Dust attenuation and Hα emission in a sample of galaxies observed with Herschel at 0.6 &lt; z &lt; 1.6

Buat, V.; Boquien, M.; Małek, K.; Corre, D.; Salas, H.; Roehlly, Y.; Shirley, R.; Efstathiou, A.

doi:10.1051/0004-6361/201833841

Cited by 75 publications

(89 citation statements)

References 72 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This is expected since Charlot & Fall (2000) built their model to reproduce the properties of the starburst galaxies analyzed by Calzetti et al (1994). However a significant difference is visible for λ > 0.5 µm: CF00 is much flatter than C00 (Chevallard et al 2013;Lo Faro et al 2017;Buat et al 2018). The average LF17 law is flatter than the two previous laws over the full wavelength range.…”

Section: Attenuation Lawsmentioning

confidence: 88%

“…It has recently been shown that effective attenuation laws are far from universal but actually vary in local and more distant galaxies (e.g., Salmon et al 2016;Salim et al 2018;Buat et al 2018). The attenuation law appears to flatten out when the amount of obscuration increases, a trend that is predicted by radiation transfer models in dusty media with idealized geometries (Chevallard et al 2013, and references therein) or more realistic distributions from hydrodynamical simulations (Jonsson et al 2010;Roebuck et al 2019;Trayford et al 2019).…”

Section: Introductionmentioning

confidence: 98%

See 1 more Smart Citation

Cold dust and stellar emissions in dust-rich galaxies observed with ALMA: a challenge for SED-fitting techniques

Buat

Ciesla

Boquien

et al. 2019

A&A

Self Cite

110

View full text Add to dashboard Cite

Context. Over the past few years the Atacama Large Millimeter Array (ALMA) has detected dust-rich galaxies whose cold dust emission is spatially disconnected from the ultraviolet (UV) rest-frame emission. This represents a challenge for modeling their spectral energy distributions (SED) with codes based on an energy budget between the stellar and dust components. This could potentially weaken the solidity of the physical parameters measured with these modeling tools. Aims. We want to verify the validity of energy balance modeling on a sample of galaxies observed from the UV to the sub-millimeter rest frame with ALMA and decipher what information can be reliably retrieved from the analysis of the full SED and from subsets of wavelengths. Methods. We select 17 sources at z 2 in the Hubble Ultra-Deep Field (HUDF) and in the GOODS-South field detected with ALMA and Herschel and for which UV to near-infrared rest-frame ancillary data are available. We fit the data with CIGALE exploring different configurations for dust attenuation and star formation histories, considering either the full dataset or one that is reduced to the stellar and dust emission. We compare estimates of the dust luminosities, star formation rates, and stellar masses. Results. The fit of the stellar continuum alone with the starburst attenuation law can only reproduce up to 50% of the total dust luminosity observed by Herschel and ALMA. This deficit is found to be marginally consistent with similar quantities estimated in the COSMOS field and is found to increase with the specific star formation rate. The combined stellar and dust SEDs are well fitted when different attenuation laws are introduced. Shallow attenuation curves are needed for the galaxies whose cold dust distribution is very compact compared to starlight. The stellar mass estimates are affected by the choice of the attenuation law. The star formation rates are robustly estimated as long as dust luminosities are available. The large majority of the galaxies are above the average main sequence of star forming galaxies and one source is a strong starburst. 1 This diagram relates the slope β of the UV continuum to IRX defined as the ratio of the IR and UV luminosities.Article number, page 1 of 15

show abstract

Section: Attenuation Lawsmentioning

confidence: 88%

Section: Introductionmentioning

confidence: 98%

Cold dust and stellar emissions in dust-rich galaxies observed with ALMA: a challenge for SED-fitting techniques

Buat

Ciesla

Boquien

et al. 2019

A&A

Self Cite

110

View full text Add to dashboard Cite

show abstract

“…An important caveat in SED fitting codes is the use of idealised attenuation curves, converted from extinction laws that do not fully incorporate the effect of the relative geometries expected to be found between dust and stars. In a recent effort to address this caveat, Buat et al (2018) measured the shape of the attenuation curves of star-forming galaxies by employing two different recipes: a flexible Calzetti attenuation law (Noll et al 2009) and a two power-law recipe based on the one inferred by Charlot & Fall (2000). Both recipes take the shape of the attenuation curve and the relative attenuation of young and old stellar populations as free parameters.…”

