bluuebunny/crossref_metadata_2025 huggingface dataset:
La historiografia economica de Mexico
Authors: Coatsworth John H.
Published: June 2010

No cabe duda alguna de que la pasada década ha presenciado un extraordinario avance en la historia de la actividad económica mexicana. Gran parte de lo que creíamos saber en 1976 ha quedado reducido a notas a pie de página, que dan fe del abandono de ideas erróneas y de la adquisición de nuevos conocimientos. En su mayoría, los avances que con buen acierto celebramos no se deben, como cabría esperar, ni a los que practican lo que seguíamos Ilamando «nueva» historia económica hasta hace un decenio, ni a los teóricos esquemáticos de los cuales tomamos aquellos rimbombantes' subtítulos con que una vez decoramos nuestros manuscritos. Este ámbito ha avanzado, por el contrario, en virtud de una sostenida acumulación de historias institucionales, financieras y regionales que han proporcionado abundantes datos nuevos y juicios más afinados sobre una amplia gama de cuestiones. Y ha avanzado también como consecuencia de la compilación y publicación de nuevas series de información cuantitativa que sólo recientemente han empezado a explotar los historiadores.
Origenes y Problemas Teoricos de la Matematizacion de la Economia en el Siglo XIX
Authors: Muñoz Carlos Camino , Bollo Eduardo Fernandez
Published: June 2010

El espectacular auge de la Economía matemática, que no se ha desmentido desde las postrimerías de la primera guerra mundial, impulsa, incluso a aquellos que mantinen serias reticencias sobre el tema, a plantearse el problema epistemológico de la relación entre las matemáticas (o la Matemática) y la Economía. Se plantea, así, la cuestión de saber hasta qué punto la matematización transforma no sólo los métodos sino la naturaleza y el estatus epistemológico de la Teoría Económica, ya sea en sentido positivo permitiéndole alcanzar un rigor científico, ya sea de manera negativa haciéndole correr el peligro de desvirtuar su desarrollo propio. Así, durante el Congreso de Economistas de Lengua Francesa, reunido en Lausanne para el centenario de Walras, Maurice Allais pudo decir que «los trabajos efectuados desde hace veinte años por los economistas han hecho, indudablemente, progresar las matemáticas, pero no la Economía Política».
Puntualizaciones A Unas Puntualizaciones
Authors: Martin Sebastian Coll
Published: June 2010

Jordi Maluquer de Motes ha tenido por conveniente escribir unas puntua-lizaciones a la reseña de que soy autor sobre el libro Catalunya, la fábrica d'Espanya, puntualizaciones que igualan en extensión a la propia reseña y que cuadruplican aproximadamente el espacio que en la misma dedicaba yo a su personal contribución. Trataré de poner por escrito en forma mucho más breve las reflexiones que me sugieren sus precisiones, las cuales, dejando al margen su teoría acerca de los medios por los cuales los aprendices de historiadores acceden a la propiedad de sus calculadoras, se pueden agrupar en dos apartados.
La demanda de textiles de las familias castellanas a finales del Antiguo Régimen, 1750–1850: ¿Aumento del consumo sin industrialización?
Authors: Palencia Fernando Carlos Ramos
Published: June 2010

En este artículo se estudia la demanda de textiles por parte de las families castellanas de la provincia de Palencia entre 1750 y 1850. A partir de un análisis sistemático de inventarios post mortem, se constata un aumento en el consumo de bienes textiles que afectó a todas las capas sociales ubicadas tanto en entornos urbanos como rurales. No obstante, existían una serie de límites al desarrollo de la demanda y del consumo: pervivencia de crisis de subsistencias y mortalidad, lento crecimiento demográfico, fluctuaciones en los niveles de precios agrícolas, integración de los mercados no uniforme, incremento de la masa de indigentes, excesiva concentración de la riqueza, etcetera. La existencia de estos límites incidieron en el resultado final: una revolutión industriosa sin industrialización.
The Co-Evolution of Galaxies and Black Holes: Current Status and Future Prospects
Authors: Heckman Timothy M.
Published: June 2010

I begin by summarizing the evidence that there is a close relationship between the evolution of galaxies and supermassive black holes. They evidently share a common fuel source, and feedback from the black hole may be needed to suppress over-cooling in massive galaxies. I then review what we know about the co-evolution of galaxies and black holes in the modern universe (z < 1). We now have a good documentation of which black holes are growing (the lower mass ones), where they are growing (in the less massive early-type galaxies), and how this growth is related in a statistical sense to star formation in the central region of the galaxy. The opportunity in the next decade will be to use the new observatories to undertake ambitious programs of 3-D imaging spectroscopy of the stars and gas in order to understand the actual astrophysical processes that produce the demographics we observe. At high redshift (z > 2), the most massive black holes and the progenitors of the most massive galaxies are forming. Here, we currently have a tantalizing but fragmented view of their co-evolution. In the next decade, the huge increase in sensitivity and discovery power of our observatories will enable us to analyze the large, complete samples we need to achieve robust and clear results.
The Early Evolution of Massive Black Holes
Authors: Volonteri Marta
Published: June 2010

