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WMAPITNPTS - WMAP 7-Year Internal Templates and Needlets New Source Catalog

HEASARC
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Overview

The authors have developed a new needlet-based method to detect point sources in cosmic microwave background (CMB) maps and have applied it to the Wilkinson Microwave Anisotropy Probe (WMAP) 7-year data. They use both the individual frequency channels as well as internal templates, the latter being the difference between pairs of frequency channels and hence having the advantage that the CMB component is eliminated. Using the area of the sky outside the Kq85 galactic mask, they detect a total of 2102 point sources at the 5-sigma level in either the frequency maps or the internal templates. Of these, 1116 are detected either at 5 sigma directly in the frequency channels or at 5 sigma in the internal templates and >= 3 sigma at the corresponding position in the frequency channels. Of the 1116 sources, 603 are detections that have not been reported so far in WMAP data. The authors have made a catalog of these sources available with position and flux estimated in the WMAP channels where they are seen. In total, they identified 1029 of the 1116 sources with counterparts at 5 GHz and 69 at other frequencies.

Catalog Bibcode

2012ApJ...753...27S

References

Detection of new point sources in WMAP 7 year data using internal templates
     and needlets.
     Scodeller S., Hansen F.K., Marinucci D.
    <Astrophys. J. 753, 27 (2012)>
    = 2012ApJ...753...27S

Provenance

This table was created by the HEASARC in July 2012 based on an electronic version of Table 6 from the reference paper which was obtained from the ApJ web site.

HEASARC Implementation

The HEASARC has converted all flux densities and their associated errors from the Jy units given in the original table into the mJy units which it uses as its standard for tables with radio- and mm-band flux densities.

Parameters

Source_Number
A running source number in order of increasing J2000.0 Right Ascension which uniquely identifies each source in the catalog.

Name
The source designation. The HEASARC created this field using the prefix '[SHM2012]' (for Scodeller, Hansen, Marinucci 2012) and the source number, in the style recommended by the Dictionary of Nomenclature of Celestial Objects.

RA
The Right Ascension of the point source in the selected equinox, given by the weighted average of the positions in all frequencies where the source was found. This was giben in J2000.0 decimal degrees to a precision of 1 millidegree in the original table. Based on the results of simulations, these positions should be accurate to a few arcminutes.

Dec
The Declination of the point source in the selected equinox, given by the weighted average of the positions in all frequencies where the source was found. This was giben in J2000.0 decimal degrees to a precision of 1 millidegree in the original table. Based on the results of simulations, these positions should be accurate to a few arcminutes.

LII
The Galactic Longitude of the point source.

BII
The Galactic Latitude of the point source.

Flux_23_GHz
The K-band (22.5 GHz) flux density of the WMAP source, in mJy. The flux densities were specified to a precision of 0.01 Jy (10 mJy) in the original table. For converting the source temperature and errors from Kelvin to Jansky, the authors used the effective beam area and relative error as presented in Table 4 of Jarosik et al. (2011, ApJS, 192, 14).

Flux_23_GHz_Error
The uncertainty in the corresponding flux density, in mJy.

Flux_23_GHz_Flag
This flag parameter is set to 'i' to indicate very weak sources for which the authors were unable to correct the corresponding flux for Eddington bias due to the low S/N level. In such cases, they used the internal template to estimate the unbiased flux in the given channel, as explained in Section 4.3 of the reference paper.

Flux_30_GHz
The Ka-band (30 GHz) flux density of the WMAP source, in mJy. The flux densities were specified to a precision of 0.01 Jy (10 mJy) in the original table. For converting the source temperature and errors from Kelvin to Jansky, the authors used the effective beam area and relative error as presented in Table 4 of Jarosik et al. (2011, ApJS, 192, 14).

Flux_30_GHz_Error
The uncertainty in the corresponding flux density, in mJy.

Flux_30_GHz_Flag
This flag parameter is set to 'i' to indicate very weak sources for which the authors were unable to correct the corresponding flux for Eddington bias due to the low S/N level. In such cases, they used the internal template to estimate the unbiased flux in the given channel, as explained in Section 4.3 of the reference paper.

