaliska Dynamiska Processer VT 2008 Susanne Höfner hoefner@astro.uu.se Aims of this Course - understanding the role and nature of dynamical processes in astrophysical contexts and how to study
Methyl Formate as a probe of temperature and structure of Orion-KL
Methyl Formate as a probe of temperature and structure of Orion-KL Cécile Favre Århus University - Institut for Fysik og Astronomy (IFA) N. Brouillet (LAB), D. Despois (LAB), A. Baudry (LAB), A. Wootten
The formation of super-stellar clusters
The formation of super-stellar clusters François Boulanger Institut d Astrophysique Spatiale Cynthia Herrera, Edith Falgarone, Pierre Guillard, Nicole Nesvadba, Guillaume Pineau des Forets Outline How
Possible Extra Credit Option
Possible Extra Credit Option Attend an advanced seminar on Astrophysics or Astronomy held by the Physics and Astronomy department. There are seminars held every 2:00 pm, Thursday, Room 190, Physics & Astronomy
The Ṁass- loss of Red Supergiants
The Ṁass- loss of Red Supergiants Dr. Donald F. Figer Director, Center for Detectors Speaker: Yuanhao (Harry) Zhang RIT 9/12/13 1 9/12/13 2 Outline IntroducJon MoJvaJon Objects Method Need for SOFIA/FORCAST
Magnetic field structure from Planck polarization observations of the diffuse Galactic ISM
Magnetic field structure from Planck polarization observations of the diffuse Galactic ISM François Boulanger Institut d Astrophysique Spatiale on behalf of the Planck Consortium Outline The Planck data
Understanding the chemistry of AGB circumstellar envelopes through the study of IRC
Understanding the chemistry of AGB circumstellar envelopes through the study of IRC +10216 Marcelino Agúndez LUTH, Observatoire de Paris 28 janvier 2010 1 1.65 m 2MASS PART I. INTRODUCTION: - Interest
Setting the stage for solar system formation
Setting the stage for solar system formation ALMA insights into the early years of young stars Jes Jørgensen! Niels Bohr Institute & Centre for Star and Planet Formation University of Copenhagen http://youngstars.nbi.dk
arxiv: v1 [astro-ph.co] 5 Oct 2010
![arxiv: v1 [astro-ph.co] 5 Oct 2010](/thumbs/88/115253906.jpg "arxiv: v1 [astro-ph.co] 5 Oct 2010")
Astronomy & Astrophysics manuscript no. ms c ESO 2018 October 30, 2018 Star Formation in Extreme Environments: The Effects of Cosmic Rays and Mechanical Heating. R. Meijerink 1, M. Spaans 2, A.F. Loenen
arxiv: v1 [astro-ph.ga] 15 Sep 2014
![arxiv: v1 [astro-ph.ga] 15 Sep 2014](/thumbs/91/106978363.jpg "arxiv: v1 [astro-ph.ga] 15 Sep 2014")
Astronomy& Astrophysics manuscript no. 24251_acc c ESO 2014 September 16, 2014 SiO excitation from dense shocks in the earliest stages of massive star formation S. Leurini 1, C. Codella 2, A. López-Sepulcre
EXCESS OF VHE COSMIC RAYS IN THE CENTRAL 100 PC OF THE MILKY WAY. Léa Jouvin, A. Lemière and R. Terrier
1 EXCESS OF VHE COSMIC RAYS IN THE CENTRAL 100 PC OF THE MILKY WAY Léa Jouvin, A. Lemière and R. Terrier 2 Excess of VHE cosmic rays (CRs) γ-ray count map Matter traced by CS 150 pc After subtracting the
Physical Processes in Astrophysics
Physical Processes in Astrophysics Huirong Yan Uni Potsdam & Desy Email: hyan@mail.desy.de 1 Reference Books: Plasma Physics for Astrophysics, Russell M. Kulsrud (2005) The Physics of Astrophysics, Frank
High energy radiation from molecular clouds (illuminated by a supernova remnant
High energy radiation from molecular clouds (illuminated by a supernova remnant A. Marcowith (L.P.T.A. Montpellier) collaboration with S. Gabici (D.I.A.S.) 1 Outlook Introduction: Scientific interests.