Massive black holes (MBHs) are nowadays believed to reside in most local galaxies. Studies have also established a number of relations between the MBH mass and properties of the host galaxy such as bulge mass and velocity dispersion. These results suggest that central MBHs, while much less massive than their hosts (~ 0.1%), are linked to the evolution of galactic structure. When did it all start? In hierarchical cosmologies, a single big galaxy today can be traced back to the stage when it was split up in hundreds of smaller components. Did MBH seeds form with the same efficiency in small proto-galaxies, or did their formation have to await the buildup of substantial galaxies with deeper potential wells? I briefly review here some of the physical processes that are conducive to the evolution of the massive black hole population. I will discuss black hole formation processes for “seed” black holes that are likely to take place at early cosmic epochs, and possible observational tests of these scenarios.
OSIRIS View of Submillimeter Galaxies: A 2–D Spectroscopic Insight to Starburst Galaxies in the High-Redshift Universe
Authors: Menéndez-Delmestre K. , Blain A. W. , Swinbank M. , Smail I. , Chapman S. C. , Ivison R. J.
Published: June 2010

Ultra-luminous infrared galaxies (LIR > 1012L⊙) are locally rare, but appear to dominate the co-moving energy density at higher redshifts (z > 2). Many of these are optically faint, dust-obscured galaxies that have been identified by the detection of their thermal dust emission in the sub-mm. Multi-wavelength spectroscopic follow-up observations of these sub-mm galaxies (SMGs) have shown that they are massive (Mstellar ~ 1011M⊙) objects undergoing intense star-formation (SFRs ~ 102–103M⊙ yr−1) with a mean redshift of z ~ 2, coinciding with the epoch of peak quasar activity. Furthermore, the presence of AGNs in ~ 28–50% of SMGs has been unveiled in the X-ray and near-IR. When both AGN and star-formation activity are present, long-slit spectroscopic techniques face difficulties in disentangling their independent contributions from integrated spectra. We have observed Hα emission from a sample of three SMGs in the redshift range z ~ 1.4–2.4 with the integral field spectrograph OSIRIS on Keck, in conjunction with Laser Guide Star Adaptive Optics. The spatially resolved, two-dimensional spectroscopic insight that these observations provide is the only viable probe of the spatial distribution and line-of-sight motion of ionized gas within these galaxies. We detect multiple galactic-scale sub-components, distinguishing the compact, broad Hα emission arising from an AGN from the more extended narrow-line emission of star-forming regions spreading over ~ 8–17 kpc. We explore the dynamics of gas in the inner galaxy halo to improve our understanding of the internal dynamics of this enigmatic galaxy population. We find no evidence of ordered orbital motion such as would be found in a gaseous disk, but rather large velocity offsets of a few hundred kilometers per second between distinct galactic-scale sub-components. Considering the disturbed morphology of SMGs, these sub-components are likely remnants of originally independent gas-rich galaxies that are in the process of merging, hence triggering the ultraluminous SMG phase.
The Quasar Continuum
Authors: Elvis Martin
Published: June 2010

The powerful compact continuum emission from quasars is understood only in outline. New surveys allow investigation of the quasar continuum over a wide range of parameters (z, L, L/LEdd) and wavelengths (radio to X-ray). I review the spectral energy distributions of quasars and how new scaling relations with physical parameters promise to take us to a deeper understanding of the quasar continuum.
X-Ray, Optical, and Near-IR Long-Term Monitoring of AGN
Authors: Lira Paulina , Arévalo Patricia , Uttley Phil , McHardy Ian , Breedt Elme
Published: June 2010

We are conducting long-term monitoring of several AGN with the aim of understanding the interplay between the emitting regions around the central black hole as well as the physics of the accreting flow. Here we present results for two of our sources, NGC 3783 and MR 2251–178, with strong evidence for disk-driven variability and the existence of cold accretion disks, where near-IR emission can be clearly detected from a region close to the black hole.
The Ying and Yang of the M 83 Nucleus
Authors: Mast Damián , Díaz Rubén J. , Dottori Horacio A. , Agüero María P. , Rodrigues Irapuán , Albacete-Colombo Juan F.
Published: June 2010

The spiral galaxy M 83, an SB(rs)b at only 4.5 Mpc, is a privileged case for study of the detailed physics on spatial scales of a tenth of a parsec. With 3-D spectroscopic observations using CIRPASS on Gemini-S, we studied the ionized gas properties in J-band with spatial resolution of 0.″5 (Figure 1). The Paβ velocity field shows two dynamical centers, neither of them coincident with the bulge center, identified with the optical nucleus (ON) and the hidden nucleus (HN), with masses, within a radius of 10 pc, of MON = (1.8±0.4)× 107M⊙ and MHN = (1.0±0.4)× 107M⊙. Using the Paβ equivalent width together with population synthesis models, we are able to estimate the ages of both mass concentrations, TON = 8 Myr and THN =6–7 Myr. Adding complexity to this puzzling scenario, we used GMOS+Gemini imaging and spectroscopy to study the radio source J133658.3–295105 (Dottori et al. 2008) and find that Hα emission at the position of this source is redshifted by ~130 km s−1 with respect to an M 83 H II region, leading us to face the possibility of that we are witnessing the ejection of an object by gravitational recoil from the M 83 nucleus. A fit to the X-ray spectrum obtained Chandra supports the association between this source and the disk of M 83 by the presence of the Fe Kα line at 6.7 keV.
Dusty Structure Around Type 1 AGNs
Authors: Mor Rivay , Netzer Hagai , Elitzur Moshe
Published: June 2010

We present a detailed investigation of the MIR continuum emission of type 1 QSOs and define the main emission components. Our model requires three components: a clumpy torus, dusty narrow-line region (NLR) clouds and a blackbody-like hot dust.
Submillijansky Radio-Quiet and Radio-Loud AGN in the Chandra Deep Field South
Authors: Padovani Paolo , Kellermann Ken , Fomalont Edward , Miller Neal , Tozzi Paolo , Mainieri Vincenzo , Rosati Piero
Published: June 2010

