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375 results for “compactness”
Canadian Galactic Plane Survey (CGPS) 1420-MHz Compact Source Catalog
This table contains a catalog of compact sources of radio emission at 1420 MHz in the northern Galactic plane from the Canadian Galactic Plane Survey (CGPS). The catalog contains 72,758 compact sources with an angular size less than 3 arcminutes within the Galactic longitude range 52 < l<sub>II</sub> < 192 degrees down to a 5-sigma detection level of ~1.2 mJy. Linear polarization properties are included for 12,368 sources with signals greater than 4 x sigma<sub>QU</sub> in the CGPS Stokes Q and U images at the position of the total intensity peak. In the reference paper, the authors compare the CGPS flux densities with the catalogued flux densities in the Northern VLA Sky Survey (NVSS) catalog for 10,897 isolated unresolved sources with CGPS flux density greater than 4 mJy in order to search for sources that show variable flux density on timescales of several years. They identify 146 candidate variables that exhibit high fractional variations between the two surveys. In addition, they identify 13 candidate transient sources that have CGPS flux density above 10 mJy but that are not detected in the NVSS. In the CGPS, the Synthesis Telescope at the Dominion Radio Astrophysical Observatory (the DRAO ST) provided arcminute-resolution images of the radio continuum and atomic-hydrogen line emission of the northern Galactic Plane. The CGPS DRAO radio continuum observations provided images of Stokes I, Q, and U in four 7.5-MHz sub-bands spanning 35 MHz, centered on 1420 MHz. The observations were carried out in three phases beginning in 1995 and ending in 2009. The sky coverage of each phase and the observing dates are listed in Table 1 of the reference paper. The Galactic plane was covered with a width in Galactic latitude of 9 degrees, centered at b<sub>II</sub> = 1 degree to accommodate the warp of the Galactic disk. The longitude coverage was constrained by the southern Declination limit of ~20 degrees, the range that could be effectively imaged by a linear east-west synthesis telescope array. The Phase II observations included an extension to higher latitudes (b<sub>II</sub> = 17.5 degrees) over a restricted range of longitude. In this table, we present the CGPS 1420-MHz compact source catalog covering 1,464 square degrees and spanning a range of 140 degrees of Galactic longitude between 52 and 192 degrees. This table was created by the HEASARC in June 2017 based upon a machine-readable version of Table 2 from the reference paper that was obtained from the AJ web site. This is a service provided by NASA HEASARC .
Selected Hickson Compact Groups Chandra X-Ray Point Source Catalog
This table contains the Chandra X-ray point source catalogs for 9 Hickson Compact Groups (HCGs, 37 galaxies) at distances of 34 to 89 Mpc. The authors perform detailed X-ray point source detection and photometry and interpret the point source population by means of simulated hardness ratios. They thus estimate X-ray luminosities (L<sub>X</sub>) for all sources, most of which are too weak for reliable spectral fitting. For all sources, they provide counts, count rates, power-law indices (Gamma), hardness ratios, and L<sub>X</sub>, in the full (0.5-8.0 keV), soft (0.5-2.0 keV) and hard (2-8 keV) bands. In their paper, the authors use optical emission-line ratios from the literature to re-classify 24 galaxies as star-forming, accreting onto a supermassive black hole (AGNs), transition objects, or low-ionization nuclear emission regions. Two-thirds of their galaxies have nuclear X-ray sources with Swift/UVOT counterparts. Two nuclei have full-band X-ray luminosities >= 10<sup>42</sup> erg s<sup>-1</sup>, are strong multi-wavelength AGNs, and follow the known alpha<sub>OX</sub> - nu L_nu(near-UV)_ correlation for strong AGNs. Otherwise, most nuclei are X-ray faint, consistent with either a low-luminosity AGN or a nuclear X-ray binary population, and fall into the 'non-AGN' locus in alpha<sub>OX</sub> - nu L_nu(near-UV)_ space, which also hosts other normal galaxies. Each group was observed at the aim point of the back-illuminated S3 CCD of Chandra's Advanced CCD Imaging Spectrometer (ACIS), with the exception of HCG 90, which was observed with the ACIS-I array. The details of the 9 Chandra observations analyzed herein are given in Table 1 of the reference paper. The full details of the X-ray analysis and point source detection procedures are given in Section 3 of the reference paper. This table was created by the HEASARC in June 2014 based on electronic versions of Tables 2 and 3 from the reference paper which were obtained from the ApJS web site. Some of the values for the name parameter in the HEASARC's implementation of this table were corrected in April 2018. This is a service provided by NASA HEASARC .
