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

Slides:

Advertisements

Similar presentations

Infall and Rotation around Young Stars Formation and Evolution of Protoplanetary Disks Michiel R. Hogerheijde Steward Observatory The University of Arizona.

Advertisements

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

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.

Observations and Magnetic Field Modeling of CMEs’ Source Regions Yingna Su Harvard-Smithsonian Center for Astrophysics Collaborators: Adriaan van Ballegooijen,

How do stars get their masses? and A short look ahead Phil Myers CfA Dense Core LXV Newport, RI October 23, 2009.

Segunda parte. IRAS Vela Shell IRAS 100µ (30° x 30°)  Pup  Vel Feitzinger & Stüwe 1984 Fig. 1 14°x14°

circular polarizer orthomode transducer

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

Polarization 101 Absorption Emission Scattering. PolarizationPolarization of Background Starlight.

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

“Magnets in Space” Alyssa A. Goodman Harvard-Smithsonian Center for Astrophysics.

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

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

Submillimeter Astronomy in the era of the SMA, 2005, Cambridge, MA Observations of Extragalactic Star Formation in [CI] (370  m) and CO J=7-6 T. Nikola.

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

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.

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.

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),

Polarization Surveys with the DRAO 26-m Telescope at 1.4 GHz Maik Wolleben, T. Landecker, O. Davison Dominion Radio Astrophysical Observatory W. Reich,

10 January 2006AAS EVLA Town Hall Meeting1 The EVLA: A North American Partnership The EVLA Project on the Web

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.

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

AAS ALMA Town Meeting, Washington, DC 2006 Community Input into the operations of the Global ALMA project and North American ALMA Science Center.

Massive Star Formation: The Role of Disks Cassandra Fallscheer In collaboration with: Henrik Beuther, Eric Keto, Jürgen Sauter, TK Sridharan, Sebastian.

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.

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

The properties of starless cores in intermediate-/high-mass protoclusters Francesco Fontani European Southern Observatory (ESO) Institut de RadioAstronomie.

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.

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.

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

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)

ASIAA Interferometry Summer School – 2006 Introduction – Radio Astronomy Tatsuhiko Hasegawa (ASIAA) 1. Atmospheric window to the electromagnetic waves.

Kashi1 Radio continuum observations of the Sombrero galaxy NGC4594 (M104) and other edge-on spirals Marita Krause MPIfR, Bonn Michael Dumke ESO,

Magnetic fields in Planetary and Proto Planetary

From Clouds to Cores: Magnetic Field Effects on the Structure of Molecular Gas Shantanu Basu University of Western Ontario, Canada Collaborators: Takahiro.

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 Observations of proto-planetary disks I HD – P.I. Casassus 2013 Nature 493, 191 Herbig Ae star 140 pc, 2 Myr, 1.9 M , disk mass 0.1 M  Left:

Philamentary Structure and Velocity Gradients in the Orion A Cloud

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)

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

Strength and Structure of the Coronal Magnetic Field Steven R. Spangler University of Iowa.

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

CO Spectral Line Energy Distributions in Orion Sources: Templates for Extragalactic Observations Nick Indriolo & Ted Bergin University of Michigan June.

Master in Astrophysics, Particle Physics, and Cosmology Academic year Fall semester Mon, Tue, Wed, 16:10 – 17:30, room N07P Stellar Structure and.

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.

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.

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

The Structures on Sub-Jeans Scales, Fragmentation, and the Chemical Properties in Two Extremely Dense Orion Cores Zhiyuan Ren, Di Li (NAOC) and Nicolas.

