... Fitting the observed dependence includes calculations of the polarization cross-sections averaged over particles orientation and size distribution, their normalization and the comparison of obtained dependencies with Serkowski's curve representing observational data for a chosen star. ... Variations of the polarization factors with wavelength are shown in Fig. 16 for homogeneous spheroidal particles with PF orientation. ... The distinction between prolate and oblate spheroids is also clearly seen. ...

... The sample of the Local Volume galaxies (distance smaller than 10 Mpc) gives a unique opportunity to study the properties of galaxies including the weakest objects: the absolute magnitude M B -10 and the virial mass M vir 10 9 M x263C;. ... Luminosity function of the Local Volume galaxies. ... The luminosity functions for galaxies are presented: red dashed line - from the 2dFGRS survey (Norberg et al. 2002); blue dash-dotted line - from the SDSS survey (Blanton et al. ...

... ATNF Home . About ATNF . ... About ATNF overview . ... Australia Telescope Steering Committee . ... Australia Telescope User Committee . ... Australian Square Kilometre Array Pathfinder . Murchison Radio-astronomy Observatory . ... Parkes radio telescope . Australia Telescope Compact Array . Mopra radio telescope . ... Australia Telescope Online Archive (ATOA) . ... Visiting Parkes radio telescope . Visiting Australia Telescope Compact Array . ... Parkes radio telescope webcam . ...

Chiaki Kobayashi, Ralph Sutherland How galaxies did form and evolution? - to answer this unsolved problem, we are simulating the formation and evolutionary history of galaxies in the Universe, including star formation, supernovae feedback, and chemical enrichment. Comparing the spacial distribution of elements within galaxies with observations, we will examine fundamental physical processes that drive galaxy formation. ... COALA : Universe Galaxy AGN Star Planet ...

... ALMA . ... ARC Staff at ESO . ... The European ALMA Regional Centre (ARC) provides the interface between the ALMA project and the European science community. ... Below you can read the latest Announcements from the European ARC Network.. ... The call for 1-mm Very Long Baseline Interferometry (VLBI) proposals to use phased ALMA at Band 6 in Cycle 4, in collaboration with the Event Horizon Telescope Consortium (EHTC), will be released to coincide with the ALMA Cycle 4 Call for Proposals in March 2016...

NMW survey overview . Access image archive . ... The New Milky Way survey aims to detect bright (V<13.5) optical transients near the Galactic plane using an automated wide-field (8x6 deg.) system capable of surveying the whole Milky Way area visible from the observing site in one night. ... All images obtained during the transient search survey are available online (please use the image archive access form ). ... Images per field: . ... Images per night: . ... Milky Way imaging time: . ...

The calculated flux distribution in the 300 to 400 nm region only fits the observed distribution closely for both the Sun and Arcturus when the complete ATLAS9 line list is used. ... Moreover, for Arcturus, even the sub-set of high quality lines can only provide a close fit to the observed high resolution spectrum if we include, ad hoc, an extra amount of continuous absorption opacity. ...

J/MNRAS/429/2080 Lockman Hole 10C sources radio spectral indices (Whittam+ 2013) ================================================================================ The faint source population at 15.7 GHz. ... 2011, Cat. ... 2008, Cat. ... For 10C sources without a counterpart in the GMRT image, three times the local noise is included as an upper limit on the flux density at 610MHz. ... 1.4-GHz flux density value from NVSS catalogue, including upper limits for undetected sources 76 I1 --- f_SNVSS [0/1]? ...

Computer models of objects (galaxies, circumstellar disks, etc.) are often generated to compare with observed images. ... When comparing models to WFPC2 images, it is often forgotten that the instrumental PSF can have a very significant effect. ... Also, the undersampling of the WFPC2 cameras makes the model image very sensitive to subpixel alignment. ... Left) WFPC2 WFC F814W image of HH30 (0.1 arcsec/pixel); (Middle) Model of HH30 disk; (Right) Model of HH30 disk convolved with a Tiny Tim model PSF. ...

... The following charts/text are intended as tools for monitoring the Type Ia supernovae ( SNe ) event visually or photographically (utilizing telescope equipped CCD equipment).The files include: A replication of The Type Ia SNe , V- magnitude (with data point checks from other cited references)and color index (B-V) templete (to indicate a general color-related trend of the type Ia ... I believe this might help alleviate some of the problems involving the making of acceptable amateur light curves...