Molonglo Galactic Plane Survey 2nd Epoch Compact Source Catalog
This table contains the Molonglo Galactic Plane Survey 2nd Epoch (MGPS-2) Compact Source Catalog. The MGPS-2 was carried out with the Molonglo Observatory Synthesis Telescope (MOST) at a frequency of 843 MHz and with a restoring beam of 45" x 45" cosec |(delta)|, where delta is the declination, making it the highest resolution large-scale radio survey of the southern Galactic plane to date. It covers the range |b| < 10 degrees and 245 < l < 365 degrees, where l and b are the Galactic longitude and latitude, and is the Galactic counterpart to the SUMSS (<a href="https://cdsarc.cds.unistra.fr/ftp/cats/VIII/81">CDS Cat. VIII/81</a>) Catalog which covers that portion of the southern sky with delta < -30 degrees, |b| > 10 degrees. This version of the catalog (15-Aug-2007) consists of 48850 compact sources, made by fitting elliptical Gaussians in the MGPS-2 mosaics to a limiting peak brightness of 10 mJy/beam. The authors used a custom method (described in the associated reference publication) to remove extended sources from the catalog. Positions in the catalog are accurate to 1" - 2". The authors have carried out an analysis of the compact source density across the Galactic plane and find that the source density is not statistically higher than the density expected from the extragalactic source density alone. See <a href="http://www.astrop.physics.usyd.edu.au/mosaics">http://www.astrop.physics.usyd.edu.au/mosaics</a> for access to the MGPS-2 mosaic images. This HEASARC table was created in January 2008 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/382/382">CDS catalog J/MNRAS/382/382</a> file mgpscat.dat. This is a service provided by NASA HEASARC .
Planck Catalog of Compact Sources 100GHz Catalog
The Planck Catalogue of Compact Sources (PCCS) is a sample of reliable sources, both Galactic and extragalactic, extracted directly from the Planck nominal maps. The first public version of the PCCS, a component of Planck Data Release 1, is derived from the data acquired by Planck between August 13 2009 and November 26 2010. The PCCS consists of nine lists of sources, extracted independently from each of Planck's nine frequency channels. The source lists contain 24 columns per source at the LFI and HFI bands. The 857 GHz source list has six additional columns which give the flux densities and flux density uncertainties at the three adjacent lower frequencies: 217, 353, and 545 GHz.
New Catalog of Compact 20cm Sources in the Galactic Plane
This table contains the New Catalog of Compact Radio (20-cm) Sources in the Galactic Plane of White et al. (2005). Archival data were combined with more recent observations of the Galactic plane using the Very Large Array to create two new catalogs of compact centimetric radio sources. The 20-cm source catalog contained here covers a longitude range from -20 to +120 degrees in Galactic longitude l; the latitude coverage varies from b = +/- 0.8 to +/- 2.7 degrees. The total survey area is about 331 square degrees; coverage is 90% complete at a flux density threshold of about 14 mJy, and over 5000 sources are recorded. The 6-cm catalog (also available in the HEASARC Browse system as the table WBHGP6CM) covers 43 square degrees in the region -10 degrees < l <42 degrees, |b| < 0.4 degrees to a 90% completeness threshold of 2.9 mJy; over 2700 sources are found. Both surveys have an angular resolution of about 6". These catalogs provide a 30% (at 20 cm) to 50% (at 6 cm) increase in the number of high-reliability compact sources in the Galactic plane, as well as greatly improved astrometry, uniformity, and reliability; they should prove useful for comparison with new mid- and far-infrared surveys of the Milky Way. The images from which this catalog was constructed are available at the MAGPIS web site, <a href="http://third.ucllnl.org/gps">http://third.ucllnl.org/gps</a> This table was created by the HEASARC in July 2006 based on the combination of CDS tables J/AJ/130/586 table3.dat and table4.dat. This is a service provided by NASA HEASARC .
M 108 Chandra X-Ray Compact Source Catalog
This table contains a list of discrete sources found in a 60-ks Chandra ACIS-S observation of the isolated edge-on spiral galaxy NGC 3556 (M108). In the reference paper in which the authors present this table, they also give a multiwavelength analysis of the various discrete X-ray sources and of the diffuse X-ray features. Among 33 discrete X-ray sources detected within the I<sub>B</sub> = 25 mag arcsec<sup>-2</sup> isophotal ellipse of the galaxy, the authors identify a candidate for the galactic nucleus, an ultraluminous X-ray source that might be an accreting intermediate-mass black hole, a possible X-ray binary with a radio counterpart, and two radio-bright giant H II regions. They also detect large amounts of extraplanar diffuse X-ray emission, which extend about 10 kpc radially in the disk and >~4 kpc away from the galactic plane. The diffuse X-ray emission exhibits significant substructures, possibly representing various blown-out superbubbles or chimneys of hot gas heated in massive star-forming regions. This Chandra observation of NGC 3556 (observation ID 2025) was taken between 2001 September 8 and 9 for an exposure of 60 ks. The ACIS-S instrument was at the focal plane of the telescope. This table was created by the HEASARC in August 2015 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/598/969">CDS Catalog J/ApJ/598/969</a> file table2.dat. This is a service provided by NASA HEASARC .
