1. Nagayoshi Ohashi, ASIAA Kyoto Univ. 09.11.2009 Observations of Circumstellar Disks around YSOs

2. Outline of Talk Brief introduction of the SMA Project Star formation and disk formation/evolution Overview Disks around PMSs; HD 142527 Disks around protostars; B335 Brief introduction of the SMA Project Star formation and disk formation/evolution Overview Disks around PMSs; HD 142527 Disks around protostars; B335 LAB, France 07.01.20092

3. SMA Project Joint project of the SAO and ASIAA. ASIAA joined the project in 1996. SMA consists of eight 6-m telescopes operating at submm wavelengths (1mm to 350 m) at the top of Mauna Kea. ASIAA has delivered two telescopes with receiver systems. Currently 230, 345, and 690 GHz bands are under regular operation. The SMA was dedicated in November 2003. The SMA is the fore-runner to ALMA. Joint project of the SAO and ASIAA. ASIAA joined the project in 1996. SMA consists of eight 6-m telescopes operating at submm wavelengths (1mm to 350 m) at the top of Mauna Kea. ASIAA has delivered two telescopes with receiver systems. Currently 230, 345, and 690 GHz bands are under regular operation. The SMA was dedicated in November 2003. The SMA is the fore-runner to ALMA. Kyoto Univ. 09.11.20093

4. Science using SMA Star formation Star formation Jet/outflow Jet/outflow Circumstellar disks Circumstellar disks Magnetic field Magnetic field Extragalactic Extragalactic Nearby galaxies/AGN Nearby galaxies/AGN High-z galaxies High-z galaxies Evolved stars Evolved stars Astrochemistry Astrochemistry Solar system Solar system Star formation Star formation Jet/outflow Jet/outflow Circumstellar disks Circumstellar disks Magnetic field Magnetic field Extragalactic Extragalactic Nearby galaxies/AGN Nearby galaxies/AGN High-z galaxies High-z galaxies Evolved stars Evolved stars Astrochemistry Astrochemistry Solar system Solar system LAB, France 07.01.2009 4 Syfert/AGN Outflow Magnetic field Solar system

5. Star and Planet Formation: Overview LAB, France 07.01.20095 Dense molecular cloud A low-mass star (protostar) is formed in a dense molecular cloud core through its gravitational collapse. The dense cloud becomes flatted (along the associated magnetic field). The associated magnetic field is also dragged inward. A circumstellar disk is also formed around a YSO. A molecular outflow takes place at some point. Infall is terminated and a dense core is dispersed. The central star becomes optically visible (T Tauri star). Planets are formed in the circumstellar disk? A low-mass star (protostar) is formed in a dense molecular cloud core through its gravitational collapse. The dense cloud becomes flatted (along the associated magnetic field). The associated magnetic field is also dragged inward. A circumstellar disk is also formed around a YSO. A molecular outflow takes place at some point. Infall is terminated and a dense core is dispersed. The central star becomes optically visible (T Tauri star). Planets are formed in the circumstellar disk? Takakuwa et al. 2003 Lada et al. 2003, Alves et al. 2001 Optically invisible! Girart et al. 2006

6. Research on Protostellar Disks and Protoplanetary Disks Formation of protostellar/protoplanetary disks; early phase (class 0 or even younger protostars) Evolution of PSD/PPD; intermediate phase (class I and II) Dissipation of PPD/Planet formation; late phase (class II and III) Disks around massive stars and brown dwarfs. Formation of protostellar/protoplanetary disks; early phase (class 0 or even younger protostars) Evolution of PSD/PPD; intermediate phase (class I and II) Dissipation of PPD/Planet formation; late phase (class II and III) Disks around massive stars and brown dwarfs. LAB, France 07.01.20096

7. HH211 SiO 8–7 at 0.2 (60 AU) resolution Lee et al. ApJ in press A possible velocity gradient across the innermost pair of knots ~0.5 km /s at ~10 AU A possible velocity gradient across the innermost pair of knots ~0.5 km /s at ~10 AU 7LAB, France 07.01.2009

8. 8 NGC1333/IRAS4A 345 GHz Total Intensity and Linear Polarization (B field) Dust Polarization & Magnetic Field Girart et al. 2006 Crutcher (2006), Science, 313, 771

