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ALMA: HI and He+ Lines and Dust in Starbursts, AGN and High-z Galaxies

Published online by Cambridge University Press:  25 July 2014

Nick Scoville*
Affiliation:
Astronomy 249-17, California Institute of Technology, Pasadena, CA 91125, USA email: nzs@astro.caltech.edu
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Abstract

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We describe preliminary results for two ALMA projects – 1) imaging the HCN(4-3) line and H26α lines in Arp 220 and 2) measurements of the dust continuum in a sample of 107 high redshift galaxies to probe the evolution of the ISM masses. The HCN observations in Arp 220 at 1/2″ resolution provide the first high resolution imaging of the dense star forming gas in this prototypical ULIRG. The HCN is seen in two clearly delineated, counter-rotating disks. The H26α line is a definitive probe of the star formation rate in Arp 220, avoiding obscuration by dust and contamination by AGN luminosity contributions. In the second project, the remarkable continuum sensitivity of ALMA in Band 7 is used to measure the long wavelength Rayleigh-Jeans tail of the dust emission from a sample of 120 galaxies in COSMOS at z = 0.3 to 2.2, providing estimates for the dust masses and hence their ISM masses. This technique will enable measurements for hundreds of galaxies at high-z with observations of typically ~10 min per galaxy. This is in contrast to CO line imaging which typically requires a few hours per galaxy even with the sensitivity of ALMA. The dust-based mass estimates also avoid the uncertainties associated with the CO-to-H2 conversion factor.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2014 

References

Draine, B. T., et al. 2007, ApJ 663, 866CrossRefGoogle Scholar
Eales, S., et al. 2012, ApJ 761, 168Google Scholar
Erb, D. K., Shapley, A. E., Pettini, M., Steidel, C. C., Reddy, N. A., & Adelberger, K. L. 2006, ApJ 644, 813Google Scholar
Planck Collaboration 2011a, A&A 536, A21Google Scholar
Planck Collaboration 2011b, A&A 536, A25Google Scholar
Sakamoto, K., Scoville, N. Z., Yun, M. S., Crosas, M., Genzel, R., & Tacconi, L. J. 1999, ApJ 514, 68CrossRefGoogle Scholar
Scoville, N. & Murchikova, L. 2013, ApJ 779, 75Google Scholar
Scoville, N. Z. 2012, ArXiv e-printsGoogle Scholar
Scoville, N. Z., et al. 2014, ApJ 000, 000Google Scholar
Tacconi, L. J., et al. 2013, ApJ 768, 74CrossRefGoogle Scholar