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HERSCHEL HIFI FIRST RESULTS

HERSCHEL HIFI FIRST RESULTS. Cecilia Ceccarelli. OUTLINE. INTRODUCTION TO HERSCHEL & HIFI HIFI FIRST RESULTS from HEXOS HIFI FIRST RESULTS from CHESS. HERSCHEL in a nutshell. A 3.5-mt passively cooled telescope Payload cooled at the Helium superfluid temperature

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HERSCHEL HIFI FIRST RESULTS

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  1. HERSCHEL HIFI FIRST RESULTS Herschel HIFI first results Cecilia Ceccarelli

  2. OUTLINE • INTRODUCTION TO HERSCHEL & HIFI • HIFI FIRST RESULTS from HEXOS • HIFI FIRST RESULTS from CHESS Herschel HIFI first results

  3. HERSCHEL in a nutshell A 3.5-mt passively cooled telescope Payload cooled at the Helium superfluid temperature Launched last year in a L2 orbit around the Earth-Moon Will work for about 3 years -> 2012 3 instruments on board : PACS: imaging photometer or an integral field spectrometer over the spectral band from 57 to 210 m. SPIRE: spectral and photometric observations in 200 -670 m. HIFI: high resolution spectrometer between 500 and 2000 GHz (200 and 500 m). Introduction Herschel HIFI first results

  4. HERSCHEL observations Two types of “times” for observations: Guarantee Time (GT): instruments + HSO Instrument Scientists + ESA team Open Time (OT): ~70%, open to the general community Two “types” of observations: Key Programs:about 50% of HSO is allocated to large programs, i.e. programs requiring more than ~200 hrs and that are key for the astronomical community Proposals: standard “little” (in time) focused proposals OT PROPOSAL SUBMISSION: 22 JULY Introduction Herschel HIFI first results

  5. HERSCHEL HIFI Heterodyne Instrument for the Far-Infrared Introduction Herschel HIFI first results

  6. HERSCHEL HIFI Introduction Herschel HIFI first results

  7. Why Herschel HIFI Atmospheric transmission in fantastic weather conditions Frequencies larger than 500 GHz are almost completely blocked by the terrestrial atmosphere Introduction HIFI RANGE Herschel HIFI first results

  8. HIFI in a nutshell HIFI is an instrument with a continuous frequency coverage from 480 to 1250 GHz in five bands,1410-1910 GHz,in two further bands at an unrivalled spectral resolution and ultimate sensitivity. HIFI is able to perform rapid and complete spectral line surveys with resolving powers from 105 up to 107 (3 - 0.03 km/s) and deep line observations. After a false start in August, HIFI is now working at full speed ! Introduction Herschel HIFI first results

  9. HIFI in a nutshell IN-ORBIT SYSTEM TEMPERATURES Introduction De Grauuw wt al. 2010 – A&A Herschel Special Issue • For comparison: • JCMT Sys. Noise @ 465GHz is 1300K for excellent (=never seen) weather conditions • To cover 40 GHz with 30 mKrms at CSO takes ~ 36 hours. In 50 hours of HIFI time we have covered 1150 GHz! Herschel HIFI first results

  10. HIFI in a nutshell THE TWO MAJOR DRIVES FOR HIFI: COMPLETE SPECTRAL SURVEYS WATER LINES Introduction Herschel HIFI first results

  11. HIFI in a nutshell THE TWO MAJOR DRIVES FOR HIFI: COMPLETE SPECTRAL SURVEYS WATER LINES Introduction Herschel HIFI first results

  12. OUTLINE • INTRODUCTION TO HERSCHEL & HIFI • HIFI FIRST RESULTS from HEXOS • HIFI FIRST RESULTS from CHESS Herschel HIFI first results

  13. E. Bergin (Univ. of Michigan)on behalf of the HEXOS Team HEXOS First Results from the Herschel observations of EXtra-Ordinary Sources (HEXOS) Key Program

  14. Contain THE CLASSIC EXAMPLES of phenomena found throughout the ISM Hot Cores: Orion KL, Sgr B2 N Photodissociation Region: The Orion Bar Shocks: Orion KL Diffuse gas in Milky Way: Sgr B2 M peers through the galaxy Main part of program: Full HIFI spectral scans of Orion KL, Orion S, Orion Bar, Sgr B2 (M), Sgr B2(N) PACS range scans of same sources Water Maps of shock/deep integrations/search for large molecules Orion and Sgr B2:Extra-Ordinary Objects HEXOS

