chris wilson mcmaster university

Chris Wilson McMaster University

•  W. Gear, S. Madden; S. Eales, A. Boselli, C. Wilson

R Auld, M Baes, M Barlow, G Bendo, J Bock, M Bradford, V Buat, N Castro Rodriguez, P Chanial, S Charlot, D Clements, D Cormier, L Cortese, J Davies, E Dwek, D Elbaz, M Galametz, F Galliano, J Glenn, H Gomez, M Griffin, S Hony, K Isaak, L Levenson, N Lu, B O'Halloran, K Okumura, S Oliver, M Page, P Panuzzo, A Papageorgiou, T Parkin, I Perez Fournon, M Smith, M Pohlen, N Rangwala, E Rigby, H Roussel, A Rykala, N Sacchi , M Sauvage, B Schulz, M Schirm, L Spinoglio, J Stevens, M Symeonidis, M Vaccari, L Vigroux, H Wozniak, G Wright, W Zeilinger

•  Introduction and motivation •  CO ladder in M82 •  CO and water in M82 (HIFI team) •  Rich chemistry in Arp 220 •  Water in Mrk 231 (HerCULES survey) •  Mapping far-infrared lines in Centaurus A •  Links to ALMA

•  Weiss et al. 2005; evidence for diffuse gas surrounding a high pressure central region

Figures from Weiss et al. 2007 (first NAASC conference)

•  70-80% predominantly starbursts •  20-30% predominantly AGN

Genzel et al. 1998

M51 M81 N891

N1068

M51 M81 N891 N2403

M83 M82 N4038/9 CenA

N1068 N4151 N205 N4125

Arp220

250/350/500 µm images by L. Cortese

•  Spectrum from central pixel scaled to sample a 43” beam at all wavelengths

•  Best-fit model has T=545 K and 1.2x107 Mo of warm H2 gas –  warm H2 also seen directly (Beirao et al. 2008)

•  Low-J lines dominated by cold gas (e.g. Ward et al. 2003)

Loenen et al. 2010

A. Weiβ et al. 2010

Arp 220: the nearest ultraluminous infrared galaxy

Wilson et al 2006 (HST ACS image)

•  Large masses of molecular gas within R<2 kpc •  Broad line widths imply large dynamical masses •  Rotation curves can be quite complex

Arp 220 (Sakamoto et al. 2008)

Rangwala et al., in prep.

Rangwala et al., in prep. Traces turbulent dissipation, Falgarone et al., Goddard et al. 2010

Rangwala et al., in prep. Most important H2O+ lines; may be blended with OH+ and H2O lines

Rangwala et al., in prep.

(awaiting JPL confirmation of frequency)

Arp 220 M82

Gonzalez-Alfonso et al., 2010

•  Fit dust continuum with 3 components

•  Water appears to be radiatively excited

•  Water from both compact and extended regions

(Gonzalez-Alfonso et al., 2010)

•  Continuum emission from disk but also from radio jet at longest SPIRE wavelengths

•  Central source variable in mm (Israel et al. 2008)

SPIRE 250, 350, 500 micron GALEX UV

Map is dust temperature (except AGN and jets; contamination from non-thermal emission); T. Parkin et al., in prep.

ALMA Band 9 ALMA Band 8

ALMA Band 10

•  Herschel: –  Strong molecular and atomic emission lines seen

in M82, including hot H2 gas –  Arp 220: detection of thermal water in emission in

an external galaxy along with a wealth of other emission/absorption lines

–  [NII] observations of Cen A show promise of mapping mode with SPIRE FTS

We anticipate additional exciting new results from these and future observations of very nearby galaxies!