https://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Compact_Source_catalogues&feed=atom&action=historyCompact Source catalogues - Revision history2024-03-29T08:26:29ZRevision history for this page on the wikiMediaWiki 1.31.6https://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Compact_Source_catalogues&diff=13854&oldid=prevDscott at 02:01, 2 July 20182018-07-02T02:01:01Z<p></p>
<table class="diff diff-contentalign-left" data-mw="interface">
<col class="diff-marker" />
<col class="diff-content" />
<col class="diff-marker" />
<col class="diff-content" />
<tr class="diff-title" lang="en-GB">
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 02:01, 2 July 2018</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l2" >Line 2:</td>
<td colspan="2" class="diff-lineno">Line 2:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The Planck Catalogue of Compact Sources (PCCS) is a set of single frequency lists of sources, both Galactic and extragalactic, extracted from the Planck maps.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The Planck Catalogue of Compact Sources (PCCS) is a set of single frequency lists of sources, both Galactic and extragalactic, extracted from the Planck maps.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>The first public version of the PCCS was derived from the nominal mission data acquired by Planck between 13 August 2009 and 26 November 2010, as described in {{PlanckPapers|planck2013-p05}}; it consisted of nine lists of sources, one per channel between 30 and 857 GHz. The second public version of the catalogue (PCCS2) has been produced using the full mission data obtained between 13 August 2009 and 3 August 2013, as described in {{PlanckPapers|planck2014-a35}}; it consists of fifteen lists of sources, one list per channel at 30, 44 and 70 GHz, and two lists per channel at 100, 143, 217, 353, 545 and 857 GHz.  </div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>The first public version of the PCCS was derived from the nominal mission data acquired by Planck between 13 August 2009 and 26 November 2010, as described in {{PlanckPapers|planck2013-p05}}; it consisted of nine lists of sources, one per channel between 30 and 857 GHz. The second public version of the catalogue (PCCS2) has been produced using the full mission data obtained between 13 August 2009 and 3 August 2013, as described in {{PlanckPapers|planck2014-a35}}; it consists of fifteen lists of sources, one list per channel at 30, 44<ins class="diffchange diffchange-inline">, </ins>and 70 GHz, and two lists per channel at 100, 143, 217, 353, 545<ins class="diffchange diffchange-inline">, </ins>and 857 GHz.  </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The maps used to produce these catalogues are the 2015 full mission frequency maps (LFI_SkyMap_0??_1024_R2.01_full.fits and HFI_SkyMap_???_2048_R2.00_full.fits).</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The maps used to produce these catalogues are the 2015 full mission frequency maps (LFI_SkyMap_0??_1024_R2.01_full.fits and HFI_SkyMap_???_2048_R2.00_full.fits).</div></td></tr>
</table>Dscotthttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Compact_Source_catalogues&diff=12425&oldid=prevDscott at 01:48, 12 January 20172017-01-12T01:48:37Z<p></p>
<table class="diff diff-contentalign-left" data-mw="interface">
<col class="diff-marker" />
<col class="diff-content" />
<col class="diff-marker" />
<col class="diff-content" />
<tr class="diff-title" lang="en-GB">
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 01:48, 12 January 2017</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l1" >Line 1:</td>
<td colspan="2" class="diff-lineno">Line 1:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Planck Catalogue of Compact Sources==</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Planck Catalogue of Compact Sources==</div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>The Planck Catalogue of Compact Sources is a set of single frequency lists of sources, both Galactic and extragalactic, extracted from the Planck maps.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>The Planck Catalogue of Compact Sources <ins class="diffchange diffchange-inline">(PCCS) </ins>is a set of single frequency lists of sources, both Galactic and extragalactic, extracted from the Planck maps.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The first public version of the PCCS was derived from the nominal mission data acquired by Planck between 13 August 2009 and 26 November 2010, as described in {{PlanckPapers|planck2013-p05}}; it consisted of nine lists of sources, one per channel between 30 and 857 GHz. The second public version of the catalogue (PCCS2) has been produced using the full mission data obtained between 13 August 2009 and 3 August 2013, as described in {{PlanckPapers|planck2014-a35}}; it consists of fifteen lists of sources, one list per channel at 30, 44 and 70 GHz, and two lists per channel at 100, 143, 217, 353, 545 and 857 GHz.  </div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The first public version of the PCCS was derived from the nominal mission data acquired by Planck between 13 August 2009 and 26 November 2010, as described in {{PlanckPapers|planck2013-p05}}; it consisted of nine lists of sources, one per channel between 30 and 857 GHz. The second public version of the catalogue (PCCS2) has been produced using the full mission data obtained between 13 August 2009 and 3 August 2013, as described in {{PlanckPapers|planck2014-a35}}; it consists of fifteen lists of sources, one list per channel at 30, 44 and 70 GHz, and two lists per channel at 100, 143, 217, 353, 545 and 857 GHz.  </div></td></tr>
</table>Dscotthttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Compact_Source_catalogues&diff=12424&oldid=prevDscott: /* Planck Catalogue of Compact Sources */2017-01-12T01:46:29Z<p><span dir="auto"><span class="autocomment">Planck Catalogue of Compact Sources</span></span></p>
<table class="diff diff-contentalign-left" data-mw="interface">
<col class="diff-marker" />
<col class="diff-content" />
<col class="diff-marker" />
<col class="diff-content" />
<tr class="diff-title" lang="en-GB">
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 01:46, 12 January 2017</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l65" >Line 65:</td>
<td colspan="2" class="diff-lineno">Line 65:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* Cirrus/ISM: The upper bands of HFI could be contaminated with sources associated with Galactic interstellar medium (ISM) features or cirrus. The values of the parameters, CIRRUS N and SKY BRIGHTNESS in the catalogues may be used as indicators of contamination. CIRRUS N may be used to flag sources that might be clustered together and thereby associated with ISM structure. In order to provide some indications of the range of values of these parameters that could indicate contamination, we compared the properties of the IRAS-identified and non-IRAS-identified sources for both the PCCS2 and the PCCS2E, since outside the Galactic plane at Galactic latitudes |<i>b</i>| > 20&deg;, we can use the Revised IRAS-FSC Redshift Catalogue (RIFSCz {{BibCite|wang2014}}) to provide a guide to the likely nature of sources. We cross-match the PCCS2 857-GHz catalogue and the PCCS2E 857-GHz catalogue with IRAS sources in the RIFSCz using a 3 arcmin matching radius. Of the 4891 sources in the PCCS2 857-GHz catalogue 3094 have plausible IRAS counterparts, while 1797 do not. Examination of histograms of the CIRRUS N and SKY BRIGHTNESS parameters in the PCCS2 show that these two classes of objects behave rather differently. The IRAS-identified sources have a peak sky brightness at about 1 MJy&thinsp;sr<sup>−1</sup>, while the non-IRAS-identified sources have a bimodal distribution with a slight peak at 1 MJy&thinsp;sr<sup>−1</sup> and a second peak at about 2.6 MJy&thinsp;sr<sup>−1</sup>. Both distributions have a long tail, but the non-IRAS-identified tail is much longer. On this basis, sources with SKY BRIGHTNESS > 4 MJy&thinsp;sr<sup>−1</sup> should be treated with caution. In contrast non-IRAS-identified sources with SKY BRIGHTNESS < 1.4 MJy&thinsp;sr<sup>−1</sup> are likely reliable. Examination of their sky distribution, for example, shows that many such sources lie in the IRAS coverage gaps. The CIRRUS N flag tells a rather similar story. Both IRAS-matched and IRAS non-matched sources have a peak CIRRUS N value of 2, but the non-matched sources have a far longer tail. Very few IRAS-matched sources have a value > 8, but many non- matched sources do; these should be treated with caution. The PCCS2E 857-GHz catalogue contains 10&thinsp;470 sources with |<i>b</i>| > 20&deg;, of which 1235 are matched to IRAS sources in the RIIFSCz and 9235 are not. As with the PCCS2 catalogue the distributions of CIRRUS N and SKY BRIGHTNESS are different, with the differences even more pronounced for these PCCS2E sources. Once again, few IRAS-matched sources have SKY BRIGHTNESS > 4 MJy&thinsp;sr<sup>−1</sup>, but the non-matched sources have brightnesses extending to > 55 MJy&thinsp;sr<sup>−1</sup>. Similarly, hardly any of the IRAS-matched sources have CIRRUS N > 8, but nearly half the unmatched sources do. The WHICH ZONE flag in the PCCS2E encodes the region in which the source sits, either inside the filament mask (WHICH ZONE=1), in the Galactic region (WHICH ZONE=2), or both (WHICH ZONE=3). Of the 9235 PCCS2E 857-GHz sources that do not match an IRAS source and that lie in the region |<i>b</i>| > 20&deg;, 1850 (20%) have WHICH ZONE=1, 2637 (29 %) have WHICH ZONE=2, and 4748 (51 %) have WHICH ZONE=3. The PCCS2E covers 30.36 % of the region |<i>b</i>| > 20&deg;, where 2.47 % is in the filament mask, 23.15 % in the Galactic region, and 4.74 % in both. If the 9235 unmatched detections were distributed uniformly over the region, |<i>b</i>| > 20&deg;, we can predict the number of non-matched sources in each zone and compare this to the values we have. We find that there are 2.5 and 3.3 times more sources than expected in zones 1 and 3, showing that the filament mask is indeed a useful criterion for regarding sources detected within it as suspicious. It should be noted that the EXTENDED flag could also be used to identify ISM features, but nearby Galactic and extragalactic sources that are extended at Planck spatial resolution will also meet this criterion.