The Great Observatories All-Sky LIRG Survey: Herschel Image Atlas and Aperture Photometry
Jason K. Chu, D. B. Sanders, K. L. Larson, J. M. Mazzarella, J. H. Howell, T. Díaz-Santos, K. C. Xu, R. Paladini, B. Schulz, D. Shupe, P. Appleton, L. Armus, N. Billot, B. H. P. Chan, A. S. Evans, D. Fadda, D. T. Frayer, S. Haan, C. M. Ishida, K. Iwasawa, D.-C. Kim, S. Lord, E. Murphy, A. Petric, G. C. Privon, J. A. Surace, E. Treister
TThe Great Observatories All-Sky LIRG Survey:
Herschel
Image Atlas andAperture Photometry Jason K. Chu , D. B. Sanders , K. L. Larson , , J. M. Mazzarella , J. H. Howell , T.D´ıaz-Santos , , K. C. Xu , R. Paladini , B. Schulz , D. Shupe , P. Appleton , L. Armus , N.Billot , B. H. P. Chan , A. S. Evans , , D. Fadda , D. T. Frayer , S. Haan , C. M. Ishida , K.Iwasawa , D.-C. Kim , S. Lord , E. Murphy , A. Petric , G. C. Privon , J. A. Surace , E.Treister ABSTRACT
Far-infrared (FIR) images and photometry are presented for 201 Luminous and Ultraluminous In-frared Galaxies [LIRGs: log ( L IR /L (cid:12) ) = 11 . − . , ULIRGs: log ( L IR /L (cid:12) ) = 12 . − . ], inthe Great Observatories All-Sky LIRG Survey (GOALS) based on observations with the Herschel SpaceObservatory
Photodetector Array Camera and Spectrometer (PACS) and the Spectral and PhotometricImaging Receiver (SPIRE) instruments. The image atlas displays each GOALS target in the three PACSbands (70, 100, and 160 µ m) and the three SPIRE bands (250, 350, and 500 µ m), optimized to revealstructures at both high and low surface brightness levels, with images scaled to simplify comparison ofstructures in the same physical areas of ∼ × kpc . Flux densities of companion galaxies in merg-ing systems are provided where possible, depending on their angular separation and the spatial resolutionin each passband, along with integrated system fluxes (sum of components). This dataset constitutes theimaging and photometric component of the GOALS Herschel
OT1 observing program, and is comple-mentary to atlases presented for the
Hubble Space Telescope (Evans et al . Spitzer SpaceTelescope (Mazzarella et al . Chandra X-ray Observatory (Iwasawa et al . Subject headings: atlases — galaxies: active — galaxies: interactions — galaxies: starburst — galaxies: structure —infrared: galaxies Institute for Astronomy, University of Hawaii, 2680 Wood-lawn Drive, Honolulu, HI 96822; [email protected],[email protected] Infrared Processing & Analysis Center, MS 100-22, CaliforniaInstitute of Technology, Pasadena, CA 91125; bchan, jhhowell, klar-son, lee, [email protected], [email protected] Nucleo de Astronom´ıa de la Facultad de Ingenier´ıa, Universi-dad Diego Portales, Av. Ejercito Libertador 441, Santiago, Chile;[email protected] NASA Herschel Science Center, MS 100-22, California Insti-tute of Technology, Pasadena, CA 91125; apple, bschulz, cxu, pala-dini, [email protected] Observatoire de l’Universit´e de Gen´eve, 51 chemin des Mail-lettes, 1290 Versoix, Switzerland; [email protected] Department of Astronomy, University of Virginia, Char-lottesville, VA 22904-4325; [email protected] National Radio Astronomy Observatory, 520 EdgemontRoad, Charlottesville, VA 22903-2475; dfrayer, dkim, [email protected], [email protected] Department of Physics and Astronomy, University of Hawaii atHilo, Hilo, HI, 96720; [email protected] ICREA and Institut del Ci`encies del Cosmos (ICC), Universi-
1. Introduction
The Great Observatories All-Sky LIRG Survey(GOALS, Armus et al. 2009), combines both imag-ing and spectroscopic data for the complete sam-ple of 201 Luminous Infrared Galaxies (LIRGs: tat de Barcelona (IEEC-UB), Mart´ı i Franqu`es 1, 08028 Barcelona,Spain; [email protected] SETI Institute; [email protected] Canada France Hawaii Telescope Corp., Conc´epcion, Chile;[email protected] Instituto de Astrof´ısica, Facultad de F´ısica, Pontificia Univer-sidad Cat´olica de Chile, Casilla 306, Santiago 22, Chile; gprivon,[email protected] Spitzer Science Center, MS 314-6, California Institute of Tech-nology, Pasadena, CA 91125; [email protected] Based on
Herschel Space Observatory observations.
Herschel is an ESA space observatory with science instruments provided byEuropean-led Principal Investigator consortia and with importantparticipation from NASA. a r X i v : . [ a s t r o - ph . GA ] F e b og ( L IR /L (cid:12) ) > . ) selected from the IRAS Re-vised Bright Galaxy Sample (RBGS, Sanders et al.2003). The full RBGS contains 629 objects, represent-ing a complete sample of extragalactic sources withIRAS 60 µ m flux density, S > . Jy, coveringthe entire sky above a Galactic latitude of | b | > ◦ .The median redshift of objects in the GOALS sam-ple is (cid:104) z (cid:105) = 0 . , with a maximum redshift of z max = 0 . . As the nearest and brightest 60 µ m extragalactic objects, they represent a sample thatis the most amenable for study at all wavelengths.The primary objective of the GOALS multi-wavelengthsurvey is to fully characterize the diversity of proper-ties observed in a large, statistically significant sampleof the nearest LIRGs. This allows us to probe the fullrange of phenomena such as normal star formation,starbursts, and active galactic nuclei (AGN) that powerthe observed far-infrared emission, as well as to bet-ter characterize the range of galaxy types (i. e. normaldisks, major and minor interactions/mergers, etc.) thatare associated with the LIRG phase. A secondary ob-jective is to provide a data set that is ideally suited forcomparison with LIRGs observed at high redshifts.GOALS currently includes imaging and spec-troscopy from the Spitzer , Hubble , GALEX , Chandra , XMM-Newton , and now
Herschel space-borne obser-vatories, along with complementary ground-based ob-servations from ALMA, Keck, and other telescopes.The GOALS project is described in more detail athttp://goals.ipac.caltech.edu/.Due to limitations in angular resolution, wavelengthcoverage, and sensitivity of pre-
Herschel ( IRAS , ISO , Spitzer , AKARI ) far-infrared (FIR) data, the spatial dis-tribution of FIR emission within the GOALS sources,and the total amount of gas and dust in these sys-tems, are poorly determined. The
Herschel data willallow us for the first time to directly probe the criticalFIR and submillimeter wavelength regime of these in-frared luminous systems, enabling us to accurately de-termine the bolometric luminosities, infrared surfacebrightnesses, star formation rates, and dust masses andtemperatures on spatial scales of 2 – 5 kpc within theGOALS sample.This paper presents imaging and photometry for all201 LIRGs and LIRG systems in the IRAS RBGS thatwere observed during our GOALS
Herschel
OT1 pro-gram. A more complete description of the GOALSsample is given in §
2. The data acquisition is describedin § §
4. The image atlas is presented in §
5, and photomet- ric measurements are given in §
6. Section 7 containsa discussion of basic results, including comparisonswith prior measurements, and a summary is given in §
8. A reference cosmology of Ω Λ = 0 . , Ω m = 0 . and H = 70 km sec. − Mpc − is adopted, howeverwe also take into account local non-cosmological ef-fects by using the three-attractor model of Mould et al.(2000).
2. The GOALS Sample
The IRAS RBGS contains a total of 179 LIRGs(log ( L IR /L (cid:12) ) = 11 . − . ), and 22 ultra-luminousinfrared galaxies (ULIRGs: log ( L IR /L (cid:12) ) ≥ . );these 201 objects comprise the GOALS sample (Ar-mus et al. 2009), a statistically complete flux-limitedsample of infrared-luminous galaxies in the local uni-verse. In addition to the Herschel observations re-ported here, the GOALS objects have been the subjectof an intense multi-wavelength observing campaign,including VLA 20 cm (Condon et al. 1990, 1996), mil-limeter wave spectral line observations of CO(1 → µ m and 850 µ m (Dunne et al. 2000), near-infrared images from 2MASS (Skrutskie et al. 2006),optical and K -band imaging (Ishida 2004), as well asspace-based imaging from the Spitzer Space Telescope (IRAC and MIPS, Mazzarella et al . Hubble Space Telescope (ACS, Evans et al . GALEX (NUV and FUV, Howell et al. 2010),and the
Chandra X-ray Observatory (ACIS, Iwasawaet al. 2011, 2017 in prep). Extensive spectroscopy dataalso exist on the GOALS sample, such as in the op-tical (Kim et al. 1995) and with
Spitzer
IRS in themid-infrared (Stierwalt et al. 2013).
Herschel
PACSspectroscopy was obtained in Cycles 1 and 2 target-ing the [C II ] 157.7 µ m, [O I ] 63.2 µ m, and [O III ]88 µ m emission lines and the OH 79 µ m absorptionfeature for the entire sample, as well as the [N II ] 122 µ m line in 122 GOALS galaxies (D´ıaz-Santos et al.2013, 2014, 2017 in prep). In addition, Herschel
SPIRE FTS spectroscopy were obtained to probe theCO spectral line energy distribution from J = 4 → up to J = 13 → for 93 of the GOALS objects(Lu et al. 2014, 2015, 2017, submitted), as well as the[N II ] 205 µ m emission line for 122 objects Zhao et al.(2013, 2016).Out of the original list of 203 GOALS systems,two were omitted from our Herschel sample, makingfor a final tally of 201 objects. IRAS F13097–1531 2NGC 5010) was part of the original RBGS sample ofSanders et al. (2003), however due to a revision in theredshift of the object it was much closer than thought.This caused the resulting far-IR luminosity to drop sig-nificantly below the LIRG threshold of L (cid:12) . Theother object we excluded from our sample is IRAS05223+1908, which we believe is a young stellar ob-ject (YSO), due to the fact that its spectral energy dis-tribution (SED) peaks in the submillimeter part of thespectrum.Table 1 presents the basic GOALS information.Column 1 is the index number of galaxies in theGOALS sample, and correspond to the same galaxiesin Tables 2, 3, and 4. Column 2 is the IRAS name ofthe galaxy, ordered by ascending RA. Galaxies withthe “F” prefix originate from the IRAS
Faint SourceCatalog, and galaxies with no “F” prefix are from thePoint Source Catalog. Column 3 is a list of commonoptical counterpart names. Columns 4 and 5 are the
Spitzer µ m centers of the system in J2000 from Maz-zarella et al . (2017). For galaxy systems with two ormore components, the coordinate is taken to be thegeometric midpoint between the component galaxies.Column 6 gives the angular diameter distance to thegalaxy in Mpc, from Mazzarella et al . (2017). Col-umn 7 is the map size used in the atlas, denoting thephysical length of a side in each atlas image in kpc.Column 8 is the systemic heliocentric redshift of thegalaxy system, and Column 9 is the measured helio-centric radial velocity in km sec − , that corresponds tothe redshift. Both of these columns take into accountcosmological as well as non-cosmological effects (seeMould et al. 2000). Finally Column 10 is the indica-tive 8–1000 µ minfrared luminosity in log ( L IR /L (cid:12) ) of the entire system from Armus et al. (2009). Simi-lar to Columns 8 and 9, the L IR values in Table 1 takeinto account the effect of the local attractors to D A ,than one would normally obtain from pure cosmologi-cal effect. 3 ABLE ASIC
GOALS D
ATA D A Map Size Redshift Velocity L IR — — — HH : MM : SS DD : MM : SS
Mpc kpc — km s − log (cid:16) LL (cid:12) (cid:17) (1) (2) (3) (4) (5) (6) (7) (8) (9) (10)1 F00073+2538 NGC 23
00 : 09 : 53 .