We report on some preliminary results on the evolution and luminosity functions of submillijansky (sub-mJy) radio sources, based on the VLA Chandra Deep Field South (CDFS) sample.
Distinguishing Between AGN and Star-Forming Galaxies in ATLAS
Authors: Randall Kate E. , Hopkins Andrew M. , Norris Ray P.
Published: June 2010

The Australia Telescope Large Area Survey (ATLAS; Norris et al. 2006) is the widest deep radio survey to date, covering approximately 7 square degrees over two fields, with extensive complementary data. We are investigating all possible discriminants between active galactic nuclei (AGN) and star-forming galaxies (SFG) in ATLAS, to determine a robust formula for distinguishing the two.
Kinematics and Principal Component Analysis from IFU Spectroscopy of the Post-Starburst Quasar SDSS J0210–0903
Authors: Sanmartim David , Storchi-Bergmann Thaisa , Brotherton Michael S.
Published: June 2010

We present 2-D mapping and analysis of the gaseous kinematics of the inner 7″ × 5″ of one of nearest (z = 0.0414) and brightest post-starburst quasars (PSQ) by using spectra obtained with the Integral Field Unit (IFU) of the Gemini Multi-Object Spectrograph on the Gemini North Telescope (Allington-Smith et al. 2002). Such quasars are broad-lined AGNs that also show the Balmer jumps and the high-order Balmer absorption lines from A stars typical of massive post-starburst populations of a few hundred Myrs (Brotherton et al. 2007). From measurements of the emission-line profiles, we constructed two-dimensional maps for the flux distributions, line ratios, radial velocities and gas velocity dispersions for the Hβ and [Oiii] emitting gas, similar to those of previous studies by our group (e.g., Barbosa et al. 2009).
Beware of Fake AGNs
Authors: Stasińska G. , Vale Asari N. , Cid Fernandes R.
Published: June 2010

In the BPT diagram, the distribution of the emission-line galaxies from the Sloan Digital Sky Survey (SDSS) evokes the wings of a seagull. Traditionally, galaxies in the right wing are considered to host AGNs. Our study of the stellar populations of SDSS galaxies showed that ~ 1/4 of galaxies thought to host LINERs are in fact “retired galaxies,” i.e., galaxies that stopped forming stars and are ionized by hot post-AGB stars and white dwarfs (Stasińska et al. 2008). When galaxies that lack some of the lines needed to place them in the BPT diagram are included, the fraction of retired galaxies is even larger (Cid Fernandeset al., these proceedings).
Toward Precision Measurement of Central Black Hole Masses
Authors: Peterson Bradley M.
Published: June 2010

We review briefly direct and indirect methods of measuring the masses of black holes in galactic nuclei, and then focus attention on supermassive black holes in active nuclei, with special attention to results from reverberation mapping and their limitations. We find that the intrinsic scatter in the relationship between the AGN luminosity and the broad-line region size is very small, ~0.11 dex, comparable to the uncertainties in the better reverberation measurements. We also find that the relationship between reverberation-based black hole masses and host-galaxy bulge luminosities also seems to have surprisingly little intrinsic scatter, ~0.17 dex. We note, however, that there are still potential systematics that could affect the overall mass calibration at the level of a factor of a few.
Fossil SMBHs in the Milky Way Halo
Authors: Bellovary Jillian , Governato Fabio , Quinn Tom
Published: June 2010

As galaxies assemble through hierarchical merging, some black holes grow to become the central black holes of massive galaxies; however, others may be stripped via interactions into regions of galaxies where they will remain quiescent. Such objects may be the source of observed off-nuclear intermediate-mass black hole candidates, as detected by Farrell et al. (2009). We use a cosmological N-body simulation of a disk-dominated galaxy (Vc = 140 km s−1, presented by Governato et al. 2009) to examine the formation and merging histories of seed black holes during hierarchical assembly. Our method incorporates star formation, supernova feedback, a physically motivated description of black hole seed creation, growth, and merging.
An Hα Dynamical Mass for HE 0047–1756
Authors: Inskip K. J. , Jahnke K. , Rix H.-W. , Peng C. Y.
Published: June 2010

We derive Mbulge for HE 0047–1756 via Hα gas dynamics. The resulting large value of MBH/Mbulge may imply evolution in the correlation at high redshifts.
Quasar and Supermassive Black Hole Evolution
Authors: Croom Scott M. , Fine Stephen ,   the 2SLAQ Survey Team
Published: June 2010

We present results from statistical analysis of the largest quasar surveys currently in existence: the Sloan Digital Sky Survey (SDSS), the 2dF QSO Redshift Survey (2QZ), and the 2dF-SDSS LRG and QSO (2SLAQ) Survey. The quasar luminosity function shows highly significant (>99.9%) evidence of downsizing: the number density of faint quasars peaks at lower redshift than bright quasars. We measure the distribution of quasar broad-line widths as a function of luminosity, particularly focusing on the Mg ii λ2799 line. There is a clear trend, such that more luminous quasars show less scatter in line width than fainter quasars. However, the scatter in line width for any given luminosity (particularly in the brightest objects) is so small that it challenges our current understanding of virial black hole mass estimates.
AGN Evolution from Large and Deep X-Ray Surveys
Authors: Brusa Marcella
Published: June 2010