Planck Catalog of Compact Sources 70GHz Catalog
The Planck Catalogue of Compact Sources (PCCS) is a sample of reliable sources, both Galactic and extragalactic, extracted directly from the Planck nominal maps. The first public version of the PCCS, a component of Planck Data Release 1, is derived from the data acquired by Planck between August 13 2009 and November 26 2010. The PCCS consists of nine lists of sources, extracted independently from each of Planck's nine frequency channels. The source lists contain 24 columns per source at the LFI and HFI bands. The 857 GHz source list has six additional columns which give the flux densities and flux density uncertainties at the three adjacent lower frequencies: 217, 353, and 545 GHz.
Sgr A* Region Compact Radio Source Catalog
Recent broad-band 34- and 44-GHz radio continuum observations of the Galactic center have revealed 41 massive stars identified with near-IR (NIR) counterparts, as well as 44 proplyd candidates within 30 arcseconds of Sgr A*. Radio observations obtained in 2011 and 2014 have been used to derive proper motions of eight young stars near Sgr A*. The accuracy of proper motion estimates based on NIR observations by Lu et al. (2009, ApJ, 690, 1463) and Paumard et al. (2006, ApJ, 643, 1011) have been investigated by using their proper motions to predict the 2014 epoch positions of NIR stars and comparing the predicted positions with those of radio counterparts in the 2014 radio observations. Predicted positions from Lu et al. show an rms scatter of 6 milliarcseconds (mas) relative to the radio positions, while those from Paumard et al. show rms residuals of 20 mas. In the reference paper, the authors also determine the mass-loss rates of 11 radio stars, finding rates that are on average ~2 times smaller than those determined from model atmosphere calculations and NIR data. Clumpiness of ionized winds would reduce the mass loss rate of WR and O stars by additional factors of 3 and 10, respectively. One important implication of this is a reduction in the expected mass accretion rate onto Sgr A* from stellar winds by nearly an order of magnitude to a value of a few x 10<sup>-7</sup> solar masses per year. The authors carried out A-array observations of the Galactic center region (VLA program 14A-232) in the Ka (9 mm, 34.5 GHz) band on 2014 March 9 in which they detected 318 compact radio sources within 30" of Sgr A*. The authors searched for NIR counterparts to these compact radio sources using high-angular resolution AOs-assisted imaging observations acquired with the VLT/NACO. A K<sub>s</sub>-band (central wavelength 2.18 micron) image was obtained in a rectangular dither pattern on 2012 September 12. L'-band (3.8 micron) observations were obtained during various observing runs between 2012 June and September. The authors found that 45 of the compact radio sources had stellar counterparts in the K<sub>s</sub> and L' bands. This table contains the details of the 318 compact radio sources detected at 34.5 GHz and their NIR counterparts. This table was created by the HEASARC in November 2016 based on CDS table J/ApJ/809/10, file table6.dat. This is a service provided by NASA HEASARC .
Planck Catalog of 100-GHz Compact Sources (PCCS) Release 2
Planck was a European Space Agency (ESA) mission, with significant contributions from the National Aeronautics and Space Agency (NASA). It was the third generation of space-based cosmic microwave background experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in orbit checkout, Planck initiated the First Light Survey on 12 August 2009. Planck then continuously measured the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 micron) with spatial resolutions ranging from about 33 to 5 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provided temperature and polarization information using radiometers which operated between 30 and 70 GHz. The High Frequency Instrument (HFI) used pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but did not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest Planck frequencies overlapped with WMAP, and the highest frequencies extended far into the submillimeter in order to improve separation between Galactic foregrounds and the cosmic microwave background (CMB). By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck provided an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Second Planck Catalogue of Compact Sources is a list of discrete objects detected in single-frequency maps from the full duration of the Planck mission and supersedes previous versions. It consists of compact sources, both Galactic and extragalactic, detected over the entire sky. Compact sources detected in the lower frequency channels are assigned to the PCCS2, while at higher frequencies they are assigned to one of two subcatalogs, the PCCS2 or PCCS2E, depending on their location on the sky. The first of these (PCCS2) covers most of the sky and allows the user to produce subsamples at higher reliabilities than the target 80% integral reliability of the catalog. The second (PCCS2E) contains sources detected in sky regions where the diffuse emission makes it difficult to quantify the reliability of the detections. Both the PCCS2 and PCCS2E include polarization measurements, in the form of polarized flux densities, or upper limits, and orientation angles for all seven polarization-sensitive Planck channels. The improved data-processing of the full-mission maps and their reduced noise levels allow the authors to increase the number of objects in the catalog, improving its completeness for the target 80% reliability as compared with the previous versions, the PCCS and the Early Release Compact Source Catalogue (ERCSC). The Low Frequency Instrument (LFI) Data Processing Center (DPC) produced the 30, 44, and 70 GHz maps after the completion of eight full surveys (spanning the period from 12 August 2009 to 3 August 2013). In addition, special LFI maps