Examinando por Autor "Runco, J. N."

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Acceso Abierto
Herschel/PACS OH Spectroscopy of Seyfert, LINER, and Starburst Galaxies
(The Institute of Physics (IOP), 2020-12-11) Runco, J. N.; Malkan, M. A.; Fernández Ontiveros, J. A.; Spinoglio, L.; Pereira Santaella, M.; Agenzia Spaziale Italiana (ASI); Science and Technology Facilities Council (STFC); Comunidad de Madrid; National Aeronautics and Space Administration (NASA); 0000-0003-4852-8958; 0000-0001-6919-1237; 0000-0001-9490-899X; 0000-0001-8840-1551; 0000-0002-4005-9619; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
We investigated the 65, 71, 79, 84, 119, and 163 μm OH doublets of 178 local (0 < z < 0.35) galaxies. They were observed using the Herschel/Photoconductor Array Camera and Spectrometer, including Seyfert galaxies, low-ionization nuclear emission-line regions, and star-forming galaxies. We observe these doublets exclusively in absorption (OH71), primarily in absorption (OH65, OH84), mostly in emission (OH79), only in emission (OH163), and an approximately even mix of the both (OH119). In 19 galaxies we find P Cygni or reverse P Cygni line profiles in the OH doublets. We use several galaxy observables to probe spectral classification, brightness of a central active galactic nucleus (AGN)/starburst component, and radiation field strength. We find that OH79, OH119, and OH163 are more likely to display strong emission for bright, unobscured AGNs. For less luminous, obscured AGNs and nonactive galaxies, we find populations of strong absorption (OH119), weaker emission (OH163), and a mix of weak emission and weak absorption (OH79). For OH65, OH71, and OH84, we do not find significant correlations with the observables listed above. For OH79 and OH119, we find relationships with both the 9.7 μm silicate feature and Balmer decrement dust extinction tracers in which more dust leads to weaker emission/stronger absorption. The origin of emission for the observed OH doublets, whether from collisional excitation or from radiative pumping by infrared photons, is discussed.
Restringido
Phase Identification and Temperature-Dependent Magnetization of Ti-Rich Titanomagnetite (0.5 <= x <= 1) in Different Atmospheres
(Institute of Electrical and Electronics Engineers, 2013-07-15) Lan, S.; Groschner, C.; Runco, J. N.; Wise, A.; Díaz Michelena, M.; Laughlin, David E.; McHenry, M. E.
Reduced titanomagnetite solid solutions, xFe 2 TiO 4 - (1 - x)Fe 3 O 4 , with 0.5 ≤ × ≤ 1, were synthesized by sintering in 99.996% pure flowing argon. Samples showed a systematic variation in the second phase amount as a function of x. A wustite second phase primarily forms near the surface of titanomagnetite pellets. The amount of wustite decreases with increasing Ti concentration. XRD data confirms that samples with x > 0.8 have less than 1% wustite. M(T) curves were measured by vibrating sample magnetometer (VSM). A magnetization hump is observed in M(T) during heating and explained by ferrimagnetic phases formed by exsolution and precipitation processes. These phases were identified as titanomaghemite and magnetite by fitting M(T) cooling curves with a multi-phase Brillouin function.