bluuebunny/crossref_metadata_2025 huggingface dataset:
La Revolucion Industrial y la Nueva Historia Economica (I)
Authors: Mokyr Joel
Published: June 2010

Ha transcurrido casi un siglo desde la publicación de la famosa obra de Arnold Toynbee, Lectures on the Industrial Revolution (1884). Desde entonces, historiadores de todas las escuelas han llegado a la conclusión de que la Revolución Industrial en Gran Bretaña constituyó un nuevo punto de partida en la historia de la humanidad, un hecho de tanta importancia para la vida cotidiana que puede compararse con la aparición del monoteísmo o con el desarrollo del lenguaje. De este modo, ha surgido una extensa literatura escrita por historiadores, economistas y sociólogos, ingleses y extranjeros, tanto de izquierdas como de derechas, que trata de sus diversos aspectos. Sin embargo, los expertos no se han puesto de acuerdo sobre los problemas fundamentales. En primer lugar se encuentra la mera cuestión de la definición: ¿qué fue exactamente la Revolución Industrial? De los muchos intentos que se han efectuado para resumir lo que supuso la Revolución Industrial, el de Perkin es quizá el más elocuente. En sus propias palabras, fue «una revolución en el acceso de los hombres a los medios de vida, en el control de su entorno ecológico, en su capacidad de escapar de la tiranía y de la mezquindad de la naturaleza (…) abrió el camino a los hombres para completar el dominio de su entorno físico, sin la ineludible necesidad de explotarse unos a otros» (Perkin, 1969, pp. 3–5). En Gran Bretaña cambiaron muchas cosas, y no solamente la manera en que se producían los bienes y servicios. Se transformó la naturaleza de la familia y del hogar, el status de las mujeres y los niños, el papel de la Iglesia, cómo las personas elegían a los gobernantes y mantenían a los pobres, lo que sabían acerca del mundo y lo que querían saber. El descubrimiento de cómo estas transformaciones no económicas afectaron y se vieron afectadas por el cambio económico es un proyecto continuo La revolución fue, en frase irresistible de Perkin, «algo más que una Revolución Industrial». Al centrarnos en la economía aislamos sólo una parte, aunque fundamental, de la modernizatión de Gran Bretaña.
La industria azucarera española, 1914–1936
Authors: Rodriguez Manuel Martin
Published: June 2010

España había sido uno de los últimos países europeos en introducir el cultivo de la remolacha azucarera. Hasta 1882, fecha en que se construyó la primera fábrica de azúcar de remolacha en la Vega de Granada, el mercado nacional se había abastecido básicamente mediante importaciones procedentes de las reliquias del Imperio —Cuba, Puerto Rico y Filipinas—, complementadas con una corta producción de azúcar de caña obtenida en la propia metrópoli a lo largo de una estrecha franja costera mediterránea de las provincias de Almería, Granada y Málaga.
A proposito de la Historia de Cataluña en los siglos XVI–XVII
Authors: Shaw Carlos Martinez
Published: June 2010

Me siento en la obligación de expresar públicamente mi profunda discrepancia con la recensión que sobre el libro de Ricardo García Cárcel (Historia de Cataluña, siglos XVI–XVII) firma Gaspar Feliu en esta misma Revista de Historia Económica que hoy acepta mi réplica y a la que agradezco su acogida. Me he decidido a romper mi costumbre de no interferirme en los juicios críticos ajenos a causa de la manifiesta hostilidad que desprende la citada reseña y que parece desplazar animadversiones personales al terreno de la obra científica y a causa de la inadmisible descalificación final que condena inquisi-torialmente y sin atenuantes un trabajo de investigación serio en su planteamiento y dilatado en su realización.
El Sector Terciario en España antes de 1936: Una nota de escepticismo sobre las estimaciones al uso
Authors: Tortella Gabriel
Published: June 2010

Con la excepción de Mulhall y Prados de la Escosura, no se han hecho estimaciones de la «Renta Terciaria» o renta del Sector Servicios para períodos anteriores a 1900. Para la primera mitad del siglo xx, aparte de la ya citada y recientísima de Prados, contamos tan sólo con dos estimaciones, que son parte de las conocidas series de Renta Nacional calculadas por el Consejo de Economía Nacional (CEN) y por Julio Alcaide Inchausti. Hace algún tiempo, con motivo de una larga investigación en equipo (el llamado «Proyecto Europeo», patrocinado por el Banco de España), tuve ocasión de examinar con algún detalle los trabajos donde se explica cómo se Ilevó a cabo la confección de estas dos series. El resultado de este examen fue la redacción de un informe acerca de los graves problemas de fiabilidad que planteaba el uso de estas estimaciones. El informe circuló entre los miembros del equipo, pero no tuvo ninguna publicidad. La presente nota es una versión abreviada y actualizada de aquel informe. Me han animado a publicarla, de un lado, los compañeros del equipo y, de otro, el deseo de poner en guardia a los colegas de los peligros que entranañ el depositar excesiva confianza en las tan citadas series.
La dinamica salarial durante el franquismo. El caso de RENFE
Authors: Ferner Anthony , Fina Lluis
Published: June 2010

El análisis de una cuestión tan importante como es la evolución del poder adquisitivo de los trabajadores durante el período franquista tropieza con graves dificultades debido a la inexistencia de series estadísticas continuas y suficientemente fiables acerca de los niveles salariales prevalecientes en dichos años. El Instituto Nacional de Estadística (INE) no inició hasta 1963 la elaboración de una Encuesta de Salarios dirigida a establecimientos seleccionados por muestreo aleatorio. Aunque la nueva encuesta tenía una cobertura limi tada y adolecía de diversos problemas metodológicos (Serrano y Malo de Molina, 1979: 331–346; Lorente, 1982), supuso una mejora muy importante respecto a la situación anterior en que la única información oficial disponible se limitó a unos datos de ganancias obtenidos por el INE desde 1953, que constituyen el precedente inmediato de la Encuesta de Salarios mencionada, y unos datos de «tarifas salariales» publicados por el mismo Instituto.
Una nota sobre la produccion agraria de Andalucia oriental en 1874-1914
Authors: Critz Jose Morilla
Published: June 2010

