bluuebunny/crossref_metadata_2025 huggingface dataset:
Los negocios de Cabarrús con la Real Hacienda (1780–1783)
Authors: de Lorca Pedro Tedde
Published: June 2010

Francisco Cabarrús, banquero madrileño de origen francés, vinculado financieramente a un activo grupo de comerciantes y cambistas también franceses—con enclaves en París y Cádiz—, además de a otras casas españolas, y relacionado política e intelectualmente con la minoría ilustrada, en los últimos años del decenio de 1770 y primeros del siguiente, fue el principal responsable de la emisión de vales reales, peculiar modalidad de deuda pública que llevaba incorporadas características de papel moneda. Como Hamilton ha revelado, ése es el primer ensayo de circulación de dinero en billetes en España. El presente artículo se dirige a demostrar que la emisión de vales reales se inscribe en un conjunto de operaciones crediticias que Cabarrús desarrolló para auxiliar a la Real Hacienda en los años en que España intervino en la guerra de independencia de los Estados Unidos. También se intentan explicar las circunstancias de estas emisiones, las reacciones que suscitaron, los efectos económicos que produjeron, así como el beneficio derivado de todo ello para la economía particular del propio banquero.
La sericicultura murciana. Producción, difusión y coyuntura, siglos XVI–XX
Authors: Picazo M. Teresa Perez , Lemeunier Guy
Published: June 2010

La sericicultura murciana presenta una serie de rasgos específicos que permiten considerarla como un caso particular de este tipo de aprovechamiento.

Primero, su evolución sigue una cronología distinta a la de otras regiones vecinas como Andalucía o Valencia, donde la producción sedera fue más precoz, tanto en el despegue como en la desaparición. En ambas, el cultivo de la morera aparece antes del xvi y se hunde en la segunda mitad del xix, mientras que en Murcia surge en las primeras décadas del quinientos y sobrevive hasta después de la guerra civil.
Grupos empresariales e inversion de capital en Vizcaya, 1886–1913
Authors: Gago Jesus Ma. Valdaliso
Published: June 2010

Esta investigación se basa en una explotación sistemática de una fuente hasta ahora sólo utilizada para reconstruir indicadores económicos de larga duración, los Libros de Sociedades del Registro Mercantil. Pero, además, es susceptible de una explotación mucho más intensiva que consistíne, básicamente, en la reconstrucción de los grupos empresariales y de su dinámica inversore, mediante la recogida de los nombres de los inversores que aparecen en las Escrituras de Constitución de cada Sociedad.
Leon Walras en la historiografia del pensamiento economico: Materiales para una reinterpretacion
Authors: Segura Julio
Published: June 2010

La obra de Léon Walras (1834–1910) es, en su mayoría, casi desconocida, incluso por el público especializado. La escasa lectura directa de Walras ha dado lugar a la transmisión de una imagen incompleta y, lo que es peor, deformada de uno de los economistas más importantes de la historia del pensamiento económico.

Existen varias razones que explican el porqué la escasa lectura de Walras. En primer lugar, su obra, muy extensa y dispersa, está escrita en un estilo farragoso y reiterativo que no sólo la convierte en poco atractiva desde el punto de vista literario, sino que, además, la hace a veces poco inteligible.
La crisis de 1873 y la deuda externa latinoamericana: Una reevaluacion critica
Authors: Marichal Carlos
Published: June 2010

Hace algunos años, el historiador inglés D. C. M. Platt publicó un incisivo artícule. en el Economic History Review en el cual hizo un llamado para que se efectuara una revisión global de las estimaciones estadísticas de las exportaciones de capital británico a lo largo del siglo XIX. Más recientemente, el mismo autor ha publicado un libro que profundiza en esta temática y que está destinado a provocar cambios significativos en la manera en que los historiadores interpretan la cantidad, el origen, las funciones y la distribución de la inversión de capital en Europa y Estados Unidos desde 1815 hasta 1870.
Politica y negocios: En torno a las «Memorias» de Cambo
Authors: Gortazar Guillermo
Published: June 2010

La reciente publicación de las Memorias de Francisco Cambó (1876–1936) en Alianza Editorial y una nueva biografía escrita por Ignacio Buqueras en Plaza y Janés, en su colección de Biografías y Memorias, ha reactualizado la figura de uno de los principales protagonistas de la vida política y económica española del primer tercio del siglo XX.

Desde el punto de vista de la historia política, las Memorias constituyen lectura obligada, en particular en lo que se refiere a la explicación de la forma en la que el nacionalismo moderado catalán, el catalanismo, supo convertirse en una poderosa y constructiva palanca de gobierno y de canalización del sentimiento nacionalista.
La coyuntura de la mineria y de la metalurgia europeas (siglos XIII–XVIII)
Authors: de Prada Valentin Vazquez
Published: June 2010

Resulta, sin duda, excesivamente atrevido el tratar de esbozar la coyuntura de la minería y la metalurgia europeas durante más de cinco siglos. La variabilidad de la producción y las vacilaciones de la demanda, impuestas por razones í, tecnológicas y económicas, hacen la empresa muy difícil. Un recurso, casi imprescindible, es el de soslayar la producción de aquellos metales menos significativos, a la vez que intentar ofrecer una perspectiva general que recoja los grandes trazos de la coyuntura.
Importacion, Niveles de Proteccion Y Produccion Del Material Electrico En España (1890–1935)
Authors: Junguito Antonio Tena
Published: June 2010