Over the last few years, the existence of mutual feedback effects between accreting supermassive black holes powering AGN and star formation in their host galaxies has become evident. This means that the formation and the evolution of AGN and galaxies should be considered as one and the same problem. As a consequence, the search for, and the characterization of the evolutionary and physical properties of AGN over a large redshift interval is a key topic of present research in the field of observational cosmology. Significant advances have been obtained in the last ten years thanks to the sizable number of XMM–Newton and Chandra surveys, complemented by multiwavelength follow-up programs. I will present some of the recent results and the ongoing efforts (mostly from the COSMOS and CDFS surveys) aimed at obtaining a complete census of accreting black holes in the universe, and a characterization of the properties of the host galaxies.
Using Ark 564 and I Zw 1 as Laboratories for Modeling the Fe II Pseu0do-Continuum in QSOs
Authors: Eufrasio R. T. , Bruhweiler F. , Verner E. , Wills B. , Crenshaw D. M.
Published: June 2010

In this work, we use the low-redshift, narrow-line Seyfert 1 (NLS1) galaxies Ark 564 and I Zw 1 as laboratories for modeling the Fe ii emission features in the wavelength range 1200–6700 Å. We utilize data acquired with the Hubble Space Telescope and the 2.7-m telescope at McDonald Observatory.
Mergers of Luminous Early-Type Galaxies
Authors: Wen Z. L. , Han J. L. , Liu F. S.
Published: June 2010

Galaxy mergers play an important role in many astrophysical processes, such as growth of massive galaxies, triggering AGN, formation of supermassive black hole (SMBH) binaries, and gravitational wave (GW) radiation. Merger rate is one of key quantities for these studies. Previous studies show that the pair fraction varies in a range of 1%–10% in the redshift range of z = 0.2–1.2. These merger rates are usually calculated from projected close pairs, and very few previous authors have carefully checked the merging fraction of a large sample of pairs.
The Impact of Nuclear Star Formation on Gas Inflow to AGN
Authors: Davies R. I. , Hicks E. , Schartmann M. , Genzel R. , Tacconi L. J. , Engel H. , Burkert A. , Krause M. , Sternberg A. , Mueller Sánchez F. , Maciejewski W.
Published: June 2010

Our adaptive optics observations of nearby AGN at spatial resolutions as small as 0.″085 show strong evidence for recent, but no longer active, nuclear star formation. We begin by describing observations that highlight two contrasting methods by which gas can flow into the central tens of parsecs. Gas accumulation in this region will inevitably lead to a starburst, and we discuss the evidence for such events. We then turn to the impact of stellar evolution on the further inflow of gas by combining a phenomenological approach with analytical modelling and hydrodynamic simulations. These complementary perspectives paint a picture in which all the processes are ultimately regulated by the mass accretion rate into the central hundred parsecs, and the ensuing starburst that occurs there. The resulting supernovae delay accretion by generating a starburst wind, which leaves behind a clumpy interstellar medium. This provides an ideal environment for slower stellar outflows to accrete inwards and form a dense turbulent disk on scales of a few parsecs. Such a scenario may resolve the discrepancy between the larger scale structure seen with adaptive optics and the small-scale structure seen with VLTI.
Inflows and Outflows in Nearby AGN from Integral Field Spectroscopy
Authors: Storchi-Bergmann Thaisa
Published: June 2010

I report recent results on the kinematics of the inner few hundred parsecs (pc) around nearby active galactic nuclei (AGN) at a sampling of a few pc to a few tens of pc, using optical and near-infrared (near-IR) integral field spectroscopy obtained with the Gemini telescopes. The stellar kinematics of the hosts — comprised mostly of spiral galaxies — are dominated by circular rotation in the plane of the galaxy. Inflows with velocities of ~50 km s−1 have been observed along nuclear spiral arms in (optical) ionized gas emission for low-luminosity AGN and in (near-IR) molecular gas emission for higher-luminosity AGN. We have also observed gas rotating in the galaxy plane, sometimes in compact (few tens of pc) disks which may be fuelling the AGN. Outflows have been observed mostly in ionized gas emission from the narrow-line region, whose flux distributions and kinematics frequently correlate with radio flux distributions. Channel maps along the emission-line profiles reveal velocities as high as ~ 600 km s−1. Mass outflow rates in ionized gas range from 10−2 to 10−3M⊙ yr−1 and are 10–100 times larger than the mass accretion rates on to the AGN, supporting an origin for the bulk of the outflow in gas from the galaxy plane entrained by a nuclear jet or accretion disk wind.
Precession in Extragalactic Parsec-Scale Accretion Disks
Authors: Caproni Anderson , Livio Mario , Abraham Zulema , Mosquera Cuesta Herman J.
Published: June 2010

In this work, we study the feasibility of four physical mechanisms for driving jet/disk precession in the galaxies NGC 4258, NGC 1068, 3C 120, OJ 287 and Arp 102B. Given the many observational uncertainties that still exist in the parameters of those AGN, we find that it is difficult to discriminate unambiguously what mechanism is actually responsible for precession.
Dynamics of Black Holes in Rotating Cores
Authors: Fiestas Jose A. , Spurzem Rainer
Published: June 2010

We study the dynamical interaction between stars surrounding black holes in self-gravitating galaxy cores by using realistic N-body techniques, calibrated by Fokker–Planck approximated models (Fiestas, Spurzem, & Kim 2006). We study the evolution over the relaxation time (collisional nuclei) of non-spherical (triaxial) models as flattening of the system due to rotation is allowed. We follow the interplay between velocity diffusion due to relaxation and black hole star accretion and study accretion rates and cusp formation in spherically symmetric and axisymmetric models.
On the Origin of the Galactic Center S Stars
Authors: Griv Evgeny
Published: June 2010

