Dust Attenuation Curves at z similar to 0.8 from LEGA-C: Precise Constraints on the Slope and 2175 angstrom Bump Strength
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Dust Attenuation Curves at z similar to 0.8 from LEGA-C : Precise Constraints on the Slope and 2175 angstrom Bump Strength. / Barisic, Ivana; Pacifici, Camilla; van der Wel, Arjen; Straatman, Caroline; Bell, Eric F.; Bezanson, Rachel; Brammer, Gabriel; D'Eugenio, Francesco; Franx, Marijn; van Houdt, Josha; Maseda, Michael V.; Muzzin, Adam; Sobral, David; Wu, Po-Feng.
In: Astrophysical Journal, Vol. 903, No. 2, 146, 01.11.2020.Research output: Contribution to journal › Journal article › Research › peer-review
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TY - JOUR
T1 - Dust Attenuation Curves at z similar to 0.8 from LEGA-C
T2 - Precise Constraints on the Slope and 2175 angstrom Bump Strength
AU - Barisic, Ivana
AU - Pacifici, Camilla
AU - van der Wel, Arjen
AU - Straatman, Caroline
AU - Bell, Eric F.
AU - Bezanson, Rachel
AU - Brammer, Gabriel
AU - D'Eugenio, Francesco
AU - Franx, Marijn
AU - van Houdt, Josha
AU - Maseda, Michael V.
AU - Muzzin, Adam
AU - Sobral, David
AU - Wu, Po-Feng
PY - 2020/11/1
Y1 - 2020/11/1
N2 - We present a novel approach to measure the attenuation curves of 485 individual star-forming galaxies with M-* > 10(10) M-circle dot based on deep optical spectra from the VLT/VIMOS LEGA-C survey and multiband photometry in the COSMOS field. Most importantly, we find that the attenuation curves in the rest-frame 3000-4500 angstrom range are typically almost twice as steep as the Milky Way, LMC, SMC, and Calzetti attenuation curves, which is in agreement with recent studies of the integrated light of present-day galaxies. The attenuation at 4500 angstrom and the slope strongly correlate with the galaxy inclination: face-on galaxies show less attenuation and steeper curves compared to edge-on galaxies, suggesting that geometric effects dominate observed variations in attenuation. Our new method produces 2175 angstrom UV bump detections for 260 individual galaxies. Even though obvious correlations between UV bump strength and global galaxy properties are absent, strong UV bumps are most often seen in face-on, lower-mass galaxies (10 < log(10)(M-*/M-circle dot) < 10.5) with low overall attenuation. Finally, we produce a typical attenuation curve for star-forming galaxies at z similar to 0.8; this prescription represents the effect of dust on the integrated spectral energy distributions of high-redshift galaxies more accurately than commonly used attenuation laws.
AB - We present a novel approach to measure the attenuation curves of 485 individual star-forming galaxies with M-* > 10(10) M-circle dot based on deep optical spectra from the VLT/VIMOS LEGA-C survey and multiband photometry in the COSMOS field. Most importantly, we find that the attenuation curves in the rest-frame 3000-4500 angstrom range are typically almost twice as steep as the Milky Way, LMC, SMC, and Calzetti attenuation curves, which is in agreement with recent studies of the integrated light of present-day galaxies. The attenuation at 4500 angstrom and the slope strongly correlate with the galaxy inclination: face-on galaxies show less attenuation and steeper curves compared to edge-on galaxies, suggesting that geometric effects dominate observed variations in attenuation. Our new method produces 2175 angstrom UV bump detections for 260 individual galaxies. Even though obvious correlations between UV bump strength and global galaxy properties are absent, strong UV bumps are most often seen in face-on, lower-mass galaxies (10 < log(10)(M-*/M-circle dot) < 10.5) with low overall attenuation. Finally, we produce a typical attenuation curve for star-forming galaxies at z similar to 0.8; this prescription represents the effect of dust on the integrated spectral energy distributions of high-redshift galaxies more accurately than commonly used attenuation laws.
KW - Interstellar dust extinction
KW - STAR-FORMING GALAXIES
KW - ULTRAVIOLET EXTINCTION CURVES
KW - SPECTRAL ENERGY-DISTRIBUTION
KW - INTERSTELLAR EXTINCTION
KW - INSIGHTS
KW - SHAPES
KW - PHOTOMETRY
KW - SCATTERING
KW - STARLIGHT
KW - EVOLUTION
U2 - 10.3847/1538-4357/abba37
DO - 10.3847/1538-4357/abba37
M3 - Journal article
VL - 903
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
M1 - 146
ER -
ID: 319533486