HI line flux (flux corresponding to the area under the 21-cm line profile) is generally expressed in converted in magnitude m21 according to the formula adopted in RC3: m21 = -2.5 log f + 17.40 where f is the area of the 21-cm line profile expressed in Jy*km/s (the constant is 16.6 if the flux is in 10**-22 W/m**2). Non-detections (or upper limits) are not stored in the database, therefore galaxies with no HI measurements available may either be too faint or not have been observed. ... HyperLeda . ...

Next: Program use Up: Description of program searchdup Previous: Description of program searchdup . Parameter input is done with a graphic user interface. ... Input file: Name of the input catalog file. It has to be formatted, one record per source/observation, according to the format used in the Arcetri observations and source archives. ... Minimum number of observations per source Source with less than this number of independent observations are not included in the output file . ...

... Observational Zoo of Binaries with Compact Stars . Evolutionary Scenarios of Binary Systems . ... Evolution of Magnetic Rotators . ... Mixing types of E-P-A binary systems with non-zero orbital . ... Binary Pulsar Diversity and High Neutron Star Birth Velocity . ... Ejectors in Massive Binary Systems . ... Other Candidates for Ejecting Stars in Binary Systems . ... Cosmic Rays and Evolution of Binary . ... Sky in Gravitational Waves . ... Gravitational Waves from Coalescing Compact Binary Stars . ...

Next: HST Paper Products: A New Way to Look at HST Data . ... After providing on-the-fly re-calibration of HST data to archive users, ST-ECF has embarked on a new project aiming at grouping, cosmic ray cleaning and drizzling images taken by most HST instruments. ... The production of the missing jitter files combined with the extraction of additional engineering parameters will greatly enhance the homogeneity and the scientific value of the entire archive. ... 1995, HST Data Handbook, STScI, 107 . ...

... Meta Index / Home Page This section documents the parameters recognized by this task (if any). ... The name of the FITS dataset+table which contains the input source list. ... Switch which specifies whether the source list (after filtering with expression ) should be truncated at some maximum number, specified by parameter ncut . ... This parameter is read by the task if withlabels =`yes' and controls how source labels are assigned. ... This parameter is read if outfilestyle =`prefix'. outfile . ...

2014 May version . ... Green D. A., 2014 , Bulletin of the Astronomical Society of India, 42 , 47-58. ( .pdf , or arXiv.org:1409.0637 ) If you make use of the detailed version of the catalogue, then plaese also cite: . Green D. A., 2014, `A Catalogue of Galactic Supernova Remnants (2014 May version)' , Cavendish Laboratory, Cambridge, United Kingdom (available at "http://www.mrao.cam.ac.uk/surveys/snrs/" ). ... Copyright D. A. Green 2014. 25872nd access to this version of the catalogue. ...

Find Similar Abstracts (with default settings below ) . ... Also-Read Articles . ... Parameters of the 41 Dra system components . ... 00/2001 . ... Stars: Binaries, Binaries: Fundamental Parameters, Binaries: Individual . ... 61B Based on spectral and speckle-interferometric observations of the system 41 Dra, model atmosphere parameters of the system components have been derived: component Aa - T eff = 6500K, lg g = 3.99, R = 1.87 R solar , component Ab - T eff = 6500K, lg g = 4.11, R = 1.61 R solar . ...

Orbital data : INTERBALL AZ GSE and GSM cartesian coordinates, GSE cartesian velocity (once per 10 minutes). ... Magnetic field data from IMAP experiment. Magnetic fileld absolute value and magnetic field index (the difference between absolute value and model value), status flag. ... Counts of H+ and O+ ions are accumulated during one spin period by detectors D6 (antisunward looking), D8 (spin plane), D10 (sunward looking) of TRICS2 subsystem (1.0-30 keV). ... TRICS1, TRICS2, TRICS3 subsystems: . ...

... The overall globular cluster population is divided by gap in the metallicity function at [Fe/H]=-1.0 into two discrete groups with well-defined maxima at [Fe/H]=-1.60?0.03 dex, and -0.60?0.04 dex. ...