J/A+A/688/A20 COSMOS2020-MIPS-PACS-SPIRE-SCUBA catalog (Wang+, 2024)
Probabilistic and progressive deblended far-infrared and
sub-millimetre point source catalogues.
I. Methodology and first application in the COSMOS field.
Wang L., La Marca A., Gao F., Pearson W.J., Margalef-Bentabol B.,
Bethermin M., Bing L., Donnellan J., Hurley P.D., Oliver S.J., Hale C.L.,
Jarvis M.J., Marchetti L., Vaccari M., Whittam I.H.
<Astron. Astrophys. 688, A20 (2024)>
=2024A&A...688A..20W 2024A&A...688A..20W (SIMBAD/NED BibCode)
ADC_Keywords: Galaxy catalogs ; Photometry, millimetric/submm
Keywords: catalogs - surveys - galaxies: general
Abstract:
Single-dish far-infrared (far-IR) and sub-millimetre (sub-mm) point
source catalogues and their connections with galaxy catalogues at
other wavelengths are of paramount importance to studying galaxy
evolution. However, due to the large mismatch in spatial resolution,
cross-matching galaxies detected at different wavelengths is not
straightforward.
This work aims to develop the next-generation deblended far-IR and
sub-mm catalogues in deep extragalactic survey fields, by extracting
photometry at the positions of known sources. We present the first
application of our methodology in the COSMOS field.
Our progressive deblending used the Monte Carlo Markov Chain
(MCMC)-based Bayesian probabilistic framework known as XID+. The
deblending process started from the Spitzer/MIPS 24um data, using an
initial prior list composed of sources selected from the COSMOS2020
catalogue and radio catalogues from the VLA and the MeerKAT surveys,
based on spectral energy distribution (SED) modelling which predicts
fluxes of the known sources at the deblending wavelength. To speed up
flux prediction, we made use of a neural network-based emulator. After
deblending the 24um data, we proceeded to the Herschel PACS (100 &
160um) and SPIRE wavebands (250, 350 & 500um). Each time we
constructed a tailor-made prior list based on the predicted fluxes of
the known sources, taking into account the deblended photometry from
the previous steps.
Using simulated far-IR and sub-mm sky, we detailed the performance of
our deblending pipeline. After validation with simulations, we then
deblended the real observations from 24 to 500um and compared with
blindly extracted catalogues and previous versions of deblended
catalogues. As an additional test, we deblended the SCUBA-2 850um map
and compared our deblended fluxes with ALMA measurements,
demonstrating a higher level of flux accuracy compared to previous
results. We publicly release our XID+ deblended point source
catalogues, including best estimates and posterior probability
distribution functions. These deblended long-wavelength data, which
are cross-matched with multi-band photometry by construction, are
crucial for studies such as deriving the fraction of dust-obscured
star formation and better separation of quiescent galaxies from dusty
star-forming galaxies.
Description:
Based on testing using realistic simulations of the far-IR and sub-mm
sky, we have demonstrated the good performance of our deblending
methodology. For the Spitzer/MIPS 24um map and the Herschel/PACS 100 &
160um maps which are dominated by instrument noise, we can deblend
fluxes which are median unbiased and have approximately Gaussian
uncertainties all the way down to the 1 instrument noise. For the
Herschel/SPIRE maps which are dominated by confusion noise, we show
that with our deblending methodology we can deblend fluxes down to
roughly the 1σ confusion noise. There is a slight systematic
flux underestimation towards faint flux levels, which reaches
approximately 10%, 15% and 25% at 250, 350 and 500um, respectively,
for the faintest sources. After testing with simulations, we deblend
the real data and compare with previous blindly extracted catalogues
and the super-deblended catalogue from Jin et al.
