Galaxy and mass assembly (GAMA): dust obscuration in galaxies and their recent star formation histories

Wijesinghe, Dinuka; Hopkins, A. M.; Sharp, Robert; Gunawardhana, Madusha; Brough, Sarah; Sadler, E. M.; Driver, Simon P.; Baldry, I. K.; Bamford, Steven P.; Liske, J.; Loveday, Jon; Norberg, Peder; Peacock, J. A.; Popescu, Cristina; Tuffs, R.; Bland-Hawthorn, Joss; Cameron, Ewan; Croom, S. M.; Frenk, Carlos S.; Hill, D. T.; Jones, D. Heath; Kampen, E. van; Kelvin, Lee S.; Kuijken, Konrad; Madore, Barry F.; Nichol, Bob; Parkinson, H; Pimbblet, Kevin A.; Prescott, M.; Robotham, Aaron S. G.; Seibert, Mark; Simmat, Ellen; Sutherland, William J.; Taylor, Edward N.; Thomas, Daniel

doi:10.1111/j.1365-2966.2010.17599.x

Cited by 34 publications

(41 citation statements)

References 58 publications

(205 reference statements)

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“…This environmental effect may be responsible for the difference between the results of, for example, von der Linden et al (2010) and Wijesinghe et al (2012). As Wijesinghe et al (2012) used Hα equivalent widths derived from single fibre spectroscopy at the centre of the galaxy as a proxy for specific star formation rate, and calculated the star formation rate assuming that the emission line intensity as measured within the fibre was representative of the entire galaxy (Wijesinghe et al 2011). If environmental effects primarily influence the outskirts of galaxies then the integrated star formation rates in dense environments may have been systematically overestimated (see Richards et al 2016, for a discussion of these aperture effects).…”

Section: Stellar Line Indicesmentioning

confidence: 99%

The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies

Schaefer

Croom

Allen

et al. 2016

Mon. Not. R. Astron. Soc.

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We use data from the Sydney-AAO Multi-Object Integral Field Spectrograph (SAMI) Galaxy Survey and the Galaxy And Mass Assembly (GAMA) survey to investigate the spatially-resolved signatures of the environmental quenching of star formation in galaxies. Using dust-corrected measurements of the distribution of Hα emission we measure the radial profiles of star formation in a sample of 201 star-forming galaxies covering three orders of magnitude in stellar mass (M * ; 10 8.1 -10 10.95 M ) and in 5 th nearest neighbour local environment density (Σ 5 ; 10 −1.3 -10 2.1 Mpc −2 ). We show that star formation rate gradients in galaxies are steeper in dense (log 10 (Σ 5 /Mpc 2 ) > 0.5) environments by 0.58 ± 0.29 dex r e −1 in galaxies with stellar masses in the range 10 10 < M * /M < 10 11 and that this steepening is accompanied by a reduction in the integrated star formation rate. However, for any given stellar mass or environment density the star-formation morphology of galaxies shows large scatter. We also measure the degree to which the star formation is centrally concentrated using the unitless scaleradius ratio (r 50,Hα /r 50,cont ), which compares the extent of ongoing star formation to previous star formation. With this metric we find that the fraction of galaxies with centrally concentrated star formation increases with environment density, from ∼ 5 ± 4% in low-density environments (log 10 (Σ 5 /Mpc 2 ) < 0.0) to 30 ± 15% in the highest density environments (log 10 (Σ 5 /Mpc 2 ) > 1.0). These lines of evidence strongly suggest that with increasing local environment density the star formation in galaxies is suppressed, and that this starts in their outskirts such that quenching occurs in an outside-in fashion in dense environments and is not instantaneous.

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Section: Stellar Line Indicesmentioning

confidence: 99%

The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies

Schaefer

Croom

Allen

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Previous studies have attempted to overcome this issue through estimating attenuation-corrected SFRs by applying attenuation estimates based on the UV spectral slope (β) and luminosity corrections, such as those derived by Meurer, Heckman & Calzetti (1999) -e.g. Wijesinghe et al 2011. Such corrections apply general scaling to all galaxies and may not be appropriate for specific galaxy classes (e.g.…”

Section: Short-duration Attenuation-corrected Uv Continuum and Magphymentioning

confidence: 99%

“…In this manner, we use each galaxy's full SED to estimate the attenuation correction to be applied to the UV luminosity for each individual galaxy instead of applying a general β correction. We convert UV luminosity to SFR using the calibrations given in Wijesinghe et al 2011:…”

Section: Short-duration Attenuation-corrected Uv Continuum and Magphymentioning

confidence: 99%

Galaxy And Mass Assembly (GAMA): the effect of close interactions on star formation in galaxies

Davies

Robotham

Driver

et al. 2015

Mon. Not. R. Astron. Soc.

