1. Watching the Interstellar Medium Move Alyssa A. Goodman Harvard University

2. Bart Bok and the “Dark Nebulae” “They are no good, and only a damn fool would be bothered by such a thing. A sensible person does not get involved with the dark nebulae but steers to the clear parts in between.” -- Pieter van Rhijn, Bok’s Thesis Advisor (commenting on Bok’s book, “The Distribution of Stars in Space,” in 1937)

3. Taurus Dark Cloud Complex Optical Image

4. Taurus Dark Cloud Complex 100  m ISSA image 3 pc

5. 6 5 4 3 2 1 0 A V [mag] 282726252423 Declination [deg, 1950] Arce & Goodman 1998 Star counting Taurus: Star Counting

6. Taurus: Star Counting, Color Excess of Stars

7. Taurus: All Methods of Measuring Extinction Arce & Goodman 1998 Star counting Stars with spectral classification ISSA in star pixel ISSA (cut width average) Average color excess Schlegel, Finkbeiner & Davis 1998 COBE+ISSA

8. Bart Bok in 1955 “With the increased angular resolution to be provided by paraboloid antennas now under construction, and with continued emphasis on the improvement of electronic equipment, 21 cm research promises to provide increasingly useful information on the cloud structure of the interstellar medium. By continuing our efforts to blend optical and radio studies of the interstellar medium into one whole, we have real hope of greatly advancing our knowledge of the interstellar medium in years to come.” --Bart Bok, AJ, 60, p. 148.

9. Adding a Third Dimension No loss of information Loss of 1 dimension

11. Watching the ISM Move W3: Massive Star-Forming RegionW3: Massive Star-Forming Region –velocity information explains magnetic field geometry & star formation Ursa Major: High-Latitude CloudUrsa Major: High-Latitude Cloud –velocity analysis shows “dripping” & impact Dense CoresDense Cores –velocity dimension reveals “coherence” Spectral Correlation FunctionSpectral Correlation Function –should lead to better simulations & more

12. W3 -49to-41km/sec Kannappan & Goodman 1998; Dowell 1998 o4%polarizatin 13 CO Integrated Intensity Dust Thermal Emission

13. The Origin and Evolution of High-Latitude Clouds Pound & Goodman 1997 Ursa Major HLC Complex

14. very nearby“High-latitude”= very nearby (D UMAJ ~100 pc) ~No star formation~No star formation 1 Energy distribution very differentEnergy distribution very different than star- forming regions High Latitude Cloud High Latitude Cloud 2 Gravitational << Magnetic n Kinetic Star-Forming Cloud Star-Forming Cloud 3 Gravitational n Magnetic n Kinetic (1) Magnani et al. 1996; (2) Myers, Goodman, Güsten & Heiles 1995; (3) Myers & Goodman 1988 High-latitude Clouds

15. The Velocity Field in Ursa Major Ursa MajorUrsa Major H I CO Pound & Goodman 1997

16.  v and v LSR Gradients. 35.00 36.25 37.50 38.75 142.50141.00 3 6 9 12 15 02468 vv v LSR Latitude [deg] Longitude [deg] Hat Creek H I Data

17.  v z,obs  v z, y z  Line width primarily tangential Line width primarily radial z  -y  v rad  v tan Line width primarily radial Line width primarily tangential  v tan   v rad  v tan   v rad In General......in Ursa Major implication:  

18. Confirmation: Position Velocity Diagrams for H I and CO CO H I Position Along Filament 1 Position Along Filament 2 CO Blueshifted w.r.t. H I in both filaments, in arc-like pattern

19. v z,obs Red Blue Observed in Ursa Major CO blueshifted w.r.t H I Shell y 2 1 4 3 v z,rot v z,exp v z,rot v z,exp z

21. Implications of Ursa Major Study Many HLC’s may be related to “supershell” structures; some shells harder to identify than NCP Loop. (Commonly observed) velocity offsets between atomic and molecular gas may be due to impacts, followed by conservation of momentum. Use this as a clue in other cases.

23. Bok and his Globules “In recent years several authors have drawn attention to the possibility of the formation of stars from condensations in the interstellar medium (Spitzer 1941; Whipple 1946).” --Bok & Reilly 1947, ApJ, 105, 255, opening paragraph

24. Bok and his Globules “The globules are interesting objects… Every one of them merits further careful study with the largest available reflecting telescopes.” --Bok & Reilly 1947, ApJ, 105, 255, closing paragraph

25. 1990: “Bart Bok Was Correct!”

26. Motions Of, In and Around Dense Cloud Cores Dense Cloud Cores Dense Cloud Cores Rotation  ~0.04; enough to matter but not to fragment Velocity Coherence –Cores as “Islands of Calm in a Turbulent Sea” Bulk motion –Infall: see Ho, Lada, Keto, Myers, Williams, Wilner, Zhang... –Outflow: see Arce, Lada, Raymond...

27. Coherent Cores: “Islands of Calm in a Turbulent Sea” "Rolling Waves" by KanO Tsunenobu © The Idemitsu Museum of Arts.