36 +25 : 55 : 27 . . . .
00 : 11 : 06 . −
12 : 06 : 28 . . . .
00 : 18 : 50 . −
10 : 22 : 05 . . . .
00 : 36 : 52 . −
33 : 33 : 17 . . . .
00 : 42 : 49 . −
23 : 33 : 04 . . . .
00 : 54 : 03 .
88 +73 : 05 : 05 . . . .
00 : 57 : 39 .
72 +43 : 47 : 47 . . . .
01 : 07 : 47 . −
17 : 30 : 25 . . . .
01 : 10 : 08 . −
16 : 51 : 09 . . . .
10 F01159-4443 ESO 244-G012
01 : 18 : 08 . −
44 : 27 : 51 . . . .
11 F01173+1405 CGCG 436-030
01 : 20 : 02 .
63 +14 : 21 : 42 . . . .
12 F01325-3623 ESO 353-G020
01 : 34 : 51 . −
36 : 08 : 14 . . .
016 4797 11 .
13 F01341-3735 RR 032, ESO 297-G011/012
01 : 36 : 23 . −
37 : 19 : 51 . . .
14 F01364-1042
01 : 38 : 52 . −
10 : 27 : 12 . . . .
15 F01417+1651 III Zw 035
01 : 44 : 30 .
56 +17 : 06 : 09 . . . .
16 F01484+2220 NGC 695
01 : 51 : 14 .
34 +22 : 34 : 56 . . . .
17 F01519+3640 UGC 01385
01 : 54 : 57 .
78 +36 : 55 : 07 . . . .
18 F02071-1023 NGC 838
02 : 09 : 31 . −
10 : 09 : 30 . . . .
19 F02070+3857 NGC 828
02 : 10 : 09 .
53 +39 : 11 : 24 . . . .
20 F02114+0456 IC 214
02 : 14 : 00 .
77 +05 : 10 : 13 . . . .
21 F02152+1418 NGC 877
02 : 17 : 56 .
46 +14 : 31 : 58 . . . .
22 F02203+3158 MCG+05-06-036
02 : 23 : 20 .
47 +32 : 11 : 33 . . . .
23 F02208+4744 UGC 01845
02 : 24 : 07 .
97 +47 : 58 : 11 . . .
24 F02281-0309 NGC 958
02 : 30 : 42 . −
02 : 56 : 20 . . . .
25 F02345+2053 NGC 992
02 : 37 : 25 .
46 +21 : 06 : 02 . . . .
26 F02401-0013 NGC 1068
02 : 42 : 40 . −
00 : 00 : 47 . . . .
27 F02435+1253 UGC 02238
02 : 46 : 17 .
46 +13 : 05 : 44 . . . .
28 F02437+2122
02 : 46 : 39 .
13 +21 : 35 : 10 . . . .
28 F02437+2123 a
02 : 46 : 45 .
05 +21 : 33 : 23 . . . .
29 F02512+1446 UGC 02369
02 : 54 : 01 .
79 +14 : 58 : 26 . . . .
30 F03117+4151 UGC 02608
03 : 15 : 01 .
47 +42 : 02 : 08 . . . .
30 F03117+4151 a UGC 02612
03 : 15 : 14 .
58 +41 : 58 : 50 . . . .
31 F03164+4119 NGC 1275
03 : 19 : 48 .
18 +41 : 30 : 42 . . . .
32 F03217+4022
03 : 25 : 05 .
37 +40 : 33 : 32 . . . .
33 F03316-3618 NGC 1365
03 : 33 : 36 . −
36 : 08 : 25 . . . .
34 F03359+1523
03 : 38 : 47 .
07 +15 : 32 : 54 . . . .
35 F03514+1546 CGCG 465-012
03 : 54 : 15 .
95 +15 : 55 : 43 . . . .
35 F03514+1546 a CGCG 465-011
03 : 54 : 07 .
67 +15 : 59 : 24 . . . .
36 03582+6012
04 : 02 : 32 .
47 +60 : 20 : 40 . . . .
37 F04097+0525 UGC 02982
04 : 12 : 22 .
68 +05 : 32 : 49 . . . .
38 F04118-3207 ESO 420-G013
04 : 13 : 49 . −
32 : 00 : 25 . . . .
39 F04191-1855 ESO 550-IG 025
04 : 21 : 20 . −
18 : 48 : 48 . . .
40 F04210-4042 NGC 1572
04 : 22 : 42 . −
40 : 36 : 03 . . . .
41 04271+3849
04 : 30 : 33 .
09 +38 : 55 : 47 . . . .
42 F04315-0840 NGC 1614
04 : 33 : 59 . −
08 : 34 : 46 . . . .
43 F04326+1904 UGC 03094
04 : 35 : 33 .
81 +19 : 10 : 18 . . . .
44 F04454-4838 ESO 203-IG001
04 : 46 : 49 . −
48 : 33 : 30 . . .
45 F04502-3304 MCG-05-12-006
04 : 52 : 04 . −
32 : 59 : 26 . . . .
46 F05053-0805 NGC 1797
05 : 07 : 44 . −
08 : 01 : 08 . . . . ABLE Continued D A Map Size Redshift Velocity L IR — — — HH : MM : SS DD : MM : SS
Mpc kpc — km s − log (cid:16) LL (cid:12) (cid:17) (1) (2) (3) (4) (5) (6) (7) (8) (9) (10)46 F05053-0805 a NGC 1799
05 : 07 : 44 . −
07 : 58 : 09 . . . .
47 F05054+1718 CGCG 468-002
05 : 08 : 20 .
46 +17 : 21 : 57 . . . .
48 05083+2441
05 : 11 : 27 .
46 +24 : 45 : 41 . . . .
49 F05081+7936 VII Zw 031
05 : 16 : 46 .
39 +79 : 40 : 12 . . . .
50 05129+5128
05 : 16 : 55 .
96 +51 : 31 : 56 . . . .
51 F05189-2524
05 : 21 : 01 . −
25 : 21 : 46 . . .
52 F05187-1017
05 : 21 : 06 . −
10 : 14 : 46 . . . .
53 05368+4940 MCG+08-11-002
05 : 40 : 43 .
70 +49 : 41 : 41 . . . .
54 F05365+6921 NGC 1961
05 : 42 : 04 .
55 +69 : 22 : 42 . . . .
55 F05414+5840 UGC 03351
05 : 45 : 48 .
03 +58 : 42 : 03 . . . .
56 05442+1732
05 : 47 : 08 .
49 +17 : 33 : 29 . . . .
57 F06076-2139
06 : 09 : 45 . −
21 : 40 : 28 . . . .
58 F06052+8027 UGC 03410
06 : 14 : 13 .
75 +80 : 27 : 47 . . . .
59 F06107+7822 NGC 2146
06 : 18 : 37 .
82 +78 : 21 : 24 . . . .
60 F06259-4708 ESO 255-IG007
06 : 27 : 22 . −
47 : 10 : 49 . . . .
61 F06295-1735 ESO 557-G002
06 : 31 : 46 . −
17 : 38 : 00 . . . .
62 F06538+4628 UGC 03608
06 : 57 : 34 .
41 +46 : 24 : 10 . . . .
63 F06592-6313
06 : 59 : 40 . −
63 : 17 : 52 . . . .
64 F07027-6011 AM 0702-601
07 : 03 : 26 . −
60 : 16 : 02 . . . .
65 07063+2043 NGC 2342
07 : 09 : 15 .
04 +20 : 37 : 10 . . .
66 F07160-6215 NGC 2369
07 : 16 : 37 . −
62 : 20 : 36 . . . .
67 07251-0248
07 : 27 : 37 . −
02 : 54 : 54 . . . .
68 F07256+3355 NGC 2388
07 : 28 : 46 .
38 +33 : 50 : 22 . . . .
69 F07329+1149 MCG+02-20-003
07 : 35 : 43 .
44 +11 : 42 : 34 . . .
69 F07329+1149 a NGC 2416
07 : 35 : 41 .
53 +11 : 36 : 42 . . .
70 08355-4944
08 : 37 : 01 . −
49 : 54 : 30 . . . .
71 F08339+6517
08 : 38 : 23 .
18 +65 : 07 : 15 . . . .
72 F08354+2555 NGC 2623
08 : 38 : 24 .
11 +25 : 45 : 16 . . . .
73 08424-3130 ESO 432-IG006
08 : 44 : 28 . −
31 : 41 : 40 . . . .
74 F08520-6850 ESO 060-IG016
08 : 52 : 31 . −
69 : 01 : 57 . . . .
75 F08572+3915
09 : 00 : 25 .
35 +39 : 03 : 54 . . . .
76 09022-3615
09 : 04 : 12 . −
36 : 27 : 01 . . . .
77 F09111-1007
09 : 13 : 37 . −
10 : 19 : 24 . . . .
78 F09126+4432 UGC 04881
09 : 15 : 55 .
10 +44 : 19 : 54 . . . .
79 F09320+6134 UGC 05101
09 : 35 : 51 .
59 +61 : 21 : 11 . . . .
80 F09333+4841 MCG+08-18-013
09 : 36 : 34 .
02 +48 : 28 : 18 . . . .
81 F09437+0317 Arp 303, IC 0563/4
09 : 46 : 20 .
70 +03 : 03 : 30 . . .
02 5996 11 .
82 F10015-0614 NGC 3110
10 : 03 : 59 . −
06 : 29 : 08 . . . .
83 F10038-3338 ESO 374-IG 032
10 : 06 : 04 . −
33 : 53 : 06 . . . .
84 F10173+0828
10 : 20 : 00 .
24 +08 : 13 : 32 . . . .
85 F10196+2149 NGC 3221
10 : 22 : 19 .
98 +21 : 34 : 10 . . . .
86 F10257-4339 NGC 3256
10 : 27 : 51 . −
43 : 54 : 14 . . . .
87 F10409-4556 ESO 264-G036
10 : 43 : 07 . −
46 : 12 : 44 . . . .
88 F10567-4310 ESO 264-G057
10 : 59 : 01 . −
43 : 26 : 25 . . . .
89 F10565+2448
10 : 59 : 18 .
15 +24 : 32 : 34 . . . .
90 F11011+4107 MCG+07-23-019
11 : 03 : 53 .
98 +40 : 51 : 00 . . . .
91 F11186-0242 CGCG 011-076
11 : 21 : 10 . −
02 : 59 : 20 . . . .
92 F11231+1456 IC 2810
11 : 25 : 47 .
31 +14 : 40 : 21 . .
034 10192 11 .
93 F11255-4120 ESO 319-G022
11 : 27 : 54 . −
41 : 36 : 51 . . . . ABLE Continued D A Map Size Redshift Velocity L IR — — — HH : MM : SS DD : MM : SS
Mpc kpc — km s − log (cid:16) LL (cid:12) (cid:17) (1) (2) (3) (4) (5) (6) (7) (8) (9) (10)94 F11257+5850 NGC 3690, Arp 299
11 : 28 : 32 .
35 +58 : 33 : 43 . . . .
95 F11506-3851 ESO 320-G030
11 : 53 : 11 . −
39 : 07 : 49 . . . .
96 F12043-3140 ESO 440-IG058
12 : 06 : 51 . −
31 : 56 : 52 . . .