  15. The ORION KL spectrum HEXOS

  16. ORION KL spectrum around 900GHz HEXOS Methanol (CH3OH) Emission Methanol (CH3OH) Emission Methanol (CH3OH) Emission

  17. ORION KL spectrum around 900GHz HEXOS methanol (CH3OH) Methanol (CH3OH) Emission Methanol (CH3OH) Emission Methanol (CH3OH) Emission

  18. ORION KL spectrum around 900GHz HEXOS methanol (CH3OH) sulphur dioxide (SO2) Methanol (CH3OH) Emission Methanol (CH3OH) Emission Methanol (CH3OH) Emission

  19. ORION KL spectrum around 900GHz HEXOS sulphur dioxide (SO2) Methanol (CH3OH) Emission Methanol (CH3OH) Emission Methanol (CH3OH) Emission

  20. ORION KL : HD18O DETECTION Preliminary Estimate: HDO/H2O ~ 3 x 10-3 Previous value ~ 10-4 HEXOS TA* (K) E. Bergin Methanol (CH3OH) Emission Methanol (CH3OH) Emission Detection of HD18O Methanol (CH3OH) Emission

  21. OUTLINE • INTRODUCTION TO HERSCHEL & HIFI • HIFI FIRST RESULTS: HEXOS & WISH • CHESS HIFI FIRST RESULTS Herschel HIFI first results

  22. http://www-laog.obs.ujf-grenoble.fr/heberges/chess/index.php CHESS FIRST RESULTS Cecilia Ceccarelli A.Bacmann, A.Boogert, E.Caux, C.Comito, C.Dominik, B.Lefloch, D.Lis, F.vanderTak and the CHESS team Herschel HIFI first results

  23. ULTIMATE GOAL CHEMICAL SURVEYS during the EARLY PHASES of STAR FORMATION FOCUS A coherent study of the line spectra in the HIFI frequency range of Star Forming Regions METHOD HIFI (and PACS) unbiased spectral surveys in sources representative of SFRs and processes QUESTIONS What atomic/molecular lines are present? In emission or absorption? How many and when? IMMEDIATE GOALSGuide successive HIFI observations & provide a legacy database for the general community The CHESS KP in a nutshell Herschel HIFI first results

  24. WHY ARE FIR/submm LINE SPECTRA SO IMPORTANT? because FIR/submm lines are a very powerful diagnostic of the physical conditionsin the Star Formation Regions (SFRs); because FIR/submm lines spectra permit to reconstruct the chemical composition of the gas, which greatly affects the physical and dynamical evolution of the SFRs, and viceversa; because the chemical composition in the first phases of star formation mayaffectthe chemical composition of the objects that will eventually form the planetary system: planets, comets and asteroids. The CHESS KP in a nutshell Herschel HIFI first results

  25. From low- to high- mass protostars; From pre- to post- collapse; From the source to the surroundings. CHESS TARGETS Herschel HIFI first results

  26. L1157-B1 IRAS16293-2422 I16293E CHESS NEARBY LOW LUMINOSITY (<1000Lo) TARGETS Herschel HIFI first results L1544 OMC2-FIR4

  27. CHESS DISTANT HIGH LUMINOSITY (>1000Lo)TARGETS W51 NGC6334 AFGL2591 10 Kpc Herschel HIFI first results NOTE: ISM clouds at different galactocentric distances in the line of sight

  28. NOTE: OBTAINED DURING MARCH-APRIL, SOME ONLY TWO WEEKS OLD…. OBTAINED OBSERVATIONS Herschel HIFI first results NOTE: not fully covered frequency range

  29. CO H2O SO NH3 CH3OH OVERVIEW of 555-635GHz SPECTRA CS Luminosity CH3OCH3 Herschel HIFI first results

  30. HCl H2CO HCN OVERVIEW of 555-635GHz SPECTRA H13CO+ CH3OH Luminosity CH3OH Herschel HIFI first results

  31. 1- ONE SIZE DOES NOT FIT ALL CH3OH SO SAMPLEs OF OBSERVED SPECTRA HDCO HCN 2- AFGL2541 (HIGH MASS) SPECTRUM MORE SIMILAR TO THAT OF IRAS16293 (LOW MASS) THAN TO OMC2-FIR4 (INTERMEDIATE MASS) ONE Herschel HIFI first results

  32. A bit of statistics OVERVIEW of 555-635GHz SPECTRA Herschel HIFI first results

  33. HCl ZOOM ON HCl Tmb (K) REACHED RMS ~ 10-20 mK Frequency (GHz) IN OPTICALLY THIN LINES, THE HYPERFINE COMPONENTS INTENSITY ARE 2:3:1 Herschel HIFI first results

