J/MNRAS/486/4166 SCUBA-2 850µm component of JINGLE (Smith+, 2019)
JINGLE, a JCMT legacy survey of dust and gas for galaxy evolution studies:
II. SCUBA-2 850 µm data reduction and dust flux density catalogues.
Smith M.W.L., Clark C.J.R., De Looze I., Lamperti I., Saintonge A.,
Wilson C.D., Accurso G., Brinks E., Bureau M., Chung E.J., Cigan P.J.,
Clements D.L., Dharmawardena T., Fanciullo L., Gao Y., Gao Y., Gear W.K.,
Gomez H.L., Greenslade J., Hwang H.S., Kemper F., Lee J.C., Li C., Lin L.,
Liu L., Molnar D.C., Mok A., Pan H.-A., Sargent M., Scicluna P.,
Smith C.M.A., Urquhart S., Williams T.G., Xiao T., Yang C., Zhu M.
<Mon. Not. R. Astron. Soc., 486, 4166-4185 (2019)>
=2019MNRAS.486.4166S 2019MNRAS.486.4166S (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, photometry ; Galaxy catalogs ; Photometry, infrared ;
Photometry, millimetric/submm
Keywords: galaxies: ISM - galaxies: photometry - galaxies: spiral -
submillimetre: ISM
Abstract:
We present the SCUBA-2 850µm component of JINGLE, the new JCMT
large survey for dust and gas in nearby galaxies, which with 193
galaxies is the largest targeted survey of nearby galaxies at
850µm. We provide details of our SCUBA-2 data reduction pipeline,
optimized for slightly extended sources, and including a calibration
model adjusted to match conventions used in other far-infrared (FIR)
data. We measure total integrated fluxes for the entire JINGLE sample
in 10 infrared/submillimetre bands, including all WISE, Herschel-PACS,
Herschel-SPIRE, and SCUBA-2 850µm maps, statistically accounting
for the contamination by CO(J=3-2) in the 850µm band. Of our
initial sample of 193 galaxies, 191 are detected at 250µm with a
≥5σ significance. In the SCUBA-2 850µm band we detect 126
galaxies with ≥3σ significance. The distribution of the JINGLE
galaxies in FIR/sub-millimetre colour-colour plots reveals that the
sample is not well fit by single modified-blackbody models that assume
a single dust-emissivity index (β). Instead, our new 850µm
data suggest either that a large fraction of our objects require
β<1.5, or that a model allowing for an excess of sub-mm emission
(e.g. a broken dust emissivity law, or a very cold dust
component~<10K) is required. We provide relations to convert FIR
colours to dust temperature and β for JINGLE-like galaxies. For
JINGLE the FIR colours correlate more strongly with star-formation
rate surface-density rather than the stellar surface-density,
suggesting heating of dust is greater due to younger rather than older
stellar-populations, consistent with the low proportion of early-type
galaxies in the sample.
Description:
The sources in the JINGLE survey are selected based on detections from
the H-ATLAS survey (Eales et al. 2010PASP..122..499E 2010PASP..122..499E) which observed
∼600deg2 with Herschel (Pilbratt et al. 2010A&A...518L...1P 2010A&A...518L...1P).
H-ATLAS observed in parallel mode using PACS at 100 and 160µm, and
SPIRE at 250, 350, and 500µm simultaneously. As JCMT is in the
Northern hemisphere, JINGLE selected objects in the equatorial GAMA
fields (161deg2) and the North Galactic Pole (NGP) field
(180.1deg2). For our photometry we use the PACS maps provided in
H-ATLAS DR1 (GAMA fields, Valiante et al. 2016MNRAS.462.3146V 2016MNRAS.462.3146V, Cat.