covering the period 1 April 2013 to 30 June 2013 were produced in order to compare the Planck flux-density scales with those of the Very Large Array and the Australia Telescope Compact Array, by performing simultaneous observations of a sample of sources over that period. The High Frequency Instrument (HFI) DPC produced the 100-, 143-, 217-, 353-, 545-, and 857-GHz maps after five full surveys (from 2009 August 12 to 2012 January 11). As in the PCCS, the PCCS2 provides four different measures of the flux density for each source. They are determined by the source detection algorithm (DETFLUX), aperture photometry (APERFLUX), point spread function fitting (PSFFLUX), and Gaussian fitting (GAUFLUX). Only the first is obtained from the filtered maps; the other measures are estimated from the full-sky maps at the positions of the sources. The source detection algorithm photometry, the aperture photometry, and the point spread function (PSF) fitting use the Planck band-average effective beams, calculated with FEBeCoP (Fast Effective Beam Convolution in Pixel space). Note that only the PSF fitting algorithm takes into account the variation of the PSF with position on the sky. The PCCS2 has been produced from the Planck full-mission maps (eight sky surveys in the LFI and five sky surveys in the HFI), and therefore supersedes the previous catalogs (for the PCCS only 1.5 surveys were analyzed). It also includes the latest calibration and beam information, and the authors have improved some of the algorithms used to measure the photometry of the sources. This table contains the PCCS2 subsample of the PCCS Public Release 2 table of sources detected at 100 GHz. One of the primary differences of this release of the PCCS from previous releases is the division of the six highest frequency catalogs into two subcatalogs, the PCCS2 a
WSRT Galactic Plane Compact 327-MHz Source Catalog
The Westerbork Synthesis Radio Telescope (WSRT) in the Netherlands has been used to survey the section of the galactic plane from +42 to +92 degrees Galactic Longitude l at a radio frequency of 327 MHz. Twenty-three overlapping synthesis fields were observed in the Galactic Latitude b band of |b| < 1.6 degrees. Each field was observed at two epochs, several years apart, to identify variable sources. Intensity data from the separate epochs were combined, and the resulting images mosaicked to produce a single image of the entire survey region. The sensitivity of the mosaic is typically a few mJy, corresponding to a detection level as low as 10 mJy/beam. The spatial resolution is 1' by 1' * cosec(Dec). The survey image provided the first high resolution view of the Galaxy at low radio frequencies, and included sections of the Sagittarius and Cygnus arms. These sections contain numerous extended features, among them supernova remnants, H II regions, "bubbles" of thermal emission, and large patches of amorphous galactic thermal emission. The inter-arm region is characterized by lower densities of extended features, but numerous discrete compact radio sources, most of which are background objects such as quasars and other types of active galactic nuclei. However, the resolution, sensitivity and low frequency of this survey make it ideal for detecting weak, non-thermal compact galactic sources, e.g. compact, low surface brightness SNRs and radio stars. Inspection of the survey image has produced a catalog of nearly 4000 discrete sources with sizes of less than about 3'. Gaussian model parameters for each compact source in the mosaicked images were obtained using the AIPS routine IMFIT. The background-removed intensity distribution of each source was fitted by a 2-dimensional Gaussian, parametrized by the source position, peak intensity, major and minor axes, and the position angle of the major axis. The catalog contains all sources having peak intensity > 5 times the rms noise level measured in the surrounding area of the image, and lists RA, Dec, flux density, and, if the source is resolved, the deconvolved major and minor axis and the position angle of the source. Sources were identified based on visual inspection of the images. In practice, a source had to have dimensions of less than a few arcminutes to be classified as a compact source. Most (85%) of the sources are either unresolved or only slightly resolved (major axis < 60"), but some sources have dimensions as large as 6'. A source was considered resolved if the area of its Gaussian model was greater than the area of the beam by more than 4 times its uncertainty. Approximately 15% of the sources are resolved, with dimensions of 1'- 3'. The spatial distribution of resolved sources shows concentrations toward the spiral arms and follows the warping of the Galactic disk over the length of the survey region, indicating that a sizable fraction is Galactic. In the reference paper, spectral indices are calculated for 1313 sources detected in other radio surveys at frequencies greater than 408 MHz. The resolved sources exhibit a bimodal spectral index distribution, with distinct non-thermal and thermal populations. Comparison with the IRAS Point Source Catalogue results in 118 identifications between WSRT and IRAS sources, which are listed in Table 1 of the reference paper. Most of these are thermal radio sources associated with compact Galactic objects such as H II regions and planetary nebulae. A search for variability among 2148 of the compact sources has resulted in 29 candidate low-frequency variable sources, which are listed in Table 2 of the reference paper. See the project website at <a href="http://www.ras.ucalgary.ca/wsrt_survey.html">http://www.ras.ucalgary.ca/wsrt_survey.html</a> for the WSRTGP images available in JPEG, PostScript, and FITS formats. This table was created by the HEASARC in February 2012 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/107/239">CDS Catalog J/ApJS/107/239</a> file wsrt.dat. This is a service provided by NASA HEASARC .