(2018ApJ...864...56J 2018ApJ...864...56J, Cat. J/ApJ/864/56). As an additional test, we
deblend the SCUBA-2 850um and test our deblended photometry using ALMA
Band 7 continuum measurements. We present our XID+ deblended far-IR
and sub-mm point source catalogues.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
master.dat 322 131178 Master catalogue MIPS PACS SPIRE SCUBA
(table 4)
master_post.fits 2880 5484163 Master post catalogue MIPS PACS SPIRE SCUBA
--------------------------------------------------------------------------------
See also:
J/ApJ/864/56 : "Super-deblended" dust emission in gal. II. COSMOS (Jin+, 2018)
J/ApJS/258/11 : The COSMOS2020 catalog (Weaver+, 2022)
Byte-by-byte Description of file: master.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 I7 --- ID COSMOS2020 ID
(negative numbers for radio sources) (ID)
9- 23 F15.11 deg RAdeg Right Ascension (J2000) from COSMOS2020
(or radio positions) (RA)
25- 39 F15.11 deg DEdeg Declination (J2000) from COSMOS2020
(or radio positions) (Dec)
41- 49 F9.6 mJy F24 24um flux density (median) (F_24)
51- 58 F8.6 mJy/beam Sigconf24 Fitted Background of 24um map (median)
(Sigconf24)
60- 67 F8.6 mJy s_F24 Maximum of sigma+ and sigma- for
24um flux density (FErr241sig)
69- 76 F8.6 mJy/beam e_F24 Total error for 24um flux density
(Sigtot24)
78- 87 F10.6 mJy F100 ?=- 100um flux density (median) (F_100)
89- 98 F10.6 mJy F160 ?=- 160um flux density (median) (F_160)
100-108 F9.6 mJy/beam Sigconf100 ?=- Fitted Background of 100um map
(median) (Sigconf100)
110-118 F9.6 mJy/beam Sigconf160 ?=- Fitted Background of 160um map
(median) (Sigconf160)
120-127 F8.6 mJy s_F100 ?=- Maximum of sigma+ and sigma- for
100um flux density (FErr1001sig)
129-137 F9.6 mJy/beam e_F100 ?=- Total error for 100um flux density
(Sigtot100)
139-147 F9.6 mJy s_F160 ?=- Maximum of sigma+ and sigma- for
160um flux density (FErr1601sig)
149-157 F9.6 mJy/beam e_F160 ?=- Total error for 160um flux density
(Sigtot160)
159-169 F11.6 mJy F250 ?=- 250um flux density (median) (F_250)
171-180 F10.6 mJy F350 ?=- 350um flux density (median) (F_350)
182-191 F10.6 mJy F500 ?=- 500um flux density (median) (F_500)
193-200 F8.5 mJy/beam Sigconf250 ?=- Fitted Background of 250um map
(median) (Sigconf250)
202-209 F8.5 mJy/beam Sigconf350 ?=- Fitted Background of 350um map
(median) (Sigconf350)
211-219 F9.6 mJy/beam Sigconf500 ?=- Fitted Background of 500um map
(median) (Sigconf500)
221-229 F9.6 mJy s_F250 ?=- Maximum of sigma+ and sigma- for
250um flux density (FErr2501sig)
231-239 F9.6 mJy/beam e_F250 ?=- Total error for 250um flux density
(Sigtot250)
241-249 F9.6 mJy s_F350 ?=- Maximum of sigma+ and sigma- for
350um flux density (FErr3501sig)
251-259 F9.6 mJy/beam e_F350 ?=- Total error for 350um flux density
(Sigtot350)
261-269 F9.6 mJy s_F500 ?=- Maximum of sigma+ and sigma- for
500um flux density (Err5001sig)
271-279 F9.6 mJy/beam e_F500 ?=- Total error for 500um flux density
(Sigtot500)
281-289 F9.6 mJy F850 ?=- 850um flux density (median) (F_850)
