dynamical regulation of star formation
play

dynamical regulation of star formation Sharon E. Meidt (MPIA) A. - PowerPoint PPT Presentation

Feb 22, 2024 •651 likes •1.84k views

dynamical regulation of star formation Sharon E. Meidt (MPIA) A. Hughes, E. Schinnerer, S. Garcia-Burillo, D. Colombo, C. Dobbs, A. Leroy, C. Kramer, K. Schuster, G. Dumas, T. Thompson Saturday, July 19, 14 Global Star Formation Relation =

  1. Garcia-Burillo et al. Present-day gravitational Torques (2005, 2009); NUGA Meidt et al. (2013) outflow inflow inertial torques stellar mass distribution - + + CO M51 - - + + - R ×∇Φ ring pile-up bar end < Γ > (R) M sol pc -2 azimuthal bins inflow to Meidt et al. (2012a) center! R(arcsec) Querjeta, Meidt et al (2014) spiral corotation Meidt et al. (2014) S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  2. gas kinematics non-circular streaming motions V azimuthal motions directed along and through spiral arm (see Roberts & Stewart 1987; V radial Wong, Blitz & Bosma 2004) S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  3. gas kinematics non-circular streaming motions V azimuthal motions directed along and through spiral arm (see Roberts & Stewart 1987; V radial Wong, Blitz & Bosma 2004) S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  4. gas kinematics non-circular streaming motions V azimuthal motions directed along and through spiral arm (see Roberts & Stewart 1987; V radial Wong, Blitz & Bosma 2004) view depends on choice of tracer! S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  5. gas kinematics non-circular streaming motions 50 different distributions CO (1”) 40 == CO (6”) 30 different kinematics (Colombo, SEM et al. 2014b) 20 HI (6”) 10 in M51 0 S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  6. gas kinematics non-circular streaming motions 50 different distributions CO (1”) 40 == CO (6”) 30 different kinematics (Colombo, SEM et al. 2014b) 20 HI (6”) 10 in M51 0 • molecular gas is • clumpier (Leroy et al. 2013) • denser, confined more to mid-plane • in spiral potential well minimum (HI typically offset; e.g. Rand & Kulkarni 1990) S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  7. Molecular Gas disk of M51 single dish (~ 500 pc) Schuster et al. (2007) Saturday, July 19, 14

  8. Molecular Gas disk of M51 single dish (~ 500 pc) Schuster et al. (2007) Saturday, July 19, 14

  9. PAWS view (Pety et al. 2013; Schinnerer et al. 2013) CO(1-­‑0) ¡in ¡central ¡9kpc ¡at (PI:Schinnerer) GMC ¡resolution ¡(40pc, ¡10 5 M sun ) IRAM ¡ Colombo et al. (2014a): 30m: ¡40 ¡hr CPROPS catalog of over 1900 Molecular Clouds PdBI: ¡170 ¡hr S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  10. Molecular Gas kinematics in M51 Colombo ¡et ¡al. ¡(2014b) bar twist ~40 km s -1 non- circular streaming motions! Saturday, July 19, 14

  11. Molecular Gas kinematics in M51 Colombo ¡et ¡al. ¡(2014b) bar twist ~40 km s -1 non- circular streaming motions! Saturday, July 19, 14

  12. Molecular Gas kinematics in M51 Colombo ¡et ¡al. ¡(2014b) bar twist ~40 km s -1 non- circular streaming motions! Saturday, July 19, 14