Los cambios que tuvieron lugar en las economías de los países occidentales desde los últimos años del siglo xix hasta el primer tercio del xx han venido asimilándose por la literatura reciente a la aceleración de la productividad de los factores producida por la rápida incorporación de nuevas tecnologías y cambios en los sistemas de organización de las empresas. Una de las principales nuevas tecnologías que contribuyeron a esta aceleración fue la incorporación y rápida expansión de la electricidad en el proceso productivo.
La Electrificacion de la Periferia Un tema recuperado recientemente por la historiografía
Authors: Romero-Balmas Gregorio Nuñez
Published: June 2010

La creación en 1982 de la Association pour l'Histoire de l'Electricité en France ha representado una fecunda llamada de atención sobre un tema hasta hace poco tiempo olvidado en países como Francia y España: el desarrollo industrial de la electricidad desde 1880. La simple enumeración de sus fundadores podría dar cuenta de la importancia del proyecto, y los nombres Maurice Aymard, François Bédarida, Fernand Braudel, François Caron y Michel Crozier resultan familiares para cualquier historiador o estudioso de las ciencias sociales; a ellos hay que añadir los de altos funcionarios de la Administración francesa como George Maleville, Jean Claude Colli y Guy Thuillier, e importante sdirectivos de la empresa nacional Electricité de France, con el presidente mismo de su consejo de administración, Marcel Boiteux. Unos y otros dan muestra del interés por el tema, que viene a atender a un doble aniversario: el centenario de la electrificación, que convencionalmente ha sido establecido en 1980, y el 40 aniversario de EDF, que tendría lugar en 1986. Los intereses científicos se han dado la mano en esta ocasión con el deseo conmemorativo y han dado origen a un movimiento de investigación, publicación y divulgación de un vigor inusitados en nuestra especialidad.
The Manichaean Turkish Texts of the Stein Collection at the British Library
Authors: ZIEME PETER
Published: June 2010

In this article the author presents an overview of the British Library's Manichaean Turkish text fragments (written in Runic, Manichaean and Sogdo-Uigur script). Besides information on all fragments published so far several pieces of a confession text on the Blessed Small Feast Day are edited in full and compared to parallels in other collections.
Doctrinal Dispute within Interdenominational Missions: The Shanghai Tract Committee in the 1840s
Authors: LAI JOHN T. P.
Published: June 2010

Both interdenominational co-operation and denominational competition featured in the Protestant missionary literary enterprise in nineteenth-century China. The interdenominational Religious Tract Society in London became the most vital link between the missionary translators, printing presses and target audiences in the production, publication and distribution of Christian tracts. Ideally, interdenominational missions would pool resources and promote cooperation among missionaries with different denominational affiliations. Doctrinal disputes, however, seem to have been inevitable among them in the everyday operation of missions. The first tract committee established in China, the Shanghai Tract Committee in the 1840s is a case in point. Unequal denominational representation resulted in heated doctrinal controversies and the resignation of a Committee member over the publication of a problematic tract in Chinese.
Cold Food, Fire and Ancestral Production: Mid-spring Celebrations in Central China
Authors: AIJMER GÖRAN
Published: June 2010

This article seeks to explain the traditional celebration of Cold Food and some other springtime customs in the mid-Yangzi basin in central China. In these rituals the ancestors and their influence in the production of new rice were highlighted while, at the same time, social reproduction through women was temporarily suspended. Female generative energy was not allowed to compete with the creative force of the ancestors in the fields. Cold Food is seen as a trope on seasonal agricultural tasks. The myth of moral constancy, which accompanied the festival, was on another deeper level an iconic exploration of the preparation of the agricultural fields. Death was seen to propel life, ancestral energy being transferred to the living through rice.
Metallicity Evolution of AGNs
Authors: Nagao T. , Maiolino R. , Marconi A. , Matsuoka K. , Taniguchi Y.
Published: June 2010

Chemical properties of AGNs and their redshift evolution are of interest to understand the star-formation history of AGN host galaxies and the co-evolution between galaxies and supermassive black holes (SMBHs). One important observational clue on this issue is a tight correlation between the AGN luminosity and the metallicity of the broad-line region. Surprisingly this relation shows no redshift evolution, even up to z ~ 6. This correlation is attributable mainly to the positive correlation between metallicity and SMBH mass, rather than to the relation between metallicity and Eddington ratio. A significant positive correlation between the metallicity and the AGN luminosity is also seen in narrow-line regions, not only in broad-line regions. Possible implications of these results on the galaxy–SMBH co-evolution are briefly mentioned.
PCA Tomography and Its Application to Nearby Galactic Nuclei
Authors: Steiner J. E. , Menezes R. B. , Ricci T. V. , de Oliveira A. S.
Published: June 2010

With the development of modern technologies such as integral field units, it is possible to obtain data cubes in which one produces images with spectral resolution. Extracting information from them can be quite complex, and hence the development of new methods of data analysis is desirable. We briefly describe a method of analysis of data cubes (data from single field observations, containing two spatial and one spectral dimension) that uses principal component analysis to express the data in the form of reduced dimensionality, facilitating efficient information extraction from very large data sets. We applied the method, for illustrative purposes, to the central region of the LINER galaxy NGC 4736, and demonstrate that it has a type 1 active nucleus, which was not known before. Furthermore, we show that it is displaced from the center of its stellar bulge.
Environmental Effects on Properties of Type 2 QSOs
Authors: Chen Lin-wen , Hsu Li-Ting
Published: June 2010