Planck Catalog of 545-GHz Compact Sources (PCCS) Release 2
Planck was a European Space Agency (ESA) mission, with significant contributions from the National Aeronautics and Space Agency (NASA). It was the third generation of space-based cosmic microwave background experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in orbit checkout, Planck initiated the First Light Survey on 12 August 2009. Planck then continuously measured the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 micron) with spatial resolutions ranging from about 33 to 5 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provided temperature and polarization information using radiometers which operated between 30 and 70 GHz. The High Frequency Instrument (HFI) used pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but did not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest Planck frequencies overlapped with WMAP, and the highest frequencies extended far into the submillimeter in order to improve separation between Galactic foregrounds and the cosmic microwave background (CMB). By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck provided an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Second Planck Catalogue of Compact Sources is a list of discrete objects detected in single-frequency maps from the full duration of the Planck mission and supersedes previous versions. It consists of compact sources, both Galactic and extragalactic, detected over the entire sky. Compact sources detected in the lower frequency channels are assigned to the PCCS2, while at higher frequencies they are assigned to one of two subcatalogs, the PCCS2 or PCCS2E, depending on their location on the sky. The first of these (PCCS2) covers most of the sky and allows the user to produce subsamples at higher reliabilities than the target 80% integral reliability of the catalog. The second (PCCS2E) contains sources detected in sky regions where the diffuse emission makes it difficult to quantify the reliability of the detections. Both the PCCS2 and PCCS2E include polarization measurements, in the form of polarized flux densities, or upper limits, and orientation angles for all seven polarization-sensitive Planck channels. The improved data-processing of the full-mission maps and their reduced noise levels allow the authors to increase the number of objects in the catalog, improving its completeness for the target 80% reliability as compared with the previous versions, the PCCS and the Early Release Compact Source Catalogue (ERCSC). The Low Frequency Instrument (LFI) Data Processing Center (DPC) produced the 30, 44, and 70 GHz maps after the completion of eight full surveys (spanning the period from 12 August 2009 to 3 August 2013). In addition, special LFI maps covering the period 1 April 2013 to 30 June 2013 were produced in order to compare the Planck flux-density scales with those of the Very Large Array and the Australia Telescope Compact Array, by performing simultaneous observations of a sample of sources over that period. The High Frequency Instrument (HFI) DPC produced the 100-, 143-, 217-, 353-, 545-, and 857-GHz maps after five full surveys (from 2009 August 12 to 2012 January 11). As in the PCCS, the PCCS2 provides four different measures of the flux density for each source. They are determined by the source detection algorithm (DETFLUX), aperture photometry (APERFLUX), point spread function fitting (PSFFLUX), and Gaussian fitting (GAUFLUX). Only the first is obtained from the filtered maps; the other measures are estimated from the full-sky maps at the positions of the sources. The source detection algorithm photometry, the aperture photometry, and the point spread function (PSF) fitting use the Planck band-average effective beams, calculated with FEBeCoP (Fast Effective Beam Convolution in Pixel space). Note that only the PSF fitting algorithm takes into account the variation of the PSF with position on the sky. The PCCS2 has been produced from the Planck full-mission maps (eight sky surveys in the LFI and five sky surveys in the HFI), and therefore supersedes the previous catalogs (for the PCCS only 1.5 surveys were analyzed). It also includes the latest calibration and beam information, and the authors have improved some of the algorithms used to measure the photometry of the sources. This table contains the PCCS Public Release 2 table of sources detected at 545 GHz. Where the HEASARC parameter names differ from those used in the original table, the original names are listed parenthetically in upper case at the end of the parameter description. This table
New Catalog of Compact 6cm Sources in the Galactic Plane
This table contains the New Catalog of Compact Radio (6-cm) Sources in the Galactic Plane of White et al. (2005). Archival data were combined with more recent observations of the Galactic plane using the Very Large Array to create two new catalogs of compact centimetric radio sources. The 20-cm source catalog (available in the HEASARC Browse system as the table WBHGP20CM) covers a longitude range from -20 to +120 degrees in Galactic longitude l; the latitude coverage varies from b = +/- 0.8 to +/- 2.7 degrees. The total survey area is about 331 square degrees; coverage is 90% complete at a flux density threshold of about 14 mJy, and over 5000 sources are recorded. The 6-cm catalog described here covers 43 square degrees in the region -10 degrees < l <42 degrees, |b| < 0.4 degrees to a 90% completeness threshold of 2.9 mJy; over 2700 sources are found. Both surveys have an angular resolution of about 6". These catalogs provide a 30% (at 20 cm) to 50% (at 6 cm) increase in the number of high-reliability compact sources in the Galactic plane, as well as greatly improved astrometry, uniformity, and reliability; they should prove useful for comparison with new mid- and far-infrared surveys of the Milky Way. The images from which this catalog was constructed are available at the MAGPIS web site, <a href="http://third.ucllnl.org/gps">http://third.ucllnl.org/gps</a> This table was created by the HEASARC in July 2006 based on the combination of CDS tables J/AJ/130/586 table5.dat and table6.dat. This is a service provided by NASA HEASARC .