  13. the role of spiral arms M51 HST ACS & ORGANIZATION STRUCTURE • streaming motions funnel gas through/along spiral arms star • build up high densities formation • + reduce shear (always?) S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  14. the role of spiral arms M51 HST ACS ORGANIZATION • streaming motions funnel gas through/along spiral arms star • build up high densities formation • + reduce shear (always?) STRUCTURE S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  15. the role of spiral arms M51 HST ACS ORGANIZATION • streaming motions funnel gas through/along spiral arms star • build up high densities formation • + reduce shear (always?) STRUCTURE • large-scale down to scale of Giant Molecular Clouds , the star-forming unit !! S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  16. the role of spiral arms M51 HST ACS ORGANIZATION • streaming motions funnel gas through/along spiral arms star • build up high densities formation • + reduce shear (always?) STRUCTURE • large-scale down to scale of Giant Molecular Clouds , the star-forming unit !! • massive clouds build/form in spiral arms via convergent flows, collisions & self-gravity (M51, IC 342; Hirota et al. 2011; Koda et al. 2009; Egusa, Koda & Scoville 2010) S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  17. the role of spiral arms • Colombo et al. - cloud Cumulative Mass Spectra (2014a): PAWS Columbo et al. GMC catalog of (2014a) over 1900 clouds across central 9 kpc in M51 log N cl [(m>M)/kpc 2 ] spiral arms help build more and larger clouds dispersal in inter- arm due to shear, feedback log M lum [M sun ] S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  18. the role of spiral arms • Colombo et al. - cloud Cumulative Mass Spectra (2014a): PAWS Columbo et al. GMC catalog of (2014a) over 1900 clouds across central 9 kpc in M51 log N cl [(m>M)/kpc 2 ] spiral arms help build more and larger clouds dispersal in inter- center arm due to shear, spiral feedback interarm log M lum [M sun ] S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  19. the role of spiral arms • Colombo et al. - cloud Cumulative Mass Spectra (2014a): PAWS Columbo et al. GMC catalog of (2014a) over 1900 clouds across central 9 kpc in M51 log N cl [(m>M)/kpc 2 ] spiral arms help build more and larger clouds dispersal in inter- center arm due to shear, spiral feedback interarm log M lum [M sun ] S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  20. the role of spiral arms • Colombo et al. - cloud Cumulative Mass Spectra (2014a): PAWS more Columbo et al. GMC catalog of (2014a) over 1900 clouds across central 9 kpc in M51 log N cl [(m>M)/kpc 2 ] spiral arms help build more and larger clouds dispersal in inter- center arm due to shear, spiral feedback larger interarm log M lum [M sun ] S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  21. the role of spiral arms - cloud properties, scaling relations Hughes et al. (2013b) log (velocity dispersion) log (CO Luminosity) M51 ) 7 8 S c -­‑2 ( ¡ p W M33 M M sun ¡ 4 LMC 4 exgal. ¡(B08) 4 ¡ B08 Σ H2 = ¡4 ¡M sun pc -­‑2 log (radius) log (radius) large range of gas surface densities no size-line width relation ➱ ➱ GMC properties are not universal clouds are not (always) virialized no universal free-fall time! scatter in KS relation S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14 completely unexpected:

  22. the role of spiral arms - cloud properties, scaling relations Hughes et al. (2013b) log (velocity dispersion) log (CO Luminosity) M51 ) 7 8 S c -­‑2 ( ¡ p W M33 M M sun ¡ 4 LMC 4 exgal. ¡(B08) 4 ¡ clouds in ARM are B08 Σ H2 = ¡4 ¡M sun pc -­‑2 • brighter, • more massive, log (radius) • higher gas surface density log (radius) large range of gas surface densities no size-line width relation ➱ ➱ compared to inter-ARM GMC properties are not universal clouds are not (always) virialized no universal free-fall time! scatter in KS relation S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14 completely unexpected:

  23. varying properties with dynamical environment the role of external pressure S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  24. varying properties with dynamical environment the role of external pressure • how do clouds inherit from environment? • Pint~Pext (Hughes, SEM et al. 2013a) S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  25. varying properties with dynamical environment the role of external pressure Hughes, Meidt et al. • how do clouds inherit from (2013a) environment? • Pint~Pext (Hughes, SEM et al. 2013a) S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  26. varying properties with dynamical environment the role of external pressure Hughes, Meidt et al. • how do clouds inherit from (2013a) environment? • Pint~Pext (Hughes, SEM et al. 2013a) clouds coupled to surroundings S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  27. varying properties with dynamical environment the role of external pressure Hughes, Meidt et al. • how do clouds inherit from (2013a) environment? • Pint~Pext (Hughes, SEM et al. 2013a) clouds coupled to surroundings • changes in pressure-balance (due to non-circ motions) alter cloud stability (Meidt et al. 2013) KEY: surface pressure important! S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  28. dynamical pressure Meidt et al. (2013) cf. Jog (2013a,b) S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  29. dynamical pressure Meidt et al. (2013) cf. Jog (2013a,b) ` S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  30. dynamical pressure Meidt et al. (2013) cf. Jog (2013a,b) ` • Bernoulli: gas in motion, reduced pressure within gas, on clouds S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  31. dynamical pressure Meidt et al. (2013) cf. Jog (2013a,b) ` • Bernoulli: gas in motion, reduced pressure within gas, on clouds • increased cloud stable mass (bigger before collapse) • fewer collapse-unstable clouds • lower star formation, longer τ dep S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  32. dynamical pressure Meidt et al. (2013) cf. Jog (2013a,b) ` • Bernoulli: gas in motion, reduced pressure within gas, on clouds cloud mass spectrum • increased cloud stable mass log ¡N cl ¡[(m>M)/kpc 2 ] ¡ (bigger before collapse) • fewer collapse-unstable clouds • lower star formation, longer τ dep log ¡M lum ¡[M sun ] ¡ S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  33. dynamical pressure Meidt et al. (2013) cf. Jog (2013a,b) ` • Bernoulli: gas in motion, reduced pressure within gas, on clouds cloud mass spectrum • increased cloud stable mass log ¡N cl ¡[(m>M)/kpc 2 ] ¡ unstable stable (bigger before collapse) • fewer collapse-unstable clouds • lower star formation, longer τ dep log ¡M lum ¡[M sun ] ¡ S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  34. dynamical pressure Meidt et al. (2013) cf. Jog (2013a,b) ` • Bernoulli: gas in motion, reduced pressure within gas, on clouds cloud mass spectrum • increased cloud stable mass log ¡N cl ¡[(m>M)/kpc 2 ] ¡ unstable stable (bigger before collapse) • fewer collapse-unstable clouds • lower star formation, longer τ dep log ¡M lum ¡[M sun ] ¡ S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  35. depletion time variation due to dynamics depletion time M51 0.5 τ dep = Σ H2 / Σ SFR lines of constant τ dep Ê velocity ) . s 10 8.5 Gyr log 10 S SFR H Msol pc - 2 yr - 1 L Ha + 24 micron n 0.0 e Ê d Ê Ê . Ê Ê f r 10 9 Gyr u Ê Ê - 0.5 Ê s Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê R Ê Ê Ê Ê Ê Ê F Ê Ê S Ê Ê Ê ( Ê Ê Ê Ê Ê 10 9.5 Gyr Ê Ê Ê Ê Ê Ê g Ê - 1.0 Ê Ê Ê o Ê Ê Ê Ê l Ê Ê Ê Ê - 1.5 1.9 2.0 2.1 2.2 2.3 2.4 2.5 PAWS CO log (molecular surface density) log 10 S H2 H Msol kpc - 2 L S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  36. Molecular Gas disk of M51 ¡ CO(1-0) in central 9kpc at cloud resolution (40pc, 10 5 M sun ) ? ? Saturday, July 19, 14

  37. Spatial Relation b/n Gas and Star Formation white contours: CO Saturday, July 19, 14

  38. Spatial Relation b/n Gas and Star Formation white contours: CO Saturday, July 19, 14

  39. Spatial Relation b/n Gas and Star Formation white contours: CO ln gas depletion time ‘universal’ time (Bigiel et al. 2008) Saturday, July 19, 14