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* Cirrus/ISM: The upper bands of HFI could be contaminated with sources associated with Galactic interstellar medium (ISM) features or cirrus. The values of the parameters, CIRRUS N and SKY BRIGHTNESS in the catalogues may be used as indicators of contamination. CIRRUS N may be used to flag sources that might be clustered together and thereby associated with ISM structure. In order to provide some indications of the range of values of these parameters that could indicate contamination, we compared the properties of the IRAS-identified and non-IRAS-identified sources for both the PCCS2 and the PCCS2E, since outside the Galactic plane at Galactic latitudes |<i>b</i>| > 20&deg;, we can use the Revised IRAS-FSC Redshift Catalogue (RIFSCz {{BibCite|wang2014}}) to provide a guide to the likely nature of sources. We cross-match the PCCS2 857-GHz catalogue and the PCCS2E 857-GHz catalogue with IRAS sources in the RIFSCz using a 3 arcmin matching radius. Of the 4891 sources in the PCCS2 857-GHz catalogue 3094 have plausible IRAS counterparts, while 1797 do not. Examination of histograms of the CIRRUS N and SKY BRIGHTNESS parameters in the PCCS2 show that these two classes of objects behave rather differently. The IRAS-identified sources have a peak sky brightness at about 1 MJy&thinsp;sr<sup>−1</sup>, while the non-IRAS-identified sources have a bimodal distribution with a slight peak at 1 MJy&thinsp;sr<sup>−1</sup> and a second peak at about 2.6 MJy&thinsp;sr<sup>−1</sup>. Both distributions have a long tail, but the non-IRAS-identified tail is much longer. On this basis, sources with SKY BRIGHTNESS > 4 MJy&thinsp;sr<sup>−1</sup> should be treated with caution. In contrast non-IRAS-identified sources with SKY BRIGHTNESS < 1.4 MJy&thinsp;sr<sup>−1</sup> are likely reliable. Examination of their sky distribution, for example, shows that many such sources lie in the IRAS coverage gaps. The CIRRUS N flag tells a rather similar story. Both IRAS-matched and IRAS non-matched sources have a peak CIRRUS N value of 2, but the non-matched sources have a far longer tail. Very few IRAS-matched sources have a value > 8, but many non- matched sources do; these should be treated with caution. The PCCS2E 857-GHz catalogue contains 10&thinsp;470 sources with |<i>b</i>| > 20&deg;, of which 1235 are matched to IRAS sources in the RIIFSCz and 9235 are not. As with the PCCS2 catalogue the distributions of CIRRUS N and SKY BRIGHTNESS are different, with the differences even more pronounced for these PCCS2E sources. Once again, few IRAS-matched sources have SKY BRIGHTNESS > 4 MJy&thinsp;sr<sup>−1</sup>, but the non-matched sources have brightnesses extending to > 55 MJy&thinsp;sr<sup>−1</sup>. Similarly, hardly any of the IRAS-matched sources have CIRRUS N > 8, but nearly half the unmatched sources do. The WHICH ZONE flag in the PCCS2E encodes the region in which the source sits, either inside the filament mask (WHICH ZONE=1), in the Galactic region (WHICH ZONE=2), or both (WHICH ZONE=3). Of the 9235 PCCS2E 857-GHz sources that do not match an IRAS source and that lie in the region |<i>b</i>| > 20&deg;, 1850 (20%) have WHICH ZONE=1, 2637 (29 %) have WHICH ZONE=2, and 4748 (51 %) have WHICH ZONE=3. The PCCS2E covers 30.36 % of the region |<i>b</i>| > 20&deg;, where 2.47 % is in the filament mask, 23.15 % in the Galactic region, and 4.74 % in both. If the 9235 unmatched detections were distributed uniformly over the region, |<i>b</i>| > 20&deg;, we can predict the number of non-matched sources in each zone and compare this to the values we have. We find that there are 2.5 and 3.3 times more sources than expected in zones 1 and 3, showing that the filament mask is indeed a useful criterion for regarding sources detected within it as suspicious. It should be noted that the EXTENDED flag could also be used to identify ISM features, but nearby Galactic and extragalactic sources that are extended at Planck spatial resolution will also meet this criterion.</div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div><del style="font-weight: bold; text-decoration: none;"></del></div></td><td colspan="2"> </td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div><!--- ---------------------------------------></div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div><!--- ---------------------------------------></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
</table>Dscotthttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Compact_Source_catalogues&diff=12423&oldid=prevDscott at 01:43, 12 January 20172017-01-12T01:43:56Z<p></p>
<table class="diff diff-contentalign-left" data-mw="interface">
<col class="diff-marker" />
<col class="diff-content" />
<col class="diff-marker" />
<col class="diff-content" />
<tr class="diff-title" lang="en-GB">
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 01:43, 12 January 2017</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l31" >Line 31:</td>
<td colspan="2" class="diff-lineno">Line 31:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>In the PCCS2 we still have an 80% reliability goal, but a new approach has been followed. There was a demand for the possibility of producing an even higher reliability catalogue from Planck, and a new reliability flag was added to the catalogues for this purpose.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>In the PCCS2 we still have an 80% reliability goal, but a new approach has been followed. There was a demand for the possibility of producing an even higher reliability catalogue from Planck, and a new reliability flag was added to the catalogues for this purpose.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>In this version of the Planck catalogue of compact sources, for the 100 to 857 GHz channels, we split the catalogue into two, PCCS2 and PCCS2E, based on our ability to validate each of the sources.  </div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>In this version of the Planck catalogue of compact sources, for the 100 to 857<ins class="diffchange diffchange-inline">-</ins>GHz channels, we split the catalogue into two, PCCS2 and PCCS2E, based on our ability to validate each of the sources.  </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>For the lower frequencies, between 30 and 70 GHz, we still use an S/N threshold of 4. Moreover, as will be explained below, we use external catalogues and a multi-frequency analysis to validate the sources. For the higher frequency channels, at 100 GHz and above, there is very little external information available to validate the catalogues and the validation has instead been done statistically and by applying Galactic plane and cirrus masks.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>For the lower frequencies, between 30 and 70 GHz, we still use an S/N threshold of 4. Moreover, as will be explained below, we use external catalogues and a multi-frequency analysis to validate the sources. For the higher frequency channels, at 100 GHz and above, there is very little external information available to validate the catalogues and the validation has instead been done statistically and by applying Galactic plane and cirrus masks.</div></td></tr>
<tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l64" >Line 64:</td>
<td colspan="2" class="diff-lineno">Line 64:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* Colour correction: The flux density estimates have not been colour corrected. Colour corrections are described in {{PlanckPapers|planck2013-p02}}, {{PlanckPapers|planck2014-a03}}, {{PlanckPapers|planck2013-p03}}, and{{PlanckPapers|planck2014-a08}}.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* Colour correction: The flux density estimates have not been colour corrected. Colour corrections are described in {{PlanckPapers|planck2013-p02}}, {{PlanckPapers|planck2014-a03}}, {{PlanckPapers|planck2013-p03}}, and{{PlanckPapers|planck2014-a08}}.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>* Cirrus/ISM: The upper bands of HFI could be contaminated with sources associated with Galactic interstellar medium (ISM) features or cirrus. The values of the parameters, CIRRUS N and SKY BRIGHTNESS in the catalogues may be used as indicators of contamination. CIRRUS N may be used to flag sources that might be clustered together and thereby associated with ISM structure. In order to provide some indications of the range of values of these parameters that could indicate contamination, we compared the properties of the IRAS-identified and non-IRAS-identified sources for both the PCCS2 and the PCCS2E, since outside the Galactic plane at Galactic latitudes |<i>b</i>| > 20&deg;, we can use the Revised IRAS-FSC Redshift Catalogue (RIFSCz {{BibCite|wang2014}}) to provide a guide to the likely nature of sources. We cross-match the PCCS2 857-GHz catalogue and the PCCS2E 857-GHz catalogue with IRAS sources in the RIFSCz using a 3 arcmin matching radius. Of the 4891 sources in the PCCS2 857-GHz catalogue 3094 have plausible IRAS counterparts, while 1797 do not. Examination of histograms of the CIRRUS N and SKY BRIGHTNESS parameters in the PCCS2 show that these two classes of objects behave rather differently. The IRAS-identified sources have a peak sky brightness at about 1 MJy&thinsp;sr<sup>−1</sup>, while the non-IRAS-identified sources have a bimodal distribution with a slight peak at 1 MJy&thinsp;sr<sup>−1</sup> and a second peak at about 2.6 MJy&thinsp;sr<sup>−1</sup>. Both distributions have a long tail, but the non-IRAS-identified tail is much longer. On this basis, sources with SKY BRIGHTNESS > 4 MJy&thinsp;sr<sup>−1</sup> should be treated with caution. In contrast non-IRAS-identified sources with SKY BRIGHTNESS < 1.4 MJy&thinsp;sr<sup>−1</sup> are likely reliable. Examination of their sky distribution, for example, shows that many such sources lie in the IRAS coverage gaps. The CIRRUS N flag tells a rather similar story. Both