TY  - JOUR
A1  - Finley, Hayley
A1  - Bouche, Nicolas
A1  - Contini, Thierry
A1  - Epinat, Benoit
A1  - Bacon, Roland
A1  - Brinchmann, Jarle
A1  - Cantalupo, Sebastiano
A1  - Erroz-Ferrer, Santiago
A1  - Marino, Aella Anna
A1  - Maseda, Michael
A1  - Richard, Johan
A1  - Schroetter, Ilane
A1  - Verhamme, Anne
A1  - Weilbacher, Peter Michael
A1  - Wendt, Martin
A1  - Wisotzki, Lutz
T1  - Galactic winds with MUSE: A direct detection of Fe II* emission from a z=1.29 galaxy
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Emission signatures from galactic winds provide an opportunity to directly map the outflowing gas, but this is traditionally challenging because of the low surface brightness. Using very deep observations (27 h) of the Hubble Deep Field South with the Multi Unit Spectroscopic Explorer (MUSE) instrument, we identify signatures of an outflow in both emission and absorption from a spatially resolved galaxy at z = 1.29 with a stellar mass M-star = 8 x 10(9) M-circle dot, star formation rate SFR = 77(-25)(+40) M-circle dot yr(-1), and star formation rate surface brightness Sigma(SFR) = 1.6 M-circle dot kpc(-2) within the [OII] lambda lambda 3727, 3729 half-light radius R-1/2, ([OII]) = 2.76 +/- 0.17 kpc. From a component of the strong resonant Mg II and Fe II absorptions at -350 km s(-1), we infer a mass outflow rate that is comparable to the star formation rate. We detect non-resonant Fe II* emission, at lambda 2365, lambda 2396, lambda 2612, and lambda 2626, at 1.2-2.4-1.5-2.7 x 10-(18) erg s(-1) cm(-2) respectively. The flux ratios are consistent with the expectations for optically thick gas. By combining the four non-resonant Fe II* emission lines, we spatially map the Fe II* emission from an individual galaxy for the first time. The Fe II* emission has an elliptical morphology that is roughly aligned with the galaxy minor kinematic axis, and its integrated half-light radius, R-1/2, (Fe II*) = 4.1 +/- 0.4 kpc, is 70% larger than the stellar continuum (R-1/2,(star) similar or equal to 2.34 +/- 0.17) or the [O II] nebular line. Moreover, the Fe II* emission shows a blue wing extending up to -400 km s(-1), which is more pronounced along the galaxy minor kinematic axis and reveals a C-shaped pattern in a p - v diagram along that axis. These features are consistent with a bi-conical outflow.
KW  - galaxies: evolution
KW  - galaxies: formation
KW  - galaxies: starburst
KW  - galaxies: ISM
KW  - ISM: jets and outflows
KW  - ultraviolet: ISM
Y1  - 2017
U6  - https://doi.org/10.1051/0004-6361/201730428
SN  - 1432-0746
VL  - 605
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Wendt, Martin
A1  - Husser, Tim-Oliver
A1  - Kamann, Sebastian
A1  - Monreal-Ibero, Ana
A1  - Richter, Philipp
A1  - Brinchmann, Jarle
A1  - Dreizler, Stefan
A1  - Weilbacher, Peter Michael
A1  - Wisotzki, Lutz
T1  - Mapping diffuse interstellar bands in the local ISM on small scales via MUSE 3D spectroscopy A pilot study based on globular cluster NGC 6397
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Context. We map the interstellar medium (ISM) including the diffuse interstellar bands (DIBs) in absorption toward the globular cluster NGC6397 using VLT/MUSE. Assuming the absorbers are located at the rim of the Local Bubble we trace structures on the order of mpc (milliparsec, a few thousand AU). Aims. We aimed to demonstrate the feasibility to map variations of DIBs on small scales with MUSE. The sightlines defined by binned stellar spectra are separated by only a few arcseconds and we probe the absorption within a physically connected region. Methods. This analysis utilized the fitting residuals of individual stellar spectra of NGC6397 member stars and analyzed lines from neutral species and several DIBs in Voronoi-binned composite spectra with high signal-to-noise ratio (S/N). Results. This pilot study demonstrates the power of MUSE for mapping the local ISM on very small scales which provides a new window for ISM observations. We detect small scale variations in Na-I and K-I as well as in several DIBs within few arcseconds, or mpc with regard to the Local Bubble. We verify the suitability of the MUSE 3D spectrograph for such measurements and gain new insights by probing a single physical absorber with multiple sight lines.
KW  - techniques: imaging spectroscopy
KW  - globular clusters: individual: NGC 6397
KW  - dust, extinction
KW  - ISM: structure
KW  - ISM: lines and bands
Y1  - 2017
U6  - https://doi.org/10.1051/0004-6361/201629816
SN  - 1432-0746
VL  - 607
PB  - EDP Sciences
CY  - Les Ulis
ER  -