97 F12112+0305
12 : 13 : 46 .
02 +02 : 48 : 42 . . . .
98 F12116+5448 NGC 4194
12 : 14 : 09 .
71 +54 : 31 : 35 . . . .
99 F12115-4656 ESO 267-G030
12 : 14 : 12 . −
47 : 13 : 42 . . .
99 F12115-4656 a ESO 267-G029
12 : 13 : 52 . −
47 : 16 : 25 . . .
100 12116-5615
12 : 14 : 22 . −
56 : 32 : 32 . . . .
101 F12224-0624
12 : 25 : 03 . −
06 : 40 : 52 . . . .
102 F12243-0036 NGC 4418
12 : 26 : 59 . −
00 : 53 : 32 . . . .
103 F12540+5708 UGC 08058, Mrk 231
12 : 56 : 14 .
25 +56 : 52 : 24 . . . .
104 F12590+2934 NGC 4922
13 : 01 : 24 .
89 +29 : 18 : 39 . . . .
105 F12592+0436 CGCG 043-099
13 : 01 : 50 .
28 +04 : 20 : 00 . . . .
106 F12596-1529 MCG-02-33-098
13 : 02 : 20 . −
15 : 46 : 01 . . . .
107 F13001-2339 ESO 507-G070
13 : 02 : 52 . −
23 : 55 : 17 . . . .
108 13052-5711
13 : 08 : 18 . −
57 : 27 : 30 . . . .
109 F13126+2453 IC 0860
13 : 15 : 03 .
49 +24 : 37 : 07 . . . .
110 13120-5453
13 : 15 : 06 . −
55 : 09 : 22 . . . .
111 F13136+6223 VV 250a
13 : 15 : 32 .
82 +62 : 07 : 37 . . . .
112 F13182+3424 UGC 08387
13 : 20 : 35 .
37 +34 : 08 : 22 . . .
113 F13188+0036 NGC 5104
13 : 21 : 23 .
09 +00 : 20 : 33 . . . .
114 F13197-1627 MCG-03-34-064
13 : 22 : 21 . −
16 : 43 : 06 . . . .
115 F13229-2934 NGC 5135
13 : 25 : 44 . −
29 : 50 : 00 . . . .
116 13242-5713 ESO 173-G015
13 : 27 : 23 . −
57 : 29 : 21 . . . .
117 F13301-2356 IC 4280
13 : 32 : 53 . −
24 : 12 : 25 . . . .
118 F13362+4831 NGC 5256
13 : 38 : 17 .
52 +48 : 16 : 37 . . . .
119 F13373+0105 Arp 240, NGC 5257/8
13 : 39 : 55 .
34 +00 : 50 : 09 . . . .
120 F13428+5608 UGC 08696, Mrk 273
13 : 44 : 42 .
12 +55 : 53 : 13 . . . .
121 F13470+3530 UGC 08739
13 : 49 : 13 .
94 +35 : 15 : 26 . . . .
122 F13478-4848 ESO 221-IG010
13 : 50 : 56 . −
49 : 03 : 18 . . . .
123 F13497+0220 NGC 5331
13 : 52 : 16 .
32 +02 : 06 : 18 . . . .
124 F13564+3741 Arp 84, NGC 5394/5
13 : 58 : 35 .
80 +37 : 26 : 20 . . . .
125 F14179+4927 CGCG 247-020
14 : 19 : 43 .
27 +49 : 14 : 11 . . . .
126 F14280+3126 NGC 5653
14 : 30 : 10 .
44 +31 : 12 : 55 . . . .
127 F14348-1447
14 : 37 : 38 . −
15 : 00 : 24 . . . .
128 F14378-3651
14 : 40 : 59 . −
37 : 04 : 32 . . . .
129 F14423-2039 NGC 5734
14 : 45 : 10 . −
20 : 53 : 30 . . . .
130 F14547+2449 VV 340a, Arp 302
14 : 57 : 00 .
51 +24 : 36 : 45 . . . .
131 F14544-4255 IC 4518A/B
14 : 57 : 43 . −
43 : 07 : 56 . . . .
132 F15107+0724 CGCG 049-057
15 : 13 : 13 .
07 +07 : 13 : 32 . . .
013 3897 11 .
133 F15163+4255 VV 705
15 : 18 : 06 .
24 +42 : 44 : 41 . . . .
134 15206-6256 ESO 099-G004
15 : 24 : 57 . −
63 : 07 : 29 . . . .
135 F15250+3608
15 : 26 : 59 .
42 +35 : 58 : 37 . . . .
136 F15276+1309 NGC 5936
15 : 30 : 00 .
85 +12 : 59 : 22 . . . .
137 F15327+2340 Arp 220, UGC 09913
15 : 34 : 57 .
23 +23 : 30 : 11 . . . .
138 F15437+0234 NGC 5990
15 : 46 : 16 .
41 +02 : 24 : 55 . . . .
139 F16030+2040 NGC 6052
16 : 05 : 12 .
87 +20 : 32 : 33 . . . .
140 F16104+5235 NGC 6090
16 : 11 : 40 .
84 +52 : 27 : 27 . . . .
141 F16164-0746
16 : 19 : 11 . −
07 : 54 : 03 . . . . ABLE Continued D A Map Size Redshift Velocity L IR — — — HH : MM : SS DD : MM : SS
Mpc kpc — km s − log (cid:16) LL (cid:12) (cid:17) (1) (2) (3) (4) (5) (6) (7) (8) (9) (10)142 F16284+0411 CGCG 052-037
16 : 30 : 54 .
89 +04 : 04 : 41 . . . .
143 16304-6030 NGC 6156
16 : 34 : 52 . −
60 : 37 : 08 . . .
144 F16330-6820 ESO 069-IG006
16 : 38 : 12 . −
68 : 26 : 42 . . . .
145 F16399-0937
16 : 42 : 40 . −
09 : 43 : 13 . . . .
146 F16443-2915 ESO 453-G005
16 : 47 : 30 . −
29 : 20 : 14 . . . .
147 F16504+0228 NGC 6240
16 : 52 : 58 .
90 +02 : 24 : 03 . . . .
148 F16516-0948
16 : 54 : 23 . −
09 : 53 : 20 . . . .
149 F16577+5900 NGC 6286, Arp 293
16 : 58 : 27 .
81 +58 : 56 : 47 . . . .
150 F17132+5313
17 : 14 : 20 .
45 +53 : 10 : 31 . . . .
151 F17138-1017
17 : 16 : 35 . −
10 : 20 : 40 . . . .
152 F17207-0014
17 : 23 : 21 . −
00 : 17 : 00 . . . .
153 F17222-5953 ESO 138-G027
17 : 26 : 43 . −
59 : 55 : 55 . . . .
154 F17530+3447 UGC 11041
17 : 54 : 51 .
82 +34 : 46 : 34 . . .
155 F17548+2401 CGCG 141-034
17 : 56 : 56 .
65 +24 : 01 : 02 . . . .
156 17578-0400
18 : 00 : 28 . −
04 : 01 : 16 . . .
157 18090+0130
18 : 11 : 35 .
91 +01 : 31 : 41 . . . .
158 F18131+6820 NGC 6621, Arp 81
18 : 12 : 57 .
46 +68 : 21 : 38 . . . .
159 F18093-5744 IC 4687
18 : 13 : 39 . −
57 : 44 : 00 . . . .
160 F18145+2205 CGCG 142-034
18 : 16 : 37 .
26 +22 : 06 : 42 . . . .
161 F18293-3413
18 : 32 : 41 . −
34 : 11 : 27 . . .
162 F18329+5950 NGC 6670A/B
18 : 33 : 36 .
00 +59 : 53 : 20 . . . .
163 F18341-5732 IC 4734
18 : 38 : 25 . −
57 : 29 : 25 . . . .
164 F18425+6036 NGC 6701
18 : 43 : 12 .
52 +60 : 39 : 11 . . . .
165 F19120+7320 VV 414, NGC 6786, UGC 11415
19 : 10 : 59 .
19 +73 : 25 : 04 . . . .
166 F19115-2124 ESO 593-IG008
19 : 14 : 31 . −
21 : 19 : 06 . . . .
167 F19297-0406
19 : 32 : 22 . −
04 : 00 : 01 . . . .
168 19542+1110
19 : 56 : 35 .
78 +11 : 19 : 04 . . . .
169 F19542-3804 ESO 339-G011
19 : 57 : 37 . −
37 : 56 : 08 . . . .
170 F20221-2458 NGC 6907
20 : 25 : 06 . −
24 : 48 : 32 . . . .
171 20264+2533 MCG+04-48-002
20 : 28 : 31 .
98 +25 : 43 : 42 . . . .
172 F20304-0211 NGC 6926
20 : 33 : 06 . −
02 : 01 : 38 . . . .
173 20351+2521
20 : 37 : 17 .
73 +25 : 31 : 37 . . . .
174 F20550+1655 CGCG 448-020, II Zw 096
20 : 57 : 24 .
01 +17 : 07 : 41 . . .
175 F20551-4250 ESO 286-IG019
20 : 58 : 26 . −
42 : 39 : 00 . . .
043 12890 12 .
176 F21008-4347 ESO 286-G035
21 : 04 : 11 . −
43 : 35 : 36 . . . .
177 21101+5810
21 : 11 : 29 .
28 +58 : 23 : 07 . . . .
178 F21330-3846 ESO 343-IG013
21 : 36 : 10 . −
38 : 32 : 37 . . . .
179 F21453-3511 NGC 7130
21 : 48 : 19 . −
34 : 57 : 04 . . . .
180 F22118-2742 ESO 467-G027
22 : 14 : 39 . −
27 : 27 : 50 . . . .
181 F22132-3705 IC 5179
22 : 16 : 09 . −
36 : 50 : 37 . . . .
182 F22287-1917 ESO 602-G025
22 : 31 : 25 . −
19 : 02 : 04 . . . .
183 F22389+3359 UGC 12150
22 : 41 : 12 .
21 +34 : 14 : 56 . . . .
184 F22467-4906 ESO 239-IG002
22 : 49 : 39 . −
48 : 50 : 58 . . . .
185 F22491-1808
22 : 51 : 49 . −
17 : 52 : 24 . . . .
186 F23007+0836 NGC 7469, IC 5283, Arp 298
23 : 03 : 16 .
84 +08 : 53 : 00 . . .
187 F23024+1916 CGCG 453-062
23 : 04 : 56 .
55 +19 : 33 : 07 . . . .
188 F23128-5919 ESO 148-IG002
23 : 15 : 46 . −
59 : 03 : 15 . . . .
189 F23135+2517 IC 5298
23 : 16 : 00 .
67 +25 : 33 : 24 . . . .
190 F23133-4251 NGC 7552
23 : 16 : 10 . −
42 : 35 : 05 . . . . ABLE Continued D A Map Size Redshift Velocity L IR — — — HH : MM : SS DD : MM : SS
Mpc kpc — km s − log (cid:16) LL (cid:12) (cid:17) (1) (2) (3) (4) (5) (6) (7) (8) (9) (10)191 F23157+0618 NGC 7591
23 : 18 : 14 .
89 +06 : 34 : 17 . . . .
192 F23157-0441 NGC 7592
23 : 18 : 22 . −
04 : 24 : 57 . . .
193 F23180-6929 ESO 077-IG014
23 : 21 : 04 . −
69 : 12 : 54 . . . .
194 F23254+0830 NGC 7674, HCG 96
23 : 27 : 57 .
73 +08 : 46 : 51 . . . .
195 23262+0314 NGC 7679
23 : 28 : 46 .
