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Peter Schilke Submillimeter Astronomy June 15, 2005 Line Surveys Peter Schilke, MPIfR.

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Presentation on theme: "Peter Schilke Submillimeter Astronomy June 15, 2005 Line Surveys Peter Schilke, MPIfR."— Presentation transcript:

1 Peter Schilke Submillimeter Astronomy June 15, 2005 Line Surveys Peter Schilke, MPIfR

2 Peter Schilke Submillimeter Astronomy June 15, 2005 Why line surveys? Unbiased and complete –Pioneers: roadmap “because it’s there” –Inventory of lines and species –Finding the unexpected New species New lines (e.g. of highly excited states) Incomplete –Molecular fingerprints

3 Peter Schilke Submillimeter Astronomy June 15, 2005 Orion at 650 GHz Schilke et al. 2001

4 Peter Schilke Submillimeter Astronomy June 15, 2005 SiH: tentative detection Schilke et al. 2001

5 Peter Schilke Submillimeter Astronomy June 15, 2005 Why more line surveys? Having dozens or hundreds of lines for each species (and isotopologues) offers very strong constraints on models of –Temperature structure –Density structure –Abundance structure Comparison of several species –Constrain chemical models –Constrain history (chemical memory of freeze-out phase, shocks etc.)

6 Peter Schilke Submillimeter Astronomy June 15, 2005 Where? Star Forming Regions –High Mass (hot cores) [Orion] –High Mass Protostellar Objects –Low Mass Protostars –Protostellar Disks ISM –Absorption lines Stars –AGB stars [IRC ] –PPN –PN Galaxies

7 Peter Schilke Submillimeter Astronomy June 15, 2005 How? Single dish (submm+FIR only) –Ground based (CSO, JCMT, ASTE, APEX) –Airplane based (SOFIA) –Space based (ISO, Herschel/HIFI) Interferometer –mm (PdB, OVRO+BIMA=CARMA, NMA) –submm (SMA, ALMA)

8 Peter Schilke Submillimeter Astronomy June 15, 2005 Historic line surveys Almost complete: –Orion-KL Fairly good: –SgrB2(M) and (N), –IRC Partial: –Various UCHIIs.

9 Peter Schilke Submillimeter Astronomy June 15, 2005 Line surveys of Orion-KL

10 Peter Schilke Submillimeter Astronomy June 15, 2005 Orion at 345, 650 and 850 GHz Schilke et al. 1997, 2001 Comito et al. 2005

11 Peter Schilke Submillimeter Astronomy June 15, 2005 NGC 6334 I Thorwirth et al. in prep

12 Peter Schilke Submillimeter Astronomy June 15, 2005 SgrB2(M+N) at 3mm BIMA + NRAO 12m Friedel et al. 2004

13 Peter Schilke Submillimeter Astronomy June 15, 2005 SgrB2(M+N) at 3mm 30 m telescope Belloche, Comito, Hieret, Menten, Schilke, in prep.

14 Peter Schilke Submillimeter Astronomy June 15, 2005 SgrB2 with ISO LPW Polehampton et al. in prep

15 Peter Schilke Submillimeter Astronomy June 15, 2005 IRC Cernicharo et al. 2000

16 Peter Schilke Submillimeter Astronomy June 15, 2005 Interferometric line surveys Orion KL: spectra Blake et al See next talk by Beuther!!!

17 Peter Schilke Submillimeter Astronomy June 15, 2005 Orion KL: spatial structure Blake et al. 1996

18 Peter Schilke Submillimeter Astronomy June 15, 2005 Interferometric line surveys Interferometric line surveys are –Very rich in information –Very cheap to get (one night of data) –A nightmare to interpret Particularly if the UV plane isn’t fully sampled  need for high fidelity imaging Since the tools aren’t there

19 Peter Schilke Submillimeter Astronomy June 15, 2005 W3(OH/H 2 O) Wyrowski et al. 1999

20 Peter Schilke Submillimeter Astronomy June 15, 2005 W3(OH/H 2 O): complex molecules Wyrowski et al. 1999

21 Peter Schilke Submillimeter Astronomy June 15, 2005 W3(H 2 O): temperature Wyrowski et al. 1999

22 Peter Schilke Submillimeter Astronomy June 15, 2005 W3(H 2 O): H 2 column density Wyrowski et al. 1999

23 Peter Schilke Submillimeter Astronomy June 15, 2005 W3(OH) abundances Wyrowski et al. 1999

24 Peter Schilke Submillimeter Astronomy June 15, 2005 Why should YOU care? With sensitive instruments and wide backends involuntary Line Surveys (at least partial ones) will become commonplace You’ll get more than you think in more source classes than you think Be prepared!

25 Peter Schilke Submillimeter Astronomy June 15, 2005 G10.47: hot core Leurini et al. in prep

26 Peter Schilke Submillimeter Astronomy June 15, 2005 IRAS : HMPO Leurini et al. in prep

27 Peter Schilke Submillimeter Astronomy June 15, 2005 IRAS 16293: hot corino Caux, Castets, Parise et al. in prep Lifetime problem: secondary molecules shouldn’t be there don’t understand gas dynamics don’t understand chemistry

28 Peter Schilke Submillimeter Astronomy June 15, 2005 Galaxies: NGC 253 Martin et al. in prep  see poster

29 Peter Schilke Submillimeter Astronomy June 15, 2005 Future line surveys/surveys in progress More source types/more sources –PPN, PN, HMPOs, Galaxies, PDRs Wide frequency ranges: –Submm telescopes –SOFIA –Herschel/HIFI Adding spatial dimension –Interferometric line surveys

30 Peter Schilke Submillimeter Astronomy June 15, 2005 Herschel/HIFI line survey

31 Peter Schilke Submillimeter Astronomy June 15, 2005 Bottlenecks I Line identification –Line databases incomplete –Lots of interstellar weed lines missing (vibrationally excited C 2 H 5 CN etc.) –Prospects for identification of complex new molecules bleak  see Poster by Müller et al.

32 Peter Schilke Submillimeter Astronomy June 15, 2005 Bottlenecks II Modeling tools –Few 1-d LTE models for multi-molecule modeling available –Nothing more sophisticated for multi-molecule fits Transfer: LVG, ALI, MC Collision rates for many molecules not available –Need to be automatized to deal with large data volumes that even today are being produced –Close interaction with theorists Star formation processes Chemical processes

33 Peter Schilke Submillimeter Astronomy June 15, 2005 Rotation diagram analysis Completely academic for large line surveys, requires fitting of hundreds of lines

34 Peter Schilke Submillimeter Astronomy June 15, 2005 LTE modeling

35 Peter Schilke Submillimeter Astronomy June 15, 2005 CRL 618 Pardo et al. in prep

36 Peter Schilke Submillimeter Astronomy June 15, 2005 Methanol LVG modeling Leurini et al. in prep

37 Peter Schilke Submillimeter Astronomy June 15, 2005 Outlook The Good: –New instruments are bringing, and will bring, lots of new data, which potentially can constrain models of star formation and early stellar evolution, and stellar evolution, and galaxy evolution, and… The Bad: –We are lacking the tools to exploit these data. The Ugly: –Funding agencies are very hesitant to pay for development of such tools


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