atoms H. * Infrared **Optical l - linear c-cyclic

Transcription

1 atoms H *,* 2 C 3 * c-c 3 H C 5 * C 5 H C 6 H AlF C 2 H l-c 3 H C 4 H l-h 2 C 4 CH 2 CHCN AlCl C 2 O C 3 N C 4 Si C 2 H 4 CH 3 C 2 H C 2 ** C 2 S C 3 O l-c 3 H 2 CH 3 CN HC 5 N CH CH 2 C 3 S c-c 3 H 2 CH 3 NC HCOCH 3 *CH + HCN C 2 H 2 * CH 2 CN CH 3 OH NH 2 CH 3 CN HCO CH 2 D +? CH 4 * CH 3 SH c-c 2 H 4 O CO HCO + HCCN HC 3 N HC 3 NH + H 2 CCHOH CO + HCS + HCNH + HC 2 NC HC 2 CHO CP HOC + HNCO HCOOH NH 2 CHO CSi H 2 O HNCS H 2 CHN C 5 N HCl H 2 S HOCO + H 2 C 2 O l-hc 4 H* KCl HNC H 2 CO H 2 NCN HD* *H 3+,H 2 D +,HD + 2 HN + 2 NH 3, ND 3 * Infrared **Optical l - linear c-cyclic

2 Big Molecules 8 atoms CH 3 C 3 N CH 3 C 4 H CH 3 C 5 N? HC 9 N C 6 H 6 *? HC 11 N HCOOCH 3 CH 3 CH 2 CN (CH 3 ) 2 CO CH 3 COOH (CH 3 ) 2 O (CH 2 OH) 2? C 7 H CH 3 CH 2 OH H 2 NCH 2 COOH Glycine?? H 2 C 6 HC 7 N CH 2 OHCHO? C 8 H l-hc 6 H*

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5 Abundance of the Elements Cosmic % a %Earth Crust H 3.3x He 4.6x10 4 8x10-7 C N O F Ne x10-9 Na Mg Al Si Fe

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8 n=109 >108 He C Radio Spectrum of H Atom

9 CECILIA PAYNE-GAPOSCHKIN: ASTRONOMER AND ASTROPHYSICIST "THE MOST BRILLIANT Ph.D. THESIS EVER WRITTEN IN ASTRONOMY"

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13 CO J=1 0 in Orion 115.3GHz

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16 Horsehead nebula in Orion. Observed by microwave emission of carbon monoxide The green and yellow regions are of greater concentrations of carbon monoxide. Cal Tech

17 Chemical Equilibrium CO + 3H 2 = CH 4 + H 2 O H 0 = kcal; G 0 = -45 kcal (20K) K=[CH 4 ][H 2 O]/[CO][H 2 ] 3 = cm 6 Observation [CO]/[H 2 ] =10-4 [H 2 O] 10-4 [CO] [CH 4 ] < 10-4 [CO] Prediction/Observation >10 500

18 [H]/[H [H]/[H 2 ] 2 ] =???? H + H = H 2 grain 2 grain surface H hn hn = 2 H n=2 v ^ 14.7ev ` v

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20 Primary Ionization H 2 + crp( 100Mev)= H 2 + He + crp( 100Mev)= He + Secondary Reactions H H 2 = H H fast (10 min [H 2 ]= 10 6 cm -1 He + + H 2 HeH + + H very slow at low T He + H + + H H CO = HCO + + H 2 He + + CO = C + + O + He [He] 10 3 [CO]

