UC Berkeley GBT Measurements of the Zeeman Effect in the Eridanus/Orion Region Tim Robishaw Carl Heiles.

Slides:



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

H 2 Formation in the Perseus Molecular Cloud: Observations Meet Theory.
MAGNETIC FIELDS IN THE MILKY WAY AND BEYOND Carl Heiles, UC Berkeley.
Study of Magnetic Helicity Injection in the Active Region NOAA Associated with the X-class Flare of 2011 February 15 Sung-Hong Park 1, K. Cho 1,
Solar Erupting Filaments and Magnetic Field Configurations of IP Magnetic Clouds Yuming Wang 1, 2 & Jie Zhang 1 (Presenting) 1 George Mason University.
A Method of Resolving the 180- Degree Ambiguity by Employing the Chirality of Solar Features S. F. Martin, Y. Lin, O. Engvold 2008, Sol. Phys. 250, 31.
Radiation & Photometry AS4100 Astrofisika Pengamatan Prodi Astronomi 2007/2008 B. Dermawan.
The Relation between Filament Skew Angle and Magnetic Helicity of Active Regions Masaoki HAGINO, Y.J. MOON (Korea Astronomy and Space Science Institute)
2. 1 Yes, signal! Physical Properties of diffuse HI gas in the Galaxy from the Arecibo Millennium Survey T. H. Troland Physics & Astronomy Department.
3-D Simulations of Magnetized Super Bubbles J. M. Stil N. D. Wityk R. Ouyed A. R. Taylor Department of Physics and Astronomy, The University of Calgary,
The Green Bank Telescope a powerful instrument for enhancing ALMA science Unblocked Aperture Low sidelobes gives high dynamic range Resistance to Interference.
Polarization 101 Absorption Emission Scattering. PolarizationPolarization of Background Starlight.
Magnetic Fields in Star Formation Alyssa A. Goodman Harvard-Smithsonian Center for Astrophysics Tyler Bourke Smithsonian Astrophysical Observatory/SMA.
STAR FORMATION STUDIES with the CORNELL-CALTECH ATACAMA TELESCOPE Star Formation/ISM Working Group Paul F. Goldsmith (Cornell) & Neal. J. Evans II (Univ.
Magnetic fields in Orion’s Veil T. Troland Physics & Astronomy Department University of Kentucky Microstructures in the Interstellar Medium April 22, 2007.
Order, Chaos and the Space Between the Stars Alyssa A. Goodman Harvard-Smithsonian Center for Astrophysics WIYN Image: T.A. Rector (NOAO/AURA/NSF) and.
21 October Introduction to M4 Science Observe 95  m Polarized Radiation l Map the “Magnetic Field of the Milky Way” (Central 100 degrees in l and.
Mapping Hydrogen in the Galaxy, Galactic Halo and Local Group with the Galactic Arecibo L-Band Feed Array (GALFA) The GALFA-HI Survey starting with TOGS.
Direct Measurement of a Magnetic Field at z=0.692 Art Wolfe Regina Jorgenson: IOA Tim Robishaw: UCB Carl Heiles:UCB Jason X. Prochaska:UCSC.
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.
Kagoya/Inoue Optical: Slotnick, Slotnick & Block The Black Hole Accretion Disk in NGC4258: One of Nature’s Most Beautiful Dynamical Systems Alice Argon.
1 Magnetic fields in star forming regions: theory Daniele Galli INAF-Osservatorio di Arcetri Italy.
Molecular absorption in Cen A on VLBI scales Huib Jan van Langevelde, JIVE Ylva Pihlström, NRAO Tony Beasley, CARMA.
2005 June 2260th Symposium on Molecular Spectroscopy Outflows and Magnetic Fields in L1448 IRS3 Woojin Kwon Leslie W. Looney Richard M. Crutcher Jason.
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),
The quantitative analysis of the spiral chirality of penumbral filament 1 Helicity Thinkshop on Solar Physics, Oct. 2013, Beijing Liu J.H., Su J.T. et.
THE GOLDEN AGE OF RADIO ASTRONOMY: INTERSELLAR MOLECULES AND ASTROCHEMISTRY IAU 2015 Jack Welch, University of California Berkeley.
The Galactic Center at Low Radio Frequencies Namir Kassim (NRL) Crystal Brogan (IfA) J. Lazio (NRL), Ted LaRosa (Kennesaw State), M. Nord (NRL/UNM), W.
$100 $200 $300 $400 $500 $100 $200 $300 $400 $500 $100 $200 $300 $400 $500 $100 $200 $300 $400 $500 $100 $200 $300 $400 $500 $100 $200 $300.
Signatures of Magnetic Field Structure in Planetary Nebulae P. J. Huggins, New York University PNe as MHD systems PNe as MHD systems.
ARE MAGNETIC FIELDS AND OUTFLOWS ALIGNED IN PROTOSTELLAR CORES? Chat Hull University of California, Berkeley Radio Astronomy Laboratory 4 April 2013 Institute.
GASKAP The Galactic ASKAP Survey On behalf of the GASKAP team Dr Andrew Walsh.
Great Barriers in High Mass Star Formation, Townsville, Australia, Sept 16, 2010 Patrick Koch Academia Sinica, Institute of Astronomy and Astrophysics.
The Polar Fields Seen in 17 GHz Microwave Flux and with Magnetographs Leif Svalgaard Stanford University 6 January, 2012.
ARE MAGNETIC FIELDS AND OUTFLOWS ALIGNED IN PROTOSTELLAR CORES? Chat Hull University of California, Berkeley Radio Astronomy Laboratory 28 September 2013.
