STS 61-B crewmembers egress the Shuttle Atlantis after landing at Edwards

NASA Image and Video Library

1985-12-03

61B-S-071 (3 Dec 1985) --- George W.S. Abbey, director of flight crew operations at the Johnson Space Center (JSC), shakes hands with astronaut Brewster Shaw Jr., STS 61-B mission commander, as the seven-member crew descends the steps from its space-bound "home" for the last week. Following Shaw down the steps (bottom to top) were astronauts Bryan D. O'Connor, Sherwood C. Spring, Mary L. Cleave, Jerry L. Ross and Payload Specialists Charles D. Walker and Rodolfo Neri.

Stability of Tranexamic Acid after 12-Week Storage at Temperatures from -20 deg C to 50 deg C

DTIC Science & Technology

2013-07-01

PRELIMINARY REPORTS STABILITY OF TRANEXAMIC ACID AFTER 12-WEEK STORAGE AT TEMPERATURES FROM –20◦C TO 50◦C Rodolfo de Guzman, Jr., MT, I. Amy...Polykratis, BS, Jill L. Sondeen, PhD, Daniel N. Darlington, PhD, Andrew P. Cap, MD, PhD, Michael A. Dubick, PhD ABSTRACT Background. Tranexamic acid (TXA) is... tranexamic acid ; temperature stability; HPLC; thromboelastography; storage PREHOSPITAL EMERGENCY CARE 2013;17:394–400 BACKGROUND Hemorrhage is the leading

STS 61-B crew insignia

NASA Image and Video Library

2008-08-26

S85-36635 (October 1985) --- This is the insignia designed by the STS-61B crew members to represent their November 1985 mission aboard the space shuttle Atlantis, depicted here in Earth orbit, making only its second spaceflight. The design is surrounded by the surnames of the seven crew members. They are astronauts Brewster Shaw Jr., commander; Bryan D. O'Conner, pilot; Mary L. Cleave, Jerry L. Ross and Sherwood C. Spring, all mission specialists; and payload specialists Charles D. Walker, representing McDonnell Douglas, and Rodolfo Neri, representing Morelos of Mexico (note flag). The NASA insignia design for space shuttle flights is reserved for use by the astronauts and for other official use as the NASA Administrator may authorize. Public availability has been approved only in the forms of illustrations by the various news media. When and if there is any change in this policy, which is not anticipated, the change will be publicly announced. Photo credit: NASA

[La combinazione di gemcitabina e oxaliplatino (GEMOX) nel trattamento del carcinoma pancreatico in fase avanzata di malattia: le notizie sulla mia morte sono state esagerate?

PubMed

Giuliani, Jacopo; Bonetti, Andrea

2017-12-01

Riassunto. L'analisi è stata condotta al fine di valutare l'effetto sia sulla sopravvivenza globale (OS) sia sulla sopravvivenza libera da progressione di malattia (PFS) della chemioterapia di combinazione in prima linea per il carcinoma pancreatico in fase avanzata di malattia. La presente analisi è limitata agli studi randomizzati controllati (RCT) di fase III. Successivamente è stata applicata la European Society for Medical Oncology Magnitude of Clinical Benefit Scale (ESMO-MCBS) agli RCT di fase III analizzati per ricavare uno score relativo all'entità del beneficio clinico ottenuto per ciascun RCT. Sono state calcolate inoltre le differenze in termini di PFS tra i diversi bracci di trattamento rapportandole con i costi dei farmaci necessari per ottenere il beneficio di PFS. La nostra analisi ha valutato 11 RCT di fase III, per un totale di 4572 pazienti. Combinando i costi della terapia con la misura dell'efficacia espressa dalla PFS, è stato ottenuto un costo di 74,12 euro (€) per mese di vita guadagnato in termini di PFS con la combinazione di 5-fluorouracil, leucovorin, irinotecan e oxaliplatino (FOLFIRINOX), 90,14 € per la combinazione di gemcitabina e oxaliplatino (GEMOX) e 4708,7 € per la combinazione di nab-paclitaxel e gemcitabina. Da questo punto di vista riteniamo che l'utilizzo delle "vecche chemioterapie di combinazione" (per es., GEMOX) non dovrebbe essere completamente abbandonato, ma valutato sul singolo paziente, sulla base di diversi fattori (età, ECOG PS, comorbilità, carico di malattia), al fine di ottenere una reale "tailored therapy".

STS 61-B crewmembers training on the KC-135 in zero-G

NASA Image and Video Library

1985-08-21

STS 61-B crewmembers training on the KC-135 in zero-G. Views include Payload specialist Charles D. Walker attempting to down the lower torso of his extravehicular mobility unit (EMU) in zero-G in the KC-135. He is being assisted by other participants in the training (39135); Payload specialist Rodolfo Neri floating in midair during training in the KC-135 (39136,39138); Mission specialist Mary L. Cleave floating in midair during her training aboard the KC-135 (39137); Astronaut Bryan D. O'Connor assists Astronaut Sherwood C. Spring in completing his donning of the EMU in the KC-135 (39139); Technicians aid Spring with his EMU in the KC-135 (39140); O'Connor appears to be leaping up in zero-G aboard the KC-135 (39141); Astronaut Brewster Shaw is assisted by a technician to don his EMU (39142); Shaw is attempting to don the EMU gloves while O'Connor watches (39143); Shaw does jumping jacks while Neri attempts to travel down a rope guideline (39144).

The Experiments on Electrical Anesthesia in Italy in the Second Half of the Nineteenth Century. A Dispute Between a Fearless Surgeon Patriot and a Positivist Researcher.

PubMed

Cascella, Marco

2015-10-01

Electric anesthesia is the anesthesia, usually general anesthesia, produced by the application of an electrical current. This fascinating issue of the anesthesia history was made possible thanks to the pioneering experiments on electrotherapy and electrophysiology performed by two researchers: the neurologist Guillaume Duchenne (1806-1875) and the biologist Stéphane Leduc (1853-1939). The aim of this study is the review of the dispute between two Italian scientists on the effectiveness of electric anesthesia in the second half of the 19th century. One of the two contenders was Rodolfo Rodolfi (1827-1896), an Italian surgeon and patriot who took part in the First Italian War of Independence of 1848, whereas the other protagonist of the dispute was the positivist Plinio Schivardi (1833-1908), a pupil of Duchenne who brought to Italy his knowledge of electrotherapy, collecting these experiences in the Theoretical Practical Manual of Electrotherapy, the first book on the subject written in Italian. Copyright © 2015 Elsevier B.V. All rights reserved.

Short-wavelength free-electron laser sources and science: a review

NASA Astrophysics Data System (ADS)

Seddon, E. A.; Clarke, J. A.; Dunning, D. J.; Masciovecchio, C.; Milne, C. J.; Parmigiani, F.; Rugg, D.; Spence, J. C. H.; Thompson, N. R.; Ueda, K.; Vinko, S. M.; Wark, J. S.; Wurth, W.

2017-11-01

This review is focused on free-electron lasers (FELs) in the hard to soft x-ray regime. The aim is to provide newcomers to the area with insights into: the basic physics of FELs, the qualities of the radiation they produce, the challenges of transmitting that radiation to end users and the diversity of current scientific applications. Initial consideration is given to FEL theory in order to provide the foundation for discussion of FEL output properties and the technical challenges of short-wavelength FELs. This is followed by an overview of existing x-ray FEL facilities, future facilities and FEL frontiers. To provide a context for information in the above sections, a detailed comparison of the photon pulse characteristics of FEL sources with those of other sources of high brightness x-rays is made. A brief summary of FEL beamline design and photon diagnostics then precedes an overview of FEL scientific applications. Recent highlights are covered in sections on structural biology, atomic and molecular physics, photochemistry, non-linear spectroscopy, shock physics, solid density plasmas. A short industrial perspective is also included to emphasise potential in this area. Dedicated to John M J Madey (1943-2016) and Rodolfo Bonifacio (1940-2016) whose perception, drive and perseverance paved the way for the realisation and development of short-wavelength free-electron lasers.

[Clinical features and outcome of community-acquired methicillin-resistant Staphylococcus aureus pneumonia].

PubMed

Obed, Mora; García-Vidal, Carolina; Pessacq, Pedro; Mykietiuk, Analia; Viasus, Diego; Cazzola, Laura; Domínguez, M Angeles; Calmaggi, Anibal; Carratalà, Jordi

2014-01-01

The aim of this study is to describe the epidemiological and clinical features, treatment and prognosis of community-acquired pneumonia (CAP) caused by methicillin-resistant Staphylococcus aureus (MRSA) in two different geographic regions where community-acquired MRSA (CA-MRSA) infections have different frequencies. Observational study of patients admitted to two hospitals (one in Argentina, the other in Spain) between March 2008 and June 2012. We documented 16 cases of CAP caused by MRSA. MRSA accounted for 15 of 547 (2.7%) cases of CAP in Hospital Rodolfo Rossi and 1 of 1258 (0,08%) cases at the Hospital Universitari de Bellvitge (P ≤ .001). Most patients were young and previously healthy. Multilobar infiltrates, cavitation and skin and soft tissue involvement were frequent. All patients had positive blood cultures. Five patients required admission to the intensive care unit. Early mortality (≤ 48 hours) was 19%, and overall mortality (≤ 30 days) was 25%. CAP caused by MRSA causes high morbidity and mortality rates. It should be suspected in areas with a high prevalence of CA-MRSA infections, and especially in young and healthy patients who present with multilobar pneumonia with cavitation. Mortality is mainly related to septic shock and respiratory failure and occurs early in most cases. Copyright © 2012 Elsevier España, S.L. All rights reserved.

Comparative randomized study on the efficaciousness of treatment of BOO due to BPH in patients with prostate up to 100 gr by endoscopic gyrus prostate resection versus open prostatectomy. Preliminary data.

PubMed

Giulianelli, Roberto; Brunori, Stefano; Gentile, Barbara Cristina; Vincenti, Giorgio; Nardoni, Stefano; Pisanti, Francesco; Shestani, Teuta; Mavilla, Luca; Albanesi, Luca; Attisani, Francesco; Mirabile, Gabriella; Schettini, Manlio

2011-06-01

With the advent of medical management and minimally techniques for benign prostate hypeplasia (BPH), invasive surgical procedures such open prostatectomy (OPSU) have become less common, although selected patients may still benefit from open prostatectomy. Aim of this study was to evaluate efficacy and safety of Bipolar TURP (Gyrus electro surgical system) versus standard open prostatectomy in patients with lower urinary tract symptoms (LUTS) due to bladder outlet obstruction (BOO) with markedly enlarged glands refractory to medical therapy. From January 2003 to January 2004, 140 patients affected by mild-severe LUTS, secondary to BOO from BPH, refractory to medical therapy, with markedly enlarged glands, were randomized in two groups (1:1), and subjected to open prostatectomy (OPSU) carried out with traditional method (Bracci Thechnique) versus transurethral resection of the prostate (TURP) utilizing the bipolar methodology. Preoperative work-up included IPSS, IIEF-5 and Qol questionnaires. All patients were submitted to uroflowmetry, transrectal ultrasound (TRUS), measurament of postvoidal residual urine and PSA determination. IPSS, IIEF-5 and Qol, uroflowmetry, TRUS, measurement of post-voidal residual urine, PSA determination and number of reoperations were evaluated at 1, 3, 6, 12, 18, 24, 30 and 36 months. Operative time, resected tissue weight and perioperative complications were also registered. Total post-operative catheter time, total postoperative hospital stay, haemoglobin loss were recorded in the 2 groups. Comparative data on IPSS symptom score, IIEF-5 and Qol, PSA, peak urinary flow rates and post-void residual urine volume in the 2 groups were similar but showed a significative improvement with respect to baseline value. Postoperative haemoglobin levels, postoperative catheterization, hospital stay and 3-yr overall surgical re-treatment-free rate were significantly better in the Bipolar group. In the treatment of LUTS due to bladder outlet obstruction (BOO) with markedly enlarged glands refractory to medical therapy, Bipolar TURP has a comparable outcome to open prostatectomy at short and medium term according to both subjective and objective outcome measures.

