... OOF software . ... Memos . ... Raw data . ... We present a Bayesian approach to calculating the coefficients that convert the outputs of ALMA 183 GHz water-vapour radiometers into estimates of path fluctuations that can be used to correct the observed interferometric visibilities. ... Please note that the files"COPYING" in each of the distribution packages have GPL listed but it is in fact LGPL which applies. ... This is the raw data from the SMA used in the analysis shown in Section 4 of the memo. ...

... Up: Software Systems and Tools . ... The Starlink Software is a collection of astronomical packages and utilities comprising over 120 separate components. When built, the system needs between 500 and 650 MB disk space (without source) making it ideal for distribution on CD-ROM. Each component has been individually packaged into an easy-to-install bundle for users to obtain over the Internet via a ``point and click'' WWW interface from the Starlink Software Store. ...

... 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 . ...

... If your workstation can run any of the standard data reduction systems, it can run Draco. ... The Draco source files and executable will require about 20Mb of disk space. Draco is written in Common Lisp, specifically Allegro Common Lisp 4.2 beta by Franz, Inc. The distribution includes an executable image, so you don't need a Lisp system at your site. We chose Lisp since it offered a powerful, high-level development environment that is available on many different machines. ...

... The MIDAS system is available, free of charge, to all non--profit research institutes, whereas other organisations or companies may be charged a nominal fee to cover distribution. Institutes interested in using MIDAS must sign a User Agreement before they receive MIDAS. The necessary forms can be obtained by contacting the Data Analysis Group at ESO/Munich. ... The current system at ESO/Munich is frozen several months prior to the official release. ...

Next: Star Formation Rate and Up: No Title Previous: Calculation of Evolutionary Tracks . To start calculations, we choose the distributions of the initial binary parameters: the mass of the primary ZAMS component, , binary mass ratio, , orbital separation a . ... whereas the mass ratio distribution is not. ... The zero assumption often made is that the mass ratio distribution has a flat shape, that is binaries with a high mass ratio occur as frequently as those with equal masses. ...

Next: stecf.cplucy - Enhanced Two-channel Up: The ``stecf" IRAF Layered Previous: The ``stecf" IRAF Layered . For many years the ST-ECF has developed IRAF tasks and packages for HST and related data analysis. ... To allow wider and more efficient distribution and to bring all components to a uniform level of quality and documentation we have decided to combine these components into a standard-format IRAF package to be called ``stecf''. ...

... PPTA timeline . ... List of projects . ... However, our time series are not equally sampled, so classical spectrum analysis cannot be applied immediately. ... Normally when analysing time series with very steep spectra one would use a "prewhitening" technique and perhaps a low sidelobe spectral window (e.g. the Hanning window). ... The idea is to separate the steep and flatter spectrum components so they can be analysed separately. ... The upper panel has raw data, interpolated data and red...

EPIC MOS response Steve Sembay, R.D. Saxton 10 December 2004 1 CCF components Name of CCF VALDATE EVALDATE Blocks changed XSCS ag EMOS1 REDIST 0043.CCF 1999-12-10 2000-07-15 CCD REDISTRIBUTION-n NO EMOS1 REDIST 0044.CCF 2000-07-15 2000-11-09 CCD REDISTRIBUTION-n NO EMOS1 REDIST 0045.CCF 2000-11-09 2001-04-18 CCD REDISTRIBUTION-n NO EMOS1 REDIST 0046.CCF 2001-04-18 2001-08-18 CCD ... This release contains a new set of CCFs which enable rmfgen to generate the correct rmfs. ...

CIMA is more than just the observing tool - in fact, the observing tool is just a part of a bigger package called the CIMA software package. ... There is also a another package called the CIMA WAPP software which contains the WAPP software, the special Tcl/Tk interpreter used by CIMA and support libraries. ... All CIMA software components recognize the following general options that are part of the CIMA version selection system: . ... The select_cima script can be used to set up a default version. ...