Most, if not all, galaxies with a significant bulge component harbor a central supermassive black hole. In our own Milky Way Galaxy, a disk of stars at a distance r ~ 0.05–1 pc orbits the radio source Sgr A* at the center. Stellar orbits show that the gravitational potential on a scale of ~ 0.5 pc is dominated by a concentrated mass of MBH ≈ 3.6 × 106M⊙, which is associated with a supermassive black hole. In addition to the black hole, the models require the presence of an extended mass of (0.5–1.5) × 106M⊙ in the central parsec, which can be explained well by the mass of the stars that make up the cluster. Thus, the Galactic center star cluster is composed of a central supermassive black hole and a self-gravitating disk that is several Gyrs old and comprised of late-type CO absorption stars. Significant disk rotation in the sense of the general Galactic rotation has been detected. This system is probably a strongly warped, thin single disk; the mean eccentricity of the observed stellar orbits in the disk is e ≈ 0.36 ± 0.06.
The Circumnuclear Spiral Pattern of NGC 5427
Authors: Hernandez-Jimenez J. A. , Dottori H. , Grosbøl P. , Vera-Villamizar N.
Published: June 2010

We have studied Hubble Space Telescope archive imagery of the central region of the Seyfert 2 galaxy NGC 5427. The images were taken with F606W (V-band) and F160W (H-band) filters with the Wide Field and Planetary Camera 2 and the Near Infrared Camera and Multi-Object Spectrometer, respectively.
Integral Field Spectroscopy of z ~ 0.1 QSO Host Galaxies
Authors: Nugroho Dading , Jahnke Knud , Husemann Bernd , Inskip Katherine , Sánchez Sebastian F. , Wisotzki Lutz
Published: June 2010

We observed a volume-limited sample of 19 luminous type 1 QSO host galaxies at MV ~ −23 mag and redshift 0.06 < z < 0.2 (Jahnke et al. 2004) using the VLT/VIMOS Integral Field Spectrograph. After removal of the QSO contribution (using the method of Husemann et al. 2008), we construct 2D intensity maps and gas velocity fields of the host galaxies in the Hα and [O iii] emission lines. Two representative cases are shown in Figure 1.
SMBH Luminosity in the Starburst Environment
Authors: Silich Sergiy , Tenorio-Tagle Guillermo , Hueyotl-Zahuantitla Filiberto , Palouš Jan , Wünsch Richard
Published: June 2010

We claim that in the starburst environment there is no accretion of the ISM onto the BH and thus, in such cases, the BH luminosity is regulated by the mass-loss rate from massive stars in the star forming region. We calculate the accretion rate and show that it is usually small during the superwind stage and grows at the post-starburst stage, when the matter reinserted by intermediate–mass stars remains gravitationally bound and fuels the central BH.
Radio-Mode Feedback in Massive Galaxies at Redshift 0 < z < 1
Authors: Sadler Elaine M. , Croom Scott M. , Ching John H. Y. , Johnston Helen M. , Cannon Russell D. , Mauch Tom
Published: June 2010

We have carried out a large observational study of the radio luminosities, stellar populations, and environments of massive galaxies over the redshift range 0 < z < 1. Radio jets powered by an accreting central black hole are common in massive galaxies, and there is a large class of “optically quiet AGN,” with radio emission but no optical/IR signature of black-hole accretion. The central black holes in these galaxies are probably accreting in a radiatively inefficient mode, and our results suggest that “radio-mode feedback” as described by Croton et al. is likely to occur in all masssive early-type galaxies at z < 0.8. While it appears that radio-loud AGN occur episodically in all massive early-type galaxies, we also identify a sub-population of galaxies with powerful radio sources and a prominent younger (~ 108 yr) stellar population that may have undergone recent mergers.
Multi-Zone Warm and Cold Clumpy Absorbers in Three Seyfert Galaxies
Authors: Ricci Claudio , Beckmann Volker , Audard Marc , Courvoisier T. J.-L.
Published: June 2010

A soft (E≲2 keV) excess over the power-law component dominant at higher energies has been found in the X-ray spectra of many Seyfert galaxies. The origin of the soft excess is still an open issue. In the past it was often associated with the high-energy tail of the thermal emission of the accretion disk, but it has been shown recently that the temperature of the disk should be constant (0.1–0.2 keV), regardless of the mass and luminosity of the AGN (Gierlinski & Done 2004). This result implies that some other mechanism is at work, as the temperature of the disk should depend on both the mass of the black hole and the accretion rate.
Direct Evidence for AGN-Driven Winds in a z = 1.5 Radio Galaxy
Authors: Steinbring Eric
Published: June 2010

Feedback from AGN is a key component in most current models of galaxy formation and evolution. For the most massive galaxies, heating and removal of gas by the AGN could precipitate an abrupt quenching of star formation during a dramatic blow-out phase. The “smoking gun” for such a scenario would be direct evidence of powerful outflows associated with the jet. I present some preliminary results of a program to look for these in high-z radio galaxies (HzRGs). Recent observations of the z = 1.5 radio galaxy 3C 230 obtained with the NIFS integral-field spectrograph and Altair laser adaptive optics facility on Gemini North are shown. These reveal with unprecedented resolution the complex kinematics of this system in redshifted Hα and [N ii] emission. The bi-polar velocity field is aligned with the jet axis, with a kinematic center associated with the radio core itself, and turbulent edges approaching the galaxy's escape velocity. This suggests a gas mass of roughly 1011M⊙ has been propagating outwards for 107 to 108 years, corresponding to a mass loss of roughly 102–3M⊙ yr−1, based on its velocity and spatial extent. This is in good agreement with the energetics and typical ages of radio jets, and likely heralds the onset of the “red and dead” stage for this HzRG.
Cold and Warm Gas Outflows in Radio AGN
Authors: Morganti Raffaella , Holt Joanna , Tadhunter Clive , Oosterloo Tom
Published: June 2010

