Hostname: page-component-cd9895bd7-gvvz8 Total loading time: 0 Render date: 2024-12-25T18:25:59.462Z Has data issue: false hasContentIssue false
  • English
  • Français

Average radio spectral energy distribution of highly star-forming galaxies

Published online by Cambridge University Press:  08 May 2018

K. Tisanić ,
V. Smolčić ,
J. Delhaize ,
M. Novak ,
H. Intema ,
I. Delvecchio ,
E. Schinnerer  and
G. Zamorani
K. Tisanić
Affiliation:
Department of Physics, Faculty of Science, University of Zagreb, Bijenička cesta 32, 10000 Zagreb, Croatia, email: ktisanic@phy.hr
V. Smolčić
Affiliation:
Department of Physics, Faculty of Science, University of Zagreb, Bijenička cesta 32, 10000 Zagreb, Croatia, email: ktisanic@phy.hr
J. Delhaize
Affiliation:
Department of Physics, Faculty of Science, University of Zagreb, Bijenička cesta 32, 10000 Zagreb, Croatia, email: ktisanic@phy.hr
M. Novak
Affiliation:
Department of Physics, Faculty of Science, University of Zagreb, Bijenička cesta 32, 10000 Zagreb, Croatia, email: ktisanic@phy.hr
H. Intema
Affiliation:
Leiden Observatory, Leiden University, Niels Bohrweg 2, 2333 CA Leiden, The Netherlands
I. Delvecchio
Affiliation:
Department of Physics, Faculty of Science, University of Zagreb, Bijenička cesta 32, 10000 Zagreb, Croatia, email: ktisanic@phy.hr
E. Schinnerer
Affiliation:
MPI for Astronomy, Königstuhl 17, D-69117, Heidelberg, Germany
G. Zamorani
Affiliation:
INAF-Osservatorio Astronomico di Bologna, via Gobetti 93/3, 40129, Bologna, Italy
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The infrared-radio correlation (IRRC) offers a way to assess star formation from radio emission. Multiple studies found the IRRC to decrease with increasing redshift. This may in part be due to the lack of knowledge about the possible radio spectral energy distributions (SEDs) of star-forming galaxies. We constrain the radio SED of a complete sample of highly star-forming galaxies (SFR > 100 M⊙/ yr) based on the VLA-COSMOS 1.4 GHz Joint and 3 GHz Large Project catalogs. We reduce archival GMRT 325 MHz and 610 MHz observations, broadening the rest-frame frequency range to 0.3-15 GHz. Employing survival analysis and fitting a double power law SED, we find that the slope steepens from a spectral index of α1 = 0.51±0.04 below 4.5 GHz to α2 = 0.98±0.07 above 4.5 GHz. Our results suggest that the use of a K-correction assuming a single power-law radio SED for star forming galaxies is likely not the root cause of the IRRC trend.

Keywords

Galaxy: evolutiongalaxies: statisticsradio continuum: galaxies
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S333: Peering towards Cosmic Dawn , October 2017 , pp. 191 - 194
Copyright
Copyright © International Astronomical Union 2018 

References

Bondi, M., Ciliegi, P., Zamorani, G., et al. 2003, A&A, 403, 857Google Scholar
Chabrier, G., 2003, PASP, 115, 763Google Scholar
Calistro Rivera, G., Williams, W. L., Hardcastle, M. J., et al. 2017, MNRAS, 469, 3468CrossRefGoogle Scholar
Clemens, M. S., Vega, O., Bressan, A., et al. 2008, A&A, 477, 95Google Scholar
Condon, J. J., 1992, ARA&A, 30, 575Google Scholar
Delhaize, J., Smolčić, V., Delvecchio, I., et al. 2017, A&A, 602, A4Google Scholar
Delvecchio, I., Smolčić, V., Zamorani, G., et al. 2017, A&A, 602, A3Google Scholar
Galvin, T., Seymour, N, Marvil, J, et al. 2017, arXiv:1710.01967Google Scholar
Hales, C. A., Murphy, T., Curran, J. R., et al. 2012, MNRAS, 425, 979Google Scholar
Helou, G., Soifer, B. T., & Rowan-Robinson, M., 1985, ApJ, 298, L7CrossRefGoogle Scholar
Intema, H. T., Jagannathan, P., Mooley, K. P., & Frail, D. A., 2017, A&A, 598, A78Google Scholar
Ivison, R. J., Magnelli, B., Ibar, E., et al. 2010, A&A, 518, L31Google Scholar
Kennicutt, R. C., Jr,1998, ARA&A, 36, 189Google Scholar
Kennicutt, R. C. Jr, 1998, ApJ, 498, 541CrossRefGoogle Scholar
Leroy, A. K., Evans, A. S., Momjian, E., et al. 2011, ApJ, 739, L25Google Scholar
Magnelli, B., Ivison, R. J., Lutz, D., et al. 2015, A&A, 573, A45Google Scholar
Schinnerer, E., Smolčić, V., Carilli, C. L., et al. 2007, ApJS, 172, 46CrossRefGoogle Scholar
Schinnerer, E., Sargent, M. T., Bondi, M., et al. 2010, ApJS, 188, 384Google Scholar
Scoville, N., Aussel, H., Brusa, M., et al. 2007, ApJS, 172, 1Google Scholar
Smolčić, V., Novak, M., Bondi, M., et al. 2017, A&A, 602, A1Google Scholar
Smolčić, V., Delvecchio, I., Zamorani, G., et al. 2017, A&A, 602, A2Google Scholar
Tabatabaei, F. S., Schinnerer, E., Krause, M., et al. 2017, ApJ, 836, 185Google Scholar
van der Kruit, P. C., 1971, A&A, 15, 110Google Scholar