Automated data reduction workflows for astronomy

Freudling, W.; Romaniello, M.; Bramich, D. M.; Ballester, P.; Forchì, Vincenzo; García-Dabló, C. E.; Moehler, S.; Neeser, Mark

doi:10.1051/0004-6361/201322494

Cited by 641 publications

(507 citation statements)

References 12 publications

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“…The data analysed here have been reduced using version 1.2.1 of the MUSE pipeline (Weilbacher et al 2014) and the Reflex environment (Freudling et al 2013). This pipeline layout includes the standard processes like bias subtraction and flatfielding, flux and wavelength calibration.…”

Section: Data and Galaxy Samplementioning

confidence: 99%

The shape of oxygen abundance profiles explored with MUSE: evidence for widespread deviations from single gradients

Sánchez-Menguiano

Sanchez

Pérez

et al. 2018

A&A

150

146

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We characterised the oxygen abundance radial distribution of a sample of 102 spiral galaxies observed with VLT/MUSE using the O3N2 calibrator. The high spatial resolution of the data allowed us to detect 14345 H ii regions with the same image quality as with photometric data, avoiding any dilution effect. We developed a new methodology to automatically fit the abundance radial profiles, finding that 55 galaxies of the sample exhibit a single negative gradient. The remaining 47 galaxies also display, as well as this negative trend, either an inner drop in the abundances (21), an outer flattening (10), or both (16), which suggests that these features are a common property of disc galaxies. The presence and depth of the inner drop depends on the stellar mass of the galaxies with the most massive systems presenting the deepest abundance drops, while there is no such dependence in the case of the outer flattening. We find that the inner drop appears always around 0.5 r e , while the position of the outer flattening varies over a wide range of galactocentric distances. Regarding the main negative gradient, we find a characteristic slope in the sample of α O/H = − 0.10 ± 0.03 dex/r e . This slope is independent of the presence of bars and the density of the environment. However, when inner drops or outer flattenings are detected, slightly steeper gradients are observed. This suggests that radial motions might play an important role in shaping the abundance profiles. We define a new normalisation scale ('the abundance scale length', r O/H ) for the radial profiles based on the characteristic abundance gradient, with which all the galaxies show a similar position for the inner drop (∼ 0.5 r O/H ) and the outer flattening (∼ 1.5 r O/H ). Finally, we find no significant dependence of the dispersion around the negative gradient with any property of the galaxies, with values compatible with the uncertainties associated with the derivation of the abundances.

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Section: Data and Galaxy Samplementioning

confidence: 99%

The shape of oxygen abundance profiles explored with MUSE: evidence for widespread deviations from single gradients

Sánchez-Menguiano

Sanchez

Pérez

et al. 2018

A&A

150

146

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“…The data were reduced with the ESO/X-Shooter pipeline v2.5.2 (Modigliani et al 2010) using the Reflex interface (Freudling et al 2013). The spectra have been rectified on a grid with 0.2 Å/pixel in the UVB and VIS arm and 0.6 Å/pixel in the NIR arm, thus slightly oversampling even the highest-resolution spectra while minimizing the correlation between adjacent pixels in the rectification.…”

Section: Sample Descriptionmentioning

confidence: 99%

An X-Shooter composite of bright 1 <z< 2 quasars from UV to infrared

Selsing

Fynbo

Christensen

et al. 2015

A&A

165

180

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Quasi-stellar object (QSO) spectral templates are important both to QSO physics and for investigations that use QSOs as probes of intervening gas and dust. However, combinations of various QSO samples obtained at different times and with different instruments so as to expand a composite and to cover a wider rest frame wavelength region may create systematic effects, and the contribution from QSO hosts may contaminate the composite. We have constructed a composite spectrum from luminous blue QSOs at 1 < z < 2.1 selected from the Sloan Digital Sky Survey (SDSS). The observations with X-Shooter simultaneously cover ultraviolet (UV) to nearinfrared (NIR) light, which ensures that the composite spectrum covers the full rest-frame range from Lyβ to 11 350 Å without any significant host contamination. Assuming a power-law continuum for the composite we find a spectral slope of α λ = 1.70 ± 0.01, which is steeper than previously found in the literature. We attribute the differences to our broader spectral wavelength coverage, which allows us to effectively avoid fitting any regions that are affected either by strong QSO emissions lines (e.g., Balmer lines and complex [Fe II] blends) or by intrinsic host galaxy emission. Finally, we demonstrate the application of the QSO composite spectrum for evaluating the reddening in other QSOs.

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“…The data reductions were performed with the standard ESO pipeline ESOREX (Freudling et al 2013) which consists of dark, flat, detector linearity, geometric distortion corrections and wavelength calibrations using Neon and Argon arcs. Sky was subtracted using the nearest sky frames.…”

Section: Sinfonimentioning

confidence: 99%

Shutting down or powering up a (U)LIRG? Merger components in distinctly different evolutionary states in IRAS 19115−2124 (the Bird)

Vaïsänen

Reunanen

Kotilainen

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present new SINFONI near-infrared integral field unit (IFU) spectroscopy and SALT optical long-slit spectroscopy characterising the history of a nearby merging luminous infrared galaxy, dubbed the Bird (IRAS19115-2114). The NIR line-ratio maps of the IFU data-cubes and stellar population fitting of the SALT spectra now allow dating of the star formation (SF) over the triple system uncovered from our previous adaptive optics data. The distinct components separate very clearly in a line-ratio diagnostic diagram. An off-nuclear pure starburst dominates the current SF of the Bird with 60-70% of the total, with a 4-7 Myr age, and signs of a fairly constant long-term star formation of the underlying stellar population. The most massive nucleus, in contrast, is quenched with a starburst age of > 40 Myr and shows hints of budding AGN activity. The secondary massive nucleus is at an intermediate stage. The two major components have a population of older stars, consistent with a starburst triggered 1 Gyr ago in a first encounter. The simplest explanation of the history is that of a triple merger, where the strongly star forming component has joined later. We detect multiple gas flows in different phases. The Bird offers an opportunity to witness multiple stages of galaxy evolution in the same system; triggering as well as quenching of SF, and the early appearance of AGN activity. It also serves as a cautionary note on interpretations of observations with lower spatial resolution and/or without infrared data. At high-redshift the system would look like a clumpy starburst with crucial pieces of its puzzle hidden, in danger of misinterpretations.

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Automated data reduction workflows for astronomy

Cited by 641 publications

References 12 publications

The shape of oxygen abundance profiles explored with MUSE: evidence for widespread deviations from single gradients

The shape of oxygen abundance profiles explored with MUSE: evidence for widespread deviations from single gradients

An X-Shooter composite of bright 1 <z< 2 quasars from UV to infrared

Shutting down or powering up a (U)LIRG? Merger components in distinctly different evolutionary states in IRAS 19115−2124 (the Bird)

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