J/MNRAS/462/3146) and DR2 (NGP; Smith et al. 2017ApJS..233...26S 2017ApJS..233...26S). For
SPIRE we use the same timelines used to generate the maps in the DR1
and DR2 releases, except we apply the relative gain corrections and
calibration corrections to optimize the maps for extended sources.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
jingle.dat 436 193 JINGLE sample catalog
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See also:
J/MNRAS/481/3497 : JINGLE, Survey overview and first results (Saintonge+, 2018)
Byte-by-byte Description of file: jingle.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- ID [0/192] JINGLE Catalogue ID
5- 23 A19 --- Name SDSS name (JHHMMSS.ss+DDMMSS.s)
25 I1 --- Flagph [0-2] Photometry Flag (1)
27- 35 F9.4 --- SNRW3.4 WISE 3.4um Peak Signal-To-Noise Ratio
37- 44 F8.4 mJy FW3.4 ? WISE 3.4um Flux Density
46- 52 F7.5 mJy e_FW3.4 Error on FW3.4
54- 60 F7.5 --- ACFW3.4 ? WISE 3.4um Aperture Correction Factor
62- 70 F9.4 --- SNRW4.6 WISE 4.6um Peak Signal-To-Noise Ratio
72- 79 F8.4 mJy FW4.6 ? WISE 4.6um Flux Density
81- 87 F7.5 mJy e_FW4.6 Error on FW4.6
89- 95 F7.5 --- ACFW4.6 ? WISE 4.6um Aperture Correction Factor
97-105 F9.4 --- SNRW12 WISE 12um Peak Signal-To-Noise Ratio
107-114 F8.4 mJy FW12 ? WISE 12um Flux Density
116-122 F7.5 mJy e_FW12 Error on FW12
124-130 F7.5 --- ACFW12 ? WISE 12um Aperture Correction Factor
132-140 F9.4 --- SNRW22 WISE 22um Peak Signal-To-Noise Ratio
142-150 F9.4 mJy FW22 ? WISE 22um Flux Density
152-158 F7.5 mJy e_FW22 Error on FW22
160-166 F7.5 --- ACFW22 ? WISE 22um Aperture Correction Factor
168-174 F7.4 --- SNRP100 ? PACS 100um Peak Signal-To-Noise Ratio
176-185 F10.4 mJy FP100 ? PACS 100um Flux Density
187-195 F9.5 mJy e_FP100 ? Error on FP100
197-203 F7.5 --- ACFP100 ? PACS 100um Aperture Correction Factor
205-212 F8.4 --- SNRP160 ? PACS 160um Peak Signal-To-Noise Ratio
214-223 F10.4 mJy FP160 ? PACS 160um Flux Density
225-233 F9.5 mJy e_FP160 ? Error on FP160
235-241 F7.5 --- ACFP160 ? PACS 160um Aperture Correction Factor
243 I1 --- metS250 [0/1] SPIRE 250um Extraction Method (2)
245-252 F8.4 --- SNRS250 SPIRE 250um Peak Signal-To-Noise Ratio
254-262 F9.4 mJy FS250 ? SPIRE 250um Flux Density
264-272 F9.5 mJy e_FS250 Error on FS250
274-280 F7.5 --- ACF250 ? SPIRE 250um Aperture Correction Factor
282 I1 --- metS350 [0/1] SPIRE 250um Extraction Method (2)
284-290 F7.4 --- SNRS350 SPIRE 350um Peak Signal-To-Noise Ratio
292-300 F9.4 mJy FS350 ? SPIRE 350um Flux Density
302-309 F8.5 mJy e_FS350 Error on FS350
311-317 F7.5 --- ACF350 ? SPIRE 350um Aperture Correction Factor
319 I1 --- metS500 [0/1] SPIRE 500um Extraction Method (2)
321-327 F7.4 --- SNRS500 SPIRE 500um Peak Signal-To-Noise Ratio
329-336 F8.4 mJy FS500 ? SPIRE 500um Flux Density
338-345 F8.5 mJy e_FS500 Error on FS500
347-353 F7.5 --- ACF500 ? SPIRE 500um Aperture Correction Factor
355 I1 --- metS850 SCUBA2 850um Extraction Method (2)
357-363 F7.4 --- SNRS850 SCUBA2 850um Peak Signal-To-Noise Ratio
365-369 F5.2 mJy FSCO32 SCUBA2 850um Predicted CO(3-2) Flux Density
Contamination
371-378 F8.4 mJy FS850 ? SCUBA2 850um Flux Density (CO(3-2)
Corrected)
380-387 F8.5 mJy e_FS850 Error on FS850
389-397 F9.5 --- ACFS850 ? SCUBA2 850um Aperture Correction Factor
399-405 F7.5 --- FCFS850 ? SCUBA2 850um Filter Correction Factor
407-413 F7.4 arcsec a250 ? Aperture Major Radius at 250um (3)
415-421 F7.4 arcsec b250 ? Aperture Minor Radius at 250um (3)
423-436 F14.10 deg AperPA ? Aperture Position Angle
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Note (1): Flag as follows:
1 = Upper Limit
2 = Overlapping Sources
Note (2): Extraction method as follows:
0 = Apertures
1 = Point Source Fitting
Note (3): In bands other than the SPIRE 250um, we use a matched aperture to the
250um band, except we correct for the difference in beam size by
modifying the size of the semimajor and semiminor axis. This is
achieved by taking the 250um aperture size and subtracting in
quadrature the 250um FWHM/2 and adding the current band's FWHM/2.
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History:
From electronic version of the journal
References:
Saintonge et al., Paper I 2018MNRAS.481.3497S 2018MNRAS.481.3497S, Cat. J/MNRAS/481/3497
(End) Ana Fiallos [CDS] 25-Oct-2022