Detected Supernovae . The search have produced till now the detections of 4 SNe. ... This result highlights the power of infrared monitoring in detecting Obscured SNe and indicates that optical surveys are probably missing a significant fraction of SNe, especially in obscured systems such as starburst galaxies. ... In Fig. we show the archival SOFI image of NGC3256 (left) and the first image obtained in 2001 (right) where SN2001db has been detected. ...

... Radial velocities derived from different absorption lines show variability within the same spectrum. ... The atlas demonstrates certain spectral properties of IRAS 01005: P Cyg-like profiles of some spectral lines, nebular emissions, reduced metallicity. ... The velocity resolution of profiles is 2 km/s. Figure 1: Fragment of spectral atlas of IRAS 01005 and 9 Cep The hydrogen Balmer lines from H to H have asymmetric single-peaked emission profiles which are variable, but blue slope remains constant...

... 1994: . As a result of comparing the spectra of active solar regions from the observations with high spatial resolution in the microwave range at the RATAN-600 (the S-component) with a flare component observed at meter wavelengths on the VLA (USA) we revealed the presence of a strong and prolonged noise storm exactly where a weak decaying active region (with the presence of powerful active regions in the disk) is located. ... Archive . ...

FGS Instrument Handbook for Cycle 24 . ... Fine Guidance Sensor Instrument Handbook for Cycle 24 > Appendix B: FGS1r PerformanceSummary > B.2 Angular Resolution Test . ... At the time of the test, the predicted angular separation of the components was 0.085" (Franz and Wasserman, private communication). ... By rolling the HST in 6 increments, the projected separation along the X axis varied from the predicted angular resolution limit of FGS1r (~6 mas) to the resolution limit of FGS3 (~20 mas). ...

... Galaxies 99 Cosmic background with model of cloudy interstellar medium Yu. ... Figure 1: Averaged spectrum of the cosmic background I f in frequency range 0.25 200 MHz for the Galactic poles. ... First interpretation of the cosmic noise background spectrum at broad band frequency range 0.25 200 MHz with a model of the cloudy interstellar medium ISM is presented here. ... Synthesized background spectra I f for regions of the Galactic poles at the frequency range 0.25 200 MHz is presented in Fig. ...

Intrinsic Short Term Variability in W3-OH and W49N Hydroxyl Masers W.M. Goss National Radio Astronomy Observatory Socorro , New Mexico, USA A.A. Deshpande, Raman Research Institute Bangalore India R. Ramachandran , San Jose CA, USA The method-W3 OH · Use the VLBA with a beam of 5 mas and a velocity resolution of 0.1 km/s. Only simple sources are analyzed. ie no confusion from multiple components within the 2 arc sec maser region. ... About 400 or so time samples. ... Zeeman pairs at 1612 and 1720 MHz. ...

... The high angular resolution CGPS images of atomic hydrogen emission reveal a wide-spread, cold atomic hydrogen component of the interstellar medium in the form of dark self-absorption cloud complexes. These clouds resemble molecular cloud complexes in structure and trace the spiral arm structure of the Galaxy. ... Nevertheless, continuum absorption studies show that some of the cold atomic hydrogen clouds have temperatures as low as 15 - 20 K --- similar to dense molecular clouds. ...

... For GK Hya excess emis­ sion was observed in the Balmer lines and Mg I b lines while TY Pyx showed excess emission in the Balmer lines and Ca II H & K lines. The emission from GK Hya arises from a global phenomenon associated solely with the secondary component. The lack of significant He I D 3 excess absorption and an analy­ sis of the flux ratio in the Balmer lines suggest that the emission originates in prominence­like material seen off the limb of the star. ...

... The emission line galaxies observed are listed in Table 3 containing the following information: . column 1: The object's IAU-type name with the prefix HS. column 2: Right ascension for equinox B1950. column 3: Declination for equinox B1950. ... Two very faint objects (HS 1134+3640 and HS 1308+3845) are probably super-associations in the dwarf spiral NGC 3755 and in the Im galaxy UGC 8261. ... HS 1134+3639 : Probable low-mass companion of the galaxy NGC 3755 (the distance is 230 or 25 kpc). ...

To appear in "Fourth Workshop on Robotic Autonomous Observatories (2015)"RevMexAA(SC) METEOR OBSERVATIONS WITH MINI-MEGATORTORA WIDE-FIELD MONITORING SYSTEM S. Karpov, 1, 3 N. Orekhova2 G. Beskin, 1, 3 A. Biryukov3,4 S. Bondar,2 E. Ivanov,2 E. Katkova,2 A. Perkov, and V. Sasyuk3 RESUMEN 2 Favor de prop orcionar un resumen en espanol. ... The faintest detected meteors has the peak brightness about 10 mag, while the ma jority - from 4 to 8 mag. ... 2010; Karpov et al. 2013; Beskin et al. ...