Type 2 QSOs (QSO2s) are intrinsically luminous QSOs embedded in dusty environments. In this work, we study the radio, optical, and soft X-ray properties of 887 optically selected [O III]-based QSO2s (Reyes et al. 2008) at z<0.83 to investigate the connection between QSO2s and their environments. We use SDSS data to measure the luminosity-limited galaxy counts in a volume centered on each QSO2 and defined by Δ z<0.1 (based on photometric redshifts) and within a projected distance of 1.5 Mpc of the QSO2 (δ1.5Mpc). We used ROSAT All Sky Survey (RASS) data to estimate the X-ray excess. Hsu & Chen (2010), after correcting for Galactic absorption, obtain a lower limit for the intrinsic neutral hydrogen column density (NH) toward each of the QSO2s. About 50% of these sources have NH > 1022 cm−2. We take this value as a threshold to subdivide QSO2s into high- and low-NH groups, and compare their environments. The distributions δ1.5Mpc of the two populations show that, in regions of higher galaxy density, QSO2s are dominated by the high-NH population (Figure 1), suggesting a closer connection between more obscured QSO2s and surrounding galaxies.
Multiwavelength Detection of Cluster AGN
Authors: Klesman Alison J. , Sarajedini Vicki L.
Published: June 2010

We present the initial results of a multiwavelength study to detect AGN in several galaxy clusters at moderate redshifts (0.5 < z < 0.9). By using multiple epochs of HST data, we identify 10–15 optically variable galactic nuclei in each cluster. The variable and non-variable galaxies are compared with X-ray point sources.
Host Galaxies of Obscured Quasars: Infant Starbursts Caught in Action
Authors: Liu Xin , Zakamska Nadia L. , Greene Jenny E. , Strauss Michael A. , Krolik Julian H.
Published: June 2010

Supermassive black holes (SMBHs) in the centers of massive galaxies are thought to predominantly grow in brief Eddington-rate quasar phases accompanied by starbursts, but on-going starbursts in luminous quasars are difficult to observe. Buried under the natural coronagraph, obscured quasars offer a unique window for direct, robust host-galaxy spectroscopy otherwise virtually inaccessible for luminous quasars. Our pilot study at z ~ 0.5 (Liu et al. 2009) revealed a substantial contribution from very young stellar populations with ages less than ~ 100 Myr in all of the observed host galaxy spectra. More dramatically, in three out of the nine SDSS quasars observed, we have witnessed strong infant starbursts with ages of ~ 5 Myr, clocked by the telltale Wolf–Rayet emission features.
The Coronal Emission-Line Region in AGNs: A Hubble Space Telescope View
Authors: Mazzalay X. , Rodríguez-Ardila A. , Komossa S.
Published: June 2010

We present a study of HST/STIS optical spectra of a sample of ten Seyfert galaxies aimed at analyzing the structure and physical properties of the coronal line region. The high spatial resolution provided by STIS (about 7 pc for the closest objects) allowed us to resolve the coronal line region and obtain key information about the kinematics of the coronal-line gas, measure directly its spatial scale, and study the mechanisms that drive the high-ionization lines.
Byurakan–IRAS Galaxy Pairs as Indicators of Starburst and Galaxy Evolution
Authors: Mickaelian A. M. , Sargsyan L. A. , Mikayelyan G. A.
Published: June 2010

The Byurakan–IRAS galaxies (BIG objects; Mickaelian 1995) are the result of a project of optical identifications of IRAS Point Source Catalog (PSC; IRAS 1988) in a 1500 square degree high-galactic latitude (|b|>15°) area based on the Digitized Sky Survey (DSS) images and the Digitized First Byurakan Survey (DFBS, or digitized Markarian survey) low-dispersion spectra. As a result, 1278 galaxies have been identified (as well as galactic objects, Byurakan–IRAS Stars [BIS]), including 42 PSC sources identified with 103 galaxies that make up 30 physical pairs and 12 multiples.
The Infrared Nuclear Emission of Seyfert Galaxies on Parsec Scales: Testing the Clumpy Torus Models
Authors: Ramos Almeida C. , Levenson N. A. , Rodríguez Espinosa J. M. , Alonso Herrero A. , Asensio Ramos A. , Radomski J. T. , Packham C. , Fisher R. S. , Telesco C. M.
Published: June 2010

We present subarcsecond resolution mid-infrared (mid-IR) photometry in the range from 8 to 20 μm of 18 nearby Seyfert galaxies, reporting high spatial resolution nuclear fluxes for the entire sample (see Table 3 of Ramos Almeida et al. 2009). We construct spectral energy distributions (SEDs) that the AGN dominates, relatively uncontaminated by starlight, adding near-IR measurements from the literature at similar angular resolution. We find that the IR SEDs of intermediate-type Seyferts are flatter and present higher 10 to 18 μm ratios than those of Seyfert 2 (Sy2) galaxies.
Near-Infrared Spectral Energy Distributions of Seyfert Galaxies: Stellar Population, Active Nucleus, and Hot Dust
Authors: Riffel Rogério , Pastoriza Miriani G. , Carciofi Alex , Rodríguez-Ardila Alberto , Bonatto Charles
Published: June 2010

We investigate the NIR spectra of 24 Seyfert galaxies observed with the instrument SpeX at the NASA Infrared Telescope Facility (ITRF) in the short cross-dispersed mode. The results of the spectral synthesis fitting procedure are presented and discussed in details by Riffel et al. (2009). The approach followed here is based on the starlight code (see Cid Fernandes et al. 2005). The spectral synthesis shows that the NIR continuum of active galaxies can be explained in terms of at least three components: a non-thermal continuum, dust emission, and the stellar population of the circumnuclear region. The study of the stellar population is a critical step in the analysis of the continuum emission of Seyfert galaxies. Moreover, our results are consistent with the predictions of the unified model for AGNs, as the non-thermal continuum and the hot dust emission are present in all Sy 1 sources and only in a small fraction of the Sy 2s. Regarding the stellar population component, our results point to a mean metallicity solar to above solar, if we consider the light-weighted values, while for the mass-weighted mean metallicity our results indicate a sub-solar value. We associate this discrepancy with the well known age–metallicity degeneracy: i.e., for a fixed mass, a high-metallicity stellar population looks cooler — and older — than a low-metallicity population, thus resulting in a higher M/L ratio. Moreover, this is consistent with a galaxy chemical enrichment scenario in which the young population is enriched by the evolution of the early massive stars. In this context, the light-weighted metallicity is more sensitive to the young component, while the mass-weighted metallicity to the old stellar population.
AGN in the GOODS Fields: Variability and Multiwavelength Detection
Authors: Sarajedini Vicki L. , Koo David C. , Klesman Alison J.
Published: June 2010