... Radio astronomers at Arecibo Observatory observe a wide variety of phenomena in the Milky Way and in other galaxies. ... Some REU projects are carried out on pre-existing data, and others rely on obtaining new data. ... Deriving a new shape model from existing radar images has been a popular student project in past years, and there are data sets that could be used for this. We are collecting thermal infrared emission data for many of the near-Earth asteroids that are also observed with radar. ...

home education > activities . SEARCH ASP SITE: Match ALL words Match ANY word . ... Activities . ... Astronomy . ... Activities on the . ... This is more about space technology than astronomy, but in this interactive module, students simulate what the astronauts go through when they go up to service the Hubble Space Telescope. ... Younger students are shown a drawing that can be interpreted in two ways and then apply what they learn to planetary images. ... table of contents . ...

... RATAN-600 data for the BL Lacertae objects (multi-frequency catalogue, Version 1.0) . GPS radio sources . ... BL Lacertae objects . ... The difference between these objects is the peak frequency of the synchrotron component of their spectral energy distribution (HBLs: high-energy peak, LBLs: low-energy peak, IBLs: intermediate). ... The observations were carried out with the RATAN-600 radio telescope during 2006-2011 at six frequencies: 1.1, 2.3, 4.8, 7.7, 11.2 and 21.7 GHz. ...

... New Mexico State University is seeking a technical and computer-oriented person as a Support Astronomer for nighttime astronomical observing at Apache Point Observatory (APO) with the Astrophysical Research Consortium (ARC) 3.5m Telescope. б  . ... Paper/email documents will not be accepted. ... TELESCOPE OPERATIONS SPECIALIST . ... Responsibilities include nightly operation of the 3.5m telescope and instruments, Quality monitoring the data streams and system performance and observing efficiency. ...

... NICS will be the only infrared instrument for the first light of the TNG; as a consequence, we decided to incorporate a sufficient degree of operation flexibility by providing the instrument with six different observing modes, three aimed at imaging and three at spectroscopy: . ... It will be possible to use the narrow band filters as order sorters; this will allow to perform high resolution long-slit spectroscopy in the wavelength ranges covered by the available narrow band filters. ...

Isabel Leonor University of Oregon searched 25 S2 GRBs for coincident G-waves of duration ~1 ­ 10 ms used crosscorrelation method explored data conditioning in the frequency domain, included whitening and phase correction ­ luxury of limited on-source and off-source data to analyze injected signals to study sensitivity of pipeline used playground data with no GRB trigger data analysis code (standalone), injection and calibration scripts, written using Matlab ...

Next: NICMOS/HST H-band (F160W) Images Up: NICMOS Science Previous: HST NICMOS Observations of . ... Observations of P . ... The NICMOS team has devised a comprehensive program of observations of the Galactic Center. ... Data in hand give a first look at variability and a detailed look at the search for the tip of the main sequence will be discussed where NICMOS has demonstrated adequate sensitivity and photometric precision to identify likely O8-B1 stars at the Galactic Center. ...

... We demonstrate through numerical simulations that model parameters estimated with our technique are essentially bias-free, even when the average number of counts per bin is 1. ... The IW technique avoids such biases by estimating through successive iterations, where for each iteration, j, , and the best-fit parameters are determined by minimization of . ... In our sample, we find that the minimum values and best-fit parameters converge after about 6 iterations. ...

XmCCD ----- The programs provided here offer a Linux graphical user interface to astronomical and scientific CCD cameras. ... It is the latest one they offer and the files included allow support for Android and Mac OS X. This distribution of XmCCD includes source code to utilize the SBIG shared library libsbigudrv.so with a Motif-based graphical user interface. ... The XmCCD source package includes and will install: SAOimage ds9 xpa cfitsio SAOimage is the primary image display for XmCCD. ...

... We compare our results with the GRANAT X-ray observations of the Galactic center (Churazov et al. ... It is instructive to compare our results for the Galactic center starburst with what might be expected for a continuous star formation, with the average rate characteristic for the whole Galaxy. For this continuous star formation model, we would expect to observe in the region of around the Galactic center about 10% of the total number of X-ray sources in the Galaxy. ...