  40. depletion time variation due to dynamics depletion time M51 0.5 τ dep = Σ H2 / Σ SFR lines of constant τ dep Ê velocity ) . s 10 8.5 Gyr log 10 S SFR H Msol pc - 2 yr - 1 L Ha + 24 micron n 0.0 e Ê d Ê Ê . Ê Ê f r 10 9 Gyr u Ê Ê - 0.5 Ê s Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê R Ê Ê Ê Ê Ê Ê F Ê Ê S Ê Ê Ê ( Ê Ê Ê Ê Ê 10 9.5 Gyr Ê Ê Ê Ê Ê Ê g Ê - 1.0 Ê Ê Ê o Ê Ê Ê Ê l Ê Ê Ê Ê - 1.5 1.9 2.0 2.1 2.2 2.3 2.4 2.5 PAWS CO log (molecular surface density) log 10 S H2 H Msol kpc - 2 L S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  41. depletion time variation due to dynamics depletion time M51 0.5 τ dep = Σ H2 / Σ SFR lines of constant τ dep Ê velocity ) . s 10 8.5 Gyr log 10 S SFR H Msol pc - 2 yr - 1 L Ha + 24 micron n 0.0 e Ê d Ê Ê . Ê Ê f r 10 9 Gyr star formation still occurs near spiral arms, u Ê Ê - 0.5 Ê s Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê R Ê Ê Ê Ê but not as efficiently as it ‘could’ Ê Ê F Ê Ê S Ê Ê Ê ( Ê Ê Ê Ê Ê 10 9.5 Gyr Ê Ê Ê Ê Ê Ê g Ê - 1.0 Ê Ê Ê o Ê Ê Ê Ê l Ê Ê Ê Ê - 1.5 1.9 2.0 2.1 2.2 2.3 2.4 2.5 PAWS CO log (molecular surface density) log 10 S H2 H Msol kpc - 2 L S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  42. depletion time variation due to dynamics depletion time M51 0.5 τ dep = Σ H2 / Σ SFR lines of constant τ dep Ê velocity ) . s 10 8.5 Gyr log 10 S SFR H Msol pc - 2 yr - 1 L Ha + 24 micron n 0.0 e Ê d Ê Ê . Ê Ê f r 10 9 Gyr star formation still occurs near spiral arms, u stronger spiral (stronger streaming), Ê Ê - 0.5 Ê s Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê R Ê Ê Ê Ê but not as efficiently as it ‘could’ Ê more suppression Ê F Ê Ê S Ê Ê Ê ( Ê Ê Ê Ê Ê 10 9.5 Gyr Ê Ê Ê Ê Ê Ê g Ê - 1.0 Ê Ê Ê o Ê Ê Ê Ê l Ê Ê Ê Ê - 1.5 1.9 2.0 2.1 2.2 2.3 2.4 2.5 PAWS CO log (molecular surface density) log 10 S H2 H Msol kpc - 2 L S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  43. depletion time variation due to dynamics depletion time M51 0.5 τ dep = Σ H2 / Σ SFR lines of constant τ dep Ê velocity ) . s 10 8.5 Gyr log 10 S SFR H Msol pc - 2 yr - 1 L Ha + 24 micron n 0.0 e Ê d Ê Ê . Ê Ê f r 10 9 Gyr star formation still occurs near spiral arms, u stronger spiral (stronger streaming), Ê Ê - 0.5 Ê s Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê R Ê Ê Ê Ê but not as efficiently as it ‘could’ Ê more suppression Ê F Ê Ê S Ê Ê Ê ( Ê Ê Ê Ê Ê 10 9.5 Gyr Ê Ê Ê Ê Ê Ê g Ê - 1.0 Ê Ê Ê o Ê Ê Ê Ê l Ê Ê Ê Ê - 1.5 1.9 2.0 2.1 2.2 2.3 2.4 2.5 NGC 4303 PAWS CO log (molecular surface density) log 10 S H2 H Msol kpc - 2 L S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  44. depletion time variation due to dynamics since spirals stronger in more massive disks, τ dep larger in (well-defined dispersion relation) S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  45. depletion time variation due to dynamics mass since spirals stronger in more massive disks, Leroy et al. 2013 τ dep larger in (well-defined dispersion relation) ‘starburst’ what if we also limit cloud lifetimes? weak streaming strong streaming S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  46. COLD GASS global measurements Saintonge et al. (2013) S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  47. depletion time variation due to dynamics in massive Early-type galaxies S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  48. depletion time variation due to dynamics in massive shear Early-type Davis et al. (2014) galaxies fast rising slow rising = rotation curve shape (flat) (solid-body=1) S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  49. depletion time variation due to dynamics in massive shear Early-type Davis et al. (2014) galaxies (but β =0 in fast rising slow rising = rotation curve shape disks) (flat) (solid-body=1) S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  50. Shear limits cloud lifetimes • cloud lifetime in M51 ~ shear timescale Oort A -1 (Meidt & PAWS in prep.) • also found in numerical simulations (Dobbs & Pringle 2013) t orb 1 A -1 = π (1- β ) in disks, in the centers, β =0 and t orb very long! β =0 but t orb short! • short cloud lifetimes<t ff , perhaps not long enough for star formation S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  51. Take Away • not all cold, dense (molecular) clouds form stars..... S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  52. Take Away • not all cold, dense (molecular) clouds form stars..... ➡ dynamics regulates organization, structure and stability of molecular gas S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  53. Take Away • not all cold, dense (molecular) clouds form stars..... ➡ dynamics regulates organization, structure and stability of molecular gas ➡ same large-scale processes that fuel centers also suppress star formation S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  54. S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  55. short gmc lifetimes: an observational estimate