28. Hint #1: Independent Core Rotation Goodman, Benson, Fuller & Myers 1993

29. Hint #2: Constant Line Width in Cores?

30. Types of Line width-Size Relations. Tracer 5 Tracer 1 Tracer 2 Tracer 3 Tracer 4 Ensemble of Clouds FWHM of Various Tracers Shown Observed Size Non-thermal Line Width Type 1: “Larson’s Law” Gives overall state of ISM~magnetic virial equilibrium. See Larson 1981; Myers & Goodman 1988 for examples.  v~R 0.5

31. Types of Line width-Size Relations.. Observed Size “Type 3:” Single Cloud Observed in Multiple Tracers Non-thermal Line Width Gives pressure structure of an individual cloud. See Fuller & Myers 1992.

32. Types of Line width-Size Relations.. Observed Size “Type 3:” Single Cloud Observed in Multiple Tracers Non-thermal Line Width Density

33. Types of Line width-Size Relations.. “Type 4:” Single Cloud Observed in a Single Tracer Gives information on power spectrum of velocity fluctuations. See Barranco & Goodman 1998; Goodman, Barranco, Heyer & Wilner 1998.. Observed Size Type 4 Non-thermal Line Width

34. An Example of the (Original) Evidence for Coherence 2 3 4 5 6 7 8 9 1  v NT [km s ] 6789 0.1 23456789 1 T A [K] 3456789 0.1 23 "Radius" from Peak [parsecs] TMC-1C, NH 3 (1, 1)  v NT =(0.20±0.02)T A -0.11±0.07 2 3 4 5 6 7 8 9 1  v NT [km s ] 3456789 1 2 T A [K] 345678 0.1 2345678 1 2345 "Radius" from Peak [parsecs]  v NT =(0.64±0.05)T A -0.7±0.2 TMC-1C, OH 1667 MHz  v NT  (1.0  0.2)R 0.27  0.08  v NT  (0.30  0.09)R 0.12  0.08 Type 4 Line width-“Size” Relations

35. The (Newer) Evidence for Coherence Type 4 slope appears to decrease with density, as predicted.

36. Coherent Dense Core ~0.1 pc (in Taurus)

37. “Coherence” in Spatial Distribution of Stars Surface Density of Stellar Companions (Taurus) Parameterized Line Width-Size Relation Coherent Turbulent 8 6 4 2 log  c (  ) [stars/sq. deg] -5-4-3-20  log  [deg ] 10 -4 10 -3 10 -2 10 10 0 Size [pc] R o 0.1 2 3 4 5 6 7 8 9 1  NT [km s -1 ] Larson 1995; see also Gomez et al. 1993; Simon 1997Goodman et al. 1998.

38. The Cause of Coherence? No ambipolar diffusion yet... 3D MHD simulation of Ostriker, Gammie & Stone (in prep.) Most likely suspect: Loss of magnetic support due to reduced ionization fraction in core. (Scale gives clues.) Interesting question raised: What causes residual non-thermal line width?

39. Learning More from “Too Much” Data 2000 1990 1980 1970 1960 1950 Year 10 0 1 2 3 4 N channels, S/N in 1 hour, N pixels 10 2 3 4 5 6 7 8 (S/N)*N pixels *N channels N pixels S/N Product N channels

40. The Spectral Correlation Function Figure from Falgarone et al. 1994 Simulation

41. Goals of “SCF” Project Develop a “sharp tool” for statistical analysis of ISM, using as much data of a data cube as possible Compare information from this tool with other tools (e.g CLUMPFIND, GAUSSCLUMPS, ACF, Wavelets), applied to same cubes Use best suite of tools to compare “real” & “simulated” ISM Adjust simulations to match, understanding physical inputs

42. How the SCF Works Measures similarity of neighboring spectra within a specified “beam” size –lag & scaling adjustable –signal-to-noise equalized See: Rosolowsky, Goodman, Wilner & Williams 1998.

43. A “Real” Molecular Cloud IRAM Key Project Data

44. Initial Comparisons using the SCF Falgarone et al. 1994 L1512 (Real Cloud)“Matching?” Turbulence Simulation IRAM Key Project Data

45. Initial Comparisons using the SCF Gammie, Ostriker & Stone 1998 L1512 (Real Cloud) IRAM Key Project Data Better? MHD Simulation

46. Goals of “SCF” Project Develop a “sharp tool” for statistical analysis of ISM, using as much data of a data cube as possible Compare information from this tool with other tools (e.g CLUMPFIND, GAUSSCLUMPS, ACF, Wavelets), applied to same cubes Use best suite of tools to compare “real” & “simulated” ISM Adjust simulations to match, understanding physical inputs

47. Watching the ISM Move W3: Massive Star-Forming RegionW3: Massive Star-Forming Region –velocity information explains field geometry & star formation Ursa Major: High-Latitude CloudUrsa Major: High-Latitude Cloud –velocity analysis shows “dripping” & impact Dense CoresDense Cores –velocity dimension reveals “coherence” Spectral Correlation FunctionSpectral Correlation Function –should lead to better simulations & more

48. Next section contains "optional" slides, not used.

49. Optical View of W3 Region

50. Magnetic Fields “Go no further than A V ~1.3 mag.” 3.0 2.5 2.0 1.5 1.0 0.5 0.0 P R [%] 43210 43210 A V [mag] Background to Cold Dark Cloud Arce et al. 1998 Background to General ISM

51. “Star and Planet Formation” Giant Molecular Clouds "Cores" and Outflows Jets and Disks Solar System Formation

52. The Velocity Field in Ursa Major Ursa MajorUrsa Major Pound & Goodman 1997