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Dust and gas power spectrum in M 33 (HERM33ES)

Combes, F. and Boquien, M. and Kramer, C. and Xilouris, E. M. and Bertoldi, F. and Braine, J. and Buchbender, C. and Calzetti, D. and Gratier, P. and Israel, F. and Koribalski, B. and Lord, S. and Quintana-Lacaci, G. and Relaño, M. and Röllig, M. and Stacey, G. and Tabatabaei, F. S. and Tilanus, R. P. J. and van der Tak, F. and van der Werf, P. and Verley, S. (2012) Dust and gas power spectrum in M 33 (HERM33ES). Astronomy and Astrophysics, 539 . Art. No. A67. ISSN 0004-6361. http://resolver.caltech.edu/CaltechAUTHORS:20120608-142718745

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Abstract

Power spectra of deprojected images of late-type galaxies in gas or dust emission are very useful diagnostics of the dynamics and stability of their interstellar medium. Previous studies have shown that the power spectra can be approximated as two power laws, a shallow one on large scales (larger than 500 pc) and a steeper one on small scales, with the break between the two corresponding to the line-of-sight thickness of the galaxy disk. The break separates the 3D behavior of the interstellar medium on small scales, controlled by star formation and feedback, from the 2D behavior on large scales, driven by density waves in the disk. The break between these two regimes depends on the thickness of the plane, which is determined by the natural self-gravitating scale of the interstellar medium. We present a thorough analysis of the power spectra of the dust and gas emission at several wavelengths in the nearby galaxy M 33. In particular, we use the recently obtained images at five wavelengths by PACS and SPIRE onboard Herschel. The wide dynamical range (2–3 dex in scale) of most images allows us to clearly determine the change in slopes from −1.5 to −4, with some variations with wavelength. The break scale increases with wavelength from 100 pc at 24 and 100 μm to 350 pc at 500 μm, suggesting that the cool dust lies in a thicker disk than the warm dust, perhaps because of star formation that is more confined to the plane. The slope on small scales tends to be steeper at longer wavelength, meaning that the warmer dust is more concentrated in clumps. Numerical simulations of an isolated late-type galaxy, rich in gas and with no bulge, such as M 33, are carried out to better interpret these observed results. Varying the star formation and feedback parameters, it is possible to obtain a range of power spectra, with two power-law slopes and breaks, that nicelybracket the data. The small-scale power-law does indeed reflect the 3D behavior of the gas layer, steepening strongly while the feedback smoothes the structures by increasing the gas turbulence. M 33 appears to correspond to a fiducial model with an SFR of ~ 0.7 M_⊙/yr, with 10% supernovae energy coupled to the gas kinematics.


Item Type:Article
Related URLs:
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http://dx.doi.org/10.1051/0004-6361/201118282DOIArticle
http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/201118282&Itemid=129PublisherArticle
ORCID:
AuthorORCID
Calzetti, D.0000-0002-5189-8004
van der Werf, P.0000-0001-5434-5942
Additional Information:© 2012 ESO. Article published by EDP Sciences. Received 16 October 2011; Accepted 17 January 2012. Published online 27 February 2012. We warmly thank the anonymous referee for his/her constructive comments and suggestions. We made use of the NASA/IPAC Extragalactic Database (NED). Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
Subject Keywords:galaxies: structure; galaxies: spiral; galaxies: ISM; Local Group; galaxies: general; galaxies: individual: M 33
Record Number:CaltechAUTHORS:20120608-142718745
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20120608-142718745
Official Citation:Dust and gas power spectrum in M 33 (HERM33ES) F. Combes, M. Boquien, C. Kramer, E. M. Xilouris, F. Bertoldi, J. Braine, C. Buchbender, D. Calzetti, P. Gratier, F. Israel, B. Koribalski, S. Lord, G. Quintana-Lacaci, M. Relaño, M. Röllig, G. Stacey, F. S. Tabatabaei, R. P. J. Tilanus, F. van der Tak, P. van der Werf and S. Verley A&A 539 A67 (2012) DOI: http://dx.doi.org/10.1051/0004-6361/201118282
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:31856
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:08 Jun 2012 23:10
Last Modified:18 Aug 2017 00:17

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