62 +03 : 30 : 41 . . . .
195 23262+0314 a NGC 7682
23 : 29 : 03 .
91 +03 : 31 : 59 . . . .
196 F23365+3604
23 : 39 : 01 .
32 +36 : 21 : 08 . . . .
197 F23394-0353 MCG-01-60-022
23 : 42 : 00 . −
03 : 36 : 54 . . . .
197 F23394-0353 a MCG-01-60-021, Mrk 933
23 : 41 : 46 . −
03 : 39 : 42 . . . .
198 23436+5257
23 : 46 : 05 .
44 +53 : 14 : 01 . . . .
199 F23444+2911 Arp 86, NGC 7752/3
23 : 47 : 01 .
73 +29 : 28 : 16 . . . .
200 F23488+1949 NGC 7771
23 : 51 : 13 .
55 +20 : 07 : 41 . . . .
201 F23488+2018 Mrk 331
23 : 51 : 22 .
73 +20 : 34 : 55 . . . . N OTE .—The column descriptions are (1) The row reference number. (2) The IRAS name of the galaxy, ordered by ascending RA. Galaxies withthe “F” prefix originate from the
IRAS
Faint Source Catalog, and galaxies with no “F” prefix are from the Point Source Catalog. (3) Common opticalcounterpart names to the galaxy systems. (4) — (5) are the
Spitzer µ m centers of the system in J2000 (see Mazzarella et al . Herschel atlas images are centered on these coordinates. For widely separated systems, the coordinate is taken to be half way between the component galaxies.(6) The angular diameter distance to the galaxy in Mpc, from Mazzarella et al . (2017). (7) The map size used in the atlas, denoting the physical length ofa side in each atlas image, in kpc. (8) The non-relativistic redshifts as reported by NED, which also corresponds to the heliocentric velocity (Column 9),and includes both cosmological and non-cosmological effects. (9) The measured heliocentric radial velocity corresponding to the redshift in Column 8in km / sec from Armus et al. (2009), which includes both cosmological and non-cosmological effects. (10) The indicative infrared luminosity, measuredin log ( L/L (cid:12) ) of the entire system, from Armus et al. (2009). These values take into account the effect of the local attractor to the distances than onewould normally obtain from pure cosmological effects. a These are very widely separated galaxy pairs that required two
Herschel
PACS observations. . Herschel Space Observatory
Observations
The
Herschel Space Observatory (Pilbratt et al.2010) imaging observations of the GOALS sampletook place between the dates of March 2011 throughJune 2012, through our Cycle 1 open time observingprogram OT1 dsanders 1 (PI: D. Sanders, Program ID µ m, 100 µ m, and 160 µ m, and thethree SPIRE bands at 250 µ m, 350 µ m, and 500 µ m.The normalized filter transmission curves are shown inFigure 1. Each SPIRE band has two curves associatedwith the filter, corresponding to the point source re-sponsitivity (solid) and extended source responsitivity(dashed), which is important since some of the objectsin our sample are extended even at SPIRE wavelengths(i. e. the LIRG IRAS F03316–3618/NGC 1365).Within the GOALS sample there are eight systemsconsisting of widely separated pairs where two sep-arate PACS observations were needed, but only oneSPIRE observation was made since its field of viewwas larger. These galaxies are denoted in both Tables1 and 2, giving a total of
201 + 8 = 209 observa-tion datasets. We note for the galaxy system IRASF07256+3355 which has three components, only twoare visible in the PACS imagery, due to the smallerfield of view of PACS. The third component (NGC2385) is far to the west and still within SPIRE’s largerfield of view. Using the SPIRE fluxes as a roughproxy for infrared luminosity strength, NGC 2385 con-tributes very little to the overall infrared luminosity ofthe system. IRAS F23488+1949 also has a third com-ponent (NGC 7769) to the NNW in the SPIRE images,but is outside of the PACS scan area. However fromthe SPIRE fluxes NGC 7769 appears to have a moder-ate contribution to the system’s infrared luminosity. In sum we achieved a very high degree of coverage andcompleteness for each GOALS object with
Herschel . The Photoconductor Array Camera and Spectrom-eter (PACS, Poglitsch et al. 2010) is one of three farinfrared instruments onboard the
Herschel Space Ob-servatory and covers a wavelength range between 60– 210 µ m. In the photometer mode it can image twosimultaneous wavelength bands centered at 160 µ m,and at either 70 µ m or 100 µ m. These three broadbands are referred to as the blue channel (60 – 85 µ m),green channel (85 – 130 µ m) and red channel (130 –210 µ m). For any given observation, the blue cameraobserves at either 70 µ m or 100 µ m, while the red cam-era only observes at 160 µ m. A dichroic beam-splitterwith a designed transition wavelength of 130 µ m di-rects the incoming light into the blue and red cameras,and a filter in front of the blue camera selects either theblue or green band.The detectors for both the blue and red camerascomprise a filled bolometer array of square pixels thatinstantaneously samples the entire beam from the tele-scope’s optics. The layout of the blue camera’s focalplane consists of 4 × ×
16 pix-els in each subarray. Similarly the red camera consistsof 2 × ×
16 pixels each. On thesky each bolometer pixel subtends an angle of 3 . (cid:48)(cid:48) × . (cid:48)(cid:48) . (cid:48)(cid:48) × . (cid:48)(cid:48) . (cid:48) × . (cid:48)
75 field of view on the sky at any giveninstant.In the photometer mode there are two astronomicalobserving templates (AOT) available, in addition to aPACS/SPIRE parallel observing mode. For our
Her-schel
GOALS program we used the scan map tech-nique for all of our astronomical observing requests(AOR), which is ideal for mapping large areas of thesky and/or targets where extended flux may be present.Our scan map observations involve slewing the tele-scope at constant speed along parallel lines separatedby 15 (cid:48)(cid:48) from each other, perpendicular to the scan di-rection. Two example PACS observation footprintsare shown in Figure 2 panels (a) and (c), overlaid onimages from the Digital Sky Survey (DSS). The area 9 erschel PACS and SPIRE Transmission Curves
100 1000Wavelength [ µ m]0.00.20.40.60.81.0 N o r m a li ze d R e s p o n s e Fig. 1.— The normalized filter transmission curves for our
Herschel data. From left to right are the PACS 70 µ m,100 µ m, 160 µ m channels, followed by the SPIRE 250 µ m, 350 µ m, and 500 µ m channels. For the SPIRE bands, thepoint source response is shown with a solid curve, while the extended source response is shown with a dashed curve.Note the large difference in response for the SPIRE 500 µ m transmission curve.of maximum coverage is the inner region centered onthe red box, where the requested observation is cen-tered. For the GOALS observations we chose to ob-serve 7 scan legs in each scan and cross-scan using the20 (cid:48)(cid:48) /sec scan speed, with scan leg lengths ranging be-tween 3 – 6 (cid:48) depending on the size of the target. At thisscan speed the beam profiles for each wavelength havemean FWHM values of 5 . (cid:48)(cid:48)
6, 6 . (cid:48)(cid:48)
8, and 11 . (cid:48)(cid:48) µ m, 100 µ m, and 160 µ m channels respectively.Before each PACS photometer observation is a 30sec. chopped calibration measurement between two in-ternal calibration sources (the calibration block), fol-lowed by 5 sec. of idle for telescope stability beforethe science observation is executed. As the telescopeis scanned across the sky during science observations,all of the bolometer pixels are read out at a frequencyof 40 Hz, even during periods where the telescope wasturning around for the next scan leg. However due tosatellite data-rate limitations, all PACS data are aver-aged over four frames effectively downsampling thedata to 10 Hz. The result is a data timeline of the fluxseen by each detector pixel as a function of time (andby extension position on the sky) as the telescope isscanned over the target field.In order to accurately reconstruct the image, twoscan map AORs at orthogonal angles are required.This is because as the telescope scans a field, the off-sets of each bolometer subarray, and even each pixel,may be different from its neighbor resulting in stripes or gradients in the final reconstructed map. Howeverif the same field is scanned in two orthogonal direc-tions, many of these map artifacts can be successfullyremoved, by virtue of multiple different bolometerssampling each patch of the sky. Furthermore in or-der to maximally sample a given sky pixel by as manybolometer pixels as possible, we chose our scan an-gle to be 45 ◦ and 135 ◦ with respect to the detector ar-ray. The orthogonal scans similarly help remove driftsin the bolometer timelines, which are time-dependentvariations in the detector or subarray offsets, caused byfor example cosmic ray hits and other instrument ef-fects. For our survey the typical PACS scan duration isabout 200 sec., however larger maps with deeper cov-erage can be as long as ∼ IRAS µ m flux of at least 5.24 Jy, thegalaxies or galaxy systems are bright enough such thatonly one repetition was needed for each PACS scanand cross scan. With one pair of scan and cross-scanobservations, we achieved a 1- σ point source sensitiv-ity of approximately 4 mJy in the central area, and ap- 10roximately 8 mJy averaged over the entire map forboth blue and green observations. By combining allfour red channel scans and cross-scans we achieved a1- σ point source sensitivity of about 6 mJy in the cen-tral area, and about 12 mJy averaged over the entiremap. On the other hand the extended flux sensitivitiesfor one repetition (one scan and cross-scan pair) are5.3 MJy sr − , 5.2 MJy sr − , and 1.7 MJy sr − for the70 µ m, 100 µ m, and 160 µ m channels respectively. The Spectral and Photometric Imaging Receiver(SPIRE, Griffin et al. 2010) is a submillimeter cam-era on
Herschel that operates between the 194-671 µ m wavelength range. In the imaging mode, it cansimultaneously observe in three different broad band-passes ( λ/ ∆ λ ∼ ), centered at 250 µ m, 350 µ m,and 500 µ m. Similar to PACS, SPIRE images a fieldby scan mapping, where the instrument field of view(4 (cid:48) × (cid:48) ) is scanned across the sky to maximize thespatial coverage. The three detector arrays use hexag-onal feedhorn-coupled bolometers, with 139, 88, and43 bolometers for the PSW (250 µ m), PMW (350 µ m),and PLW (500 µ m) channels respectively. The beamprofiles for each wavelength have mean FWHM val-ues of 18 . (cid:48)(cid:48)
1, 25 . (cid:48)(cid:48)
2, and 36 . (cid:48)(cid:48) µ m, 350 µ m,and 500 µ m photometer arrays, and mean ellipticitiesof 7%, 12%, and 9% (the beam shape changes slightlyas a function of off-axis angle).There are three main observing modes avail-able: point source photometry, field/jiggle map-ping, and scan mapping. For our observing program(dsanders OT1 1) we chose the scan-map mode at ascan rate of 30 (cid:48)(cid:48) /sec., since it gave the best data qual-ity and also larger field of view for the final map thanthe other two mapping modes. Nominal scan anglesof 42.4 ◦ and 127.2 ◦ with respect to the detector ar-rays were used to maximize sky coverage by as manydetectors as possible, and to minimize the effect of in-dividual bolometer drift during data processing. LikePACS, two scans are needed for data redundancy aswell as cross-linking, however the scan and cross-scanwith SPIRE are observed within a single AOR. Withinour program, the vast majority of our targets were ob-served in the small map mode ( ∼
150 targets), whilethe rest were taken in the large map mode ( ∼
20 tar-gets). The typical scan durations are ∼