Active galactic nuclei can be identified in deep HST surveys using different selection techniques and multiwavelength data. We aim to produce a complete sample of AGN in the GOODS South and North fields by combining X-ray, optical and mid-IR selection criteria, including galaxies displaying nuclear optical variability.
Nuclear IR SED of Type 2 Seyfert Galaxies
Authors: Videla L. , Lira P. , Alonso-Herrero A. , Alexander D. M. , Ward M.
Published: June 2010

We obtained deep images for 49 Seyfert 2 galaxies in 6 infrared bands: J, H, K, L, M, and N with the VLT at Paranal, the NTT at La Silla, and Gemini at Pachón, to compile their nuclear infrared (IR) spectral energy distributions (SEDs). These galaxies were extracted from the Extended 12 μm Galaxy Sample (Rush et al. 1993).
Automated Classification of Quasars and Stars
Authors: Zhang Yanxia , Zhao Yongheng , Zheng Hongwen
Published: June 2010

We investigate selection and weighting of features by applying a random forest algorithm to multiwavelength data. Then we employ a k-nearest neighbor method to distinguish quasars from stars. We then compare the performance of this approach based on all features, weighted features, and selected features. We find that the k-nearest neighbor approach combined with random forests effectively separates quasars from stars.
What Do Statistics Reveal About the MBH–Mbulge Correlation and Co-Evolution?
Authors: Peng Chien Y.
Published: June 2010

Observational data show that the correlation between the masses of supermassive black holes MBH and galaxy bulge masses Mbulge follows a nearly linear trend, and that the correlation is strongest with the bulge rather than the total stellar mass Mgal. With increasing redshift, the ratio Γ=MBH/Mbulge relative to z = 0 also seems to be larger for MBH≳108.5M⊙. This study looks more closely at statistics to see what effect it has on creating, and observing, the MBH–Mbulge correlation. It is possible to show that if galaxy merging statistics can drive the correlation, minor mergers are responsible for causing a convergence to linearity most evident at high masses, whereas major mergers have a central limit convergence that more strongly reduces the scatter. This statistical reasoning is agnostic about galaxy morphology. Therefore, combining statistical prediction (more major mergers ⟹ tighter correlation) with observations (bulges = tightest correlation), would lead one to conclude that more major mergers (throughout an entire merger tree, not just the primary branch) give rise to more prominent bulges. Lastly, with regard to controversial findings that Γ increases with redshift, this study shows why the luminosity function (LF) bias argument, taken correctly at face value, actually strengthens, rather than weakens, the findings. However, correcting for LF bias is unwarranted because the BH mass scale for quasars is bootstrapped to the MBH–σ* correlation in normal galaxies at z = 0, and quasar–quasar comparisons are mostly internally consistent. In Monte-Carlo simulations, high Γ galaxies are indeed present: they are statistical outliers (i.e., “under-merged”) that take longer to converge to linearity via minor mergers. Additional evidence that the galaxies are undermassive at z≳2 for their MBH is that the quasar hosts are very compact for their expected mass.
Determination of the Intrinsic Scatter in the MBH–σ and MBH–Lbulge Relations
Authors: Gültekin Kayhan
Published: June 2010

We derive improved versions of the relations between supermassive black hole mass MBH and host-galaxy bulge velocity dispersion σ and luminosity L (the MBH–σ and MBH–Lbulge relations), based on ~ 50 MBH measurements and ~ 20 upper limits. Particular attention is paid to recovery of the intrinsic scatter (ϵ0) in both relations. We find the scatter to be significantly larger than estimated in most previous studies. The large scatter requires revision of the local black hole mass function, and it implies that there may be substantial selection bias in studies of the evolution of the MBH–σ and MBH–Lbulge relations. When only considering ellipticals, the scatter decreases. These results appear to be insensitive to a wide range of assumptions about the measurement errors and the distribution of intrinsic scatter. We also investigate the effects on the fits of culling the sample according to the resolution of the black hole's sphere of influence.
Accurate AGN Black Hole Masses and the Scatter in the MBH–Lbulge Relationship
Authors: Gaskell C. Martin
Published: June 2010

A new empirical formulae is given for estimating the masses of black holes in AGNs from the Hβ velocity dispersion and the continuum luminosity at 5100 Å. It is calibrated to reverberation-mapping and stellar-dynamical estimates of black hole masses. The resulting mass estimates are as accurate as reverberation-mapping and stellar-dynamical estimates. The new mass estimates show that there is very little scatter in the MBH–Lbulge relationship for high-luminosity galaxies, and that the scatter increases substantially in lower-mass galaxies.
Adaptive Optics-Based Measurements of the Black Hole in Abell 2162–BCG
Authors: McConnell Nicholas J. , Graham James R. , Ma Chung-Pei , Gebhardt Karl , Lauer Tod R.
Published: June 2010

