The Fourth Uhuru (4U) Catalog lists 339 X-ray sources that were observed with the Uhuru (SAS A) X-ray observatory. It contains positional information in the form of 90% confidence level error boxes, 2-6 keV intensities, possible optical and radio counterparts, and alternative names for sources observed in earlier compilations. The major classes of identified objects include binary stellar systems, supernova remnants, Seyfert galaxies, clusters of galaxies, and possibly the new class of superclusters of galaxies. The Uhuru satellite was a scanning X-ray instrument with a narrow (1 by 10 degree FWFM) and a wide (10 by 10 degree FWFM) collimator (cf. Giacconi et al. 1971, ApJ, 165, L27). Typically, the scan rate was 0.5 degree/second, with the spin axis in one position for roughly one day. During the interval for which the spin axis was fixed, repeated scans were made of the same 10 by 360 degrees band of the sky. For this catalog, the individual scans were superposed using aspect data from an orthogonally mounted triad of magnetometers and a Sun sensor onboard the spacecraft, supplemented by observations of well-located X-ray sources. The observations employed in producing this catalog were obtained over a total of 429 days between 1970 December 12 and 1973 March 18, apart from a gap between 1972 July and December when the spacecraft's transmitter was operating improperly. This online catalog was created by the HEASARC in March 2003 based on a table obtained originally from the ADC website (<a href="https://heasarc.gsfc.nasa.gov/FTP/heasarc/dbase/misc_files/uhuru4/4u.dat">https://heasarc.gsfc.nasa.gov/FTP/heasarc/dbase/misc_files/uhuru4/4u.dat</a>), which was modified by the HEASARC to include some parameters that were in the published catalog (Table 1 in the reference) but were not in the ADC table. The HEASARC made a small number of other changes and corrections to the table which are listed in the HEASARC_Implementation section of this help. Notice that the ADC table itself differs in a number of respects from the published Table 1, e.g., the comments are sometimes abbreviated and/or different, some of the names are slightly different (usually by one digit in the RA minutes part), and three of the entries have differing names and positions. This is a service provided by NASA HEASARC .
We present a photometric catalog of 2244 objects detected by the Ultraviolet Imaging Telescope in the near-ultraviolet (NUV; 1650A<lambda<2900A) during the Astro-1 Space Shuttle mission. Sources in the catalog are as faint as m_nuv~18.8, or f_nuv~1.1x10^-16ergs/s/cm^2/A, but the survey is not complete to this level. Optical catalogs were used to cross identify sources and derive NUV-V colors. A majority of the objects (88%) do indeed have proposed optical identifications from catalogs, and most are stars. Our purpose in creating the catalog is to form a database useful for identifying very blue objects and performing Galactic UV stellar population studies.
We present a detailed analysis of a sample of radio-detected quasars, obtained by matching together objects from the FIRST (<VIII/71>) survey and the 2dF Quasar Redshift Survey (2dF, <VII/223>). The data set consists of 113 sources, spanning a redshift range 0.35<~z<~2.2, with optical magnitudes 18.25<=bj<=20.85 and radio fluxes S_1.4GHz_>=1mJy. These objects exhibit properties such as redshift and colour distribution in full agreement with those derived for the whole quasar population, suggesting that the mechanism(s) controlling the birth and lifetime of quasars are independent of their level of radio emission. The long-debated question of the radio-loud/radio quiet (RL/RQ) dichotomy is then investigated for the combined FIRST-2dF and FIRST-LBQS (Large Bright Quasar Survey) samples, as they present similar selection criteria.
The UKIDSS Galactic Plane Survey (GPS) is one of the five near infrared Public Legacy Surveys that are being undertaken by the UKIDSS consortium, using the Wide Field Camera on the United Kingdom Infrared Telescope. It is surveying 1868 deg^2^ of the northern and equatorial Galactic plane at Galactic latitudes -5{deg}<b<5{deg} in the J, H and K filters and a ~300 deg^2^ area of the Taurus-Auriga-Perseus molecular cloud complex in these three filters and the 2.12{mu}m (1-0)S(1)H_2_ filter. It will provide data on ~ 3x10^9^ sources. The survey use the Wide Field Camera (WFCAM, see Casali et al. 2007A&A...467..777C) on the United Kingdom Infrared Telescope (UKIRT). The typical 90% completeness limits in uncrowded fields are K=18.0, H=18.75, J=19.5, with uncertainties of about 0.2mag.