A GRAND VIEW OF THE BIRTH OF 'HEFTY' STARS - 30 DORADUS NEBULA MONTAGE

NASA Technical Reports Server (NTRS)

2002-01-01

This picture, taken in visible light with the Hubble Space Telescope's Wide Field and Planetary Camera 2 (WFPC2), represents a sweeping view of the 30 Doradus Nebula. But Hubble's infrared camera - the Near Infrared Camera and Multi-Object Spectrometer (NICMOS) - has probed deeper into smaller regions of this nebula to unveil the stormy birth of massive stars. The montages of images in the upper left and upper right represent this deeper view. Each square in the montages is 15.5 light-years (19 arcseconds) across. The brilliant cluster R136, containing dozens of very massive stars, is at the center of this image. The infrared and visible-light views reveal several dust pillars that point toward R136, some with bright stars at their tips. One of them, at left in the visible-light image, resembles a fist with an extended index finger pointing directly at R136. The energetic radiation and high-speed material emitted by the massive stars in R136 are responsible for shaping the pillars and causing the heads of some of them to collapse, forming new stars. The infrared montage at upper left is enlarged in an accompanying image. Credits for NICMOS montages: NASA/Nolan Walborn (Space Telescope Science Institute, Baltimore, Md.) and Rodolfo Barba' (La Plata Observatory, La Plata, Argentina) Credits for WFPC2 image: NASA/John Trauger (Jet Propulsion Laboratory, Pasadena, Calif.) and James Westphal (California Institute of Technology, Pasadena, Calif.)

Occupation and Risk of Non-Hodgkin Lymphoma and Its Subtypes: A Pooled Analysis from the InterLymph Consortium

PubMed Central

‘t Mannetje, Andrea; De Roos, Anneclaire J.; Boffetta, Paolo; Vermeulen, Roel; Benke, Geza; Fritschi, Lin; Brennan, Paul; Foretova, Lenka; Maynadié, Marc; Becker, Nikolaus; Nieters, Alexandra; Staines, Anthony; Campagna, Marcello; Chiu, Brian; Clavel, Jacqueline; de Sanjose, Silvia; Hartge, Patricia; Holly, Elizabeth A.; Bracci, Paige; Linet, Martha S.; Monnereau, Alain; Orsi, Laurent; Purdue, Mark P.; Rothman, Nathaniel; Lan, Qing; Kane, Eleanor; Costantini, Adele Seniori; Miligi, Lucia; Spinelli, John J.; Zheng, Tongzhang; Cocco, Pierluigi; Kricker, Anne

2015-01-01

Background: Various occupations have been associated with an elevated risk of non-Hodgkin lymphoma (NHL), but results have been inconsistent across studies. Objectives: We investigated occupational risk of NHL and of four common NHL subtypes with particular focus on occupations of a priori interest. Methods: We conducted a pooled analysis of 10,046 cases and 12,025 controls from 10 NHL studies participating in the InterLymph Consortium. We harmonized the occupational coding using the 1968 International Standard Classification of Occupations (ISCO-1968) and grouped occupations previously associated with NHL into 25 a priori groups. Odds ratios (ORs) adjusted for center, age, and sex were determined for NHL overall and for the following four subtypes: diffuse large B-cell lymphoma (DLBCL), follicular lymphoma (FL), chronic lymphocytic leukemia/small lymphocytic lymphoma (CLL/SLL), and peripheral T-cell lymphoma (PTCL). Results: We confirmed previously reported positive associations between NHL and farming occupations [field crop/vegetable farm workers OR = 1.26; 95% confidence interval (CI): 1.05, 1.51; general farm workers OR = 1.19; 95% CI: 1.03, 1.37]; we also confirmed associations of NHL with specific occupations such as women’s hairdressers (OR = 1.34; 95% CI: 1.02, 1.74), charworkers/cleaners (OR = 1.17; 95% CI: 1.01, 1.36), spray-painters (OR = 2.07; 95% CI: 1.30, 3.29), electrical wiremen (OR = 1.24; 95% CI: 1.00, 1.54), and carpenters (OR = 1.42; 95% CI: 1.04, 1.93). We observed subtype-specific associations for DLBCL and CLL/SLL in women’s hairdressers and for DLBCL and PTCL in textile workers. Conclusions: Our pooled analysis of 10 international studies adds to evidence suggesting that farming, hairdressing, and textile industry–related exposures may contribute to NHL risk. Associations with women’s hairdresser and textile occupations may be specific for certain NHL subtypes. Citation: ‘t Mannetje A, De Roos AJ, Boffetta P, Vermeulen R, Benke G, Fritschi L, Brennan P, Foretova L, Maynadié M, Becker N, Nieters A, Staines A, Campagna M, Chiu B, Clavel J, de Sanjose S, Hartge P, Holly EA, Bracci P, Linet MS, Monnereau A, Orsi L, Purdue MP, Rothman N, Lan Q, Kane E, Seniori Costantini A, Miligi L, Spinelli JJ, Zheng T, Cocco P, Kricker A. 2016. Occupation and risk of non-Hodgkin lymphoma and its subtypes: a pooled analysis from the InterLymph Consortium. Environ Health Perspect 124:396–405; http://dx.doi.org/10.1289/ehp.1409294 PMID:26340796

Bicarbonate Values for Healthy Residents Living in Cities Above 1500 Meters of Altitude: A Theoretical Model and Systematic Review.

PubMed

Ramirez-Sandoval, Juan C; Castilla-Peón, Maria F; Gotés-Palazuelos, José; Vázquez-García, Juan C; Wagner, Michael P; Merelo-Arias, Carlos A; Vega-Vega, Olynka; Rincón-Pedrero, Rodolfo; Correa-Rotter, Ricardo

2016-06-01

Ramirez-Sandoval, Juan C., Maria F. Castilla-Peón, José Gotés-Palazuelos, Juan C. Vázquez-García, Michael P. Wagner, Carlos A. Merelo-Arias, Olynka Vega-Vega, Rodolfo Rincón-Pedrero, and Ricardo Correa-Rotter. Bicarbonate values for healthy residents living in cities above 1500 m of altitude: a theoretical model and systematic review. High Alt Med Biol. 17:85-92, 2016.-Plasma bicarbonate (HCO3(-)) concentration is the main value used to assess the metabolic component of the acid-base status. There is limited information regarding plasma HCO3(-) values adjusted for altitude for people living in cities at high altitude defined as 1500 m (4921 ft) or more above sea level. Our aim was to estimate the plasma HCO3(-) concentration in residents of cities at these altitudes using a theoretical model and compare these values with HCO3(-) values found on a systematic review, and with those venous CO2 values obtained in a sample of 633 healthy individuals living at an altitude of 2240 m (7350 ft). We calculated the PCO2 using linear regression models and calculated plasma HCO3(-) according to the Henderson-Hasselbalch equation. Results show that HCO3(-) concentration falls as the altitude of the cities increase. For each 1000 m of altitude above sea level, HCO3(-) decreases to 0.55 and 1.5 mEq/L in subjects living at sea level with acute exposure to altitude and in subjects acclimatized to altitude, respectively. Estimated HCO3(-) values from the theoretical model were not different to HCO3(-) values found in publications of a systematic review or with venous total CO2 measurements in our sample. Altitude has to be taken into consideration in the calculation of HCO3(-) concentrations in cities above 1500 m to avoid an overdiagnosis of acid-base disorders in a given individual.

Otto LaPorte Lecture: Ultimate Rayleigh-Bénard and Taylor-Couette turbulence

NASA Astrophysics Data System (ADS)

Lohse, Detlef

2017-11-01

Rayleigh-Bénard flow - the flow in a box heated from below and cooled from above - and Taylor-Couette flow - the flow between two coaxial co- or counter-rotating cylinders - are the two paradigmatic systems in physics of fluids and many new concepts have been tested with them. They are mathematically well defined, namely by the Navier-Stokes equations and the respective boundary conditions, and share many features. While the low Reynolds number regime (i.e., weakly driven systems) has been very well explored in the '80s and '90s of the last century, in the fully turbulent regime major research activity only developed in the last two decades. In this talk we will first briefly review this recent progress in our understanding of fully developed Rayleigh-Bénard (RB) and Taylor-Couette (TC) turbulence, from the experimental, theoretical, and numerical point of view. We will explain the parameter dependences of the global transport properties of the flow and the local flow organisation, including velocity profiles and boundary layers, which are closely connected to the global properties. Next, we will discuss transitions between different (turbulent) flow states. We will in particular focus on the so-called ultimate regime, in which the boundary layer has become turbulent, and which therefore has enhanced transport properties. In the mechanical driven TC flow this ultimate regime can also be achieved in our high-performance numerical simulations, showing excellent agreement with our experiments on the Twente Turbulent Taylor-Couette (T3 C) facility. In the last part of the talk we will discuss RB and TC turbulence with rough walls. There the results can be expressed in terms of the skin-friction factor, revealing analogy to turbulent flow in rough pipes. Finally, we will present our results on RB and TC flow with bubbles, focusing on bubbly drag reduction and its origin. This is joint work with many colleagues over the years, and I in particular would like to name Chao Sun, Roberto Verzicco, Siegfried Grossmann, Richard Stevens, Erwin van der Poel, Rodolfo Ostilla-Monico, Xiaojue Zhu, Dennis van Gils, Sander Huisman, Ruben Verschoof, and Gert-Wim Bruggert.

