Sampling, Intervention, Prediction, Aggregation: A Generalized Framework for Model-Agnostic Interpretations

Model-agnostic interpretation techniques allow us to explain the behavior of any predictive model. Due to different notations and terminology, it is difficult to see how they are related. A unified view on these methods has been missing. We present the generalized SIPA (sampling, intervention, prediction, aggregation) framework of work stages for model-agnostic interpretations and demonstrate how several prominent methods for feature effects can be embedded into the proposed framework. Furthermore, we extend the framework to feature importance computations by pointing out how variance-based and performance-based importance measures are based on the same work stages. The SIPA framework reduces the diverse set of model-agnostic techniques to a single methodology and establishes a common terminology to discuss them in future work

SBS 0335-052W - an Extremely Low Metallicity Dwarf Galaxy

We present Multiple Mirror Telescope (MMT) and Keck II telescope spectrophotometry and 3.5m Calar Alto telescope R, I photometry of the western component of the extremely low-metallicity blue compact galaxy SBS 0335-052. The components, separated by 22 kpc, appear to be members of a unique, physically connected system. It is shown that SBS 0335-052W consists of at least three stellar clusters and has the same redshift as SBS 0335-052. The oxygen abundance in its two brightest knots is extremely low, 12+log(O/H)= 7.22+/-0.03 and 7.13+/-0.08, respectively. These values are lower than in SBS 0335-052 and are nearly the same as those in I Zw 18. The (R-I) color profiles are very blue in both galaxies due to the combined effects of ionized gas and a young stellar population emission. We argue that SBS 0335-052W is likely to be a nearby, young dwarf galaxy.Comment: 18 pages, 4 EPS figures, to appear in ApJ, 1 July 199

Wide Field Imaging. I. Applications of Neural Networks to object detection and star/galaxy classification

[Abriged] Astronomical Wide Field Imaging performed with new large format CCD detectors poses data reduction problems of unprecedented scale which are difficult to deal with traditional interactive tools. We present here NExt (Neural Extractor): a new Neural Network (NN) based package capable to detect objects and to perform both deblending and star/galaxy classification in an automatic way. Traditionally, in astronomical images, objects are first discriminated from the noisy background by searching for sets of connected pixels having brightnesses above a given threshold and then they are classified as stars or as galaxies through diagnostic diagrams having variables choosen accordingly to the astronomer's taste and experience. In the extraction step, assuming that images are well sampled, NExt requires only the simplest a priori definition of "what an object is" (id est, it keeps all structures composed by more than one pixels) and performs the detection via an unsupervised NN approaching detection as a clustering problem which has been thoroughly studied in the artificial intelligence literature. In order to obtain an objective and reliable classification, instead of using an arbitrarily defined set of features, we use a NN to select the most significant features among the large number of measured ones, and then we use their selected features to perform the classification task. In order to optimise the performances of the system we implemented and tested several different models of NN. The comparison of the NExt performances with those of the best detection and classification package known to the authors (SExtractor) shows that NExt is at least as effective as the best traditional packages.Comment: MNRAS, in press. Paper with higher resolution images is available at http://www.na.astro.it/~andreon/listapub.htm

Spectroscopic and photometric studies of low-metallicity star-forming dwarf galaxies. I. SBS 1129+576

