1. SIRTF Legacy From Molecular Cores to Planet-forming Disks

2. Infrared Great Observatory –3 --  m wavelength range –Background Limited Performance –85 cm f/12 Beryllium Telescope, T < 5.5K –6.  m Diffraction Limit –Instrumental Capabilities Imaging/Photometry, 3-180  m Spectroscopy, 5-40  m Spectrophotometry, 50-  m –Planetary Tracking, 1 arcsec/sec –>75% of observing time for the General Scientific Community –2.5 yr Lifetime/5 yr Goal –Launched in August 2003 (Delta 7920H) –Solar Orbit Space Infrared Telescope Facility

3. The Launch August 25, 2003, Kennedy Space Center

4. First Light

5. SIRTF Instrumentation Overview Infrared Array Camera (IRAC), G.G.Fazio, SAO, PI. Wide-field (5x5 arcmin) imaging. Simultaneous viewing at 3.6, 4.5, 5.8,  m InSb and Si:As IBC arrays, 256x256 pixel format Infrared Spectrograph (IRS), J.R.Houck, Cornell, PI. R=600 echelle spectrographs, 10-20 and 20-40  m R=50 long-slit spectrographs, 5-15  m and 15-44  m Imaging/Photometry, 15  m Si:As and Si:Sb IBC arrays, 128x128 pixel format Multi-band Imaging Photometer for SIRTF (MIPS), G.Rieke, Arizona, PI. Imaging and photometry: 24, 70, 160  m; optimized for efficient large area surveys and superresolution; R~15 spectrophotometry, 50-100  m Si:As IBC and Ge:Ga arrays, 128x128 and 32x32 format Stressed Ge:Ga array, 2x20 format

6. SIRTF Legacy Science Requirements –Large, coherent scientific investigations - not realizable as series of smaller GO Programs –Programs whose data are of general and lasting importance to the broad community and also stimulate SIRTF follow-on –Data are non-proprietary, enabling timely and effective opportunities for both SIRTF follow-on and archival research Possible Scope –Legacy Programs typically have hundreds of hours of observing time –Legacy science may utilize up to 50% of the first year of SIRTF observing time

7. Extra-galactic Legacy Programs Great Observatories Origins Deep Survey (GOODS) –M. Dickinson (STScI) and 40 co-Is at 14 institutions –Deep 300 square arcmin IRAC and MIPS (24 microns) survey overlapping HST and CXO deep fields –Galaxy formation and Evolution, z = 1 to 6 The SIRTF Wide-area Infrared Extragalactic Survey (SWIRE) –C. Lonsdale (IPAC/CIT ) and 19 co-Is at 9 institutions –~100 sq. deg., high latitudes, reaching z ~ 2.5 –Evolution of dusty, star-forming galaxies, AGN The SIRTF Nearby Galaxies Survey (SINGS): Physics of the star- forming ISM and Galaxy Evolution –R. Kennicutt (Arizona) and 14 co-Is at 7 institutions –Imaging and spectroscopy of 75 nearby galaxies –Connections between ISM and star formation, templates for high z

8. Space Infrared Telescope Facility Extragalactic Science in the Legacy Program Sky Coverage Area SINGS 75 galaxies SWIRE ~100 sq. deg. GOODS ~0.1 sq. deg. GOODS SINGS SWIRE

9. Galactic Legacy Programs The SIRTF Galactic Plane Survey (GLIMPSE) –E. Churchwell (Wisconsin) and 13 co-Is at 6 institutions –240 square deg. IRAC survey of inner Galactic plane –Galaxy structure and star formation From Molecular Cores to Planet-forming Disks (c2d) –N. Evans (Texas) and 10 co-Is at 8 institutions –Imaging (IRAC and MIPS) and spectroscopy of star forming regions –Evolution of molecular cores to stars, disks, sub-stellar objects The Formation and Evolution of Planetary Systems: Placing our Solar System in Context (FEPS) –M. Meyer (Arizona) and 18 co-Is at 12 institutions –Imaging and spectroscopy of 300 young stars with disks –Evolution from accretion disks to planet formation

10. What will GLIMPSE see? MSX point srcs61321 (10 7 )Dark Clouds210 (?)Open Clusters76 (10 4 ) IRAS point srcs15501Galaxies157 (?)Planetary Nebulae65 (?) HII/SFR regions1174 (10 4 )ASCA pt srcs144Wolf-Rayet stars50 (10 3 ) ROSAT pt srcs459SNR100Globular Clusters1 (?) Radio pulsars264O/B stars76 (10 4 ?) Known Objects in the GLIMPSE Survey Region l=300 o to 320 o, |b| <1 o MSX 8 micron band (Price et al 2001), b