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The modification of star formation (SF) in galaxy interactions is a complex process, with SF observed to be both enhanced in major mergers and suppressed in minor pair interactions. Such changes likely to arise on short timescales and be directly related to the galaxy-galaxy interaction time. Here we investigate the link between dynamical phase and direct measures of SF on different timescales for pair galaxies, targeting numerous star-formation rate (SFR) indicators and comparing to pair separation, individual galaxy mass and pair mass ratio. We split our sample into the higher (primary) and lower (secondary) mass galaxies in each pair and find that SF is indeed enhanced in all primary galaxies but suppressed in secondaries of minor mergers. We find that changes in SF of primaries is consistent in both major and minor mergers, suggesting that SF in the more massive galaxy is agnostic to pair mass ratio.We also find that SF is enhanced/suppressed more strongly for short-time duration SFR indicators (e.g. Hα), highlighting recent changes to SF in these galaxies, which are likely to be induced by the interaction. We propose a scenario where the lower mass galaxy has its SF suppressed by gas heating or stripping, while the higher mass galaxy has its SF enhanced, potentially by tidal gas turbulence and shocks. This is consistent with the seemingly contradictory observations for both SF suppression and enhancement in close pairs.

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“…In the nearby universe, the UV wavelength range has been investigated thanks to GALEX observations, but the results remain controversial. Wijesinghe et al (2011) analyse the consistency of SFR indicators based on GALEX measurements in the far-ultraviolet (FUV) and near-ultraviolet (NUV) bands and fluxes in the H α line, and conclude that they must consider an obscuration curve without any 2175 Å feature. Instead, from a careful analysis of pairs of galaxy SEDs, Wild et al (2011) conclude that the UV slope of the attenuation curve is consistent with the presence of a bump at 2175 Å, a conclusion also reached by Conroy et al (2010) from an analysis of the GALEX-SDSS colours of galaxies.…”

Section: Introductionmentioning

confidence: 99%

GOODS-Herschel: dust attenuation properties of UV selected high redshift galaxies

Buat

Noll

Burgarella

et al. 2012

A&A

203

275

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Context. Dust attenuation in galaxies is poorly known, especially at high redshift. And yet the amount of dust attenuation is a key parameter to deduce accurate star formation rates from ultraviolet (UV) rest-frame measurements. The wavelength dependence of the dust attenuation is also of fundamental importance to interpret the observed spectral energy distributions (SEDs) and to derive photometric redshifts or physical properties of galaxies. Aims. We want to study dust attenuation at UV wavelengths at high redshift, where the UV is redshifted to the observed visible light wavelength range. In particular, we search for a UV bump and related implications for dust attenuation determinations. Methods. We use photometric data in the Chandra Deep Field South (CDFS), obtained in intermediate and broad band filters by the MUSYC project, to sample the UV rest-frame of 751 galaxies with 0.95 < z < 2.2. When available, infrared (IR) Herschel/PACS data from the GOODS-Herschel project, coupled with Spitzer/MIPS measurements, are used to estimate the dust emission and to constrain dust attenuation. The SED of each source is fit using the CIGALE code. The amount of dust attenuation and the characteristics of the dust attenuation curve are obtained as outputs of the SED fitting process, together with other physical parameters linked to the star formation history. Results. The global amount of dust attenuation at UV wavelengths is found to increase with stellar mass and to decrease as UV luminosity increases. A UV bump at 2175 Å is securely detected in 20% of the galaxies, and the mean amplitude of the bump for the sample is similar to that observed in the extinction curve of the LMC supershell region. This amplitude is found to be lower in galaxies with very high specific star formation rates, and 90% of the galaxies exhibiting a secure bump are at z < 1.5. The attenuation curve is confirmed to be steeper than that of local starburst galaxies for 20% of the galaxies. The large dispersion found for these two parameters describing the attenuation law is likely to reflect a wide diversity of attenuation laws among galaxies. The relations between dust attenuation, IR-to-UV flux ratio, and the slope of the UV continuum are derived for the mean attenuation curve found for our sample. Deviations from the average trends are found to correlate with the age of the young stellar population and the shape of the attenuation curve.

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Galaxy and mass assembly (GAMA): dust obscuration in galaxies and their recent star formation histories

Cited by 34 publications

References 58 publications

The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies

The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies

Galaxy And Mass Assembly (GAMA): the effect of close interactions on star formation in galaxies

GOODS-Herschel: dust attenuation properties of UV selected high redshift galaxies

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