next up previous contents index
Next: Foreword Up: INAF Osservatorio Astrofisico di Previous: List of Tables   Contents   Index


List of Figures

  1. Image of the extended solar corona obtained by the LASCO C1 coronagraph on board SOHO on October 30, 1997, through a narrow-band Fabry-Pèrot filter at the centre of the ion Fe XIV 5303 $\AA$  line. Superposed on the LASCO image are the UVCS slit fields of view (white lines) at nominal slit height of 1.75 R$_{\odot}$, for P.A. = 330 deg (a) and P.A. = 270 deg (b). The nominal heliocentric distance and P.A. for each slit refer to the distance and P.A. of the point along the slit that is closest to the limb (shown as a white dot). The Ly$\alpha$ and O VI 1032 $\AA$  total line intensities and 1/2 half-widths, as well as the O VI line ratios, vs. position angle alonf the slit (a) and (b) are shown at the bottom of the figure.
  2. Two subsets of the TSI and SSI time series during the minimum of solar cycle 23 (open diamonds) with their respective best fits (solid lines) are plotted in panels (a), (c), (e) and (g) for the labelled passbands in the left and right columns, respectively. The model is usually embedded into the data sequence, except when data gaps are present. The residuals are plotted in the corresponding lower panels (b), (d), (f) and (h), respectively. The time is indicated in days from 1$^{\rm st}$ January 1996 on the lower scale and in years on the upper scale. The data subsets range from 13 July 1996 to 11 September 1996 on the left panels, including the intervals previously analysed by Eker et al. (2003) and Fligge et al. (2000, Fig. 6), and from 5 November 1996 to 4 January 1997 on the right panels, previously analysed by Fligge et al. (2000, Fig. 7), respectively.
  3. The same as Fig. 1.2 for two data subsets close to the maximum of solar cycle 23, ranging from 29 January 2000 to 29 March 2000 in the left panels, and from 29 March 2000 to 28 May 2000 in the right panels, respectively. These time series were previously modelled by Krivova et al. (2003, Fig. 3 right panels).
  4. The relative squared sound-speed differences between two standard solar models, differing for the chemical composition, and the Sun, as obtained by inversion of a set of MDI oscillation frequencies.
  5. Solar profile of the $\lambda8498$ line (solid, thick line), compared to the synthetic photospheric profile of a star with \ensuremath{T_\mathrm{eff}}=5780 K and \ensuremath{\log g}=4.44 (dashed line). The residual profile (solid, thin line) is also shown (from ()).
  6. Upper panel: The $(O-C)$ of the primary eclipses of RS CVn versus time. The reference ephemeris is: $ Min\; I = 2410102.4280 + 4.797817 \times E$, where $E$ is the number of orbital cycles elapsed from the initial epoch. The dashed line is a third-order polynomial best fit to the data. Middle panel: The residual $(O-C)_{I}$ versus time obtained by subtracting the third-order polynomial fit to the $(O-C)$ variation in the upper panel. Lower panel: The total spotted area on the K2IV active component of RS CVn as derived by Rodonò et al. (1995).
  7. The expected relative orbital period variation of a star-planet system versus the orbital period of the planet according to an extrapolation of the model by Lanza & Rodonò (1999). The central star is assumed to be a late-type dwarf of mass $M=0.7  M_{\odot }$ and radius $R=0.86  R_{\odot }$. The plots are labelled by the rotation period $P_{rot}$ of the central star: $P_{rot} = 3$ days (solid line), $P_{rot} = 10$ days (dashed line) and $P_{r
ot} = 30$ days (dotted line).
  8. Radial-velocity curves (circles for Fekel (1983) data, asterisks for IUE, squares for Frasca & Lanza () data) and best-fit solution for HR 1099. The solid lines are the radial-velocity curves computed according to Fekel's ephemeris, the dashed lines are the actual radial-velocity curves, fitted to the observational data by varying the phase of superior conjunction $\phi_{0}$. This sequence of radial velocity curves make evident the orbital period change of HR 1099 versus time.
  9. The \ensuremath{R _\mathrm{IRT}} index (calculated for the $\lambda$8542 CaIIIRT line as $CD_{calculated}$ - $CD_{observed}$) versus \ensuremath{\log{R^{'}_\mathrm{HK}}}for a sample of stars observed with the SARG spectrograph at TNG .
  10. Observed (dots) and synthetic (full lines) light and temperature curves of VY Ari. The $B-V$ curve is also shown in the lower box with the solution superimposed for comparison. A schematic map of the starspot distribution, as seen at two different rotational phases, is also shown.
  11. Grids of solutions for VY Ari. The filled circles represent the solutions for light curve, while the filled diamonds represent the solutions for temperature curve. The hatched area, in each box, is the locus of the allowed solutions accounting for data errors.
  12. Examples of short- and long-term activity cycle.
  13. Correlation among activity centers longitude (panels a, b), rotational period variation (c), and spot area variation (d) on II Peg
  14. Correlation between H$\alpha$ EW and V-band light curve of II Peg (from Lanzafame et al., in progress)
  15. Radial velocity curves of the primary (filled circles) and secondary components (open circles) of KO Aql and S Equ and their best fits (solid and dashed lines).
  16. The relative isothermal squared sound-speed differences between Procyon A and a stellar model as obtained by inversion of Martic et al. (2004) data. The model used here is characterized by $M/M_{\odot}=1.47$, $Age=1.78$ (Gyr), $L/L_{\odot}=6.88$, $T_{\rm eff}= 6501 (\mathrm{K})$, $ R/R_{\odot}=2.07$, $Z=0.016$.