Planck Catalog of Compact Sources 217GHz Catalog
The Planck Catalogue of Compact Sources (PCCS) is a sample of reliable sources, both Galactic and extragalactic, extracted directly from the Planck nominal maps. The first public version of the PCCS, a component of Planck Data Release 1, is derived from the data acquired by Planck between August 13 2009 and November 26 2010. The PCCS consists of nine lists of sources, extracted independently from each of Planck's nine frequency channels. The source lists contain 24 columns per source at the LFI and HFI bands. The 857 GHz source list has six additional columns which give the flux densities and flux density uncertainties at the three adjacent lower frequencies: 217, 353, and 545 GHz.
MGN ALTIMETER EXPERIMENT DATA RECORD ON COMPACT DISK
This data set contains the Magellan ALT-EDR (Altimeter Experiment Data Record) archive products. It also contains documentation files which describe the ALT-EDRs. Each ALT-EDR data directory contains the raw altimeter data returned from one orbit and the ancillary files necessary to understand the data. The ALT-EDR products archived on this volume are the exact products released by the Magellan Project.
Shakhabazian (Shk) Compact Groups of Galaxies: Individual Galaxies Data
The largest survey of compact galaxy groups was published by Shakhbazian et al. (the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VII/89">CDS catalog VII/89</a>, implemented by the HEASARC as the SHK database table). This present catalog provides accurate positions of the individual galaxies in the groups; photometric properties of the Southern sky (delta not greater than +2.5 degrees) are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. This catalog contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: (i) there are no data for groups 001 (already published by other authors), 206 and 241 (could not be re-identified), 252 (this is identical with 214), 301 and 353 (could not be re-identified); (ii) Group 328 was published twice (in North and South); and (iii) Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B). This HEASARC version of the catalog contains a total of 3435 individual galaxies identified as members of the compact groups, 2574 from the northern part of this survey (taken from the ADS Catalog VII/196 file north.dat), and 861 from the southern part of this survey (extracted from the 10746 entries in the ADS Catalog VII/196 file south.dat by including only entries corresponding to bona fide group members). This database table was created by the HEASARC in June, 2000, based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VII/196">CDS Catalog VII/196</a> (files north.dat and south.dat). This is a service provided by NASA HEASARC .
NGC 1332 Chandra X-Ray Compact Source Catalog
Chandra ACIS-S3 (Advanced CCD Imaging Spectrometer) observations of the nearby S0 galaxy NGC 1332 resolve much of the X-ray emission into 73 point sources, of which 37 lie within the D<sub>25</sub> isophote. The remaining galaxy emission comprises hot, diffuse gas and unresolved sources and is discussed in two companion papers. The point-source X-ray luminosity function (XLF) shows the characteristic break seen in other early-type galaxies at ~2 x 10<sup>38</sup> ergs s<sup>-1</sup>. After applying corrections for detection incompleteness at low luminosities due to source confusion and contamination from diffuse galactic emission, the break vanishes and the data are well described as a single power law. This result casts further doubt on there being a "universal" XLF break in early-type galaxies, marking the division between neutron star and black hole systems. The logarithmic slope of the differential XLF (dN/dL), beta = 2.7 +/- 0.5, is marginally (~2.5 sigma) steeper than has been found for analogous completeness-corrected fits of other early-type galaxies but closely matches the behavior seen at high luminosities in these systems. Two of the sources within D<sub>25</sub> are ultraluminous X-ray sources (ULXs), although neither have LX > 2 x 10<sup>39</sup> ergs s<sup>-1</sup>. The absence of very luminous ULXs in early-type galaxies suggests a break in the XLF slope at ~1-2 x 10<sup>39</sup> ergs s<sup>-1</sup>, although the data were not of sufficient quality to constrain such a feature in NGC 1332. The sources have a spatial distribution consistent with the optical light and display a range of characteristics that are consistent with an LMXB population. The general spectral characteristics of the individual sources, as well as the composite source spectra, are in good agreement with observations of other early-type galaxies, although a small number of highly absorbed sources are seen. Two sources have very soft spectra, two show strong variability, indicating compact binary nature, and one source shows evidence of an extended radial profile. The authors do not detect a central source in NGC 1332, but find a faint (L<sub>X</sub> = 2 +/- 1 x 10<sup>38</sup> ergs s<sup>-1</sup>) point source coincident with the center of the companion dwarf galaxy NGC 1331. The region of sky containing NGC 1332 was observed with the ACIS instrument aboard Chandra between 2002 September 19 10:39 and September 20 02:59 UTC for a nominal ~60 ksec exposure.. This table contains the 73 bona fide X-ray compact sources detected in this observation, excluding one source centered within 1" of the galaxy centroid that is actually the central part of the diffuse galactic emission, one source within the D<sub>25</sub> isophote of the neighboring galaxy NGC 1331, and one source with no photons within the 0.5-7.0 keV band which is likely to be spurious. The spatial extent of 72 of the 73 sources is consistent with the instrumental PSF. One source (number 14) is clearly more extended than the PSF. This table was created by the HEASARC in May 2018 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/612/848">CDS Catalog J/ApJ/612/848</a> file table1.dat, the list of detected X-ray sources in the Chandra observation of NGC 1332. This is a service provided by NASA HEASARC .
