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

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

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.

Andrew Walsh, James Cook University Narrated by James Green (CASS) – thanks Jimi! (Psshhh aaahhh sssss push it) The Case for High Frequency Line Observations.

1)Disks and high-mass star formation: existence and implications 2)The case of G : characteristics 3)Velocity field in G31.41: rotation or expansion?

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

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.

Star & Planet Formation Alyssa A. Goodman Harvard-Smithsonian Center for Astrophysics.

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.

SMA Observations of Sgr A* Dan P. Marrone, Ram Rao, Jim Moran, Jun-Hui Zhao Harvard-Smithsonian Center for Astrophysics Sgr A * at 337 GHz 2004 May 25.

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

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.

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.

7/2/2015Richter - UC Davis1 EXES, the echelon-cross-echelle spectrograph for SOFIA Matthew J. Richter (UC Davis) with Mark McKelvey (NASA Ames Research.

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

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,

By James Moran Harvard-Smithsonian Center for Astrophysics University of Barcelona, October 5, 2012 Dinnertime for Sgr A* (The Black Hole in the Center.

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 (

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

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

ALMA Observations of Keplerian Disks around Protostars: the case of L1527 Nagayoshi Ohashi (NAOJ) NMA With K. Saigo, Y. Aso, S.-W. Yen, S. Takakuwa, S.

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.

Anchoring Magnetic Fields in Turbulent Molecular Clouds Hua-bai Li.

Are magnetic fields and outflows aligned in protostellar cores?

1 mm Polarization Science with CARMA

ALMA Science Examples Min S. Yun (UMass/ANASAC). ALMA Science Requirements  High Fidelity Imaging  Precise Imaging at 0.1” Resolution  Routine Sub-mJy.

Maite Beltrán Osservatorio Astrofisico di Arcetri The intringuing hot molecular core G

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)

Early O-Type Stars in the W51-IRS2 Cluster A template to study the most massive (proto)stars Luis Zapata Max Planck Institut für Radioastronomie, GERMANY.

Possible Future Spectroscopic Star Formation Surveys James Di Francesco (National Research Council Herzberg)

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

150GHz 100GHz 220GHz Galactic Latitude (Deg) A Millimeter Wave Galactic Plane Survey with the BICEP Polarimeter Evan Bierman (U.C. San Diego) and C. Darren.

A Survey of the Global Magnetic Fields of Giant Molecular Clouds Giles Novak, Northwestern University Instrument: SPARO Collaborators: P. Calisse, D. Chuss,

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

Characterizing Magnetized Turbulence through Magnetic Field Dispersion Martin Houde The University of Western Ontario CC2YSO - 19 May 2010.

Searching for the Synchrotron Cosmic Web with the Murchison Widefield Array Bryan Gaensler Centre for All-sky Astrophysics / The University of Sydney Natasha.

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.

Astrochemistry with the Upgraded Combined Array for Research in Millimeter-wave Astronomy D. N. Friedel Department of Astronomy University of Illinois.

Martin Bureau, University of Oxford WISDOM: mm-Wave Interferometric Survey of Dark Object Masses Martin Bureau, Oxford University CO (WISDOM: Leo Blitz,

The Submillimeter Array 1 David J. Wilner

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

SMA and ASTE Observations of Low-mass Protostellar Envelopes in the Submillimeter CS (J = 7-6) and HCN (J = 4-3) Lines Shigehisa Takakuwa 1, Takeshi Kamazaki.

OBSERVATIONS OF BINARY PROTOSTARS

Polarization in forming stars Probing small scales with carma

Linear and Circular Polarization from Sagittarius A*

Presentation transcript:

POLARIZATION SCIENCE WITH CARMA PROBING SMALL-SCALE MAGNETIC FIELDS IN STAR-FORMING REGIONS Chat Hull University of California, Berkeley Radio Astronomy Laboratory 10 April 2013 Special Session: Polarization ALMA 2013 Rocks! Kona, Hawai’i

Outline CARMA 1mm polarization system Science results & future proposals TADPOL survey: protostellar polarization Circumstellar disk polarization & formation Other projects: Serpens, SgrA*

Outline CARMA 1mm polarization system Science results & future proposals TADPOL survey: protostellar polarization Circumstellar disk polarization & formation Other projects: Serpens, SgrA*

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)

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

Wideband, 2-section polarizer λ/2 retarder at 15° λ/4 retarder at 74.5° Plambeck & Engargiola, CARMA Memo #54

R L    Receiver Sky Credit: Greg Engargiola Polarizer simulation LCP RCP X Y  Feed horn (sky) OMT  X Y Plambeck & Engargiola, CARMA Memo #54

Outline CARMA 1mm polarization system Science results & future proposals TADPOL survey: protostellar polarization Circumstellar disk polarization & formation Other projects: Serpens, SgrA*

Credit: Bill Saxton, Harvard-Smithsonian Center for Astrophysics

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

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 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)

TADPOL results L1157 See also: Stephens, Looney, Kwon, Hull et al. 2013, ApJL, submitted

Credit: Bill Saxton, Harvard-Smithsonian Center for Astrophysics

NGC 1333-IRAS 4B NGC 1333-IRAS 4A TADPOL results

L1527 NGC 1333-IRAS 2A

TADPOL results Ser-emb 8

Cumulative Distribution Function (CDF) (Projected) angle between outflow & B-field (deg) Outflow vs. B-field: distribution 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) Hull+ 2013, ApJ, accepted Preprint: arXiv: arXiv:

Upper limits on circumstellar disk polarization CARMA + SMA results Disks are not strongly polarized at ~100 AU scales: Hughes, Hull, Wilner, & Plambeck 2013, AJ, 145, 115

Implications for disk formation Weak & misaligned B- fields in cores could aid disk formation Addresses “magnetic braking catastrophe” Points are from simulations in Joos We find that ~10– 50% of Class 0/I stars should form Keplerian disks Krumholz, Crutcher, & Hull 2013, ApJL, 767, L11 Flux-to-mass ratio cos( between B-field & disk axis )

Other projects Filamentary B-field structure in Serpens Observing same field as ALMA (Mundy et al.) Galactic center (SgrA*) Rotation measure, simultaneous with SMA G2 cloud

CARMA 1 mm polarization system is fully functional, and accepting proposals (next deadline is next month (May, ‘13)) Wide array of science TADPOL results: 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 TADPOL results: arXiv: arXiv: TADPOL survey (CARMA key project): tadpol.astro.illinois.edutadpol.astro.illinois.edu Questions? Summary

Fin