The ALMA SKA Synergy For Star and Stellar Cluster Formation

Transcription

1 The ALMA SKA Synergy For Star and Stellar Cluster Formation Gary Fuller Jodrell Bank Centre for Astrophysics & UK ALMA Regional Centre Node University of Manchester

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3 What is ALMA? Atacama Large Millimetre/Sub-millimetre Array Aperture synthesis array optimised for millimetre and submillimetre wavelengths (1cm - 0.3mm/ GHz) High, dry site, Chajnantor Plateau, Chile (5000m) International: Europe (ESO), North America (NRAO), East Asia (NAOJ) + Joint ALMA Office in Chile 66 antennas (12m and 7m diameter) 61 now on high site Inauguration 13 March 2013 (Early science Oct 2012 Cycle 0) Cycle 2 observations start June 2014 Cycle 3 deadline expected ~June

4 ALMA Science Drivers Image spectral line emission from CO or C+ in a galaxy with similar mass to the Milky Way at a redshift of z = 3, in less than 24 hours of observation. Image the gas kinematics in a solar-mass protostellar/ protoplanetary disk at a distance of 150 pc. Study the physical, chemical, and magnetic field structure of the disk and detect the tidal gaps created by planets undergoing formation. Provide precise images at a resolution of 0.1 arcsec. 4

5 Transparent site allows full spectral coverage 5

6 ALMA & SKA1 Thermal dust Ionised gas 0.1pc 4kpc 100AU 140pc 4kpc 6

7 Evolved Stars AGB star R Sculptoris CO J=3-2 spiral 1.3'' Thermal pulse 1800 yr ago for 200 yr Shaped by binary 7 (Maercker etal 2012)

8 Circumstellar Disks Dust continuum emission Survey: Upper Sco OB Association Age 5-11 Myr Carpenter et al

9 Disk Structure Pérez et al SKA: Growth dust to pebbles and COMs Transition disks ~20% mass asymmetry ~2 Jupiter mass Oph-IRS GHz cont. 0.25'' beam 19um VISIR van der Marel

10 Disks around Protostars Younger objects R Cor Aus IRS7B 2.3Mo star (5Lo) Mo disk Lindberg et al

11 Outflows HH46 CO J=3-2 3'', 29 pointing mosaic Swept up material Wind/Jet? SKA Arce et al 2014 L1551 HI VLA HI wind/jet component Ionised wind/jet Giovanrdi et al 2000 Continuum RRL Tb~25-50K Wind/jet composition, structure, origin 11

12 Infall Infall Around Low Mass Protostars COMs: Glycolaldehyde Pineda et al 2012 Kristensen et al 2013 Jorgensen et al Zapata et al

13 Peretto et al 2013 Massive Star Formation Avison et al 2014 ALMA 3mm cont. GLIMPSE 8μm 25GHz continuum Collapse 5000 Mo clump ALMA 3mm continuum: 500 Mo 0.05pc core 3 sources earlier than B1/B0 forming + sufficient mass for OB association SKA Origin of clouds & cores Inflow onto stars 13

14 HI & The Age of Clouds Goldsmith et al 2006 Conversion of HI to H2 in fixed density profile cloud Wave of H2 formation propagates out from high density central region of cloud 14

15 Disk Accretion Shock? Neufeld & Hollenbach 1996 Envelope infall on to disk 15

16 Flow into the Protostar Matt & Pudritz 2005 Brickhouse et al

17 Accretion (?) on to low mass YSOs Hα TW Hya Dupree et al 2014 Optical/IR photometric & spectral variability X-ray variability Radio flares YWL15A Xrays Imanishi et al 2001 V773 Tau 8-40 GHz Massi et al 2002 DQ Tau 3mm flare Salter et al TTauri photometric periods Xiao et al

18 Low Protostars? 70% of Class I detected protostars detected in radio Thermal winds Non-thermal? 16 GHz SKA Nature of emission Variability Scaife etal 2011,2012 Periodic? Spots Rotation rates Massive protostars? Can have strong (<20kG) B fields (TTauri stars ~5kG) Spots, rotation? 18

19 Protostars? 70% of Class I detected protostars detected in radio Thermal winds Non-thermal? 16 GHz SKA Nature of emission Variability Rosen et al 2012 Periodic? Spots Rotation rates Massive protostars? Can have strong (<20kG) B fields (TTauri stars ~5kG) Spots, rotation? 19

20 Flickering UCHII Regions Change in size and flux of UCHII/HCHII regions as mass accretion varies Peters et al 2010; Galavan-Madrid et al % /yr changes in size & flux Match observations Eg Franco-Hernandez et al. 2004; Galvan-Madrid et al 2008 Other possible explanations Swelling of protostar SKA: Survey clusters to trace infall onto ionizing sources & estimate mass accretion rates. 20

21 Massive Protostar Photospheres Are the massive protostars small & hot or bloated and cool? Klassen etal 2012 Inayoshi et al 2013 Flux? AFGL2591 (0.04'') 1 (van der Tak & Menten 2005), ->15 GHz 24μJy, 8GHz 7μJy Mira 20GHz, 2kpc 0.2μJy SKA2? 21

22 Molecular lines: H2CO 4.8 GHz and 14.5 GHz line 4.8 GHz GHz GHz ALMA Also many other H2CO lines 4.8/14.5 ratio density Ginsburg et al

23 Proplyds Orion Disk lifetimes & mass distributions in clusters ALMA: dust & molecular gas HST ALMA 345GHz dust Mjup SKA: Atomic & ionised flow off disks Mann et al

24 ALMA-SKA Synergy SKA ALMA Cold/warm dust & molecular gas Reservoirs & flow towards star (Rathborne) SKA: wide field SKA1Mid Project Multi-frequency, multi-epoch full Stokes continuum (+lines) surveys of forming clusters Feedback Flow to star accretion/outflow Molecules Neutral atomic & ionised gas H2CO, CH3OH, COMs (Viti) Stars B fields Variability Rotation Tomography of star forming regions (Loinard) UCHII evolution accretion histories/protostar evolution Disks Making rocks (Bourke) COMs 24