Spatially resolved physical conditions of molecular gas: a zoom-in from circumnuclear region of M83 to Carina nebula
Spatially resolved physical conditions of molecular gas: a zoom-in from circumnuclear region of M83 to Carina nebula Motivation Outline Star formation tracers in the ISM Molecular gas and star formation
The influence of cosmic rays on the chemistry in Sagittarius B2(N)
The influence of cosmic rays on the chemistry in Sagittarius B2(N) Mélisse Bonfand A. Belloche, K. M. Menten, R. Garrod Sagittarius B2 APEX Telescope Large Area Survey of the Galaxy Sgr B2 Sgr B2(N) Galactic
arxiv: v1 [astro-ph.ga] 12 Nov 2013
![arxiv: v1 [astro-ph.ga] 12 Nov 2013](/thumbs/79/80113155.jpg "arxiv: v1 [astro-ph.ga] 12 Nov 2013")
Astronomy& Astrophysics manuscript no. l1157-h2o-accepted c ESO 2018 March 18, 2018 The CHESS survey of the L1157-B1 bow-shock: high and low excitation water vapor G. Busquet 1, B. Lefloch 2,3, M. Benedettini
Stellar evolution Part I of III Star formation
Stellar evolution Part I of III Star formation The interstellar medium (ISM) The space between the stars is not completely empty, but filled with very dilute gas and dust, producing some of the most beautiful
arxiv:astro-ph/ v1 15 Mar 2007
Noname manuscript No. (will be inserted by the editor) Sulfur chemistry in the Horsehead An interferometric view of the Horsehead PDR arxiv:astro-ph/0703393v1 15 Mar 2007 J.R. Goicoechea 1 J. Pety 1,2
INITIAL CONDITIONS. Paola Caselli. School of Physics and Astronomy FACULTY OF MATHEMATICS & PHYSICAL SCIENCES. Protoplanetary disks
Paola Caselli School of Physics and Astronomy FACULTY OF MATHEMATICS & PHYSICAL SCIENCES Protoplanetary disks INITIAL CONDITIONS Boley 2009 Quiescent molecular clouds High-mass star forming regions Pre-stellar
ACTIVE GALACTIC NUCLEI: FROM THE CENTRAL BLACK HOLE TO THE GALACTIC ENVIRONMENT
Julian H. Krolik ACTIVE GALACTIC NUCLEI: FROM THE CENTRAL BLACK HOLE TO THE GALACTIC ENVIRONMENT PRINCETON UNIVERSITY PRESS Princeton, New Jersey Preface Guide for Readers xv xix 1. What Are Active Galactic
Chemical Diagnostics of Star Forming Regions
School of Physics and Astronomy FACULTY OF MATHEMATICS & PHYSICAL SCIENCES Chemical Diagnostics of Star Forming Regions Paola Caselli N 2 H + (1-0) Di Francesco et al. 2004 N 2 H + (3-2) Bourke et al.
Astrophysics of Gaseous Nebulae
Astrophysics of Gaseous Nebulae Astrophysics of Gaseous Nebulae Bright Nebulae of M33 Ken Crawford (Rancho Del Sol Observatory) Potsdam University Dr. Lidia Oskinova lida@astro.physik.uni-potsdam.de HST
First detection of a THz water maser in NGC7538-IRS1
First detection of a THz water maser in NGC7538-IRS1 Fabrice Herpin Laboratoire d Astrophysique de Bordeaux - France A. Baudry, A.M.S Richards, M.D. Gray, N. Schneider, K.M. Menten, F. Wyrowski, S. Bontemps,
Lecture 23 Internal Structure of Molecular Clouds
Lecture 23 Internal Structure of Molecular Clouds 1. Location of the Molecular Gas 2. The Atomic Hydrogen Content 3. Formation of Clouds 4. Clouds, Clumps and Cores 5. Observing Molecular Cloud Cores References
Models of FUV Illuminated Shocks:
Models of FUV Illuminated Shocks: Understanding the Water Abundances Observed With Herschel Michael Kaufman San Jose State University in support of Herschel/WISH and with collaboration of Gary Melnick
within entire molecular cloud complexes
The earliest phases of high-mass stars within entire molecular cloud complexes Frédérique Motte (CEA-Saclay, AIM) Collaborators: S. Bontemps (Obs Bordeaux), N. Schneider, J. Grac (CEA-Saclay), P. Schilke,
Astr 2310 Thurs. March 23, 2017 Today s Topics
Astr 2310 Thurs. March 23, 2017 Today s Topics Chapter 16: The Interstellar Medium and Star Formation Interstellar Dust and Dark Nebulae Interstellar Dust Dark Nebulae Interstellar Reddening Interstellar
An Introduction to Radio Astronomy
An Introduction to Radio Astronomy Bernard F. Burke Massachusetts Institute of Technology and Francis Graham-Smith Jodrell Bank, University of Manchester CAMBRIDGE UNIVERSITY PRESS Contents Preface Acknowledgements
On Today s s Radar. Reading and Events SECOND MID-TERM EXAM. ASTR 1040 Accel Astro: Stars & Galaxies. Another useful experience (we hope)
ASTR 1040 Accel Astro: Stars & Galaxies Prof. Juri Toomre TA: Nicholas Nelson Lecture 20 Thur 17 Mar 2011 zeus.colorado.edu/astr1040-toomre toomre Edge-on spiral galaxy NGG 4013 On Today s s Radar Look
Radiative Processes in Astrophysics
Radiative Processes in Astrophysics 11. Synchrotron Radiation & Compton Scattering Eline Tolstoy http://www.astro.rug.nl/~etolstoy/astroa07/ Synchrotron Self-Absorption synchrotron emission is accompanied