ARE MAGNETIC FIELDS AND OUTFLOWS ALIGNED IN PROTOSTELLAR CORES? Chat Hull University of California, Berkeley (USA) Radio Astronomy Laboratory 5 February.

Slides:

Advertisements

Similar presentations

Magnetic Fields in T Tauri Disks A. Meredith Hughes Wesleyan University What Millimeter Polarimetry Can Tell Us Chat Hull, David Wilner, Sean Andrews,

Advertisements

The Combined Array for Research in Millimeter-Wave Astronomy

BIMA Array Detections of HCN in Comets LINEAR (C/2002 T7) and NEAT (C/2001 Q4) D. N. Friedel (University of Illinois) Collaborators: A. Remijan (NASA GSFC)

The Serpens Star Forming Region in HCO +, HCN, and N 2 H + Michiel R. Hogerheijde Steward Observatory The University of Arizona.

Methanol maser polarization in W3(OH) Lisa Harvey-Smith Collaborators: Vlemmings, Cohen, Soria-Ruiz Joint Institute for VLBI in Europe.

Ammonia and CCS as diagnostic tools of low-mass protostars Ammonia and CCS as diagnostic tools of low-mass protostars Itziar de Gregorio-Monsalvo (ESO.

The Galactic Center: Molecular Line Mapping with Broadband Spectrometers Jürgen Ott ESO 3D Meeting 11 June 2008 The Galactic Center: Molecular Line Mapping.

Studying circumstellar envelopes with ALMA

Portrait of a Forming Massive Protocluster: NGC6334 I(N) Todd Hunter (NRAO/North American ALMA Science Center) Collaborators: Crystal Brogan (NRAO) Ken.

SMA Observations of the Binary Protostar System in L723 Josep Miquel Girart 1, Ramp Rao 2, Robert Estalella 3 & Josep Mª Masqué 3 1 Institut de Ciències.

circular polarizer orthomode transducer

Polarization 101 Absorption Emission Scattering. PolarizationPolarization of Background Starlight.

SOFIA/HAWC polarimetry of low-mass YSOs and their environs.

21st-Century Astronomy Sensitivity Higher Sensitivity Enables: –Large surveys –Deep exposures Resolution Higher Resolution Enables: –Detailed view of nearby.

Millimeter Spectroscopy Joanna Brown. Why millimeter wavelengths? >1000 interstellar & circumstellar molecular lines Useful for objects at all different.

The Galactic Center: From the Black Hole to the Minispiral Jim Moran Harvard-Smithsonian Center for Astrophysics Institut d’Astrophysique de Paris and.

Outflow-Envelope Interactions at the Early Stages of Star Formation Héctor G. Arce (AMNH) & Anneila I. Sargent (Caltech) Submillimeter Astronomy: in the.

Magnetic Fields in Star Formation Alyssa A. Goodman Harvard-Smithsonian Center for Astrophysics Tyler Bourke Smithsonian Astrophysical Observatory/SMA.

ORBITAL MOTIONS IN BINARY AND MULTIPLE PROTOSTARS L. F. Rodríguez (IAUNAM, Morelia) L. Loinard, M. Rodríguez, & P. D’Alessio (IAUNAM, Morelia) S. Curiel,

STAR FORMATION STUDIES with the CORNELL-CALTECH ATACAMA TELESCOPE Star Formation/ISM Working Group Paul F. Goldsmith (Cornell) & Neal. J. Evans II (Univ.

Magnetic Field Morphologies in NGC1333 IRAS4A: Evidence for Hour Glass Structure R. Rao (CfA) J. M. Girart (CSIC/IEEC) D. P. Marrone (CfA)

CARMA Dick Plambeck UC Berkeley (for the CARMA consortium) URSI, 24 June 2003, Columbus, Ohio.

Is SOFIA the large or the small scale? ALMA: resolution up to 0.02  / (mm), shortest  330  m Connecting Large and Small Scale Magnetic Fields.

Structure of circumstellar envelope around AGB and post-AGB stars Dinh-V-Trung Sun Kwok, P.J. Chiu, M.Y. Wang, S. Muller, A. Lo, N. Hirano, M. Mariappan,

Submillimeter Astronomy in the era of the SMA, Cambridge, June 14, 2005 Star Formation and Protostars at High Angular Resolution with the SMA Jes Jørgensen.

Definitive Science with Band 3 adapted from the ALMA Design Reference Science Plan (

Dick Plambeck UC Berkeley (for the CARMA consortium)

University of Chicago 2007 July 30 SOFIA-POL 2007 The Infrared - Millimeter Polarization Spectrum John Vaillancourt California Institute of Technology.

SCUBA Polarization results: Jane Greaves, Joint Astronomy Centre, Hawaii with special thanks to: Wayne Holland, Tim Jenness, David Berry and.

ARE MAGNETIC FIELDS AND OUTFLOWS ALIGNED IN PROTOSTELLAR CORES? Chat Hull UC Berkeley, Radio Astronomy Laboratory 10 January 2013 Session 426. Star Formation.