Section: Attenuation Lawmentioning

confidence: 99%

High-resolution, 3D radiative transfer modelling

Nersesian

Verstocken

Viaene

et al. 2020

A&A

View full text Add to dashboard Cite

Context. Dust in late-type galaxies in the local Universe is responsible for absorbing approximately one third of the energy emitted by stars. It is often assumed that dust heating is mainly attributable to the absorption of ultraviolet and optical photons emitted by the youngest (≤ 100 Myr) stars. Consequently, thermal re-emission by dust at far-infrared wavelengths is often linked to the starformation activity of a galaxy. However, several studies argue that the contribution to dust heating by much older stellar populations might be more significant than previously thought. Advances in radiation transfer simulations finally allow us to actually quantify the heating mechanisms of diffuse dust by the stellar radiation field. Aims. As one of the main goals in the DustPedia project, we have developed a framework to construct detailed 3D stellar and dust radiative transfer models for nearby galaxies. In this study, we analyse the contribution of the different stellar populations to the dust heating in four nearby face-on barred galaxies: NGC 1365, M 83, M 95, and M 100. We aim to quantify the fraction directly related to young stellar populations, both globally and on local scales, and to assess the influence of the bar on the heating fraction. Methods. From 2D images we derive the 3D distributions of stars and dust. To model the complex geometries, we used SKIRT, a state-of-the-art 3D Monte Carlo radiative transfer code designed to self-consistently simulate the absorption, scattering, and thermal re-emission by the dust for arbitrary 3D distributions. Results. We derive global attenuation laws for each galaxy and confirm that galaxies of high specific star-formation rate have shallower attenuation curves and weaker UV bumps. On average, 36.5% of the bolometric luminosity is absorbed by dust in our galaxy sample. We report a clear effect of the bar structure on the radial profiles of the dust-heating fraction by the young stellar populations, and the dust temperature. We find that the young stellar populations are the main contributors to the dust heating, donating, on average ∼ 59% of their luminosity to this purpose throughout the galaxy. This dust-heating fraction drops to ∼ 53% in the bar region and ∼ 38% in the bulge region where the old stars are the dominant contributors to the dust heating. We also find a strong link between the heating fraction by the young stellar populations and the specific star-formation rate.

show abstract

“…Commonly used codes such as MAGPHYS and CIGALE (da Cunha et al 2008;Noll et al 2009) treat attenuation toward the birth-clouds and in the diffuse ISM separately, which allows for more flexible effective attenuation curves. However, recent work suggests there may need to be additional modification to allow for greater flexibility (Charlot & Fall 2000;Lo Faro et al 2017;Buat et al 2018). Both observational and theoretical studies have shown that such flexibility is required since a single attenuation curve is not appropriate for all star-forming galaxies either locally or at high-z (e.g.…”

Section: Introductionmentioning

confidence: 99%

Simulations Find Our Accounting of Dust-obscured Star Formation May Be Incomplete

Roebuck

Sajina

Hayward

et al. 2019

ApJ

View full text Add to dashboard Cite

The bulk of the star-formation rate density peak at cosmic noon was obscured by dust. How accurately we can assess the role of dust obscured star-formation is affected by inherent biases in our empirical methods -both those that rely on direct dust emission and those that rely on the inferred dust attenuation of starlight. We use a library of hydrodynamic simulations with radiative transfer to explore these biases. We find that for IR luminous galaxies that are in rapidly quenching systems (e.g. post-coalescence) standard luminosity-to-SFR relations can strongly overestimate the true SFRs. We propose using the L IR /L 1.6 color to both help identify such systems and provide more accurate SFRs. Conversely, we find that the diagnostic UVJ plot misidentifies a subset of dusty star-forming galaxies. This is due to variability in the effective attenuation curves including being much grayer in the optical-to-near-IR regime than the Calzetti starburst law. This is in agreement with recent observations of IR-selected galaxies at cosmic noon. Our results support the view that we need a panchromatic approach from the rest-frame UV through the IR and SED modeling that includes realistic SFHs and allows for variable attenuation curves if we want to fully account for dust obscured star-formation across the epochs of greatest galaxy build-up.

show abstract

Dust attenuation and Hα emission in a sample of galaxies observed with Herschel at 0.6 < z < 1.6

Cited by 75 publications

References 72 publications

Cold dust and stellar emissions in dust-rich galaxies observed with ALMA: a challenge for SED-fitting techniques

Cold dust and stellar emissions in dust-rich galaxies observed with ALMA: a challenge for SED-fitting techniques

High-resolution, 3D radiative transfer modelling

Simulations Find Our Accounting of Dust-obscured Star Formation May Be Incomplete

Contact Info

Product

Resources

About