IRAS-matched and IRAS non-matched sources have a peak CIRRUS N value of 2, but the non-matched sources have a far longer tail. Very few IRAS-matched sources have a value > 8, but many non- matched sources do; these should be treated with caution. The PCCS2E 857 GHz catalogue contains 10&thinsp;470 sources with |<i>b</i>| > 20&deg;, of which 1235 are matched to IRAS sources in the RIIFSCz and 9235 are not. As with the PCCS2 catalogue the distributions of CIRRUS N and SKY BRIGHTNESS are different, with the differences even more pronounced for these PCCS2E sources. Once again, few IRAS-matched sources have SKY BRIGHTNESS > 4 MJy&thinsp;sr<sup>−1</sup>, but the non-matched sources have brightnesses extending to > 55 MJy&thinsp;sr<sup>−1</sup>. Similarly, hardly any of the IRAS-matched sources have CIRRUS N > 8, but nearly half the unmatched sources do. The WHICH ZONE flag in the PCCS2E encodes the region in which the source sits, either inside the filament mask (WHICH ZONE=1), in the Galactic region (WHICH ZONE=2), or both (WHICH ZONE=3). Of the 9235 PCCS2E <del class="diffchange diffchange-inline">857GHz </del>sources that do not match an IRAS source and that lie in the region |<i>b</i>| > 20&deg;, 1850 (20%) have WHICH ZONE=1, 2637 (29 %) have WHICH ZONE=2, and 4748 (51 %) have WHICH ZONE=3. The PCCS2E covers 30.36 % of the region |<i>b</i>| > 20&deg;, where 2.47 % is in the filament mask, 23.15 % in the Galactic region, and 4.74 % in both. If the 9235 unmatched detections were distributed uniformly over the region, |<i>b</i>| > 20&deg;, we can predict the number of non-matched sources in each zone and compare this to the values we have. We find that there are 2.5 and 3.3 times more sources than expected in zones 1 and 3, showing that the filament mask is indeed a useful criterion for regarding sources detected within it as suspicious. It should be noted that the EXTENDED flag could also be used to identify ISM features, but nearby Galactic and extragalactic sources that are extended at Planck spatial resolution will also meet this criterion.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>* Cirrus/ISM: The upper bands of HFI could be contaminated with sources associated with Galactic interstellar medium (ISM) features or cirrus. The values of the parameters, CIRRUS N and SKY BRIGHTNESS in the catalogues may be used as indicators of contamination. CIRRUS N may be used to flag sources that might be clustered together and thereby associated with ISM structure. In order to provide some indications of the range of values of these parameters that could indicate contamination, we compared the properties of the IRAS-identified and non-IRAS-identified sources for both the PCCS2 and the PCCS2E, since outside the Galactic plane at Galactic latitudes |<i>b</i>| > 20&deg;, we can use the Revised IRAS-FSC Redshift Catalogue (RIFSCz {{BibCite|wang2014}}) to provide a guide to the likely nature of sources. We cross-match the PCCS2 857-GHz catalogue and the PCCS2E 857-GHz catalogue with IRAS sources in the RIFSCz using a 3 arcmin matching radius. Of the 4891 sources in the PCCS2 857-GHz catalogue 3094 have plausible IRAS counterparts, while 1797 do not. Examination of histograms of the CIRRUS N and SKY BRIGHTNESS parameters in the PCCS2 show that these two classes of objects behave rather differently. The IRAS-identified sources have a peak sky brightness at about 1 MJy&thinsp;sr<sup>−1</sup>, while the non-IRAS-identified sources have a bimodal distribution with a slight peak at 1 MJy&thinsp;sr<sup>−1</sup> and a second peak at about 2.6 MJy&thinsp;sr<sup>−1</sup>. Both distributions have a long tail, but the non-IRAS-identified tail is much longer. On this basis, sources with SKY BRIGHTNESS > 4 MJy&thinsp;sr<sup>−1</sup> should be treated with caution. In contrast non-IRAS-identified sources with SKY BRIGHTNESS < 1.4 MJy&thinsp;sr<sup>−1</sup> are likely reliable. Examination of their sky distribution, for example, shows that many such sources lie in the IRAS coverage gaps. The CIRRUS N flag tells a rather similar story. Both IRAS-matched and IRAS non-matched sources have a peak CIRRUS N value of 2, but the non-matched sources have a far longer tail. Very few IRAS-matched sources have a value > 8, but many non- matched sources do; these should be treated with caution. The PCCS2E 857<ins class="diffchange diffchange-inline">-</ins>GHz catalogue contains 10&thinsp;470 sources with |<i>b</i>| > 20&deg;, of which 1235 are matched to IRAS sources in the RIIFSCz and 9235 are not. As with the PCCS2 catalogue the distributions of CIRRUS N and SKY BRIGHTNESS are different, with the differences even more pronounced for these PCCS2E sources. Once again, few IRAS-matched sources have SKY BRIGHTNESS > 4 MJy&thinsp;sr<sup>−1</sup>, but the non-matched sources have brightnesses extending to > 55 MJy&thinsp;sr<sup>−1</sup>. Similarly, hardly any of the IRAS-matched sources have CIRRUS N > 8, but nearly half the unmatched sources do. The WHICH ZONE flag in the PCCS2E encodes the region in which the source sits, either inside the filament mask (WHICH ZONE=1), in the Galactic region (WHICH ZONE=2), or both (WHICH ZONE=3). Of the 9235 PCCS2E <ins class="diffchange diffchange-inline">857-GHz </ins>sources that do not match an IRAS source and that lie in the region |<i>b</i>| > 20&deg;, 1850 (20%) have WHICH ZONE=1, 2637 (29 %) have WHICH ZONE=2, and 4748 (51 %) have WHICH ZONE=3. The PCCS2E covers 30.36 % of the region |<i>b</i>| > 20&deg;, where 2.47 % is in the filament mask, 23.15 % in the Galactic region, and 4.74 % in both. If the 9235 unmatched detections were distributed uniformly over the region, |<i>b</i>| > 20&deg;, we can predict the number of non-matched sources in each zone and compare this to the values we have. We find that there are 2.5 and 3.3 times more sources than expected in zones 1 and 3, showing that the filament mask is indeed a useful criterion for regarding sources detected within it as suspicious. It should be noted that the EXTENDED flag could also be used to identify ISM features, but nearby Galactic and extragalactic sources that are extended at Planck spatial resolution will also meet this criterion.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div><!--- ---------------------------------------></div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div><!--- ---------------------------------------></div></td></tr>
<tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l87" >Line 87:</td>
<td colspan="2" class="diff-lineno">Line 87:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>A 2D Gaussian fit provides an estimate of the position angle and FWHM size along the major and minor axes. The ellipse defined by the FWHM values is used in aperture photometry to derive the flux density estimates in all four bands. Based on the quality of the flux density estimates in all four bands, PGCC sources are divided into three categories of FLUX_QUALITY:</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>A 2D Gaussian fit provides an estimate of the position angle and FWHM size along the major and minor axes. The ellipse defined by the FWHM values is used in aperture photometry to derive the flux density estimates in all four bands. Based on the quality of the flux density estimates in all four bands, PGCC sources are divided into three categories of FLUX_QUALITY:</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* FLUX_QUALITY=1, sources with flux density estimates at S/N > 1 in all bands ;</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* FLUX_QUALITY=1, sources with flux density estimates at S/N > 1 in all bands ;</div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>* FLUX_QUALITY=2, sources with flux density estimates at S/N > 1 only in 857, 545, and 353 GHz Planck bands, considered as very cold source candidates ;</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>* FLUX_QUALITY=2, sources with flux density estimates at S/N > 1 only in 857<ins class="diffchange diffchange-inline">-</ins>, 545<ins class="diffchange diffchange-inline">-</ins>, and 353<ins class="diffchange diffchange-inline">-</ins>GHz Planck bands, considered as very cold source candidates ;</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* FLUX_QUALITY=3, sources without any reliable flux density estimates, listed as poor candidates.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* FLUX_QUALITY=3, sources without any reliable flux density estimates, listed as poor candidates.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>We also set a flag for the blending between sources, which can be used to quantify the reliability of the aperture photometry processing.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>We also set a flag for the blending between sources, which can be used to quantify the reliability of the aperture photometry processing.</div></td></tr>
</table>Dscotthttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Compact_Source_catalogues&diff=12422&oldid=prevDscott: /* Catalogue of Planck Galactic Cold Clumps */2017-01-12T01:41:32Z<p><span dir="auto"><span class="autocomment">Catalogue of Planck Galactic Cold Clumps</span></span></p>
<table class="diff diff-contentalign-left" data-mw="interface">
<col class="diff-marker" />
<col class="diff-content" />
<col class="diff-marker" />
<col class="diff-content" />
<tr class="diff-title" lang="en-GB">
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 01:41, 12 January 2017</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l78" >Line 78:</td>
