Integral field spectroscopy of a sample of nearby galaxies: II. Properties of the H ii regions
Por:
Sánchez S.F., Rosales-Ortega F.F., Marino R.A., Iglesias-Páramo J., Vílchez J.M., Kennicutt R.C., Díaz A.I., Mast D., Monreal-Ibero A., García-Benito R., Bland-Hawthorn J., Pérez E., González Delgado R., Husemann B., López-Sánchez A.R., Cid Fernandes R., Kehrig C., Walcher C.J., Gil De Paz A., Ellis S.
Publicada:
1 ene 2012
Resumen:
We analyse the spectroscopic properties of thousands of H ii regions identified in 38 face-on spiral galaxies. All galaxies were observed out to 2.4 effective radii using integral field spectroscopy (IFS) over the wavelength range ~3700 to ~6900 Å. The near uniform sample has been assembled from the PPAK IFS Nearby Galaxy (PINGS) survey and a sample described in Paper I. We develop a new automatic procedure to detect H ii regions, based on the contrast of the H? intensity maps extracted from the datacubes. Once detected, the algorithm provides us with the integrated spectra of each individual segmented region. In total, we derive good quality spectroscopic information for ~2600 independent H ii regions/complexes. This is by far the largest H ii region survey of its kind. Our selection criteria and the use of 3D spectroscopy guarantee that we cover the regions in an unbiased way. A well-tested automatic decoupling procedure has been applied to remove the underlying stellar population, deriving the main properties (intensity, dispersion and velocity) of the strongest emission lines in the considered wavelength range (covering from [O ii] ?3727 to [S ii] ?6731). A final catalogue of the spectroscopic properties of H ii regions has been created for each galaxy, which includes information on morphology, spiral structure, gaskinematics, and surface brightness of the underlying stellar population. In the current study, we focus on the understanding of the average properties of the H ii regions and their radial distributions. We find a significant change in the ionisation characteristics of H ii regions within r < 0.25 r e due to contamination from sources with different ionising characteristics, as we discuss. We find that the gas-phase oxygen abundance and the H? equivalent width present a negative and positive gradient, respectively. The distribution of slopes is statistically compatible with a random Gaussian distribution around the mean value, if the radial distances are measured in units of the respective effective radius. No difference in the slope is found for galaxies of different morphologies, e.g. barred/non-barred, grand-design/flocculent. Therefore, the effective radius is a universal scale length for gradients in the evolution of galaxies. Some properties have a large varian
Filiaciones:
Sánchez S.F.:
Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía s/n, Aptdo. 3004, 18080 Granada, Spain
Centro Astronomico Hispano Aleman, Calar Alto, CSIC-MPG, C/Jesus Durban Remon 2-2, 04004 Almeria, Spain
Rosales-Ortega F.F.:
Centro Astronomico Hispano Aleman, Calar Alto, CSIC-MPG, C/Jesus Durban Remon 2-2, 04004 Almeria, Spain
Departamento de Física Teórica, Universidad Autónoma de Madrid, 28049 Madrid, Spain
Marino R.A.:
CEI Campus Moncloa, UCM-UPM, Universidad Complutense de Madrid, Avda. Complutense s/n, 28040 Madrid, Spain
Iglesias-Páramo J.:
Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía s/n, Aptdo. 3004, 18080 Granada, Spain
Centro Astronomico Hispano Aleman, Calar Alto, CSIC-MPG, C/Jesus Durban Remon 2-2, 04004 Almeria, Spain
Vílchez J.M.:
Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía s/n, Aptdo. 3004, 18080 Granada, Spain
Kennicutt R.C.:
Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, United Kingdom
Díaz A.I.:
Departamento de Física Teórica, Universidad Autónoma de Madrid, 28049 Madrid, Spain
Mast D.:
Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía s/n, Aptdo. 3004, 18080 Granada, Spain
Centro Astronomico Hispano Aleman, Calar Alto, CSIC-MPG, C/Jesus Durban Remon 2-2, 04004 Almeria, Spain
Monreal-Ibero A.:
Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía s/n, Aptdo. 3004, 18080 Granada, Spain
García-Benito R.:
Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía s/n, Aptdo. 3004, 18080 Granada, Spain
Bland-Hawthorn J.:
Sydney Institute for Astronomy, School of Physics A28, University of Sydney, NSW 2006, Australia
Pérez E.:
Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía s/n, Aptdo. 3004, 18080 Granada, Spain
González Delgado R.:
Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía s/n, Aptdo. 3004, 18080 Granada, Spain
Husemann B.:
Leibniz-Institut fur Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany
López-Sánchez A.R.:
Australian Astronomical Observatory, PO box 296, Epping, NSW 1710, Australia
Department of Physics and Astronomy, Macquarie University, NSW 2109, Australia
Cid Fernandes R.:
Departamento de Física-CFM-Universidade Federal de Santa Catarina, PO Box 476, 88040-900, Florianópolis, SC, Brazil
Kehrig C.:
Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía s/n, Aptdo. 3004, 18080 Granada, Spain
Walcher C.J.:
Leibniz-Institut fur Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany
Gil De Paz A.:
CEI Campus Moncloa, UCM-UPM, Universidad Complutense de Madrid, Avda. Complutense s/n, 28040 Madrid, Spain
Ellis S.:
Sydney Institute for Astronomy, School of Physics A28, University of Sydney, NSW 2006, Australia
Australian Astronomical Observatory, PO box 296, Epping, NSW 1710, Australia
Bronze
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