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

Sébastien Viaene UGent, M Sarzi, Maarten Baes UGent, J Fritz and I Puerari (2017) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. 472(2). p.1286-1299
abstract
The newest generation of integral field unit spectrographs brings three-dimensional mapping of nearby galaxies one step closer. While the focus up to this point was mostly on stars and ionized gas, it is also possible to look at dust in a new, more complete way. Using MUSE science verification observations of NGC 5626, we map the interstellar matter in this dusty lenticular. We use the resolving power of MUSE to measure the optical attenuation with a spectral resolution of 6.25 angstrom, at physical scales of 0.1-1 kpc. The integrated attenuation curve of NGC 5626 shows a smooth, slightly steeper than Milky Way and SMC attenuation curves. Several sharp features are superimposed: we measure lower attenuation at spectral emission lines and higher attenuation for the sodium line doublet. No correlation was observed between sodium line strength and reddening by dust on spatially resolved scales. Additionally, the continuum attenuation was found to be independent from the Balmer decrement (tracing ionized gas attenuation). We model and interpret the variations in the attenuation curves of each spatial resolution element of NGC 5626. We find that the amount and distribution of dust along the line of sight is highly degenerate with any variation in the intrinsic extinction law. Our analysis shows that the interstellar matter in NGC 5626 resides in a regular and well-settled disc. Our results preach caution in the application of simple recipes to de-redden global galaxy spectra and underlines the need for more realistic dust geometries when constructing such correction formulas.
Please use this url to cite or link to this publication:
author
organization
year
type
journalArticle (original)
publication status
published
subject
keyword
dust, extinction, galaxies: fundamental parameters, galaxies: individual: NGC 5626, galaxies: ISM, EARLY-TYPE GALAXIES, DIFFUSE INTERSTELLAR BANDS, EXTRAGALACTIC EXTINCTION LAW, RADIATIVE-TRANSFER, FORMING GALAXIES, VIRGO-CLUSTER, ELLIPTIC GALAXIES, COLOR GRADIENTS, DISC GALAXIES, IONIZED-GAS
journal title
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Mon. Not. Roy. Astron. Soc.
volume
472
issue
2
pages
1286 - 1299
Web of Science type
Article
Web of Science id
000413082900003
ISSN
0035-8711
1365-2966
DOI
10.1093/mnras/stx1781
language
English
UGent publication?
yes
classification
A1
copyright statement
I have transferred the copyright for this publication to the publisher
id
8538463
handle
http://hdl.handle.net/1854/LU-8538463
date created
2017-11-22 08:45:32
date last changed
2017-12-15 15:40:15
@article{8538463,
  abstract     = {The newest generation of integral field unit spectrographs brings three-dimensional mapping of nearby galaxies one step closer. While the focus up to this point was mostly on stars and ionized gas, it is also possible to look at dust in a new, more complete way. Using MUSE science verification observations of NGC 5626, we map the interstellar matter in this dusty lenticular. We use the resolving power of MUSE to measure the optical attenuation with a spectral resolution of 6.25 angstrom, at physical scales of 0.1-1 kpc. The integrated attenuation curve of NGC 5626 shows a smooth, slightly steeper than Milky Way and SMC attenuation curves. Several sharp features are superimposed: we measure lower attenuation at spectral emission lines and higher attenuation for the sodium line doublet. No correlation was observed between sodium line strength and reddening by dust on spatially resolved scales. Additionally, the continuum attenuation was found to be independent from the Balmer decrement (tracing ionized gas attenuation). We model and interpret the variations in the attenuation curves of each spatial resolution element of NGC 5626. We find that the amount and distribution of dust along the line of sight is highly degenerate with any variation in the intrinsic extinction law. Our analysis shows that the interstellar matter in NGC 5626 resides in a regular and well-settled disc. Our results preach caution in the application of simple recipes to de-redden global galaxy spectra and underlines the need for more realistic dust geometries when constructing such correction formulas.},
  author       = {Viaene, S{\'e}bastien and Sarzi, M and Baes, Maarten and Fritz, J and Puerari, I},
  issn         = {0035-8711},
  journal      = {MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY},
  keyword      = {dust,extinction,galaxies: fundamental parameters,galaxies: individual: NGC 5626,galaxies: ISM,EARLY-TYPE GALAXIES,DIFFUSE INTERSTELLAR BANDS,EXTRAGALACTIC EXTINCTION LAW,RADIATIVE-TRANSFER,FORMING GALAXIES,VIRGO-CLUSTER,ELLIPTIC GALAXIES,COLOR GRADIENTS,DISC GALAXIES,IONIZED-GAS},
  language     = {eng},
  number       = {2},
  pages        = {1286--1299},
  title        = {MUSE stares into the shadows : the high-resolution dust attenuation curve of NGC 5626},
  url          = {http://dx.doi.org/10.1093/mnras/stx1781},
  volume       = {472},
  year         = {2017},
}

Chicago
Viaene, Sébastien, M Sarzi, Maarten Baes, J Fritz, and I Puerari. 2017. “MUSE Stares into the Shadows : the High-resolution Dust Attenuation Curve of NGC 5626.” Monthly Notices of the Royal Astronomical Society 472 (2): 1286–1299.
APA
Viaene, Sébastien, Sarzi, M., Baes, M., Fritz, J., & Puerari, I. (2017). MUSE stares into the shadows : the high-resolution dust attenuation curve of NGC 5626. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 472(2), 1286–1299.
Vancouver
1.
Viaene S, Sarzi M, Baes M, Fritz J, Puerari I. MUSE stares into the shadows : the high-resolution dust attenuation curve of NGC 5626. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. 2017;472(2):1286–99.
MLA
Viaene, Sébastien, M Sarzi, Maarten Baes, et al. “MUSE Stares into the Shadows : the High-resolution Dust Attenuation Curve of NGC 5626.” MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 472.2 (2017): 1286–1299. Print.