21 University of Bologna O/ O =

22 Bruce Mahan Accounts Chem. Research 1975 He + +H+H v=0 (H 2 -He) + He +H+H +

23 atoms H *,* 2 C 3 * c-c 3 H C 5 * C 5 H C 6 H AlF C 2 H l-c 3 H C 4 H l-h 2 C 4 CH 2 CHCN AlCl C 2 O C 3 N C 4 Si C 2 H 4 CH 3 C 2 H C 2 ** C 2 S C 3 O l-c 3 H 2 CH 3 CN HC 5 N CH CH 2 C 3 S c-c 3 H 2 CH 3 NC HCOCH 3 *CH + HCN C 2 H 2 * CH 2 CN CH 3 OH NH 2 CH 3 CN HCO CH 2 D +? CH 4 * CH 3 SH c-c 2 H 4 O CO HCO + HCCN HC 3 N HC 3 NH + H 2 CCHOH CO + HCS + HCNH + HC 2 NC HC 2 CHO CP HOC + HNCO HCOOH NH 2 CHO CSi H 2 O HNCS H 2 CHN C 5 N HCl H 2 S HOCO + H 2 C 2 O l-hc 4 H* KCl HNC H 2 CO H 2 NCN HD* *H 3+,H 2 D +,HD + 2 HN + 2 NH 3, ND 3 * Infrared **Optical l - linear c-cyclic

24 Big Molecules 8 atoms atms CH 3 C 3 N CH 3 C 4 H CH 3 C 5 N? HC 9 N C 6 H 6 *(?) HC 11 N HCOOCH 3 CH 3 CH 2 CN (CH 3 ) 2 CO CH 3 COOH (CH 3 ) 2 O (CH 2 OH) 2? C 7 H CH 3 CH 2 OH H 2 NCH 2 COOH Glycine?? H 2 C 6 HC 7 N CH 2 OHCHO? C 8 H l-hc 6 H*

25 Hydrocarbon Synthesis C + + H 2 = CH hn (slow radiative association) C + H 3 + = CH + + H 2 ; CH 2+ + H CH + + H 2 = CH H CH H 2 = CH H CH H 2 = CH hn ( radiative association) [CH 5+ + e = CH 4 + H, CH 3 + H 2 ] CH 5+ + CO = CH 4 + HCO +

26 CH 4 + C + = C 2 H H 2 = C 2 H H C 2 H e = C 2 H + H C H + + e = C H+ H = C H + H 2 2 C H + C+ = C H + + H C H + + H = C H + + hn C H + + e =C H, C H linear&cyclic

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30 On Glycine in the ISM Very recently, there has been a report on the detection of glycine in Sgr B2(N-LMH), Orion KL, and W51 e1/e2: Y.-J. Kuan, S. B. Charnley, H.-C. Huang, W.-L. Tseng, and Z. Kisiel, Interstellar Glycine Astrophys. J. 593, (2003). This paper has caused quite a stir in the astronomical community, if one considers the following paper: J. M. Hollis, J. A. Pedelty, L. E. Snyder, P. R. Jewell, F. J. Lovas, P. Palmer, and S.-Y. Liu, A Sensitive Very Large Array Search for Small-Scale Glycine Emission toward OMC-1 Astrophys. J. 588, (2003). It should be noted that the number of supposedly positively identified transitions reported by Kuan et al. is fairly large. Therefore, the report may be considered quite convincing. However, it was brought to our attention that there seem to be some inconsistencies in the intensities of the lines. In particular, some of the observed lines seem to be too weak by a substantial amount that seems to be incompatible with the derived abundances and rotational temperatures. This may cast doubt on the derived abundances and possibly even on the interstellar detection. At the moment it appears as if the publication of these reported inconsistencies will not settle the dispute of the glycine detection. The paper alluded to in the previous paragraph is about to appear: L. E. Snyder, F. J. Lovas, J. M. Hollis, D. N. Friedel, P. R. Jewell, A. Remijan, V. V. Ilyushin, E. A. Alekseev, and S. F. Dyubko, A Rigorous Attempt to Verify Interstellar Glycine Astrophys. J. 619, (2005). Overall, we would recommend the detection of glycine to be taken very cautiously

31 Ap. J.472, L49 (1996) F l u x GHz

32 Interesting Ions Observed H 3+ Protonating species He + Direct Test of Model Enhances C + production HCO + Major Ion, HCNH + Source of HNC,HCN HOCO + {CO 2 }, HN 2+ {N 2 } {C 3 H 3+ } Source C 3 H 2,C 3 H H O + hot OH, H O 3 2 H D +, HD + Major 2 2 Deuterating species