291-301 F11.6 mJy/beam Sigconf850 ?=- Fitted Background of 850um map
(median) (Sigconf850)
303-310 F8.6 mJy s_F850 ?=- Maximum of sigma+ and sigma- for
850um flux density (FErr8501sig)
312-322 F11.6 mJy/beam e_F850 ?=- Total error for 850um flux density
(Sigtot850)
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Description of file: master_post.fits
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Column Units Label Explanations
--------------------------------------------------------------------------------
1 --- ID COSMOS2020 ID
(negative numbers for radio sources) (ID)
2 deg RAdeg Right Ascension (J2000) from COSMOS2020
(or radio positions) (RA)
3 deg DEdeg Declination (J2000) from COSMOS2020
(or radio positions) (Dec)
4 mJy F24 24um flux density (median) (F_24)
5 mJy E_F24 24um flux density 84th Percentile (FErr24u)
6 mJy e_F24 24um flux density 16th Percentile (FErr24l)
7 mJy/beam Bkg24 Fitted Background of 24um map (median) (Bkg_24)
8 MJy/beam Sigconf24 Fitted Background of 24um map (median)
(Sigconf24)
9 mJy et_F24 Maximum of sigma+ and sigma- for
24um flux density (FErr241sig)
10 mJy/beam s_F24 Total error for 24um flux density (Sigtot24)
11 --- Rhat24 24um Convergence Statistic (ideally < 1.2)
(Rhat_24)
12 --- Neff24 24um Number of effective samples (ideally > 40)
(neff24)
13 mJy Post24 3000 samplings from the posterior PDF of the
24um flux density (Post_24) (3000E13.6)
14 --- tileMIPS ?=- MIPS tile number
15 mJy F100 ?=- 100um flux density (median) (F_100)
16 mJy E_F100 ?=- 100um flux density 84th Percentile
(FErr100u)
17 mJy e_F100 ?=- 100um flux density 16th Percentile
(FErr100l)
18 mJy F160 ?=- 160um flux density (median) (F_100)
19 mJy E_F160 ?=- 160um flux density 84th Percentile
(FErr160u)
20 mJy e_F160 ?=- 160um flux density 16th Percentile
(FErr160l)
21 mJy/beam Bkg100 ?=- Fitted Background of 100um map (median)
(Bkg_100)
22 mJy/beam Bkg160 ?=- Fitted Background of 160um map (median)
(Bkg_160)
23 mJy/beam Sigconf100 ?=- Fitted Background of 100um map (median)
(Sigconf100)
24 mJy/beam Sigconf160 ?=- Fitted Background of 160um map (median)
(Sigconf160)
25 mJy et_F100 ?=- Maximum of sigma+ and sigma- for
100um flux density (FErr1001sig)
26 mJy/beam s_F100 ?=- Total error for 100um flux density
(Sigtot100)
27 mJy et_F160 ?=- Maximum of sigma+ and sigma- for
160um flux density (FErr1601sig)
28 mJy/beam s_F160 ?=- Total error for 160um flux density
(Sigtot160)
29 --- Rhat100 ?=- 24um Convergence Statistic (ideally < 1.2)
(Rhat_100)
30 --- Rhat160 ?=- 24um Convergence Statistic (ideally < 1.2)
(Rhat_160)
31 --- Neff100 ?=- 24um Number of effective samples
(ideally > 40) (neff24)
32 --- Neff160 ?=- 24um Number of effective samples
(ideally > 40) (neff160)
33 --- Post100 ?=- 3000 samplings from the posterior PDF of
the 100um flux density (Post_100)
34 --- Post160 ?=- 3000 samplings from the posterior PDF of
the 160um flux density (Post_160)
35 --- tilePACS ?=- PACS tile number
36 mJy F250 ?=- 150um flux density (median) (F_250)
37 mJy E_F250 ?=- 150um flux density 84th Percentile
(FErr250u)