with PAWS! S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  56. short gmc lifetimes: an observational estimate with PAWS! ‘upstream’ dynamical environments zone II ‘downstream’ zone I ARM center S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  57. short gmc lifetimes: an observational estimate with PAWS! ‘upstream’ dynamical environments • mostly only destruction zone II ‘downstream’ zone I ARM • interarm easy to dynamically characterize • clouds follow circular paths (very little center radial excursion) S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  58. short gmc lifetimes: an observational estimate with PAWS! ‘upstream’ dynamical environments • mostly only destruction zone II ‘downstream’ zone I ARM • interarm easy to dynamically characterize • clouds follow circular paths (very little center radial excursion) S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  59. short gmc lifetimes: an observational estimate with PAWS! ‘upstream’ dynamical environments • mostly only destruction zone II ‘downstream’ zone I ARM • interarm easy to dynamically zone II characterize zone I • clouds follow circular paths (very little center phase radial excursion) S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  60. short gmc lifetimes: an observational estimate with PAWS! ‘upstream’ dynamical environments zone II ‘downstream’ zone I • cloud numbers decreases from zone I to ARM zone II (Colombo et al. 2013) zone II • mass spectrum evolution: shear and star zone I center formation feedback destroy clouds, phase limit lifetimes S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  61. short gmc lifetimes: an observational estimate with PAWS! ‘upstream’ dynamical environments zone II ‘downstream’ zone I • cloud numbers decreases from zone I to ARM zone II (Colombo et al. 2013) zone II • mass spectrum evolution: shear and star zone I center formation feedback destroy clouds, phase limit lifetimes S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  62. short gmc lifetimes: an observational estimate with PAWS! ‘upstream’ dynamical environments zone II ‘downstream’ zone I • cloud numbers decreases from zone I to ARM zone II (Colombo et al. 2013) zone II • mass spectrum evolution: shear and star zone I center formation feedback destroy clouds, phase limit lifetimes shear Oort A feedback = Ω -B = Ω /2 (for V flat) S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  63. short gmc lifetimes: an observational estimate with PAWS! ‘upstream’ dynamical environments zone II ‘downstream’ zone I • cloud numbers decreases from zone I to ARM zone II (Colombo et al. 2013) zone II • mass spectrum evolution: shear and star zone I center formation feedback destroy clouds, phase limit lifetimes mass loss and dispersal shear Oort A feedback = Ω -B = Ω /2 (for V flat) S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  64. short gmc lifetimes: an observational estimate with PAWS! ‘upstream’ dynamical environments zone II ‘downstream’ zone I • cloud numbers decreases from zone I to ARM zone II (Colombo et al. 2013) zone II • mass spectrum evolution: shear and star zone I center formation feedback destroy clouds, phase limit lifetimes mass loss and dispersal shear Oort A feedback = Ω -B transformation = Ω /2 (for V flat) S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  65. a (simple) framework if cloud numbers decrease from zone I to zone II then lifetime < travel time from arm to arm S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  66. a (simple) framework if cloud numbers decrease from zone I to zone II then Eulerian vs. lifetime < travel time from arm to arm Lagrangian arm time II I arm S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  67. a (simple) framework if cloud numbers decrease from zone I to zone II then Eulerian vs. lifetime < travel time from arm to arm Lagrangian arm time split interarm in half, II I count N I and N II original arm lost half arm-to-arm travel time; measure from t orb S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  68. a (simple) framework if cloud numbers decrease from zone I to zone II then Eulerian vs. lifetime < travel time from arm to arm Lagrangian arm time split interarm in half, II I count N I and N II original arm lost half arm-to-arm travel time; measure from t orb • still sources + sinks (feedback cloud splitting, etc.) and when i.e. mostly losses S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  69. a (simple) framework if cloud numbers decrease from zone I to zone II then Eulerian vs. lifetime < travel time from arm to arm Lagrangian arm time split interarm in half, II I count N I and N II original high F lost small F lost arm long τ short τ pop. growth lost (transformation) half arm-to-arm travel ≈ time; measure from t orb • still sources + sinks (feedback cloud splitting, etc.) and when i.e. mostly losses S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

