Neal J. Evans II University of Texas at Austin and the c2d Team

1. From Molecular Cores to Planet-forming Disks: Overview and Recent Results from the Spitzer Space Telescope Neal J. Evans II University of Texas at Austin and the c2d Team

2. From Cores to Disks (c2d)

3. Science Goals • Complete database for nearby (< 350 pc), Low mass star and substar 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.

4. Observations • (275 hr) IRAC and MIPS Mapping • Map ~5 large clouds (~20 sq. deg.) • ~135 smaller cores • (50 hr) IRAC and MIPS Photometry • ~190 stars • (75 hr) Spectroscopy of disk material (IRS) • about 200 targets • Ancillary/complementary data from optical to mm • Collecting a very large data base • Will be publicly available eventually

5. Early Results from Spitzer • Mostly validation data (about 1% of total) • Observed two small cores (IRAC/MIPS) • One (L1228) with a known infrared source • One (L1014) without • Observed six IRS targets • B5 IRS • HH46/47 IRS (with ERO team) • Recently received data (little analysis done) • Ophiuchus, a few cores

6. A Typical Starless Core L1014 distance ~ 200 pc, but somewhat uncertain. R-band image from DSS

7. A Surprise from Spitzer Three Color Composite: Blue = 3.6 microns Green = 8.0 microns Red = 24 microns R-band image from DSS at Lower left. We see many stars through the cloud not seen in R. The central source is NOT a background star. L1014 is not “source-less”. Larger size in red is PSF. C. Young et al. ApJS, in press

8. Source Peaks on mm Emission Both long-wave maps are 3-sigma contours. C. Young et al. ApJS, in press Left: 8 micron on 1.2 mm MAMBO dust continuum emission (Kauffmann & Bertoldi) Right: 24 micron on 850 micron SCUBA data (Visser et al. 2002)

9. Models Model of SED for d = 200 pc. Central object has very low luminosity: 0.09 Lsun. Requires BB plus disk (red line) in an envelope. M(envelope) about 2 Msun. Cannot be a stellar-mass object with significant accretion. Probably sub-stellar at this point. Alternative model: more distant (2.6 kpc) object lined up by chance with peak of a foreground core (dashed line) C. Young et al. ApJS, in press, Poster 41.15

10. Lessons from L1014 • “Starless” cores may not be • Or may have substellar objects • Very low luminosity sources may exist • Must be low mass and low accretion • Caveat: possible background source • Are there others?

11. Check the Thumbprint Another “starless” core, the thumbprint nebula. Has scattered light all around periphery. Barely detected with ISO; consistent with heating only by the ISRF. See Lehtinen et al. 1998, Astr. Ap. 333,702.

12. Another clue? Blue is DSS-red, green is 24 microns, red is 70 microns MIPS data are very preliminary, not cleaned up. IRAC not available yet.

13. HH46/47 Outflow Structure Noriega-Crespo et al. ApJS, in press

14. Shock Spectrum Noriega-Crespo et al. ApJS, in press

15. Icy Dust Grains Rich spectrum of ices: CO2, H2O, CH3OH, OCN– and others. Can study ice evolution in regions forming sun-like stars. Little processing at T>50 K, some evidence for lower temperature processing. Spitzer IRS plus Keck/NIRSPEC or VLT/ISAAC Boogert et al. ApJS, in press

16. Ices in low-mass stars

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

18. Silicates CH4 PAH? Silicates CO2 CH3OH+? H2O NH3 CH3OH+? Band positions, not ID FeO F F E/F E E/F E E E PAH/F PAH PAH PAH PAH PAH E/F E E F F F F PAH E F E Silicates Silicates F PAH PAH PAH E/F F E/F F FeO F F F Silicates Silicates C2D IRS Validation Data

19. Debris Disks around wTTS Model has 0.1 Mmoon of 30 mm size dust grains in a disk from 30–60 AU Bars are 3 s Model based on disks around A stars Not enough data yet to say anything.

20. A Surprise from the wTTs RXJ1301.0-7654 Move from DSS to 24 microns in steps. Nondescript nearby star on DSS is the strong one at 24 microns. Which is the X-ray source?

21. Very Recent Data • Preliminary reduction • Minimal analysis

22. Ophiuchus AV = 3 and AORs IRAC AORS Outline of AV = 3 1o MIPS AORs

23. L1689 at 24 microns

24. High-extinction regions are dark at 24 microns Cuts: Black is AV; Red is emission Red: 24 micron emission, Blue: extinction from 2MASS and Weingartner and Draine extinction law, binned to 40” resolution.

25. IRAC on L1689 Blue is IRAC-1 (3.6); Green is IRAC-2 (4.5); Red is IRAC-4 (8) Extremely preliminary, obtained data a few days ago.

26. Bolocam map of Ophiuchus Bolocam map (1.2 mm) of region in Spitzer survey. Covers very large area (> 10 sq. deg.) compared to any previous map. Rms noise ~ 50 mJy, with about half the data. K. Young et al. In prep

27. CG30/31 Cores Collection of cores in the Gum nebula (d ~ 200 pc).

28. MIPS-24

29. MIPS-70

30. Color Composite Blue is DSS-red Green is 24 microns Red is 70 microns Very preliminary reduction. No IRAC data available yet.

31. Lots more to come… • Maps of Chamaeleon, Serpens delivered • Working on data • About 20 small cores observed • Other clouds, many small cores • Photometry of stars • IRS targets