Spectroscopy and V,I CCD photometry of the dwarf irregular galaxy SBS 1129+576 are presented for the first time. The CCD images reveal a chain of compact H II regions within the elongated low-surface-brightness (LSB) component of the galaxy. Star formation takes place mainly in two high-surface-brightness H II regions. The mean (V-I) colour of the LSB component in the surface brightness interval between 23 and 26 mag/sq.arcsec is relatively blue ~0.56+/-0.03 mag, as compared to the (V-I)~0.9-1.0 for the majority of known dwarf irregular and blue compact dwarf (BCD) galaxies. Spectroscopy shows that the galaxy is among the most metal-deficient galaxies with an oxygen abundance 12+log(O/H)= 7.36+/-0.10 in the brightest H II region and 7.48+/-0.12 in the second brightest H II region, or 1/36 and 1/28 of the solar value, respectively. Hbeta and Halpha emission lines and Hdelta and Hgamma absorption lines are detected in a large part of the LSB component. We use two extinction-insensitive methods based on the equivalent widths of (1) emission and (2) absorption Balmer lines to put constraints on the age of the stellar populations in the galaxy. In addition, we use two extinction-dependent methods based on (3) the spectral energy distribution (SED) and (4) the (V-I) colour. The observed properties of the LSB component can be reproduced by a stellar population forming continuously since 10 Gyr ago, provided that the star formation rate has increased during the last 100 Myr by a factor of 6 to 50 and no extinction is present. However, the observational properties of the LSB component can be reproduced equally well by continuous star formation which started not earlier than 100 Myr ago and stopped at 5 Myr, if some extinction is assumed.(Abridged)Comment: 17 pages, 12 figures, Accepted for publication in A&

An Atlas of Warm AGN and Starbursts from the IRAS Deep Fields

We present 180 AGN candidates based on color selection from the IRAS slow-scan deep observations, with color criteria broadened from the initial Point-Source Catalog samples to include similar objects with redshifts up to z=1 and allowing for two-band detections. Spectroscopic identifications have been obtained for 80 (44%); some additional ones are secure based on radio detections or optical morphology, although yet unobserved spectroscopically. These spectroscopic identifications include 13 Sy 1 galaxies, 17 Sy 2 Seyferts, 29 starbursts, 7 LINER systems, and 13 emission-line galaxies so heavily reddened as to remain of ambiguous classification. The optical magnitudes range from R=12.0-20.5; counts suggest that incompleteness is important fainter than R=15.5. Redshifts extend to z=0.51, with a significant part of the sample at z>0.2. The sample includes slightly more AGN than star-forming systems among those where the spectra contain enough diagnostic feature to make the distinction. The active nuclei include several broad-line objects with strong Fe II emission, and composite objects with the absorption-line signatures of fading starbursts. These AGN with warm far-IR colors have little overlap with the "red AGN" identified with 2MASS; only a single Sy 1 was detected by 2MASS with J-K > 2. Some reliable IRAS detections have either very faint optical counterparts or only absorption-line galaxies, potentially being deeply obscured AGN. The IRAS detections include a newly identified symbiotic star, and several possible examples of the "Vega phenomenon", including dwarfs as cool as type K. Appendices detail these candidate stars, and the optical-identification content of a particularly deep set of high-latitude IRAS scans (probing the limits of optical identification from IRAS data alone).Comment: ApJ Suppl, in press. Figures converted to JPEG/GIF for better compression; PDF with full-resolution figures available before publication at http://www.astr.ua.edu/keel/aoagn.pd

Study of DDO 68: nearest candidate for a young galaxy?

We present the results of optical spectroscopy and imaging with the SAO 6m telescope for the dwarf galaxy DDO 68 (UGC 5340 = VV 542), falling into the region of very low density of luminous (L > L*) galaxies (Lynx-Cancer void). Its deep images in V,R bands and in the narrow H-alpha-filter show that the galaxy has the very irregular morphology, with a long curved tail on the South and a ring-like structure at the Northern edge. The latter consists of 5 separate regions, in three of which we could measure O/H by the classical T_e method. Their weighted mean oxygen abundance corresponds to 12+log(O/H)=7.21+-0.03, coincident within uncertainties with those for IZw18. The (V-R) colour of DDO 68 is rather blue all over the galaxy, indicating the youth of its stellar populations. Comparing the (V-R)_0 colour of the underlying exponential disk of 0.12+-0.04 with the PEGASE.2 models for the evolving stellar clusters, we give the first estimate of the ages of the oldest stellar population, which needs confirmation by the other colours and the photometry of resolved stars. These ages are in the range of 200-900 Myr for continuous star formation law, and 100-115 Myr for the instantaneous starburst. We discuss the properties and the possible youth of this nearby object (2.3 times closer than the famous young galaxy IZw18) in the context of its atypical environment.Comment: 13 pages, including 7 tables and 3 postscript figures. Accepted for publication in Astron.Astrophys. Small language corrections are made after the A&A Language Edito