No creo exagerado decir que esta obra de Jiménez Blanco constituye, hoy por hoy, el trabajo más importante sobre la agricultura de Andalucía Oriental en el siglo XIX. Por otra parte, son dignas de destacar sus exhaustivas exposiciones del estado de la cuestión en cada subsector y las pormenorizadas explicaciones sobre la situación y utilización de las fuentes. Esto es particularmente útil en una parcela de la historia de Andalucía, caracterizada por la multiplicación de trabajos de ámbito reducido. Todo ello creo que justifica una nota crítica de los dos volúmenes en que se divide el trabajo, más amplia y detallada que lo que permite una simple recensión.
Puntualizaciones sobre un golpe de Estado
Authors: Fuertes Juan Velarde
Published: June 2010

El mundo histórico de la Dictadura, iniciado con el golpe de Estado de 13 de septiembre de 1923, tuvo un primer tratamiento apresurado. Se trata del desatado a partir de su caída, en 1930, con el prólogo de lo escrito por los opositores a Primo de Rivera en plena vigencia del proceso dictatorial. No conviene despreciar estos materiales. Pero, lo mismo que acontece con los. hagiográficos que abundaron de septiembre de 1923 a enero de 1930, han de someterse a juicios críticos muy fuertes. Todos los que han trabajado el período —si han querido ser solventes— los han utilizado tras rectificarlos a fondo.
Poder y Beneficio. Urbanizacion y Cambio en la Historia
Authors: Ringrose David R.
Published: June 2010

Hace algunos meses esta revista publicó una interesante discusión sobre historia urbana basada en mi reciente obra,Madrid y la economía española, 1560–1850. En su artículo, el profesor Santos Madrazo, al tiempo que formulaba una serie de preguntas acerca de mi utilización de las fuentes, aludía también a problemas más interesantes relativos al lugar de la historia urbana en la estructura y en el proceso de cambio histórico. En concreto, Madrazo menciona tres cuestiones interrelacionadas:a) la utilidad de los supuestos «smitheanos»;b) la premisa de que las ciudades producen unos fenómenos sociales y culturales únicos o nuevos, yc) el problema de la dependencia de interpretaciones ecológicas. Estos tres temas son los más interesantes e importantes, ya que tratan del lugar de las fuerzas motrices en la historia y, por lo tanto, mi respuesta a la crítica de detalles efectuada por Madrazo la he dejado para el apéndice.
Algunas Puntualizaciones Sobre «Catalunya, La Fabrica D'espanya»
Authors: de Motes Jordi Maluquer
Published: June 2010

La Revista de Historia Económica dedicaba en su penúltimo número (V, 3, otoño de 1987, pp. 623–628) unas cuantas páginas, escritas por Sebastián Coli Martín, a la exposición «Catalunya, la fábrica d'Espanya», que tuvo lugar en Barcelona a lo largo de varios meses del año 1985, y a su catálogo. Como coautor de una cosa y de la otra no puedo menos que agradecer los elogios allí expresados, pero también me siento obligado a formular más de una puntualización y a expresar mi discrepancia con el amigo Coll en algunos puntos. El hecho de formar parte del consejo asesor de la Revista, como también Jordi Nadal, convertiría en buenas las afirmaciones equivocadas del comentarista de producirse un silencio que se tomaría lógicamente por asentimiento.
The spiral index of knots
Authors: ADAMS COLIN , HUDSON RACHEL , MORRISON RALPH , GEORGE WILLIAM , STARKSTON LAURA , TAYLOR SAMUEL , TURANOVA OLGA
Published: June 2010

In this paper, we introduce two new invariants that are closely related to Milnor's curvature-torsion invariant. The first, a particularly natural invariant called the spiral index of a knot, captures the number of local maxima in a knot projection that is free of inflection points. This invariant is sandwiched between the bridge and braid index of a knot, and captures more subtle properties. The second invariant, the projective superbridge index, provides a method of counting the greatest number of local maxima that occur in a given projection. In addition to investigating the relationships among these invariants, we use them to classify all those knots for which Milnor's curvature-torsion invariant is 6π.
‘Laissez-faire’ or Active Intervention? The Nature of the British and Foreign Bible Society's Patronage of the Translation of the Chinese Union Versions – CORRIGENDUM
Authors: MAK GEORGE KAM WAH
Published: June 2010

George Mak's article ‘Laissez-faire or Active Intervention? The Nature of the British and Foreign Bible Society's Patronage of the Translation of the Chinese Union Versions' p.171 paragraph 2; ‘On the eve of the Shanghai Conference 1890, in addition to Morrison's version, which had long been out of circulation by that time, the Delegates' Version was the only Chinese translation of the entire Bible.
MAGNETOHYDRODYNAMIC FLOW OF A MICROPOLAR FLUID IN A CIRCULAR PIPE WITH HALL EFFECTS
Authors: SRINIVASACHARYA D. , SHIFERAW MEKONNEN
Published: June 2010

Steady magnetohydrodynamic flow of an incompressible micropolar fluid through a pipe of circular cross-section is studied by considering Hall and ionic effects. The fluid motion is due to a constant pressure gradient, and an external uniform magnetic field directed perpendicular to the flow direction is applied. Expressions for the velocity, microrotation, skin friction and flow rate are obtained. The effects of the micropolar parameter, magnetic parameter, Hall parameter and ion-slip parameter on the velocity, microrotation, skin friction and flow rate are discussed.
The Role of Quasars in Galaxy Formation
Authors: Elbaz D.
Published: June 2010

