- ID:
- ivo://nasa.heasarc/pccs044ghz
- Title:
- Planck Catalog of 44-GHz Compact Sources (PCCS) Release 2
- Short Name:
- PCCS044GHZ
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- 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 44 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 was created by the HEASARC in May 2017 based upon the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/594/A26">CDS Catalog J/A+A/594/A26</a> file pccs044.dat. This is a service provided by NASA HEASARC .
Number of results to display per page
Search Results
- ID:
- ivo://nasa.heasarc/rssgrbag
- Title:
- Radio-Selected Gamma-Ray Burst Afterglow Catalog
- Short Name:
- RSSGRBAG
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains a catalog of radio afterglow observations of gamma-ray bursts (GRBs) over a 14 year period from 1997 to 2011. This sample of 304 afterglows consists of 2,995 flux density measurements (including upper limits) at frequencies between 0.6 GHz and 660 GHz, with the majority of data taken in the 8.5-GHz frequency band (1,539 measurements). The authors use this dataset to carry out a statistical analysis of the radio-selected sample. The detection rate of radio afterglows stayed unchanged almost at 31% before and after the launch of the Swift satellite. The canonical long-duration GRB radio light curve at 8.5 GHz peaks at three to six days in the source rest frame, with a median peak luminosity of 10<sup>31</sup> erg/s/Hz. The peak radio luminosities for short-hard bursts, X-ray flashes, and the supernova-GRB classes are an order of magnitude or more fainter than this value. There are clear relationships between the detectability of a radio afterglow and the fluence or energy of a GRB, and the X-ray or optical brightness of the afterglow. However, the authors find few significant correlations between these same GRB and afterglow properties and the peak radio flux density. In their paper, they also produce synthetic light curves at centimeter and millimeter bands using a range of blast wave and microphysics parameters derived from multi-wavelength afterglow modeling, and use them to compare with the radio sample. Finding agreement, the authors extrapolate this behavior to predict the centimeter and millimeter behavior of GRBs which will observed by the Expanded Very Large Array and the Atacama Large Millimeter Array. The compiled sample consists of 304 GRBs observed with radio telescopes between 1997 January and 2011 January, along with the 2011 April 28 Fermi burst, GRB 110428A. The sample consists of a total of 2,995 flux density measurements taken in the frequency range from 0.6 to 660 GHz and spanning a time range from 0.026 to 1,339 days. Most of the afterglows (270 in total) in this sample were observed as part of VLA radio afterglow programs, whereas 15 bursts were observed by the Expanded VLA (EVLA), and 19 southern bursts with the Australia Telescope Compact Array (ATCA). This catalog describes the radio, optical and X-ray afterglow detections (see Section 2.2 of the reference paper): out of the 304 bursts, 123 bursts were observed in the pre-Swift epoch from 1997 until 2004. The remaining 181 bursts were observed between 2005 and 2011 April (the post-Swift epoch). Out of the 95 radio-detected afterglows (see Section 2.2 of the reference paper), 63 had radio lightcurves (i.e., three or more detections in a single radio band), whereas 32 bursts had less than three detections. For the GRBs for which the light curves were available, the authors determined the peak flux density and the time of the peak in the VLA frequency bands (i.e., 1.4 GHz, 4.9 GHz, 8.5 GHz, 15 GHz, and 22.5 GHz bands) by fitting the data with forward shock formula of the form (Frail 2005, IAU Coll. 192, p. 451) given in equation (1) of the reference paper. This formula may not accurately represent the full complexity of the radio lightcurve evolution. However, it is good enough to determine the approximate values for the peak flux density F<sub>m</sub> and the time of the peak t<sub>m</sub>. See the discussion in Section 3.5 of the reference paper for more details and some caveats. For the remaining bursts, the flux density values were taken directly from the data, and hence do not have the best-fit errors for the peak flux, peak time and rest-frame peak time parameters F<sub>m</sub>, t<sub>m</sub> and t<sub>m</sub>/(1+z), respectively. This table was created by the HEASARC in November 2013 based on CDS catalog J/ApJ/746/156 files table1.dat and table4.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/ros13hrvla
- Title:
- ROSAT/XMM-Newton 13-hr Deep Field VLA 20-cm Source Catalog
- Short Name:
- ROS13HRVLA
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- In order to determine the relationship between the faint X-ray and faint radio source populations, and hence to help understand the X-ray and radio emission mechanisms in those faint source populations, the authors have made a deep 1.4-GHz Very Large Array radio survey of the 13<sup>h</sup> 34<sup>m</sup> 37<sup>s</sup>, +37<sup>o</sup> 54' 44" (J2000) ROSAT/XMM-Newton X-ray Survey Area (McHardy et al. 1998, MNRAS, 295, 641; Loaring et al. 2005, MNRAS, 362, 1371: the catalog of XMM-Newton sources from the latter paper is available at the HEASARC as the ROS13HRXMM table). From a combined VLA data set of 10 hours of B-configuration data and 14 hours of A-configuration data, maps with 3.35-arcsec resolution and a noise limit of 7.5 microJansky (uJy) were constructed. A complete sample of 449 sources was detected within a 30-arcmin diameter region above a 4-sigma detection limit of 30 uJy, at the map center, making this one of the deepest radio surveys at this frequency. The differential source count shows a significant upturn at sub-milliJansky flux densities, similar to that seen in other deep surveys at 1.4 GHz (e.g. the Phoenix survey, Hopkins et al. 2003, AJ, 125, 465: available at the HEASARC as the PDS1P4GHZ table), but larger than that seen in the Hubble Deep Field (HDF) which may have been selected to be underdense. This upturn is well modeled by the emergence of a population of medium-redshift star-forming galaxies which dominate at faint flux densities. The brighter source counts are well modeled by active galactic nuclei. This HEASARC table contains the catalog of 449 radio sources in a region of 30-arcmin diameter centered on the ROSAT/XMM 13-hours field which were detected at 1.4 GHz (20 cm) above a detection threshold of 4 sigma, equivalent to 30 uJy at the phase center. This table was created by the HEASARC in July 2013 based on CDS Catalog J/MNRAS/352/131 file table a1.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/sgraregcsc
- Title:
- Sgr A* Region Compact Radio Source Catalog
- Short Name:
- SGRAREGCSC
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- 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 .