BOOK REVIEW: A First Course in Loop Quantum Gravity A First Course in Loop Quantum Gravity

NASA Astrophysics Data System (ADS)

Dittrich, Bianca

2012-12-01

Students who are interested in quantum gravity usually face the difficulty of working through a large amount of prerequisite material before being able to deal with actual quantum gravity. A First Course in Loop Quantum Gravity by Rodolfo Gambini and Jorge Pullin, aimed at undergraduate students, marvellously succeeds in starting from the basics of special relativity and covering basic topics in Hamiltonian dynamics, Yang Mills theory, general relativity and quantum field theory, ending with a tour on current (loop) quantum gravity research. This is all done in a short 173 pages! As such the authors cannot cover any of the subjects in depth and indeed this book should be seen more as a motivation and orientation guide so that students can go on to follow the hints for further reading. Also, as there are many subjects to cover beforehand, slightly more than half of the book is concerned with more general subjects (special and general relativity, Hamiltonian dynamics, constrained systems, quantization) before the starting point for loop quantum gravity, the Ashtekar variables, are introduced. The approach taken by the authors is heuristic and uses simplifying examples in many places. However they take care in motivating all the main steps and succeed in presenting the material pedagogically. Problem sets are provided throughout and references for further reading are given. Despite the shortness of space, alternative viewpoints are mentioned and the reader is also referred to experimental results and bounds. In the second half of the book the reader gets a ride through loop quantum gravity; the material covers geometric operators and their spectra, the Hamiltonian constraints, loop quantum cosmology and, more broadly, black hole thermodynamics. A glimpse of recent developments and open problems is given, for instance a discussion on experimental predictions, where the authors carefully point out the very preliminary nature of the results. The authors close with an 'open issues and controversies' section, addressing some of the criticism of loop quantum gravity and pointing to weak points of the theory. Again, readers aiming at starting research in loop quantum gravity should take this as a guide and motivation for further study, as many technicalities are naturally left out. In summary this book fully reaches the aim set by the authors - to introduce the topic in a way that is widely accessible to undergraduates - and as such is highly recommended.

A GRAND VIEW OF THE BIRTH OF 'HEFTY' STARS - 30 DORADUS NEBULA DETAILS

NASA Technical Reports Server (NTRS)

2002-01-01

These are two views of a highly active region of star birth located northeast of the central cluster, R136, in 30 Doradus. The orientation and scale are identical for both views. The top panel is a composite of images in two colors taken with the Hubble Space Telescope's visible-light camera, the Wide Field and Planetary Camera 2 (WFPC2). The bottom panel is a composite of pictures taken through three infrared filters with Hubble's Near Infrared Camera and Multi-Object Spectrometer (NICMOS). In both cases the colors of the displays were chosen to correlate with the nebula's and stars' true colors. Seven very young objects are identified with numbered arrows in the infrared image. Number 1 is a newborn, compact cluster dominated by a triple system of 'hefty' stars. It has formed within the head of a massive dust pillar pointing toward R136. The energetic outflows from R136 have shaped the pillar and triggered the collapse of clouds within its summit to form the new stars. The radiation and outflows from these new stars have in turn blown off the top of the pillar, so they can be seen in the visible-light as well as the infrared image. Numbers 2 and 3 also pinpoint newborn stars or stellar systems inside an adjacent, bright-rimmed pillar, likewise oriented toward R136. These objects are still immersed within their natal dust and can be seen only as very faint, red points in the visible-light image. They are, however, among the brightest objects in the infrared image, since dust does not block infrared light as much as visible light. Thus, numbers 2 and 3 and number 1 correspond respectively to two successive stages in the birth of massive stars. Number 4 is a very red star that has just formed within one of several very compact dust clouds nearby. Number 5 is another very young triple-star system with a surrounding cluster of fainter stars. They also can be seen in the visible-light picture. Most remarkable are the glowing patches numbered 6 and 7, which astronomers have interpreted as 'impact points' produced by twin jets of material slamming into surrounding dust clouds. These 'impact points' are perfectly aligned on opposite sides of number 5 (the triple-star system), and each is separated from the star system by about 5 light-years. The jets probably originate from a circumstellar disk around one of the young stars in number 5. They may be rotating counterclockwise, thus producing moving, luminous patches on the surrounding dust, like a searchlight creating spots on clouds. These infrared patches produced by jets from a massive, young star are a new astronomical phenomenon. Credits for NICMOS image: NASA/Nolan Walborn (Space Telescope Science Institute, Baltimore, Md.) and Rodolfo Barba' (La Plata Observatory, La Plata, Argentina) Credits for WFPC2 image: NASA/John Trauger (Jet Propulsion Laboratory, Pasadena, Calif.) and James Westphal (California Institute of Technology, Pasadena, Calif.)

PREFACE: XV Chilean Physics Symposium, 2006

NASA Astrophysics Data System (ADS)

Soto, Leopoldo; Moreno, José; Ávila, Ricardo; Cubillos, Karla

2008-02-01

The Chilean Physics Symposium is the main gathering of Physics in Chile, and its organization is one of the central activities of the Chilean Physical Society (Sociedad Chilena de Física, SOCHIFI). The Symposium assembles the largest number of Chilean and foreign physicists resident in the country. Recent advances in the various research areas in Physics are presented, by researchers from Universities and national research centres. At the same time this is an occasion for the participation of Physics students from both the pre- and post-graduate programs. The Symposium has gathered continuously every two years, since 1978. The organization of the XV symposium was in charge of the Thermonuclear Plasma Department of the Chilean Nuclear Energy Commission, and it took place on 15-17 November 2006, at La Reina Nuclear Studies Centre, in the city of Santiago, Chile. During this symposium the relation of research in Physics with education and with the productive sector in the country was also analysed. During the Symposium, 121 abstracts were submitted, from 255 authors. All authors were invited to submit articles for publication in the Symposium Proceedings. The articles received were reviewed by the Symposium Scientific Committee and by invited peers. The criteria for review focussed on the demand for a consistent piece of research, and a clear statement of results. Most of the articles received report the work of research groups where advanced students and young investigators are prominent. Thanks to their enthusiasm, 52 articles are presented in this issue. We would like to express our appreciation to their authors. Finally, my personal apology is in order regarding my delay in publishing these proceedings. A sequence of personal and professional highly demanding circumstances have been in the way. I would like to thank Journal of Physics: Conference Series for providing very fast publication of the proceedings, having published them online less than 4 weeks after my initial contact with the journal. Leopoldo Soto President, Chilean Physical Society Head of Plasma Department, Chilean Nuclear Energy Commission Editors: Leopoldo Soto, José Moreno, Ricardo Ávila, Karla Cubillos Scientific Committee Physicists from various research institutions, specialty areas, and regions of the country were invited by the Board of SOCHIFI to join the Symposium Scientific Committee, which was formed by: Julio Yánez, Universidad de Antofagasta Sergio del Campo, Pontificia Universidad Católica de Valparaíso Patricio Vargas, Universidad Técnica Federico Santa María Rodrigo Soto, Universidad de Chile Ulrich Volkmann, Pontificia Universidad Católica de Chile Víctor Muñoz, Universidad de Chile Rodrigo Aros, Universidad Andrés Bello Leopoldo Soto (Chairman), Comisión Chilena de Energía Nuclear Luis Huerta, Universidad de Talca Patricio Salgado, Universidad de Concepción Luis Roa, Universidad de Concepción Asticio Vargas, Universidad de la Frontera, Temuco Cristian Martínez, Centro de Estudios Científicos, Valdivia Organizing Commitee Leopoldo Soto (Chairman), Comisión Chilena de Energía Nuclear Erik Herrera, Comisión Chilena de Energía Nuclear José Moreno, Comisión Chilena de Energía Nuclear Andrea Rozas, Comisión Chilena de Energía Nuclear Rodrigo Aros, Universidad Andrés Bello Gonzalo Gutiérrez, Universidad de Chile Executive Board, Chilean Physical Society April 2006 - April 2008 Leopoldo Soto, President Joel Saavedra, Secretary Rodrigo Aros: Treasurer Rodolfo Figueroa: Director Luis Huerta: Director Conference photograph

Evolution of volcanically-induced palaeoenvironmental changes leading to the onset of OAE1a (early Aptian, Cretaceous)

NASA Astrophysics Data System (ADS)

Keller, Christina E.; Hochuli, Peter A.; Giorgioni, Martino; Garcia, Therese I.; Bernasconi, Stefano M.; Weissert, Helmut

2010-05-01

During the Cretaceous, several major volcanic events occurred that initiated climate warming, altered marine circulation and increased marine productivity, which in turn often resulted in the widespread black shale deposits of the Oceanic Anoxic Events (OAE). In the sediments underlying the early Aptian OAE1a black shales, a prominent negative carbon isotope excursion is recorded. Its origin had long been controversial (e.g. Arthur, 2000; Jahren et al., 2001) before recent studies attributed it to the Ontong Java volcanism (Méhay et al., 2009; Tejada et al., 2009). Therefore the negative C-isotope excursion covers the interval between the time, when volcanic activity became important enough to be recorded in the C-isotope composition of the oceans to the onset of widespread anoxic conditions (OAE1a). We chose this interval at the locality of Pusiano (N-Italy) to study the effect of a volcanically-induced increase in pCO2 on the marine palaeoenvironment and to observe the evolving palaeoenvironmental conditions that finally led to OAE1a. The Pusiano section (Maiolica Formation) was deposited at the southern continental margin of the alpine Tethys Ocean and has been bio- and magnetostratigraphically dated by Channell et al. (1995). We selected 18 samples from 12 black shale horizons for palynofacies analyses. Palynofacies assemblages consist of several types of particulate organic matter, providing information on the origin of the organic matter (terrestrial/marine) and conditions during deposition (oxic/anoxic). We then linked the palynofacies results to high-resolution inorganic and organic C-isotope values and total organic carbon content measurements. The pelagic Pusiano section consists of repeated limestone-black shale couplets, which are interpreted to be the result of changes in oxygenation of bottom waters. Towards the end of the negative C-isotope excursion we observe enhanced preservation of the fragile amorphous organic matter resulting in increased total organic carbon values in the black shale as well as in the limestone intervals. This shows how a rising pCO2 triggered changes in climate and oceanography and resulted in an increasing oxygen-deficiency of the bottom waters that persisted even during the 'limestone intervals' before oxygen-depletion finally became a global phenomenon. References: Arthur, M.A., 2000, Volcanic contributions to the carbon and sulfur geochemical cycles and global change, in Sigurdsson, H., Houghton, B., McNutt, S.R., Rymer, H., and Stix, J., eds., Encyclopedia of Volcanoes, Academic Press, p. 1045-1056. Channell, J.E.T., Cecca, F., and Erba, E., 1995, Correlations of Hauterivian and Barremian (Early Cretaceous) stage boundaries to polarity chrons: Earth and Planetary Science Letters, v. 134, p. 125-140. Jahren, A.H., Arens, N.C., Sarmiento, G., Guerrero, J., and Amundson, R., 2001, Terrestrial record of methane hydrate dissociation in the Early Cretaceous: Geology, v. 29, p. 159-162. Méhay, S., Keller, C.E., Bernasconi, S.M., Weissert, H., Erba, E., Bottini, C., and Hochuli, P.A., 2009, A volcanic CO2 pulse triggered the Cretaceous Oceanic Anoxic Event 1a and a biocalcification crisis: Geology, v. 37, p. 819-822. Tejada, M.L.G., Suzuki, K., Junichiro, K., Rodolfo, C., J., M.J., Naohiko, O., Tatsuhiko, S., and Yoshiyuki, T., 2009, Ontong Java Plateau eruption as a trigger for the early Aptian oceanic anoxic event: Geology, v. 37, p. 855-858.