11. The Formation & Evolution of Planetary Systems: Placing Our Solar System in Context  Michael R. Meyer (Steward Observatory, The University of Arizona, P.I.)  D. Backman (Franklin & Marshall College, D.P.I.), S.V.W. Beckwith (STScI), J.M. Carpenter (Caltech), M. Cohen (UC-Berkeley), U. Gorti (NASA-Ames), T. Henning (MPIA), L. Hillenbrand (Caltech, D.P.I.), D. Hines (Steward), D. Hollenbach (NASA-Ames), J. Lunine (LPL), J.S. Kim (Steward), R. Malhotra (LPL), E. Mamajek (Steward), A. Moro-Martin (Steward), P. Morris (SSC), J. Najita (NOAO), D. Padgett (SSC), J. Rodmann (MPIA), M. Silverstone (Steward), D. Soderblom (STScI), J.R. Stauffer (SSC), B. Stobie (Steward), S. Strom (NOAO), D. Watson (Rochester), S. Weidenschilling (PSI), S. Wolf (Caltech), and E. Young (Steward).  A SIRTF Legacy Science Program  For more information please visit  http://feps.as.arizona.edu

12. The c2d Team Co-investigators –Neal J. Evans II (Texas) –Lori E. Allen (SAO) –Geoffrey A. Blake (Caltech) –Paul M. Harvey (Texas) –David W. Koerner (Northern Arizona) –Lee G. Mundy (Maryland) –Philip C. Myers (SAO) –Deborah L. Padgett (SSC) –Anneila I. Sargent (Caltech) –Karl Stapelfeldt (JPL) –Ewine F. van Dishoeck (Leiden) 34 Associates 20 Affiliates

13. Science Goals Complete database for nearby (< 350 pc), Low mass (solar type) star formation Follow evolution from starless cores to planet-forming disks Coordinate with FEPS team to ensure complete coverage of 0 to 1 Gyr Cover range of other variables (mass, rotation, turbulence, environment, …) to separate from evolution.

14. Evolution Evolution Usual Scheme has only one variable – time. Initial rotation, turbulence, magnetic field, etc. may change the evolution. Environment (isolated or in a cluster) will affect the evolution.

15. Observations (275 hr) Map ~5 large clouds, ~135 smaller cores with IRAC and MIPS (~20 sq. deg.) (50 hr) Photometry of ~190 stars (IRAC and MIPS) (75 hr) Spectroscopy of disk material (IRS) for about 200 targets

16. Target Large Clouds Perseus Serpens Ophiuchus Lupus Chamaeleon

17. Ophiuchus (Overall view) Extinction Map (Cambresy 1999, Astr. Ap. 345) Antares artifact

18. Ophiuchus A V = 3 and AORs Outline of A V = 3 IRACAORS MIPSAORs 1o1o1o1o

19. Isolated Cores Large sample selected based on –Extinction on sky survey –Molecular emission –Reasonably compact –Some isolated, single –Some in small groups

20. Group of Cores (Mapping) Mapping mode, step = 280” IRACMIPS

21. Questions : Clouds and Cores Spatial Structure of star formation How do molecular cores become protostars and disks? –Very early evolution (sensitive to L ~ 10 -3 L sun ). –Large sample finds rare objects First hydrostatic core Other transitional objects –Very deeply embedded protostars.

22. An Evolutionary Sequence Shu collapse M = 0.29 M sun r o = 4396 AU Accretion rate= 1.1 x 10 –6 M sun /yr Envelope gone at 270,000 yr Final star mass = 0.24 M sun Final disk mass = 0.05 M sun D = 320 pc Young & Evans, in prep.

23. Questions: Brown Dwarfs Early Evolution of Brown Dwarfs 100’s of candidates down to 5 M jup at 1 Myr Detect circum-BD envelopes down to 1 M jup Detect circum-BD disks (4.5 M jup to 70  m) –Recent detections in NIR (Muench et al.) –MIR with ISO (Comeron et al.) –High fraction with excesses at 3.8  m (Liu et al.)

24. Formation of Brown Dwarfs Young BD, L=0.003 L sun, 1 M jup Envelope 10 Myr old BD, L=0.007 L sun, 4.5 M jup Disk (Chiang et al.)

25. Scientific Questions: Disks Do all solar-mass stars have disks? –Do weak-line T Tauri stars have debris disks? –Are there variables besides time? What are the timescales for disk evolution? –How does the transition from accretion disks to debris disks depend on time and other factors?