We present preliminary measurements of the central black hole mass MBH, and stellar mass-to-light ratio M*/LR, in the Brightest Cluster Galaxy of Abell 2162 (A2162–BCG), using integral-field unit (IFU) data from OSIRIS on Keck 2 with laser guide star adaptive optics (LGS-AO). Our results demonstrate early success in an ongoing effort to obtain stellar dynamical measurements of MBH in nine BCGs using ground-based AO.
Merger-Induced Quasars, Their Light Curves, and Their Host Halos
Authors: Shankar Francesco
Published: June 2010

We revisit a basic model of quasar activation by major mergers of dark matter halos (with “galactic” masses of ≲1013M⊙h−1). This model usually consists of two main ingredients: the halo merger rate describing triggering, and a quasar light curve, which describes the evolution of individual quasars. We show how the matching between model predictions and a variety of new, independent data sets allows one to efficiently constrain several aspects of black hole growth and evolution that must be taken into account in future studies by more advanced models of galaxy formation. Our results can be summarized as follows: (1) A descending phase modelled such that quasars in more massive halos shut down faster than those in less massive ones allows a good description of the bright end of the AGN luminosity function at all epochs and is compatible with downsizing, with more massive galaxies shutting down star formation earlier. (2) We measure the average bias of type 2 AGNs in SDSS to be b = 1.233 ± 0.195, independent of luminosity in the range 42.5≤ log L(erg s−1) ≤ 45.5. Such a value of the bias implies that faint AGNs at z<0.3 are mainly hosted by halos more massive than ~1011.5–12M⊙h−1. The black hole mass function predicted by this model is flatter than previously found. (3) The high clustering signal measured at z>3 in SDSS forces successful models to be characterized by rather short delay times of tdelay≲108 yr between the triggering and the shining epochs, implying massive “seed” BHs ≳ 105M⊙h−1 and initial super-Eddington growth. (4) The low number counts of X-ray AGNs measured in recent deep surveys are better reproduced by models with a minimal post-peak phase and a higher minimum hosting halo mass at high redshifts. (5) Cross-correlating the feedback-constrained MBH–M relation, with the redshift-dependent Mstar–M relation obtained from the cumulative number-matching of the stellar and halo mass functions, we find a factor of ~2 larger BH-to-stellar mass ratio at high redshifts. We discuss the meaning of such trends in connection with the mild, positive evolution in the MBH-σstar relation, and the strong observed evolution in the sizes and velocity dispersions of their hosts.
Mid-IR Properties of Seyferts: Spitzer IRS Spectroscopy of the IRAS 12 μm Seyfert Sample
Authors: Charmandaris Vassilis , Wu Yanling , Huang Jiasheng , Spinoglio Luigi , Tommasin Silvia
Published: June 2010

We performed an analysis of the mid-infrared properties of the 12 μm Seyfert sample, a complete unbiased 12 μm flux limited sample of local Seyfert galaxies selected from the IRAS Faint Source Catalog based on low-resolution spectra obtained with the Infrared Spectrograph (IRS) on-board Spitzer Space Telescope. A detailed presentation of this analysis is discussed by Wu et al. (2009). We find that, on average, the 15–30 μm slope of the continuum is 〈 α15–30〉 = −0.85 ± 0.61 for Seyfert 1s and −1.53 ± 0.84 for Seyfert 2s, and there is substantial scatter in each type. Moreover, nearly 32% of Seyfert 1s, and 9% of Seyfert 2s, display a peak in the mid-infrared spectrum at 20 μm, which is attributed to an additional hot dust component. The polycyclic aromatic hydrocarbon (PAH) equivalent width decreases with increasing dust temperature, as indicated by the global infrared color of the host galaxies. However, no statistical difference in PAH equivalent width is detected between the two Seyfert types of the same bolometric luminosity. Finally, we propose a new method to estimate the AGN contribution to the integrated 12 μm galaxy emission, by subtracting the “star formation” component in the Seyfert galaxies, making use of the tight correlation between PAH 11.2 μm luminosity and 12 μm luminosity for star forming galaxies.
AGN and Galaxy Clustering at z = 0.3–3.0 Using the Japanese Virtual Observatory
Authors: Shirasaki Yuji , Tanaka Masahiro , Ohishi Masatoshi , Mizumoto Yoshihiko , Takata Tadafumi , Yasuda Naoki
Published: June 2010

We present the results of a cross-correlation analysis of the projected positions of AGNs and galaxies at redshifts from 0.3 to 3.0. It is widely accepted that the origin of AGN activity is accretion of matter onto a massive black hole at the center of a galaxy (e.g., Lynden-Bell 1969). To explain the activity of AGNs, a large fraction of matter in the galaxy must be delivered to the inner region on a short timescale (Hopkins et al. 2008). One possible mechanism for causing rapid gas inflows into the central region is a major galaxy merger between gas-rich galaxies (e.g., Kauffmann & Haehnelt 2000). If this is the case, AGNs are expected to be found in an environment with higher galaxy density than that of typical galaxies. We investigated environments of ~ 750 AGNs, which is about a ten times larger sample than used in previous studies, and we find a significant excess of galaxies around the AGNs in the redshift range of 0.3 to 1.8. We used the Japanese Virtual Observatory (JVO) to obtain the Subaru Suprime-Cam images and UKIDSS data around known AGNs. The datasets accessed through the JVO are: Catalog of Quasars and Active Galactic Nuclei by Veron-Cetty et al. (2006), SDSS DR-5 Quasar Catalog by Schneider et al. (2007), Subaru Suprime-Cam Reduced Image Archive of JVO, and UKIDSS DR2 catalog by Warren et al. (2007). We divided all the AGN samples into four redshift groups, 0.3≲z ≲ 0.8, 0.8≲ z ≲ 1.5, 1.5≲ z ≲ 1.8, and 1.8≲ z ≲ 3.0. For each redshift group, the dataset was further divided into a fainter group (MV ≥ −25 mag) and a brighter group (MV < −25 mag). We found that the correlation length of the high-redshift bright sample (1.5≲ z ≲ 1.8) was larger than that of the low-redshift faint sample (0.3≲ z ≲ 0.8). We also found that the correlation length was larger for the faint group at redshift range 0.8≲ z ≲1.5. These results can be explained by downsizing of mass assembly. More details can be found in the paper by Shirasaki et al. (2009). Our result implies that the Japanese Virtual Observatory can be a powerful tool to investigate the co-evolution of central black holes and galaxies at the intermediate redshift universe.
Spitzer IRS Observations of Low-Mass Seyfert Galaxies
Authors: Thornton Carol E. , Barth Aaron J. , Ho Luis C. , Greene Jenny E.
Published: June 2010