We discuss evidence that quasars, and more generally radio jets, may have played an active role in the formation stage of galaxies by inducing star formation, i.e., through positive feedback. This mechanism first proposed in the 1970s has been considered as anecdotal until now, contrary to the opposite effect that is generally put forward, i.e., the quenching of star formation in massive galaxies to explain the galaxy bimodality, downsizing, and the universal black hole mass over bulge stellar mass ratio. This suggestion is based on the recent discovery of an ultra-luminous infrared galaxy, i.e., an extreme starburst, that appears to be triggered by a radio jet from the QSO HE 0450-2958 at z = 0.2863, together with the finding in several systems of a positional offset between molecular gas and quasars, which may be explained by the positive feedback effect of radio jets on their local environment.
QSONG: Supermassive Black Holes in Quasars at World's End
Authors: Im Myungshin ,   the QSONG Team
Published: June 2010

We present the initial results of the AKARI mission program QSONG (Quasar Spectroscopic Observation with NIR Grism). QSONG utilizes the unique AKARI capability of performing spectroscopic observations at 2.5–5 μm, with the aim of understanding the mass evolution of ~200 quasars at 3.4 < z < 6.5 from their rest-frame optical spectra. The program also studies the rest-frame NIR spectra of 99 well-studied quasars at low redshift (z < 0.5) and 10 red quasars. With the high-redshift QSONG observations, we detect and resolve redshifted optical lines such as Hα for the first time at this redshift, allowing us to measure the supermassive black hole (SMBH) masses at high redshift using the well-calibrated optical mass estimators and provide an independent assessment of UV line-based mass measurements whose reliability has been controversial. Until the launch of JWST, AKARI will be the only facility in the world capable of studying the rest-frame optical spectra of high-redshift objects out to z ~ 6. Our initial QSONG result indicates a lack of very massive SMBHs at z > 5.5, suggesting that we are possibly witnessing the cosmic growth history of the most massive SMBHs (~ 1010M⊙) in the early universe. Ultimately, an extensive study of the rest-frame optical spectra of high-redshift QSOs will help us understand the evolution and the growth of SMBHs in the early universe.
Emission-Line Taxonomy and the Nature of AGN-Looking Galaxies in the SDSS
Authors: Cid Fernandes Roberto , Stasińska Grażyna , Vale Asari Natalia , Mateus Abílio , Schlickmann Marielli S. , Schoenell William
Published: June 2010

Massive spectroscopic surveys like the SDSS have revolutionized the way we study AGN and their relations to the galaxies they live in. A first step in any such study is to define samples of different types of AGN on the basis of emission-line ratios. This deceivingly simple step involves decisions on which classification scheme to use and data quality censorship. Galaxies with weak emission lines are often left aside or dealt with separetely because one cannot fully classify them onto the standard star-forming, Seyfert, or LINER categories. This contribution summarizes alternative classification schemes which include this very numerous population. We then study how star-formation histories and physical properties of the hosts vary from class to class, and present compelling evidence that the emission lines in the majority of LINER-like systems in the SDSS are not powered by black-hole accretion. The data are fully consistent with them being galaxies whose old stars provide all the ionizing power needed to explain their line ratios and luminosities. Such retired galaxies deserve a place in the emission-line taxonomy.
X-Ray Selected Type 2 QSOs and Their Host Galaxies
Authors: Mainieri Vincenzo ,   the COSMOS Collaboration
Published: June 2010

We present a large sample of X-ray selected type 2 QSOs from the XMM–COSMOS survey. Type 2 QSOs are luminous AGN whose central engines are obscured by large amounts of gas and dust. The selection criteria we have used are based on high X-ray luminosity (LX > 1044 erg s−1) and heavy obscuration (NH > 1022 cm−2). We derived stellar masses and star-formation rate estimates for the host galaxies from the best fit of the observed photometry. Type 2 QSOs are generally hosted in massive galaxies with on-going star formation.
Astrometric and Photometric Variability in Quasars
Authors: Andrei A. H. , Bouquillon S. , Penna J. L. , Taris F. , Anton S. , Souchay J. , Camargo J. I. B. , da Silva Neto D. N. , Vieira Martins R. , Assafin M. , Pinto S. dos Reis Carvalho
Published: June 2010

Quasars are the choicest objects to define a quasi-inertial reference frame. At the same time, they are active galactic nuclei powered by a massive black hole. As the astrometric precision of ground-based optical observations approaches the limit set by the forthcoming GAIA mission, astrometric stability can be investigated. Though the optical emission from the core region usually exceeds the other components by a factor of a hundred, the variability of those components must surely imply some measure of variability of the astrometric baricenter. Whether this is confirmed or not, it puts important constraints on the relationship of the quasar's central engine to the surrounding distribution of matter. To investigate the correlation between long-term optical variability and what is dubbed as the “random walk” of the astrometric center, a program is being pursued at the WFI/ESO 2.2m. The sample was selected from quasars known to undergo large-amplitude and long-term optical variations (Smith et al. 1993; Teerikorpi 2000). The observations are typically made every two months. The treatment is differential, comparing the quasar position and brightness against a sample of selected stars for which the average relative distances and magnitudes remain constant. The provisional results for four objects bring strong support to the hypothesis of a relationship between astrometric and photometric variability. A full account is provided by Andrei et al. (2009).
Dramatic Change in the Spectrum of FeLoBAL SDSS J163255.46+420407.7
Authors: Aoki Kentaro , Misawa Toru
Published: June 2010

