- ID:
- ivo://nasa.heasarc/pmn
- Title:
- Parkes-MIT-NRAO (PMN) Surveys
- Short Name:
- PMN
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The PMN database contains data from the Parkes-MIT-NRAO (PMN) Southern, Zenith, Tropical and Equatorial surveys. These surveys were made using the Parkes 64-m radio telescope at a frequency of 4850 Hz with the NRAO multibeam receiver mounted at the prime focus (for a full description of the observations see Griffith & Wright, 1993, Paper I). These surveys had a spatial resolution (full width half-maximum: FWHM) of approximately 4.2 arcminutes and were made during 1990 June and November. The PMN surveys were divided into several zones. These zones are listed below, together with approximate flux limits and survey areas: <pre> Zone Name DEC limits (degrees) Flux limits Area (sr) SOUTHERN -87.5< dec <-37 20 to 50 mJy 2.50 ZENITH -37 < dec <-29 72 mJy 0.67 TROPICAL -29 < dec < -9.5 42 mJy 2.01 EQUATORIAL -9.5< dec <+10.0 40 mJy 1.90 </pre> A point source catalog was compiled directly from each of the survey zones by using an optimum filter method, as described by Griffith & Wright in detail in Paper 1. In addition, a set of images was produced for each zone in a manner very similar to that used by Condon et al. for the northern survey (<a href="https://cdsarc.cds.unistra.fr/ftp/cats/VIII/40">CDS Catalog VIII/40</a>): See e.g. Paper 4. These maps have an effective resolution (FWHM) of about 5 arcmin. For more details, refer to the publications listed in the References Section for the relevant zone. This updated version of the PMN database was created by the HEASARC in January 2001 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VIII/38">CDS Catalog VIII/38</a>. This is a service provided by NASA HEASARC .
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- ID:
- ivo://nasa.heasarc/pkscat90
- Title:
- Parkes Southern Radio Source Catalog, Version 1.01
- Short Name:
- Parkes
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- PKSCAT90 is the Parkes Catalog (1990) and consists of radio and optical data for 8,264 radio sources. It covers essentially all the sky south of declination +27 degrees but largely excludes the Galactic Plane and the Magellanic Cloud regions. The latter zones have been the subject of other, specialist surveys. A few data errors in Version 1.00 have been corrected in the present edition (see below). This version of the Parkes Radio Source Catalog is entitled "PKSCAT90 Version 1.01." The original Parkes radio catalog was compiled from major radio surveys with the Parkes radiotelescope at frequencies of 408 MHz and 2700 MHz. This work spanned a period of nearly 20 years and was undertaken largely by John Bolton and his colleagues. Since then, improved positions, optical identifications, and redshifts have been obtained for many of the sources in the catalog. Furthermore, flux densities at several frequencies have supplemented the original surveys so that the measurements now cover the frequency range 80-22,000 MHz. However, coverage at the highest frequencies is still sparse. Important contributions to the usefulness of the catalog have been radio data from the Molonglo 408-MHz survey and the 80-MHz Culgoora measurements of Slee et al. PKSCAT90 should thus be regarded as a compendium of radio and optical data about southern radio sources. However, at the moment, it contains only sources originally found in the Parkes 2700-MHz survey (see e.g. Part 14, Bolton et al, 1979, Aust J Phys, Astrophys Suppl, No. 46 and references therein.) The original radio survey data of the catalog and the optical identifications have been published in a series of papers in the Australian Journal of Physics (see above reference). The associated optical spectral data on which redshifts were obtained has also been published, mainly in Astrophysical Journal and Monthly Notices of the Royal Astronomical Society. About the completeness levels of the catalog in various parts of the sky: users should note that the sky zone between -4 and +4 degrees has been the subject of a re-survey and is now complete to 0.25 Jy. The author Alan Wright notes that "PKSCAT90 was produced at a time when relational databases were in their infancy. In the future we anticipate making the individual data sources available separately -- through such search systems as SIMBAD -- rather than in an 'omnibus' catalog like PKSCAT90. For both the Northern and Southern hemispheres, superior and deeper finding surveys now exist: the 87GB catalog in the North (Gregory and Condon et al. 1991, ApJ, 75, 1011, <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VIII/14">CDS Catalog VIII/14</a>) and the PMN catalogs (Griffith and Wright 1993, AJ, 105, 1666, <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VIII/38">CDS Catalog VIII/38</a>, available at the HEASARC as the PMN table) in the South." This table was updated by the HEASARC in July 2015 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VIII/15">CDS Catalog VIII/15</a> file pkscat90.dat, replacing a version based on the original (version 1) PKSCAT90, which was created in 1995. It was further updated in September 2015 as noted in the "Version 1.01 Modifications" section above. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/pds1p4ghz