... The Network Time Protocol (NTP) is used to synchronize the time of a computer client or server to another server or reference time source, such as a radio or satellite receiver or modem. ... Information on the NTP architecture, protocol and algorithms can be found in the Further Information and Bibliography page. The Building and Installing the Distribution page presents an overview of the procedures for compiling the distribution and installing it on a typical client or server. ...

... Big ellipse: the region of the photometric analysis Smaller ellipses: the adopted inner boundaries of the Main Body and the C component Small circles: diffuse background objects, manually selected and removed from the photometry Uncleaned CMDs [V-I, I] of I Zw 18, obtained using Aloisi et al. (left) and Izotov & Thuan (right) datasets. ... Where is the 'halo'? Blue compact dwarf galaxy SBS 1415+435 Hubble Space Telescope / Advanced Camera for Surveys NASA, ESA A. Aloisi (STScI, ESA) et al. ...

... In this first example, we allow an object to fall onto a small radar unit . The resulting Time-Frequency distribution is shown as a contour plot in Fig. 8 (a). Figure: FIGURE GOES SOMEWHERE IN THIS GENERAL VICINITY . ... Its density plot appears as an image in Fig. ... The response has a very high peak, as evidenced from Fig. ...

Peremennye Zvezdy", . ... Star Name: . GSC 3710-00312, USNO-A2.0 1425-04252279 . ... Variability type: . ... USNO-A2.0 1425-04252279 is located at the distance of 15?.7 from the X-ray source 1RXS J031707.9+572942, which is larger than the position error of the source (12?), but its hardness ratio HR1 = 0.03 0.29, typical of chromospherically active stars, and its character of variability allow us to assume that the star is related to the X-ray source. ... Eclipsing variability . Sine wave 1 . ...

... Minute Values of Geomagnetic Field Components . ... AA 1868 - Present (3 hourly and daily) (monthly) (yearly) (Lists and histograms of geomagnetic disturbance and Solar Sunspots) KP_AP 1932 - Present (3 hourly and daily) (Lists and histograms of geomagnetic disturbance and Solar Sunspots) AE_HV 1957-75, 78-88 (hourly) AE_MIN 1978-881-6;198903;1990-94 (minute) DST 1957 - Present (hourly) PC 1975 - Present (15-minute) AMANAS 1959 - Present (3 hourly and daily) KMKNKS 1983 - Present (3 hourly) . ...

. Merging cluster DLSCL J0916.2+2951 and its three matter components. Overlaid on the Hubble Space Telescope (HST) color image of the galaxies is the total mass distribution (blue) based on WL analysis of the HST images and the cluster gas distribution (red) based on Chandra X-ray observations. The bulk of the collisional gas is located between the two collisionless galaxy and mass concentrations, indicative of a dissociative merger.

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: . ...

Since the first stars and then galaxies formed the Universe has been an immense factory converting neutral gas into stellar material. ... In this seminar I will discuss recent results from the Galaxy And Mass Assembly (GAMA) survey, probing the assembly of stellar mass though both in-situ star formation (as traced by multiple SFR indicators) and interactions (both mergers and interaction induced star-formation) - in galaxies spanning ~4 decades in stellar mass. ...

... Public . Science . ... Science Users Information Science Software ESO-MIDAS jump to navigation jump to content . ... Publications with ESO Data . ... ESO-MIDAS . ... The short statement of the GNU license is included in every MIDAS file; the full text is included as a separate file in the ESO-MIDAS Release. ... Manual pages,installation guides and other documentation are generally released together with the source code and can also be obtained from the ESO-MIDAS ftp account (see below). ...

Last time we saw that flat rotation curves for galaxies, when measured in galaxies with extended gas distributions, provides unambiguous data that shows the mass distribution is dominated by an unseen, spherical halo. ... Perhaps only galaxies with extended dark matter halos are capable of retaining large gaseous extents? . ... Clusters of Galaxies: . ... The case of the Cancer cluster: . ... Below is the velocity distribution of galaxies in the Cancer cluster: . ... What's going on in Cancer? ...