We serendipitiously found that the iron-rich low-ionization broad absorption-line (FeLoBAL) quasar SDSS J 163255.46+420407.7 showed a dramatic change in its spectrum over 3.4 years in the rest frame of the quasar. A simple photoionization model suggests the increase in the nuclear radiation caused these changes. Given the recombination coefficient of Fe+, the relaxation time of the absorbing gas suggests ne > 104 cm−3.
Post-Starburst Quasars
Authors: Brotherton Michael , Cales Sabrina , Ganguly Rajib , Shang Zhaohui , Canalizo Gabriela , Stoll R. , Paul C. , Diamond-Stanic A. M.
Published: June 2010

We describe a comprehensive multi-wavelength and multi-faceted program to understand a class of quasars we call post-starburst quasars, which may represent an evolutionary phase in mutual galaxy/black hole evolution.
Co-Evolution of Brightest Cluster Galaxies and Galaxy Activity in the Host Clusters
Authors: Huang Mei-Ling , Chen Lin-wen
Published: June 2010

We have identified ~500 relatively relaxed galaxy clusters at low redshift (z < 0.3) from the maxBCG catalog with double radio lobes at the center; about 200 radio counterparts of brightest cluster galaxies (BCGs) of these clusters appear to be wide-angle tailed (WAT) radio sources, indicating ongoing interaction between its host galaxy and the surrounding ICM. Our analysis suggests that the radio power of WAT is positively correlated with the optical luminosities of host BCGs, and increases with redshift; whereas the cluster ellipticity-radio galaxy fraction relation shows no obvious difference between WAT and non-WAT clusters.
Properties of Quasar and AGN Candidates Detected in the 2MASS/ROSAT Catalogs
Authors: Kouzuma Shinjirou , Yamaoka Hitoshi
Published: June 2010

Color selection is an efficient technique for extracting candidate AGNs. Many AGNs have been selected on the basis of colors at various wavelengths. In this work, we extracted AGN candidates using near-infrared colors and investigated their properties.
Alignment of Stellar and AGN Accretion Disks from SDSS Data
Authors: Lagos Claudia del P. , Padilla Nelson D. , Strauss Michael A. , Hao Lei
Published: June 2010

Lagos, Padilla & Cora (2009) show that if alignments between the galaxy kinematics and the AGN system were to occur, massive galaxies should host BHs with high spin values, regardless of the detailed physics of the BH. Since the BH spin regulates the mass-to-energy conversion (Marconi et al. 2004) and possibly the existence of radio jets (Sikora et al. 2007), this study has a strong impact in our understanding of galaxy formation.
The Active Nucleus in NGC 4579
Authors: Menezes Roberto B. , Steiner João E. , Ricci Tiago V. , Oliveira Alexandre S.
Published: June 2010

In this work, we present an analysis of a data cube obtained with the instrument IFU/GMOS Gemini North telescope centered on the nuclear region of the LINER galaxy NGC 4579. This galaxy is known to have a type 1 AGN (see Eracleous et al. 2002 for a review). The methodology used for the analysis of the data cube was PCA tomography (Steiner et al. 2009), which consists of applying the statistical tool known as principal component analysis (PCA) to extract information from data cubes. The analysis was performed in the following way: first, the data cube for this object was transformed into a data matrix, where each row corresponded to a spatial pixel and each column corresponded to a spectral pixel. We then applied the PCA to this matrix, obtaining eigenvectors as a function of spectral pixels (which correspond to the original coordinates). These eigenvectors, which have the appearance of spectra, are called eigenspectra. We also calculated the projection of the data corresponding to the spatial pixels on each one of the eigenvectors. These images were called tomograms. Figure 1 shows Eigenspectrum E2 and tomogram T2 superposed on T1.
The TANGO Project: Thorough ANalysis of radio-Galaxies Observations
Authors: Ocaña Flaquer Breezy , Leon Tanne Stephane , Combes Francoise , Lim Jeremy
Published: June 2010

We present a sample of radio galaxies selected only on the basis of radio continuum emission and we confirm that these galaxies have lower molecular gas mass than other elliptical galaxies with different selection criteria.
AKARI Infrared Views of AGNs
Authors: Oyabu Shinki
Published: June 2010

The Japanese infrared satellite AKARI has unique capabilities for near-infrared spectroscopy and an all-sky survey in the mid- and far-infrared. We present the recent results on active galactic nuclei that use the unique capabilities of AKARI.
Radio-Optical Analysis of Extended Radio Sources in the First Look Survey Field
Authors: Paulo C. M. , Prandoni I. , Morganti R. , Cress C. M.
Published: June 2010

We combine 610 MHz GMRT data, 1.4 GHz VLA data, and 1.4 GHz WSRT observations, encompassing a ~ 4 square degree field centered on the verification strip of the Spitzer First Look Survey field, to study radio sources down to fluxes of about 0.1 mJy. The spectral index (Figure 1) analysis shows that the majority of multi-component sources are steep-spectrum sources. Nevertheless the spread in the spectral distribution is wide, with a significant number of ultra-steep, flat or inverted sources, possibly indicating a wider range of accretion modes in fainter samples. By cross-correlating 107 multi-component radio sources with the optical catalogues of Marleau et al. (2007) and Papovich et al. (2006), 23 objects were identified.
The AGN Properties of the Starburst Galaxy NGC 7582
Authors: Ricci T. V. , Steiner J. E. , Menezes R. B. , Garcia-Rissmann A. , Cid-Fernandes R.
Published: June 2010