<td colspan="2" class="diff-lineno">Line 78:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>A union catalogue is constructed from the detections by all three pipelines. A mask to remove Galactic dust, nearby galaxies and point sources (leaving 83.7% of the sky) is applied a posteriori to avoid detections in areas where foregrounds are likely to cause spurious detections.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>A union catalogue is constructed from the detections by all three pipelines. A mask to remove Galactic dust, nearby galaxies and point sources (leaving 83.7% of the sky) is applied a posteriori to avoid detections in areas where foregrounds are likely to cause spurious detections.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>== Catalogue of <del class="diffchange diffchange-inline">''Planck'' </del>Galactic Cold Clumps ==</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>== <ins class="diffchange diffchange-inline">Planck </ins>Catalogue of Galactic Cold Clumps ==</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>The <del class="diffchange diffchange-inline">catalogue </del>of <del class="diffchange diffchange-inline">''Planck'' </del>Galactic Cold Clumps (PGCC) is a list of 13188 Galactic sources and 54 sources located in the Small and Large Magellanic Clouds, identified as cold sources in Planck data, as described in {{PlanckPapers|planck2014-a37}}. The sources are extracted with the CoCoCoDeT algorithm (Montier, 2010<!--{{BibCite|Montier2010}}-->), using Planck-HFI 857, 545, and 353 GHz maps and the 3 THz IRIS map  </div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>The <ins class="diffchange diffchange-inline">Planck Catalogue </ins>of Galactic Cold Clumps (PGCC) is a list of 13188 Galactic sources and 54 sources located in the Small and Large Magellanic Clouds, identified as cold sources in Planck data, as described in {{PlanckPapers|planck2014-a37}}. The sources are extracted with the CoCoCoDeT algorithm (Montier, 2010<!--{{BibCite|Montier2010}}-->), using Planck-HFI 857<ins class="diffchange diffchange-inline">-</ins>, 545<ins class="diffchange diffchange-inline">-</ins>, and 353<ins class="diffchange diffchange-inline">-</ins>GHz maps and the 3<ins class="diffchange diffchange-inline">-</ins>THz IRIS map  </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>(Miville 2005)<!--{{BibCite|Miville2005}}-->, an upgraded version of the IRAS data at 5 arcmin resolution. This is the first all-sky catalogue of Galactic cold sources obtained with homogeneous methods and data.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>(Miville 2005)<!--{{BibCite|Miville2005}}-->, an upgraded version of the IRAS data at 5 arcmin resolution. This is the first all-sky catalogue of Galactic cold sources obtained with homogeneous methods and data.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>The CoCoCoDeT detection algorithm uses the 3 THz map as a spatial template of a warm background component. Local estimates of the average colour of the background are derived at 30 arcmin resolution around each pixel of the maps at 857, 545, and 353 GHz. Together these describe a local warm component that is subtracted, leaving <del class="diffchange diffchange-inline"> </del>857, 545, and 353 GHz maps of the cold residual component map over the full sky. A point source detection algorithm is applied to these three maps. A detection requires S/N > 4 in pixels in all Planck bands and a minimum angular distance of 5 arcmin <del class="diffchange diffchange-inline">to </del>other detections.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>The CoCoCoDeT detection algorithm uses the 3<ins class="diffchange diffchange-inline">-</ins>THz map as a spatial template of a <ins class="diffchange diffchange-inline">"</ins>warm<ins class="diffchange diffchange-inline">" </ins>background component. Local estimates of the average colour of the background are derived at 30 arcmin resolution around each pixel of the maps at 857, 545, and 353 GHz. Together these describe a local warm component that is subtracted, leaving 857<ins class="diffchange diffchange-inline">-</ins>, 545<ins class="diffchange diffchange-inline">-</ins>, and 353<ins class="diffchange diffchange-inline">-</ins>GHz maps of the cold residual component map over the full sky. A point source detection algorithm is <ins class="diffchange diffchange-inline">then </ins>applied to these three maps. A detection requires S/N > 4 in pixels in all Planck bands and a minimum angular distance of 5 arcmin <ins class="diffchange diffchange-inline">from </ins>other detections.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>A 2D Gaussian fit provides an estimate of the position angle and FWHM size along the major and minor axes. The ellipse defined by the FWHM values is used in aperture photometry to derive the flux density estimates in all four bands. Based on the quality of the flux density estimates in all four bands, PGCC sources are divided into three categories of FLUX_QUALITY:</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>A 2D Gaussian fit provides an estimate of the position angle and FWHM size along the major and minor axes. The ellipse defined by the FWHM values is used in aperture photometry to derive the flux density estimates in all four bands. Based on the quality of the flux density estimates in all four bands, PGCC sources are divided into three categories of FLUX_QUALITY:</div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>* FLUX_QUALITY=1 <del class="diffchange diffchange-inline">: </del>sources with flux density estimates at S/N > 1 in all bands ;</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>* FLUX_QUALITY=1<ins class="diffchange diffchange-inline">, </ins>sources with flux density estimates at S/N > 1 in all bands ;</div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>* FLUX_QUALITY=2 <del class="diffchange diffchange-inline">: </del>sources with flux density estimates at S/N > 1 only in 857, 545, and 353 GHz Planck bands, considered as very cold source candidates ;</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>* FLUX_QUALITY=2<ins class="diffchange diffchange-inline">, </ins>sources with flux density estimates at S/N > 1 only in 857, 545, and 353 GHz Planck bands, considered as very cold source candidates ;</div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>* FLUX_QUALITY=3 <del class="diffchange diffchange-inline">: </del>sources without any reliable flux density estimates, listed as poor candidates.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>* FLUX_QUALITY=3<ins class="diffchange diffchange-inline">, </ins>sources without any reliable flux density estimates, listed as poor candidates.</div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>We also <del class="diffchange diffchange-inline">raise </del>a flag <del class="diffchange diffchange-inline">on </del>the blending between sources which can be used to quantify the reliability of the aperture photometry processing.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>We also <ins class="diffchange diffchange-inline">set </ins>a flag <ins class="diffchange diffchange-inline">for </ins>the blending between sources<ins class="diffchange diffchange-inline">, </ins>which can be used to quantify the reliability of the aperture photometry processing.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>To estimate possible contamination by extragalactic sources we (1) cross-correlated the positions with catalogues of extragalactic sources<del class="diffchange diffchange-inline">, </del>(2) rejected detections with SED <del class="diffchange diffchange-inline">[</del>in colour-colour plots<del class="diffchange diffchange-inline">] </del>consistent with radio sources<del class="diffchange diffchange-inline">, </del>and (3) rejected detections with clear association <del class="diffchange diffchange-inline">to </del>extragalactic sources visible in <del class="diffchange diffchange-inline">DSS </del>images. Compared to the original <del class="diffchange diffchange-inline">number of sources</del>, these only resulted in a small number of rejections.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>To estimate possible contamination by extragalactic sources we<ins class="diffchange diffchange-inline">: </ins>(1) cross-correlated the positions with catalogues of extragalactic sources<ins class="diffchange diffchange-inline">; </ins>(2) rejected detections with SED <ins class="diffchange diffchange-inline">(</ins>in colour-colour plots<ins class="diffchange diffchange-inline">) </ins>consistent with radio sources<ins class="diffchange diffchange-inline">; </ins>and (3) rejected detections with clear association <ins class="diffchange diffchange-inline">with </ins>extragalactic sources visible in <ins class="diffchange diffchange-inline">Digitized Sky Survey </ins>images. Compared to the original <ins class="diffchange diffchange-inline">catalogue</ins>, these only resulted in a small number of rejections.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Distance estimates, combining seven different methods, have been obtained for 5574 sources with estimates ranging from hundreds of pc in local molecular clouds up to 10.5 kpc along the Galactic plane.  The methods include cross-correlation with kinematic distances previously listed for infrared dark clouds (IRDCs)<del class="diffchange diffchange-inline">, </del>optical and near-infrared extinction using SDSS and 2MASS data, respectively<del class="diffchange diffchange-inline">, </del>association with molecular clouds with known distances<del class="diffchange diffchange-inline">, </del>and finally referencing parallel work done on a small sample of sources followed up with Herschel. Most PGCC sources appear to be located in the solar neighbourhood.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Distance estimates, combining seven different methods, have been obtained for 5574 sources<ins class="diffchange diffchange-inline">, </ins>with estimates ranging from hundreds of pc in local molecular clouds up to 10.5 kpc along the Galactic plane.  The methods include cross-correlation with kinematic distances previously listed for<ins class="diffchange diffchange-inline">: </ins>infrared dark clouds (IRDCs)<ins class="diffchange diffchange-inline">; </ins>optical and near-infrared extinction using SDSS and 2MASS data, respectively<ins class="diffchange diffchange-inline">; </ins>association with molecular clouds with known distances<ins class="diffchange diffchange-inline">; </ins>and finally referencing parallel work done on a small sample of sources followed up with Herschel. Most PGCC sources appear to be located in the solar neighbourhood.