- Title:
- Phoenix Deep Survey 1.4-GHz Catalog
- Short Name:
- PDS1P4GHZ
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The initial Phoenix Deep Survey (PDS) observations with the Australia Telescope Compact Array (ATCA) have been supplemented by additional 1.4 GHz observations over the past few years. Here we present details of the construction of a new mosaic image covering an area of 4.56 deg<sup>2</sup> referred to as the Phoenix Deep field (PDF), an investigation of the reliability of the source measurements, and the 1.4 GHz source counts for the compiled radio catalog. The mosaic achieves a 1-sigma rms noise of 12 µJy at its most sensitive, and a homogeneous radio-selected catalog of over 2000 sources reaching flux densities as faint as 60 µJy has been compiled. The source parameter measurements are found to be consistent with the expected uncertainties from the image noise levels and the Gaussian source fitting procedure. A radio-selected sample avoids the complications of obscuration associated with optically selected samples, and by utilizing complementary PDS observations, including multicolor optical, near-infrared, and spectroscopic data, this radio catalog will be used in a detailed investigation of the evolution in star formation spanning the redshift range 0 < z < 1. The homogeneity of the catalog ensures a consistent picture of galaxy evolution can be developed over the full cosmologically significant redshift range of interest. The PDF covers a high-latitude region that is of low optical obscuration and devoid of bright radio sources. ATCA 1.4 GHz observations were made in 1994, 1997, 1999, 2000, and 2001 in the 6A, 6B, and 6C array configurations, accumulating a total of 523 hr of observing time. The initial 1994 ATCA observations (Hopkins et al. 1998, MNRAS, 296, 839; Hopkins 1998, PhD thesis) consisted of 30 pointings on a hexagonal tessellation, resulting in a 2 degrees diameter field centered on R.A. = 01<sup>h</sup> 14<sup>m</sup> 12.16<sup>s</sup>, Dec = -45<sup>o</sup> 44' 8.0" (J2000.0), with roughly uniform sensitivity of about 60 µJy rms. This survey was supplemented from 1997 to 2001 by extensive observations of a further 19 pointings situated on a more finely spaced hexagonal grid, centered on R.A. = 01<sup>h</sup> 11<sup>m</sup> 13.0<sup>s</sup>, Dec = -45<sup>o</sup> 45' 00" (J2000.0). The locations of all pointing centers are given in Table 1 of the reference paper. The final mosaic constructed from all 49 pointings was trimmed to remove the highest noise regions at the edges by masking out regions with an rms noise level greater than 0.25 mJy. The trimmed PDF mosaic image covers an area of 4.56 deg<sup>2</sup> and reaches to a measured level of 12 µJy rms noise in the most sensitive regions. The table contained here is the final merged catalog of PDS surveys based on the union of the 10% false discovery rate (FDR) threshold catalog (PDS_atca_fdr10_full_vis.cat) for the trimmed mosaic, visually edited to remove objects clearly associated with artifacts close to bright sources, containing 2058 sources, and the 10% FDR threshold catalog (PDS_atca_fdr10_deep.cat) for the 33' x 33' region centered on the most sensitive portion of the mosaic, containing 491 sources. The merged catalog was constructed to contain all unique catalogued sources; where common sources were identified, only the entry from PDS_atca_fdr10_deep.cat was retained. There are a total of 2148 sources in the final merged catalog, of which up to 10% may be false. This table was created by the HEASARC in November 2012 based on the file PDS_atca_fdr10_merge.cat, the merged PDS catalog (derived from the individual catalogs PDS_atca_fdr10_full_vis.cat and PDS_atca_fdr10_deep.cat as discussed in the Overview above), which was obtained from the first author's website <a href="https://web.archive.org/web/20171009234923/www.physics.usyd.edu.au/~ahopkins/phoenix/">https://web.archive.org/web/20171009234923/www.physics.usyd.edu.au/~ahopkins/phoenix/</a>. 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 .
