The Planck Catalogue of Galactic Cold Clumps

Transcription

1 The Planck Catalogue of Galactic Cold Clumps L. Montier on behalf of the Cold Core Project

2 I Overview History of the PGCC 2007: First meeting about the detection method 2009: First internal release with 30% of Planck data Used to select the 3 sources of the Herschel SDP call (Science Demonstration Phase) 2010: CoCoCoDeT method Method package released to IPAC Herschel Selection from PGCC internal release 2011: First official release of the subsample ECC: 915 sources Statistical analysis on full PGCC on PGCC 2015: Official release of the PGCC ( Montier et al ) ( Planck Collaboration VII 2011 ) ( Planck Collaboration XXII & XXIII 2011 ) ( Planck Collaboration XXVIII 2015 )

3 I Overview Planck L. Montier Cold Core Meeting

4 II The PGCC Catalogue Detection Method CoCoCoDeT: Warm Background removal Wavelet filtering Montier et al. 2010

5 II The PGCC Catalogue Detection Method Data : Planck Data Release 2015 Official full mission (48 months) 857 x 545 x 353 GHz IRIS 100um 857GHz Method: Improved CoCoCoDeT Catalogue Band Merging Final Catalog IRAS 100 um 545GHz + 353GHz L. Montier Cold Core Meeting

6 II The PGCC Catalogue All-sky Catalogue sources Planck Collaboration XXVIII 2015

7 II The PGCC Catalogue Photometry Quality Classification of the Flux Density Quality: Flux Quality Flag = 1 S3000 / σ3000 > 1 S857 / σ857 > 1 S545 / σ545 > 1 S353 / σ353 > 1 All freq OK Flux Quality Flag = 2 S3000 / σ3000 < 1 S857 / σ857 > 1 S545 / σ545 > 1 S353 / σ353 > 1 No 100um Flux Quality Flag = 3 No reliable flux Bad shape fit Detection only

8 II The PGCC Catalogue Photometry Quality FQ =

9 II The PGCC Catalogue Photometry Quality FQ =

10 II The PGCC Catalogue Photometry Quality FQ =

11 II The PGCC Catalogue Extra-Galactic Contamination Color Rejection: S353 / S545 > 0.9 (typical of flat radio spectrum) XCheck with Extra-Galactic Catalogues: Messier NGC IC 3C & 4C Optical Counter-parts: Borders of extended galaxies Sources Rejected

12 II The PGCC Catalogue Nearby Hot Sources Contamination CoCoCoDeT method applies detection on the Cold Residual maps Sources colder than their environment Nearby Hot Sources may produce temperature gradient Detection of spurious or warm sources 100um 857GHz Cold Residual Hot Source False Detection?

13 II The PGCC Catalogue Nearby Hot Sources Contamination Building Catalogue of warm sources: Detection of sources applied on the Warm Residual = - Cold Residual Warm sources 6569 X-correlation between C3PO & Warm Rejection: If distance Hot-Cold < 5 48 rejections Flag: If 5 < distance Hot-Cold < flagged sources

14 II The PGCC Catalogue X-Check with Planck Catalogues Planck PCCS (2015) 45% of PGCC sources newly identified! => PGCC deeper catalogue of Cold sources Planck ECC (2011) 97.5% of ECC sources in PGCC sources rejected due to increased robustness. Planck SZ (2013) 0.5 % of PGCC correlation 4% of PSZ contaminated by Galactic sources?

15 III PGCC properties 1. Kinematic: Xcheck with Simon et al 2006 Distance Estimates Comparison 2. Optical Extinction: SDSS Data 4 sub-methods (Peregrine s analysis) 4. NIR Extinction: Xcheck towards IRDCs 2MASS data (Doug s analysis) 5. Molecular Complexes: 11 complexes 6. Herschel-KP estimates: (Julien s analysis)

16 III PGCC properties Distance Estimates Methods are prioritized as above Comparison Check consistency between estimates: Estimates within 1 sigma are OK Distance Quality Flag 1 = Few consistent estimates 2 = Single estimate 3 = Few inconsistent estimates 4 = Upper-Limit only

17 III PGCC properties Distance Estimates 5574 Inhomogeneous..

18 III PGCC properties Galactic Distribution Observations: Close to the solar neighbourhood A few far objects (up to 7kpc) Highly inhomogeneous Perspectives: Extended Kinematic estimates using Molecular Follow-Up MOPRA / APEX... Use of Gaia & new Besançon Model Update of optical extinction?

19 III PGCC properties Temperature: <T> = 14K Cold sources Physical Properties NH2 : Large range of column density Size : Highly correlated with distance. Mass : Highly correlated with distance. No physical distribution

20 III PGCC properties Physical Properties Correlation between D & size D & Mass IRDCs

21 III PGCC properties Physical Properties Monte Carlo Simulations True Distribution T No sources with T < 8K at Planck 5 resolution M We reached the Mass detection limit

22 III PGCC properties Wide Range of Physical Properties 90 % of sources with T < 16.7 K 50 % of sources with T < 14.2 K Angular size close to Planck beam Mo < Mass < 5.7x104 Mo 4.1 cm-3 < n < 3.9x104 cm-3 Size [log pc] Core Clumps Clouds T [K] Classification by Williams et al Mass [log M] 1 Density [log cm -3 ]

23 III PGCC properties Wide Range of Physical Properties 90 % of sources with T < 16.7 K 50 % of sources with T < 14.2 K Angular size close to Planck beam Mo < Mass < 5.7x104 Mo 4.1 cm-3 < n < 3.9x104 cm-3 Size [log pc] Core Clumps Clouds C3PO T [K] Classification by Williams et al Mass [log M] 1 Density [log cm -3 ]

24 IV Herschel Follow-up Cores PGCC vs Herschel sources PGCC detections trace the densest and coldest Herschel sources Composed by multiple sources, YSO and starless sources

25 Perspectives Classification Learning Algorithms using WISE data (Gabor? ) X-correlation with other catalogues Physical Properties T-beta analysis (Claude?) Filament analysis on Planck Data X-correlation with AKARI filaments (Yasuo) HI Loop analysis (Sarolta) New distance estimates? Polarization analysis with Planck p decreament by stacking analysis (Isabelle) Correlation between B filed and Herschel Point Sources (Julien) Application of the detection method to other data Herschel surveys