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>The derived physical properties of the PGCC sources are: temperature<del class="diffchange diffchange-inline">, </del>column density<del class="diffchange diffchange-inline">, </del>physical size<del class="diffchange diffchange-inline">, </del>mass<del class="diffchange diffchange-inline">, </del>density and luminosity.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>The derived physical properties of the PGCC sources are: temperature<ins class="diffchange diffchange-inline">; </ins>column density<ins class="diffchange diffchange-inline">; </ins>physical size<ins class="diffchange diffchange-inline">; </ins>mass<ins class="diffchange diffchange-inline">; </ins>density<ins class="diffchange diffchange-inline">; </ins>and luminosity.</div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>PGCC sources exhibit an average temperature of about 14K, and ranging from 5.8 to 20K. They span a large range of physical properties (such as column density, mass and density) covering a large varety of objects, from dense cold cores to large molecular clouds.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>PGCC sources exhibit an average temperature of about 14K, and ranging from 5.8 to 20K. They span a large range of physical properties (such as column density, mass<ins class="diffchange diffchange-inline">, </ins>and density) covering a large varety of objects, from dense cold cores to large molecular clouds.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>The validation of this catalogue has been performed with a Monte Carlo <del class="diffchange diffchange-inline">Quality Assessment </del>analysis wich allowed us to quantify the statistical reliability of the flux densities and of the source position and geometry estimates. The position accuracy is better than 0.2<del class="diffchange diffchange-inline">' </del>and 0.8<del class="diffchange diffchange-inline">' </del>for 68% and 95% of the sources, respectively, while the ellipticity of the sources is recovered with an accuracy better than 10% at 1<del class="diffchange diffchange-inline"><math>\</del>sigma<del class="diffchange diffchange-inline"></math></del>. This kind of analysis is also very powerful <del class="diffchange diffchange-inline">to characterize </del>the selection function of the CoCoCoDeT algorithm applied to Planck data. The completeness of the <del class="diffchange diffchange-inline">detection </del>has been studied as a function of the temperature of the injected sources. It has been shown that sources with FLUX_QUALITY=2 are effectively sources with low temperatures and have a high completeness level for temperatures below 10K.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>The validation of this catalogue has been performed with a Monte Carlo <ins class="diffchange diffchange-inline">quality assessment </ins>analysis wich allowed us to quantify the statistical reliability of the flux densities and of the source position and geometry estimates. The position accuracy is better than 0.2 <ins class="diffchange diffchange-inline">arcmin </ins>and 0.8 <ins class="diffchange diffchange-inline">arcmin </ins>for 68% and 95% of the sources, respectively, while the ellipticity of the sources is recovered with an accuracy better than 10% at 1<ins class="diffchange diffchange-inline">&</ins>sigma<ins class="diffchange diffchange-inline">;</ins>. This kind of analysis is also very powerful <ins class="diffchange diffchange-inline">for characterizing </ins>the selection function of the CoCoCoDeT algorithm applied to Planck data. The completeness of the <ins class="diffchange diffchange-inline">detections </ins>has been studied as a function of the temperature of the injected sources. It has been shown that sources with FLUX_QUALITY=2 are effectively sources with low temperatures and have a high completeness level for temperatures below 10K.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>We computed the cross-correlation between the PGCC catalogue and the other internal <del class="diffchange diffchange-inline">''</del>Planck<del class="diffchange diffchange-inline">'' </del>catalogues<del class="diffchange diffchange-inline">: </del>PCCS2, PCCS2E, PSZ and <del class="diffchange diffchange-inline">PH''z''</del>. The PGCC catalogue contains about 45% new sources, not simultaneously detected in the 857, 545, and 353 GHz bands of the PCCS2 and PCCS2E. A <del class="diffchange diffchange-inline">few </del>sources (65) are also detected in the PSZ2 and PGCC catalogues, suggesting <del class="diffchange diffchange-inline">a </del>dusty nature of these candidates. Finally there are only 15 sources in common between the PGCC and PHz (which is focused on extragalactic sources at high redshift), <del class="diffchange diffchange-inline">that </del>require further analysis to elucidate.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>We computed the cross-correlation between the PGCC catalogue and the other internal Planck catalogues<ins class="diffchange diffchange-inline">, i.e., </ins>PCCS2, PCCS2E, PSZ<ins class="diffchange diffchange-inline">, </ins>and <ins class="diffchange diffchange-inline">PHz</ins>. The PGCC catalogue contains about 45% new sources, not simultaneously detected in the 857, 545, and 353 GHz bands of the PCCS2 and PCCS2E. A <ins class="diffchange diffchange-inline">smaller number of </ins>sources (65) are also detected in the PSZ2 and PGCC catalogues, suggesting <ins class="diffchange diffchange-inline">the </ins>dusty nature of these candidates. Finally there are only 15 sources in common between the PGCC and PHz (which is focused on extragalactic sources at high redshift), <ins class="diffchange diffchange-inline">which </ins>require further analysis to elucidate.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>The PGCC catalogue contains <del class="diffchange diffchange-inline">also </del>54 sources located in the Small and Large Magellanic Clouds (SMC and LMC), two nearby galaxies <del class="diffchange diffchange-inline">which </del>are so close that we can identify individual clumps in them.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>The PGCC catalogue <ins class="diffchange diffchange-inline">also </ins>contains 54 sources located in the Small and Large Magellanic Clouds (SMC and LMC), two nearby galaxies <ins class="diffchange diffchange-inline">that </ins>are so close that we can identify individual clumps in them.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
</table>Dscotthttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Compact_Source_catalogues&diff=12421&oldid=prevDscott: /* Planck Catalogue of compact Sources */2017-01-12T01:33:04Z<p><span dir="auto"><span class="autocomment">Planck Catalogue of compact Sources</span></span></p>
<table class="diff diff-contentalign-left" data-mw="interface">
<col class="diff-marker" />
<col class="diff-content" />
<col class="diff-marker" />
<col class="diff-content" />
<tr class="diff-title" lang="en-GB">
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 01:33, 12 January 2017</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l1" >Line 1:</td>
<td colspan="2" class="diff-lineno">Line 1:</td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>==Planck Catalogue of <del class="diffchange diffchange-inline">compact </del>Sources==</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>==Planck Catalogue of <ins class="diffchange diffchange-inline">Compact </ins>Sources==</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The Planck Catalogue of Compact Sources is a set of single frequency lists of sources, both Galactic and extragalactic, extracted from the Planck maps.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The Planck Catalogue of Compact Sources is a set of single frequency lists of sources, both Galactic and extragalactic, extracted from the Planck maps.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<!-- diff cache key wiki_planck_legacy_archive:diff::1.12:old-12420:rev-12421 -->
</table>Dscotthttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Compact_Source_catalogues&diff=12420&oldid=prevDscott: /* Planck Sunyaev-Zeldovich catalogue */2017-01-12T01:32:29Z<p><span dir="auto"><span class="autocomment">Planck Sunyaev-Zeldovich catalogue</span></span></p>
<table class="diff diff-contentalign-left" data-mw="interface">
<col class="diff-marker" />
<col class="diff-content" />
<col class="diff-marker" />
<col class="diff-content" />
<tr class="diff-title" lang="en-GB">
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 01:32, 12 January 2017</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l68" >Line 68:</td>
<td colspan="2" class="diff-lineno">Line 68:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div><!--- ---------------------------------------></div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div><!--- ---------------------------------------></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>==Planck Sunyaev-Zeldovich <del class="diffchange diffchange-inline">catalogue</del>==</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>==Planck <ins class="diffchange diffchange-inline">Catalogue of </ins>Sunyaev-Zeldovich <ins class="diffchange diffchange-inline">Sources</ins>==</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>The Planck <del class="diffchange diffchange-inline">SZ catalogue </del>is a nearly full-sky list of SZ detections obtained from the Planck data. It is fully described in {{PlanckPapers|planck2013-p05a}} and {{PlanckPapers|planck2014-a36}}. The catalogue is derived from the HFI frequency channel maps after masking and filling the bright point sources (S/N &ge; 10) from the PCCS catalogues in those channels. Three detection pipelines were used to construct the catalogue, two implementations of the matched multi-filter (MMF) algorithm and PowellSnakes (PwS), a Bayesian algorithm. All three pipelines use a circularly symmetric pressure profile, the non-standard universal profile from {{BibCite|arnaud2010}}, in the detection approach.