Integral field spectroscopy of H ii region complexes: the outer disc of NGC 6946

García-Benito, R.; Díaz, Ángeles I.; Hägele, G. F.; Montero, E. Pérez; López, Javier Piqueras; Vı́lchez, J. M.; Pérez, E.; Terlevich, Elena; Terlevich, R.; Rosa-González, D.

doi:10.1111/j.1365-2966.2010.17269.x

Cited by 38 publications

(42 citation statements)

References 92 publications

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“…A.4). The reason for this is that the light of a standard star covered by a PPak fiber inevitably changes with wavelength because of atmospheric dispersion, thoroughly discussed in García-Benito (2009), García-Benito et al (2010) and Rosales-Ortega (2009). These classical aperture losses occur even if the standard star has been centered on a single fiber as accurately as possible for panchromatic observation as performed with the V500 setup.…”

Section: A7 Flux Calibrationmentioning

confidence: 99%

CALIFA, the Calar Alto Legacy Integral Field Area survey

Husemann

Jahnke

Sánchez

et al. 2013

A&A

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197

114

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We present the first public data release (DR1) of the Calar Alto Legacy Integral Field Area (CALIFA) survey. It consists of science-grade optical datacubes for the first 100 of eventually 600 nearby (0.005 < z < 0.03) galaxies, obtained with the integral-field spectrograph PMAS/PPak mounted on the 3.5 m telescope at the Calar Alto observatory. The galaxies in DR1 already cover a wide range of properties in color-magnitude space, morphological type, stellar mass, and gas ionization conditions. This offers the potential to tackle a variety of open questions in galaxy evolution using spatially resolved spectroscopy. Two different spectral setups are available for each galaxy, (i) a low-resolution V500 setup covering the nominal wavelength range 3745-7500 Å with a spectral resolution of 6.0 Å (FWHM), and (ii) a medium-resolution V1200 setup covering the nominal wavelength range 3650-4840 Å with a spectral resolution of 2.3 Å (FWHM). We present the characteristics and data structure of the CALIFA datasets that should be taken into account for scientific exploitation of the data, in particular the effects of vignetting, bad pixels and spatially correlated noise. The data quality test for all 100 galaxies showed that we reach a median limiting continuum sensitivity of 1.0 × 10 −18 erg s −1 cm −2 Å −1 arcsec −2 at 5635 Å and 2.2 × 10 −18 erg s −1 cm −2 Å −1 arcsec −2 at 4500 Å for the V500 and V1200 setup respectively, which corresponds to limiting r and g band surface brightnesses of 23.6 mag arcsec −2 and 23.4 mag arcsec −2 , or an unresolved emission-line flux detection limit of roughly 1 × 10 −17 erg s −1 cm −2 arcsec −2 and 0.6 × 10 −17 erg s −1 cm −2 arcsec −2 , respectively. The median spatial resolution is 3. 7, and the absolute spectrophotometric calibration is better than 15% (1σ). We also describe the available interfaces and tools that allow easy access to this first public CALIFA data at http://califa.caha.es/DR1.

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Section: A7 Flux Calibrationmentioning

confidence: 99%

CALIFA, the Calar Alto Legacy Integral Field Area survey

Husemann

Jahnke

Sánchez

et al. 2013

A&A

Self Cite

197

114

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“…Other authors have used these parameters, together with the excitation measured by the ratio of [OII]/[OIII], to study the ionisation structure of HII regions (García-Benito et al 2010, Monreal-Ibero et al 2011. Here, we exploit these parameters to distinguish between the various regions in our data (pillars, surrounding HII region, stars, young stellar objects, and protostellar outflows).…”

Section: Abundance Tracers and Ionic Abundancesmentioning

confidence: 99%

“…BPT diagrams have been used for IFU observations of HII regions (Monreal-Ibero et al 2011, García-Benito et al 2010 as well, but since these are spatially resolved observations caution is advised: one is comparing a 3D structure with a 1D photoionisation model, and in a 2D projection of a 3D structure the line ratio will show variations from pixel to pixel because of the local gas conditions along the line of sight on each pixel (Allen et al 2008) but we do not see values that high, we suggest that the dominant excitation mechanism at the pillar tips is photoionisation. This agrees very well with the BPT diagrams of our SPH simulations (see Fig.…”