Modeling the emission line sequence of H II galaxies

Using a sample of unprecedented size (about 400 objects) of H II galaxies in which the oxygen abundances have been obtained using the temperature derived from the [OIII] 4363/5007 line ratio, we confirm that the H II galaxies form a very narrow sequence in many diagrams relating line ratios and Hbeta equivalent width. We divide our sample in three metallicity bins, each of which is compared with sequences of photoionization models for evolving starbursts with corresponding metallicity. Our aim is to find under what conditions a theoretical sequence can reproduce all the observed trends. Taking into account the presence of an older, non-ionizing stellar population, for which independent indications exist, we find that the simple model of an adiabatic expanding bubble reproduces the observational diagrams very well if account is taken of an aperture correction and the covering factor is assumed to decrease with time exponentially with an e-folding time of 3 Myr. We find that the He II 4686 nebular line emission occurs too frequently and in too wide a range of EW(Hbeta) to be attributable to either the hard radiation field from Wolf-Rayet stars or the X-rays produced by the latest stellar generation. Assuming that the He II 4686 line is due to photoionization by a hot plasma at a temperature of 10^6 K, a total X-ray luminosity of 10^40 - 4x10^40 erg/s is required for at least half of the sources. We find evidence for self-enrichment in nitrogen on a time scale of several Myr, and argue for a possible self-enrichment in oxygen as well.Comment: 15 pages, 6 Postscript figures, to appear in Astronomy & Astrophysic

Changing youth? : continuities and ruptures in transitions into adulthood among Catalan young people

The globalisation process has an impact at the micro-level on life-course patterns: concretely, the trajectories of young people into adulthood are being sharply modified. At a European level, the extension, de-linearisation, reversibility and diversification of youth trajectories have been identified as major changes. However, the extent to which these changes affect young people within each country depends on their respective welfare regimes. This article analyses how the Mediterranean welfare regime shapes youth trajectories among Catalan young people and explores the hypothesis that these constraints will make those trajectories less sensitive to the general trends of change identified at a European level. The research is based on an analysis of the Catalan Youth Survey, an official statistic that contains retrospective data on Educational, Work, Housing and Family transitions. The results offer an integrated typology of youth transitions in Catalonia and show how the persistence of traditional patterns of transition are the logical result of the particular articulation of the welfare regime and cultural patterns among Catalan young people

Communication studies cartography in the Lusophone world

Within the Lusophone community of over 250 million speakers only a minority developed a sense of belonging based on their common language, a phenomenon that is still very real today. According to the Mozambican writer, Mia Couto, Lusophony is not a ‘loud’ reality, rather a “luso-aphonic” one, that is, a place of low voices, no knowledge and no acknowledgement of the commonalities between themselves in this vast geographic and cultural space. Recognizing precisely this gap, Communication research associations in Lusophone countries (Lusocom) have promoted the setting up of a research cooperation network primarily between Portuguese and Brazilian researchers, and then extending it to the Galician community, and subsequently to the entire Lusophone space. This movement is based on the assumption that linguistic diversity enriches science and that science should be globally and contextually relevant. Lusophony can be discussed from various points of view, all related to the cultural identity of the Portuguese-speaking countries. I would like to explain my point of view, focused on the social status of language. Then, I will refer to the English language has a dominant language. Finally, I would like to point out some challenges that, from my perspective, the Lusophone research groups have to face in a global world dominated by English and anglo-saxon paradigms. My approach is in fact focused on the perspective of language, understood as a cultural manifestation, the expression of thought, a relational space, and an instrument of symbolic organization of the world. Such understanding is coincident with the symbolic power of language (Pierre Bourdieu’s theory), and with the post-colonial perspective which questions the domination, submission, subordination and control of peripheries, minorities, diasporas, migrants…(undefined)info:eu-repo/semantics/publishedVersio