NGC 7582 was identified as a starburst galaxy in the optical (Veron et al. 1981) but its X-ray emission is typical of a Seyfert 1 galaxy (Ward et al. 1978). We analyzed a datacube on this object obtained with the GMOS-IFU on the Gemini-South telescope. After a subtraction of the stellar component using the starlight code (Cid Fernandes et al. 2005), we looked for optical signatures of the AGN. We detected a broad Hα component (Figure 1) in the source where Bianchi et al. (2007) identified the AGN in an HST optical image. We also found a broad Hβ feature (Figure 2), but its emission reveals a extended source. We suggest that it is the light of the AGN scattered in the ionization cone. We propose that NGC 7582 is a Seyfert 1 galaxy. A number of other “hot-spots” and Wolf–Rayet features were also identified.
Fe II Emission in the NLS1 galaxy I Zw 1: Results from NIR Spectroscopy
Authors: Rodríguez-Ardila Alberto , Garcia Rissmann Aurea
Published: June 2010

Fe ii comprises up to one third of the line emission in AGNs. For that reason it is an important coolant that needs to be taken into account to fully understand the energetics of the broad line region (BLR). As such, Fe+ is a potential diagnostic of gas density, column density, turbulence, temperature and continuum shape. However, understanding Fe ii is complicated because of the energy level configuration and different mechanisms that may contribute to the line emission.
A 5.5–35 μm Spectral Analysis of Active Galactic Nuclei
Authors: Sales D. A. , Pastoriza M. G. , Riffel R.
Published: June 2010

The spectroscopic properties of a sample of nine Seyfert 1, six NLS1, 26 Seyfert 2, and three starburst galaxies have been studied at mid-infrared wavelengths in order to determine if the frequency of detection of the brightest emission lines and the continuum shape are correlated with the degree of activity. The raw data were obtained from the Spitzer Infrared Spectrograph (IRS) archive and reduced with the pipeline (version 17.2). The spectra of the galaxies were grouped by type of activity. We conclude through this study that in general the continuum shape of the active galactic nuclei (AGN) is flat between 5 μm and 12 μm, and strong variations are found at longer wavelengths in this sample.
Dust Masses in Early-Type AGN and Inactive Galaxies
Authors: Simões-Lopes Ramiro D. , Martini Paul , Storchi-Bergmann Thaisa
Published: June 2010

It has been known for some time that elliptical galaxies have some form of dust structure at their centers (Kormendy & Djorgovski 1989; van Dokkum & Franx 1995). Nevertheless the exact amount and the origin of the dust is still unknown. In a previous paper, we have shown that all early-type galaxies hosting an AGN have dust at their centers as opposed to only a quarter of the inactive galaxies in a pair-matched sample (Simões Lopes et al. 2007). Here we use Spitzer (IRAC and MIPS) observations of the same sample — 32 active and 32 inactive early-type galaxies — and state-of-the-art spectral modelling from Draine & Li (2007) to estimate the dust mass present in these galaxies. We have also created PAH images by estimating and subtracting the stellar-only contribution to the flux at the 7.9 μm image from the 3.6 μm image.
Spectral Energy Distributions of LIRGs
Authors: U Vivian , Sanders D. B. ,   the GOALS Team
Published: June 2010

We present preliminary results from a study of the SEDs of a complete sample of 65 LIRGs from GOALS. The spectral shapes at λ > 10μm are similar, while the largest variations occur in the NIR (L1μm5μm/L⊙ ~ 1.0–0.01) and UV (L1μm0.12μm/L⊙ ~ 2.0–0.005). Using stellar population synthesis models to fit the UV–NIR continuum data, we derive stellar masses for the host galaxies of log (M*/M⊙) ~ 10.2–11.4 with a mean of ~ 10.8.
Discrimination Between Quasars and Stars by Support Vector Machines
Authors: Zhang Yanxia , Zheng Hongwen
Published: June 2010

We investigated the use of support vector machines (SVMs) to distinguish quasars from stars using survey databases from different wavebands. We first employed a random forest approach for selection and weighting of features. We find that SVMs are an effective method to preselect quasar candidates from multiwavelength data.
New Reverberation Mapping Results from the Lick AGN Monitoring Project
Authors: Bentz Misty C. ,   the LAMP Collaboration
Published: June 2010

Eight new black hole masses have been derived from a recent reverberation-mapping experiment carried out at Lick Observatory. The masses lie in the range ~ 106–107M⊙ and will allow us to extend the low end of AGN scaling relationships by a factor of ~10.
High-Redshift Quasar Monitoring Campaign: Preliminary Results
Authors: Botti Ismael , Lira Paulina , Netzer Hagai , Kaspi Shai
Published: June 2010

We present a monitoring campaign on high-luminosity quasars which will extend the existing reverberation mapping results by two orders of magnitude in luminosity, probing the broad-line region size and black hole mass of luminous AGN at redshift ~ 2 – 3.
The Ultraviolet Flare at the Center of the Elliptical Galaxy NGC 4278
Authors: Cardullo A. , Dalla Bontà E. , Corsini E. M. , Beifiori A. , Buson L. , Morelli L. , Pizzella A. , Bertola F.
Published: June 2010

A large fraction of otherwise normal galaxies shows weak nuclear activity. One of the signatures of the low-luminosity active galactic nuclei (LLAGNs) is the ultraviolet variability which was serendipitously discovered in the center of some low-ionization nuclear emission-line region (LINER) galaxies (see Ho 2008 for a review).
Limits on the Masses of Supermassive Black Holes in 105 Nearby Galaxies
Authors: Corsini E. M. , Beifiori A. , Sarzi M. , Dalla Bontà E. , Pizzella A. , Coccato L. , Bertola F.
Published: June 2010