  34. PRELIMINARY ESTIMATES from CHESS obs ZOOM ON HCl Solar 3.1 HCl PREDICTED TO BE THE MOST ABUNDANT Cl RESERVOIR IN MOLECULAR GAS, ~70% (e.g. Neufeld &Wolfire 2009). Cl FORMED IN >10Mo STARS IN SN EXPLOSION OBSERVED DIFFERENCES DUE TO DIFFERENT “INITIAL” CONDITIONS ? Herschel HIFI first results

  35. IRAS16293-2422 solar type protostar L1157-B1 outflow shock The CHESS observed targets NGC6334I high mass protostar OMC2-FIR4 intermediate mass protostar Herschel HIFI first results

  36. L1157-B1 outflow shock The CHESS observed targets Herschel HIFI first results

  37. The CHESS PV observationsof L1157-B1 L1157-B1 outflow shock PdB observations Palteau de Bure observations HIFI PV data, Aug 2009 Spectrum between 561 and 633GHz (HIFI band 1b) at the position B1, a spot with a molecular shock. Herschel HIFI first results

  38. An unbiasedview of HIFI Band 1b DETECTED SEVERAL LINES FROM SEVERAL SPECIES L1157-B1 outflow shock Herschel HIFI first results

  39. Origin of the Molecular Emission High-sensitivity of HIFI  emission in CO and H2O detected up to v ≈ -30 km/s Broad H2O line L1157-B1 outflow shock ThreeVelocity Components : HVC : v < - 7 km/s LVC : v > -7 km/s : MV / LV LVC LV HVC MV Herschel HIFI first results

  40. WATER ABUNDANCE in L1157-B1 L1157-B1 outflow shock Palteau de Bure observations Herschel HIFI first results Lefloch et al.Herschel Special issue

  41. Differenttracers at differentvelocities L1157-B1 outflow shock Palteau de Bure observations Tgas>200K and a rich chemistry: CH3OH, H2CO, NH3,HCN,…. Herschel HIFI first results Codella et al.Herschel Special issue

  42. IRAS16293-2422 solar type protostar The CHESS observed targets Herschel HIFI first results

  43. 450mm SiO IRAS16293-2422 solar type protostar The low mass protostar IRAS16293-2422 Envelope temperature profile hot corino cold envelope H2CO abundance jump at T>100K ENVELOPE + BINARY SYSTEM + a little of OUTFLOW in the HIFI BEAM (~36” in band 1) 20” Herschel HIFI first results

  44. IRAS16293-2422 solar type protostar HIFI observationsof IRAS16293-2422: first results NH2 is a radical representing an important intermediate-step towards ammonia. Previously detected in SgrB2 only. Observations like this will finally allow to clarify the Nitrogen chemistry in a variety of sources! P.Hily-Blant et al. : THEABSORPTION SPECTRUM of NH2 Herschel HIFI first results

  45. IRAS16293-2422 solar type protostar HIFI observationsof IRAS16293-2422: first results First firm detection of ND ! Previously tentatively detected in Orion by ODIN. ESTIMATED ND/NH~30% Credits: CASSIS (Caux et al.) at http://cassis.cesr.fr/ Bacmann et al. : THE ABSORPTION SPECTRUM of ND Herschel HIFI first results

  46. First detection of ortho-D2O ESTIMATED ORTHO/PARA RATIO=2 IRAS16293-2422 solar type protostar HIFI observationsof IRAS16293-2422: first results Vastel et al. : THE ABSORPTION of the fondamental line of ortho-D2O Herschel HIFI first results

  47. The CHESS observed targets OMC2-FIR4 intermediate mass protostar Herschel HIFI first results

  48. FIR3 HIFI observations of OMC2-FIR4 IRAS16293-2422 solar type protostar OMC2-FIR4 intermediate mass protostar PdBI: Fuente et al. 2010 Crimier et al. 2010 FIR4 FIR5 ENVELOPE + a little of OUTFLOW in the HIFI BEAM (~36” in band 1) Herschel HIFI first results

  49. Band 1b in PSP2: rich spectrum Some examples: Methanol lines: a warm component previously undetected/unpredicted HIFI observations of OMC2-FIR4: first results IRAS16293-2422 solar type protostar OMC2-FIR4 intermediate mass protostar Water ground line: brighter than predicted HCl: first (easy!) detection in an IM protostar Herschel HIFI first results Kama et al. HIFI Special issue Crimier et al. HIFI Special issue

  50. The CHESS observed targets NGC6334I high mass protostar Herschel HIFI first results

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