The Sloan Digital Sky Survey has made it possible to identify the first samples of active galaxies with estimated black hole masses below ~ 106M⊙. We have obtained Spitzer IRS low-resolution spectra, covering 5–38 μm, of a sample of 41 Seyfert galaxies with low-mass black holes. Our sample includes SDSS-selected objects from the low-mass Seyfert 1 sample of Greene & Ho (2004) and the low-mass Seyfert 2 sample of Barth et al. (2008), as well as NGC 4395 and POX 52. The goals of this work are to examine the dust emission properties of these objects and investigate the relationship between type 1 and type 2 AGNs at low luminosities and low masses, to search for evidence of star formation, and to use emission-line diagnostics to constrain physical conditions within the narrow-line regions. Here we present preliminary results from this project.
Probing the Evolution of Black Hole Mass Through Cosmic Time
Authors: Trakhtenbrot Benny , Netzer Hagai , Lira Paulina , Shemmer Ohad
Published: June 2010

Our research addresses the observed evolution of MBH and L/LEdd of type 1 radio-quiet AGNs. Measurements of MBH and L/LEdd in a sample of sources at z<0.75 using the “Hβ method” (Netzer & Trakkhtenbrot 2007) as well as new measurements of these properties at 0.75<z<2 using the “Mg ii λ2798 method”) show significant evolution of L/LEdd for any value of MBH up to z = 2 (see Figure 1). In a dedicated near-IR project we obtained the most reliable sample of MBH and L/LEdd estimates for z ~ 2.3 and z ~ 3.4 AGN (Netzer et al. 2007; Shemmer et al. 2004); the distribution of L/LEdd is very broad (Figure 1) and ~ 1/2 of the sources have L/LEdd<0.2, implying tgrowth>tuniverse and hence an earlier epoch of fast growth. Our on-going Gemini–VLT campaign focuses on z ~ 4.8 sources, with the Mg ii line observed in the H-band (Figure 2). The analysis of ~ 1/3 of the spectra uncovers, again, a broad distribution of L/LEdd, with several sources having L/LEdd ≫ 1, suggesting an early episode of fast BH growth.
Accretion and Outflow in Active Galaxies
Authors: King Andrew
Published: June 2010

I review accretion and outflow in active galactic nuclei. Accreti4on appears to occur in a series of very small-scale, chaotic events, whose gas flows have no correlation with the large-scale structure of the galaxy or with each other. The accreting gas has extremely low specific angular momentum and probably represents only a small fraction of the gas involved in a galaxy merger, which may be the underlying driver.

Eddington accretion episodes in AGN must be common in order for the supermassive black holes to grow. I show that they produce winds with velocities v ~ 0.1c and ionization parameters implying the presence of resonance lines of helium-like and hydrogen-like iron. The wind creates a strong cooling shock as it interacts with the interstellar medium of the host galaxy, and this cooling region may be observable in an inverse Compton continuum and lower-excitation emission lines associated with lower velocities. The shell of matter swept up by the shocked wind stalls unless the black hole mass has reached the value Mσ implied by the M–σ relation. Once this mass is reached, further black hole growth is prevented. If the shocked gas did not cool as asserted above, the resulting (“energy-driven”) outflow would imply a far smaller SMBH mass than actually observed. Minor accretion events with small gas fractions can produce galaxy-wide outflows, including fossil outflows in galaxies where there is little current AGN activity.
Star Cluster Migration Near the Galactic Center
Authors: Fujii Michiko , Iwasawa Masaki , Funato Yoko , Makino Junichiro
Published: June 2010

We performed a self-consistent N-body simulation of star clusters in the Galactic center (GC), taking into account the collisions of stars and formation of an intermediate-mass black hole (IMBH). We find that if an IMBH forms in the cluster, it carries young stars to the GC by a 1:1 resonance.
Large-Scale Outflows from AGN: A Link Between Central Black Holes and Galaxies
Authors: Proga Daniel , Kurosawa Ryuichi , Nagamine Kentaro
Published: June 2010

We summarize the results from numerical simulations of mass outflows from AGN. We focus on simulations of outflows driven by radiation from large-scale inflows. We discuss the properties of these outflows in the context of the so-called AGN feedback problem. Our main conclusion is that this type of outflow is efficient in removing matter but inefficient in removing energy.
Feedback in the Dark Domain
Authors: Wada Keiichi
Published: June 2010

In order to clarify the physics of AGN feedback and feeding, we need to understand the interstellar medium (ISM) in the central several tens of parsecs in galaxies where our observational and theoretical knowledge is relatively poor. Here we discuss feedback processes due to strong far UV and X-ray radiation, as well as the dynamical effect of a supermassive black hole (SMBH) based on new high-resolution numerical simulations of the ISM in the central R ≤ 32 pc region around a SMBH at the center of a galaxy.
GMOS IFU Observations of the Gas Kinematics in the Radio Galaxy Arp 102B
Authors: Couto Guilherme d. S. , Storchi-Bergmann Thaisa , Riffel Rogemar A. , Axon D. J. , Robinson A.
Published: June 2010