NoRH Observations of Prominence Eruption Masumi Shimojo Nobeyama Solar Radio Observatory NAOJ/NINS 2004/10/28 Nobeyama Symposium SeiSenRyo.
CARMA Large Area Star-formation SurveY  Completing observations of 5 regions of square arcminutes with 7” angular resolution in the J=1-0 transitions.
Cosmic magnetism ( KSP of the SKA)‏ understand the origin and evolution of magnetism in the Galaxy, extragalactic objects, clusters and inter-galactic/-cluster.
Allen et al. (2005) Johnstone et al. (2000). Oph B2 850  m continuum (JCMT) NH 3 (1,1) int. intensity (GBT) NH 3 emission shows excellent (but not perfect)
From Clouds to Cores: Magnetic Field Effects on the Structure of Molecular Gas Shantanu Basu University of Western Ontario, Canada Collaborators: Takahiro.
A Brief discussion of interstellar HI structure with special reference to filaments Gerrit Verschuur Physics Department, University of Memphis.
The core of what I am going to talk about is shown
Some atomic physics u H I, O III, Fe X are spectra –Emitted by u H 0, O 2+, Fe 9+ –These are baryons u For absorption lines there is a mapping between.
Are magnetic fields and outflows aligned in protostellar cores?
1. Twist propagation in Hα surges Patricia Jibben and Richard C. Canfield 2004, ApJ, 610, Observation of the Molecular Zeeman Effect in the G Band.
Discussion Section Falgarone, Reynolds, Cox, Meyer, Spangler, Deshpande, Goss, Stanimirovic, Heiles BUT….. It’s more fun to do this together!
OH maser sources in W49N: probing differential anisotropic scattering with Zeeman pairs desh Raman Research Institute, Bangalore + Miller Goss, Eduardo.
AGN: Linear and Circular Polarization
EVLA Observations of the Low Density Component of the Cold Neutral Medium and Limits on the Thermally-Unstable Warm Neutral Medium Miller Goss, Ayesha.
CO Spectral Line Energy Distributions in Orion Sources: Templates for Extragalactic Observations Nick Indriolo & Ted Bergin University of Michigan June.
Galactic Legacy Projects Naomi McClure-Griffiths Australia Telescope National Facility, CSIRO NRAO Legacy Projects Meeting, 17 May 2006.
A Survey of the Global Magnetic Fields of Giant Molecular Clouds Giles Novak, Northwestern University Instrument: SPARO Collaborators: P. Calisse, D. Chuss,
VLBA Observations of AU- scale HI Structures Crystal Brogan (NRAO/NAASC) W. M. Goss (NRAO), T. J. W. Lazio (NRL) SINS Meeting, Socorro, NM, May 21, 2006.
Is the Inner Radio Jet of BL Lac Precessing? R. L. Mutel University of Iowa Astrophysics Seminar 17 September 2003.
Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array NRAO Instruments Provide.
Polarized Light from Star-Forming Regions
OH MASERS in THE MILKY WAY and BEYOND. There is a sense that field DIRECTIONS in the small, highly concentrated OH masers tend to mirror the LARGE-SCALE.
A Fan Beam Model for Radio Pulsars Hongguang Wang (王洪光) Center for Astrophysics, Guangzhou University 广州大学天体物理中心 Fast Pulsar Symposium 4.
HCO+ in the Helix Nebula
A Cold, Nearby Cloud in the Local Bubble
Thin, Cold Strands of Hydrogen in the Riegel-Crutcher Cloud
W3 Preliminary Polarimetry Data
Radio Astronomy -- Other Than ALFA Surveys
T.G.Arshakian MPI für Radioastronomie (Bonn)
Faraday Rotation Measure Gradients From A Helical Magnetic Field In 3C273 Zavala & Taylor 2005, ApJ, 626, L73.
Transition Observing and Science
Shane O’Sullivan University College Cork
EVN observations of OH maser burst in OH
Presentation transcript:

UC Berkeley GBT Measurements of the Zeeman Effect in the Eridanus/Orion Region Tim Robishaw Carl Heiles

The Orion Molecular Cloud Complex Heiles 1997 Hat Creek 85 ft 9 years of Zeeman data Distance ~535 pc Bower, Sandstrom, Goldston in prep.

Starlight Polarization Orientations Breger 1976, Vrba et al. 1988

Starlight Polarization Orientations Breger 1976, Vrba et al. 1988

The GBT Is a Zeeman Machine! Off-Axis Design Minimizes Blockage Minimizes Sidelobes!!

The GBT Is a Zeeman Machine!

Verschuur’s Indictment 1993 BAAS BAAS ApJ 451: ApJ 451: 645

Verschuur’s Indictment

3 hours

The GBT Hat Creek 85 foot 3 hours

OH

Summary The GBT can be used as a Zeeman detector Apparent HI self-absorption samples the molecular component of the filament LOS B field measured in emission changes sign across axis of filament –Detections consistent with previous HI emission measurements: they were reliable! Field reverses within central half-degree of filament (~ 4.5 pc) Highest resolution data for modeling of helical magnetic field structure