Astronomical tuning of black cherts in the Cenomanian Scaglia Bianca as precursors of the Bonarelli level (OAE2) at Furlo, Italy

NASA Astrophysics Data System (ADS)

Batenburg, S. J.; Montanari, A.; Sprovieri, M.; Hilgen, F. J.; Coccioni, R.; Gale, A. S.

2012-04-01

Astronomical tuning of the Cenomanian Oceanic Anoxic Event (OAE2) critically depends on the phase relationship between eccentricity forcing and ocean-climate response. The mechanisms leading to oceanic anoxia are heavily debated, and both maxima and minima in eccentricity have been suggested to trigger the widespread deposition of organic-rich sediments. At the Furlo section in the north-eastern Apennines of Italy, the rhythmically bedded Scaglia Bianca formation forms a cyclic prologue to the Bonarelli level, the Tethyan sedimentary expression of OAE2. Regularly occurring black cherts are precursors of the extreme conditions leading to the oceanic anoxic event, and show the hierarchical stacking pattern of eccentricity modulated precession. Previous orbital tuning attempts have placed the occurrence of black cherts either in eccentricity maxima (Mitchell et al. 2008) or eccentricity minima (Lanci et al. 2010). These scenarios require distinctly different oceanographic regimes. Eccentricity maxima enhance the seasonal contrast, thereby intensifying monsoons, leading to an estuarine circulation in the Cretaceous North Atlantic with upwelling and increased productivity (Mitchell et al. 2008), potentially spurred by input of nutrients from volcanic activity (Trabucho Alexandre et al. 2010). Alternatively, it has been suggested that eccentricity minima could cause decreased seasonality, leading to stagnation and reduced ventilation of bottom waters (Lanci et al. 2010; Herbert and Fischer 1986), although eccentricity minima would not lower seasonality but rather avoid large seasonal extremes for a prolonged period of time. Lanci et al. (2010) attempted to establish this phase relation by measurements of CaCO3 content in carbonates, but failed to incorporate the cherts, which reflect a much larger variability in carbonate content. New high-resolution lithological, geophysical and stable isotope data from the Furlo section unequivocally indicate that the timing of black chert deposition, as well as the onset of the oceanic anoxic event itself, is related to eccentricity maxima. The stable 405-kyr periodicity of eccentricity is readily discernible in the data records and can be used for tuning to the astronomical solution (Laskar et al. 2011). A total of five and a half 405-kyr cycles can be identified below the Bonarelli level, which itself comprises a 405-kyr cycle. This cyclostratigraphy can potentially be anchored to the absolute time scale by using the newly determined Cenomanian-Turonian boundary age of 93.9 ± 0.15 Ma, which is based on intercalibration of astrochronological and radioisotopic data for the Cenomanian-Turonian boundary interval near the GSSP in Colorado, USA (Meyers et al., 2012). Correlation to the orbitally tuned Turonian interval of the nearby Gubbio and Contessa sections in Italy (De Vleeschouwer et al., this session) allows the construction of an anchored astronomical time scale for the Cenomanian-Turonian interval of > 5 Ma. Herbert, T. D., and A. G. Fischer. 1986. "Milankovitch climatic origin of mid-Cretaceous black shale rhythms in central Italy." Nature 321 (19): 739-743. Lanci, L., G. Muttoni, and E. Erba. 2010. "Astronomical tuning of the Cenomanian Scaglia Bianca Formation at Furlo, Italy." Earth and Planetary Science Letters. Laskar, J., A. Fienga, M. Gastineau, and H. Manche. 2011. "La2010: A new orbital solution for the long term motion of the Earth." Astronomy and Astrophysics arXiv:1103.1084v1. Mitchell, Ross N., David M. Bice, Alessandro Montanari, Laura C. Cleaveland, Keith T. Christianson, Rodolfo Coccioni, and Linda A. Hinnov. 2008. "Oceanic anoxic cycles? Orbital prelude to the Bonarelli Level (OAE 2)." Earth and Planetary Science Letters 267: 1-16. Trabucho Alexandre, J., E. Tuenter, G. A Henstra, K. J van der Zwan, R. S.W van de Wal, H. A Dijkstra, and P. L de Boer. 2010. "The mid-Cretaceous North Atlantic nutrient trap: Black shales and OAEs." Paleoceanography 25 (4).

Gluon polarization in the proton: Constraints at low x from the measurement of the double longitudinal spin asymmetry for forward-rapidity hadrons with the PHENIX detector at RHIC

NASA Astrophysics Data System (ADS)

McKinney, Cameron Palmer

In the 1980s, polarized deep inelastic lepton-nucleon scattering experiments revealed that only about a third of the proton's spin of ½ h is carried by the quarks and antiquarks, leaving physicists with the puzzle of how to account for the remaining spin. As gluons carry roughly 50% of the proton's momentum, it seemed most logical to look to the gluon spin as another significant contributor. However, lepton-nucleon scattering experiments only access the gluon helicity distribution, Delta g, through effects on the quark distributions via scaling violations. Constraining Deltag through scaling violations requires experiments that together cover a large range of Q 2. Such experiments had been carried out with unpolarized beams, leaving g(x) (the unpolarized gluon distribution) relatively well-known, but the polarized experiments have only thus far provided weak constraints on Deltag in a limited momentum fraction range. With the commissioning in 2000 of the Relativistic Heavy Ion Collider, the first polarized proton-proton (pp) collider, and the first polarized pp running in 2002, the gluon distributions could be accessed directly by studying quark-gluon and gluon-gluon interactions. In 2009, data from measurements of double longitudinal spin asymmetries, ALL, at the STAR and PHENIX experiments through 2006 were included in a QCD global analysis performed by Daniel de Florian, Rodolfo Sassot, Marco Stratmann, and Werner Vogelsang (DSSV), yielding the first direct constraints on the gluon helicity. The DSSV group found that the contribution of the gluon spin to the proton spin was consistent with zero, but the data provided by PHENIX and STAR was all at mid-rapidity, meaning Delta g was constrained by data only a range in x from 0.05 to 0.2, leaving out helicity contributions from the huge number of low- x gluons. A more recent analysis by DSSV from 2014 including RHIC data through 2009 for the first time points to significant gluon polarization at intermediate momentum fractions, meaning gluon polarization measurements may be more interesting than anticipated, especially at momentum fractions where no constraints exist as of yet. A forward detector upgrade in PHENIX, the Muon Piston Calorimeter (MPC), was designed with the purpose of extending the sensitivity to Delta g to lower x. Monte Carlo simulations indicate that measurements of hadrons in the MPC's pseudorapidity of range 3.1 < eta <3.9 probe asymmetric collisions between high-x quarks and low-x gluons, with the x of the gluons reaching below 0.01 at a collision energy √s = 500 GeV. We access Deltag through measurements of ALL for electromagnetic clusters in the MPC; this thesis details the measurement from the Run 11 (2011) data set at √ s = 500GeV. We find ALL≈ 0, but the statistical uncertainties from this measurement mean we likely cannot resolve the small expected asymmetries. However, improved techniques for determining the relative luminosity between bunch crossings with different helicity configurations will allow data from a much larger data set in Run 13 to be most impactful in constraining Deltag, whereas previous measurements of ALL have had difficulties limiting the systematic uncertainty from relative luminosity. In this thesis, we begin by presenting an overview of the physics motivation for this experiment. Then, we discuss the experimental apparatus at RHIC and PHENIX, with a focus on those systems integral to our analysis. The analysis sections of the thesis cover calibration of the Muon Piston Calorimeter, a careful examination of the relative luminosity systematic uncertainty, and the process of obtaining a final physics result.

Ontong Java volcanism initiated long-term climate warming that caused substantial changes in terrestrial vegetation several tens of thousand years before the onset of OAE1a (Early Aptian, Cretaceous)

NASA Astrophysics Data System (ADS)

Keller, Christina E.; Hochuli, Peter A.; Giorgioni, Martino; Garcia, Therese I.; Bernasconi, Stefano M.; Weissert, Helmut

2010-05-01

During Cretaceous times, several intense volcanic episodes are proposed as trigger for episodic climate warming, for changes in marine circulation patterns and for elevated marine productivity, which resulted in the widespread black shale deposits of the Oceanic Anoxic Events (OAE). In the sediments underlying the early Aptian OAE1a black shales, a prominent negative carbon isotope excursion is recorded. Its origin had long been controversial (e.g. Arthur, 2000; Jahren et al., 2001) before recent studies attributed it to the Ontong Java volcanism (Méhay et al., 2009; Tejada et al., 2009). Volcanic outgassing results in an increased pCO2 and should lead to a rise in global temperatures. We therefore investigated if the volcanically-induced increase in pCO2 at the onset of OAE1a in the early Aptian led to a temperature rise that was sufficient to affect terrestrial vegetation assemblages. In order to analyse changes in terrestrial palynomorph assemblages, we examined 15 samples from 12 black shale horizons throughout the early Aptian negative C-isotope spike interval of the Pusiano section (Maiolica Formation; N-Italy). These sediments were deposited at the southern continental margin of the alpine Tethys Ocean and have been bio- and magnetostratigraphically dated by Channell et al. (1995). In order to obtain a continuous palynological record of the negative C-isotope spike interval and the base of OAE1a, we combined this pre-OAE1a interval of Pusiano with the OAE1a interval of the nearby Cismon section (Hochuli et al., 1999). The sporomorph assemblages at the base of this composite succession feature abundant bisaccate pollen, which reflects a warm-temperate climate. Rather arid conditions are inferred from low trilete spore percentages. Several tens of thousand years before the onset of OAE1a, C-isotope values started to decrease. Some thousand years later, bisaccate pollen began to decrease, whereas an increase of Classopollis spp. and Araucariacites spp. percentages indicate a rise in temperatures. Maximum temperatures (suggested by a dominance of Classopollis spp.) were only reached after the most negative inorganic C-isotope values and after the onset of OAE1a. Our study shows that the volcanically-induced increase in pCO2, which ultimately led to OAE1a caused a substantial climate warming that seriously affected terrestrial vegetation. References: Arthur, M.A., 2000, Volcanic contributions to the carbon and sulfur geochemical cycles and global change, in Sigurdsson, H., Houghton, B., McNutt, S.R., Rymer, H., and Stix, J., eds., Encyclopedia of Volcanoes, Academic Press, p. 1045-1056. Channell, J.E.T., Cecca, F., and Erba, E., 1995, Correlations of Hauterivian and Barremian (Early Cretaceous) stage boundaries to polarity chrons: Earth and Planetary Science Letters, v. 134, p. 125-140. Hochuli, P.A., Menegatti, A.P., Weissert, H., Riva, A., Erba, E., and Silva, I.P., 1999, Episodes of high productivity and cooling in the early Aptian Alpine Tethys: Geology, v. 27, p. 657-660. Jahren, A.H., Arens, N.C., Sarmiento, G., Guerrero, J., and Amundson, R., 2001, Terrestrial record of methane hydrate dissociation in the Early Cretaceous: Geology, v. 29, p. 159-162. Méhay, S., Keller, C.E., Bernasconi, S.M., Weissert, H., Erba, E., Bottini, C., and Hochuli, P.A., 2009, A volcanic CO2 pulse triggered the Cretaceous Oceanic Anoxic Event 1a and a biocalcification crisis: Geology, v. 37, p. 819-822. Tejada, M.L.G., Suzuki, K., Junichiro, K., Rodolfo, C., J., M.J., Naohiko, O., Tatsuhiko, S., and Yoshiyuki, T., 2009, Ontong Java Plateau eruption as a trigger for the early Aptian oceanic anoxic event: Geology, v. 37, p. 855-858.