- ID:
- ivo://nasa.heasarc/pdsoid
- Title:
- Phoenix Deep Survey Optical and Near-Infrared Counterparts Catalog
- Short Name:
- PDSOID
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Using a deep Australia Telescope Compact Array (ATCA) radio survey covering an area of ~3 deg<sup>2</sup> to a 4-sigma sensitivity of >= 100 µJy (µJy) at 1.4 GHz, the authors study the nature of faint radio galaxies. The region, 2 degrees in diameter and centered on RA and Dec (J2000.0) of 1<sup>h</sup> 14<sup>m</sup> 12.16<sup>s</sup>, -45<sup>o</sup> 44' 08.0" (Galactic latitude of -71<sup>o</sup>), is known as the Phoenix Deep Field. About 50% of the detected radio sources are identified with an optical counterpart revealed by CCD photometry to m<sub>R</sub> = 22.5 magnitudes. Near-infrared (K-band) data are also available for a selected sample of the radio sources, while spectroscopic observations have been carried out for about 40% of the optically identified sample. These provide redshifts and information on the stellar content. Emission-line ratios imply that most of the emission-line sources are star-forming galaxies, with a small contribution (~ 10%) from Seyfert 1/Seyfert 2 type objects. The authors also find a significant number of absorption-line systems, likely to be ellipticals. These dominate at high flux densities ( > 1 mJy) but are also found at sub-mJy levels. Using the Balmer decrement, they find a visual extinction A<sub>V</sub> = 1.0 for the star-forming faint radio sources. This moderate reddening is consistent with the (V - R) and (R - K) colors of the optically identified sources. For emission-line galaxies, there is a correlation between the radio power and the H-alpha luminosity, in agreement with the result of Benn et al. (1993, MNRAS, 263, 98). This suggests that the radio emission of starburst radio galaxies is a good indicator of star formation activity. When calculating luminosities, the authors assume a cosmology with a Hubble constant H<sub>0</sub> of 50 km s<sup>-1</sup> Mpc<sup>-1</sup> and a deceleration parameter q<sub>0</sub> of 0.5. This table was created by the HEASARC in June 2013 based on an electronic version of Table 1 from the reference paper, which details the photometric (optical and near-infrared), radio, spectroscopic and intrinsic properties of the faint radio sources in the PDS with established redshifts, which was obtained from the CDS web site (their catalog J/MNRAS/306/708 file table1.dat). This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/pdsoid2
- Title:
- Phoenix Deep Survey Optical and Near-Infrared Counterparts Catalog 2
- Short Name:
- PDSOID2
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Phoenix Deep Survey (PDS) is a multi-wavelength galaxy survey based on deep 1.4-GHz radio imaging. The revised version of the radio source catalog was published by Hopkins et al. (2003). The primary goal of the PDS is to investigate the properties of star formation in galaxies and to trace the evolution in those properties to a redshift z = 1, covering a significant fraction of the age of the universe. By compiling a sample of star-forming galaxies based on selection at radio wavelengths, Sullivan et al. (2004, the reference paper for this present catalog) eliminate possible biases due to dust obscuration, a significant issue when selecting objects at optical and ultraviolet wavelengths. In this study, they present the catalogs and results of deep optical (UBVRI) and near-infrared (K<sub>s</sub>) imaging of the deepest region of the existing decimetric radio imagery. The observations and data processing are summarized and the construction of the optical source catalogs described in their paper, together with the details of the identification of candidate optical counterparts to the radio catalogs. Based on their UBVRIK<sub>s</sub> imaging, photometric redshift estimates for the optical counterparts to the radio detections are explored. Two pointings (labeled 7 and 3 in Table 1 of the reference paper) were observed in BVRi, and one (pointing 11 in ibid.) in BVi on the nights of 2001 August 13 and 14, with the WFI camera on the Anglo-Australian Telescope (AAT). The same three pointings were also observed in U with the Mosaic-II camera on the Cerro Tololo Inter-American Observatory (CTIO) 4-m Blanco telescope on 2002 September 3. Finally, four of the PDS fields (2, 3, 6, 7) were observed in U with the WFI on the European Southern Observatory (ESO) 2.2-m telescope on the night of 2001 August 18. The NIR imaging data come from the Hawaii HgCdTe 1024 x 1024 pixel array SoFI camera on the 3.6-m ESO New Technology Telescope (NTT). The field of view was 4.9' x 4.9' with a pixel scale of 0.29". Nine contiguous pointings, in a 3 x 3 pattern, were observed over the deepest region of the PDS (a sub-region of pointing 7; see Fig. 1 of the reference paper), during 2000 October 10 and October 11. Throughout this study, the authors assume an Omega<sub>Lambda</sub> = 0.7, Omega<sub>M</sub> = 0.3, h = 0.70 (where H<sub>0</sub> = 100 h km s<sup>-1</sup> Mpc<sup>-1</sup>) cosmology. This table was created by the HEASARC in June 2013 based on an electronic version of Table 6 from the reference paper, which details the photometric (optical and near-infrared) properties and redshifts of 778 radio sources in the PDS, which was obtained from the CDS web site (their catalog J/ApJS/155/1 file table6.dat). The HEASARC has changed the name prefixes of the sources in this table from 'PDS' (Phoenix Deep Survey) to 'PDF' (Phoenix Deep Field) as recommended by the CDS Dictionary of Astronomical Nomenclature. Three duplicate entries were removed from the catalog in June 2019. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/pacobscat
- Title:
- Planck-ATCA Co-eval Observations (PACO) Project Bright Sample Catalog
- Short Name:
- PACOBSCAT
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Planck Australia Telescope Compact Array (Planck-ATCA) Co-eval Observations (PACO) have provided flux density measurements of well-defined samples of Australia Telescope 20-GHz (AT20G) radio sources at frequencies below and overlapping with Planck frequency bands, almost simultaneously with Planck observations. The authors have observed with the ATCA a total of 482 sources in the frequency range between 4.5 and 40 GHz in the period between 2009 July and 2010 August. Several sources were observed more than once. In their paper, the authors present the aims of the project, the selection criteria, and the observation and data reduction procedures. They also discuss the data in total intensity for a complete sample of 189 sources with 20-GHz flux densities > 500 mJy, Galactic latitude |b| > 5 degrees and Declination < -30 degrees, and some statistical analysis of the spectral behavior and variability of this sample, referred to as the 'bright PACO sample'. Finally, the authors discuss how these data could be used to transfer absolute calibrations to ground-based telescopes using the cosmic microwave background dipole calibrated flux densities measured by the Planck satellite, and they provide some test fluxes on bright calibrators. This table contains the catalog of 1004 observations of 180 of the 189 sources that comprise the 'bright PACO sample'. Thus, each row in this table corresponds to a specific observation of a source, and there can be several rows for any source, corresponding to different observations. The ATCA observations were made in 6 2-GHz wide observing bands: 4732 - 6780 MHz, 8232 - 10280 MHz, 17232 - 19280 MHz, 23232 - 25280 MHz, 32232 - 34280 MHz and 38232 - 40280 MHz. In order to properly define the detailed source spectral behavior, the authors have split each 2-GHz band into 4 x 512 MHz sub-bands, and calibrated each sub-band independently. Thus, for each observation, the flux density at 24 frequencies is given. The frequency identifier in the flux density appears (at least to this HEASARC scientist) to be the lower frequency of the sub-band rather than its central frequency. In order to provide the easiest way to extrapolate the observed counts or model predictions from one frequency to another, the authors have modeled the observed source spectra. As their observations covered a wide frequency range from 4.5 to 40 GHz over which a single power law is not enough to describe the spectral behavior of the sources, they studied the spectra of the 174 point-like sources in this sample by fitting the observed data with a double power law of the form S<sub>nu</sub> = S<sub>0</sub>/[(nu/nu<sub>0</sub>)<sup>-a</sup> + (nu/nu<sub>0</sub>)<sup>-b</sup>], where nu is the frequency, S<sub>nu</sub> is the flux density in Jy, and S<sub>0</sub>, nu<sub>0</sub>, a and b are free parameters. The authors considered only those sources for which they had at least four data points for each of the 2 x 2 GHz bands considered. Full details of the fitting procedure are given in Section 3.1 of the reference paper. This table was created by the HEASARC in January 2014 based on the machine-readable version of Table S1 from the reference paper which was obtained from the CDS (their catalog J/MNRAS/415/1597 file table1.dat). This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/pacofscat
- Title:
- Planck-ATCA Co-eval Observations (PACO) Project Faint Sample Catalog
- Short Name:
- PACOFSCAT