Next: Cross References between CCF Up: Applications of CCF Previous: Applications of CCF Contents . Table 2: Cross reference of mirror CCF components to In-Flight Calibration Plan. Target Name . ... PSF . ... FilTransX, QuantumEf, XAreaEf . ... Table 3: Cross reference of EPIC CCF components to In-Flight Calibration Plan. ... Table 4: Cross reference of EPIC Inflight Calibration Targets to CCF components . ... Table 7: Cross reference of In-Flight Calibration Targets to OM CCF components . ...

... Science Users Information > Science and Technical Meetings > Conferences 2010 > The Origin and Fate of the Sun: Evolution of Solar-mass Stars Observed with High Angular Resolution . ... Observing Facilities . ... Observing with ESO Telescopes . ... The goal of this workshop is to review recent results on solar-mass stars obtained with infrared and millimeter interferometers, and to discuss their importance for our understanding of stellar evolution from star formation to stellar end products. ...

Magnetic Fields around Radio Galaxies Robert Laing (ESO) Laing et al. ... 2008) Negligible depolarization and 2 rotation Almost all Faraday effects must be due to foreground material How to fit depolarization caused by foreground Faraday rotation Complex polarization Rotation measure Integrate over a beam Observed RM for 0 2 rotation and depolarization Faraday rotation and depolarization 5.5 arcsec FWHM Faraday effects at high resolution FWHM = 1.5 ...

The ESA/ESO Astronomy Exercise Series 2 . The Distance to Messier 100 as Determined by Cepheid Variable Stars . ... The small variations in distance to the individual Cepheid variable stars in the Cloud are negligible compared with the much larger distance to the SMC. ... In this way Cepheid variable stars can be used as one of the 'standard candles' in the Universe that act either as distance indicators themselves or can be used to calibrate (or set the zero point for) other distance indicators. ...

... Archives . ... The PCA and ICA is used for separating mixed components with some assumptions. ... The need of source separation methods in astronomy has led various adaptations of decomposition methods available. ... I rarely come up with a paper which gathered and summarized component separation methods applicable to astronomical data. In that regards, the following paper seems useful to overview methods of reducing dimensionality for astronomers. [arxiv:0805.0269] . ... Chandra Blog . ...

Marc White . ... Turbulent entrainment processes may play an important role in the outflows from young stellar objects at all stages of their evolution. In particular, lateral entrainment of ambient material by high-velocity, well-collimated protostellar jets may be the cause of the multiple emission-line velocity components observed in the microjet-scale outflows driven by classical T Tauri stars. ... University of Amsterdam; STARPLAN, Copenhagen, Jul 2013 . ... E marc.white@anu.edu.au . ...

... Previous: ESO C Library for an Image Processing Software Environment (eclipse) . ... A new CLEAN-type algorithm searches for model components not in the dirty image but in the multi-resolution wavelet transform of the dirty image based on the dirty beam. ... The improvement of this prototype Wavelet CLEAN, which does convolve with the dirty beam, can be attributed to a suppression of noise and aliasing in the dirty image by use of information in the sidelobes of the whole image domain. ...

... Initial mass function and binary stars . ... The principal goal of this study is to show that the real shape of the initial mass function for low- and intermediate-mass stars differs from the observed one. In particular, comparison of radii of eclipsing binary components and single stars shows a noticeable difference for B0V-G0V components of eclipsing binaries and single stars of the corresponding spectral type. ...

... SB, Porb = 55.9212d. V0745 Cas| ... Component B of the double system observed brighter than in the Hipparcos Input Catalogue. ... The variability may be due to the fainter component. ... Type ELL: is also possible. pi Cas| ... Variability type and spectral type (F2/F3Ib/II) do not agree. ... Variability type and spectral type (F3/F5II) do not agree. ... Variability may be due to component B. VZ Pic| ... Variability may be due to component B. V1377 Ori| ... SB, Porb = 9.073d. V0421 Cep|105091| ...

Text of these problems is available also in other languages : . ... What can one see in the Moon's sky more often - the Sun or the Earth? ... There are about of 250 millions of stars in the elliptical galaxy M32 (a satellite of Andromeda galaxy). ... The masses of Capella's components. ... You are proposed to estimate the masses of Capella's components, using our observational data. ... A galaxy's mass. ... Estimate the mass of FGC 1908 and compare it to the mass of our galaxy. ...