33 Molecules from Other Galaxies CO HCN HNC CH CN NH 3 HCO + N 2 H + C 3 H 2 CH 3 OH C 2 H OCS H 2 CO OH H 2 O SiO SO HCCCN HNCO CH 3 CCH CH 3 CN Phil Solomon

34 93.206GHz

35 Interstellar van der Waals Molecules?? Carrying Along the Third Body HCO + The most abundant ion HCO + + H 2 = HCO + -H 2 + h k =10-18 CO + HCO + -H 2 = OC-HCO + + H 2 OC-HCO + + H = H 2 CO + + CO H 2 CO + + H 2 = H 2 COH + +H H 2 COH + + e - = H 2 CO + H A gas phase synthesis of Formaldehyde

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37 D E T E C T I O N O F T R I P L Y D E U T E R A T E D A M M O N I A I N T H E B A R N A R D 1 C L O U D D. C. L i s, E. R o u e f f, M. G e r i n, T. G. P h i l l i p s, L. H. C o u d e r t, F. F. S. v a n d e r T a k, a n d P. S c h i l k e ND 3 /NH 3 8x10-4 Observed HD/H 2 =10-5 Cosmic Abundance Ratio T h e o b s e r v e d a b u n d a n c e r a t i o s c a n b e e x p l a i n e d i n t h e f r a m e w o r k o f g a s - p h a s e c h e m i c a l m o d e l s, The Astrophysical Journal, 571:L55 L58, 2002

38 LABORATORY SUBMILLIMETER- WAVE DETECTION OF D2H : A NEW PROBE INTO MULTIPLE DEUTERATION? T. Hirao and T. Amano Received 2003 September 4; accepted 2003 September 17; published 2003 October 9 A pure rotational transition ( ) of D2H is measured (19) GHz This accurately measured transition frequency should be of great use for astronomical identification of this ion. DETECTION OF D2H IN THE DENSE INTERSTELLAR MEDIUM C. Vastel and T. G. Phillips Downs, H. Yoshida, Received 2004 February 26; accepted 2004 March 23; published 2004 April 9 The 692 GHz para ground-state line of D2H toward the prestellar core 16293E. The derived D2H abundance is comparable to that of H 2D, as determined by observations of the 372 GHz line of ortho-h2d.

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40 Abundance of the Elements Cosmic % a C N O F Ne Na Mg Al Si Fe

41 Oxygen problem H 2 O /CO = 10-4 SWAS Observation of Cold Molecular Clouds O 2 unobserved O 2 /CO <10-3 SWAS, Odin CO 2 nonpolar but observable as HOCO + Very low abundance.

42 Cosmic abundances Oxygen in solid form C 100 N 30.9 O Na 0.6 Mg 10.6 MgCO3. H2O 42 Al 0.8 Al2O3 1 Si 9.9 Si(OH)4 40 S 5.1 H2SO4. H2O 25 Fe 8.9 Fe2O3 13

43 Orion Orion Log N/[nH 2 ] Ridge Hot Core TMC1 L183 T/K H 2 cm -3 10^6 ^7 ^4 ^4 N[CO] cm -2 8x10^18 8x10^17 7x10^17 Log[CO/H 2 ] Log[SiO/H 2 ] <-11.6 <-11.4 SO SO < CS -8.4 < H 2 S < HCN (-8.0) -8.4 HNC -8.6 (-7.9) HCO < NH H 2 CO C.M.Walmsley J.Chem.Soc.Faraday Trans. 89,2113 (1993)

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47 HCO + + H 2 = H 2 -- HCO + 3.9kCal/m 1370cm -1 Infrared Spectrum B 0 = (±11)MHz o-h 2 B 0 = (±16)MHz p-h 2 Bieske, Nizkorodov, Bennett,Maier J.Chem Phys. 102, 5152 (1995) HCO + + CO = OC- HCO + 14kcal/m 4900cm -1 O C H C O n CH 2700cm Å O C H C O E = 1100 cm -1 B e =1906 MHz

48 The UMIST Database for Astrochemistry 1999 Y.H. Le Teuff, T.J. Millar & A.J. Markwick Astronomy & Astrophysics Supplement Series, 146, 157, > 4000 Reaction Rates