Secure measurements of the mass of the central supermassive black hole, MBH, in external galaxies are traditionally obtained through the modeling of the stellar and/or gaseous kinematics, most often derived using Hubble Space Telescope (HST) observations in the optical domain. The modeling of the nuclear ionized-gas kinematics has led to accurate MBH measurements at a relatively cheap cost in terms of observation time compared to stellar-dynamical MBH determinations. But only a handful of the objects have turned out to have sufficiently regular gas velocity fields for the purpose of modeling. Nevertheless, the HST archive contains a yet untapped resource that can be used to better constrain the MBH budget across the different morphological types of galaxies, which consists of the vast number of the Space Telescope Imaging Spectrograph (STIS) spectra from which a central emission-line width can be measured. These data allow to put an upper limit on MBH for a large number of galaxies and promise to compensate for the lack of exact measurements when studying the MBH–host galaxy relationships.
Reverberation Mapping Results from MDM Observatory
Authors: Denney Kelly D. , Peterson B. M. , Pogge R. W. , Bentz M. C. , Gaskell C. M. , Minezaki T. , Onken C. A. , Sergeev S. G. , Vestergaard M.
Published: June 2010

Reverberation mapping takes advantage of the presence of a time delay or lag, τ, between continuum and emission line flux variations observed through spectroscopic monitoring campaigns to infer the radius of the broad-line region (BLR) and, subsequently, the central black hole mass in type 1 AGNs. We present results from a multi-month reverberation mapping campaign undertaken primarily at MDM Observatory with supporting observations from around the world. We measure BLR radii and black hole masses for six objects. The primary goal of this campaign was to obtain either new or improved Hβ reverberation lag measurements for several relatively low-luminosity AGNs. Using cross correlation techniques to measure the time delay between the mean optical continuum flux density around 5100 Å and the integrated Hβ flux, we determine the Hβ lags and black hole mass measurements listed in columns 2 and 3 of Table 1, respectively. Column 4 tells if this measurement is new, an improvement meant to replace a previous, less reliable measurement, or simply an additional measurement not used to replace a previous value. The complete results from this study are currently being prepared for publication. A subsequent velocity-resolved analysis of the Hβ response shows that three of the six primary targets demonstrate kinematic signatures (column 5) of infall, outflow, and non-radial virialized motions (see Denney et al. 2009).
Evolution of Supermassive Black Holes
Authors: Filloux Charline , de Freitas Pacheco J. A. , Durier Fabrice , Silk Joseph
Published: June 2010

Cosmological simulations describing both the evolution of supermassive black holes and their host galaxies were performed by using the tree PM-SPH code GADGET-2 (Springel 2005). Physical mechanisms affecting the dynamics and the physical conditions of the gas (ionization and cooling processes, local heating by stars, injection of mechanical energy by supernovae, chemical enrichment) were introduced in the present version of the code (Filloux 2009). Black holes in a state of accretion (AGNs) also inject mechanical energy in the surrounding medium, contributing for quenching the star formation activity. In all simulations a ΛCDM cosmology was adopted (h = 0.7, ΩΛ=0.7, Ωm=0.3, Ωb=0.046 and σ8=0.9). Simulations were performed in a volume with a side of 50h−1 Mpc, starting at z = 50 and through the present time (z = 0). For low and intermediate resolution runs, the initial gas mass particles are respectively 5.35× 108M⊙ and 3.09×108M⊙. Black holes (BHs) are represented by collisionless particles and seeds of 100 M⊙ were introduced in density peaks at z = 15, growing either by accretion or coalescence. The accretion rate from the “disk mode” is based on a turbulent viscous thin disk model whereas in the “spherical mode” the rate is given by the Bondi–Hoyle formula. When accreting matter, jets, modeled by conical regions perpendicular to the disk plane, inject kinetic energy into the surrounding medium. Two models were tested: in the first, the injected energy rate is about 10% of the gravitational energy rate released in the accretion process while in the second, the injected energy rate is based on the Blandford & Znajek (1977) mechanism. All simulations give, at z = 0, similar black hole mass function but they overestimate slightly the BH density for masses above ~ 108M⊙. The resulting BH density in this mass range is affected by feedback processes since they control the amount of gas available for accretion. The present simulations are not able to produce very massive BHs (~109M⊙) at z ~ 6. However the evolution of the BH mass density derived from our simulations are in quite good agreement with that derived from the QSO luminosity function. This indicates that our simulations reproduce quite well the average accretion rate history of BHs. Correlations between the BH mass and properties of the host galaxy (velocity dispersion for bulge systems or the stellar mass or the dark halo mass) are also well reproduced. In conclusion, these exploratory simulations reproduce the data at z = 0 quite well. However, the present adopted recipe for the accretion rate in the “disk mode” seems to be inefficient to produce massive BHs as early as z ~ 6. Higher resolution simulations including a new approach for modeling the “disk mode” are presently under way and that particular difficulty is expected to be solved.
Investigating the High-Luminosity End of the Active Galaxy MBH–σ* Relation
Authors: Grier C. J. , Watson L. C. , Peterson B. M. , Martini P. , Bentz M. C. , Dasyra K. M. , Denney K. D. , Dietrich M. , Ferrarese L. , Pogge R. W. , Tacconi L. J.
Published: June 2010

While characterization of the MBH–σ* relationship in AGNs has improved due to the increase in available data and the improvement in accuracy of both MBH and σ* measurements, additional data at the high-luminosity end of the distribution of quasars are needed, as recent studies indicate that perhaps the relation steepens in this regime. To this end, we present three new measurements in objects at the high-luminosity end of the relation.
No Evolution in the MBH–M*,total Relation Over the Last 9 Gyrs
Authors: Jahnke Knud , Cisternas Mauricio , Inskip Katherine J. ,   the COSMOS Collaboration
Published: June 2010

We investigate 10 QSO host galaxies at 1<z<2 in the COSMOS field (Scoville et al. 2007), observed with the HST in both ACS/WFC I-band and NICMOS/NIC3 H-band. We find that our galaxies with mean z = 1.4 follow the local MBH–Mbulge relation exactly – however, not with an explicit bulge mass, but with their total stellar mass.
Black Hole Demographics: Statistical Characteristics of Accreting Black Holes
Authors: Netzer Hagai
Published: June 2010

