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Explorations of Disk Formation and Multiplicity with the Ngvla

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Explorations of Disk Formation and Multiplicity with the Ngvla Explorations of Disk Formation and Multiplicity with the ngVLA John Tobin University of Oklahoma http://nhn.ou.edu/~jjtobin/VANDAM/ Image: Bill Saxton (NRAO) Thanks to the VANDAM Team! VANDAM: VLA/ALMA Nascent Disk and Multiplicity Survey VANDAM Perseus Team: VANDAM Orion Team: John Tobin (PI) John Tobin (PI) Leslie Looney (Illinois) VANDAM Perseus+ Zhi-Yun Li (Virginia) Tom Megeath (Toldeo) Claire Chandler (NRAO) Magnus Persson (Onsala) Mike Dunham (CfA) Mihkel Kama (Cambridge) Kaitlin Kratter (Arizona) Nadia Murillo (Leiden) Dominique Segura-Cox (Illinois) Stella Offner (UMASS) Sarah Sadavoy (MPIA) Marina Kounkel (Michigan) Laura Perez (Bonn/UC Chile) Ewine van Dishoeck (Leiden) Carl Melis (UCSD) Ana Karla Diaz Rodriguez (IAA) Robert Harris (Illinois) Mayra Osorio (IAA) Lukasz Tychoniec (Leiden/AMU-Poland) Guillem Anglada (IAA) Erin Cox (Illinois) Joesph Booker (Toledo) Frederick Wyrowski (MPIfR) Elise Furlan (IPAC) Ruud Visser (ESO) James Di Francesco (HIA) Nick Reynolds (OU) Brian Stephenson (OU) Lisa Patel (OU) Nicole Karnath (Toledo) Disks in the Protostellar Phase ● Proto-planetary disk – disk around pre- main sequence star; no infalling envelope ● Protostellar disk – disk around embedded protostar; infalling envelope feeding disk ● Disk forms and grows w/protostar ● Significant growth, evolution prior to PPD state, ~ few x Myr ● Grain growth may be happening early ● PPDs might start with large grains TW Hya (Andrews+2016) Multiple Star Formation Separation log (AU) 0.01 0.1 1 10 100 1000 10000 ● Large fraction of MS stars are multiple ● Dependence on spectral type (mass) ● Multiplicity important aspect of star and planet formation U A 0 ● Protostellar multiplicity only examined 5 for small region of parameter space ● Most protostars multiple in this range Chen+2013 Lada 2006 Raghavan+10 ● Sub/Millimeter/Centimeter interferometry essential for characterizing early multiplicity VLA and ALMA Nascent Disk And Multiplicity (VANDAM) Survey ● VANDAM I: Perseus – 264 hour VLA large program (executed 2013-2015) ● 92 protostars, 0.06” (~15AU); 0.1 - ~40 Lsun ● 8 mm, 1 cm, 4 cm, 6.4 cm ● ALMA follow-up for subset ● VANDAM II: Orion – 350 hour VLA large program; 9 hour ALMA (2016-2017) ● 330 protostars (ALMA); 150 (VLA); 0.1 - ~1000 Lsun ● 0.06” - 0.12” (25 – 50 AU) ● 0.87 mm, 8 mm, 1 cm Western Perseus Molecular Cloud NGC 1333 B1 L1448 L1451 2 pc L1455 Herschel 250, 350, 500 μm Pezzuto+2012 VANDAM Class 0Disk Candidates VANDAM Segura-Cox+2017 L1448 NGC 1333 B1 0.2 pc Spitzer L1451 3.6, 4.5, 8.0 μm Tobin+2007 Tobin+2016 Evidence for Fragmenting Disks 1.3 mm Orbit of Pluto! Tobin+2016 ● Companions detected @ < 20 AU toward 3 protostars ● Disk optically thick at 1.3 mm – Difficult for ALMA to detect such a binary system Perseus Separation Distribution Disk Frag. Turbulent Frag. Tobin+2016 ● Suggest that disk and turbulent fragmentation operating for distinct scales Highlights from Orion Orion Multiplicity Highlights (NGC 2071 IR) ALMA Tobin+in prep Orion Multiplicity Highlights (NGC 2071 IR) VLA Tobin+in prep Orion Multiplicity Highlights (NGC 2071 IR) VLA Tobin+in prep Orion Multiplicity Highlights (NGC 2071 IR) VLA Tobin+in prep Frontiers Opened by the ngVLA ● Number of Number protostars atfor < d statistics is limiting pc 300 Perseus Separation Distribution ngVLA 10x limit – 1.5 AU VLA limit ~15 AU ● ● pc has protostarsOrion @~ 400 420 Closest systemsngVLA Closest need Orion SeparationOrion Distribution ngVLA 10x limit – 3 AU VLA limit ~30 AU @ 420@ pc ● ngVLA opens door outdoor to for kpc! opens regions 1.5 SF ngVLA Cygnus - X SeparationDistribution ngVLA 10x limit – 7 AU @ 1500@ pc VLA limit ~ 91 AU IRAS 03292- A Benchmark System 1.3 mm Orbit of Pluto! ● Fν (9 mm) ~ A: 170 μJy/bm (S/N ~ 17), B: 130 μJy/bm (S/N ~ 13) – @ Orion/Serpens: Fν ~ A: 51 μJy/bm, B: 39 μJy/bm – @ 1.5 kpc: Fν ~ A: 4 μJy/bm, B: 3 μJy/bm ● ngVLA rms @ 30 GHz: 0.79 