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  • 1. Ashworth, G.
    et al.
    Fumagalli, Michele
    Adamo, Angela
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Krumholz, Mark R.
    Theoretical predictions for IMF diagnostics in UV spectroscopy of star clusters2018In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 480, no 3, p. 3091-3104Article in journal (Refereed)
    Abstract [en]

    We explore the possibility of using UV spectroscopy in combination with broad-band photometry as diagnostic tools for understanding the shape of the initial mass function (IMF) in unresolved stellar populations. Building on our previous work, we extend the Stochastically Lighting Up Galaxies (SLUG) code to include a high-resolution UV spectral synthesizer and equivalent width calculation capabilities. We first gain a qualitative understanding of how UV spectral features behave as the parameters that define a star cluster in SLUG (mass, age, extinction, and IMF slope alpha(3)) are changed. We then exploit Bayesian inference techniques to recover the alpha(3) values for clusters simulated with SLUG, using mock observations of these clusters comprised of broad-band photometry and equivalent width measurements of a selection of UV spectral features. We find some improvement when compared to attempts using broad-band photometry alone (with the interquartile range of the alpha(3) posterior PDF shrinking by similar or equal to 32%), although we still do not yet fully break the known degeneracy between the cluster mass and alpha(3). Finally, we make predictions about how effective real observations will be by quantifying our ability to constrain alpha(3) as a function of limiting equivalent width. We find that observations sensitive to a modest equivalent width of similar or equal to 9 angstrom are sufficient to improve the recovery of the IMF slope parameter by similar or equal to 32% (interquartile range of posterior PDF median residuals), moving to similar or equal to 39% when we include all the significant spectral features in the wavelength range 900 - 3000 angstrom.

  • 2. Hunter, Deidre A.
    et al.
    Gallardo, Samavarti
    Zhang, Hong-Xin
    Adamo, Angela
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Cook, David O.
    Oh, Se-Heon
    Elmegreen, Bruce G.
    Kim, Hwihyun
    Kahre, Lauren
    Ubeda, Leonardo
    Bright, Stacey N.
    Ryon, Jenna E.
    Fumagalli, Michele
    Sacchi, Elena
    Kennicutt, R. C.
    Tosi, Monica
    Dale, Daniel A.
    Cignoni, Michele
    Messa, Matteo
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Grebel, Eva K.
    Gouliermis, Dimitrios A.
    Sabbi, Elena
    Grasha, Kathryn
    Gallagher, John S.
    Calzetti, Daniela
    Lee, Janice C.
    A Study of Two Dwarf Irregular Galaxies with Asymmetrical Star Formation Distributions2018In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 855, no 1, article id 7Article in journal (Refereed)
    Abstract [en]

    Two dwarf irregular galaxies, DDO 187 and NGC 3738, exhibit a striking pattern of star formation: intense star formation is taking place in a large region occupying roughly half of the inner part of the optical galaxy. We use data on the H I distribution and kinematics and stellar images and colors to examine the properties of the environment in the high star formation rate (HSF) halves of the galaxies in comparison with the low star formation rate halves. We find that the pressure and gas density are higher on the HSF sides by 30%-70%. In addition we find in both galaxies that the H I velocity fields exhibit significant deviations from ordered rotation and there are large regions of high-velocity dispersion and multiple velocity components in the gas beyond the inner regions of the galaxies. The conditions in the HSF regions are likely the result of large-scale external processes affecting the internal environment of the galaxies and enabling the current star formation there.

  • 3. Krumholz, Mark R.
    et al.
    Adamo, Angela
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC). Centre of Excellence for Astronomy in Three Dimensions (ASTRO-3D), Australia.
    Fumagalli, Michele
    Calzetti, Daniela
    SLUG IV: a novel forward-modelling method to derive the demographics of star clusters2019In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 482, no 3, p. 3550-3566Article in journal (Refereed)
    Abstract [en]

    We describe a novel method for determining the demographics of a population of star clusters, for example distributions of cluster mass and age, from unresolved photometry. This method has a number of desirable properties: it fully exploits all the information available in a data set without any binning, correctly accounts for both measurement error and sample incompleteness, naturally handles heterogenous data (e.g. fields that have been imaged with different sets of filters or to different depths), marginalizes over uncertain extinctions, and returns the full posterior distributions of the parameters describing star cluster demographics. We demonstrate the method using mock star cluster catalogues and show that our method is robust and accurate, and that it can recover the demographics of star cluster populations significantly better than traditional fitting methods. For realistic sample sizes, our method is sufficiently powerful that its accuracy is ultimately limited by the accuracy of the underlying physical models for stellar evolution and interstellar dust, rather than by statistical uncertainties. Our method is implemented as part of the Stochastically Lighting Up Galaxies (SLUG) stellar populations code, and is freely available.

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