CARMA observations of magnetic fields in star-forming filaments Chat Hull Jansky Fellow — Harvard-Smithsonian Center for Astrophysics National Radio Astronomy.

Star Formation Research Now & With ALMA Debra Shepherd National Radio Astronomy Observatory ALMA Specifications: Today’s (sub)millimeter interferometers.

TURBULENCE AND HEATING OF MOLECULAR CLOUDS IN THE GALACTIC CENTER: Natalie Butterfield (UIowa) Cornelia Lang (UIowa) Betsy Mills (NRAO) Dominic Ludovici.

2005 June 2260th Symposium on Molecular Spectroscopy Outflows and Magnetic Fields in L1448 IRS3 Woojin Kwon Leslie W. Looney Richard M. Crutcher Jason.

Masers observations of Magnetic fields during Massive Star Formation Wouter Vlemmings (Argelander-Institut für Astronomie, Bonn) with Gabriele Surcis,

Magnetic Fields Near the Young Stellar Object IRAS M. J Claussen (NRAO), A. P. Sarma (E. Kentucky Univ), H.A. Wootten (NRAO), K. B. Marvel (AAS),

Water maser emission in Bok globules Bok Globules Bok globules are small (

Probing Magnetic Fields in Protostars with near-IR Polarimetry Barbara Whitney University of Wisconsin-Madison.

Radio Interferometry and ALMA T. L. Wilson ESO. A few basics: Wavelength and frequency  -1 temperature max (mm) ~ 3/T(K) (for blackbody) Hot gas radiates.

ARE MAGNETIC FIELDS AND OUTFLOWS ALIGNED IN PROTOSTELLAR CORES? Chat Hull University of California, Berkeley Radio Astronomy Laboratory 4 April 2013 Institute.

SPIRE-FTS spectrum of Arp 220, Mrk 231 and NGC Bright CO (J = 4-3 to J = 13-12), water, and atomic fine-structure line transitions are labeled. The.

Great Barriers in High Mass Star Formation, Townsville, Australia, Sept 16, 2010 Patrick Koch Academia Sinica, Institute of Astronomy and Astrophysics.

How Stars Form Shantanu Basu Physics & Astronomy University of Western Ontario Preview Western, May 3/4, 2003.

Primary Beam Shape Calibration from Mosaicked, Interferometric Observations Chat Hull Collaborators : Geoff Bower, Steve Croft, Peter Williams, Casey Law,

1 mm Polarization Science with CARMA Chat Hull UC Berkeley, Radio Astronomy Laboratory Collaborators: Dick Plambeck, Greg Engargiola, & all the CARMA staff.

ARE MAGNETIC FIELDS AND OUTFLOWS ALIGNED IN PROTOSTELLAR CORES? Chat Hull University of California, Berkeley Radio Astronomy Laboratory 28 September 2013.

The Galactic Plane Infrared Polarization Survey (GPIPS) Current Members: Michael Pavel Dan Clemens (PI) Lauren Cashman Sadia Hoq Jordan Montgomory Ian.

Magnetic fields in the Galaxy via Faraday effect: Future prospects with ASKAP and the SKA Lisa Harvey-Smith Collaborators: Bryan CSIRO SKA Project ScientistGaensler.

CARMA Large Area Star-formation SurveY  Completing observations of 5 regions of square arcminutes with 7” angular resolution in the J=1-0 transitions.

Magnetic Fields in Molecular Clouds Richard M. Crutcher University of Illinois Collaborators:Tom Troland, University of Kentucky Edith Falgarone, Ecole.

The North American ALMA Science Center North America’s ALMA Regional Center The North American ALMA Science Center acts as the gateway to ALMA for North.

POLARIZATION SCIENCE WITH CARMA PROBING SMALL-SCALE MAGNETIC FIELDS IN STAR-FORMING REGIONS Chat Hull University of California, Berkeley Radio Astronomy.

The JCMT in the ALMA Era Surveying the Sub-millimetre Sky (Canada / Netherlands / Great Britain) Doug Johnstone NRC/HIA.

Seeing Stars with Radio Eyes Christopher G. De Pree RARE CATS Green Bank, WV June 2002.

Protostellar jets and outflows — what ALMA can achieve? — 平野尚美 (Naomi Hirano) 中研院天文所 (ASIAA)

Shih-Ping Lai 賴詩萍 (National Tsing-Hua University, Taiwan) 清華大學, 台灣.

Magnetic fields in Planetary and Proto Planetary

Are magnetic fields and outflows aligned in protostellar cores?

1 mm Polarization Science with CARMA

Fitting Magnetized Molecular Cloud Collapse Models to NGC 1333 IRAS 4A Pau Frau Josep Miquel Girart Daniele Galli Institut de Ciències de l’Espai (IEEC-CSIC)

Héctor G. Arce Yale University Image Credit: ESO/ALMA/H. Arce/ B. Reipurth Shocks and Molecules in Protostellar Outflows.