The study of the conditions and the kinematics of the gas in the central region of AGN provides important information on the relevance of feedback effects connected to the nuclear activity. Quantifying these effects is key for constraining galaxy evolution models. Here we present a short summary of our recent efforts to study the occurrence and the impact of gas outflows in radio-loud AGN that are in their first phase of their evolution. Clear evidence for AGN-induced outflows has been found for the majority of these young radio sources. The outflows are detected both in (warm) ionized as well in (cold) atomic neutral gas, and they are likely to be driven (at least in most of the cases) by the interaction between the expanding jet and the medium. The mass outflow rates of the cold gas (Hi) appear to be systematically higher than those of the ionized gas. The former reach up to ~50 M⊙ yr−1 and are in the same range as “mild” starburst-driven superwinds in ULIRGs, whilst the latter are currently estimated to be a few solar masses per year. However, the kinetic powers associated with these gaseous outflows are a relatively small fraction (a few × 10−4) of the Eddington luminosity of the galaxy. Thus, they do not appear to match the requirements of the galaxy evolution feedback models.
FUV Emission in Cool-Core Clusters
Authors: Oonk J. B. R. , Jaffe W. , Bremer M. N. , Hatch N.
Published: June 2010

Far ultraviolet (FUV) emission is observed in the central regions of cool-core clusters with the Hubble Space Telescope (HST). It is traced out to 20 kpc from the nuclei of the brightest cluster galaxies and found to be distributed in clumps and filaments, as shown in Figure 1. The FUV emission matches the global structure of the ionized gas nebulae. If produced by stars, this emission can account for the ionization but not the temperature of the gas (Voit & Donahue 1997; Oonk et al. in preparation).
Relationship between ocean velocity and motionally induced electrical signals: 1. In the presence of horizontal velocity gradients
Authors: Szuts Zoltan B.
Published: June 2010

Motionally induced electric fields and electric currents in the ocean depend to first order solely on the vertical dimension. We investigate the significance of two‐dimensional (2‐D) perturbations that arise in the presence of horizontal velocity gradients. The full electric response is calculated for two schematic geometries that contain horizontal velocity gradients, have a two‐layer ocean with a layer of sediment beneath, and are described by four nondimensional parameters. When considered over the realistic ranges of oceanic aspect ratio (the ratio of water depth to the width of velocity), sediment thickness, and sediment conductivity, velocity errors arising from 2‐D perturbations are found to be less than a few percent of the dominant one‐dimensional (1‐D) signal. All errors depend on the aspect ratio to the power of 1.9 (1) for signals induced by the vertical (horizontal) component of the Earth's magnetic field. Depth‐uniform velocity errors are proportional to the 1‐D sediment conductance ratio, whereas depth‐varying velocity errors are independent of sediment thickness or conductivity. Errors are weakly (proportionally) dependent on the jet depth for signals induced by the vertical (horizontal) component of the magnetic field. Two‐dimensional perturbations decay away from the forcing region with a half width of 0.2–1 times the 1‐D effective water depth. This study extends the first‐order theory to the maximum expected aspect ratios for oceanic flow and finds small perturbations with simple dependencies on the nondimensional parameters.
Feasibility of soil moisture monitoring with heated fiber optics
Authors: Sayde Chadi , Gregory Christopher , Gil‐Rodriguez Maria , Tufillaro Nick , Tyler Scott , van de Giesen Nick , English Marshall , Cuenca Richard , Selker John S.
Published: June 2010

Accurate methods are needed to measure changing soil water content from meter to kilometer scales. Laboratory results demonstrate the feasibility of the heat pulse method implemented with fiber optic temperature sensing to obtain accurate distributed measurements of soil water content. A fiber optic cable with an electrically conductive armoring was buried in variably saturated sand and heated via electrical resistance to create thermal pulses monitored by observing the distributed Raman backscatter. A new and simple interpretation of heat data that takes advantage of the characteristics of fiber optic temperature measurements is presented. The accuracy of the soil water content measurements varied approximately linearly with water content. At volumetric moisture content of 0.05 m3/m3 the standard deviation of the readings was 0.001 m3/m3, and at 0.41 m3/m3 volumetric moisture content the standard deviation was 0.046 m3/m3. This uncertainty could be further reduced by averaging several heat pulse interrogations and through use of a higher‐performance fiber optic sensing system.
Insights into processes and deposits of hazardous vulcanian explosions at Soufrière Hills Volcano during 2008 and 2009 (Montserrat, West Indies)
Authors: Komorowski J.‐C. , Legendre Y. , Christopher T. , Bernstein M. , Stewart R. , Joseph E. , Fournier N. , Chardot L. , Finizola A. , Wadge G. , Syers R. , Williams C. , Bass V.
Published: June 2010

During the Soufrière Hills eruption, vulcanian explosions have generally occurred 1) in episodic cycles; 2) isolated during pauses in extrusion, and 3) after major collapses of the dome. In a different eruptive context, significant vulcanian explosions occurred on 29 July 2008, 3 December 2008, and 3 January 2009. Deposits are pumiceous except for the 3 December event. We reconstructed the dispersal pattern of the deposits and their textural characteristics to evaluate erupted volume and vesicularity of the magma at fragmentation. We discuss the implications of these explosions in terms of eruptive processes and chronology, and the hazards posed by their sudden and often unheralded occurrence. We suggest that overpressurization of the conduit can develop over time‐scales of months to weeks by a process of self‐sealing of conduit walls and/or the cooling dome by silica polymorphs. This work provides new insights for understanding the generation of hazardous vulcanian explosions at andesitic volcanoes.
SnowSlide: A simple routine for calculating gravitational snow transport
Authors: Bernhardt M. , Schulz K.
Published: June 2010