170 sec. forsmall maps ( ∼ (cid:48) × (cid:48) guaranteed map coverage area),and up to ∼ Her-schel optics and SPIRE instrument, only one repetitionwas observed for every target in our observing pro-gram. The SPIRE instrument has a confusion limit of5.8, 6.3, and 6.8 mJy beam − for the 250 µ m, 350 µ m,and 500 µ m channels, which is defined as the stan-dard deviation of the flux density in the limit of zeroinstrument noise (Nguyen et al. 2010). On the otherhand the instrument noise is about 9, 7.5, and 10.8 mJybeam − at 250 µ m, 350 µ m, and 500 µ m for one rep-etition (scan and cross-scan) at the nominal scan speedof 30 (cid:48)(cid:48) /sec. Since many of our targets have extendedfeatures, SPIRE’s 1- σ sensitivities to extended flux areat the 1.4 MJy sr − , 0.8 MJy sr − , and 0.5 MJy sr − levels for 250 µ m, 350 µ m, and 500 µ m for one repe-tition. These flux levels are already dominated by con-fusion noise, and is more than enough to detect anycold dust components in our sample. Table 2 below lists the observing log for our datasample. Column 1 is the galaxy reference number, andcolumn 2 is the IRAS name of the galaxy, ordered byascending RA. Column 3 is the common optical coun-terpart names to the galaxy systems. Columns 4 –7 are the observation IDs for PACS imaging. Bluecorresponds to a wavelength of 70 µ m, while greencorresponds to 100 µ m. Each blue and green ob-servation pair simultaneously observes the red 160 µ m channel. Two orthogonal observations are madeat each wavelength to reduce imaging artifacts. Wenote that four galaxies in our sample do not have 100 µ m observations available since they were from otherprograms that did not observe them: IRAS F02401-0013 (NGC 1068), IRAS F09320+6134 (UGC 05101),IRAS F15327+2340 (Arp 220), and IRAS F21453-3511 (NGC 7130). Column 8 is the PACS observa-tion duration for each scan and cross-scan, unless oth-erwise noted. We note these are not exposure times,but instead the amount of time for each scan andcross-scan. Columns 9 – 10 are the observation dates(in YYYY-MM-DD) for each pair of PACS scan andcross-scan, unless otherwise noted, while column 11 11s the Program ID of the PACS program from whichthe data were obtained. We list the PID correspond-ing to each number in Table 2’s caption. The bulkof the data ( ∼ µ m, 350 µ m, and500 µ m observations. The scans and cross-scans foreach target is combined into one observation. Column13 is the SPIRE observation duration, which is similarto the PACS duration. Column 14 is the SPIRE obser-vation date, and column 15 is the PID of the SPIREprogram from which the data were obtained, similar tothe PACS PID column. 12 a) (b)(c) (d) Fig. 2.— The PACS and SPIRE observation footprints for two galaxies, IRAS F18145+2205 (CGCG 142-034) in thetop row, and IRAS F20221-2458 (NGC 6907) on the bottom. These figures were generated using HSPOT, the Herschelobservation planning tool, while the background images used are from DSS. The red box in each panel indicates thecentral coordinate for each observation. The PACS observations are shown in panels (a) and (c), which show a 9 (cid:48) × (cid:48) field of view around the target coordinate. Each scan leg in one direction is repeated several times (nominally 7times) for maximal coverage of the source galaxy (or galaxies). The SPIRE observations are shown in panels (b) and(d), and have a 25 (cid:48) × (cid:48) field of view, which is much larger than the PACS field of view. Panel (b) shows a small mapscan, while the bottom panel shows a large map scan. 13 A B LE H E R S C H EL O B S E R VA T I ON L OG P A C SSP I R E I R A S N a m e O p ti ca l N a m e B l u e B l u e G r ee n1 G r ee n2 D u r a ti on B l u e G r ee n P A C S O b s . I DD u r a ti on O b s . D a t e SP I R E O b s . I DO b s . I DO b s . I DO b s . I D ( s ec . ) O b s . D a t e O b s . D a t e P I D ( s ec . ) P I D ( )( )( )( )( )( )( )( )( )( )( )( )( )( )( ) F + NG C - - - - - -
181 2 F - NG C , M r k93813422124631342212464134221246513422124662762011 - - - - - -
293 3 F - A r p256 , M C G - - - / - - - - - -
181 4 F - E S O -I G , H a r o11134221063613422106371342197713134219771465 b - - - - - - F - NG C - - - - - -
181 6 F + M C G + - - - - - - - -
294 7 F + NG C B - - - - - -
271 8 F - I C , A r p2361342212754134221275513422128461342212847652011 - - - - - -
292 9 F - M C G - - - - - - - - -
181 10 F - E S O - G - - - - - -
181 11 F + C G C G - - - - - - -
141 12 F - E S O - G - - - - - -
181 13 F - RR , E S O - G / - - - - - -
181 14 F - - - - - - -
021 15 F + III Z w - - - - - -
151 16 F + NG C - - - - - -
271 17 F + UG C - - - - - -
271 18 F - NG C - - - - - -
141 19 F + NG C - - - - - -
011 20 F + I C - - - - - -
271 21 F + NG C - - - - - -
271 22 F + M C G + - - - - - - - -
271 23 F + UG C - - - - - -
291 24 F - NG C - - - - - -
271 25 F + NG C - - - - - -
011 26 F - NG C ······ - - - - - -
178 27 F + UG C - - - - - -
271 28 F + - - - - - -
011 28 F + a M A S X J + - - - - ············ F + UG C - - - - - -
011 30 F + UG C - - - - - -
011 30 F + a UG C - - - - ············ F + NG C - - - - - -
242 32 F + - - - - - -
011 33 F - NG C - - - - - - A B LE — C on ti nu e d P A C SSP I R E I R A S N a m e O p ti ca l N a m e B l u e B l u e G r ee n1 G r ee n2 D u r a ti on B l u e G r ee n P A C S O b s . I DD u r a ti on O b s . D a t e SP I R E O b s . I DO b s . I DO b s . I DO b s . I D ( s ec . ) O b s . D a t e O b s . D a t e P I D ( s ec . ) P I D ( )( )( )( )( )( )( )( )( )( )( )( )( )( )( ) F + - - - - - -
011 35 F + C G C G - - - - - - -
011 35 F + a C G C G - - - - - ············ + - - - - - -
291 37 F + UG C - - - - - -
011 38 F - E S O - G - - - - - -
011 39 F - E S O -I G - - - - - -
011 40 F - NG C - - - - - -
011 4104271 + - - - - - -
211 42 F - NG C - - - - - -
244 43 F + UG C - - - - - -
011 44 F - E S O -I G - - - - - -
011 45 F - M C G - - - - - - - - -
221 46 F - NG C - - - - - -
011 46 F - a NG C - - - - ············ F + C G C G - - - - - - -
011 4805083 + - - - - - -
231 49 F + V II Z w - - - - - -
211 5005129 + - - - - - -
211 51 F - - - - - - -
244 52 F - - - - - - -
011 5305368 + M C G + - - - - - - - -
211 54 F + NG C - - - - - -
021 55 F + UG C - - - - - -
211 5605442 + - - - - - -
231 57 F - - - - - - -
011 58 F + UG C - - - - - -
211 59 F + NG C - - - - - -
255 60 F - E S O -I G - - - - - -
161 61 F - E S O - G - - - - - -
011 62 F + UG C - - - - - -
231 63 F - - - - - - -
231 64 F - A M - - - - - - -
231 6507063 + NG C - - - - - -
101 66 F - NG C - - - - - - A B LE — C on ti nu e d P A C SSP I R E I R A S N a m e O p ti ca l N a m e B l u e B l u e G r ee n1 G r ee n2 D u r a ti on B l u e G r ee n P A C S O b s . I DD u r a ti on O b s . D a t e SP I R E O b s . I DO b s . I DO b s . I DO b s . I D ( s ec . ) O b s . D a t e O b s . D a t e P I D ( s ec . ) P I D ( )( )( )( )( )( )( )( )( )( )( )( )( )( )( ) - - - - - - -
111 68 F + NG C - - - - c - -
221 69 F + M C G + - - - - - - - -
221 69 F + a NG C - - - - d ············ - - - - - - -
201 71 F + - - - - - -
211 72 F + NG C - - - - - -
104 7308424 - E S O -I G - - - - - -
111 74 F - E S O -I G - - - - - -
161 75 F + - - - - - -
106 7609022 - - - - - - -
116 77 F - - - - - - -
111 78 F + UG C - - - - - -
111 79 F + UG C ······ - - - - - -
217 80 F + M C G + - - - - - - - -
101 81 F + A r p303 , I C / - - - - - -
111 82 F - NG C e e e e - - - - - -
181 83 F - E S O -I G - - - - - -
171 84 F + - - - - - -
221 85 F + NG C - - - - - -
031 86 F - NG C - - - - - -
162 87 F - E S O - G - - - - - -
021 88 F - E S O - G - - - - - -
021 89 F + - - - - - -
186 90 F + M C G + - - - - - - - -
221 91 F - C G C G - - - - - - -
181 92 F + I C - - - - - -
201 93 F - E S O - G - - - - - -
171 94 F + NG C , A r p29913422106001342210601134221110413422111054852010 - - - - - -
292 95 F - E S O - G - - - - - -
094 96 F - E S O -I G - - - - - -
021 97 F + - - - - - -
181 98 F + NG C - - - - - -
111 99 F - E S O - G - - - - - -
171 99 F - a E S O - G - - - - ············ A B LE — C on ti nu e d P A C SSP I R E I R A S N a m e O p ti ca l N a m e B l u e B l u e G r ee n1 G r ee n2 D u r a ti on B l u e G r ee n P A C S O b s . I DD u r a ti on O b s . D a t e SP I R E O b s . I DO b s . I DO b s . I DO b s . I D ( s ec . ) O b s . D a t e O b s . D a t e P I D ( s ec . ) P I D ( )( )( )( )( )( )( )( )( )( )( )( )( )( )( ) - - - - - - -
201 101 F - - - - - - -
181 102 F - NG C - - - - - -
181 103 F + UG C , M r k2311342199861134219986213422067041342206705652010 - - - - - -
262 104 F + NG C - - - - - -
181 105 F + C G C G - - - - - - -
181 106 F - M C G - - - - - - - - -
171 107 F - E S O - G - - - - - -
171 10813052 - - - - - - -
201 109 F + I C - - - - - -
181 11013120 - - - - - - -
206 111 F + VV a - - - - - -
221 112 F + UG C - - - - - -
124 113 F + NG C - - - - - -
011 114 F - M C G - - - - - - - - -
011 115 F - NG C - - - - - -
074 11613242 - E S O - G - - - - - -
234 117 F - I C - - - - - -
021 118 F + NG C - - - - - -
091 119 F + A r p240 , NG C / - - - - - -
171 120 F + UG C , M r k27313422084441342208445134221043213422104331532010 - - - - - -
262 121 F + UG C - - - - - -
011 122 F - E S O -I G - - - - - -
281 123 F + NG C - - - - - -
011 124 F + A r p84 , NG C / - - - - - -
011 125 F + C G C G - - - - - - -
091 126 F + NG C - - - - - -
011 127 F - - - - - - -
286 128 F - - - - - - -
286 129 F - NG C - - - - - -
011 130 F + VV a , A r p30213422353821342235383134223538413422353851982011 - - - - - -
171 131 F - I C A / B - - - - - -
021 132 F + C G C G - - - - - - -
154 133 F + VV - - - - - -
221 13415206 - E S O - G - - - - - - A B LE — C on ti nu e d P A C SSP I R E I R A S N a m e O p ti ca l N a m e B l u e B l u e G r ee n1 G r ee n2 D u r a ti on B l u e G r ee n P A C S O b s . I DD u r a ti on O b s . D a t e SP I R E O b s . I DO b s . I DO b s . I DO b s . I D ( s ec . ) O b s . D a t e O b s . D a t e P I D ( s ec . ) P I D ( )( )( )( )( )( )( )( )( )( )( )( )( )( )( ) F + - - - - - -
176 136 F + NG C - - - - - -
281 137 F + A r p220 , UG C ······ - - - - - -
298 138 F + NG C - - - - - -
281 139 F + NG C - - - - - -
231 140 F + NG C - - - - - -
221 141 F - - - - - - -
231 142 F + C G C G - - - - - - -
231 14316304 - NG C - - - - - -
221 144 F - E S O -I G - - - - - -
111 145 F - - - - - - -
221 146 F - E S O - G - - - - - -
221 147 F + NG C - - - - - -
232 148 F - - - - - - -
221 149 F + NG C , A r p29313422093311342209332134220933313422093344852010 - - - - - -
211 150 F + - - - - - -
211 151 F - - - - - - -
221 152 F - - - - - - -
234 153 F - E S O - G - - - - - -
221 154 F + UG C - - - - - -
221 155 F + C G C G - - - - - - -
221 15617578 - - - - - - -
221 15718090 + - - - - - -
221 158 F + NG C , A r p8113422120291342212030134221203113422120324032010 - - - - - -
131 159 F - I C - - - - - -
254 160 F + C G C G - - - - - - -
221 161 F - - - - - - -
214 162 F + NG C A / B - - - - - -
211 163 F - I C - - - - - -
221 164 F + NG C - - - - - -
211 165 F + VV , NG C , UG C - - - - - -
081 166 F - E S O -I G - - - - - -
131 167 F - - - - - - -
116 16819542 + - - - - - -
111 169 F - E S O - G - - - - - - A B LE — C on ti nu e d P A C SSP I R E I R A S N a m e O p ti ca l N a m e B l u e B l u e G r ee n1 G r ee n2 D u r a ti on B l u e G r ee n P A C S O b s . I DD u r a ti on O b s . D a t e SP I R E O b s . I DO b s . I DO b s . I DO b s . I D ( s ec . ) O b s . D a t e O b s . D a t e P I D ( s ec . ) P I D ( )( )( )( )( )( )( )( )( )( )( )( )( )( )( ) F - NG C - - - - - -
111 17120264 + M C G + - - - - - - - -
301 172 F - NG C - - - - - -
101 17320351 + - - - - - -
301 174 F + C G C G - , II Z w - - - - - -
301 175 F - E S O -I G - - - - - -
116 176 F - E S O - G - - - - - -
111 17721101 + - - - - - -
081 178 F - E S O -I G - - - - - -
121 179 F - NG C ······ - - - - - -
237 180 F - E S O - G - - - - - -
061 181 F - I C - - - - - -
111 182 F - E S O - G - - - - - -
181 183 F + UG C - - - - - -
131 184 F - E S O -I G - - - - - -
191 185 F - - - - - - -
186 186 F + NG C , I C , A r p29813422117751342211776134221177713422117784852010 - - - - - -
244 187 F + C G C G - - - - - - -
191 188 F - E S O -I G - - - - - -
092 189 F + I C - - - - - -
191 190 F - NG C - - - - - -
232 191 F + NG C - - - - - -
191 192 F - NG C - - - - - -
191 193 F - E S O -I G - - - - - -
111 194 F + NG C , H C G - - - - - -
189 19523262 + NG C - - - - - -
191 19523262 + a NG C - - - - ············ F + - - - - - -
186 197 F - M C G - - - - - - - - -
191 197 F - a M C G - - - , M r k93313422218011342221799134222180013422217982402011 - - - - ············ + - - - - - -
031 199 F + A r p86 , NG C / - - - - - -
181 200 F + NG C - - - - - -