  70. GMC lifetimes S. E. Meidt--Q&Q July 2014 Saturday, July 19, 14

Recommend

OPEN PROBLEMS IN STAR FORMATION OUTLINE OUTLINE: THE BIG QUESTIONS Regulation of the star

OPEN PROBLEMS IN STAR FORMATION OUTLINE OUTLINE: THE BIG QUESTIONS Regulation of the star

MARK KRUMHOLZ OPEN PROBLEMS IN STAR FORMATION OUTLINE OUTLINE: THE BIG QUESTIONS Regulation of the star formation rate Global vs. local regulation Universal versus variable efficiency Bound clusters versus unbound associations

681 views • 32 slides
Dwarf Galaxy Formation with Dwarf Galaxy Formation with H 2 -regulated Star Formation H 2

Dwarf Galaxy Formation with Dwarf Galaxy Formation with H 2 -regulated Star Formation H 2

Dwarf Galaxy Formation with Dwarf Galaxy Formation with H 2 -regulated Star Formation H 2 -regulated Star Formation Michael Kuhlen, UC Berkeley arXiv:1105.2376 w/ M. Krumholz, P. Madau, B. Smith, J. Wise August 9 th 2011 2011 UC Santa Cruz

708 views • 33 slides
comments on star formation at the peak of the galaxy formation epoch its all different and

comments on star formation at the peak of the galaxy formation epoch its all different and

comments on star formation at the peak of the galaxy formation epoch its all different and still so similar Reinhard Genzel MPE &amp; UCB star formation and feedback at the peak of the galaxy formation epoch continuous LIRGs accretion

349 views • 9 slides
STACKED STAR FORMATION RATE PROFILES OF BURSTY GALAXIES EXHIBIT COHERENT STAR FORMATION

STACKED STAR FORMATION RATE PROFILES OF BURSTY GALAXIES EXHIBIT COHERENT STAR FORMATION

STACKED STAR FORMATION RATE PROFILES OF BURSTY GALAXIES EXHIBIT COHERENT STAR FORMATION GalFresca 2017, Pasadena, CA August 25, 2017 Matt Orr Dr. Philip F. Hopkins TAPIR | California Institute of Technology At high z (~1), observations

402 views • 21 slides
Measuring Star Formation Measuring Star Formation in Local and Distant Galaxies in Local and

Measuring Star Formation Measuring Star Formation in Local and Distant Galaxies in Local and

Measuring Star Formation Measuring Star Formation in Local and Distant Galaxies in Local and Distant Galaxies Daniela Calzetti (UMass) A Century of Cosmology, Venice, August 27-31, 2007 SINGS SINGS (Spitzer Infrared Nearby Galaxies Survey)

418 views • 26 slides
A Report of IAU Symposium 270 Computatioal Star Formation M. Yamada 1

A Report of IAU Symposium 270 Computatioal Star Formation M. Yamada 1

A Report of IAU Symposium 270 Computatioal Star Formation M. Yamada 1 Introduction/Contents Program of the symposium: a wide variety in scales, observations 1) individual star formation (low-/high-mass), clusters 2) feedback,

563 views • 27 slides
Self-regulated star formation Andreas Burkert C. Dobbs, E. Ntormousi, K. Fierlinger, Bigiel

Self-regulated star formation Andreas Burkert C. Dobbs, E. Ntormousi, K. Fierlinger, Bigiel

Self-regulated star formation Andreas Burkert C. Dobbs, E. Ntormousi, K. Fierlinger, Bigiel et al. J. Ngoumou, J. Pringle, S. Walch + SINS Munich Santa Cruz Evidence for self-regulation SFR = M H 2 with sf 1 2 10

