MUSE stares into the shadows: the high-resolution dust attenuation curve of NGC 5626

Viaene, S.; Sarzi, Marc; Baes, M.; Fritz, J.; Puerari, I.

doi:10.1093/mnras/stx1781

Cited by 25 publications

(26 citation statements)

References 74 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…this work), as well as resolved attenuation studies through Balmer decrements and in the continuum (e.g. Viaene et al 2017), and studies of the gas and stellar kinematics (e.g. Guérou et al 2017).…”

Section: Muse Spectrophotometrymentioning

confidence: 89%

A systematic metallicity study of DustPedia galaxies reveals evolution in the dust-to-metal ratios

Vis

Jones

Viaene

et al. 2019

A&A

Self Cite

176

102

View full text Add to dashboard Cite

Observations of evolution in the dust-to-metal ratio allow us to constrain the dominant dust processing mechanisms. In this work, we present a study of the dust-to-metal and dust-to-gas ratios in a sub-sample of ∼ 500 DustPedia galaxies. Using literature and MUSE emission line fluxes, we derived gas-phase metallicities (oxygen abundances) for over 10000 individual regions and determine characteristic metallicities for each galaxy. We study how the relative dust, gas, and metal contents of galaxies evolve by using metallicity and gas fraction as proxies for evolutionary state. The global oxygen abundance and nitrogen-to-oxygen ratio are found to increase monotonically as galaxies evolve. Additionally, unevolved galaxies (gas fraction > 60%, metallicity 12 + log(O/H) < 8.2) have dust-to-metal ratios that are about a factor of 2.1 lower (a factor of six lower for galaxies with gas fraction > 80%) than the typical dust-to-metal ratio (M d /M Z ∼ 0.214) for more evolved sources. However, for high gas fractions, the scatter is larger due to larger observational uncertainties as well as a potential dependence of the dust grain growth timescale and supernova dust yield on local conditions and star formation histories. We find chemical evolution models with a strong contribution from dust grain growth describe these observations reasonably well. The dust-to-metal ratio is also found to be lower for low stellar masses and high specific star formation rates (with the exception of some sources undergoing a starburst). Finally, the metallicity gradient correlates weakly with the Hi-to-stellar mass ratio, the effective radius and the dust-to-stellar mass ratio, but not with stellar mass.

show abstract

Section: Muse Spectrophotometrymentioning

confidence: 89%

A systematic metallicity study of DustPedia galaxies reveals evolution in the dust-to-metal ratios

Vis

Jones

Viaene

et al. 2019

A&A

Self Cite

176

102

View full text Add to dashboard Cite

show abstract

“…For full generality in the case of a thick disk, a small fraction (w = 1 − f − b) of the total light may originate within the disk and therefore experience "mixed" attenuation. Rewriting Equation 6 of Viaene et al (2017) in terms of the extinction A λ , the wavelengthdependent ratio F /F 0 of observed to intrinsic integrated stellar light takes the form…”

Section: Disk Extinction Modelingmentioning

confidence: 99%

A Precision Measurement of the Mass of the Black Hole in NGC 3258 from High-resolution ALMA Observations of Its Circumnuclear Disk

Boizelle

Barth

Walsh

et al. 2019

ApJ

102

View full text Add to dashboard Cite

We present ∼ 0. 10−resolution Atacama Large Millimeter/submillimeter Array (ALMA) CO(2−1) imaging of the arcsecond-scale (r ≈ 150 pc) dusty molecular disk in the giant elliptical galaxy NGC 3258. The data provide unprecedented resolution of cold gas disk kinematics within the dynamical sphere of influence of a supermassive black hole, revealing a quasi-Keplerian central increase in projected rotation speed rising from 280 km s −1 at the disk's outer edge to > 400 km s −1 near the disk center. We construct dynamical models for the rotating disk and fit beam-smeared model CO line profiles directly to the ALMA data cube. Our models incorporate both flat disks and tilted-ring disks that provide a better fit of the mildly warped structure in NGC 3258. We show that the exceptional angular resolution of the ALMA data makes it possible to infer the host galaxy's mass profile within r = 150 pc solely from the ALMA CO kinematics, without relying on optical or near-infrared imaging data to determine the stellar mass profile. Our model therefore circumvents any uncertainty in the black hole mass that would result from the substantial dust extinction in the galaxy's central region. The best model fit yields M BH = 2.249 × 10 9 M with a statistical model-fitting uncertainty of just 0.18%, and systematic uncertainties of 0.62% from various aspects of the model construction and 12% from uncertainty in the distance to NGC 3258. This observation demonstrates the full potential of ALMA for carrying out highly precise measurements of M BH in early-type galaxies containing circumnuclear gas disks.

show abstract

“…These properties have previously been shown to have an important role in shaping attenuation curves (e.g. Granato et al 2000;Witt & Gordon 2000;Baes & Dejonghe 2001;Panuzzo et al 2007;Viaene et al 2017a). Our M33 dust attenuation curve appears much more similar to the SMC bar region of Gordon et al (2003), albeit with a strong UV bump.…”

Section: Global Attenuationmentioning

confidence: 99%

High-resolution radiative transfer modelling of M33

Williams

Baes

Looze

et al. 2019

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

In this work, we characterise the contributions from both ongoing star formation and the ambient radiation field in Local Group galaxy M33, as well as estimate the scale of the local dust-energy balance (i.e. the scale at which the dust is re-emitting starlight generated in that same region) in this galaxy through high-resolution radiative transfer (RT) modelling, with defined stellar and dust geometries. We have characterised the spectral energy distribution (SED) of M33 from UV to sub-mm wavelengths, at a spatial scale of 100 pc. We constructed input maps of the various stellar and dust geometries for use in the RT modelling. By modifying our dust mix (fewer very small carbon grains and a lower silicate-to-carbon ratio as compared to the Milky Way), we can much better fit the sub-mm dust continuum. Using this new dust composition, we find that we are able to well reproduce the observed SED of M33 using our adopted model. In terms of stellar attenuation by dust, we find a reasonably strong, broad UV bump, as well as significant systematic differences in the amount of dust attenuation when compared to standard SED modelling. We also find discrepancies in the residuals of the spiral arms versus the diffuse interstellar medium (ISM), indicating a difference in properties between these two regimes. The dust emission is dominated by heating due to the young stellar populations at all wavelengths (∼80% at 10 µm to ∼50% at 1 mm). We find that the local dust-energy balance is restored at spatial scales greater than around 1.5 kpc.

show abstract

MUSE stares into the shadows: the high-resolution dust attenuation curve of NGC 5626

Cited by 25 publications

References 74 publications

A systematic metallicity study of DustPedia galaxies reveals evolution in the dust-to-metal ratios

A systematic metallicity study of DustPedia galaxies reveals evolution in the dust-to-metal ratios

A Precision Measurement of the Mass of the Black Hole in NGC 3258 from High-resolution ALMA Observations of Its Circumnuclear Disk

High-resolution radiative transfer modelling of M33

Contact Info

Product

Resources

About