- ID:
- ivo://nasa.heasarc/smc1400mhz
- Title:
- Small Magellanic Cloud ATCA and Parkes 1400-MHz Source Catalog
- Short Name:
- SMC1400MHZ
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains a new catalog of radio-continuum sources in the field of the Small Magellanic Cloud (SMC). This catalog contains 1560 radio-continuum sources detected at 1400 MHz (lambda = 20 cm) from a set of new high-resolution radio-continuum mosaic images of the SMC created by combining observations from ATCA and Parkes (Wong et al. 2011, SerAJ, 182, 43). The 20 cm mosaic image (Fig. 2 in above reference)was created by combining data from ATCA project C1288 (Mao et al. 2008, ApJ, 688, 1029) with data obtained for a Parkes radio-continuum study of the SMC (Filipovic et al. 1997, A&AS, 121, 321). This image had a beam size of 17.8 x 12.2 arcseconds and an rms noise of 0.7 mJy/beam. The MIRIAD task 'imsad' was used to detect sources in the 20-cm image, requiring a fitted Gaussian flux density > 5 sigma (3.5 mJy). All sources were then visually examined to confirm that they were genuine point sources, excluding extended emission, bright side lobes, etc. This table was created by the HEASARC in September 2014 based on CDS Catalog J_other/Ser/183.103/ file tablea2.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/smc4800mhz
- Title:
- Small Magellanic Cloud ATCA 4800-MHz Source Catalog
- Short Name:
- SMC4800MHZ
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains a new catalog of radio-continuum sources in the field of the Small Magellanic Cloud (SMC). This catalog contains sources found at 4800 MHz (lambda = 6 cm) by combining data from various Australia Telescope Compact Array (ATCA) projects that covered the SMC. Some 601 sources have been detected at 6 cm in the new high-sensitivity and resolution radio-continuum image of the SMC from Crawford et al. (2011, SerAJ, 183, 95). The 6 cm map has a resolution of 30 arcseconds, and a sensitivity of 0.7 mJy/beam. The field size of the image used in this study covered from 00<sup>h</sup> 26<sup>m</sup> to 01<sup>h</sup> 28<sup>m</sup> in RA (J2000.0) and from -70<sup>o</sup> 29' to -75<sup>o</sup> 29' in Dec (J2000.0). The MIRIAD task 'imsad' was used to detect sources in the 6 cm image, requiring a fitted Gaussian flux density > 5 sigma (3.5 mJy). All sources were then visually examined to confirm that they are genuine point sources, excluding extended emission, bright side lobes, etc. This table was created by the HEASARC in September 2014 based on CDS Catalog J_other/Ser/184.93/ file tablea2.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/smc8640mhz
- Title:
- Small Magellanic Cloud ATCA 8640-MHz Source Catalog
- Short Name:
- SMC8640MHZ
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains a new catalog of radio-continuum sources in the field of the Small Magellanic Cloud (SMC). This catalog contains sources found at 8640 MHz (lambda = 3 cm) by combining data from various Australia Telescope Compact Array (ATCA) projects that covered the SMC. Some 457 sources have been detected at 3 cm in the new high-sensitivity and resolution radio-continuum image of the SMC from Crawford et al. (2011, SerAJ, 183, 95). The 3 cm map has a resolution of 20 arcseconds, and a sensitivity of 0.8 mJy/beam. The field size of the image used in this study covered from 00<sup>h</sup> 26<sup>m</sup> to 01<sup>h</sup> 27<sup>m</sup> in RA (J2000.0) and from -70<sup>o</sup> 35' to -75<sup>o</sup> 21' in Dec (J2000.0). The MIRIAD task 'imsad' was used to detect sources in the 3 cm image, requiring a fitted Gaussian flux density > 5 sigma (3.5 mJy). All sources were then visually examined to confirm that they are genuine point sources, excluding extended emission, bright side lobes, etc. This table was created by the HEASARC in September 2014 based on CDS Catalog J_other/Ser/184.93/ file tablea1.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/smcradio
- Title:
- Small Magellanic Cloud ATCA Radio Continuum Sources
- Short Name:
- SMCRadio
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the classification of 717 radio-continuum sources from the Australia Telescope Compact Array (ATCA) Catalog of the Small Magellanic Cloud (SMC). All 717 sources have been categorised into one of three groups: supernova remnants (SNRs), HII regions and background sources. In total, 71 sources are named as HII regions (or candidates) and 21 sources are named as SNRs (or candidates). Six sources are named as either HII regions or background sources and two are candidate radio planetary nebulae. One source is coincident with an X-ray binary. 616 objects are classified as background sources and their statistics are presented in the published paper II from which this table is taken. This table was created by the HEASARC in March 2005 based on CDS table J/MNRAS/355/44/table2.dat . This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/smc843mhz