294 201 F + M r k33113422252421342225243134222524013422252412402011 - - - - - - O TE . — T h ec o l u m nd e s c r i p ti on s a r e ( ) t h e r o w r e f e r e n ce nu m b e r . ( ) T h e I R A S n a m e o f t h e g a l a xy , o r d e r e dby a s ce nd i ng R A . G a l a x i e s w it h t h e“ F ” p r e fi xo r i g i n a t e fr o m t h e I RA S F a i n t S ou r ce C a t a l og , a ndg a l a x i e s w it hno “ F ” p r e fi x a r e fr o m t h e P o i n t S ou r ce C a t a l og . ( ) C o mm onop ti ca l c oun t e r p a r t n a m e s t o t h e g a l a xy s y s t e m s . ( ) – ( ) a r e t h e ob s e r v a ti on I D s f o r P A C S i m a g i ng . B l u ec o rr e s pond s t o a w a v e l e ng t ho f µ m , w h il e g r ee n c o rr e s pond s t o100 µ m . E ac hb l u ea ndg r ee nob s e r v a ti on s i m u lt a n e ou s l yob s e r v e s t h e r e d160 µ m c h a nn e l . E ac hob s e r v a ti onn ee d s a s e p a r a t e s ca n a nd c r o ss - s ca n t o r e du ce i m a g i ng a r ti f ac t s . F ou r g a l a x i e s i nou r s a m p l e dono t h a v e µ m ob s e r v a ti on s a v a il a b l e s i n ce t h e y w e r e fr o m o t h e r p r og r a m s : I R A SF - ( NG C ) , I R A SF + ( UG C ) , I R A S F + ( A r p220 ) , a nd I R A SF - ( NG C ) . ( ) T h e P A C S ob s e r v a ti ondu r a ti on f o r eac h s ca n a nd c r o ss - s ca n , un l e ss o t h e r w i s e no t e d . W e no t e t h e s ea r e no t e xpo s u r e ti m e s . ( ) – ( ) T h e ob s e r v a ti ond a t e s f o r eac h s ca n a nd c r o ss - s ca n , un l e ss o t h e r w i s e no t e d . ( ) T h e P I o f t h e P A C S p r og r a m fr o m w h i c h t h e d a t a w e r e ob t a i n e d . S ee P I li s t b e l o w . ( ) T h e SP I R E ob s e r v a ti on I D , w h i c h i n c l ud e s a llt h r ee µ m , µ m , a nd500 µ m ob s e r v a ti on s . T h e s ca n s a nd c r o ss - s ca n s f o r eac h t a r g e ti s c o m b i n e d i n t oon e ob s e r v a ti on . ( ) T h e SP I R E ob s e r v a ti ondu r a ti on . W e no t e t h e s ea r e no t e xpo s u r e ti m e s . ( ) T h e SP I R E ob s e r v a ti ond a t e . ( ) T h e P I D o f t h e SP I R E p r og r a m fr o m w h i c h t h e d a t a w e r e ob t a i n e d . S ee P I D li s t b e l o w . P I li s t: = O T s a nd e r s ; = K P G T e s t u r m ; = G T m s a n c h ez ; = K P O T pv a nd e r w ; = K P O T r k e nn i c u1 ; = O T f a rr a h1 ; = G T l s p i nog l ; = c w il s o011 ( i n c l ud i ng K P G T ) ; = O T m c l uv e r ; = K P G T s m a dd e . a T h e s ea r e v e r y w i d e l y s e p a r a t e dg a l a xyp a i r s t h a t r e qu i r e d t w o H e rs c h e l P A C S ob s e r v a ti on s . b G r ee n1 a nd G r ee n2h a v e du r a ti on s o f s ec ., B l u e a s a du r a ti ono f s ec . a nd B l u e a s a du r a ti ono f s ec . c G r ee n2 w a s ob s e r v e don2012 - - . d G r ee n2 w a s ob s e r v e don2012 - - . e R e s c h e du l e d t o r e p l ace p r e v i ou s P A C S ob s e r v a ti on s : . . Data Processing and Reduction The data processing for our
Herschel data was per-formed using the Herschel Interactive Processing En-vironment (HIPE, Ott 2010) version 14 software tool,which provides the means to download, reduce, andanalyze our data. All of our data reduction routines arederived from the standard pipeline scripts found withinHIPE, where the programming language of choice isJython (a Java implementation of the popular Pythonlanguage). In addition to handling the data processing,HIPE also downloads and maintains all of the instru-ment calibration files needed for the data processing.
Due to the bolometer and scanning nature of thePACS instrument, it was important to determine thebest map-making software to translate the time ordereddata (TOD) into an image. The PACS bolometers(indeed all bolometers) produce noise that increasesas one approaches lower temporal frequencies, com-monly referred to as /f noise, that must be removedby the map-maker. If this noise is left uncorrectedin the time ordered data, the result would be severestriping or even gradients across the image. In addi-tion the map making software must also remove thebolometers’ common mode drift (which is a chang-ing offset as function of time) from the TOD, termed pre-processing , as well as cosmic ray hits and individ-ual bolometer drift. The PACS team released a Map-making Tool Analysis and Benchmarking report inNovember 2013 with an update in March 2014 thatcharacterized in detail the six different map makingpackages available to reduce PACS data. We sum-marize the information presented in this report belowto decide upon the best map making software to use,since it was important that all of the Herschel data onour sample were processed uniformly.The PACS team tested the performance of sixdifferent publicly available map-making packages:MADMap (Microwave Anisotropy Dataset mapper,Cantalupo et al. 2010), SANEPIC (Signal And NoiseEstimation Procedure Including Correlation, Patan-chon et al. 2008), Scanamorphos (Roussel 2013), JS-canam (Jython Scanamorphos ), Tamasis (Tools for http://herschel.esac.esa.int/twiki/pub/Public/PacsCalibrationWeb/pacs mapmaking report ex sum v3.pdf This is the HIPE/PACS implementation of the Scanamorphos algo-
Advanced Map-making, Analysis and SImulationsof Submillimeter surveys, Barbey et al. 2011), andUnimap (Piazzo et al. 2015) (see § § . – Jy, while the“faint flux regime” is defined to be . – . Jy (seeFigure 5). Below we summarize the five tests per-formed on each map maker from the benchmarkingreport:1) A power spectrum analysis which tests the mapmaker’s ability to remove noise while preserving ex-tended fluxes over large angular sizes on the map. Thistests each code’s performance in removing the /f noise from the PACS data, and consequently how wellgradients and stripes are removed from the maps.2) A difference matrix is computed for each mapmaker’s output, which evaluates differences in fluxesfor individual sky pixels over the entire image. ( S − S true ) is computed for each pixel and plotted against S true , and the resulting scatter, offset, and slope isevaluated.3) Each map maker’s performance in point sourcephotometry is compared to fluxes measured from theHPF maps for both bright ( . – Jy) and faint ( . – . Jy) cases. Since the HPF maps produced byHIPE are designed specifically for the case of pointsources, they provide the most accurate reference pointsource fluxes.4) Extended source photometry tests each mapmaker’s ability to recover extended flux over largeareas of the map. To assess this, each code’s output iscompared to IRAS data on M31 from the ImprovedReprocessing of the IRAS Survey (IRIS, Miville-Deschˆenes & Lagache 2005).5) The noise characteristics each map maker intro-duces into the final map are evaluated. This includesstatistical tests on the pixel-to-pixel variance as well asthe shape of the overall distribution of fluxes in eachmap pixel. The noise patterns are also evaluated with rithm however they both differ in many assumptions, hence why theywere tested separately. ( S − S true ) vs. S true plot, and it yielded themost accurate photometry for both point and extendedsources in both channels.For a small fraction of our maps where JScanamcould not remove all of the image artifacts (usuallygradients due to non-optimal baseline subtraction), weused Unimap to process the data, since it performedjust as well as JScanam. Unlike JScanam, Unimapapproaches map making differently, using the Gen-eralized Least Square (GLS) approach, which is alsoknown as the Maximum Likelihood method if thenoise has a Gaussian distribution. For a very few caseswhere even Unimap did not produce optimal results,we resorted to using MADMap. This map maker re-quires that the noise properties of the detectors are de-termined a-priori , from which a noise filter can be gen-erated to filter out the /f noise. Finally, despite thatnot all of the PACS maps were generated using thesame map maker, we note that the resulting photom-etry from all three map makers are remarkably con-sistent as shown in the Benchmarking report (and ad-dendum) from the PACS team, hence giving one thefreedom to use the map maker that produces the bestimage quality. All of our
Herschel -GOALS PACS data were re-duced in HIPE 14 using the latest available PACS cal-ibration version 72 0 released in December 2015. Inorder to alleviate the processing time for all 211 ob-jects, we started our data processing from the Level 1 products downloaded from the HSA. These Level 1data products have the advantage of an improved re-construction of the actual
Herschel spacecraft point-ing, which reduces distortions on the PSF due to jittereffects. Compared to previous maps from our data pro-cessing, the new maps have slight shifts of up to ∼ . (cid:48)(cid:48) photAssignRaDec to assign theRA and declination coordinates to each pixel in eachframe which allows JScanam to run faster. The nextstep was to remove the unnecessary frames taken dur-ing each turnaround in the scan or cross-scan usingthe scanamorphosRemoveTurnarounds task.We opted to use the default speed limit which is ± of our nominal scan speed (20 (cid:48)(cid:48) /sec.), so anyframes taken at scan speeds below 10 (cid:48)(cid:48) /sec. or above30 (cid:48)(cid:48) /sec. were removed. After turnaround removal the scanamorphosMaskLongTermGlitches taskin JScanam goes through the detector timelines andmasks any long term glitches.At this point we have a detector timeline of flux de-tected by the bolometers as a function of time with theturnarounds and long term glitches removed. Usingthe scanamorphosScanlegBaselineFitPerPixel task, our next step is to subtract a linearly fit baselinefrom each bolometer pixel of every scan leg, with theintention of creating a “naive” map for source mask-ing purposes. This is done iteratively where the mostimportant parameter is the nSigma variable, whichcontrols the threshold limit for source removal. Forour data any points above nSigma =2 times the stan-dard deviation of the unmasked data are consideredreal sources, until the iteration converges.The next step is to join the scan and cross-scan datatogether for a higher signal-to-noise map to create thesource mask. In the scanamorphosCreateSourceMask task we set a nSgima =4 , so that any emission above 22 standard deviations is masked out. At this point itis not necessary to mask out all of the faint extendedemission, only the brightest regions. After the sourcemask is determined, they are applied to the individualscan and cross-scan timelines and the real processingbegins.With the galactic option set to “true” in scana-morphosBaselineSubtraction , we only wantto remove an offset in the time ordered data over allthe scan legs, and subtract it from all the frames. Thisis done by calculating a median offset over only theunmasked part of the data which importantly does notinclude any bright emission, and subtracting it fromeach pixel’s timeline. This is so that extended flux istreated correctly when subtracting the baseline (due tothe telescope’s own infrared emission) from the signaltimelines, even in cases where the emission is not con-centrated in a small region. We emphasize this doesnot imply the subtraction of the Galactic foregroundemission from our maps.Once the baseline is removed we need to iden-tify and mask the signal drifts produced by the cal-ibration block observation. In previous versions ofour reduction, these drifts have produced very no-ticeable gradients in our final maps. To do this thetask scanamorphosBaselinePreprocessing assumes that the scan and cross-scan are orthogonalto each other, which would result in gradients in dif-ferent directions. The drift removal is also based onthe assumption that the drift power increases with thelength of the considered time (1/ f noise). For thisreason the first iteration removes the drift componentover the longest time scale which corresponds to theentire scan (or cross-scan). After that drifts are re-moved over four scan legs, and finally over one scanleg, with the remaining drift in each successive iter-ation becoming weaker. In order to actually calculatethe drift in each iteration, a single scan (or scan legs) isback projected over itself in the orthogonal direction,which transforms the generally increasing or decreas-ing signal drift into oscillatory drifts that cancel out onlarge time scales. The orthogonal back projected time-line is then subtracted from the scan timeline, and thedifference which represents the drift is fitted by a line.At this point the scan and cross-scan data have beencleaned enough to be combined. Since signal driftswere only eliminated over timescales down to one scanleg, the next step is to remove them from over timescales shorter than one scan leg. These drifts are due tofor example cosmic ray hits on the PACS instruments, which