Extended mid-infrared emission from VV 114: probing the birth of a ULIRG

We present our 5-16 micron spectro-imaging observations of VV114, an infrared luminous early-stage merger, taken with the ISOCAM camera on-board ISO. We find that only 40% of the mid-infrared (MIR) flux is associated with a compact nuclear region, while the rest of the emission originates from a rather diffuse component extended over several kpc. This is in stark contrast with the very compact MIR starbursts usually seen in luminous infrared galaxies. A secondary peak of MIR emission is associated with an extra-nuclear star forming region which displays the largest Halpha equivalent width in the whole system. Comparing our data with the distribution of the molecular gas and cold dust, as well as with radio observations, it becomes evident that the conversion of molecular gas into stars can be triggered over large areas at the very first stages of an interaction. The presence of a very strong continuum at 5 microns in one of the sources indicates that an enshrouded active galactic nucleus may contribute to 40% of its MIR flux. We finally note that the relative variations in the UV to radio spectral properties between the merging galaxies provide evidence that the extinction-corrected star formation rate of similar objects at high z, such as those detected in optical deep surveys, can not be accurately derived from their rest-frame UV properties.Comment: 14 pages, 5 figures, accepted for publication in A&

Mid-infrared observations of the ultraluminous galaxies IRAS14348-1447, IRAS19254-7245, and IRAS23128-5919

We present a study of the three ultraluminous infrared galaxies IRAS14348-1447, IRAS19254-7245, and IRAS23128-5919, based on mid-infrared (MIR) spectro-imaging (5-18microns) observations performed with ISOCAM. We find that the MIR emission from each system, which consists of a pair of interacting late type galaxies, is principally confined to the nuclear regions with diameters of 1-2kpc and can account for more than 95% of their IRAS 12micron flux. In each interacting system, the galaxy hosting an active galactic nucleus (AGN) dominates the total spectrum and shows stronger dust continuum (12-16microns) relative to the Unidentified Infrared Band (UIB) emission (6-9microns), suggestive of its enhanced radiation field. The MIR dominant galaxy also exhibits elevated 15micron/Halpha and 15micron/K ratios which trace the high extinction due to the large quantities of molecular gas and dust present in its central regions. Using only diagnostics based on our mid-infrared spectra, we can establish that the Seyfert galaxy IRAS19254-7245 exhibits MIR spectral features of an AGN while the MIR spectrum of the Seyfert (or LINER) member of IRAS23128-5919 is characteristic of dust emission principally heated by star forming regions.Comment: Accepted for publication in Astronomy & Astrophysics, 13 pages, 9 figure

The Physical Conditions and Dynamics of the Interstellar Medium in the Nucleus of M83: Observations of CO and CI

This paper presents CI, CO J=4-3, and CO J=3-2 maps of the barred spiral galaxy M83 taken at the James Clerk Maxwell Telescope. Observations indicate a double peaked structure which is consistent with gas inflow along the bar collecting at the inner Lindblad resonance. This structure suggests that nuclear starbursts can occur even in galaxies where this inflow/collection occurs, in contrast to previous studies of barred spiral galaxies. However, the observations also suggest that the double peaked emission may be the result of a rotating molecular ring oriented nearly perpendicular to the main disk of the galaxy. The CO J=4-3 data indicate the presence of warm gas in the nucleus that is not apparent in the lower-J CO observations, which suggests that CO J=1-0 emission may not be a reliable tracer of molecular gas in starburst galaxies. The twelve CI/CO J=4-3 line ratios in the inner 24'' x 24'' are uniform at the 2 sigma level, which indicates that the CO J=4-3 emission is originating in the same hot photon-dominated regions as the CI emission. The CO J=4-3/J=3-2 line ratios vary significantly within the nucleus with the higher line ratios occurring away from peaks of emission along an arc of active star forming regions. These high line ratios (>1) likely indicate optically thin gas created by the high temperatures caused by star forming regions in the nucleus of this starburst galaxy.Comment: 15 pages with 10 figures. To appear in the August 10 1998 issue of The Astrophysical Journa

Lattice and spin excitations in multiferroic h-YMnO3

We used Raman and terahertz spectroscopies to investigate lattice and magnetic excitations and their cross-coupling in the hexagonal YMnO3 multiferroic. Two phonon modes are strongly affected by the magnetic order. Magnon excitations have been identified thanks to comparison with neutron measurements and spin wave calculations but no electromagnon has been observed. In addition, we evidenced two additional Raman active peaks. We have compared this observation with the anti-crossing between magnon and acoustic phonon branches measured by neutron. These optical measurements underly the unusual strong spin-phonon coupling

Temperature-induced Change in the Fermi Surface Topology in the Spin Density Wave Phase of Sr(Fe1−x_{1-x}Cox_x)2_2As2_2

