ORCID Profile
0000-0001-6150-2854
Current Organisation
Universidad Complutense de Madrid
Does something not look right? The information on this page has been harvested from data sources that may not be up to date. We continue to work with information providers to improve coverage and quality. To report an issue, use the Feedback Form.
Publisher: American Astronomical Society
Date: 12-2007
DOI: 10.1086/523853
Publisher: American Astronomical Society
Date: 07-2008
DOI: 10.1086/588580
Publisher: EDP Sciences
Date: 10-2016
Publisher: American Astronomical Society
Date: 06-02-2020
Publisher: American Astronomical Society
Date: 17-01-2019
Publisher: American Astronomical Society
Date: 02-2021
Publisher: American Astronomical Society
Date: 12-2007
DOI: 10.1086/516642
Publisher: Oxford University Press (OUP)
Date: 22-11-2019
Abstract: Using Hubble Space Telescope ACS/WFC data we present the photometry and spatial distribution of resolved stellar populations of four fields within the extended ultraviolet disc (XUV disc) of M83. These observations show a clumpy distribution of main-sequence stars and a mostly smooth distribution of red giant branch stars. We constrain the upper end of the initial mass function (IMF) in the outer disc using the detected population of main-sequence stars and an assumed constant star formation rate (SFR) over the last 300 Myr. By comparing the observed main-sequence luminosity function to simulations, we determine the best-fitting IMF to have a power-law slope α = −2.35 ± 0.3 and an upper mass limit $M_{\\rm u}=25_{-3}^{+17} \\, \\mathrm{M}_\\odot$. This IMF is consistent with the observed H $\\rm \\alpha$ emission, which we use to provide additional constraints on the IMF. We explore the influence of deviations from the constant SFR assumption, finding that our IMF conclusions are robust against all but strong recent variations in SFR, but these are excluded by causality arguments. These results, along with our similar studies of other nearby galaxies, indicate that some XUV discs are deficient in high-mass stars compared to a Kroupa IMF. There are over one hundred galaxies within 5 Mpc, many already observed with HST, thus allowing a more comprehensive investigation of the IMF, and how it varies, using the techniques developed here.
Publisher: American Astronomical Society
Date: 27-07-2005
DOI: 10.1086/444534
Publisher: American Astronomical Society
Date: 20-01-2006
DOI: 10.1086/498296
Publisher: Royal Society of Chemistry (RSC)
Date: 2019
DOI: 10.1039/C9NA00435A
Abstract: Defective Mo(S,Se) 2 and (Mo,W)S 2 nanosheets are synthesized by a supercritical hydrothermal process without highly toxic sources in a short time.
Publisher: American Astronomical Society
Date: 27-07-2020
Publisher: Royal Society of Chemistry (RSC)
Date: 2018
DOI: 10.1039/C8RA07205A
Abstract: Structural defects, including point defects, dislocation and planar defects, significantly affect the physical and chemical properties of low-dimensional materials, such as layered compounds.
Publisher: American Astronomical Society
Date: 18-03-2005
DOI: 10.1086/429377
Publisher: American Astronomical Society
Date: 17-01-2005
DOI: 10.1086/425251
Publisher: Oxford University Press (OUP)
Date: 18-04-2023
Abstract: Multiwavelength studies indicate that nuclear activity and bulge properties are closely related, but the details remain unclear. To study this further, we combine Hubble Space Telescope bulge structural and photometric properties with 1.5 GHz, e-MERLIN nuclear radio continuum data from the LeMMINGs survey for a large s le of 173 ‘active’ galaxies (LINERs and Seyferts) and ‘inactive’ galaxies (H iis and absorption line galaxies, ALGs). Dividing our s le into active and inactive, they define distinct (radio core luminosity)–(bulge mass), $L_{\\rm R,core}-M_{*, \\rm bulge}$ , relations, with a mass turnover at $M_{*, \\rm bulge}\\sim 10^{9.8 \\pm 0.3} \\rm { M_{\\odot }}$ (supermassive blackhole mass $M_{\\rm BH} \\sim 10^{6.8 \\pm 0.3} \\rm M_{\\odot }$ ), which marks the transition from AGN-dominated nuclear radio emission in more massive bulges to that mainly driven by stellar processes in low-mass bulges. None of our 10/173 bulge-less galaxies host an AGN. The AGN fraction increases with increasing $M_{*,\\rm bulge}$ such that $f_{\\rm optical\\_AGN}\\propto M_{*,\\rm bulge}^{0.24 \\pm 0.06}$ and $f_{\\rm radio\\_AGN}\\propto M_{*,\\rm bulge}^{0.24 \\pm 0.05}$ . Between $M_{*,\\rm bulge}\\sim 10^{8.5}$ and $10^{11.3} \\rm M_{\\odot }$ , $f_{\\rm optical\\_AGN}$ steadily rises from 15 ± 4 to 80 ± 5 per cent. We find that at fixed bulge mass, the radio loudness, nuclear radio activity, and the (optical and radio) AGN fraction exhibit no dependence on environment. Radio-loud hosts preferentially possess an early-type morphology than radio-quiet hosts, the two types are however indistinguishable in terms of bulge Sérsic index and ellipticity, while results on the bulge inner logarithmic profile slope are inconclusive. We finally discuss the importance of bulge mass in determining the AGN triggering processes, including potential implications for the nuclear radio emission in nearby galaxies.
Publisher: American Astronomical Society
Date: 17-10-2019
Publisher: Elsevier BV
Date: 03-2020
Publisher: American Astronomical Society
Date: 10-11-2006
DOI: 10.1086/507766
Publisher: American Astronomical Society
Date: 22-07-2016
Publisher: American Astronomical Society
Date: 11-02-2021
No related grants have been discovered for Armando Gil de Paz.