학술논문
Differential attenuation in star-forming galaxies at 0.3 $\lesssim$ $z$ $\lesssim$ 1.5 in the SHARDS/CANDELS field
Document Type
Working Paper
Author
Rodríguez-Muñoz, L.; Rodighiero, G.; Pérez-González, P. G.; Talia, M.; Baronchelli, I.; Morselli, L.; Renzini, A.; Puglisi, A.; Grazian, A.; Zanella, A.; Mancini, C.; Feltre, A.; Romano, M.; García, A. Vidal; Franceschini, A.; Pampliega, B. Alcalde; Cassata, P.; Costantin, L.; Sánchez, H. Domínguez; Espino-Briones, N.; Iani, E.; Koekemoer, A.; Lumbreras-Calle, A.; Rodríguez-Espinosa, J. M.
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Subject
Language
Abstract
We use a sample of 706 galaxies, selected as [OII]$\lambda$3727 ([OII]) emitters in the Survey for High-$z$ Absorption Red and Dead Sources (SHARDS) on the CANDELS/GOODS-N field, to study the differential attenuation of the nebular emission with respect to the stellar continuum. The sample includes only galaxies with a counterpart in the infrared and $\mathrm{log}_{10}(M_{*}/\mathrm{M}_{\odot})$ $>$ 9, over the redshift interval 0.3 $\lesssim$ $z$ $\lesssim$ 1.5. Our methodology consists in the comparison of the star formation rates inferred from [OII] and H$\alpha$ emission lines with a robust quantification of the total star-forming activity (${SFR}_{\mathrm{TOT}}$) that is independently estimated based on both infrared and ultraviolet (UV) luminosities. We obtain $f$$=$$E(B-V)_{\mathrm{stellar}}$/$E(B-V)_{\mathrm{nebular}}$ $=$ 0.69$^{0.71}_{0.69}$ and 0.55$^{0.56}_{0.53}$ for [OII] and H$\alpha$, respectively. Our resulting $f$-factors display a significant positive correlation with the UV attenuation and shallower or not-significant trends with the stellar mass, the $SFR_{\mathrm{TOT}}$, the distance to the main sequence, and the redshift. Finally, our results favour an average nebular attenuation curve similar in shape to the typical dust curve of local starbursts.
Comment: 23 pages, 10 figures, 3 tables; accepted for publication in MNRAS
Comment: 23 pages, 10 figures, 3 tables; accepted for publication in MNRAS