Knowledge about lateral snow transport processes is essential for the description of the spatial distribution of snow and therefore for the distribution of water on the lands surface. While numerous snow hydrological models are accounting for wind induced snow transport, they are mostly neglecting gravitational snow transport processes. This leads to unrealistic calculations of snow cover distributions in high Alpine regions effecting the subsequent prediction of individual components of the water and energy cycles at the land surface. “SnowSlide” as presented here is a fast and parsimonious model component allowing for the calculation of gravitational snow transport processes in an integral way. The functionality and performance of SnowSlide is demonstrated a) for artificial land surfaces and b) for two winter periods at the Watzmann massif in south‐east Germany. It is shown that the integration of SnowSlide into the snow‐hydrological model “SnowModel” is significantly improving the prediction of spatially distributed snow patterns in high Alpine areas and therefore generating more realistic descriptions of Alpine water and energy balances.
Analysis of Specific Heat Data in the Critical Region of Magnetic Solids
Authors: Cook F. J.
Published: June 2010

A detailed analysis of specific heat data in the critical region of magnetic solids is presented. An inverse power law, whose strength is measured by the exponent α, is used to describe the temperature dependence of the magnetic specific heat. Other parameters used include the power law coefficient A, the critical temperature Tc, and a constant background term B. Advanced techniques of data analysis suitable for estimation of nonlinear parameters and their errors under conditions of realistically weighted experimental data were used to obtain the dependence of α, Tc, A, and B on the range of data points included in the fit. Those exponents and parameters that provide the best overall fit to the data have been found. Literature references to 49 experiments from 1935 to 1971 are given. We present in tabular form the values of α, A, and B for 24 different magnetic crystals. With some exceptions, the best fits to the data suggest that in the temperature range studied the magnetic specific heat is not symmetric; the exponent α depends on the range of data included in the fit, varies widely from material to material, and in many cases is definitely negative below the critical temperature; and that there is little evidence that the asymptotic region is being adequately sampled by experiment. These results have the implication that until such time as we can adequately account for departures from the expected sharp peak in the data at Tc (data rounding) and corrections to asymptotic scaling, then comparisons between magnetic specific heat experiments and lowest order scaling predictions are to this date still tenuous.
Soft X-Ray Emission Spectra of Metallic Solids: Critical Review of Selected Systems
Authors: McAlister A. J. , Dobbyn R. C. , Cuthill J. R. , Williams M. L.
Published: June 2010

Theory and experimental practice in the field of soft x-ray emission from metallic solids are briefly reviewed, and measurements on a number of systems (Al, Al in AuAl2, Al and Mg in Al-Mg, Cu, Cu and Ni in Cu-Ni, Li, Mg, Na, and Ni) are critically evaluated and compared with the results of other techniques and theory, with a view to establishing the pertinence of the soft x-ray measurements and indicating specific guidelines for enhancing their value.
Elastic Properties of Metals and Alloys, I. Iron, Nickel, and Iron-Nickel Alloys
Authors: Ledbetter H. M. , Reed R. P.
Published: June 2010

A comprehensive compilation is given of elastic properties of iron-nickel alloys. When sufficient data exist, preferred values are recommended. This compilation covers, besides pure iron and pure nickel, the entire binary composition range, both b.c.c. and f.c.c. phases. Elastic constants included are: Young's modulus, shear modulus, bulk modulus (reciprocal compressibility), Poisson's ratio, and single-crystal elastic stiffnesses, both second-order and higher-order. Data are compiled for variation of elastic constants with composition, temperature, pressure, magnetic field, mechanical deformation, annealing, and crystallographic transitions. An overview is given from the vantage points of the electron theory of metals, elasticity theory, and crystallographic theory. Also included are discussions of iso-thermal and adiabatic elastic constants, interrelationships among engineering elastic constants, computation of the latter from single-crystal elastic stiffnesses, and similar topics. Where key data have not been measured, they were generated if possible from existing data using standard formulae. Other gaps, both theoretical and experimental, in the elastic properties of iron-nickel alloys are indicated. A few theoretical results are included where experimental data are nonexistent or scarce. A semantic scheme is proposed for distinguishing elastic constants of solids.
Microwave Spectra of Molecules of Astrophysical Interest V. Water Vapor
Authors: DeLucia Frank C. , Helminger Paul , Kirchhoff William H.
Published: June 2010

The available data on the microwave spectrum of water vapor are critically reviewed for information applicable to radio astronomy. Molecular data such as rotational constants, centrifugal distortion constants, hyperfine coupling parameters, and dipole moments are tabulated. A detailed centrifugal distortion calculation has been carried out for the most abundant isotopic form of this molecule H216O, as well as for H218O and HD16O. Transitions have been predicted and tabulated for the frequency range 1 MHz to 800 GHz. All predicted transitions include 95 percent confidence limits; estimated error limits have been reported for all measured transitions. Observed transitions of H217O are also listed.
A Critical Review of H-Atom Transfer in the Liquid Phase: Chlorine Atom, Alkyl, Trichloromethyl, Alkoxy, and Alkylperoxy Radicals
Authors: Hendry D. G. , Mill T. , Piszkiewicz L. , Howard J. A. , Eigenmann H. K.
Published: June 2010