Flux_41_GHz
The Q-band (41 GHz) flux density of the WMAP source, in mJy. The flux densities were specified to a precision of 0.01 Jy (10 mJy) in the original table. For converting the source temperature and errors from Kelvin to Jansky, the authors used the effective beam area and relative error as presented in Table 4 of Jarosik et al. (2011, ApJS, 192, 14).

Flux_41_GHz_Error
The uncertainty in the corresponding flux density, in mJy.

Flux_41_GHz_Flag
This flag parameter is set to 'i' to indicate very weak sources for which the authors were unable to correct the corresponding flux for Eddington bias due to the low S/N level. In such cases, they used the internal template to estimate the unbiased flux in the given channel, as explained in Section 4.3 of the reference paper.

Flux_61_GHz
The V-band (61 GHz) flux density of the WMAP source, in mJy. The flux densities were specified to a precision of 0.01 Jy (10 mJy) in the original table. For converting the source temperature and errors from Kelvin to Jansky, the authors used the effective beam area and relative error as presented in Table 4 of Jarosik et al. (2011, ApJS, 192, 14).

Flux_61_GHz_Error
The uncertainty in the corresponding flux density, in mJy.

Flux_61_GHz_Flag
This flag parameter is set to 'i' to indicate very weak sources for which the authors were unable to correct the corresponding flux for Eddington bias due to the low S/N level. In such cases, they used the internal template to estimate the unbiased flux in the given channel, as explained in Section 4.3 of the reference paper.

Flux_94_GHz
The W-band (94 GHz) flux density of the WMAP source, in mJy. The flux densities were specified to a precision of 0.01 Jy (10 mJy) in the original table. For converting the source temperature and errors from Kelvin to Jansky, the authors used the effective beam area and relative error as presented in Table 4 of Jarosik et al. (2011, ApJS, 192, 14).

Flux_94_GHz_Error
The uncertainty in the corresponding flux density, in mJy.

Flux_94_GHz_Flag
This flag parameter is set to 'i' to indicate very weak sources for which the authors were unable to correct the corresponding flux for Eddington bias due to the low S/N level. In such cases, they used the internal template to estimate the unbiased flux in the given channel, as explained in Section 4.3 of the reference paper.

Detection_Flags
This parameter contains 5 flags, one for each frequency channel (K, Ka, Q, V, W), indicating whether the authors detected the source at 5 sigma in the individual channel ('C'), or in the template with a 3-sigma detection in the channel ('F'), or not at all ('.').

Catalog_Flags
This parameter contains up to 3 flags, indicating if the found source has been identified with a known source in the specified catalog in at least one frequency, using the following catalog codes:

      W = WMAP 7-Year Catalog (Gold et al. 2011, ApJS, 192, 15);
      N = NEWPS-5yr-5s Catalog (Massardi et al. 2009, MNRAS, 392, 733);
      P = Planck Early Release Compact Source (ERCSC) Catalogs
          at 30,44,70,100 GHz only (Planck Collaboration 2011, A&A, 536, A7).
  
The upper limit for cross-identification was 15 arcminutes.

Alt_Name
The identification with the GB6 Catalog (Gregory et al. 1996, ApJS, 103, 427), the PMN Catalog (Griffith et al 1994, ApJS, 90, 179; 1995, ApJS, 97, 347); Wright et al. 1994, ApJS, 91, 111; 1996, ApJS, 103, 145), or the 1 Jy Catalog (Kuehr et al. 1981, A&AS, 45, 367) when possible or else with the lower frequency NVSS (Condon et al. 1998, AJ, 115, 1693) and SUMSS (Mauch et al. 2003, MNRAS, 342, 1117) Catalog counterparts.

Offset
The angular offset, in arcminutes, of the source from the position in the identification in the indicated catalog.

Source_Flag
This parameter contains up to 2 flags, indicating source weakness and/or confusion. A flag value of 'M' is used if there are multiple possible identifications (where the authors took the brightest one) and a flag value of 'A' is used if the listed counterpart has a flux density below 100 mJy.


Contact Person

Questions regarding the WMAPITNPTS database table can be addressed to the HEASARC User Hotline.

Page Author: Browse Software Development Team
Last Modified: 25-Jul-2012