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dc.contributor.author
Roth, Martin M.
dc.contributor.author
Sandin, Christer
dc.contributor.author
Kamann, Sebastian
dc.contributor.author
Husser, Tim-Oliver
dc.contributor.author
Weilbacher, Peter M.
dc.contributor.author
Monreal-Ibero, Ana
dc.contributor.author
Bacon, Roland
dc.contributor.author
Den Brok, Mark
dc.contributor.author
Dreizler, Stefan
dc.contributor.author
Kelz, Andreas
dc.contributor.author
Marino, Raffaella Anna
dc.contributor.author
Steinmetz, Matthias
dc.date.accessioned
2018-11-28T08:29:07Z
dc.date.available
2018-11-09T05:21:56Z
dc.date.available
2018-11-28T08:29:07Z
dc.date.issued
2018-10
dc.identifier.issn
0004-6361
dc.identifier.issn
1432-0746
dc.identifier.other
10.1051/0004-6361/201833007
en_US
dc.identifier.uri
http://hdl.handle.net/20.500.11850/302363
dc.identifier.doi
10.3929/ethz-b-000302363
dc.description.abstract
Aims. As a new approach to the study of resolved stellar populations in nearby galaxies, our goal is to demonstrate with a pilot study in NGC 300 that integral field spectroscopy with high spatial resolution and excellent seeing conditions reaches an unprecedented depth in severely crowded fields. Methods. Observations by MUSE with seven pointings in NGC 300 have resulted in data cubes that are analyzed in four ways: (1) Point spread function-fitting 3D spectroscopy with PampelMUSE, as already successfully pioneered in globular clusters, yields de-blended spectra of individually distinguishable stars, thus providing a complete inventory of blue and red supergiants, and asymptotic giant branch (AGB) stars of type M and C. The technique is also applicable to emission line point sources and provides samples of planetary nebulae (PNe) that are complete down to m5007 = 28. (2) Pseudo-monochromatic images, created at the wavelengths of the most important emission lines and corrected for continuum light with the P3D visualization tool, provide maps of H II regions, supernova remnants (SNR), and the diffuse interstellar medium (ISM) at a high level of sensitivity, where also faint point sources stand out and allow for the discovery of PNe, Wolf–Rayet (WR) stars, etc. (3) The use of the P3D line-fitting tool yields emission line fluxes, surface brightness, and kinematic information for gaseous objects, corrected for absorption line profiles of the underlying stellar population in the case of Hα. (4) Visual inspection of the data cubes by browsing through the row-stacked spectra image in P3D is demonstrated to be efficient for data mining and the discovery of background galaxies and unusual objects. Results. We present a catalog of luminous stars, rare stars such as WR, and other emission line stars, carbon stars, symbiotic star candidates, PNe, H II regions, SNR, giant shells, peculiar diffuse and filamentary emission line objects, and background galaxies, along with their spectra. Conclusions. The technique of crowded-field 3D spectroscopy, using the PampelMUSE code, is capable of deblending individual bright stars, the unresolved background of faint stars, gaseous nebulae, and the diffuse component of the ISM, resulting in unprecedented legacy value for observations of nearby galaxies with MUSE.
en_US
dc.format
application/pdf
en_US
dc.language.iso
en
en_US
dc.publisher
EDP Sciences
en_US
dc.rights.uri
http://creativecommons.org/licenses/by/4.0/
dc.subject
galaxies: stellar content
en_US
dc.subject
stars: AGB and post-AGB
en_US
dc.subject
stars: Wolf–Raye
en_US
dc.subject
ISM: supernova remnants
en_US
dc.subject
HII regions
en_US
dc.subject
planetary nebulae: general
en_US
dc.title
MUSE crowded field 3D spectroscopy in NGC 300 I. First results from central fields
en_US
dc.type
Journal Article
dc.rights.license
Creative Commons Attribution 4.0 International
dc.date.published
2018-10-03
ethz.journal.title
Astronomy & Astrophysics
ethz.journal.volume
618
en_US
ethz.journal.abbreviated
Astron. astrophys.
ethz.pages.start
A3
en_US
ethz.size
36 p.
en_US
ethz.version.deposit
publishedVersion
en_US
ethz.identifier.wos
ethz.identifier.scopus
ethz.publication.place
Les Ulis
en_US
ethz.publication.status
published
en_US
ethz.leitzahl
ETH Zürich::00002 - ETH Zürich::00012 - Lehre und Forschung::00007 - Departemente::02010 - Dep. Physik / Dep. of Physics::03613 - Lilly, Simon / Lilly, Simon
ethz.leitzahl.certified
ETH Zürich::00002 - ETH Zürich::00012 - Lehre und Forschung::00007 - Departemente::02010 - Dep. Physik / Dep. of Physics::03613 - Lilly, Simon / Lilly, Simon
ethz.date.deposited
2018-11-09T05:22:05Z
ethz.source
WOS
ethz.eth
yes
en_US
ethz.availability
Open access
en_US
ethz.rosetta.installDate
2018-11-28T08:29:43Z
ethz.rosetta.lastUpdated
2020-02-15T16:06:46Z
ethz.rosetta.versionExported
true
ethz.COinS
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