Sr/Ca ratios in cold-water corals - a 'low-resolution' temperature archive?

NASA Astrophysics Data System (ADS)

Rüggeberg, Andres; Riethdorf, Jan-Rainer; Raddatz, Jacek; López Correa, Matthias; Montagna, Paolo; Dullo, Wolf-Christian; Freiwald, André

2010-05-01

One of the basic data to understand global change and past global changes is the measurement and the reconstruction of temperature of marine water masses. E.g. seawater temperature controls the density of seawater and in combination with salinity is the major driving force for the oceans circulation system. Geochemical investigations on cold-water corals Lophelia pertusa and Desmophyllum cristagalli indicated the potential of these organisms as high-resolution archives of environmental parameters from intermediate and deeper water masses (Adkins and Boyle 1997). Some studies tried to use cold-water corals as a high-resolution archive of temperature and salinity (Smith et al. 2000, 2002; Blamart et al. 2005; Lutringer et al. 2005). However, the fractionation of stable isotopes (delta18O and delta13C) and element ratios (Sr/Ca, Mg/Ca, U/Ca) are strongly influenced by vital effects (Shirai et al. 2005; Cohen et al. 2006), and difficult to interpret. Nevertheless, ongoing studies indicate the potential of a predominant temperature dependent fractionation of distinct isotopes and elements (e.g. Li/Ca, Montagna et al. 2008; U/Ca, Mg/Ca, delta18O, Lòpez Correa et al. 2008; delta88/86Sr, Rüggeberg et al. 2008). Within the frame of DFG-Project TRISTAN and Paläo-TRISTAN (Du 129/37-2 and 37-3) we investigated live-collected specimens of cold-water coral L. pertusa from all along the European continental margin (Northern and mid Norwegian shelves, Skagerrak, Rockall and Porcupine Bank, Galicia Bank, Gulf of Cadiz, Mediterranean Sea). These coral samples grew in waters characterized by temperatures between 6°C and 14°C. Electron Microprobe investigations along the growth direction of individual coral polyps were applied to determine the relationship between the incorporation of distinct elements (Sr, Ca, Mg, S). Cohen et al. (2006) showed for L. pertusa from the Kosterfjord, Skagerrak, that ~25% of the coral's Sr/Ca ratio is related to temperature, while 75% are influenced by the calcification rate of the organism. However, the Sr/Ca-temperature relation of our L. pertusa specimens suggest, that mean values are more reliable for temperature reconstruction along a larger temperature range than local high-resolution investigations. Additionally, our results plot on same line of Sr/Ca-temperature relationship like tropical corals indicating a similar behaviour of element incorporation during calcification. References: Adkins JF, Boyle EA (1997) Changing atmospheric ∆14C and the record of deep water paleoventilation ages. Paleoceanography 12:337-344 Blamart D, Rollion-Bard C, Cuif J-P, Juillet-Leclerc A, Lutringer A, Weering Tv, Henriet J-P (2005) C and O isotopes in a deep-sea coral (Lophelia pertusa) related to skeletal microstructure. In: Freiwald A, Roberts JM (eds) Cold-water Corals and Ecosystems. Springer-Verlag, Berlin Heidelberg, p 1005-1020 Cohen AL, Gaetani GA, Lundälv T, Corliss BH, George RY (2006) Compositional variability in a cold-water scleractinian, Lophelia pertusa: New insights into vital effects. Geochemistry, Geophysics, Geosystems 7:Q12004, doi:12010.11029/12006GC001354 López Correa M, Montagna P, Rüggeberg A, McCulloch M, Taviani M, Freiwald A (2008) Trace elements and stable isotopes in recent North Atlantic Lophelia pertusa along a latitudal gradient and from fossil Mediterranean sites. ASLO 2008 Summer Meeting, St. John's, Newfoundland & Labrador, Canada, 08.06.-13.06.2008, p. 47 Lutringer A, Blamart D, Frank N, Labeyrie L (2005) Paleotemperatures from deep-sea corals: scale effects. In: Freiwald A, Roberts JM (eds) Cold-water Corals and Ecosystems. Springer-Verlag, Berlin, Heidelberg, p 1081-1096 Montagna P, López-Correa M, Rüggeberg A, McCulloch M, Rodolfo-Metalpa R, Dullo W-C, Ferrier-Pagès C, Freiwald A, Henderson G, Mazzoli C, Russo S, Silenzi S, Taviani M (2008) Coral Li/Ca in micro-structural domains as a temperature proxy. Goldschmidt Conference, Vancouver, British Columbia, Canada Rüggeberg A, Fietzke J, Liebetrau V, Eisenhauer A, Dullo W-C, Freiwald A (2008) Stable strontium isotopes (delta88/86Sr) in cold-water corals — A new proxy for reconstruction of intermediate ocean water temperatures. Earth and Planetary Science Letters 269:569-574 Shirai K, Kusakabe M, Nakai S, Ishii T, Watanabe T, Hiyagon H, Sano Y (2005) Deep-sea coral geochemistry: Implication for the vital effect. Chemical Geology 224:212-222 Smith JE, Schwarcz HP, Risk MJ (2002) Patterns of isotopic disequilibria in azooxanhtellate coral skeletons. Hydrobiologia 471:111-115 Smith JE, Schwarcz HP, Risk MJ, McConnaughey TA, Keller N (2000) Paleotemperatures from deep-sea corals: Overcoming 'vital effects'. Palaios 15:25-32

From surfaces to magnetic properties: special section dedicated to Juan Rojo

NASA Astrophysics Data System (ADS)

Mascaraque, A.; Rodríguez de la Fuente, O.; González-Barrio, Miguel A.

2013-12-01

Surface physics and magnetism, in particular the connection between surface defects, reduced dimensionality or size, crystal structure, electronic density of states and the mechanical and magnetic properties of solids, were always at the core of Juan Rojo's scientific interest and output. Both fields seem to meet at the nanoscale, a privileged playing field which is ideal for testing theoretical concepts, exploring new physics or probing a wealth of new, stunning and unheard-of applications. Upon reducing size or dimensionality, either in bulk systems or in thin films, surfaces and surface effects are telling. Thus, for instance, an ultra-thin coating can make nanoparticles of non-magnetic materials exhibit magnetic behaviour; or atomic steps can modify the local mechanical properties of a metallic single crystal. In this special section there are eight invited papers by disciples and close collaborators of Juan Rojo, that cover an ample spectrum of the above mentioned topics. The first paper, by Palacio et al, investigates the temperature and oxygen partial pressure conditions for FeO mono- and bi-layer growth on Ru(0001). The following paper, by Cortés-Gil et al, reports on the dramatic change in the electric resistivity of the manganite perovskite (La0.5Ca0.5)z MnO3 as a function of Ca content, an effect related to the removal of a charge-ordered state and a magnetic transition. Baeza et al study biomaterials for bone cancer treatment and skeletal reinforcing, as well as targeted magnetic nanoparticles used for intracell hyperthermia in cancer therapies. In the following paper, Marcano et al, assisted by a multi-technique approach, revisit the extraordinarily rich magnetic phase diagram of the Kondo system CeNi1- x Cux down to 100 mK temperatures. The magnetic field dependence of the martensitic transition temperature of the meta-magnetic shape memory alloy Ni50Mn34.5In15.5 in a crystalline and amorphous phase, in fields up to 13 T, is the subject of the paper by Barandiarán et al. In the following paper, Crespo et al review the effect of organic and inorganic coatings on magnetic nanoparticles, showing that the coating can tune the magnetic properties of metallic and oxide nano-sized particles. Barja et al report on ordered magnetic ion structures formed by evaporation of Mn and Fe on self-assembled layers of tetracyanoquinodimethane (TCNQ) molecules on Cu(111). Finally, Rodríguez de la Fuente et al investigate the role of surface defects on the physico-chemical properties of metals and oxides in a variety of scenarios, showing how the surface controls the mechanical properties probed at the nanoscale or the chemical reactivity. Acknowledgments The editors are grateful to all the invited contributors to this special section of Journal of Physics: Condensed Matter . We also thank the staff of IOP Publishing for handling the administrative matters and the refereeing process, and for their patience and helpful disposition. From surfaces to magnetic properties contents From surfaces to magnetic properties: special section dedicated to Juan RojoA Mascaraque, O Rodríguez de la Fuente and Miguel A González-Barrio Juan Rojo: the surface science and science politics maker in SpainA Mascaraque, O Rodríguez de la Fuente, Miguel A González-Barrio, Javier Solana, Luis Oro and Ana Crespo Initial stages of FeO growth on Ru(0001)I Palacio, M Monti, J F Marco, K F McCarty and J de la Figuera Surprising resistivity decrease in manganites with constant electronic densityR Cortés-Gil, M L Ruiz-González, J M Alonso, J L Martínez, A Hernando, M Vallet-Regí, and J M González-Calbet Thermoseeds for interstitial magnetic hyperthermia: from bioceramics to nanoparticlesA Baeza, D Arcos and M Vallet-Regí Revisited magnetic phase diagram for CeNi1-xCux system: spin-glass in the weak interaction limitN Marcano, J I Espeso and J C Gómez Sal Magnetic field and atomic order effect on the martensitic transformation of a metamagnetic alloyJ M Barandiaran, V A Chernenko, E Cesari, D Salas, J Gutierrez and P Lazpita Magnetism in nanoparticles: tuning properties with coatingsPatricia Crespo, Patricia de la Presa, Pilar Marín, Marta Multigner, José María Alonso, Guillermo Rivero, Félix Yndurain, José María González-Calbet and Antonio Hernando Ordered arrays of metal-organic magnets at surfacesSara Barja, Daniel Stradi, Bogdana Borca, Manuela Garnica, Cristina Díaz, Josefa M Rodriguez-García, Manuel Alcamí, Amadeo L Vázquez de Parga, Fernando Martín and Rodolfo Miranda Surface defects and their influence on surface propertiesO Rodríguez de la Fuente, M A González-Barrio, V Navarro, B M Pabón, I Palacio and A Mascaraque

KANTBP 2.0: New version of a program for computing energy levels, reaction matrix and radial wave functions in the coupled-channel hyperspherical adiabatic approach

NASA Astrophysics Data System (ADS)

Chuluunbaatar, O.; Gusev, A. A.; Vinitsky, S. I.; Abrashkevich, A. G.