produce different effects on the time ordereddata depending on which part is hit. If an individualbolometer or bolometer wall is hit, it only affects thosebolometer(s). However if a cosmic ray hits the readoutelectronics, it introduces a strong positive or negativesignal for all of the bolometers read by the electron-ics, which can be anything from a single bolometer toan entire detector group. These jumps typically last afew tens of seconds before settling to the previous levelagain, and would result in stripes across the final mapif not properly removed.To remove these individual drifts, we use thetask scanamorphosIndividualDrifts to firstmeasure the scan speed and calculate the size of a mappixel that can hold six subsequent samples of a detec-tor pixel crossing it. We use a threshold of nSigma =5 which is large enough to include the strongest drifts butstill masking out the real source. Then the average fluxvalue and standard deviation from the detector pixelscrossing that map pixel is calculated, along with thenumber of detector pixels falling into that map pixel.Using the threshold noise value (from the calibrationfiles), we eliminate any individual detector fluxes forthat map pixel that has a standard deviation greaterthan the noise threshold. The missing values are thenlinearly interpolated, and the individual drift is sub-tracted from the detector timeline.After all of the individual drifts are corrected, thetime ordered data are saved and we project the time-lines from both the scans and cross-scans into our finalmap using the photProject task. We use a pixelscale of 1 . (cid:48)(cid:48) − for the 70 µ m and 100 µ m maps,and a pixel scale of 3 . (cid:48)(cid:48) − for the 160 µ m maps.By default the photProject task assumes in pro-jection an active pixel size of 640 µ m, however if we‘drizzle’ the projection we can assume smaller PACSpixels. This allows us to reduce the noise correlationbetween neighboring map pixels and also sharpens thePSF. We used a pixfrac of . , which controls theratio between the input detector pixel size and the mappixel size. At this point the 70 µ m and 100 µ m mapsare finished. For the 160 µ m data, both pairs of scanand cross-scan are identically processed separately,and then combined in the end using photProject again. 23 .2. SPIRE Data Reduction Similar to the PACS instrument, the SPIRE de-tectors exhibit certain effects that are characteristicto bolometers. Namely, they introduce an increasingamount of noise as the length of the considered timeincreases ( /f noise), as well as constant and chang-ing offsets (drifts) which could result in stripes or gra-dients in the final image. Therefore any map makerfor SPIRE must be able to remove these instrumen-tal effects, while preserving flux (point source and ex-tended) and creating distortion-free maps. The SPIREteam released a Map Making Test Report in January2014 that benchmarked in depth seven different mapmaking codes, several of which were also present inthe PACS Map Making report. The map makers thatparticipated in the benchmarking were the Naive Map-per, Destriper in two flavors (P0 and P1), Scanamor-phos, SANEPIC, and Unimap. The two flavors of theDestriper differ in the polynomial order used to sub-tract the baseline, where P0 corresponds to a polyno-mial order of 0 (i. e. the mean) and P1 corresponds toan order of 1. Two additional super-resolution mapmakers were also tested, however we did not considerthem for processing our SPIRE data. For a summaryof each map maker we refer the reader to the SPIREMap Making Test Report.For the Map Making Test Report, the authors testedthese five map makers based on a variety of bench-marks that are very similar to the PACS Map-MakingTool Analysis and Benchmarking report. A combi-nation of real and simulated SPIRE data were used,covering the full variety of science cases such as faintvs. bright sources, extended vs. point sources, andcomplex vs. empty fields. The simulated SPIRE datahave the advantage of comparing each of the map mak-ers’ outputs to the “truth” image, allowing for an unbi-ased comparison between all of the map making codes.These simulated observations were synthesized fromtwo different layers: a truth layer based on a real orartificial source, and a noise layer from real SPIREobservations so that both instrumental and confusionnoise is accurately represented. Below we summarizethe four metrics and performance results for the fivepossible map makers:1) Using simulated data, the deviation of each mapmaker’s output is compared to the original synthetic http://arxiv.org/pdf/1401.2109v1.pdf data. To quantify the deviation from truth, a scatterplot of ( S − S true ) is plotted against S true , and theresulting slopes, relative deviations, and absolute de-viations are compared.2) The 2D power spectrum of each map makers’output is compared to the “truth” image. The goal hereis to quantify how well /f noise is removed from themaps while leaving real fluxes (point and extended) in-tact, as well as how high spatial frequency (small spa-tial scale) fluxes are treated.3) Using the simulated data, point source photome-try from each of the map makers were compared to the“truth” images. This tests how well point source fluxesare recovered by each map maker in both the bright( S ≈ mJy) and faint ( S ≈ mJy) regimes.4) Finally, extended source photometry was testedbetween all the map makers using the synthetic data. Asimulated exponential disk with an e -folding radius of90 (cid:48)(cid:48) was used, and fluxes were measured using aperturephotometry.Using the results from these tests, we concludedthat the best map maker to use was the Destriper P0mapper. It performed remarkably well among the othermap makers, especially in cases where complex ex-tended emission is present. Although the Map Makingreport warned about its inability to properly removethe “cooler burp” effect, the most recent version of De-striper P0 in HIPE 14 was updated to include propertreatment of this instrument effect. On the other handDestriper P1 compared unfavorably, especially in in-troducing artificial gradients in many cases. The NaiveMapper was also ruled out due to it frequently over-subtracting the background where extended emissionis present. The map maker SANEPIC showed signifi-cant deviations from the “truth” map, because the codemakes some incorrect assumptions about the data. Fi-nally, although Scanamorphos can handle faint pixelsvery well, it showed significant deviations in the brightpixel case ( S > . Jy). This is important since manygalaxies in our sample are nearby and thus quite bright.In HIPE 14, we used a more advanced version ofthe Destriper code called the “SPIRE 2-Pass Pipeline”that was released by the SPIRE instrument team. Thebasic pipeline processing steps and settings follow ex-actly that of the Destriper P0 (or P1 if the user sochooses) map maker, with the added benefit of pro-ducing exceptionally clean maps to be used in the fi-nal
Herschel
Science Archive. Specifically, the 2-PassPipeline mitigates residual faint tails and glitches in 24he timeline, which if not removed can produce ringingeffects. The primary aim of this pipeline is to producemaps with better detections of outliers in the TOD suchas glitches, glitch tails, and signal jumps, and removeany Fourier ringing that would result from failed out-lier detections. As an overview, the first pass runs astripped down version of the pipeline using only thebare minimum tasks that excludes any Fourier analy-sis. This includes running the Second Level Deglitch-ing task to produce a mask over the glitches, which isthen applied back to the Level 0.5 products . Then asecond pass of the pipeline is executed identical to theoriginal Destriper map maker. Our final SPIRE maps were reduced in HIPE 14using the latest calibration version
SPIRECAL 14 2 released in December 2015. Below we summarizethe key data reduction steps, however a more detaileddescription on the photometer pipeline can be foundwithin Dowell et al. (2010).Our data processing begins with the Level 0 dataproducts downloaded from HSA, which are the rawdata formatted from satellite telemetry containing thereadout in ADU from each SPIRE bolometer. Afteran observation is loaded into HIPE, the first step isto execute the Common Engineering Conversion andformat it into Level 0.5 products. These products arethe uncalibrated and uncorrected timelines measuredin Volts, and contain all of the necessary informationto build science-grade maps.The first step in processing our data from Level 0.5to Level 1 is to join all the scan legs and turnaroundstogether. The turnaround occurs when the spacecraftturns around after a scan leg to begin another scan. Weopted to use the turnaround data to include as muchdata within our maps as possible. Next the pipelineproduces the pointing information for the observation,based on the positions of the SPIRE Beam SteeringMechanism as well as the offset between SPIRE andthe spacecraft itself (referred to as the Herschel Point-ing Product). This results in the SPIRE Pointing Prod-uct which is used later on in the pipeline. After calcu-lating the pointing information, the pipeline correctsfor any electrical crosstalk between the thermistor-bolometer channels. The thermistors measure the tem- The Level 0.5 products are the output after running the raw satellitetelemetry through the engineering pipeline. perature of the array bath as a function of time so thatlater we may accurately subtract the instrument ther-mal contribution, or temperature drift from the datatimelines.The next step is the signal jump detector, which de-tects and removes jumps in the thermistor timelinesthat would otherwise cause an incorrect temperaturedrift correction. To do this, the module subtracts base-lines and smoothed medians from the thermistor time-lines to identify any jumps. After deglitching the ther-mistor timelines, we must deglitch any cosmic ray hitson the bolometers themselves. This is an importantstep since any glitches that are not removed wouldmanifest itself as image artifacts on the final maps. Thepipeline does this in two steps, where the first step is toremove glitches that occur simultaneously in groups ofconnected bolometer detectors. This can occur whena cosmic ray hits the substrate of an entire photometerarray, and can leave an imprint of the array on the finalmap. The second step is to run the wavelet deglitcheron the timeline data, which uses a complex algorithmto remove glitches in Fourier space.After deglitching the detector timelines, a low passfilter response correction is applied to the TOD. This isto take into account the delay in the electronics with re-spect to the telescope position along a scan, in order toensure a match between the astrometric timeline fromthe telescope, and the detector timeline from the instru-ment. At this point we can apply the flux conversion tothe detector timelines, changing the units from Volts toJy beam − . The next step involves corrections to thetimelines due to temperature drifts, which are causedby variations of the detector array bath temperatures.First, with the coolerBurpCorrection flag setto true , the pipeline flags data that were affected bythe “cooler burp” effect. Observations taken duringthis effect, usually in the first ∼ Planck
High Frequency Instrument(HFI) for the PMW and PLW arrays (see § (cid:48)(cid:48) , 10 (cid:48)(cid:48) ,and 14 (cid:48)(cid:48) for the PSW, PMW, and PLW arrays respec-tively. For each instant of time on each bolometer’stimeline, the measured flux is added to the total signalmap and a value of 1 is added to the coverage map.Once this is done for all bolometer timelines, the total signal map is divided by the coverage map to obtainthe flux density map.Although the 2-pass pipeline does an excellent jobof removing all SPIRE image artifacts, approximatelytwenty of the maps still exhibited stripes and residualglitches in the final map. These maps were reprocessedby first using the SPIRE bolometer finder tool to iden-tify the misbehaving bolometer, and then masking theaffected portions in that bolometer’s Level 1 timeline.The data were then rerun through the Naive Mapper toproduce a clean and deglitched Level 2 science grademap.