Planck Catalog of Compact Sources 44GHz Catalog
The Planck Catalogue of Compact Sources (PCCS) is a sample of reliable sources, both Galactic and extragalactic, extracted directly from the Planck nominal maps. The first public version of the PCCS, a component of Planck Data Release 1, is derived from the data acquired by Planck between August 13 2009 and November 26 2010. The PCCS consists of nine lists of sources, extracted independently from each of Planck's nine frequency channels. The source lists contain 24 columns per source at the LFI and HFI bands. The 857 GHz source list has six additional columns which give the flux densities and flux density uncertainties at the three adjacent lower frequencies: 217, 353, and 545 GHz.
Planck Catalog of 353-GHz Compact Sources (PCCS) Release 2
Planck was a European Space Agency (ESA) mission, with significant contributions from the National Aeronautics and Space Agency (NASA). It was the third generation of space-based cosmic microwave background experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in orbit checkout, Planck initiated the First Light Survey on 12 August 2009. Planck then continuously measured the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 micron) with spatial resolutions ranging from about 33 to 5 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provided temperature and polarization information using radiometers which operated between 30 and 70 GHz. The High Frequency Instrument (HFI) used pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but did not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest Planck frequencies overlapped with WMAP, and the highest frequencies extended far into the submillimeter in order to improve separation between Galactic foregrounds and the cosmic microwave background (CMB). By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck provided an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Second Planck Catalogue of Compact Sources is a list of discrete objects detected in single-frequency maps from the full duration of the Planck mission and supersedes previous versions. It consists of compact sources, both Galactic and extragalactic, detected over the entire sky. Compact sources detected in the lower frequency channels are assigned to the PCCS2, while at higher frequencies they are assigned to one of two subcatalogs, the PCCS2 or PCCS2E, depending on their location on the sky. The first of these (PCCS2) covers most of the sky and allows the user to produce subsamples at higher reliabilities than the target 80% integral reliability of the catalog. The second (PCCS2E) contains sources detected in sky regions where the diffuse emission makes it difficult to quantify the reliability of the detections. Both the PCCS2 and PCCS2E include polarization measurements, in the form of polarized flux densities, or upper limits, and orientation angles for all seven polarization-sensitive Planck channels. The improved data-processing of the full-mission maps and their reduced noise levels allow the authors to increase the number of objects in the catalog, improving its completeness for the target 80% reliability as compared with the previous versions, the PCCS and the Early Release Compact Source Catalogue (ERCSC). The Low Frequency Instrument (LFI) Data Processing Center (DPC) produced the 30, 44, and 70 GHz maps after the completion of eight full surveys (spanning the period from 12 August 2009 to 3 August 2013). In addition, special LFI maps covering the period 1 April 2013 to 30 June 2013 were produced in order to compare the Planck flux-density scales with those of the Very Large Array and the Australia Telescope Compact Array, by performing simultaneous observations of a sample of sources over that period. The High Frequency Instrument (HFI) DPC produced the 100-, 143-, 217-, 353-, 545-, and 857-GHz maps after five full surveys (from 2009 August 12 to 2012 January 11). As in the PCCS, the PCCS2 provides four different measures of the flux density for each source. They are determined by the source detection algorithm (DETFLUX), aperture photometry (APERFLUX), point spread function fitting (PSFFLUX), and Gaussian fitting (GAUFLUX). Only the first is obtained from the filtered maps; the other measures are estimated from the full-sky maps at the positions of the sources. The source detection algorithm photometry, the aperture photometry, and the point spread function (PSF) fitting use the Planck band-average effective beams, calculated with FEBeCoP (Fast Effective Beam Convolution in Pixel space). Note that only the PSF fitting algorithm takes into account the variation of the PSF with position on the sky. The PCCS2 has been produced from the Planck full-mission maps (eight sky surveys in the LFI and five sky surveys in the HFI), and therefore supersedes the previous catalogs (for the PCCS only 1.5 surveys were analyzed). It also includes the latest calibration and beam information, and the authors have improved some of the algorithms used to measure the photometry of the sources. This table contains the PCCS2 subsample of the PCCS Public Release 2 table of sources detected at 353 GHz. One of the primary differences of this release of the PCCS from previous releases is the division of the six highest frequency catalogs into two subcatalogs, the PCCS2 a
Planck Catalog of 70-GHz Compact Sources (PCCS) Release 2