2008-11-01

A FORTRAN 77 program for calculating energy values, reaction matrix and corresponding radial wave functions in a coupled-channel approximation of the hyperspherical adiabatic approach is presented. In this approach, a multi-dimensional Schrödinger equation is reduced to a system of the coupled second-order ordinary differential equations on a finite interval with homogeneous boundary conditions: (i) the Dirichlet, Neumann and third type at the left and right boundary points for continuous spectrum problem, (ii) the Dirichlet and Neumann type conditions at left boundary point and Dirichlet, Neumann and third type at the right boundary point for the discrete spectrum problem. The resulting system of radial equations containing the potential matrix elements and first-derivative coupling terms is solved using high-order accuracy approximations of the finite element method. As a test desk, the program is applied to the calculation of the reaction matrix and radial wave functions for 3D-model of a hydrogen-like atom in a homogeneous magnetic field. This version extends the previous version 1.0 of the KANTBP program [O. Chuluunbaatar, A.A. Gusev, A.G. Abrashkevich, A. Amaya-Tapia, M.S. Kaschiev, S.Y. Larsen, S.I. Vinitsky, Comput. Phys. Commun. 177 (2007) 649-675]. Program summaryProgram title: KANTBP Catalogue identifier: ADZH_v2_0 Program summary URL:http://cpc.cs.qub.ac.uk/summaries/ADZH_v2_0.html Program obtainable from: CPC Program Library, Queen's University, Belfast, N. Ireland Licensing provisions: Standard CPC licence, http://cpc.cs.qub.ac.uk/licence/licence.html No. of lines in distributed program, including test data, etc.: 20 403 No. of bytes in distributed program, including test data, etc.: 147 563 Distribution format: tar.gz Programming language: FORTRAN 77 Computer: Intel Xeon EM64T, Alpha 21264A, AMD Athlon MP, Pentium IV Xeon, Opteron 248, Intel Pentium IV Operating system: OC Linux, Unix AIX 5.3, SunOS 5.8, Solaris, Windows XP RAM: This depends on the number of differential equations; the number and order of finite elements; the number of hyperradial points; and the number of eigensolutions required. The test run requires 2 MB Classification: 2.1, 2.4 External routines: GAULEG and GAUSSJ [2] Nature of problem: In the hyperspherical adiabatic approach [3-5], a multidimensional Schrödinger equation for a two-electron system [6] or a hydrogen atom in magnetic field [7-9] is reduced by separating radial coordinate ρ from the angular variables to a system of the second-order ordinary differential equations containing the potential matrix elements and first-derivative coupling terms. The purpose of this paper is to present the finite element method procedure based on the use of high-order accuracy approximations for calculating approximate eigensolutions of the continuum spectrum for such systems of coupled differential equations on finite intervals of the radial variable ρ∈[ρ,ρ]. This approach can be used in the calculations of effects of electron screening on low-energy fusion cross sections [10-12]. Solution method: The boundary problems for the coupled second-order differential equations are solved by the finite element method using high-order accuracy approximations [13]. The generalized algebraic eigenvalue problem AF=EBF with respect to pair unknowns ( E,F) arising after the replacement of the differential problem by the finite-element approximation is solved by the subspace iteration method using the SSPACE program [14]. The generalized algebraic eigenvalue problem (A-EB)F=λDF with respect to pair unknowns ( λ,F) arising after the corresponding replacement of the scattering boundary problem in open channels at fixed energy value, E, is solved by the LDL factorization of symmetric matrix and back-substitution methods using the DECOMP and REDBAK programs, respectively [14]. As a test desk, the program is applied to the calculation of the reaction matrix and corresponding radial wave functions for 3D-model of a hydrogen-like atom in a homogeneous magnetic field described in [9] on finite intervals of the radial variable ρ∈[ρ,ρ]. For this benchmark model the required analytical expressions for asymptotics of the potential matrix elements and first-derivative coupling terms, and also asymptotics of radial solutions of the boundary problems for coupled differential equations have been produced with help of a MAPLE computer algebra system. Restrictions: The computer memory requirements depend on: the number of differential equations; the number and order of finite elements; the total number of hyperradial points; and the number of eigensolutions required. Restrictions due to dimension sizes may be easily alleviated by altering PARAMETER statements (see Section 3 and [1] for details). The user must also supply subroutine POTCAL for evaluating potential matrix elements. The user should also supply subroutines ASYMEV (when solving the eigenvalue problem) or ASYMS0 and ASYMSC (when solving the scattering problem) which evaluate asymptotics of the radial wave functions at left and right boundary points in case of a boundary condition of the third type for the above problems. Running time: The running time depends critically upon: the number of differential equations; the number and order of finite elements; the total number of hyperradial points on interval [ ρ,ρ]; and the number of eigensolutions required. The test run which accompanies this paper took 2 s without calculation of matrix potentials on the Intel Pentium IV 2.4 GHz. References: [1] O. Chuluunbaatar, A.A. Gusev, A.G. Abrashkevich, A. Amaya-Tapia, M.S. Kaschiev, S.Y. Larsen, S.I. Vinitsky, Comput. Phys. Commun. 177 (2007) 649-675; http://cpc.cs.qub.ac.uk/summaries/ADZHv10.html. [2] W.H. Press, S.A. Teukolsky, W.T. Vetterling, B.P. Flannery, Numerical Recipes: The Art of Scientific Computing, Cambridge University Press, Cambridge, 1986. [3] J. Macek, J. Phys. B 1 (1968) 831-843. [4] U. Fano, Rep. Progr. Phys. 46 (1983) 97-165. [5] C.D. Lin, Adv. Atom. Mol. Phys. 22 (1986) 77-142. [6] A.G. Abrashkevich, D.G. Abrashkevich, M. Shapiro, Comput. Phys. Commun. 90 (1995) 311-339. [7] M.G. Dimova, M.S. Kaschiev, S.I. Vinitsky, J. Phys. B 38 (2005) 2337-2352. [8] O. Chuluunbaatar, A.A. Gusev, V.L. Derbov, M.S. Kaschiev, L.A. Melnikov, V.V. Serov, S.I. Vinitsky, J. Phys. A 40 (2007) 11485-11524. [9] O. Chuluunbaatar, A.A. Gusev, V.P. Gerdt, V.A. Rostovtsev, S.I. Vinitsky, A.G. Abrashkevich, M.S. Kaschiev, V.V. Serov, Comput. Phys. Commun. 178 (2007) 301 330; http://cpc.cs.qub.ac.uk/summaries/AEAAv10.html. [10] H.J. Assenbaum, K. Langanke, C. Rolfs, Z. Phys. A 327 (1987) 461-468. [11] V. Melezhik, Nucl. Phys. A 550 (1992) 223-234. [12] L. Bracci, G. Fiorentini, V.S. Melezhik, G. Mezzorani, P. Pasini, Phys. Lett. A 153 (1991) 456-460. [13] A.G. Abrashkevich, D.G. Abrashkevich, M.S. Kaschiev, I.V. Puzynin, Comput. Phys. Commun. 85 (1995) 40-64. [14] K.J. Bathe, Finite Element Procedures in Engineering Analysis, Englewood Cliffs, Prentice-Hall, New York, 1982.

Cannibal Stars Cause Giant Explosions in Fornax Cluster Galaxy

NASA Astrophysics Data System (ADS)

2000-07-01

The VLT Observes Most Remote Novae Ever Seen About 70 million years ago, when dinosaurs were still walking on the Earth, a series of violent thermo-nuclear explosions took place in a distant galaxy. After a very long travel across vast reaches of virtually empty space (70 million light-years, or ~ 7 x 10 20 km), dim light carrying the message about these events has finally reached us. It was recorded by the ESO Very Large Telescope (VLT) at the Paranal Observatory (Chile) during an observing programme by a group of Italian astronomers [1]. The subsequent analysis has shown that the observers witnessed the most distant nova outbursts ever seen . They were caused by "stellar cannibalism" in binary systems in which one relatively cool star loses matter to its smaller and hotter companion. An instability results that leads to the ignition of a "hydrogen bomb" on the surface of the receiving star. The "Stella Nova" Phenomenon A stellar outburst of the type now observed with the VLT is referred to as a "Stella Nova" ("new star" in Latin), or just "Nova" . Novae caused by explosions in binary stars in our home galaxy, the Milky Way system, are relatively frequent and about every second or third year one of them is bright enough to be easily visible with the naked eye. For our ancestors, who had no means to see the faint binary star before the explosion, it looked as if a new star had been born in the sky, hence the name. The most common nova explosion occurs in a binary stellar system in which a white dwarf (a very dense and hot, compact star with a mass comparable to that of the Sun and a size like the Earth) accretes hydrogen from a cooler and larger red dwarf star [2]. As the hydrogen collects on the surface of the white dwarf star, it becomes progressively hotter until a thermonuclear explosion is ignited at the bottom of the collected gas. A huge amount of energy is released and causes a million-fold increase in the brightness of the binary system within a few hours. After reaching maximum light within some days or weeks, it begins to fade as the hydrogen supply is exhausted and blown into space. The processed material is ejected at high speeds, up to ~1000 km/sec, and may later be visible as an expanding shell of emitting gas. Altogether, the tremendous flash of light involves the release of about 10 45 ergs in a few weeks, or about as much energy as our Sun produces in 10,000 years. Supernovae explosions that completely destroy heavier stars at the end of their lives are even more powerful. However, in contrast to supernovae and despite the colossal energy production, the progenitor of a nova is not destroyed during the explosion. Some time after an outburst, transfer of hydrogen from the companion star begins anew, and the process repeats itself with explosions taking place about once every 100,000 years. The nova star will finally die of "old age" when the cool companion has been completely cannibalized. Novae as Distance Indicators Due to their exceptional luminosity, novae can be used as powerful beacons that allow relative distances to different types of galaxies to be measured. The measurement is based on the assumption that novae of the same type are intrinsically equally bright, together with the physical law that states that an object's observed brightness decreases with the square of the distance to the observer. Thus, if we observe that a nova in a certain galaxy is one million times fainter than a nearby one, we know that it must be one thousand times more distant. In addition, observations of novae in other galaxies shed light on the history of formation of their stars. Despite their scientific importance, surveys of novae in distant, rich clusters of galaxies have not been very popular among astronomers. Major reasons are probably the inherent observational difficulties and the comparatively low rates of discovery. In the past, with 4-m class telescopes, tens of hours of monitoring of several galaxies have indeed been necessary to detect a few distant novae [3]. VLT observations of NGC 1316 in the Fornax Cluster ESO PR Photo 18a/00 ESO PR Photo 18a/00 [Preview - JPEG: 400 x 448 pix - 28k] [Normal - JPEG: 800 x 895 pix - 136k] [Full-Res - JPEG: 1941 x 2172 pix - 904k] Caption : Colour composite photo of the central area of NGC 1316 , a giant elliptical galaxy in the Fornax cluster of galaxies. Many dark dust clouds and lanes are visible. Some of the star-like objects in the field are globular clusters of stars that belong to the galaxy. It is based on CCD exposures, obtained with the 8.2-m VLT/ANTU telescope and the FORS-1 multi-mode instrument through B (blue), V (green-yellow) and I (here rendered as red) filters, respectively. The "pyramids" above and below the bright centre of the galaxy and the vertical lines at some of the brighter stars are caused by overexposure ("CCD bleeding"). The field measures 6.8 x 6.8 arcmin 2 , with 0.2 arcsec/pixel. The image quality of this composite is about 0.9 arcsec. North is up and East is left. NGC 1316 is a giant "dusty" galaxy ( PR Photo 18a/00 ), located in the Fornax cluster seen in the southern constellation of that name ("The Oven"). This galaxy is of special interest in connection with current attempts to establish an accurate distance scale in the Universe. In 1980 and 1981, NGC 1316 was the host of two supernovae of type Ia , a class of object that is widely used as a "cosmological standard candle" to determine the distance to very distant galaxies, cf. ESO PR 21/98. A precise measurement of the distance to NGC 1316 may therefore provide an independent calibration of the intrinsic brightness of these supernovae. The new observations were performed during 8 nights distributed over the period from January 9 to 19, 2000. They were made in service mode at the 8.2-m VLT/ANTU telescope with the FORS-1 multi-mode instrument, using a 2k x 2k CCD camera with 0.2 arcsec pixels and a field of 6.8 x 6.8 arcmin 2. The exposures lasted 20 min and were carried out with three optical filters (B, V and I). The most distant Novae observed so far ESO PR Photo 18b/00 ESO PR Photo 18b/00 [Preview - JPEG: 400 x 452 pix - 83k] [Normal - JPEG: 800 x 904 pix - 224k] ESO PR Photo 18c/00 ESO PR Photo 18c/00 [Preview - JPEG: 400 x 458 pix - 54k] [Normal - JPEG: 800 x 916 pix - 272k] Caption : Images of two of the novae in NGC 1316 that were discovered during the observational programme described in this Press Release. Both composites show the blue images (B-filter) obtained on January 9 (upper left), 12 (upper right), 15 (lower left) and 19 (lower right), 2000, respectively. The decline of the brightness of the objects is obvious. An analysis of the images that were obtained in blue light (B-filter) resulted in the detection of four novae. They were identified because of the typical change of brightness over the observation period, cf. PR Photos 18b-c/00 , as well as their measured colours. Although the time-consuming reduction of the data and the subsequent astrophysical interpretation is still in progress, the astronomers are already now very satisfied with the outcome. In particular, no less than four novae were detected in a single giant galaxy within only 11 days . This implies a rate of approximately 100 novae/year in NGC 1316, or about 3 times larger than the rate estimated for the Milky Way galaxy. This may (at least partly) be due to the fact that NGC 1316 is of a different type and contains more stars than our own galaxy. The novae in NGC 1316 are quite faint, of about magnitude 24 and decreasing towards 25-26 during the period of observation. This corresponds to nearly 100 million times fainter than what can be seen with the naked eye. The corresponding distance to NGC 1316 is found to be about 70 million light-years . Moreover, the discovery of four novae in one galaxy in the Fornax cluster was possible with only 3 hours of observing time per filter. This clearly shows that the new generation of 8-m class telescopes like the VLT, equipped with the new and large detectors, is able to greatly improve the efficiency of this type of astronomical investigations (by a factor of 10 or more) , as compared to previous searches with 4-m telescopes. The road is now open for exhaustive searches for novae in remote galaxies, with all the resulting benefits, also for the accurate determination of the extragalactic distance scale. Notes [1]: The group consists of Massimo Della Valle (Osservatorio Astrofisico di Arcetri, Firenze, Italy), Roberto Gilmozzi and Rodolfo Viezzer (both ESO). [2]: A graphical illustration of the nova phenomenon can be found at this website. [3]: For example, in 1987, Canadian astronomers Christopher Pritchet and Sidney van den Bergh , in an heroic tour de force with the 4-m Canada-France-Hawaii telescope, found 9 novae after 56 hours of monitoring of 3 giant elliptical galaxies in the Virgo cluster of galaxies.

