The Internationality Index of the Spanish Psychology journals

The concept of international publication is one of the most utilized criteria to evaluate the productivity of researchers and scientific institutions. Nevertheless, it is also one of the most polemic subjects as until the presence, no Internationality Index has been defined nor established. This descriptive study analyzes the Spanish Psychology journals included in the IN-RECS database according to the level of the internationality. Each journal was evaluated taking into account the eleven criteria of the internationality (the publication language, the impact factor -in this case the Impact Index according to the IN-RECS database-, the countries from which the members of the editorial boards are, the names of the journals, the inclusion in the Journal Citation Reports, the countries from which the authors are, the standards of publication, the internet access, the free internet access, the inclusion in the databases, and the journal’s affiliation to “international” associations). The scores of each journal in all criteria were summed up and sorted by the total scores in the internationality in the descending order which resulted in the Internationality Index of the Spanish Psychology Journals. It is important to emphasize that four of the five journals which occupy the highest positions in the ranking are indexed in the Web of Science.El concepto de publicación internacional es uno de los criterios más utilizado para evaluar la productividad de los investigadores y de las instituciones científicas. Sin embargo, también es uno de los más polémicos, dado que hasta la actualidad no se había definido ni establecido un Índice de Internacionalidad. Este estudio descriptivo analiza las revistas españolas de Psicología incluidas en la base de datos IN-RECS según su nivel de internacionalidad. Cada revista fue evaluada teniendo en cuenta los once criterios de internacionalidad (idioma de publicación, factor de impacto -en este caso el Índice de Impacto según IN-RECS-, países de procedencia de los miembros del los comités editoriales, nombres de la revista, inclusión en el Journal Citation Reports, países de procedencia de los autores, normas de publicación, acceso por internet, acceso por internet gratuito, inclusión en bases de datos y pertenencia a las instituciones “internacionales”). Se sumaron las puntuaciones en todos los criterios y los totales fueron ordenados de mayor a menor dando como resultado el Índice de Internacionalidad de las Revistas Españolas de Psicología. Entre los resultados cabe resaltar que de las cinco primeras revistas del ranking de internacionalidad cuatro son revistas indexadas en la Web of Science.O conceito de publicação internacional é um dos critérios mais utilizados para avaliar a produtividade dos investigadores e das instituições científicas. No entanto, também é um dos mais polémicos, dado que até à actualidade não se tinha definido nem estabelecido um índice de Internacionalidade. Este estudo descritivo analisa as revistas espanholas de Psicologia incluídas na base de dados IN-RECS segundo o seu nível de internacionalidade. Cada revista foi avaliada tendo em conta os onze critérios de internacionalidade (idioma de publicação, factor de impacto – neste caso o Índice de Impacto segundo IN-RECS-, países de procedência dos membros dos comités editoriais, números da revista, inclusão no Journal Citation Reports, países de procedência dos autores, normas de publicação, acesso pela Internet, acesso pela Internet gratuito, inclusão em bases de dados e pertença a instituições “internacionais”). Somaram-se as pontuações em todos os critérios e os totais foram ordenados de maior para menor dando como resultado o índice de Internacionalidade das Revistas Espanholas de Psioclogia. Entre os resultados cabe ressaltar que das cinco primeiras revistas do ranking de internacionalidade quatro são revistas indexadas na Web of Science.The study has been financed by Dirección General de Universidades (Ministerio de Educación y Ciencia) (Reference: EA2006-0016)

On the co-evolution of supermassive black holes and their host galaxies since z = 3

[Abridged] To investigate the evolution in the relation between galaxy stellar and central black hole mass we construct a volume limited complete sample of 85 AGN with host galaxy stellar masses M_{*} > 10^{10.5} M_{sol}, and specific X-ray luminosities L_{X} > 2.35 x 10^{43} erg s^{-1} at 0.4 < z < 3. We calculate the Eddington limiting masses of the supermassive black holes residing at the centre of these galaxies, and observe an increase in the average Eddington limiting black hole mass with redshift. By assuming that there is no evolution in the Eddington ratio (\mu) and then that there is maximum possible evolution to the Eddington limit, we quantify the maximum possible evolution in the M_{*} / M_{BH} ratio as lying in the range 700 < M_{*}/M_{BH} < 10000, compared with the local value of M_{*}/M_{BH} ~ 1000. We furthermore find that the fraction of galaxies which are AGN (with L_{X} > 2.35 x 10^{43} erg s^{-1}) rises with redshift from 1.2 +/- 0.2 % at z = 0.7 to 7.4 +/- 2.0 % at z = 2.5. We use our results to calculate the maximum timescales for which our sample of AGN can continue to accrete at their observed rates before surpassing the local galaxy-black hole mass relation. We use these timescales to calculate the total fraction of massive galaxies which will be active (with L_{X} > 2.35 x 10^{43} erg s^{-1}) since z = 3, finding that at least ~ 40% of all massive galaxies will be Seyfert luminosity AGN or brighter during this epoch. Further, we calculate the energy density due to AGN activity in the Universe as 1.0 (+/- 0.3) x 10^{57} erg Mpc^{-3} Gyr^{-1}, potentially providing a significant source of energy for AGN feedback on star formation. We also use this method to compute the evolution in the X-ray luminosity density of AGN with redshift, finding that massive galaxy Seyfert luminosity AGN are the dominant source of X-ray emission in the Universe at z < 3.Comment: 25 pages, 10 figures, accepted for publication in MNRA