The goal of this work is to map the gas excitation and kinematics in the inner ~ 2 kiloparsecs of the radio-galaxy Arp 102B. Though being classified as an E0 galaxy, Arp 102B shows a nuclear gas spiral (Fathi et al., in preparation). Previous studies of the gas kinematics in nuclear spirals have led to the conclusion that these structures usually trace gas inflows (Fathi et al. 2006; [Storchi-Bergmann et al. 2007; [Riffel et al. 2008). We have used integral field spectroscopy obtained with GMOS instrument of the Gemini North telescope to investigate the nature of the nuclear spiral arms. The spectra cover the wavelength range 4400–7300 Å over a field of view of 5.″5 × 3.″9 (2.7 kpc × 1.9 kpc).
Feedback from AGN: The Kinetic/Radio Luminosity Function
Authors: Melini Gabriele , La Franca Fabio , Fiore Fabrizio
Published: June 2010

We have measured the probability distribution function of the ratio RX = log L1.4/LX, where L1.4/LX = ν Lν(1.4 GHz)/LX(2–10 keV), between the 1.4 GHz and the unabsorbed 2–10 keV luminosities and its dependence on LX and z. We have used a complete sample of ~1800 hard X-ray selected AGN, observed in the 1.4 GHz band, cross-correlated in order to exclude FR II-type objects, and thus obtain a contemporaneous measure of the radio and X-ray emission. The distribution P(RX|LX,z) is shown in Figure 1. Convolution of the distribution P(RX|LX,z) with the 2–10 keV X-ray AGN luminosity function from La Franca et al. (2005) and the relations between radio power and kinetic energy from Best et al. (2006) and Willott et al. (1999) allows us to derive the AGN kinetic power and its evolution. As shown in Figure 1, our results are in good agreement with the predictions of the most recent models of galaxy formation and evolution (e.g., Croton et al. 2006), where AGN radio feedback is required to quench the star formation.
Outflows of Low and High Ionization Gas in Nearby AGN
Authors: Müller Sánchez F. , Prieto A. , Davies R. I. , Hicks E. K. S.
Published: June 2010

We present results from a survey of nearby AGN using the adaptive optics assisted integral-field spectrometer SINFONI on the VLT. These data enable us to study at high angular resolution (~ 0.″08) the distribution and kinematics of the low-ionization gas traced by the BrΓλ2.17 μm recombination line and [Si vi] λ 1.96 μm, [Al ix] λ 2.04 μm, and [Ca viii] λ 2.32 μm, the most prominent coronal lines in the near-IR. Overall, our results show that the coronal lines extend to a radius similar to that of narrow Brγ emission, mimicking in most cases the narrow-line region (NLR). In addition, the kinematics of the highly ionized species, and most of the Brγ kinematics, is dominated by non-circular motions with higher dispersion along the ionization cones, indicating that material is being accelerated and outflowing from a region very close to the AGN.
Quasars, Feedback, and Galaxy Formation
Authors: Hopkins Philip F.
Published: June 2010

Recent observations of tight correlations between supermassive black hole masses and the properties of their host galaxies demonstrate that black holes and bulges are co-eval and have motivated theoretical models in which feedback from AGN activity regulates the black hole and host galaxy evolution. Combining simulations, analytic models, and recent observations, answers to a number of questions are starting to take shape: how do AGN get triggered? How long do they live? What are typical light curves and what sets them? Is feedback necessary and/or sufficient to regulate BH growth? What effects does that feedback have on the host galaxy? On the host halo? All of this also highlights questions that remain wide open: how does gas get from a few pc to the AGN? What are the actual microphysical mechanisms of feedback? What is the tradeoff between stellar and AGN feedback? And, if there are different “modes” of feedback, where/when are each important?
GALEX Constraints on AGN Feedback in Early-Type Galaxies
Authors: Yi Sukyoung K.
Published: June 2010

The absence of vigorous star formation in early-type galaxies is a mystery because early-type galaxies do have a copious supply of cold gas. Various heating mechanisms have been put forward to explain this, and AGN feedback is one of the most widely suspected culprits. The GALEX UV telescope detects even a small amount of star formation and allows an estimate of the current and recent star formation. We find that star formation is still common in early-type galaxies with low velocity dispersion where the black hole mass is believed to be small. We compare the star-formation rates of the galaxies with predictions from various semi-analytic models with different feedback prescriptions. We find that the passive behavior of central galaxies in groups and clusters is reproduced by semi-analytic models with AGN feedback. However, the same prescriptions causes satellite (i.e., non-central) galaxies to be quenched as well, much more than observed by GALEX, leading to a “satellite over-quenching problem.”
Persistence in recurrent geomagnetic activity and its connection with Space Climate
Authors: Diego P. , Storini M. , Laurenza M.
Published: June 2010