9. Protoplanetary Disk: the site of planet formation Protoplanetary disks (PPDs) are most probable sites for planet formation. Important to understand their physical conditions. Common characteristics or more variety? More than 150 extra-solar planets have been discovered. More systems with hot Jupiters and high eccentricity. How were these extra-solar planets formed? Protoplanetary disks (PPDs) are most probable sites for planet formation. Important to understand their physical conditions. Common characteristics or more variety? More than 150 extra-solar planets have been discovered. More systems with hot Jupiters and high eccentricity. How were these extra-solar planets formed? 9LAB, France 07.01.2009

10. MM High Resolution Images of PPDs Geometry: compact, disklike structures Kinematics: Kepler motions Geometry: compact, disklike structures Kinematics: Kepler motions LAB, France 07.01.200910 1.3 mm cont 0.6 x 0.7 (~80 AU x 100 AU) GM Aur (Dutrey et al. 1998)

11. Protoplanetary disks with spiral arms Fukagawa et al. 2004 AB Aur @ 1.6 micron HD 142527 @ 1.6 micron Fukagawa et al. 2006 11LAB, France 07.01.2009

12. HD 142527 Herbig Ae star (F6 IIIe; M * ~ 2Mo) Subaru observations revealed that the disk has a spiral arm (Fukagawa et al. 2006) Subaru observations at MIR revealed a hole in the disk (Fujiwara et al. 2006). ASTE observations suggested existence of a gas disk. There was no mm interferometric observations due to its low declination. Herbig Ae star (F6 IIIe; M * ~ 2Mo) Subaru observations revealed that the disk has a spiral arm (Fukagawa et al. 2006) Subaru observations at MIR revealed a hole in the disk (Fujiwara et al. 2006). ASTE observations suggested existence of a gas disk. There was no mm interferometric observations due to its low declination. 12LAB, France 07.01.2009

13. HD142527: Subaru Infrared Images 1.6 m CIAO image (Fukagawa et al. 06) 24.5 m COMICS image (Fujiwara et al. 06) 13LAB, France 07.01.2009

14. SMA Observations of HD142527 12 CO 3-2 and 340 GHz continuum simultaneous observations One track with the compact configuration One track with the extended configuration 1.2 x 0.6 for dust continuum 2.1 x 1.1 for 12 CO 3-2 Ohashi & Momose (09, submitted) 12 CO 3-2 and 340 GHz continuum simultaneous observations One track with the compact configuration One track with the extended configuration 1.2 x 0.6 for dust continuum 2.1 x 1.1 for 12 CO 3-2 Ohashi & Momose (09, submitted) SMA is a joint project between the SAO and the ASIAA. 14LAB, France 07.01.2009

15. SMA Results: 340 GHz Continuum 340 GHz continuum distribution resembles to the 1.6 m scattered emission. An arc-like structure enclosing the central star two peaks; one at the NE and the other at the NW. Peak positions are shifted to the N as compared to those seen at 1.6 m. No clear emission on the southern side. Total flux density ~1.2 Jy 340 GHz continuum distribution resembles to the 1.6 m scattered emission. An arc-like structure enclosing the central star two peaks; one at the NE and the other at the NW. Peak positions are shifted to the N as compared to those seen at 1.6 m. No clear emission on the southern side. Total flux density ~1.2 Jy HD 142527 15LAB, France 07.01.2009

16. SMA Result 12 CO 3-2 12 CO also shows a central hole, with peak emissions coincident with the infrared features. 16LAB, France 07.01.2009

17. SMA Results: Spiral arms in gas? LAB, France 07.01.200917

18. 12 CO 3-2 Mean Velocity Clear velocity gradient from NW to SE, which is probably due to rotation. Roughly consistent with Kepler rotation around a 2Mo star. Disk axis is from NE to SW? Additional velocity gradient suggestive of non-circular motion. Any relationship with gas possibly associated with the spiral arm? Clear velocity gradient from NW to SE, which is probably due to rotation. Roughly consistent with Kepler rotation around a 2Mo star. Disk axis is from NE to SW? Additional velocity gradient suggestive of non-circular motion. Any relationship with gas possibly associated with the spiral arm? 18LAB, France 07.01.2009

19. 12 CO 3-2 Channel Maps 19LAB, France 07.01.2009

20. Submm vs Infrared LAB, France 07.01.200920

21. Is 12 CO 3-2 emission optically thin? 12 CO shows similar structures to the dust emission. Low brightness temperature (8.5 K). 12 CO shows similar structures to the dust emission. Low brightness temperature (8.5 K). LAB, France 07.01.200921 Chiang & Goldreich 97 12 CO 3-2 emission may be optically thin.