This review summarizes the important properties of active black holes (BHs) up to z ~ 2; their mass, accretion rate, and growth rate. At higher redshifts, such information is only available for small samples that do not represent the entire population of active galactic nuclei (AGNs). Black hole spin is still unknown; it is speculated to change with redshift, but with little experimental evidence. The available data sets also enable a direct comparison of BH accretion rates and host galaxy star-formation rates (SFRs). The ratio of the BH growth rate g(BH) and the bulge growth rate g(bulge), suggests that the two are proportional to each other. The local value of g(bulge)/g(BH) in low-luminosity AGNs is of order 100 and the corresponding ratio in high-luminosity, high-redshift AGNs is of order 10. This has important implications regarding the parallel evolution of active BHs and their hosts.
The Clustering Properties of Intermediate X-ray Luminosity AGN at z ~ 3
Authors: Francke Harold , Gawiser Eric , Lira Paulina , Infante Leopoldo ,   the MUSYC Collaboration
Published: June 2010

We present clustering results for AGN jointly selected to have optical and X-ray data at z ~ 3 in the ECDF-S field. Using Chandra X-ray imaging and UVR optical colors from MUSYC photometry, we selected a sample of 58 z ~ 3 AGN candidates. From the optical data we also selected 1385 Lyman break galaxies (LBG) in the range 2.8 < z < 3.8 with R < 25.5 mag. From optical spectroscopy, we have also determined redshifts and AGN types and estimated the UV and X-ray luminosities for the set of active galaxies selected by this method. We performed autocorrelation and cross-correlation analyses and present here our results for the clustering amplitudes and dark matter (DM) halo masses of each sample. The clustering analysis yields median DM halo masses of log M/M⊙ = 11.9±0.2 for the LBG sample, and log M/M⊙ = 12.9+0.4−0.9 for the sample of AGN. This shows that the active supermassive black holes (SMBHs) targeted by this selection method tend to sit in galaxies more massive than the typical population of UV–continuum selected galaxies, although showing much less clustering than SDSS quasars at the same redshift. Additionally, the expected evolution of the DM halos in ΛCDM cosmology implies that today these z ~ 3 SMBHs are hosted by group-sized halos, with masses log M/M⊙ = 14.1+0.3−0.2, at the high-mass end of the distribution of LBG DM halo descendants at z = 0.
Detecting Quasars by Their Variability
Authors: Schmidt Kasper B. , Rix Hans-Walter , Jester Sebastian , Marshall Phil , Dobler Gregory , Hennawi Joseph F.
Published: June 2010

We demonstrate that quantifying the intrinsic variability of quasars by fitting individual structure function data pairs with a 2-parameter power law model separates quasars from contaminating variable and non-variable point sources with a completeness of 93% and a purity of 99%. This approach can be used to select quasar samples in surveys like that being performed by Pan-STARRS1, where the usual color selection of quasars is not possible due to a filter system that is too red.
Obscuring and Feeding Supermassive Black Holes with Evolving Nuclear Star Clusters
Authors: Schartmann M. , Burkert A. , Krause M. , Camenzind M. , Meisenheimer K. , Davies R. I.
Published: June 2010

Recently, high-resolution observations made with the help of the near-infrared adaptive optics integral field spectrograph SINFONI at the VLT proved the existence of massive and young nuclear star clusters in the centers of a sample of Seyfert galaxies. With the help of high-resolution hydrodynamical simulations with the pluto code, we follow the evolution of such clusters, especially focusing on mass and energy feedback from young stars. This leads to a filamentary inflow of gas on large scales (tens of parsecs), whereas a turbulent and very dense disk builds up on the parsec scale. Here we concentrate on the long-term evolution of the nuclear disk in NGC 1068 with the help of an effective viscous disk model, using the mass input from the large-scale simulations and accounting for star formation in the disk. This two-stage modeling enables us to connect the tens-of-parsecs scale region (observable with SINFONI) with the parsec-scale environment (MIDI observations). At the current age of the nuclear star cluster, our simulations predict disk sizes of the order 0.8 to 0.9 pc, gas masses of order 106M⊙, and mass transfer rates through the inner boundary of order 0.025 M⊙yr−1, in good agreement with values derived from observations.
Near-Eddington Luminosity Flares from Quiescent Supermassive Black Holes
Authors: Gezari Suvi
Published: June 2010

A dormant supermassive black hole lurking in the center of a galaxy will be revealed when a star passes within its tidal disruption radius, is disrupted, and a flare of electromagnetic radiation is emitted when the bound stellar debris is accreted. Although the tidal disruption of a star is a rare event in a galaxy, ~ 10−4 yr−1, observational candidates have emerged in all-sky X-ray and deep UV surveys in the form of luminous UV/X-ray flares from otherwise quiescent galaxies. We present the light curves and broadband properties of three tidal disruption candidates discovered in the UV by GALEX, and find that (1) the light curves are well-fitted by the power-law decline expected for the fallback of debris from a tidally disrupted solar-type star, and (2) the UV/optical spectral energy distributions can be attributed to thermal emission from an envelope of debris located at ten times the tidal disruption radius of the central black hole. We use the observed peak absolute optical magnitudes of the flares to predict the detection capabilities of the next generation of wide-field optical synoptic surveys.
Quasars Do Not Live in Merging Systems: No Enhanced Merger Rate at z≲0.8
Authors: Cisternas Mauricio , Jahnke Knud , Inskip Katherine J. ,   the COSMOS Collaboration
Published: June 2010