579 views • 26 slides
AGN fueling and feedback Franoise Combes Observatoire de Paris 1 M82 Seoul, October 2013

AGN fueling and feedback Franoise Combes Observatoire de Paris 1 M82 Seoul, October 2013

Star formation, AGN fueling and feedback Franoise Combes Observatoire de Paris 1 M82 Seoul, October 2013 N1433 Outline 1- Gas distribution and Star Formation Star formation law is a molecular gas law 2- Star formation modes; main

802 views • 28 slides
Contents Star formation in the early universe - from big bang ripples to protostars The

Contents Star formation in the early universe - from big bang ripples to protostars The

Ancient Universe with GRB, Kyoto, 2010 T HE F IRST S TARS Naoki Yoshida Contents Star formation in the early universe - from big bang ripples to protostars The fate of very massive stars Low-metallicity star formation References: NY,

659 views • 36 slides
Disk Formation with Ambipolar Diffusion from Low- to High- Mass Star Formation Benot Commeron

Disk Formation with Ambipolar Diffusion from Low- to High- Mass Star Formation Benot Commeron

Disk Formation with Ambipolar Diffusion from Low- to High- Mass Star Formation Benot Commeron Centre de Recherche Astrophysique de Lyon Ugo Lebreuilly, Matthias Gonzlez, Patrick Hennebelle, Gilles Chabrier, Pierre Marchand, Jacques Masson,

413 views • 20 slides
The effect of photoionising feedback on star formation in colliding clouds Kazuhiro Shima

The effect of photoionising feedback on star formation in colliding clouds Kazuhiro Shima

The effect of photoionising feedback on star formation in colliding clouds Kazuhiro Shima (Hokkaido) Elizabeth J. Tasker (ISAS/JAXA) Christoph Federrath (ANU) Asao Habe (Hokkaido) INTRODUCTION Star formation is important supernova UV

432 views • 30 slides
The Dynamics of Star Cluster Formation Juan Pablo Farias Jonathan Tan (Chalmers, U. Virginia),

The Dynamics of Star Cluster Formation Juan Pablo Farias Jonathan Tan (Chalmers, U. Virginia),

The Dynamics of Star Cluster Formation Juan Pablo Farias Jonathan Tan (Chalmers, U. Virginia), Sourav Chatterjee (TATA Institute), Madeline Gyllenhoff (U. Virginia) How is gas transformed into a star cluster? What is the star formation

637 views • 34 slides
Star Formation Rate Indicators in Galaxy Formation Simulations Jos Flores Velazquez, Alex

Star Formation Rate Indicators in Galaxy Formation Simulations Jos Flores Velazquez, Alex

Star Formation Rate Indicators in Galaxy Formation Simulations Jos Flores Velazquez, Alex Gurvich, Prof. Faucher-Gigure + FIRE Collaboration SFR Indicators H Emissions Assuming Constant SFR : SFR(H ) Indicator traces stars

641 views • 13 slides
FEEDBACK IN GALAXY FORMATION Disks SMBH growth AGN and star formation Joe Silk IAP/JHU/Oxford

FEEDBACK IN GALAXY FORMATION Disks SMBH growth AGN and star formation Joe Silk IAP/JHU/Oxford

FEEDBACK IN GALAXY FORMATION Disks SMBH growth AGN and star formation Joe Silk IAP/JHU/Oxford Collaborators: Vincenzo Antonnucio-Deloglou, Volker Gaibler, Sadegh Khochfar Feedback is needed - 2 a 3 m p t cool T 1 + 2 b M

519 views • 35 slides
Regulation A and Regulation CF Forum on Small Business Capital Formation November 19, 2015 Sara

Regulation A and Regulation CF Forum on Small Business Capital Formation November 19, 2015 Sara

Regulation A and Regulation CF Forum on Small Business Capital Formation November 19, 2015 Sara Hanks CEO, CrowdCheck, Inc. Regulation A Changes to Regulation A effective June 19, 2015 Tier 1: Up to $20 million State and SEC

157 views • 5 slides
Star formation in the Local Group Guido De Marchi (ESA), Nino Panagia (STScI) Elena Sabbi