Measurements of CaII absorption, metals, and dust in a sample of z~1 DLAs and subDLAs

We present observations of CaII, ZnII, and CrII absorption lines in 16 DLAs and 6 subDLAs at 0.6 < z < 1.3, obtained for the dual purposes of: (i) clarifying the relationship between DLAs and absorbers selected via strong CaII lines, and (ii) increasing the still limited sample of Zn and Cr abundances in this redshift range. We find only partial overlap between current samples of intermediate-z DLAs (which are drawn from magnitude limited surveys) and strong CaII absorbers: approximately 25% of known DLAs at these redshifts have an associated CaII 3935 line with REW>0.35A, the threshold of the SDSS sample assembled by Wild and her collaborators. The lack of the strongest systems (with REW>0.5A) is consistent with these authors' conclusion that such absorbers are often missed in current DLA surveys because they redden/dim the light of the background QSOs. We rule out the suggestion that strong CaII absorption is associated exclusively with the highest-N(HI) DLAs. Furthermore, we find no correlation between the strength of the CaII lines and either the metallicity or depletion, although the strongest CaII absorber in our sample is also the most metal-rich DLA yet discovered, with [Zn/H] ~ solar. We conclude that a complex mix of parameters determine the strengths of the CaII lines, including the density of particles and UV photons in the ISM of the galaxies hosting the DLAs. We find tentative evidence (given the small size of our sample) that strong CaII systems may preferentially sample regions of high gas density, perhaps akin to the DLAs exhibiting molecular hydrogen absorption at redshifts z>2. If this connection is confirmed, strong CaII absorbers would trace possibly metal-rich, H2-bearing columns of cool, dense gas at distances up to tens of kpc from normal galaxies. (abridged)Comment: Accepted for publication in MNRAS; 15 pages, 10 figure

Performance of the CMS Cathode Strip Chambers with Cosmic Rays

The Cathode Strip Chambers (CSCs) constitute the primary muon tracking device in the CMS endcaps. Their performance has been evaluated using data taken during a cosmic ray run in fall 2008. Measured noise levels are low, with the number of noisy channels well below 1%. Coordinate resolution was measured for all types of chambers, and fall in the range 47 microns to 243 microns. The efficiencies for local charged track triggers, for hit and for segments reconstruction were measured, and are above 99%. The timing resolution per layer is approximately 5 ns

Performance and Operation of the CMS Electromagnetic Calorimeter

The operation and general performance of the CMS electromagnetic calorimeter using cosmic-ray muons are described. These muons were recorded after the closure of the CMS detector in late 2008. The calorimeter is made of lead tungstate crystals and the overall status of the 75848 channels corresponding to the barrel and endcap detectors is reported. The stability of crucial operational parameters, such as high voltage, temperature and electronic noise, is summarised and the performance of the light monitoring system is presented

Swift UV/Optical Telescope Imaging of Star Forming Regions in M81 and Holmberg IX

We present Swift UV/Optical Telescope (UVOT) imaging of the galaxies M81 and Holmberg IX. We combine UVOT imaging in three near-ultraviolet (NUV) filters (uvw2: 1928 Å; uvm2: 2246 Å; uvw1: 2600 Å) with ground-based optical imaging from the Sloan Digital Sky Survey to constrain the stellar populations of both galaxies. Our analysis consists of three different methods. First, we use the NUV imaging to identify UV star-forming knots and then perform spectral energy distribution (SED) modeling on the UV/optical photometry of these sources. Second, we measure surface brightness profiles of the disk of M81 in the NUV and optical. Lastly, we use SED fitting of individual pixels to map the properties of the two galaxies. In agreement with earlier studies, we find evidence for a burst in star formation in both galaxies starting ~200 Myr ago coincident with the suggested time of an M81-M82 interaction. In line with theories of its origin as a tidal dwarf, we find that the luminosity-weighted age of Holmberg IX is a few hundred million years. Both galaxies are best fit by a Milky Way dust extinction law with a prominent 2175 Å bump. In addition, we describe a stacked median filter technique for modeling the diffuse background light within a galaxy and a Markov chain method for cleaning segment maps generated by SExtractor

Calibration of the CMS Drift Tube Chambers and Measurement of the Drift Velocity with Cosmic Rays

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CMS Data Processing Workflows during an Extended Cosmic Ray Run

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Aligning the CMS Muon Chambers with the Muon Alignment System during an Extended Cosmic Ray Run

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CMS physics technical design report : Addendum on high density QCD with heavy ions

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