Probing star formation and ISM properties using galaxy disk inclination. I. 
Evolution in disk opacity since z 0.7

Leslie, S. K.; Sargent, M. T.; Schinnerer, E.; Groves, B.; van der Wel, A.; Zamorani, G.; Fudamoto, Y.; Lang, P.; Smolčić, V.

Item

ITEM ACTIONSEXPORT

Add to Basket

Local TagsRelease HistoryDetailsSummary

Released

Journal Article

Probing star formation and ISM properties using galaxy disk inclination. I. Evolution in disk opacity since z 0.7

MPS-Authors

Leslie, S. K.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Sargent, M. T.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Schinnerer, E.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Groves, B.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

van der Wel, A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Zamorani, G.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Fudamoto, Y.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Lang, P.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Smolčić, V.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

External Resource

https://ui.adsabs.harvard.edu/abs/2018A&A...615A...7L
(Any fulltext)

Fulltext (restricted access)

There are currently no full texts shared for your IP range.

Fulltext (public)

There are no public fulltexts stored in PuRe

Supplementary Material (public)

There is no public supplementary material available

Citation

Leslie, S. K., Sargent, M. T., Schinnerer, E., Groves, B., van der Wel, A., Zamorani, G., et al. (2018). Probing star formation and ISM properties using galaxy disk inclination. I. Evolution in disk opacity since z 0.7. Astronomy and Astrophysics, 615.

Cite as: https://hdl.handle.net/21.11116/0000-0005-CC92-0

Abstract

Disk galaxies at intermediate redshift (z 0.7) have been found in previous work to display more optically thick behaviour than their local counterparts in the rest-frame B-band surface brightness, suggesting an evolution in dust properties over the past 6 Gyr. We compare the measured luminosities of face-on and edge-on star-forming galaxies at different wavelengths (Ultraviolet (UV), mid-infrared (MIR), far- infrared (FIR), and radio) for two well-matched samples of disk- dominated galaxies: a local Sloan Digital Sky Survey (SDSS)-selected sample at z 0.07 and a sample of disks at z 0.7 drawn from Cosmic Evolution Survey (COSMOS). We have derived correction factors to account for the inclination dependence of the parameters used for sample selection. We find that typical galaxies are transparent at MIR wavelengths at both redshifts, and that the FIR and radio emission is also transparent as expected. However, reduced sensitivity at these wavelengths limits our analysis; we cannot rule out opacity in the FIR or radio. Ultra-violet attenuation has increased between z 0 and z 0.7, with the z 0.7 sample being a factor of 3.4 more attenuated. The larger