English
 
User Manual Privacy Policy Disclaimer Contact us
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT

Released

Journal Article

[CII] emission and star formation in late-type galaxies

MPS-Authors
/persons/resource/persons30895

Pierini,  D.
Prof. Heinrich J. Völk, Emeriti, MPI for Nuclear Physics, Max Planck Society;

/persons/resource/persons31117

Tuffs,  R. J.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

/persons/resource/persons31141

Völk,  H. J.
Prof. Heinrich J. Völk, Emeriti, MPI for Nuclear Physics, Max Planck Society;

Locator
There are no locators available
Fulltext (public)
There are no public fulltexts available
Supplementary Material (public)
There is no public supplementary material available
Citation

Pierini, D., Leech, K. J., Tuffs, R. J., & Völk, H. J. (2001). [CII] emission and star formation in late-type galaxies. Astrophysics and Space Science, 276(2-4), 815-821. Retrieved from http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2001Ap%26SS.276.815P&db_key=AST&high=3fd59969ac20031.


Cite as: http://hdl.handle.net/11858/00-001M-0000-0011-85B9-7
Abstract
A linear correlation between the ratio of the [CII(P-2(3/2) --> (2) P-1/2)] line intensity to the [(CO)-C-12(J : 1 --> 0)] line emission, I-CII/I-CO and the H-alpha equivalent width (EW) is found, over the range 2-71 Angstrom in H-alpha EW, for a sample of 21 late-type galaxies. The latter is comprised of an optically selected sample of 12 normal Virgo Cluster spiral galaxies with [CII] detections obtained by us with ISOLWS, plus nine late-type galaxies with higher star formation rates (SFRs), for which [CII] data and, especially, H-alpha EW data are available in the literature. As a result we infer I-CII/I-CO to be a reliable tracer of the current mass-normalized global SFR for non-starburst spiral galaxies. Moreover, the ratio of the [CII] line to the total far-infrared (FIR) continuum intensity, I-CII/I-FIR, is found to decrease from similar to0.5% to similar to0.1% with decreasing SFR which we propose is due to a '[CII]-quiet' component of I-FIR from dust heated by the general interstellar radiation field (ISRF). The more 'quiescent' galaxies in the sample have values of I-CII/I-CO different from those observed in 'compact' Galactic interstellar regions. Their [CII]-emission is interpreted to be dominated by diffuse regions of the interstellar medium (ISM). For normal 'star-forming' galaxies the diffuse component of the [CII] emission is estimated to account for at least 50% of the total.