1. 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)

2. 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)

3. 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

4. 4Chat Hull – AAS Seattle – 5 January 2015 Pereyra & Magalhães 2004 10 pc E,B Musca dark cloud B-fields in large- scale filaments

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

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

7. 7Chat Hull – AAS Seattle – 5 January 2015 NGC 7538 Fallscheer+2013 10 pc

8. 8Chat Hull – AAS Seattle – 5 January 2015 NGC 7538 Wright, Hull+2014, ApJ, 796, 112 0.1 pc

9. 9Chat Hull – AAS Seattle – 5 January 2015 Frau+2014 NGC 7538 0.1 pc

10. 10Chat Hull – AAS Seattle – 5 January 2015 NGC 7538 Hull+2014, ApJS, 213, 13 0.1 pc Small-scale B-field in filament doesn’t reflect original field

11. 11Chat Hull – AAS Seattle – 5 January 2015 NGC 7538 Frau+2014 0.1 pc Magnetized filament is shaped by a combination of infall and outflow

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

13. 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

14. 14Chat Hull – AAS Seattle – 5 January 2015 1 pc Summary (1/2) Chen & Ostriker 2014 Soler+2013 Simulations & observations

15. 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

16. 16Chat Hull – AAS Seattle – 5 January 2015 Fin