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>The Planck <ins class="diffchange diffchange-inline">Catalogue of Sunyaev-Zeldovich Sources (PSZ) </ins>is a nearly full-sky list of SZ detections obtained from the Planck data. It is fully described in {{PlanckPapers|planck2013-p05a}} and {{PlanckPapers|planck2014-a36}}. The catalogue is derived from the HFI frequency channel maps after masking and filling the bright point sources (S/N &ge; 10) from the PCCS catalogues in those channels. Three detection pipelines were used to construct the catalogue, two implementations of the matched multi-filter (MMF) algorithm and PowellSnakes (PwS), a Bayesian algorithm. All three pipelines use a circularly symmetric pressure profile, the non-standard universal profile from {{BibCite|arnaud2010}}, in the detection approach.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* MMF1 and MMF3 are full-sky implementations of the MMF algorithm. The matched filter optimizes the cluster detection using a linear combination of maps, which requires an estimate of the statistics of the contamination. It uses spatial filtering to suppress both foregrounds and noise, making use of the prior knowledge of the cluster pressure profile and thermal SZ spectrum.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* MMF1 and MMF3 are full-sky implementations of the MMF algorithm. The matched filter optimizes the cluster detection using a linear combination of maps, which requires an estimate of the statistics of the contamination. It uses spatial filtering to suppress both foregrounds and noise, making use of the prior knowledge of the cluster pressure profile and thermal SZ spectrum.</div></td></tr>
</table>Dscotthttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Compact_Source_catalogues&diff=12419&oldid=prevDscott: /* Planck Sunyaev-Zeldovich catalogue */2017-01-12T01:29:04Z<p><span dir="auto"><span class="autocomment">Planck Sunyaev-Zeldovich catalogue</span></span></p>
<table class="diff diff-contentalign-left" data-mw="interface">
<col class="diff-marker" />
<col class="diff-content" />
<col class="diff-marker" />
<col class="diff-content" />
<tr class="diff-title" lang="en-GB">
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 01:29, 12 January 2017</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l70" >Line 70:</td>
<td colspan="2" class="diff-lineno">Line 70:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Planck Sunyaev-Zeldovich catalogue==</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Planck Sunyaev-Zeldovich catalogue==</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>The Planck SZ catalogue is a nearly full-sky list of SZ detections obtained from the Planck data. It is fully described in {{PlanckPapers|planck2013-p05a}}<del class="diffchange diffchange-inline">, </del>{{PlanckPapers|planck2014-a36}}. The catalogue is derived from the HFI frequency channel maps after masking and filling the bright point sources (<del class="diffchange diffchange-inline">SNR >= </del>10) from the PCCS catalogues in those channels. Three detection pipelines were used to construct the catalogue, two implementations of the matched multi-filter (MMF) algorithm and PowellSnakes (PwS), a Bayesian algorithm. All three pipelines use a circularly symmetric pressure profile, the non-standard universal profile from {{BibCite|arnaud2010}}, in the detection.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>The Planck SZ catalogue is a nearly full-sky list of SZ detections obtained from the Planck data. It is fully described in {{PlanckPapers|planck2013-p05a}} <ins class="diffchange diffchange-inline">and </ins>{{PlanckPapers|planck2014-a36}}. The catalogue is derived from the HFI frequency channel maps after masking and filling the bright point sources (<ins class="diffchange diffchange-inline">S/N &ge; </ins>10) from the PCCS catalogues in those channels. Three detection pipelines were used to construct the catalogue, two implementations of the matched multi-filter (MMF) algorithm and PowellSnakes (PwS), a Bayesian algorithm. All three pipelines use a circularly symmetric pressure profile, the non-standard universal profile from {{BibCite|arnaud2010}}, in the detection <ins class="diffchange diffchange-inline">approach</ins>.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* MMF1 and MMF3 are full-sky implementations of the MMF algorithm. The matched filter optimizes the cluster detection using a linear combination of maps, which requires an estimate of the statistics of the contamination. It uses spatial filtering to suppress both foregrounds and noise, making use of the prior knowledge of the cluster pressure profile and thermal SZ spectrum.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* MMF1 and MMF3 are full-sky implementations of the MMF algorithm. The matched filter optimizes the cluster detection using a linear combination of maps, which requires an estimate of the statistics of the contamination. It uses spatial filtering to suppress both foregrounds and noise, making use of the prior knowledge of the cluster pressure profile and thermal SZ spectrum.</div></td></tr>
</table>Dscotthttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Compact_Source_catalogues&diff=12418&oldid=prevDscott: /* Cautionary notes */2017-01-12T01:27:20Z<p><span dir="auto"><span class="autocomment">Cautionary notes</span></span></p>
<table class="diff diff-contentalign-left" data-mw="interface">
<col class="diff-marker" />
<col class="diff-content" />
<col class="diff-marker" />
<col class="diff-content" />
<tr class="diff-title" lang="en-GB">
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 01:27, 12 January 2017</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l64" >Line 64:</td>
<td colspan="2" class="diff-lineno">Line 64:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* Colour correction: The flux density estimates have not been colour corrected. Colour corrections are described in {{PlanckPapers|planck2013-p02}}, {{PlanckPapers|planck2014-a03}}, {{PlanckPapers|planck2013-p03}}, and{{PlanckPapers|planck2014-a08}}.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* Colour correction: The flux density estimates have not been colour corrected. Colour corrections are described in {{PlanckPapers|planck2013-p02}}, {{PlanckPapers|planck2014-a03}}, {{PlanckPapers|planck2013-p03}}, and{{PlanckPapers|planck2014-a08}}.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>* Cirrus/ISM: The upper bands of HFI could be contaminated with sources associated with Galactic interstellar medium (ISM) features or cirrus. The values of the parameters, CIRRUS N and SKY BRIGHTNESS in the catalogues may be used as indicators of contamination. CIRRUS N may be used to flag sources that might be clustered together and thereby associated with ISM structure. In order to provide some indications of the range of values of these parameters that could indicate contamination, we compared the properties of the IRAS-identified and non-IRAS-identified sources for both the PCCS2 and the PCCS2E, since outside the Galactic plane at Galactic latitudes |<i>b</i>| > 20&deg;, we can use the Revised IRAS-FSC Redshift Catalogue (RIFSCz {{BibCite|wang2014}}) to provide a guide to the likely nature of sources. We cross-match the PCCS2 857-GHz catalogue and the PCCS2E 857-GHz catalogue with IRAS sources in the RIFSCz using a 3 arcmin matching radius. Of the 4891 sources in the PCCS2 857-GHz catalogue 3094 have plausible IRAS counterparts, while 1797 do not. Examination of histograms of the CIRRUS N and SKY BRIGHTNESS parameters in the PCCS2 show that these two classes of objects behave rather differently. The IRAS-identified sources have a peak sky brightness at about 1 MJy&thinsp;sr<sup>−1</sup>, while the non-IRAS-identified sources have a bimodal distribution with a slight peak at 1 MJy&thinsp;sr<sup>−1</sup> and a second peak at about 2.6 MJy&thinsp;sr<sup>−1</sup>. Both distributions have a long tail, but the non-IRAS-identified tail is much longer. On this basis, sources with SKY BRIGHTNESS > 4 MJy&thinsp;sr<sup>−1</sup> should be treated with caution. In contrast non-IRAS-identified sources with SKY BRIGHTNESS < 1.4 MJy&thinsp;sr<sup>−1</sup> are likely reliable. Examination of their sky distribution, for example, shows that many such sources lie in the IRAS coverage gaps. The CIRRUS N flag tells a rather similar story. Both IRAS-matched and IRAS non-matched sources have a peak CIRRUS N value of 2, but the non-matched sources have a far longer tail. Very few IRAS-matched sources have a value > 8, but many non- matched sources do; these should be treated with caution. The PCCS2E 857 GHz catalogue contains 10&thinsp;470 sources with |<i>b</i>| > 20&deg;, of which 1235 are matched to IRAS sources in the RIIFSCz and 9235 are not. As with the PCCS2 catalogue the distributions of CIRRUS N and SKY BRIGHTNESS are different, with the differences even more pronounced for these PCCS2E sources. Once again, few IRAS-matched sources have SKY BRIGHTNESS > MJy&thinsp;sr<sup>−1</sup>, but the non-matched sources have brightnesses extending to >55 MJy&thinsp;sr<sup>−1</sup>. Similarly, hardly any of the IRAS-matched sources have CIRRUS N > 8, but nearly half the unmatched sources do. The WHICH ZONE flag in the PCCS2E encodes the region in which the source sits, either inside the filament mask (WHICH ZONE=1), in the Galactic region (WHICH ZONE=2), or both (WHICH ZONE=3). Of the 9235 PCCS2E 857GHz sources that do not match an IRAS source and that lie in the region<del class="diffchange diffchange-inline">, </del>|<i>b</i>| > 20&deg;, 1850 (20%) have WHICH ZONE=1, 2637 (29 %) have WHICH ZONE=2, and 4748 (51 %) have WHICH ZONE=3. The PCCS2E covers 30.36 % of the region |<i>b</i>| > 20&deg;, where 2.47 % is in the filament mask, 23.15 % in the Galactic region, and 4.74 % in both. If the 9235 unmatched detections were distributed uniformly over the region, |<i>b</i>| > 20&deg;, we can predict the number of non-matched sources in each zone and compare this to the values we have. We find that there are 2.5 and 3.3 times more sources than expected in zones 1 and 3, showing that the filament mask is indeed a useful criterion for regarding sources detected within it as suspicious. It should be noted that the EXTENDED flag could also be used to identify ISM features, but nearby Galactic and extragalactic sources that are extended at Planck spatial resolution will also meet this criterion.