Section: Line Ratio Maps and Bpt Diagramsmentioning

confidence: 99%

The Pillars of Creation revisited with MUSE: gas kinematics and high-mass stellar feedback traced by optical spectroscopy

McLeod¹,

Dale

Ginsburg³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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Integral field unit (IFU) data of the iconic Pillars of Creation in M16 are presented. The ionisation structure of the pillars was studied in great detail over almost the entire visible wavelength range, and maps of the relevant physical parameters, e.g. extinction, electron density, electron temperature, line-of-sight velocity of the ionised and neutral gas are shown. In agreement with previous authors, we find that the pillar tips are being ionised and photo-evaporated by the massive members of the nearby cluster NGC 6611. They display a stratified ionisation structure where the emission lines peak in a descending order according to their ionisation energies. The IFU data allowed us to analyse the kinematics of the photo-evaporative flow in terms of the stratified ionisation structure, and we find that, in agreement with simulations, the photo-evaporative flow is traced by a blueshift in the position-velocity profile. The gas kinematics and ionisation structure have allowed us to produce a sketch of the 3D geometry of the Pillars, positioning the pillars with respect to the ionising cluster stars. We use a novel method to detect a previously unknown bipolar outflow at the tip of the middle pillar and suggest that it has an embedded protostar as its driving source. Furthermore we identify a candidate outflow in the leftmost pillar. With the derived physical parameters and ionic abundances, we estimate a mass loss rate due to the photo-evaporative flow of 70 M Myr −1 which yields an expected lifetime of approximately 3 Myr.

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“…Unfortunately, for this galaxy there are fewer studies at high spectroscopic resolution. That of García-Benito et al (2010) is the most noteworthy, but unfortunately only covers a few H II regions in the outer parts of the galaxy.…”

Section: Introductionmentioning

confidence: 99%

Two-dimensional metallicity distribution of the ionized gas in NGC 628 and NGC 6946

Cedrés

Cepa

Bongiovanni

et al. 2012

A&A

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Aims. We present here two H II region catalogues with azimuthal resolution for the two grand design galaxies NGC 628 and NGC 6946. With the help of these catalogues, we study several properties of the star-forming processes occurring in spiral galaxies. Methods. We obtained direct imaging in the narrow-band filters centred at Hα, Hβ, [O II]λ3727, and [O III]λλ4959, 5007 and their respective continua. After the calibration and correction of the data, we obtained for each H II region the de-reddened fluxes in the aforementioned lines, the size, the Hα equivalent width, and, using two different empirical calibrations, the metallicity. Employing a method based on the Delaunay triangulation, a two-dimensional (2D) representation of the metallicity was obtained. Results. Data for 209 H II regions of NGC 628 and 226 H II regions of NGC 6946 are obtained. The radial behaviours of the Hα equivalent width, the excitation, and the oxygen abundance are derived. Two-dimensional representations of the metallicity and the excitation are calculated for the galaxies in the study. The two empirical calibrations of the metallicity are compared. Conclusions. The behaviours of the extinction and the Hα equivalent width are similar to those presented in the literature. The oxygen abundance gradients obtained in this study agree with previously published values. However, more regions were examined than in previous studies. We find a difference of about 0.6 dex between the two empirical calibrations employed. Finally, the 2D representations of the metallicity reveal high metallicity knots in NGC 628, and for NGC 6946 a high metallicity azimuthal structure is discovered. These high metallicity regions seem to be linked to the arms of the galaxies and are probably produced by an increase in the temperature of the ionizing clusters in the H II regions, which may be linked to variations in the initial mass functions of the galaxies between the arm and interarm regions.

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Integral field spectroscopy of H ii region complexes: the outer disc of NGC 6946

Cited by 38 publications

References 92 publications

CALIFA, the Calar Alto Legacy Integral Field Area survey

CALIFA, the Calar Alto Legacy Integral Field Area survey

The Pillars of Creation revisited with MUSE: gas kinematics and high-mass stellar feedback traced by optical spectroscopy

Two-dimensional metallicity distribution of the ionized gas in NGC 628 and NGC 6946

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