- Title:
- Small Magellanic Cloud MOST 843-MHz Source Catalog
- Short Name:
- SMC843MHZ
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains a new catalog of radio-continuum sources in the field of the Small Magellanic Cloud (SMC). This catalog contains 1689 radio-continuum sources detected at 843 MHz (lambda = 36 cm) from a radio survey of 36 square degrees containing the SMC (Turtle et al. 1998, PASA, 15, 280) conducted using the Molonglo Observatory Synthesis Telescope (MOST). These observations had a beam size of ~ 45 arcseconds and an rms noise of 0.7 mJy/beam. The MIRIAD task 'imsad' was used to detect sources in the 36-cm images, requiring a fitted Gaussian flux density > 5 sigma (3.5 mJy). All sources were then visually examined to confirm that they were genuine point sources, excluding extended emission, bright side lobes, etc. This table was created by the HEASARC in September 2014 based on CDS Catalog J_other/Ser/183.103/ file tablea3.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/sptmm87sd
- Title:
- South Pole Telescope 87-Square Degree Survey Millimeter Source Catalog
- Short Name:
- SPTMM87SD
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the results of an 87 deg<sup>2</sup> point-source survey centered at RA = 5<sup>h</sup>30<sup>m</sup>, Dec = -55<sup>o</sup> (J2000.0) taken with the South Pole Telescope at 1.4 and 2.0 mm wavelengths with arcminute resolution and milli-Jansky (mJy) depth. Based on the ratio of flux in the two bands, the authors separate the detected sources into two populations, one consistent with synchrotron emission from active galactic nuclei (AGN) and the other consistent with thermal emission from dust. In the reference paper, the authors present source counts for each population from 11 to 640 mJy at 1.4 mm and from 4.4 to 800 mJy at 2.0 mm. The 2.0-mm counts are dominated by synchrotron-dominated sources across the reported flux range; the 1.4-mm counts are dominated by synchrotron-dominated sources above ~15 mJy and by dust-dominated sources below that flux level. The authors detect 141 synchrotron-dominated sources and 47 dust-dominated sources at signal-to-noise ratio S/N > 4.5 in at least one band. All of the most significantly detected members of the synchrotron-dominated population are associated with sources in previously published radio catalogs. Some of the dust-dominated sources are associated with nearby (z << 1) galaxies whose dust emission is also detected by the Infrared Astronomy Satellite (IRAS). However, most of the bright, dust-dominated sources have no counterparts in any existing catalogs. The authors argue that these sources represent the rarest and brightest members of the population commonly referred to as sub-millimeter galaxies (SMGs). During the 2008 observing season, the 960-element South Pole Telescope (SPT) camera included detectors sensitive to radiation within bands centered at approximately 1.4 mm, 2.0 mm, and 3.2 mm (220 GHz, 150 GHz, and 95 GHz). Result in this reference paper are based on 607 hr of observing time, using only the 1.4-mm and 2.0-mm data from the 87 deg<sup>2</sup> portion of the field that was mapped with near-uniform coverage. Main-lobe beams were measured using the brightest sources in the field and were adequately fit by two-dimensional Gaussians with FWHM equal to 1.05 and 1.15 arcminutes at 1.4 mm and 2.0 mm, respectively. The typical rms of the filtered 2.0-mm and 1.4-mm maps used for source candidate identification (shown in Figures 1 and 2, respectively, of the reference paper) is 1.3 mJy at 2.0 mm and 3.4 mJy at 1.4 mm. Detections in both bands are listed in the final catalog as a single source if they are offset <30 arcseconds between the two bands. For sources detected in both bands, the authors adopt the position of the more significant detection. The argue that they are far enough above the confusion limit that this simple and intuitive method is adequate. For sources detected in only one band, the authors use the flux in the cleaned map for the second band at the position of the detection. This table lists all 3,496 sources above 3 sigma in either map. This table was created by the HEASARC in October 2017 based on an electronic version of Table 5 from the reference paper which was obtained from the CDS as their catalog J/ApJ/719/763 file table5.dat. This is a service provided by NASA HEASARC .