Star formation in the Local Group Guido De Marchi (ESA), Nino Panagia (STScI) Elena Sabbi

Star formation in the Local Group Guido De Marchi (ESA), Nino Panagia (STScI) Elena Sabbi (STScI), Giacomo Beccari (ESO) and NIRSpec GTO team ! 1 Motivation Solar mass stars account for most of the star formation in galaxies

736 views • 40 slides
The Role of Magnetic Field in Star Formation in the Disk of Milky Way Galaxy Shu-ichiro Inutsuka

The Role of Magnetic Field in Star Formation in the Disk of Milky Way Galaxy Shu-ichiro Inutsuka

Role of Magnetic Field in Star Formation &amp; Galactic Structure (Dec 2022, 2017) The Role of Magnetic Field in Star Formation in the Disk of Milky Way Galaxy Shu-ichiro Inutsuka (Nagoya University) Main Collaborators: Tsuyoshi Inoue, Doris

510 views • 47 slides
Making Black Holes - Early black hole formation scenarios - Connect with Star Formation? With:

Making Black Holes - Early black hole formation scenarios - Connect with Star Formation? With:

Making Black Holes - Early black hole formation scenarios - Connect with Star Formation? With: Matthew Turk, John Wise, Jeff Oishi, Ji-hoon Kim, Peng Simulation: John Wise &amp; Tom Abel 2011 Visualization: Ralf Khler &amp; Abel (KIPAC)

219 views • 19 slides
Triggered star formation, HII regions and Spitzer bubbles Mark Thompson Outline of the lectures

Triggered star formation, HII regions and Spitzer bubbles Mark Thompson Outline of the lectures

Triggered star formation, HII regions and Spitzer bubbles Mark Thompson Outline of the lectures 1.Observational surveys for infrared bubbles Spitzer bubbles &amp; the Milky Way Project 2.Theory of bubble formation &amp; triggered star

668 views • 33 slides
Triggered star formation, HII regions and Spitzer bubbles Mark Thompson Outline of the lectures

Triggered star formation, HII regions and Spitzer bubbles Mark Thompson Outline of the lectures

Triggered star formation, HII regions and Spitzer bubbles Mark Thompson Outline of the lectures 1.Observational surveys for infrared bubbles Spitzer bubbles &amp; the Milky Way Project 2.Theory of bubble formation &amp; triggered star

569 views • 30 slides
How to maintain the star formation of the Milky Way Galaxy? On the value of single dish

How to maintain the star formation of the Milky Way Galaxy? On the value of single dish

How to maintain the star formation of the Milky Way Galaxy? On the value of single dish full-sky surveys Jrgen Kerp 1 , Benjamin Winkel 2 , Peter Kalberla 1 and the EBHIS team 1 Argelander-Institut fr Astronomie, Universitt Bonn 2

641 views • 60 slides
The formation of spiral arms and rings in barred galaxies from the dynamical systems point of

The formation of spiral arms and rings in barred galaxies from the dynamical systems point of

The formation of spiral arms and rings in barred galaxies from the dynamical systems point of view. Merc` e Romero-G omez WSIMS 2008 Barcelona 1-5 December 2008 collaborators: J.J. Masdemont, E. Athanassoula Hubble classification scheme

668 views • 40 slides
Star formation quenching in different environments Toms Hough Instituto de Astrofsica de La

Star formation quenching in different environments Toms Hough Instituto de Astrofsica de La

Star formation quenching in different environments Toms Hough Instituto de Astrofsica de La Plata MultiDark Galaxies Workshop September 27, 2016 SAG group: Dra. Sofa A. Cora, Lic. Cristian Vega, Dr. Ignacio Gargiulo, Lic. Florencia

516 views • 29 slides
Star formation suppression by an AGN (in NGC 1266 and maybe more) Katherine Alatalo Infrared

Star formation suppression by an AGN (in NGC 1266 and maybe more) Katherine Alatalo Infrared

Star formation suppression by an AGN (in NGC 1266 and maybe more) Katherine Alatalo Infrared Processing &amp; Analysis Center Caltech kalatalo@ipac.caltech.edu ! with Philip Appleton, Carl Heiles, Kristina Nyland, Mark Lacy, Sabrina Cales,

445 views • 25 slides

More recommend