First Results from the UT1 Science Verification Programme

NASA Astrophysics Data System (ADS)

1998-11-01

Performance verification is a step which has regularly been employed in space missions to assess and qualify the scientific capabilities of an instrument. Within this framework, it was the goal of the Science Verification program to submit the VLT Unit Telescope No. 1 (UT1) to the scrutiny that can only be achieved in an actual attempt to produce scientifically valuable results. To this end, an attractive and diversified set of observations were planned in advance to be executed at the VLT. These Science Verification observations at VLT UT1 took place as planned in the period from August 17 to September 1, 1998, cf. the September issue of the ESO Messenger ( No. 93, p. 1 ) and ESO PR 12/98 for all details. Although the meteorological conditions on Paranal were definitely below average, the telescope worked with spectacular efficiency and performance throughout the entire period, and very valuable data were gathered. After completion of all observations, the Science Verification Team started to prepare all of the datasets for the public release that took place on October 2, 1998. The data related to the Hubble Deep Field South (now extensively observed by the Hubble Space Telescope) were made public world-wide, while the release of other data was restricted to ESO member states. With this public release ESO intended to achieve two specific goals: offer to the scientific community an early opportunity to work on valuable VLT data, and in the meantime submit the VLT to the widest possible scrutiny. With the public release, many scientists started to analyse scientifically the VLT data, and the following few examples of research programmes are meant to give a sample of the work that has been carried out on the Science Verification data during the past two months. They represent typical investigations that will be carried out in the future with the VLT. Many of these will be directed towards the distant universe, in order to gather insight on the formation and evolution of galaxies, galaxy clusters, and large scale structure. Others will concentrate on more nearby objects, including stars and nebulae in the Milky Way galaxy, and some will attempt to study our own solar system. The following six research programmes were presented at the Press Conference that took place at the ESO Headquarters in Garching (Germany) today. Deep Galaxy Counts and Photometric Redshifts in the HDF-S NIC3 Field The goal of this programme was to verify the capability of the VLT by obtaining the deepest possible ground-based images and using multicolour information to derive the redshifts (and hence the distances) of the faintest galaxies. The space distribution, luminosity and colour of these extreme objects may provide crucial information on the initial phases of the evolution of the universe. The method is known as photometric redshift determination . The VLT Test Camera was used to collect CCD images for a total of 16.6 hours in five spectral filters (U, B, V, R and I) in the so-called HDF-S NIC3 field. This is a small area (about 1 arcmin square) of the southern sky where very deep observations in the infrared bands J, H and K (1.1, 1.6 and 2.2µm, respectively) have been obtained by the Hubble Space Telescope (HST). The observations were combined and analyzed by a team of astronomers at ESO and the Observatory of Rome (Italy). Galaxies were detected in the field down to magnitude ~ 27-28. In most colours, the planned limiting values of the fluxes were successfully reached. ESO PR Photo 48a/98 ESO PR Photo 48a/98 [Preview - JPEG: 800 x 856 pix - 144k] [High-Res - JPEG: 3000 x 3210 pix - 728k] PR Photo 48a/98 shows some examples of photometric redshift determination for faint galaxies in the HDF-S NIC3 field. The filled points are the fluxes measured in the five colors observed with the VLT Test Camera (U, B, V, R and I) and in the infrared H spectral band with the NICMOS instrument on the Hubble Space Telescope. The curves constitute the best fit to the points obtained from a library of more than 400,000 synthetic spectra of galaxies at various redshifts (Fontana et al., in preparation). For most of these very faint sources, it is not possible to collect enough photons to measure the recession velocity (the redshift) by spectroscopy, even with an 8-m telescope. The redshifts and the main galaxy properties are then determined by comparing the colour observations with synthetic spectra (see PR Photo 48a/98 ). This has been done for more than one hundred galaxies in the field brighter than magnitude 26.5. Around 20 are found to be at redshifts larger than 2. The brighter ones are excellent candidates for future detailed studies with the UT1 instruments FORS1 and ISAAC. The scientists involved in this study are: Sandro D'Odorico, Richard Hook, Alvio Renzini, Piero Rosati, Rodolfo Viezzer (ESO) and Adriano Fontana, Emanuele Giallongo, Francesco Poli (Rome Observatory, Italy). A Gravitational Einstein Ring Because the gravitational pull of matter bends the path of light rays, astronomical objects - stars, galaxies and galaxy clusters - can act like lenses, which magnify and severely distort the images of galaxies behind them, producing weird pictures as in a hall of mirrors. In the most extreme case, where the foreground lensing galaxy and the background galaxy are perfectly lined up, the image of the background galaxy is stretched into a ring. Such an image is known as an Einstein ring , because the correct formula for the bending of light was first described by the famous phycisist Albert Einstein . ESO PR Photo 48b/98 ESO PR Photo 48b/98 [Preview - JPEG: 800 x 1106 pix - 952k] [High-Res - JPEG: 3000 x 4148 pix - 5.4Mb] ESO PR Photo 48c/98 ESO PR Photo 48c/98 [Preview - JPEG: 800 x 977 pix - 272k] [High-Res - JPEG: 3000 x 3664 pix - 1.4Mb] PR Photo 48b/98 (left) shows a new, true colour image of an Einstein ring (upper centre of photo), first discovered at ESO in 1995. The ring, which is the stretched image of a galaxy far out in the Universe, stands out clearly in green, and the red galaxy inside the ring is the lens. The discovery image was very faint, but this new picture, taken with the VLT during the Science Verification Programme allows a much clearer view of the ring because of the great light-gathering capacity of the telescope and, not least, because of the superb image quality. In Photo 48c/98 (right), four images illustrate the deduced model of the lensing effect. In the upper left, the observed ring has been enlarged and the image of the lensing galaxy removed by image processing. Below it is a model of the gravitational field (potential) around this galaxy along with the "true" image of the background galaxy shown. At the lower right is the resulting gravitationally magnified and distorted image of the background galaxy, which to the upper right has been de-sharpened to the same image quality as the observed image. The similarity between the two is most convincing. The picture shows a new, true colour image of an Einstein ring, first discovered at ESO in 1995. The ring, which is the stretched image of a galaxy far out in the Universe, stands out clearly in green, and the red galaxy inside the ring is the lens. The discovery image was very faint, but this new picture, taken with the VLT during the Science Verification Programme allows a much clearer view of the ring because of the great light-gathering capacity the telescope and, not least, because of the superb image quality. Gravitational lensing provides a very useful tool with which to study the Universe. As "weighing scales", it provides a measure of the mass within the lensing body, and as a "magnifying glass", it allows us to see details in objects which would otherwise be beyond the reach of current telescopes. This new detailed picture has allowed a much more accurate measurement of the mass of the lensing galaxy, revealing the presence of vast quantities of "unseen" matter, five times more than if just the light from the galaxy is taken into account. This additional material represents some of the Universe's dark matter . The gravitational lens action is also magnifying the background object by a factor of ten, providing an unparalleled view of this very distant galaxy which is in a stage of active star-formation. The scientists involved in this study are : Palle Møller (ESO), Stephen J. Warren (Blackett Laboratory, Imperial College, UK), Paul C. Hewett (Institute of Astronomy, Cambridge, UK) and Geraint F. Lewis (Dept. of Physics and Astronomy, University of Victoria, Canada). An Extremely Red Galaxy One of the main goals of modern cosmology is to understand when and how the galaxies formed. In the very last years, many high-redshift (i.e. very distant) galaxies have been found, suggesting that some galaxies were already assembled, when the Universe was much younger than now. None of these high-redshift galaxies have ever been found to be a bona-fide red elliptical galaxy . The VLT, however, with its very good capabilities for infrared observations, is an ideal instrument to investigate when and how the red elliptical galaxies formed. The VLT Science Verification images have provided unique multicolour information about an extremely red galaxy that was originally (Treu et al., 1998, A&A Letters, Vol. 340, p. 10) identified on the Hubble Deep Field South (HDF-S) Test Image. This galaxy is shown in PR Photo 48d/98 that is an enlargment from ESO PR Photo 35b/98. It was detected on Near-IR images and also on images obtained in the optical part of the spectrum, at the very faint limit of magnitude B ~ 29 in the blue. However, this galaxy has not been detected in the near-ultraviolet band. ESO PR Photo 48d/98 ESO PR Photo 48d/98 [Preview - JPEG: 800 x 594 pix - 264k] [High-Res - JPEG: 3000 x 2229 pix - 1.8Mb] ESO PR Photo 48e/98 ESO PR Photo 48e/98 [Preview - JPEG: 800 x 942 pix - 96k] [High-Res - JPEG: 3000 x 3533 pix - 576k] PR Photo 48d/98 (left) shows the very red galaxy (at the arrow) in the Hubble Deep Field South , discussed here. Photo 48e/98 (right) is the spectrum of a typical elliptical galaxy, redshifted to z = 1.8 and compared with the brightness of the galaxy in different wavebands (crosses), as measured during the VLT SV programme and the Hubble Deep Field South Test Program (the cross to the right). The arrow indicates the upper limit by the VLT SV in the ultraviolet