{
  "id": "1610.01194",
  "version": "v1",
  "published": "2016-10-04T20:40:00.000Z",
  "updated": "2016-10-04T20:40:00.000Z",
  "title": "Chemical distribution of HII regions towards the Galactic anticentre",
  "authors": [
    "Alba Fernández-Martín",
    "Enrique Pérez-Montero",
    "José Manuel Vílchez",
    "Antonio Mampaso"
  ],
  "comment": "Accepted for publication in Section 5. Galactic structure, stellar clusters and populations of Astronomy and Astrophysics. The official date of acceptance is 13/09/2016. 19 pages, 15 figures and 10 tables",
  "categories": [
    "astro-ph.GA"
  ],
  "abstract": "We study the physical and chemical properties of a sample of HII regions located at RG >11 kpc and present the radial distribution of abundances towards the Galaxy anticentre. We carried out optical spectroscopic observations of nine HII regions with the WHT. The sample was increased by searching the literature for optical observations of regions towards the Galactic anticentre, re-analysing them to obtain a single sample of 23 objects covering the Galactocentric radius from 11 kpc to 18 kpc to be processed in a homogeneous and consistent manner. Accurate electron densities and temperatures of several ionic species were derived in 13 HII regions. These physical parameters were applied to the spectra to determine direct total chemical abundances. For those regions without direct estimations of temperature, chemical abundances were derived by performing tailor-made photoionisation models and/or by using an empirical relation obtained from radio recombination and optical temperatures. We performed weighted least-squares fits to the distribution of the derived abundances along the Galactocentric distances to study the radial gradients of metallicity. The distributions O/H, N/H, S/H, and Ar/H towards the anticentre can be represented by decreasing linear radial gradients, while in the case of N/O abundances the radial distribution is better fitted with a two-zone model. The He/H radial gradient is presented here for the first time; we find a slope that is not significantly different from zero. The derived gradient for oxygen shows a clear decrease with distance with a slope of -0.053dex/kpc. Although a shallower slope at large Galactocentric distances is suggested by our data, the flattening of the distribution cannot be confirmed and more objects towards the anticentre need to be studied in order to establish the true form of the metallicity gradient.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2016-10-04T20:40:00.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "hii regions",
      "galactic anticentre",
      "chemical distribution",
      "determine direct total chemical abundances",
      "galactocentric distances"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 19,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}