Recurrent geomagnetic activity is mainly linked to the passage of interplanetary corotating solar wind structures in the near‐Earth space. We studied geomagnetic recurrences for which an enhanced value of the autocorrelation coefficient exists between the data of two adjacent Bartels rotations in aa, Kp, Dst, AE time series, for the period 1954–2007, covering about 5 solar cycles (from cycle 19 to cycle 23). A new index (P), based on autocorrelation analysis, has been introduced to estimate also the duration up to seven Bartels rotations of each solar structure (or group of structures) producing geomagnetic recurrences with high autocorrelation (correlation coefficient ≥ 0.3). We could infer whether recurrent geomagnetic activity is due to successive short‐lived (at least 2 Bartels rotations) or to long‐lasting corotating structures (up to 7 or more Bartels rotations). Generally, time periods characterized by recurrent geomagnetic activity are longer during the descending phase of even‐numbered cycles (20, 22). Nevertheless, we found that recurrences determined by long‐lived interplanetary structures are detected mainly in the descending phase of cycles 19 and 23. Finally, we point out that the average levels of the computed indices during the descending phase of each solar cycle show a significant anticorrelation with the sunspot area integrated over the subsequent cycle, giving new insights for Space Climate forecast.
Early Mars hydrology: Meridiani playa deposits and the sedimentary record of Arabia Terra
Authors: Andrews‐Hanna Jeffrey C. , Zuber Maria T. , Arvidson Raymond E. , Wiseman Sandra M.
Published: June 2010

The Meridiani Planum region of Mars has been identified as a region of past aqueous activity by a combination of orbital and in situ observations that revealed evidence for sulfate‐rich dirty evaporites formed in a playa setting. We investigate the hydrology and sedimentary record of this area using global and regional hydrological models in which groundwater flow is driven by a combination of precipitation, evaporation, and the surface topography. Groundwater evaporation results in evaporite precipitation and cementation of aeolian sediments, allowing the accumulation of deposits of substantial thickness, which then affect the subsequent patterns of groundwater flow. Hydrological activity is initially predicted to be isolated to the deepest craters and depressions, primarily within the Arabia Terra region surrounding Meridiani. As these depressions fill with sediments, the groundwater upwelling spreads laterally across broad regions of Arabia Terra, including Meridiani Planum, as well as regional topographic lows such as the northern lowlands and large impact basins. The model predictions are borne out by observations of large intracrater deposits, inverted valley networks, finely layered deposits, spectral evidence for hydrated sulfates, and pedestal craters that preserve the remnants of a much larger deposit that once covered much of Arabia Terra. The results suggest that the inferred playa at Meridiani was part of a regionally extensive zone of groundwater upwelling. This hydrological cycle requires that conditions in the late Noachian to early Hesperian must have been conducive to the existence of liquid water at the surface throughout much of the low latitudes of Mars.
Geomagnetic 100‐kyr variation excited by a change in the Earth's orbital eccentricity
Authors: Yokoyama Yukiko , Yamazaki Toshitsugu , Oda Hirokuni
Published: June 2010

Geomagnetic secular variations on a time scale of 10–100 kyr have important implications regarding the energy source of the geomagnetic field. Some high‐quality paleomagnetic records from marine sediment cores show quasi‐periodic variations having a time scale close to that of the Earth's orbital eccentricity. We analyzed a paleomagnetic record of core MD982185 from the equatorial Pacific and the Earth's eccentricity for the last 2.2 m.y. utilizing wavelet analysis. Variations in the geomagnetic vertical component were synchronous with those in the first derivative of the eccentricity, implying that the geomagnetic variations are excited by changes in the eccentricity.
Heterogeneous nucleation of ice on anthropogenic organic particles collected in Mexico City
Authors: Knopf D. A. , Wang B. , Laskin A. , Moffet R. C. , Gilles M. K.
Published: June 2010

This study reports on heterogeneous ice nucleation activity of predominantly organic (or coated with organic material) anthropogenic particles sampled within and around the polluted environment of Mexico City. The onset of heterogeneous ice nucleation was observed as a function of particle temperature (Tp), relative humidity (RH), nucleation mode, and particle chemical composition which is influenced by photochemical atmospheric aging. Particle analyses included computer controlled scanning electron microscopy with energy dispersive analysis of X‐rays (CCSEM/EDX) and scanning transmission X‐ray microscopy with near edge X‐ray absorption fine structure spectroscopy (STXM/NEXAFS). In contrast to most laboratory studies employing proxies of organic aerosol, we show that anthropogenic organic particles collected in Mexico City can potentially induce ice nucleation at experimental conditions relevant to cirrus formation. The results suggest a new precedent for the potential impact of organic particles on ice cloud formation and climate.
Microwave Spectra of Molecules of Astrophysical Interest: II Methylenimine
Authors: Kirchhoff William H. , Johnson Donald R. , Lovas Frank J.
Published: June 2010

The available data on the microwave spectrum of methylenimine are critically reviewed for information applicable to radio astronomy. Molecular data such as rotational constants, centrifugal distortion parameters, hyperfine coupling constants, and dipole moments are tabulated. A detailed centrifugal distortion calculation has been carried out for the most abundant isotopic form of this molecule, H2 12C 14NH. Transitions have been predicted and tabulated for the frequency range 100 MHz to 300 GHz. All predicted transitions include 95 percent confidence limits; error limits have been reported for all measured transitions.
Evaluated Chemical Kinetic Rate Constants for Various Gas Phase Reactions
Authors: Schofield Keith
Published: June 2010

The available information, up to mid-1972, for the rate constants of a series of gas phase chemical reactions has been evaluated critically. For each reaction, relevant thermodynamic data are presented and values for the equilibrium constant expressed in mathematical form. Kinetic data are presented in tabular and graphical form together with a discussion of the pertinent details. Recommended rate constant values are presented wherever possible with suggested error limits. The reactions considered involve the species H, O, C, N, S, OH, HS, S2, CS, SO, HSO2, NH2, NH3, NO, N2O, NO2, N2, O2, O4, N2, O2, O3, H2, H2O, SO2, SO3, CS2, OCS, H2S, and CO. Particular emphasis is given to reactions involving sulfur chemistry. The best available data for these reactions have been summarized in a table at the end of the paper. An appendix discussing the available evaluations and review articles published since 1960 also has been included to publicize these sources of either evaluated data or of extensive reference bibliographies.