μJy/bm/hr ● S/N=10 at 1.5 kpc w/ngVLA with ~4 hr on source! ● ngVLA resolution will enable orbital motion for nearby sources – Protostar masses! ● ● ● ● ngVLA will open-up study of more distant star forming regions ngVLA Multiplicity early in protostellar phase becoming characterized Large sample of protostellar disk candidates revealed by VLA Unbiased surveys crucial disk for and multiplicity studies – Terrestrial planet forming regions nearby for SF regions Terrestrial ~50 AU (0.2”) Summary aka HH1-2 MMS HH1-2 aka Orion Disk/Well-Resolved Highlights ALMA Tobin+in prep. Orion Disk/Well-Resolved Highlights aka OMC MMS6N VLA Tobin+in prep. Orion Multiplicity Highlights aka HH1-2 MMS ALMA Tobin+in prep, Stephenson+in prep. Orion Multiplicity Highlights aka HH1-2 MMS VLA Tobin+in prep, Stephenson+in prep. Preliminary! Orion Separations Tobin+in prep Research Supported By: ● NWO Veni Fellowship ● EU A-ERC Grant CHEMPLAN ● NASA Hubble Fellowship (formerly) ● NRAO funded by National Science Foundation Protostellar Jets: IRAS2B Tychoniec+2016 in prep. Protostellar Jets: IRAS2B x Tychoniec+2016 in prep. Protostellar Jets: IRAS2B Spectral Index Spectral Index Error α = -0.75 +/- 0.17 x Tychoniec+2016 in prep. ● X-ray emission possibly detected, blended with nearby Class III YSO ● Class III source has negative spectral index at 4 cm/6 cm Multiplicity Statistics ● Multiplicity Fraction (MF) and Companion Star Fraction (CSF) depend on scales of interest ● 15 AU to 10000 AU – Class 0 – MF = 0.57 – CSF = 1.21 – Class I – MF = 0.23 – CSF = 0.23 – due to wide Class 0/I pairs ● 15 AU to 2000 AU – Class 0 – MF = 0.35 – CSF = 0.43 – Class I – MF = 0.28 – CSF = 0.28 ● 15 AU to 1000 AU – Class 0 – MF = 0.27 – CSF = 0.30 – Class I – MF = 0.27 – CSF = 0.27 ● Most stars are born in wide multiple systems that rapid dissolve – Smaller fraction have closer companions Tobin+2015 submitted Evidence for Fragmenting Disks Western Perseus Molecular Cloud NGC 1333 B1 L1448 L1451 2 pc L1455 Herschel SPIRE Tobin+2015 in prep. Eastern Perseus Molecular Cloud IC348 Herschel SPIRE Tobin+2015 in prep. Western Perseus Molecular Cloud NGC 1333 B1 L1448 L1451 2 pc L1455 Herschel SPIRE Western Perseus Molecular Cloud NGC 1333 B1 L1448 L1451 2 pc L1455 Herschel SPIRE Tobin+2015 in prep. Western Perseus Molecular Cloud NGC 1333 B1 L1448 L1451 2 pc L1455 Herschel SPIRE Tobin+2015 submitted Western Perseus Molecular Cloud NGC 1333 B1 L1448 L1451 2 pc L1455 Herschel SPIRE 500 µm Tobin+2015 in prep. Western Perseus Molecular Cloud NGC 1333 B1 L1448 L1451 2 pc L1455 Herschel SPIRE 500 µm Tobin+2015 in prep. Protostellar Disks: Big or Small? Large, massive – Gravitaitionally Unstable Small, low-mass, and/or no rotational support Continuum of disk sizes? ~20 AU 400 AU Adapted from Kratter+2010 e.g., Vorobyov 2010, Kratter+2010 Significant magnetic braking? Allen+2003, Little or no magnetic braking (e.g. TSC 1984) Galli2006, Mellon & Li 2008, et al. ● Youngest protostellar disks have long eluded direct observation VANDAM 'Disk' Masses 0.027 M sun 0.079 M sun Tobin+2016 in prep. ● Masses from 8 mm emission corrected for free-free contribution – Extrapolation from 4 cm and 6.4 cm data – Assume Ossenkopf & Henning 1994 at 1.3 mm, β = 1 to 8 mm Perseus Separation Distribution Resolution limit Field solar-type stars Raghavan+10 Tobin+2016 ● Perseus Class 0 and Class I Separation Distribution ● Excess relative to field at ~75 AU and > 1000 AU Western Perseus Molecular Cloud NGC 1333 B1 L1448 L1451 2 pc L1455 Herschel 250, 350, 500 μm Pezzuto+2012 Western Perseus Molecular Cloud NGC 1333 B1 L1448 L1451 2 pc L1455 Herschel 250, 350, 500 μm Pezzuto+2012 Western Perseus Molecular Cloud NGC 1333 B1 L1448 0.2 pc Spitzer L1451 3.6, 4.5, 8.0 μm Tobin+2007 L1455 Western Perseus Molecular Cloud NGC 1333 B1 L1448 0.2 pc Spitzer L1451 3.6, 4.5, 8.0 μm Tobin+2007 L1455 Western Perseus Molecular Cloud NGC 1333 B1 L1448 0.2 pc Spitzer L1451 3.6, 4.5, 8.0 μm Tobin+2007 L1455 Protostellar Phase Epoch of Disk Formation outflow Envelope Envelope Disk outflow ~0.1 pc Image: Bill Saxton (NRAO).
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