Planck was a European Space Agency (ESA) mission, with significant contributions from the National Aeronautics and Space Agency (NASA). It was the third generation of space-based cosmic microwave background experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in orbit checkout, Planck initiated the First Light Survey on 12 August 2009. Planck then continuously measured the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 micron) with spatial resolutions ranging from about 33 to 5 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provided temperature and polarization information using radiometers which operated between 30 and 70 GHz. The High Frequency Instrument (HFI) used pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but did not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest Planck frequencies overlapped with WMAP, and the highest frequencies extended far into the submillimeter in order to improve separation between Galactic foregrounds and the cosmic microwave background (CMB). By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck provided an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Second Planck Catalogue of Compact Sources is a list of discrete objects detected in single-frequency maps from the full duration of the Planck mission and supersedes previous versions. It consists of compact sources, both Galactic and extragalactic, detected over the entire sky. Compact sources detected in the lower frequency channels are assigned to the PCCS2, while at higher frequencies they are assigned to one of two subcatalogs, the PCCS2 or PCCS2E, depending on their location on the sky. The first of these (PCCS2) covers most of the sky and allows the user to produce subsamples at higher reliabilities than the target 80% integral reliability of the catalog. The second (PCCS2E) contains sources detected in sky regions where the diffuse emission makes it difficult to quantify the reliability of the detections. Both the PCCS2 and PCCS2E include polarization measurements, in the form of polarized flux densities, or upper limits, and orientation angles for all seven polarization-sensitive Planck channels. The improved data-processing of the full-mission maps and their reduced noise levels allow the authors to increase the number of objects in the catalog, improving its completeness for the target 80% reliability as compared with the previous versions, the PCCS and the Early Release Compact Source Catalogue (ERCSC). The Low Frequency Instrument (LFI) Data Processing Center (DPC) produced the 30, 44, and 70 GHz maps after the completion of eight full surveys (spanning the period from 12 August 2009 to 3 August 2013). In addition, special LFI maps covering the period 1 April 2013 to 30 June 2013 were produced in order to compare the Planck flux-density scales with those of the Very Large Array and the Australia Telescope Compact Array, by performing simultaneous observations of a sample of sources over that period. The High Frequency Instrument (HFI) DPC produced the 100-, 143-, 217-, 353-, 545-, and 857-GHz maps after five full surveys (from 2009 August 12 to 2012 January 11). As in the PCCS, the PCCS2 provides four different measures of the flux density for each source. They are determined by the source detection algorithm (DETFLUX), aperture photometry (APERFLUX), point spread function fitting (PSFFLUX), and Gaussian fitting (GAUFLUX). Only the first is obtained from the filtered maps; the other measures are estimated from the full-sky maps at the positions of the sources. The source detection algorithm photometry, the aperture photometry, and the point spread function (PSF) fitting use the Planck band-average effective beams, calculated with FEBeCoP (Fast Effective Beam Convolution in Pixel space). Note that only the PSF fitting algorithm takes into account the variation of the PSF with position on the sky. The PCCS2 has been produced from the Planck full-mission maps (eight sky surveys in the LFI and five sky surveys in the HFI), and therefore supersedes the previous catalogs (for the PCCS only 1.5 surveys were analyzed). It also includes the latest calibration and beam information, and the authors have improved some of the algorithms used to measure the photometry of the sources. This table contains the PCCS Public Release 2 table of sources detected at 70 GHz. Where the HEASARC parameter names differ from those used in the original table, the original names are listed parenthetically in upper case at the end of the parameter description. This table w
Hickson Compact Groups of Galaxies (HCG) Catalog
The HCG database table is based on the Hickson Catalog, which is a list of 100 compact groups of galaxies that were identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec<sup>2</sup> and satisfies an isolation criterion. Dynamical parameters which were derived for 92 of the 100 groups are also included in the database. (Note that the Hubble constant was assumed to be Ho = 100 km/s/Mpc.) This database table essentially contains the information given in Table 1 of Hickson, P. (1982, ApJ, 255, 382) and Table 3 of Hickson, P. et al. (1992, ApJ, 399, 353). Consequently, the information on individual galaxies in the Hickson groups that is also given in these references, e.g., in Table 2 of Hickson, P. et al. (1992, ApJ, 399, 353), is not in the HCG database table; however, the latter data can be found in the related HEASARC database table HCGGALAXY. This online catalog was created by the HEASARC in August, 1999, based on machine-readable tables obtained from the ADC/CDS data centers (<a href="https://cdsarc.cds.unistra.fr/ftp/cats/VII/213:">CDS catalog VII/213:</a> files groups.dat and dynamics.dat). The HEASARC refined the coordinates, corrected the dynamics_flag values, and updated the table's metadata in August, 2005. This is a service provided by NASA HEASARC .
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Allen Brain Atlas
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Annotated Behaviour and Observability Dataset (ABODe)
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DANDI Archive for NWB datasets
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International Brain Laboratory public data
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OpenNeuro
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