38 mJy e_F250 ?=- 150um flux density 16th Percentile
(FErr250l)
39 mJy F350 ?=- 350um flux density (median) (F_350)
40 mJy E_F350 ?=- 350um flux density 84th Percentile
(FErr350u)
41 mJy e_F350 ?=- 350um flux density 16th Percentile
(FErr350l)
42 mJy F500 ?=- 500um flux density (median) (F_500)
43 mJy E_F500 ?=- 500um flux density 84th Percentile
(FErr500u)
44 mJy e_F500 ?=- 500um flux density 16th Percentile
(FErr500l)
45 mJy/beam Bkg250 ?=- Fitted Background of 250um map (median)
(Bkg_250)
46 mJy/beam Bkg350 ?=- Fitted Background of 350um map (median)
(Bkg_350)
47 mJy/beam Bkg500 ?=- Fitted Background of 500um map (median)
(Bkg_500)
48 mJy/beam Sigconf250 ?=- Fitted Background of 250um map (median)
(Sigconf250)
49 mJy/beam Sigconf350 ?=- Fitted Background of 350um map (median)
(Sigconf350)
50 mJy/beam Sigconf500 ?=- Fitted Background of 24um map (median)
(Sigconf24)
51 mJy et_F250 ?=- Maximum of sigma+ and sigma- for
250um flux density (FErr2501sig)
52 mJy/beam s_F250 ?=- Total error for 250um flux density
(Sigtot250)
53 mJy et_F350 ?=- Maximum of sigma+ and sigma- for
350um flux density (FErr3501sig)
54 mJy/beam s_F350 ?=- Total error for 350um flux density
(Sigtot350)
55 mJy et_F500 ?=- Maximum of sigma+ and sigma- for
500um flux density (FErr5001sig)
56 mJy/beam s_F500 ?=- Total error for 500um flux density
(Sigtot500)
57 --- Rhat250 ?=- 250um Convergence Statistic (ideally < 1.2)
(Rhat_250)
58 --- Rhat350 ?=- 350um Convergence Statistic (ideally < 1.2)
(Rhat_350)
59 --- Rhat500 ?=- 500um Convergence Statistic (ideally < 1.2)
(Rhat_500)
60 --- Neff250 ?=- 250um Number of effective samples
(ideally > 40) (neff250)
61 --- Neff350 ?=- 350um Number of effective samples
(ideally > 40) (neff350)
62 --- Neff500 ?=- 500um Number of effective samples
(ideally > 40) (neff500)
63 --- Post250 ?=- 3000 samplings from the posterior PDF of
the 250um flux density (Post_250)
64 --- Post350 ?=- 3000 samplings from the posterior PDF of
the 350um flux density (Post_350)
65 --- Post500 ?=- 3000 samplings from the posterior PDF of
the 500um flux density (Post_500)
66 --- tileSPIRE ?=- SPIRE tile number
67 mJy F850 ?=- 850um flux density (median) (F_850)
68 mJy E_F850 ?=- 850um flux density 84th Percentile
(FErr850u)
69 mJy e_F850 ?=- 850um flux density 16th Percentile
(FErr850l)
70 mJy/beam Bkg850 ?=- Fitted Background of 850um map (median)
(Bkg_850)
71 mJy/beam Sigconf850 ?=- Fitted Background of 850um map (median)
(Sigconf850)
72 mJy et_F850 ?=- Maximum of sigma+ and sigma- for
850um flux density (FErr8501sig)
73 mJy/beam s_F850 ?=- Total error for 850um flux density
(Sigtot850)
74 --- Rhat850 ?=- 850um Convergence Statistic (ideally < 1.2)
(Rhat_850)
75 --- Neff850 ?=- 850um Number of effective samples
(ideally > 40) (neff850)
76 --- Post850 ?=- 3000 samplings from the posterior PDF of
the 850um flux density (Post_850)
77 --- tileSCUBA ?=- SCUBAD tile number
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Acknowledgements:
Lingyu Wang, L.Wang(at)sron.nl
(End) Patricia Vannier [CDS] 04-Jun-2024