22. HD142527: Disk Mass 345 GHz total flux ~ 1.2 Jy, corresponding to 4.1E-2 M o Gas/dust mass ratio 100; T dust = 50K 12 CO 3-2 integrated flux ~ 15 Jy km/s, corresponding 6.6E-6 M o. [H 2 ]/[ 12 CO] = 10 4 ; Tex = 50 K The disk mass derived from 12 CO 3-2 is factor of 10000 smaller that that derived from 345 GHz dust. CO depletion factor ~10000? H 2 dissipation factor ~10000? Combination of CO depletion and gas dissipation? 345 GHz total flux ~ 1.2 Jy, corresponding to 4.1E-2 M o Gas/dust mass ratio 100; T dust = 50K 12 CO 3-2 integrated flux ~ 15 Jy km/s, corresponding 6.6E-6 M o. [H 2 ]/[ 12 CO] = 10 4 ; Tex = 50 K The disk mass derived from 12 CO 3-2 is factor of 10000 smaller that that derived from 345 GHz dust. CO depletion factor ~10000? H 2 dissipation factor ~10000? Combination of CO depletion and gas dissipation? 22LAB, France 07.01.2009

23. Unknown factors to estimate mass Dust temperature and CO excitation temperature Even if we assume Td=Tex=100 K, the mass difference is still more than three orders of magnitude. -index (mass opacity) Even if we assume a smaller -index, the mass derived from dust becomes just a factor of 2 smaller. CO depletion factor, f(co) Around TTSs, f(CO) has been estimated to be upto ~200. Since Td would be higher around Herbig Ae stars, f(CO) would be less than 200. Dust temperature and CO excitation temperature Even if we assume Td=Tex=100 K, the mass difference is still more than three orders of magnitude. -index (mass opacity) Even if we assume a smaller -index, the mass derived from dust becomes just a factor of 2 smaller. CO depletion factor, f(co) Around TTSs, f(CO) has been estimated to be upto ~200. Since Td would be higher around Herbig Ae stars, f(CO) would be less than 200. Even if we take into account of these unknown factors, it still seems to be difficult to explain the mass difference of 4 orders of magnitude. 23LAB, France 07.01.2009

24. Gas dispersal in disk by photoevaporation Takeuchi et al. (05; see also Alexander & Armitage 07) studied disk clearing processes. using a model taking into account combined effects of viscous evolution, photoevaporation, differential radial motion of dust grains and gas. Around an Herbig Ae/Be star with more ionizing photon, a gas-poor dust ring will be formed in 10 6 yr. Takeuchi et al. (05; see also Alexander & Armitage 07) studied disk clearing processes. using a model taking into account combined effects of viscous evolution, photoevaporation, differential radial motion of dust grains and gas. Around an Herbig Ae/Be star with more ionizing photon, a gas-poor dust ring will be formed in 10 6 yr. 24LAB, France 07.01.2009

25. Takeuchi et al. 2005 A gap is created at ~17 AU (r g ) by photoevapolation Inside the gap Both gas and dust accrete onto star due to viscosity. Outside the gap Gas is gradually evaporated from the inner edge, and the inner edge gets larger. Dust accumulates at the inner edge. A gap is created at ~17 AU (r g ) by photoevapolation Inside the gap Both gas and dust accrete onto star due to viscosity. Outside the gap Gas is gradually evaporated from the inner edge, and the inner edge gets larger. Dust accumulates at the inner edge. 25LAB, France 07.01.2009

26. Protostellar Disks around Protostars Kyoto Univ 11.09.200926

27. L1551 IRS5: Infalling Envelope Kyoto Univ 11.09.200927 C 18 O (1-0) with NMA (Momose et al. 1998) A1A1 A2A2 B1B1 B2B2 Mass ~0.08 M Radius ~ 1200 AU Freely infalling and slowly rotating Freely infalling and slowly rotating with angular momentum conserved P-V diagrams 0.1 Mo