We tackle the long-standing question “what is the relevance of major mergers and interactions as triggering mechanisms for AGN activity?” We study a sample of 83 quasars over z ~ 0.3–1.0 with high-resolution HST/ACS imaging in the F814W (broad I) band in the COSMOS field (Scoville et al. 2007), detected by their X-ray emission in the XMM-Newton survey (Hasinger et al. 2007). We perform a visual analysis of their morphologies, looking for signatures of merging and interactions in their host galaxies that could potentially be related to the AGN fueling mechanism. To get the best possible picture of the host galaxies, we remove the bright quasar by modeling each of them as a Sersic surface brightness profile plus a central point source, through a 2-D parametric fit.
Growing Supermassive Black Holes Inside Cosmological Simulations
Authors: Levine Robyn , Gnedin Nickolay Y. , Hamilton Andrew J. S.
Published: June 2010

Using a hydrodynamic adaptive mesh refinement code, we simulate the growth and evolution of a typical disk galaxy hosting a supermassive black hole (SMBH) within a cosmological volume. The simulation covers a dynamical range of 10 million, which allows us to study the transport of matter and angular momentum from super-galactic scales down to the outer edge of the accretion disk around the SMBH. A dynamically interesting circumnuclear disk develops in the central few hundred parsecs of the simulated galaxy, through which gas is stochastically transported to the central black hole.
The Variable High-Velocity Outflows Seen in X-Ray Spectra
Authors: Kaspi Shai
Published: June 2010

Several AGNs have been reported to have ultra-high velocity (UHV) outflows (of order 0.3 ≳ ν/c ≳ 0.05) that are detected in their X-ray spectrum. Re-visiting these outflow observations reveal that the spectrum has changed along with the claimed outflows. The luminous quasar PDS 456 is the brightest AGN in which a UHV outflow has been claimed to be present in its grating spectrum. We report on an XMM–Newton observation of this source, as well as analysis of past observations, which reveal its variable nature and the variable nature of UHV outflows. In this object, as well as in a few others, repeated observations failed to reproduce the previous absorption spectra. This indicates that variability is common among the UHV winds. A discussion of the reality, significance, and the interpretation of the UHV outflow phenomenon is presented. If UHV outflows exist, they might be a transiting phenomenon, as indicated from repeated observations, and this has to be taken into account when studying the influence of these outflows on the surrounding galaxy.
Black Hole Motion as a Trigger of Orbital Resonances
Authors: Boily Christian M. , Gaudin Nicolas , Richard Sabine
Published: June 2010

The motion of a black hole (BH) induces a strong response from the surrounding stellar population. We recall the case of an analytical harmonic potential where half of the stars on circular orbits in that potential shift to an orbit of lower energy, while the other half receive a positive boost and recede to a larger radius. The black hole itself remains on an orbit of fixed amplitude and merely acts as a catalyst for the evolution of the stellar energy distribution function f(E). Numerical integration with a response code show that this effect is operative out to a radius of ~3 to 4 times the radius of influence of the BH RBH. The results for the kinematic signature of BH motion are not sensitive to the shape of the potential and the temperature of the stars measured with Toomre's Q parameter. We report on the evolution of fully self-gravitating systems when damping of the BH orbit is way off the expected exponential decay obtained from the Chandrasekhar formula, a possible result from energy exchanges with the background stars.
On the Physical Mechanism Underlying PC1 and Baldwin Effect in Quasars
Authors: Dong Xiao-Bo , Wang Ting-Gui , Wang Jian-Guo , Fan Xiaohui , Wang Huiyuan , Zhou Hongyan , Yuan Weimin
Published: June 2010

Recent work (Baskin & Laor 2004; Dong et al. 2009a, b) suggests that the Eddington ratio (l ≡ L/LEdd) is the origin of all the significant first-order object-to-object variations of quasar spectral properties from the zeroth-order similarity of AGN spectra; specifically, this includes the PC1 of Boroson & Green (1992), the classic or inverse Baldwin effect (Baldwin 1977), and even blueshifting (i.e., blue asymmetry) of high-ionization emission lines (Dong et al. 2009c).
Modeling Line Emission from Disk Winds
Authors: Hall Patrick B. , Chajet Laura S.
Published: June 2010

Murray & Chiang (1997) developed a model wherein broad emission lines come from the optically thick base of a rotating, outwardly accelerating wind at the surface of an accretion disk. Photons preferentially escape radially in such a wind, explaining why broad emission lines are usually single-peaked. Less well understood are the observed shifts of emission-line peaks (from 1000 km s−1 redshifted to 2500 km s−1 blueshifted in C iv, with an average 800 km s−1 blueshift).
Feeding Versus Feedback in AGNs from Near-Infrared IFU Observations: The Case of Mrk 1066
Authors: Riffel Rogemar A. , Storchi-Bergmann Thaisa
Published: June 2010

Previous studies of the central region of active galaxies show that the molecular and ionized gas have distinct kinematics and flux distributions, with the former dominated by quiescent kinematics characteristic of rotation in the galactic plane and the latter with more disturbed kinematics and apparently extending to larger galactic latitudes. These results suggest that the molecular gas can be a tracer of the feeding of the AGN and the ionized gas a tracer of its feedback (e.g., Riffel et al. 2009, 2008, 2006; Storchi-Bergmann et al. 2009a, b). In the present study we use Gemini NIFS integral field observations of the inner 700×700 pc2 of the Seyfert galaxy Mrk 1066 at a spatial resolution of ~ 35 pc to investigate if the above scenario is also valid for this galaxy.
Tracing Outflows in High-Redshift Quasars
Authors: Simon Leah E. , Hamann Fred
Published: June 2010

We present preliminary results from the largest-ever survey of high-resolution associated absorption line (AAL) region metallicities and physical properties in a sample of high redshift (z > 3) quasars.