IV. Radiative Transfer Models The radiative transfer modeling procedure is the same procedure used in Shirley et al. (2002) except that the visibility.

ARE MAGNETIC FIELDS AND OUTFLOWS ALIGNED IN PROTOSTELLAR CORES? Chat Hull University of California, Berkeley Radio Astronomy Laboratory 8 July 2013 CARMA.

NGC7538-IRS1: Polarized Dust & Molecular Outflow C. L. H. Hull (UC Berkeley), T. Pillai (Caltech), J.-H. Zhao (CfA), G. Sandell (SOFIA-USRA, NASA), M.

NML Cyg The ARO 1 mm Survey of the Oxygen-rich Envelope of Supergiant Star NML Cygnus Jessica L. Edwards, Lucy M. Ziurys, and Nick J. Woolf The University.

Grain Growth and Substructure in Protoplanetary Disks David J. Wilner Harvard-Smithsonian Center for Astrophysics S. Corder (NRAO) A. Deller.

Polarized Light from Star-Forming Regions

OBSERVATIONS OF BINARY PROTOSTARS

Polarization in forming stars Probing small scales with carma

High Resolution Submm Observations of Massive Protostars

Presentation transcript:

ARE MAGNETIC FIELDS AND OUTFLOWS ALIGNED IN PROTOSTELLAR CORES? Chat Hull University of California, Berkeley (USA) Radio Astronomy Laboratory 5 February 2013 Session: Magnetic Fields in the ISM and Star-forming Regions I Magnetic Fields in the Universe IV Playa del Carmen, Quintana Roo, México

Credit: Bill Saxton, Harvard-Smithsonian Center for Astrophysics Simple model of SF with B-fields

Girart Rao Holland Misalignment of B-fields and outflows Outflow B-field IRAS IRAS 4A VLA 1623

CARMA Combined Array for Research in Millimeter-wave Astronomy Consortium: Berkeley, Caltech, Illinois, Maryland, Chicago – 6 10-m, 9 6-m, m telescopes – Observations at 1 cm, 3 mm, and 1 mm (polarization!) – Located in Cedar Flat, CA (near Bishop)

Waveguide circular polarizer Orthomode transducer SIS mixers WBA13 I.F. amplifiers (1-9 GHz ) 1 mm dual-polarization receivers 1 inch Credit: Dick Plambeck

TADPOL survey 35 sources Triples number of interferometric polarization maps ~300 observing hours CARMA C, D, & E arrays 1 – 4" resolution 10 higher resolution than CSO & JCMT Probes intermediate region between ~0.1 pc (single-dish) and ~100 AU (ALMA) 1 mm wavelength Ideal for dust polarization, as well as CO(2-1) for outflow mapping ≠ 75 seconds

TADPOL collaboration UC Berkeley Chat Hull (PI), Dick Plambeck, Mel Wright, Carl Heiles, Geoff Bower University of Maryland Marc Pound, Alberto Bolatto, Katherine Jameson, Lee Mundy Caltech Thushara Pillai, John Carpenter, James Lamb, Nikolaus Volgenau University of Illinois, Urbana-Champagne Ian Stephens, Leslie Looney, Woojin Kwon, Dick Crutcher, Nick Hakobian Other Dan Marrone (Arizona), Meredith Hughes (Wesleyan), John Vaillancourt & Göran Sandell (USRA-SOFIA), John Tobin (NRAO), Jason Fiege (Manitoba), Erica Franzmann (Manitoba), Martin Houde (UWO, Caltech), Brenda Matthews (NRC-CNRC)

TADPOL results L1157

NGC 1333-IRAS 2ANGC 1333-IRAS 4A TADPOL results

NGC 1333-IRAS 4B Ser-emb 8 TADPOL results

Cumulative Distribution Function (CDF) (Projected) angle between outflow & B-field (deg) Outflow vs. B-field: distribution Hull+ 2012, submitted to ApJL Preprint: arXiv: arXiv: Simulation: outflows & B-fields aligned within a 20º cone (tightly aligned) Simulation: outflows & B-fields are randomly oriented KS-test results: 20º cone ruled out ( p-value ~ ) Misaligned ( 0.79 ) and random ( 0.64 ) cannot be ruled out Simulation: outflows & B-fields aligned between 70–90º (preferentially misaligned)

Conclusions B-fields are either preferentially misaligned (perp.) or randomly aligned with respect to outflows at the ~1000 AU scale Thus, circumstellar disks are misaligned with fields in the cores from which they formed Future work: Compare polarization in filaments with ALMA data Compare B-fields in SCUBA (~0.1 pc) and CARMA (~1000 AU, or ~0.05 pc) data TADPOL results: arXiv: arXiv: TADPOL survey (CARMA key project): tadpol.astro.illinois.edutadpol.astro.illinois.edu Questions? Contact Chat Hull:

Fin