The UKIRT Infrared Deep Sky Survey (UKIDSS) is a large-scale near-IR survey which aim is to cover 7500 square degrees of the Northern sky. The survey is carried out using the Wide Field Camera (WFCAM), with a field of view of 0.21 square degrees, mounted on the 3.8m United Kingdom Infra-red Telescope (UKIRT) in Hawaii. The Large Area Survey (LAS) covers an area of 4000 square degrees in high Galactic latitudes (extragalactic) in the four bands Y(1.0um) J(1.2um) H(1.6um) and K(2.2um) to a depth of K = 18.4. Details of the survey can be found in the in the paper by Lawrence et al. (2007MNRAS.379.1599L)
The UKIRT Infrared Deep Sky Survey (UKIDSS) is a large-scale near-IR survey which aim is to cover 7500 square degrees of the Northern sky. The survey is carried out using the Wide Field Camera (WFCAM), with a field of view of 0.21 square degrees, mounted on the 3.8m United Kingdom Infra-red Telescope (UKIRT) in Hawaii. The project comprises five surveys (LAS, GCS, DXS, GPS and UDS). The Large Area Survey (LAS) covers an area of 4000 square degrees in high Galactic latitudes (extragalactic) in the four bands Y(1.0um) J(1.2um) H(1.6um) and K(2.2um) to a depth of K=18.4. This release 9 includes proper motions for a fraction (~1/6) of the sources. The Galactic Clusters Survey (GCS) aims to survey ten large open star clusters and star formation associations, covering a total of 1067 square degrees in the five bands Z (0.9um), Y(1.0um) J(1.2um) H(1.6um) and K(2.2um), plus a second pass in K for proper motions, to a depth of Z=20.4, Y=20.3, J=19.5, H=18.6, K=18.6. This release 9 includes proper motions for a fraction (~1/4) of the sources. The Deep Extragalactic Survey (DXS) aims to map 35 square degrees of sky to a 5-{sigma} point-source sensitivity of J=22.3 and K=20.8 in four carefully selected, multi-wavelength survey areas. The central regions of each field will also be mapped to H=21.8. The primary aim of the survey is to produce a photometric galaxy sample at a redshift of 1-2, within a volume comparable to that of the SDSS, selected in the same passband (rest frame optical). Details of the surveys can be found in the in the paper by Lawrence et al. (2007MNRAS.379.1599L), and at the UKIDSS Surveys site (http://www.ukidss.org/surveys/surveys.html). The data described here represent a subset of the UKIDSS data, limited to the public data and most representative columns. In the "Byte-by-byte Description" below the original names of the columns are given as bracketed names.
The UKIRT Infrared Deep Sky Survey (UKIDSS) is a large-scale near-IR survey which aim is to cover 7500 square degrees of the Northern sky. The survey is carried out using the Wide Field Camera (WFCAM), with a field of view of 0.21 square degrees, mounted on the 3.8m United Kingdom Infra-red Telescope (UKIRT) in Hawaii. The project comprises five surveys (LAS, GCS, DXS, GPS and UDS). The Large Area Survey (LAS) covers an area of 4000 square degrees in high Galactic latitudes (extragalactic) in the four bands Y(1.0um) J(1.2um) H(1.6um) and K(2.2um) to a depth of K=18.4. The Galactic Clusters Survey (GCS) aims to survey ten large open star clusters and star formation associations, covering a total of 1067 square degrees in the five bands Z (0.9um), Y(1.0um) J(1.2um) H(1.6um) and K(2.2um), plus a second pass in K for proper motions, to a depth of Z=20.4, Y=20.3, J=19.5, H=18.6, K=18.6. The Deep Extragalactic Survey (DXS) aims to map 35 square degrees of sky to a 5-{sigma} point-source sensitivity of J=22.3 and K=20.8 in four carefully selected, multi-wavelength survey areas. The central regions of each field will also be mapped to H=21.8. The primary aim of the survey is to produce a photometric galaxy sample at a redshift of 1-2, within a volume comparable to that of the SDSS, selected in the same passband (rest frame optical). Details of the surveys can be found in the in the paper by Lawrence et al. (2007MNRAS.379.1599L), and at the UKIDSS Surveys site (http://www.ukidss.org/surveys/surveys.html). The data described here represent a subset of the UKIDSS data, limited to the public data and most representative columns. In the "Byte-by-byte Description" below the original names of the columns are given as bracketed names.
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