  17. Dependence of H$_{\rm eff}$ measurements on the atomic weight
  18. Comparison between the observed and computed H$_{\delta}$ and H$_{\gamma}$ lines in HR6000
  19. Radial velocity curve of HD358 and composite H$\beta$ profile of HD216494
  20. Dereddened $I_C$ versus $(I_C-z)$ diagram for the point-like objects extracted from WFI images in the Cha II field. The lines in the plot represent the theoretical PMS isochrones for 1 (dashed line), 5 (full line) and 10 Myr (dash-dotted line), respectively, shifted to the distance modulus of Cha II (6.25 mag). The previously known PMS stars are indicated with squares. The big dots represent the objects above the 5-Myr isochrone, i.e. the "photometrically-selected" candidates. The big blue dots represent the BD candidates with $H\alpha$ emission.
  21. Upper panel: Spectral energy distribution (SED) of RX J0529.4+0041 A as deduced from observed $UBV(RI)_C JHK$ fluxes (dots) compared with calculated ones (triangles) obtained from a combination of two synthetic Next-Generation spectra with effective temperatures of 5200K and 4200K (continuous thin lines). Lower panel: comparison between observed (dots) and computed (squares) SED of RX J0529.4+0041 B, superimposed to the synthetic Next-Generation spectrum (thin continuous line) for $T_{\rm eff}=4400$K.
  22. Radial velocity curves (dots= OAC data, diamonds= ELODIE data) of two newly discovered binaries togeter with the contemporaneous $V$ ligth curves.
  23. The measured apparent magnitudes of the supernovae as a function of their redshift. The continuous line represents the prediction of the IRFP cosmology, the dashed one is the best-fit FRW model, and the dot-dashed line is a flat FRW model with zero cosmological constant.
  24. Luminosity functions for different environments. The continuous curves are Schechter fits to data from Croton et al. (2004), while filled points and triangles are predictions from our model for field (points) and ''void'' (open triangles) environments, respectively. $\delta_{8}$ is the average overdensity in spheres of $8 h^{-1}$ Mpc, $\delta_{cic}$ is the overdensity estimated in N-body simulations using a CIC estimator with 64 neighbours. The inputs MFs were derived for two different simulations with comparable mass resolution
  25. Left: Dark matter isodensity contours in a N-body simulation of a region containing few clusters. The latter are the saturated regions, while the contours trace the filament threading the cluster. Right: Shear map obtained from mass-aperture statistics (Schneider 1996). Equal contours are from 1 to 6$\sigma$. The filament is marginally detectable.
  26. Astrophisycs Laboratory: Apparatus
  27. Astrophisycs Laboratory: Possible experiments
  28. Astrophisycs Laboratory: implanter
  29. The three axes translator equipped with a reflective objective. The spot image is shown on the right as well as the 3d plot and the relative FWHM of the sub-image.
  30. Architecture of the SPADA system. The chip is assembled on a ceramic holder and on a Peltier stage (right) and is driven by the detection board (on right the schematic block diagram). The cross-section of the mechanical mounting is shown o the down part.
  31. Examples of the computation of the Power Spectral Density (PDS) with AstroMD, applied to data from FLY at a redshift of about zero, for different cell resolution values. The spectral index is approximately $2$ up to the turn-over, so Power Spectrum converges at large scale (small $k$). After the turn-over PSD decades as a power law with an exponent of approximately $-4$.
  32. Graphical outputs of the Power Spectrum of data from FLY at a redshift of approximately $10$.
  33. The FoF group finding algorithm inside AstroMD.
  34. The Astrocomp mask to upload the set of parameters for each light curve analysis.
  35. The visualization of a postscript file showing the best fit and the Mercator maps of the components of a close binary system for the Maximum Entropy solution (upper panels) and the best fit and the Mercator star maps for the Tikhonov model (lower panels), respectively.
  36. Optical layout of the spectrograph. Light enters from fibers through a preslit system into the spectrograph entrance slit.
  37. An enhnanced silver coating will guarantee a total efficiency of the two mirrors larger than 91% at any wavelengths after the three reflections.
  38. Camera layout. All-spherical surfaces and only standard glasses (Ohara S-FPL51, S-BSL7) ensure high quality, high transmission and low cost. Note the tilted focal plane to correct for axial chromatism.
  39. The right angle prism switching between the two dispersion modes.
  40. Raytraced spectral format onto the CCD. In the two column, interorder separations between adjacent orders (in pixels) and the slit height (in pixels) are shown. Box represents the CCD area.
  41. Spectrograph spot diagrams on the CCD focal plane. First three configurations (columns) show the LOW RES mode, while the other configurations show the HIGH RES mode. Boxes are 4x4 pixels wide.
  42. External view of the new building for the automatic telescopes
  43. Schematic drawing of the folding dome for the automatic telescopes. Courtesy of Gambato Costruzioni per Astronomia
  44. Solar facilities: The equatorial spar
  45. Solar facilities: H$\alpha$ a image of the Sun
  46. The 91-cm Cassegrain reflector with fibre feed interface
  47. Numbers of contacts of Out-reach and Educational activities of Catania Astrophysical Observatory from 1994



Innocenza Busa' 2005-11-14