26. Evolution of Planet Forming disks SIRTF studies will constrain disk masses –Early, through A V ~ 100 mag, can see r = 5 AU, M = M earth disks –Middle (~ 1 Myr to 1 Gyr) around sun-like stars 0.1 M moon from 30–60 AU at 150 pc MIR complementary to NIR, mm studies

27. Detect Debris Disks to 0.1 M moon Model has 0.1 M moon of 30  m size dust grains in a disk from 30–60 AU Bars are 3  Model based on disks around A stars

28. Protostellar Disks to Planetary Systems FEPS Team Cores to Disks

29. NIR (< 0.1 AU) Excess vs. Cluster Age Hillenbrand, Meyer, and Carpenter (2002); see also Haisch et al. 2001. CAI Formation? Terrestrial Planets? Chrondrules?

30. Spectral Evolution Questions How do the dust, ice, gas in disks evolve? –Amorphous to crystalline silicates? –How does the icy component evolve? –How long does gas (H 2 ) persist? What is the spectral evolution of BDs? –If they form with disks, how does the dust evolve in those disks?

31. Spectral Evolution 10 My 100 My 5 Gy Few My

32. Age, Luminosity Distributions Distributions of sources in IRS sample over age and luminosity. Ages unknown for many, esp. Class 0, I. Evans et al. PASP Aug. 2003

33. Data Products First Delivery late May 2004 Mosaics of IRAC and MIPS maps – Over very large areas (~20 sq. deg.) –Cleaned versions of mosaics Catalogs of all sources, cross references Spectral atlas of template disk spectra Ancillary Data –submillimeter maps (Bolocam) –optical spectra (NOAO)

34. Example of Bolocam Data Bolocam map of Perseus About half the data, Not fully reduced. RMS ~45 mJy 1 x 4 degrees Enoch et al. in prep.

35. Perseus Map in 12 CO from the COMPLETE team

36. Example of Bolocam Data Bolocam map of Perseus (lower half) About half the data, Not fully reduced. Rms ~45 mJy 1 x 4 degrees Enoch et al. in prep.

37. Additional Products Analytical Tools for Modeling Disks and Envelopes –K. Dullemond: Disk codes –M. Wolfire : Envelope models Enhanced data analysis tools –Contributing to IRS data reduction tool

38. Separating Sources

39. DIRT for SIRTF DIRT is being tailored to SIRTF –Wolfire (c2d and GLIMPSE) –IRAC and MIPS bandpasses –Lower luminosity models –Include heating by ISRF –Indicate wavelengths of absorption against ISRF

40. http://dustem.astro.umd.edu/wits/dirt/index.html A Sample of DIRT

41. Complementary Data Complementary: not part of original prop. Projects initiated by us, with others –JCMT SCUBA and IRAM MAMBO Map isolated cores at 850/450  m or 1300  m –ESO time SIMBA on SEST, submm mapping of far-south cores SEST molecular line mapping of far-south cores TIMMI-2 8–13  m spectra, R~200 of cTTs ISAAC 2.9–4  m spectra of embedded objects ADONIS images of wTTs WFI maps in red, H  of Cha and Lupus

42. Complementary Data (cont.) Other projects initiated by us –BIMA Key project 360 hours Projects initiated by others –CFHT optical imaging of clouds (Menard) Time allocated for mapping of Perseus snapshots of isolated cores approved –COMPLETE (Goodman et al.) Molecular line, extinction, submm cont. Key project to match Legacy survey –Others?

43. Data Analysis MIPS Raw Data (CIT/JPL) IRAC Raw Data (SAO) IRS Data and Analysis (CIT/Leiden) Mosaics, Source Extraction (UT) Band-merge, CLEAN, Model (UMD) Catalogs, Optical spectra (NAU) Submillimeter data (CIT/UT) Verification/Management (UT)

44. Legacies Molecular cloud extinction structure Spectroscopic binary candidates Shocks and outflows Brown Dwarf candidates Diffuse Emission– Dust properties Web site: http://peggysue.as.utexas.edu/SIRTF/http://peggysue.as.utexas.edu/SIRTF/ PASP paper (2003, 115, 965; preprint available on website)

45. SIRTF and You General Observer CFP: Nov. 2002 First deadline Feb. 2004 –Includes archival studies –Eventually theory Subsequent calls each year until 2007 Note also SIRTF Fellows Program –Like Hubble Fellows –See http://sirtf.caltech.edu/SSC/ –Deadline is typically Nov.

46. Thanks for the invitation…