We report electronic Raman scattering measurements of Sr(Fe$_{1-x}$Co$_x$)$_2$As$_2$ single crystals in their magnetic - Spin Density Wave (SDW) phase. The spectra display multiple, polarization-resolved SDW gaps as expected in a band-folding itinerant picture for a multiband system. The temperature dependence of the SDW gaps reveals an unusual evolution of the reconstructed electronic structure with at least one gap being activated only well below the magnetic SDW transition $T_N$. A comparison with temperature dependent Hall measurements allows us to assign this activated behavior to a change in the Fermi surface topology deep in the SDW phase, which we attribute to the disappearance of a hole-like Fermi pocket. Our results highlight the strong sensitivity of the low energy electronic structure to temperature in iron-arsenide superconductors.Comment: 10 pages, 7 figure

Evidence of triggered star formation in G327.3-0.6. Dust-continuum mapping of an infrared dark cloud with P-ArT\'eMiS

Aims. Expanding HII regions and propagating shocks are common in the environment of young high-mass star-forming complexes. They can compress a pre-existing molecular cloud and trigger the formation of dense cores. We investigate whether these phenomena can explain the formation of high-mass protostars within an infrared dark cloud located at the position of G327.3-0.6 in the Galactic plane, in between two large infrared bubbles and two HII regions. Methods: The region of G327.3-0.6 was imaged at 450 ? m with the CEA P-ArT\'eMiS bolometer array on the Atacama Pathfinder EXperiment telescope in Chile. APEX/LABOCA and APEX-2A, and Spitzer/IRAC and MIPS archives data were used in this study. Results: Ten massive cores were detected in the P-ArT\'eMiS image, embedded within the infrared dark cloud seen in absorption at both 8 and 24 ?m. Their luminosities and masses indicate that they form high-mass stars. The kinematical study of the region suggests that the infrared bubbles expand toward the infrared dark cloud. Conclusions: Under the influence of expanding bubbles, star formation occurs in the infrared dark areas at the border of HII regions and infrared bubbles.Comment: 4 page

The NICMOS Snapshot Survey of nearby Galaxies

We present ``snapshot'' observations with the NearInfrared Camera and MultiObject Spectrometer (NICMOS) on board the Hubble Space Telescope (HST) of 94 nearby galaxies from the Revised Shapley Ames Catalog. Images with 0.2 as resolution were obtained in two filters, a broad-band continuum filter (F160W, roughly equivalent to the H-band) and a narrow band filter centered on the Paschen alpha line (F187N or F190N, depending on the galaxy redshift) with the 51x51 as field of view of the NICMOS camera 3. A first-order continuum subtraction is performed, and the resulting line maps and integrated Paschen alpha line fluxes are presented. A statistical analysis indicates that the average Paschen alpha surface brightness {\bf in the central regions} is highest in early-type (Sa-Sb) spirals.Comment: Original contained error in flux calibration. Table 1 now has correct Paschen Alpha fluxes. 14 pages LaTeX with JPEG and PS figures. Also available at http://icarus.stsci.edu/~boeker/publications.htm

Fulguraçao e radiofreqüência na taquicardia ventricular

Durante um período de 10 anos, 89 casos de taquicardia ventricular (TV) resistentes aos antiarrítmicos foram tratados pelo método da fulguraçao. A série foi composta por: 37 casos de enfarte do miocárdio, com fraçao de ejeçao média de 30%, onde o acompanhamento médio dos sobreviventes foi de 61 meses e a eficácia clínica foi de 87,9%; 23 casos de displasia arritmogênica do ventrículo direito, em que a média de idade foi de 40 anos e a fraçao de ejeçao média de 57%, acompanhados durante 71 meses em média, com eficácia clínica de 83%; 12 pacientes que apresentavam TV sensíveis ao verapamil (fasciculares), com idade média de 30 anos e fraçao de ejeçao média de 65%, sendo o seu acompanhamento médio de 55 meses e eficácia clínica de 100%; 10 pacientes portadores de cardiomiopatia idiopática dilatada, idade média de 35 anos e fraçao de ejeçao média de 23% que, acompanhados por 38 meses, permitiram constatar uma eficácia clínica de 80%; 4 outros pacientes, com idade média de 21 anos, doenças congênitas operadas e com fraçao de ejeçao média de 60%, em que um acompanhamento de 36 meses demonstrou eficácia clínica de 100%. Por fim, 3 pacientes com taquicardias ventriculares idiopáticas infundibulares, idade média de 36 anos e fraçao de ejeçao média de 62%, acompanhados durante um período de 72 meses, com uma eficácia clínica de 67%. Complicaçoes nao letais foram observadas em 16% dos casos, notadamente o hemopericárdio, observado em 4,5% dos casos, tendo implicado em pericardiocentese. A mortalidade operatória no mês posterior à ablaçao foi de 9,2%, sendo principalmente observada durante a fase de aprendizagem. Em conclusao, ainda que nao seja isenta de riscos, em maos experientes a fulguraçao obteve resultados notáveis na maioria dos casos. Continua a ser indicada nas TV resistentes à radiofrequência, o que foi observado em mais da metade dos casos numa série preliminar de 41 pacientes