band. It can be seen that these observations are fully consistent with the object being an old, elliptical galaxy at the high redshift of z=1.8 , i.e. at an epoch, when the Universe was much younger than now. The new ISAAC instrument at VLT UT1 will be able to obtain an infrared spectrum of this galaxy and thus to affirm or refute this provisional conclusion. The colours measured at the VLT and on the HST Test Image are very well matched by those of an old elliptical galaxy at redshift z ~ 1.8 ; see Photo 48e/98 . All the available evidence is thus consistent with this object being an elliptical galaxy with the highest-known redshift for this galaxy type. A preliminary analysis of Hubble Deep Field South data, just released, seems to support this hypothesis. If these conclusions are confirmed by direct measurement of its spectrum, this galaxy must already have been "old" (i.e. significantly evolved) when the Universe had an age of only about one fifth of its present value. A spectroscopic confirmation is still outstanding, but is now possible with the ISAAC instrument at VLT UT1. A positive result would demonstrate that elliptical galaxies can form very early in the history of the Universe. The scientists involved in this study are: Massimo Stiavelli, Tommaso Treu (also Scuola Normale Superiore, Italy), Stefano Casertano, Mark Dickinson, Henry Ferguson, Andrew Fruchter, Crystal Martin (STSci, Baltimore, USA), Piero Rosati and Rodolfo Viezzer (ESO), Marcella Carollo (Johns Hopkins University, Baltimore, USA) and Henry Tieplitz (NASA, Goddard Space Flight Center, Greenbelt, USA). Lyman-alpha Companions and Extended Nebulosity around a Quasar at Redshift z=2.2 In current theories of galaxy formation, luminous galaxies we see to-day were built up through repeated merging of smaller protogalactic clumps. Quasars, prodigious sources pouring out 100 to 1000 times as much light as an entire galaxy, have been used as markers of galaxy formation activity and have guided astronomers in their hunting of primeval galaxies and large-scale structures at high redshift. A supermassive black-hole, swallowing stars, gas and dust, is thought to be the engine powering a quasar and the interaction of the galaxy hosting the black-hole with neighboring galaxies is expected to play a key role in "feeding the monster". At intermediate redshift, a large fraction of radio-loud quasars and radio galaxies inhabit rich clusters of galaxies, whereas radio-quiet quasars are rarely found in very rich environments. Furthermore, tidal interaction between quasars and their nearby companions is also the favoured explanation for the presence of large gaseous nebulosities associated with radio-loud quasars and radio galaxies. At high redshift, searches for Lyman-alpha quasar companions and emission-line nebulosities show strong similarities with those seen at lower redshift, although the detection rate is lower. ESO PR Photo 48f/98 ESO PR Photo 48f/98 [Preview - JPEG: 800 x 977 pix - 184k] [High-Res - JPEG: 3000 x 3662 pix - 1.1Mb] ESO PR Photo 48g/98 ESO PR Photo 48g/98 [Preview - JPEG: 800 x 966 pix - 328k] [High-Res - JPEG: 3000 x 3621 pix - 1.8Mb] PR Photo 48f/98 (left) is a false-colour reproduction of a B-band image of the field around the radio-weak quasar J2233-606 in the Hubble Deep Field South (HDF-S) . Photo 48g/98 (right) represents emission from the same direction at a wavelength that corresponds to Lyman-alpha emission at the redshift ( z = 2.2 ) of the quasar. Three Lyman-alpha candidate companions are indicated with arrows. Note also the extended nebulosity around the quasar. A search for Lyman-alpha companions to the radio-weak quasar J2233-606 in the Hubble Deep Field South (HDF-S) was conducted during the VLT UT1 SV programme in a small field of 1.2 x 1.3 arcmin 2 , centered on the quasar. Candidate Lyman-alpha companions were identified by subtracting a broad-band B (blue) image, that traces the galaxy stellar populations, from a narrow-band image, spectrally centered on the redshifted, narrow Lyman-alpha emission line of the quasar ( z = 2.2 ). Three Lyman-alpha candidate companions were discovered at angular distances of 15 to 23 arcsec, or 200 to 300 kpc (650,000 to 1,000,000 light-years) at the distance corresponding to the quasar redshift. The emission lines are very strong, relative to the continuum emission of the galaxies - this could be a consequence of the strong ionizing radiation field of the quasar. These companions to the quasar may trace a large-scale structure which would extend over larger distances beyond the observed, small field. Even more striking is the presence of a very extended nebulosity whose size (120 kpc x 160 kpc) and Lyman-alpha luminosity (3 x 10 44 erg/cm 2 /s) are among the largest observed around radio galaxies and radio-loud quasars, but rarely seen around a radio-weak quasar. Tidal interaction between the northern, very nearby companion and the quasar is clearly present: the companion is embedded in the quasar nebulosity, most of its gas has been stripped and lies in a tail westwards of the galaxy. The scientists involved in this study are: Jacqueline Bergeron (ESO), Stefano Cristiani, Stephane Arnouts, Gianni Fasano (Padova, Italy) and Patrick Petitjean (Institut d'Astrophysique, Paris, France). Very Distant Galaxy Clusters During the past years, it has become possible to detect and subsequently study progressively more distant clusters of galaxies. For this research programme, UT1 Science Verification data were used, in combination with data obtained with the SOFI instrument at the ESO New Technology Telescope (NTT) at La Silla, to confirm the existence of two very distant galaxy clusters at redshift z ~ 1 , that had originally been detected in the ESO Imaging Survey. This redshift corresponds to an epoch when the age of the Universe was only two-thirds of the present. ESO PR Photo 48h/98 ESO PR Photo 48h/98 [Preview - JPEG: 800 x 917 pix - 896k] [High-Res - JPEG: 3000 x 3438 pix - 6.0Mb] PR Photo 48h/98 (left) is a colour composite that shows the now confirmed cluster EIS0046-2930 . The image has been produced by combining the V (green-yellow), R (red) and I (Near-IR) exposures with the Test Camera obtained during the VLT-UT1 Science Verification. The yellow-orange galaxies are the cluster members and the bluer objects are galaxies belonging to the general field population. The cluster center is at the location of the largest (yellow-orange) cluster galaxy to the left of the center of the image. The field measures 90 x 90 arcsec. This was achieved by the detection of a spatial excess density of galaxies, with measured colour equal to that of elliptical galaxies at this redshift, as established by counts in the respective sky areas. The field of one these clusters is shown in PR Photo 48h/98 . These new data show that the VLT will most certainly play a major role in the studies of the cluster galaxy population in such distant systems. This will contribute to shed important new light on the evolution of galaxies. Furthermore, the VLT clearly has the potential to identify and confirm the reality of many more such clusters and thereby to increase considerably the number of known objects. This will be important in order to determine more accurate values of the basic cosmological constants, and thus for our understanding of the evolution of the Universe as a whole. The presentation was made by Lisbeth Fogh Olsen (Copenhagen Observatory, Denmark, and ESO) on behalf of the scientists involved in this study. Icy Planets in the Outer Solar System Observations with large optical telescopes during the past years have begun to cast more light on the still very little known, distant icy planets in the outer solar system. Until November 1998, about 70 of these have been discovered outside the orbit of Neptune (between 30 and 50 AU, or 4,500 to 7,500 million km, from the Sun). They are accordingly referred to as Trans-Neptunian Objects (TNOs) . Those found so far are believed to represent the "tip of the iceberg" of a large population of such objects belonging to the so-called Kuiper Belt . This is a roughly disk-shaped region between about 50 and 120 AU (about 7,500 to 18,000 million km) from the Sun, in which remnant bodies from the formation of the solar system are thought to be present. From their measured brightness and the distance, it is found that most known TNOs have diameters of the order of a few hundred kilometres. About half of those known move in elongated Pluto-like orbits, the others move somewhat further out in stable, circular orbits. During the two-week Science Verification programme, approximately 200 minutes were spent on a small observing programme aimed at obtaining images of some TNOs in different wavebands (B, V, R and I). Since this programme was primarily designed as a back-up to be executed during less favourable atmospheric conditions, some of the observations could not be used. However, images of three faint TNOs were recorded during an excellent series of 1-10 min exposures. From these data, it was possible to measure quite accurate magnitudes (and thus approximate sizes) and to determine their colours. One of them, 1996 TL66, was among the bluest TNOs ever observed. It is believed that this is because its surface has undergone recent transformation, possibly due to collisions with other objects or the breaking-off of small pieces from the surface, in both cases revealing "fresh" layers below. The combination of all available exposures made it possible to look for faint and tenous atmospheres around these TNOs, but none were found. These results show that it is possible, with little effort and even under quite unfavourable observing conditions, to obtain valuable information with the VLT about icy objects in the outer solar system. Of even greater interest will be future spectroscopic observations with FORS and ISAAC that will allow to study the surface composition in some detail, with the potential of providing direct information about (nearly?) pristine material from the early phases of the solar system. The scientists involved in this study are: Olivier Hainaut, Hermann Boehnhardt, Catherine Delahodde and Richard West (ESO) and Karen Meech (Institute of Astronomy, Hawaii, USA). How to obtain ESO Press Information ESO Press Information is made available on the World-Wide Web (URL: http://www.eso.org ). ESO Press Photos may be reproduced, if credit is given to the European Southern Observatory.