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Planck-ATCA Co-eval Observations (PACO) project collected data between 4.5 and 40 GHz for 482 sources selected within the Australia Telescope 20-GHz (AT20G) catalog and observed with the Australia Telescope Compact Array (ATCA). Observations were done almost simultaneously with the Planck satellite, in the period between 2009 July and 2010 August. In this paper, the authors present and discuss the data for the complete sample of 159 sources with AT20G flux densities > 200 mJy in the South Ecliptic Pole (SEP) region. The Planck Early Release Compact Source Catalogue (ERCSC) contains 57 of their sources. A comparison between the PACO catalog and the ERCSC confirms that the reliability of the latter is better than 95%. The missing ERCSC sources are typically associated with the Large Magellanic Cloud, the Milky Way or are otherwise extended. The spectral analysis of the PACO faint catalog shows a spectral steepening of the sources at high frequencies, confirming the results obtained from the PACO bright sample (the HEASARC PACOBSCAT table). A comparison with AT20G measurements, carried out, on average, a few years earlier, has demonstrated that, on these time-scales, these sources show a rather high variability with an rms amplitude of approximately 40% at 20 GHz. The source spectral properties are found not to vary substantially with flux density, except for an increase in the fraction of steep spectrum sources at fainter flux densities. These data also allow the authors to extend by a factor of ~ 5 downwards in flux density the source counts at ~ 33 and ~ 40 GHz obtained from the ERCSC. This allows the authors to substantially improve their control on the contribution of unresolved extragalactic sources to the power spectrum of small-scale fluctuations in cosmic microwave background (CMB) maps. The PACO faint sample, presented in this paper, is made up of 159 sources with 20-GHz flux densities >= 200 mJy in the SEP region (ecliptic latitude < -75 degrees) and with 3h < RA < 9h, Dec. < -30 degrees. Near the Ecliptic Poles, Planck's scan circles intersect. Therefore, the area is covered many times, and Planck's sensitivity is maximal in these regions. A full description of the PACO project and of its main goals is given in Massardi et al. (2011, MNRAS, 415, 1597). The aims specific to the PACO faint sample are as follows: (i) Extend to fainter flux densities the characterization of radio source spectra from 4.5 GHz to the Planck frequency range; (ii) Extend the determination of source counts at ~ 33 and ~ 40 GHz obtained from the analysis of the ERCSC downwards in flux density by a factor of ~ 5. Going down in flux density is important to control the contamination of CMB maps by faint radio sources. This table contains the catalog of 674 observations of 152 of the 159 sources that comprise the 'faint PACO sample'. Thus, each row in this table corresponds to a specific observation of a source, and there can be several rows for any source, corresponding to different observations. The ATCA observations were made in 6 2-GHz wide observing bands: 4732 - 6780 MHz, 8232 - 10280 MHz, 17232 - 19280 MHz, 23232 - 25280 MHz, 32232 - 34280 MHz and 38232 - 40280 MHz. In order to properly define the detailed source spectral behavior, the authors have split each 2-GHz band into 4 x 512 MHz sub-bands, and calibrated each sub-band independently. Thus, for each observation, the flux density at 24 frequencies is given. The frequency identifier in the flux density appears (at least to this HEASARC scientist) to be the lower frequency of the sub-band rather than its central frequency. In order to provide the easiest way to extrapolate the observed counts or model predictions from one frequency to another, the authors have modeled the observed source spectra. As their observations covered a wide frequency range from 4.5 to 40 GHz over which a single power law is not enough to describe the spectral behavior of the sources, they studied the spectra of the 174 point-like sources in this sample by fitting the observed data with a double power law of the form S<sub>nu</sub> = S<sub>0</sub>/[(nu/nu<sub>0</sub>)<sup>-a</sup> + (nu/nu<sub>0</sub>)<sup>-b</sup>], where nu is the frequency, S<sub>nu</sub> is the flux density in Jy, and S<sub>0</sub>, nu<sub>0</sub>, a and b are free parameters. The authors considered only those sources for which they had at least four data points for each of the 2 x 2 GHz bands considered. When observations at more than one epoch were available, the authors chose the one with the greatest number of data points. Full details of the fitting procedure are given in Section 3.1 of Massardi et al. (2011, MNRAS, 415, 1597) and Section 4 of the reference paper. This table was created by the HEASARC in January 2014 based on the machine-readable version of the Paco faint catalog from the reference paper which was obtained from the CDS (their catalog J/MNRAS/416/559 file catalog.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:
- 07 Mar 2025
- 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 (µJy) 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 <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/352/131">CDS Catalog J/MNRAS/352/131</a> 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:
- 07 Mar 2025
- 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:
- 07 Mar 2025
- 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 .
