Terms: Radio Continuum (308,000), radio sky (277,000), radio sky survey (311), radio sky surveys (241), continuum signal (913), Solar F10.7 flux (224), radio continuum surveys (694), continuum surveys (2,280), continuum survey (14,800), electromagnetic skies (36), electromagnetic sky (185),
Terms: galactic center (938,000), galactic center images (103), galactic cosmic radiation (21,200), radio loud (161,000), radio loud plasma (18), strong radio sources (2,270),
Astro2010: The Astronomy and Astrophysics Decadal Survey - What is the Physics of Pulsar Radio Emission?
Solar and Heliospheric Physics with Low Frequency Radio Arrays
Justin C. Kasper (Harvard-Smithsonian Center for Astrophysics) - Fluctuations in the total electron column density (TEC) in ionosphere distort the radio wavefront from the celestial sources. This distortion is time and direction dependent and can change from antenna to antenna if the antenna separation approaches or exceeds the ionospheric Fried length scale. If uncorrected, these distortions lead to an impact much like the scintillation of stellar images due to Earth’s atmosphere, and lead to blurred images. The recent advances in low frequency radio imaging are the analog of adaptive optics systems for large optical telescopes, which undo the ionospheric distortion in real time allowing one to reap the benefits of higher resolution (longer baselines for the case of radio) and higher sensitivity (larger collecting area and increased integration time). Even though the problem of ionospheric de-distortion could be mathematically well posed, it required computational power which was far beyond what was available then. In the 1990s a new ionospheric correction capability resembling adaptive optics was finally demonstrated with the 74 MHz extension of the VLA, prompting a resurgence in low frequency arrays (Cohen et al. 2006). Essentially, with sufficient sensitivity (or collecting area), bright sources in the field of view are monitored and their refraction due to ionospheric irregularities is measured. Refraction across the entire field of view is then determined by interpolating between the bright calibrator sources.
Terms: low frequency radio imaging (34), ionospheric de-distortion (1), ionospheric scintillation (20,900), interstellar scintillation (12,400), radio scintillation (1,570), radio twinkling (228), interplanetary scintillation (16,100), inter-planetary scintillation (42), radio variability (9,490),
Terms: plasma propagation (1,480), waves in plasmas (26,200), trans-ionospheric (2,500), plasma diagnostics (172,000),
Terms: intraday polarization (52), intraday variability (8,640),
Interstellar scintillation and PKS 1257-326Boolean: ionosphere +scintillation +adaptive (2,940),
Planetary Low Frequency Radio Astronomy with Large Ground Based Instruments
Terms: radio universe (60,400), radio sources (516,000), plasmas in the universe (496), interstellar plasmas (520), remote radio sources (32), cosmic microwave background (1,260,000), radio surveys (80,800), radio galaxies (231,000), strongest radio sources (398), kelvin/beam (106), mjy/beam (37,800), millijansky/beam (1), detectable radio sources (31), large radio surveys (168), pulsars (1,940,000), pulsar surveys (7,160), pulsar database (783), list of pulsars (303),
Terms: Mileura widefield array (1,260), Westerbork Northern Sky Survey (1,320), Molonglo Sky Survey (910), Faint Images of the Radio Sky (7,060), NRAO VLA (41,100), Allen Telescope Array (189,000), Murchison Wide-field Array (265), nancay decameter array (222), lofar (413,000),
Terms: kJy (643,000), kilojansky (18), pulsar subpulses (10),
Detection of crab giant pulses using the Mileura widefield array low frequency demonstrator field prototype system - detection of giant pulses from the Crab Nebula pulsar at a frequency of 200 MHz, our simple equipment is capable of detecting pulses that are brighter than 9 kJy in amplitude. The brightest giant pulse detected in our data has a peak amplitude of 50 kJy, and the implied brightness temperature is 1031.6 K.
Boolean: continuum +pulsars (87,800), "continuum emission" +pulsar (12,200), "radio signatures" +stars (665), "radio signatures" +extragalactic (68), "408 mhz" +sky +survey (5,220), "giant pulses" +crab (2,060),
The History of Radio Continuum Surveys
Very large radio surveys of the sky
Westerbork Northern Sky Survey
Radio Astronomy Laboratory, Univ. of Cal., Berkeley - CASPER - Center for Astronomy Signal Processing and Electronics Research
The John R Smith Sky Survey at 408 MHz - A radio sky survey consists of mapping the distribution of various properties of radio emission over the sky. These properties can include: intensity, polarization, spectrum, and perhaps time variability.
Multi-Beam Receiver Promises New Vistas for SETI Research - Allen Telescope Array
Terms: brightness temperature (345,000), mean brightness temperature (635), polarization in radio astronomy (8), stokes parameters (77,300), vertically polarized (156,000), horizontal polarization (148,000), radiometric observations (13,100), brightness distribution (90,400),
Terms: very large array (733,000), compact array (110,000),
Terms: jy/beam (41,700), interstellar extinction calculator (2), galactic reddening (8,920), extinction solver (130), extinction coefficients (179,000),
Terms: sz effect (24,800), thermal sz effect (903), kinematic sz effect (280), polarization sz effect (5), sz survey (839), Atacama Cosmology Telescope (7,650),
Terms: inverse compton (96,000), sunyaev zeldovich (52,500), sunyaev zel'dovich (64,500),
Sky map of velocity, brightness temperature profiles
Observational Issues in Radiometric and Interferometric Detection and Analysis of the SZ Effects - M. Birkinshaw & K. Lancaster - contents
NASA/IPAC Extragalactic Database
The Extragalactic Distance Database (EDD)
Extragalactic distance database
Sunyaev-Zel'dovich effect - Atacama Cosmology Telescope -
Two Micron All Sky Survey - all sky images
Terms: extragalactic (2,160,000), extragalactic database (489,000), high redshift (436,000), redshift independent (1,410), extragalactic distance (40,700), extragalactic distance database (67), redshift survey (149,000), galaxies (47,600,000), galaxy catalog (33,700), two micron all sky survey (79,100), 2mass all sky catalogs (32),
Wikipedia - Jansky, To calculate the flux density in janskys, the total power detected (in watts) is divided by the receiver collecting area (in square meters), divided by the detector bandwidth (in hertz), then multiplied by 10^26. Jy=10^-26 W/m2*hz
Boolean: "brightness distribution" +"of the sky" (8,130), "flux density" +jy +mhz (44,300), "brightness temperature" +sky +survey (21,300), "brightness temperature" +mk (9,630), "galactic center" +temperature (134,000),
Terms: galactic all sky survey (569), all sky survey (285,000), all sky surveys (17,500),
A Synthesis Map of the Sky at 34.5 MHz
The Discovery of the Radio Source Sagittarius A (Sgr A)
FTP directory /STP/SOLAR_DATA/SOLAR_RADIO - including second data