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

Cooling, AGN Feedback and Star Formation in Simulated Cool-Core Galaxy Clusters Yuan Li University of Michigan Collaborators: Greg L. Bryan (Columbia)

Galactic science with the Origins Space Telescope

Polarization in forming stars Probing small scales with carma

Galactic Magnetism with SKA: Primordial Origin of BSS, ASS, Ring &Vertical Fields Y. Sofue1,2, M. Machida3, T. Kudoh3, H. Nakanishi1 (1. Kagoshima U.,

ARTIST Adaptive Radiative Transfer Innovations for Submillimeter Telescopes J. JØrgensen1, F. Bertoldi5, C. Brinch1, P. Frau3, J.M. Girart3, M. Hogerheijde2,

Welcome K. Y. Lo Director, NRAO

Presentation transcript:

CARMA observations of magnetic fields in star-forming filaments Chat Hull Jansky Fellow — Harvard-Smithsonian Center for Astrophysics National Radio Astronomy Observatory AAS 225 Session 110: Star Formation I Seattle, WA 5 January 2015 Photo: Chat Hull (Harvard/NRAO)

2Chat Hull – AAS Seattle – 5 January 2015 TADPOL collaboration UC Berkeley Chat Hull (PI), Dick Plambeck, Mel Wright, Carl Heiles University of Maryland Marc Pound, Alberto Bolatto, Katherine Jameson, Lee Mundy Caltech John Carpenter, James Lamb, Nikolaus Volgenau University of Illinois, Urbana-Champaign Leslie Looney, Dick Crutcher, Nick Hakobian Other Geoff Bower (ASIAA), Thushara Pillai (Bonn), Dan Marrone (Arizona), Meredith Hughes (Wesleyan), John Vaillancourt & Göran Sandell (USRA-SOFIA), John Tobin (NRAO), Ian Stephens (BU), Jason Fiege & Erica Franzmann (Manitoba), Martin Houde (UWO, Caltech), Brenda Matthews (NRC-CNRC), Woojin Kwon (SRON)

3Chat Hull – AAS Seattle – 5 January 2015 Outline Brief filamentary introduction Magnetized filaments – High-mass: NGC 7538 – Low-mass: Ser-emb 8, 8(N) Simulations

4Chat Hull – AAS Seattle – 5 January 2015 Pereyra & Magalhães pc E,B Musca dark cloud B-fields in large- scale filaments

5Chat Hull – AAS Seattle – 5 January 2015 How do different kinds of filaments form? Low- vs. high-mass objects Large vs. small scales

6Chat Hull – AAS Seattle – 5 January 2015 High-mass star-forming region NGC 7538

7Chat Hull – AAS Seattle – 5 January 2015 NGC 7538 Fallscheer pc

8Chat Hull – AAS Seattle – 5 January 2015 NGC 7538 Wright, Hull+2014, ApJ, 796, pc

9Chat Hull – AAS Seattle – 5 January 2015 Frau+2014 NGC pc

10Chat Hull – AAS Seattle – 5 January 2015 NGC 7538 Hull+2014, ApJS, 213, pc Small-scale B-field in filament doesn’t reflect original field

11Chat Hull – AAS Seattle – 5 January 2015 NGC 7538 Frau pc Magnetized filament is shaped by a combination of infall and outflow

12Chat Hull – AAS Seattle – 5 January 2015 Low-mass star-forming cores Ser-emb 8, 8(N)

13Chat Hull – AAS Seattle – 5 January 2015 Ser-emb 8, 8(N) Hull+2014, ApJS, 213, 13 This filament is small! (d ~ 0.01 pc) How did this filament form? What does the B-field look like between the cores? 0.01 pc

14Chat Hull – AAS Seattle – 5 January pc Summary (1/2) Chen & Ostriker 2014 Soler+2013 Simulations & observations

15Chat Hull – AAS Seattle – 5 January 2015 Summary (2/2) Comparison of new dust polarization data with multi-scale, observable MHD simulations will show which processes dominate at small scales High-mass: B-fields in filaments may not reflect original configuration, and can be created by outflows, infall, etc. Low-mass: numerous formation scenarios. But what about the smallest scales? Even higher resolution ALMA observations will clear up (or further complicate?!) the situation NGC 7538 filament 2014 ApJ, 796, 112 TADPOL data release 2014 ApJS, 213, 153 TADPOL outflows/B-fields: ApJ, 768, 159

16Chat Hull – AAS Seattle – 5 January 2015 Fin