This review covers hydrogen-atom transfer from carbon-hydrogen bonds in organic compounds to chlorine atom, methyl, ethyl, trichloromethyl, t-butoxy and alkylperoxy radicals in the liquid phase. Rate constant data are presented in 38 tables. Literature is covered through most of 1972. The review is divided into six sections; an introduction plus five sections each dealing with specific radicals. Hydrogen-atom transfer to chlorine atom are presented as relative rate constants. For hydrogen-atom transfer to methyl, ethyl, trichloromethyl, and t-butoxy radicals, both relative and absolute rate constants are tabulated. For alkylperoxy radicals only absolute rate constants are listed. Each absolute rate constant has a tabulated set of rate parameters where A has been assigned and E derived from the Arrhenius equation.
Molecular dynamics simulations of Cl+ etching on a Si(100) surface
Authors: Gou F. , Neyts E. , Eckert M. , Tinck S. , Bogaerts A.
Published: June 2010

Molecular dynamics simulations using improved Tersoff–Brenner potential parameters were performed to investigate Cl+ etching of a {2×1} reconstructed Si(100) surface. Steady-state Si etching accompanying the Cl coverage of the surface is observed. Furthermore, a steady-state chlorinated reaction layer is formed. The thickness of this reaction layer is found to increase with increasing energy. The stoichiometry of SiClx species in the reaction layer is found to be SiCl:SiCl2:SiCl3=1.0:0.14:0.008 at 50 eV. These results are in excellent agreement with available experimental data. While elemental Si products are created by physical sputtering, most SiClx (0<x<4) etch products are produced by chemical-enhanced physical sputtering.
Strain relaxation effect by nanotexturing InGaN/GaN multiple quantum well
Authors: Ramesh V. , Kikuchi A. , Kishino K. , Funato M. , Kawakami Y.
Published: June 2010

The relaxation of lattice-mismatched strain by deep postetching was systematically investigated for InGaN/GaN multiple quantum wells (MQWs). A planar heterojunction wafer, which included an In0.21Ga0.79N (3.2 nm)/GaN (14.8 nm) MQW, was etched by inductively coupled plasma dry etching, to fabricate high-density nanopillar, nanostripe, and nanohole arrays. The etching depth was 570 nm for all nanostructures. The diameter of the nanopillars was varied from 50 to 300 nm, then the mesa stripe width of the nanostripes and the diameter of the nanoholes were varied from 100 nm to 440 nm and 50 nm to 310 nm, respectively. The effect of strain relaxation on various optical properties was investigated. For example, in an array of nanopillars with diameter 130 nm and interval 250 nm, a large blueshift in the photoluminescence (PL) emission peak from 510 nm (as-grown) to 459 nm occurred at room temperature (RT). PL internal quantum efficiency (defined by the ratio of PL integral intensity at 300 K to that at 4.2 K) was enhanced from 34% (as-grown) to 60%, and the PL decay time at 4.2 K was reduced from 22 ns (as-grown) to 4.2 ns. These results clearly indicate the reduction of lattice-mismatched strain by postetching, which enhanced strain reduction with decreasing nanopillar diameter down to a diameter of 130 nm, where the strain reduction became saturated. The dependence of RT-PL decay time on nanopillar diameter was measured, and the surface nonradiative recombination velocity was estimated to be 5.8×102 cm/s. This relatively slow rate indicates a little etching damage.
Modeling of radiative properties of Sn plasmas for extreme-ultraviolet source
Authors: Sasaki Akira , Sunahara Atsushi , Furukawa Hiroyuki , Nishihara Katsunobu , Fujioka Shinsuke , Nishikawa Takeshi , Koike Fumihiro , Ohashi Hayato , Tanuma Hajime
Published: June 2010

Atomic processes in Sn plasmas are investigated for application to extreme-ultraviolet (EUV) light sources used in microlithography. We develop a full collisional radiative (CR) model of Sn plasmas based on calculated atomic data using Hebrew University Lawrence Livermore Atomic Code (HULLAC). Resonance and satellite lines from singly and multiply excited states of Sn ions, which contribute significantly to the EUV emission, are identified and included in the model through a systematic investigation of their effect on the emission spectra. The wavelengths of the 4d−4f+4p−4d transitions of Sn5+ to Sn13+ are investigated, because of their importance for determining the conversion efficiency of the EUV source, in conjunction with the effect of configuration interaction in the calculation of atomic structure. Calculated emission spectra are compared with those of charge exchange spectroscopy and of laser produced plasma EUV sources. The comparison is also carried out for the opacity of a radiatively heated Sn sample. A reasonable agreement is obtained between calculated and experimental EUV emission spectra observed under the typical condition of EUV sources with the ion density and ionization temperature of the plasma around 1018 cm−3 and 20 eV, respectively, by applying a wavelength correction to the resonance and satellite lines. Finally, the spectral emissivity and opacity of Sn plasmas are calculated as a function of electron temperature and ion density. The results are useful for radiation hydrodynamics simulations for the optimization of EUV sources.
Temperature-dependence of electrical and dielectric properties of papers for electrophotography
Authors: Maldzius R. , Sirviö P. , Sidaravicius J. , Lozovski T. , Backfolk K. , Rosenholm J. B.
Published: June 2010

The temperature-dependence of the electrical and dielectric properties of paper substrates was studied using experimental papers with different NaCl contents, different thicknesses, and different grammages. Physical processes related to the charging potential, charge decay rate, conductivity, dielectric constant, and dielectric loss of papers are dependent on thermal energy, and this dependence on temperature can be described by exponential expressions. The ion content of paper not only determines the level of these properties at a given temperature, as expected but also influences their temperature-dependence. Frequency analysis of the dielectric loss confirms that new structures are formed in paper by the addition of NaCl. The results may be applicable to the design of materials and equipment, e.g., for the electrophotographic printing processes.