28. L1551 IRS5: Formation of a protostellar disk Kyoto Univ 11.09.200928 SMA CS7-6 mean velocity SMA CS 7-6 Total Intensity NMA C 18 O 1-0 Takakauwa, Ohashi + 2003

29. Specific Angular Momenta around YSOs Kyoto Univ 11.09.200929 Ohashi et al. 1997 + new data (Yen, Takakuwa, Ohashi 2009) Specific angular momentum seems to be constant within a radius of ~6000 AU.

30. B335 (IRAS 19347+0727) Class 0 Protostar Lbol ~ 1.5 Lo, Tdust ~ 30 K Associated with a well developed outflow (e.g., Hirano et al. 88, 92) Infall signatures were observed (Zhou et al. 93; Choi et al. 95; Saito et al. 99). Class 0 Protostar Lbol ~ 1.5 Lo, Tdust ~ 30 K Associated with a well developed outflow (e.g., Hirano et al. 88, 92) Infall signatures were observed (Zhou et al. 93; Choi et al. 95; Saito et al. 99). Kyoto Univ 11.09.200930

31. SMA Observations of B335 12 CO, 13 CO, C 18 O 2-1 and 230 GHz continuum simultaneous observations One track with the compact configuration 3.9 x 3.3 for dust continuum 3.7 x 3.2 for C 18 O 2-1 (Yen, Takakuwa, Ohashi 09, submitted) 12 CO, 13 CO, C 18 O 2-1 and 230 GHz continuum simultaneous observations One track with the compact configuration 3.9 x 3.3 for dust continuum 3.7 x 3.2 for C 18 O 2-1 (Yen, Takakuwa, Ohashi 09, submitted) SMA is a joint project between the SAO and the ASIAA. 31LAB, France 07.01.2009

32. B335: 1.3 mm continuum Size ~ 740 AU x 350 AU Mass ~ 0.027 Mo Size ~ 740 AU x 350 AU Mass ~ 0.027 Mo Kyoto Univ 11.09.200932

33. B335: C 18 O 2-1 Size ~ 1500 AU Partially affected by the outflow. Mass ~ 5.2 x 10 -3 Mo C 18 O depletion (f d ~10) Size ~ 1500 AU Partially affected by the outflow. Mass ~ 5.2 x 10 -3 Mo C 18 O depletion (f d ~10) Kyoto Univ 11.09.200933

34. B335: C 18 O 2-1 kinematics Kyoto Univ 11.09.200934 V infall ~ 0.31-0.44 km/s @ 370 AU, Mstar ~ 0.02-0.04 Mo, Mass infall rate ~ 4.8-6.9 x 10 -6 Mo/yr

35. B335: C 18 O 2-1 Kinematics (II) Kyoto Univ 11.09.200935 No detectable velocity gradient along the N-S direction; V rot < 0.04 km/s @ 370 AU

36. Specific Angular Momentum in B335 4.6 x 10 -3 km/s pc @ 20000 AU 5.4 x 10 -4 km/s pc @ 1000 AU (Saito et al.99) 7 x 10 -5 km/s pc @ 370 AU (SMA results) 4.6 x 10 -3 km/s pc @ 20000 AU 5.4 x 10 -4 km/s pc @ 1000 AU (Saito et al.99) 7 x 10 -5 km/s pc @ 370 AU (SMA results) Kyoto Univ 11.09.200936 The specific angular momentum is not conserved outside R ~ 370 AU. If the specific angular momentum is conserved within R ~370 AU, Rd ~ 6 AU

37. With ALMA? Observations with spatially high dynamic range (10-10000 AU scale) Kepler disk formation; age estimation based on the disk size? Observations with high sensitivity and resolution Pick up the earliest phase of the disk formation. Signature of the planet formation/disk dissipation. Observations with a large sample. Observations with spatially high dynamic range (10-10000 AU scale) Kepler disk formation; age estimation based on the disk size? Observations with high sensitivity and resolution Pick up the earliest phase of the disk formation. Signature of the planet formation/disk dissipation. Observations with a large sample. Kyoto Univ 11.09.200937