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>* Cirrus/ISM: The upper bands of HFI could be contaminated with sources associated with Galactic interstellar medium (ISM) features or cirrus. The values of the parameters, CIRRUS N and SKY BRIGHTNESS in the catalogues may be used as indicators of contamination. CIRRUS N may be used to flag sources that might be clustered together and thereby associated with ISM structure. In order to provide some indications of the range of values of these parameters that could indicate contamination, we compared the properties of the IRAS-identified and non-IRAS-identified sources for both the PCCS2 and the PCCS2E, since outside the Galactic plane at Galactic latitudes |<i>b</i>| > 20&deg;, we can use the Revised IRAS-FSC Redshift Catalogue (RIFSCz {{BibCite|wang2014}}) to provide a guide to the likely nature of sources. We cross-match the PCCS2 857-GHz catalogue and the PCCS2E 857-GHz catalogue with IRAS sources in the RIFSCz using a 3 arcmin matching radius. Of the 4891 sources in the PCCS2 857-GHz catalogue 3094 have plausible IRAS counterparts, while 1797 do not. Examination of histograms of the CIRRUS N and SKY BRIGHTNESS parameters in the PCCS2 show that these two classes of objects behave rather differently. The IRAS-identified sources have a peak sky brightness at about 1 MJy&thinsp;sr<sup>−1</sup>, while the non-IRAS-identified sources have a bimodal distribution with a slight peak at 1 MJy&thinsp;sr<sup>−1</sup> and a second peak at about 2.6 MJy&thinsp;sr<sup>−1</sup>. Both distributions have a long tail, but the non-IRAS-identified tail is much longer. On this basis, sources with SKY BRIGHTNESS > 4 MJy&thinsp;sr<sup>−1</sup> should be treated with caution. In contrast non-IRAS-identified sources with SKY BRIGHTNESS < 1.4 MJy&thinsp;sr<sup>−1</sup> are likely reliable. Examination of their sky distribution, for example, shows that many such sources lie in the IRAS coverage gaps. The CIRRUS N flag tells a rather similar story. Both IRAS-matched and IRAS non-matched sources have a peak CIRRUS N value of 2, but the non-matched sources have a far longer tail. Very few IRAS-matched sources have a value > 8, but many non- matched sources do; these should be treated with caution. The PCCS2E 857 GHz catalogue contains 10&thinsp;470 sources with |<i>b</i>| > 20&deg;, of which 1235 are matched to IRAS sources in the RIIFSCz and 9235 are not. As with the PCCS2 catalogue the distributions of CIRRUS N and SKY BRIGHTNESS are different, with the differences even more pronounced for these PCCS2E sources. Once again, few IRAS-matched sources have SKY BRIGHTNESS > <ins class="diffchange diffchange-inline">4 </ins>MJy&thinsp;sr<sup>−1</sup>, but the non-matched sources have brightnesses extending to > 55 MJy&thinsp;sr<sup>−1</sup>. Similarly, hardly any of the IRAS-matched sources have CIRRUS N > 8, but nearly half the unmatched sources do. The WHICH ZONE flag in the PCCS2E encodes the region in which the source sits, either inside the filament mask (WHICH ZONE=1), in the Galactic region (WHICH ZONE=2), or both (WHICH ZONE=3). Of the 9235 PCCS2E 857GHz sources that do not match an IRAS source and that lie in the region |<i>b</i>| > 20&deg;, 1850 (20%) have WHICH ZONE=1, 2637 (29 %) have WHICH ZONE=2, and 4748 (51 %) have WHICH ZONE=3. The PCCS2E covers 30.36 % of the region |<i>b</i>| > 20&deg;, where 2.47 % is in the filament mask, 23.15 % in the Galactic region, and 4.74 % in both. If the 9235 unmatched detections were distributed uniformly over the region, |<i>b</i>| > 20&deg;, we can predict the number of non-matched sources in each zone and compare this to the values we have. We find that there are 2.5 and 3.3 times more sources than expected in zones 1 and 3, showing that the filament mask is indeed a useful criterion for regarding sources detected within it as suspicious. It should be noted that the EXTENDED flag could also be used to identify ISM features, but nearby Galactic and extragalactic sources that are extended at Planck spatial resolution will also meet this criterion.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div><!--- ---------------------------------------></div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div><!--- ---------------------------------------></div></td></tr>
</table>Dscotthttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Compact_Source_catalogues&diff=12417&oldid=prevDscott: /* Cautionary notes */2017-01-12T01:23:55Z<p><span dir="auto"><span class="autocomment">Cautionary notes</span></span></p>
<table class="diff diff-contentalign-left" data-mw="interface">
<col class="diff-marker" />
<col class="diff-content" />
<col class="diff-marker" />
<col class="diff-content" />
<tr class="diff-title" lang="en-GB">
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 01:23, 12 January 2017</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l58" >Line 58:</td>
<td colspan="2" class="diff-lineno">Line 58:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* Contamination from CO: At infrared/submillimetre frequencies (100 GHz and above), the Planck bandpasses straddle energetically significant CO lines (see {{PlanckPapers|planck2013-p03a}}). The effect is the most significant at 100 GHz, where the line might contribute more than 50% of the measured flux density of some sources. Follow-up observations of these sources, especially those associated with Galactic star-forming regions, at a similar frequency but with a different bandpass, should correct for the potential contribution of line emission to the measured continuum flux density of the source.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* Contamination from CO: At infrared/submillimetre frequencies (100 GHz and above), the Planck bandpasses straddle energetically significant CO lines (see {{PlanckPapers|planck2013-p03a}}). The effect is the most significant at 100 GHz, where the line might contribute more than 50% of the measured flux density of some sources. Follow-up observations of these sources, especially those associated with Galactic star-forming regions, at a similar frequency but with a different bandpass, should correct for the potential contribution of line emission to the measured continuum flux density of the source.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>* Bandpass corrections: For many sources in the three lowest Planck frequency channels, the bandpass correction of the <i>Q</i> and <i>U</i> flux densities is not negligible. Even though we have attempted to correct for this effect on a source by source basis and have propagated this uncertainty into the error bars on the polarized flux densities and polarization angles, there is still room for improvement. This can be seen in the residual leakage present at the position of Taurus A in the Stokes U maps. It is anticipated that there will be future updates to the LFI PCCS2 catalogues once the bandpass corrections and errors have been improved.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>* Bandpass corrections: For many sources in the three lowest Planck frequency channels, the bandpass correction of the <i>Q</i> and <i>U</i> flux densities is not negligible. Even though we have attempted to correct for this effect on a source by source basis and have propagated this uncertainty into the error bars on the polarized flux densities and polarization angles, there is still room for improvement. This can be seen in the residual leakage present at the position of Taurus A in the Stokes <ins class="diffchange diffchange-inline"><i></ins>U<ins class="diffchange diffchange-inline"></i> </ins>maps. It is anticipated that there will be future updates to the LFI PCCS2 catalogues once the bandpass corrections and errors have been improved.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* Photometry: Each source has multiple estimates of flux density, DETFLUX, APERFLUX, GAUFLUX, and PSFFLUX, as defined above. The evaluation of APERFLUX makes the smallest number of assumptions about the data and hence is the most robust, (especially in regions of high non-Gaussian background emission), but it may have larger uncertainties than the other methods. For bright resolved sources, GAUFLUX is recommended, with the caveat that it may not be robust for sources close to the Galactic plane due to the strong backgrounds. We have noticed that at the position of some of the brightest sources in polarization there is a small spurious signal related to the complex beams in polarization. This signal can have a small impact on the measurements of the flux densities in <i>Q</i> and/or <i>U</i>. In particular, this spurious signal can affect the polarization position angle in those objects where most of the flux density of the source happens to be in one of the <i>Q</i> or <i>U</i> maps (like in the Crab Nebula). In {{PlanckPapers|planck2014-a35}} we discuss an extensive analysis of the Crab Nebula, exploring different ways to remove this effect, but the polarization angles of the other sources in the catalogue have to be used with caution.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* Photometry: Each source has multiple estimates of flux density, DETFLUX, APERFLUX, GAUFLUX, and PSFFLUX, as defined above. The evaluation of APERFLUX makes the smallest number of assumptions about the data and hence is the most robust, (especially in regions of high non-Gaussian background emission), but it may have larger uncertainties than the other methods. For bright resolved sources, GAUFLUX is recommended, with the caveat that it may not be robust for sources close to the Galactic plane due to the strong backgrounds. We have noticed that at the position of some of the brightest sources in polarization there is a small spurious signal related to the complex beams in polarization. This signal can have a small impact on the measurements of the flux densities in <i>Q</i> and/or <i>U</i>. In particular, this spurious signal can affect the polarization position angle in those objects where most of the flux density of the source happens to be in one of the <i>Q</i> or <i>U</i> maps (like in the Crab Nebula). In {{PlanckPapers|planck2014-a35}} we discuss an extensive analysis of the Crab Nebula, exploring different ways to remove this effect, but the polarization angles of the other sources in the catalogue have to be used with caution.</div></td></tr>
<tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l64" >Line 64:</td>
<td colspan="2" class="diff-lineno">Line 64:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* Colour correction: The flux density estimates have not been colour corrected. Colour corrections are described in {{PlanckPapers|planck2013-p02}}, {{PlanckPapers|planck2014-a03}}, {{PlanckPapers|planck2013-p03}}, and{{PlanckPapers|planck2014-a08}}.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* Colour correction: The flux density estimates have not been colour corrected. Colour corrections are described in {{PlanckPapers|planck2013-p02}}, {{PlanckPapers|planck2014-a03}}, {{PlanckPapers|planck2013-p03}}, and{{PlanckPapers|planck2014-a08}}.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>* Cirrus/ISM: The upper bands of HFI could be contaminated with sources associated with Galactic interstellar medium (ISM) features or cirrus. The values of the parameters, CIRRUS N and SKY BRIGHTNESS in the catalogues may be used as indicators of contamination. CIRRUS N may be used to flag sources that might be clustered together and thereby associated with ISM structure. In order to provide some indications of the range of values of these parameters that could indicate contamination, we compared the properties of the IRAS-identified and non-IRAS-identified sources for both the PCCS2 and the PCCS2E, since outside the Galactic plane at Galactic latitudes |<i>b</i>| > 20&deg;, we can use the Revised IRAS-FSC Redshift Catalogue (RIFSCz {{BibCite|wang2014}}) to provide a guide to the likely nature of sources. We cross-match the PCCS2 857-GHz catalogue and the PCCS2E 857-GHz catalogue with IRAS sources in the RIFSCz using a 3 arcmin matching radius. Of the 4891 sources in the PCCS2 857-GHz catalogue 3094 have plausible IRAS counterparts, while 1797 do not. Examination of histograms of the CIRRUS N and SKY BRIGHTNESS parameters in the PCCS2 show that these two classes of objects behave rather differently. The IRAS-identified sources have a peak sky brightness at about 1 MJy&<del class="diffchange diffchange-inline">puncsp</del>;sr<sup>−1</sup>, while the non-IRAS-identified sources have a bimodal distribution with a slight peak at 1 MJy&<del class="diffchange diffchange-inline">puncsp</del>;sr<sup>−1</sup> and a second peak at about 2.6 MJy&<del class="diffchange diffchange-inline">puncsp</del>;sr<sup>−1</sup>. Both distributions have a long tail, but the non-IRAS-identified tail is much longer. On this basis, sources with SKY BRIGHTNESS > 4 MJy&<del class="diffchange diffchange-inline">puncsp</del>;sr<sup>−1</sup> should be treated with caution. In contrast non-IRAS-identified sources with SKY BRIGHTNESS < 1.4 MJy&<del class="diffchange diffchange-inline">puncsp</del>;sr<sup>−1</sup> are likely reliable. Examination of their sky distribution, for example, shows that many such sources lie in the IRAS coverage gaps. The CIRRUS N flag tells a rather similar story. Both IRAS-matched and IRAS non-matched sources have a peak CIRRUS N value of 2, but the non-matched sources have a far longer tail. Very few IRAS-matched sources have a value > 8, but many non- matched sources do; these should be treated with caution. The PCCS2E 857 GHz catalogue contains 10&<del class="diffchange diffchange-inline">puncsp</del>;470 sources with |<i>b</i>| > 20&deg;, of which 1235 are matched to IRAS sources in the RIIFSCz and 9235 are not. As with the PCCS2 catalogue the distributions of CIRRUS N and SKY BRIGHTNESS are different, with the differences even more pronounced for these PCCS2E sources. Once again, few IRAS-matched sources have SKY BRIGHTNESS > MJy&<del class="diffchange diffchange-inline">puncsp</del>;sr<sup>−1</sup>, but the non-matched sources have brightnesses extending to >55 MJy&<del class="diffchange diffchange-inline">puncsp</del>;sr<sup>−1</sup>. Similarly, hardly any of the IRAS-matched sources have CIRRUS N > 8, but nearly half the unmatched sources do. The WHICH ZONE flag in the PCCS2E encodes the region in which the source sits, either inside the filament mask (WHICH ZONE=1), in the Galactic region (WHICH ZONE=2), or both (WHICH ZONE=3). Of the 9235 PCCS2E 857GHz sources that do not match an IRAS source and that lie in the region, |<i>b</i>| > 20&deg;, 1850 (20%) have WHICH ZONE=1, 2637 (29 %) have WHICH ZONE=2, and 4748 (51 %) have WHICH ZONE=3. The PCCS2E covers 30.36 % of the region |<i>b</i>| > 20&deg;, where 2.47 % is in the filament mask, 23.15 % in the Galactic region, and 4.74 % in both. If the 9235 unmatched detections were distributed uniformly over the region, |<i>b</i>| > 20&deg;, we can predict the number of non-matched sources in each zone and compare this to the values we have. We find that there are 2.5 and 3.3 times more sources than expected in zones 1 and 3, showing that the filament mask is indeed a useful criterion for regarding sources detected within it as suspicious. It should be noted that the EXTENDED flag could also be used to identify ISM features, but nearby Galactic and extragalactic sources that are extended at Planck spatial resolution will also meet this criterion.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>* Cirrus/ISM: The upper bands of HFI could be contaminated with sources associated with Galactic interstellar medium (ISM) features or cirrus. The values of the parameters, CIRRUS N and SKY BRIGHTNESS in the catalogues may be used as indicators of contamination. CIRRUS N may be used to flag sources that might be clustered together and thereby associated with ISM structure. In order to provide some indications of the range of values of these parameters that could indicate contamination, we compared the properties of the IRAS-identified and non-IRAS-identified sources for both the PCCS2 and the PCCS2E, since outside the Galactic plane at Galactic latitudes |<i>b</i>| > 20&deg;, we can use the Revised IRAS-FSC Redshift Catalogue (RIFSCz {{BibCite|wang2014}}) to provide a guide to the likely nature of sources. We cross-match the PCCS2 857-GHz catalogue and the PCCS2E 857-GHz catalogue with IRAS sources in the RIFSCz using a 3 arcmin matching radius. Of the 4891 sources in the PCCS2 857-GHz catalogue 3094 have plausible IRAS counterparts, while 1797 do not. Examination of histograms of the CIRRUS N and SKY BRIGHTNESS parameters in the PCCS2 show that these two classes of objects behave rather differently. The IRAS-identified sources have a peak sky brightness at about 1 MJy&<ins class="diffchange diffchange-inline">thinsp</ins>;sr<sup>−1</sup>, while the non-IRAS-identified sources have a bimodal distribution with a slight peak at 1 MJy&<ins class="diffchange diffchange-inline">thinsp</ins>;sr<sup>−1</sup> and a second peak at about 2.6 MJy&<ins class="diffchange diffchange-inline">thinsp</ins>;sr<sup>−1</sup>. Both distributions have a long tail, but the non-IRAS-identified tail is much longer. On this basis, sources with SKY BRIGHTNESS > 4 MJy&<ins class="diffchange diffchange-inline">thinsp</ins>;sr<sup>−1</sup> should be treated with caution. In contrast non-IRAS-identified sources with SKY BRIGHTNESS < 1.4 MJy&<ins class="diffchange diffchange-inline">thinsp</ins>;sr<sup>−1</sup> are likely reliable. Examination of their sky distribution, for example, shows that many such sources lie in the IRAS coverage gaps. The CIRRUS N flag tells a rather similar story. Both IRAS-matched and IRAS non-matched sources have a peak CIRRUS N value of 2, but the non-matched sources have a far longer tail. Very few IRAS-matched sources have a value > 8, but many non- matched sources do; these should be treated with caution. The PCCS2E 857 GHz catalogue contains 10&<ins class="diffchange diffchange-inline">thinsp</ins>;470 sources with |<i>b</i>| > 20&deg;, of which 1235 are matched to IRAS sources in the RIIFSCz and 9235 are not. As with the PCCS2 catalogue the distributions of CIRRUS N and SKY BRIGHTNESS are different, with the differences even more pronounced for these PCCS2E sources. Once again, few IRAS-matched sources have SKY BRIGHTNESS > MJy&<ins class="diffchange diffchange-inline">thinsp</ins>;sr<sup>−1</sup>, but the non-matched sources have brightnesses extending to >55 MJy&<ins class="diffchange diffchange-inline">thinsp</ins>;sr<sup>−1</sup>. Similarly, hardly any of the IRAS-matched sources have CIRRUS N > 8, but nearly half the unmatched sources do. The WHICH ZONE flag in the PCCS2E encodes the region in which the source sits, either inside the filament mask (WHICH ZONE=1), in the Galactic region (WHICH ZONE=2), or both (WHICH ZONE=3). Of the 9235 PCCS2E 857GHz sources that do not match an IRAS source and that lie in the region, |<i>b</i>| > 20&deg;, 1850 (20%) have WHICH ZONE=1, 2637 (29 %) have WHICH ZONE=2, and 4748 (51 %) have WHICH ZONE=3. The PCCS2E covers 30.36 % of the region |<i>b</i>| > 20&deg;, where 2.47 % is in the filament mask, 23.15 % in the Galactic region, and 4.74 % in both. If the 9235 unmatched detections were distributed uniformly over the region, |<i>b</i>| > 20&deg;, we can predict the number of non-matched sources in each zone and compare this to the values we have. We find that there are 2.5 and 3.3 times more sources than expected in zones 1 and 3, showing that the filament mask is indeed a useful criterion for regarding sources detected within it as suspicious. It should be noted that the EXTENDED flag could also be used to identify ISM features, but nearby Galactic and extragalactic sources that are extended at Planck spatial resolution will also meet this criterion.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div><!--- ---------------------------------------></div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div><!--- ---------------------------------------></div></td></tr>
<!-- diff cache key wiki_planck_legacy_archive:diff::1.12:old-12416:rev-12417 -->
</table>Dscott