5. The
Herschel -GOALS Image Atlas
In the following pages in Figure 3 we present theentire
Herschel atlas of the GOALS sample, orderedby ascending RA. The archived Herschel
GOALSmaps are in standard *.fits format with image unitsof Jy pixel − . Each page consists of six panels for the70 µ m, 100 µ m, 160 µ m, 250 µ m, 350 µ m, and 500 µ m channel maps.The IRAS name of each galaxy or galaxy system isshown at the top, along with their common names fromoptical catalogs. Each of the six panels are matchedand have the exact same map center as well as fieldof view. The center coordinates of the Herschel atlasimages are listed in Table 1. For galaxy systems withmultiple components, the center coordinate is chosento be roughly equidistant from all components. Thefield of view for each panel is shown on the bottom leftof the 70 µ m panel, and represents the physical lengthof one side of each panel. A scale bar also indicates thephysical length of 10 kpc at the distance of the galaxy(derived from the angular diameter distance in Table1), along with the equivalent angular distance. Thecircle on the bottom right of each panel represents thebeam size at that wavelength. Finally the right ascen-sion and declination coordinates are indicated in J2000sexagesimal as well as decimal format. The sexages-imal RA coordinates have the hour portion truncatedfor all but the center tick mark, to keep the tick namesizes manageable.Since many objects appear as point sources at someor all of the Herschel wavelengths, the morphologiesof these galaxies will be dominated by the PSF at thatwavelength. In the case of PACS, the PSF is char-acterized by a narrow circular core elongated in the http://irsa.ipac.caltech.edu/data/Herschel/GOALS z -direction, at 70 µ m and 100 µ m. In ad-dition there is a tri-lobe pattern at the several percentlevel at all three wavelengths, however it is strongestat 70 µ m. Finally, there are knotty structured diffrac-tion rings at the sub-percent level, again most apparentat 70 µ m and 100 µ m. In the case of SPIRE, the PSFappears mostly circular, however for the brightest ob-jects, airy rings are also visible.In order to show as much detail in these maps, weused an inverse hyperbolic sine (asinh) stretch functionto maximize the dynamic range of visible structures.Also to keep all the PACS images uniform, the back-ground for each image was adjusted such that the back-ground is very close to zero. The format in our Her-schel atlas matches that of companion image atlasesfrom
Hubble Space Telescope -ACS (Evans et al . Spitzer -IRAC/MIPS (Mazzarella et al . µ m to 500 µ m. 27 RAS F00073+2538 (NGC 23) D ec li n a t i o n
10 Kpc = 32.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +25:52:44.77+25:54:06.23+25:55:27.70+25:56:49.16+25:58:10.62 µ m µ m Right Ascension µ m µ m Fig. 3.—
The
Herschel
GOALS atlas, displaying imagery of local LIRGs and ULIRGs in the three PACS bands and three SPIRE band. An asinhtransfer function is used to maximize the dynamic range of visible structures, and a common field of view of approximately ∼ ×
100 kpc isused to facilitate comparisons across the sample and with images in the GOALS Spitzer atlas in Mazzarella et al . (2017). Scale bars indicate 10 kpcand the equivalent angular scale as derived from the angular diameter distance in Table 1. The beam sizes at each wavelength are indicated on thelower right of each panel. The atlas is ordered by increasing right ascension. RAS F00085−1223 (NGC 34/Mrk 938) D ec li n a t i o n
10 Kpc = 25.3"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −12:08:34.74−12:07:31.47−12:06:28.20−12:05:24.92−12:04:21.65 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 2 of 209). 29
RAS F00163−1039 (Arp 256) D ec li n a t i o n
10 Kpc = 18.5"FOV = 150 Kpc µ m µ m m s m s h m s m s m s −10:24:24.16−10:23:14.73−10:22:05.30−10:20:55.86−10:19:46.43 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 3 of 209). 30
RAS F00344−3349 (ESO 350−IG 038/Haro 11) D ec li n a t i o n
10 Kpc = 24.2"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −33:35:17.96−33:34:17.58−33:33:17.20−33:32:16.81−33:31:16.43 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 4 of 209). 31
RAS F00402−2349 (NGC 232) D ec li n a t i o n
10 Kpc = 22.6"FOV = 150 Kpc µ m µ m m s m s h m s m s m s −23:35:53.73−23:34:29.01−23:33:04.30−23:31:39.58−23:30:14.86 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 5 of 209). 32
RAS F00506+7248 (MCG+12−02−001) D ec li n a t i o n
10 Kpc = 30.5"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +73:02:33.56+73:03:49.73+73:05:05.90+73:06:22.06+73:07:38.23 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 6 of 209). 33
RAS F00548+4331 (NGC 317B) D ec li n a t i o n
10 Kpc = 27.8"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +43:45:28.51+43:46:38.10+43:47:47.70+43:48:57.29+43:50:06.88 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 7 of 209). 34
RAS F01053−1746 (IC 1623/Arp 236) D ec li n a t i o n
10 Kpc = 25.1"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −17:32:31.06−17:31:28.33−17:30:25.60−17:29:22.86−17:28:20.13 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 8 of 209). 35
RAS F01076−1707 (MCG−03−04−014) D ec li n a t i o n
10 Kpc = 15.3"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −16:52:26.40−16:51:48.15−16:51:09.90−16:50:31.64−16:49:53.39 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 9 of 209). 36
RAS F01159−4443 (ESO 244−G012) D ec li n a t i o n
10 Kpc = 23.5"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −44:29:49.49−44:28:50.69−44:27:51.90−44:26:53.10−44:25:54.30 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 10 of 209). 37
RAS F01173+1405 (CGCG 436−030) D ec li n a t i o n
10 Kpc = 25.1"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +14:19:36.83+14:20:39.56+14:21:42.30+14:22:45.03+14:23:47.76 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 11 of 209). 38
RAS F01325−3623 (ESO 353−G020) D ec li n a t i o n
10 Kpc = 25.1"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −36:10:19.86−36:09:17.13−36:08:14.40−36:07:11.66−36:06:08.93 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 12 of 209). 39
RAS F01341−3735 (RR 032) D ec li n a t i o n
10 Kpc = 28.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −37:22:15.13−37:21:03.51−37:19:51.90−37:18:40.28−37:17:28.66 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 13 of 209). 40
RAS F01364−1042 D ec li n a t i o n
10 Kpc = 10.8"FOV = 150 Kpc µ m µ m m s m s h m s m s m s −10:28:33.05−10:27:52.57−10:27:12.10−10:26:31.62−10:25:51.14 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 14 of 209). 41
RAS F01417+1651 (III Zw 035) D ec li n a t i o n
10 Kpc = 18.3"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +17:04:37.40+17:05:23.20+17:06:09.00+17:06:54.79+17:07:40.59 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 15 of 209). 42
RAS F01484+2220 (NGC 695) D ec li n a t i o n
10 Kpc = 15.8"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +22:33:36.91+22:34:16.45+22:34:56.00+22:35:35.54+22:36:15.08 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 16 of 209). 43
RAS F01519+3640 (UGC 01385) D ec li n a t i o n
10 Kpc = 26.8"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +36:52:53.78+36:54:00.84+36:55:07.90+36:56:14.95+36:57:22.01 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 17 of 209). 44
RAS F02071−1023 (NGC 838) D ec li n a t i o n
10 Kpc = 38.7"FOV = 130 Kpc µ m µ m m s m s h m s m s m s −10:13:42.24−10:11:36.47−10:09:30.70−10:07:24.92−10:05:19.15 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 18 of 209). 45
RAS F02070+3857 (NGC 828) D ec li n a t i o n
10 Kpc = 28.0"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +39:09:04.57+39:10:14.63+39:11:24.70+39:12:34.76+39:13:44.82 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 19 of 209). 46
RAS F02114+0456 (IC 214) D ec li n a t i o n
10 Kpc = 16.9"FOV = 175 Kpc µ m µ m m s m s h m s m s m s +05:07:46.34+05:09:00.07+05:10:13.80+05:11:27.52+05:12:41.25 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 20 of 209). 47
RAS F02152+1418 (NGC 877) D ec li n a t i o n
10 Kpc = 39.0"FOV = 75 Kpc µ m µ m m s m s h m s m s m s +14:29:31.98+14:30:45.09+14:31:58.20+14:33:11.30+14:34:24.41 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 21 of 209). 48
RAS F02203+3158 (MCG+05−06−036) D ec li n a t i o n
10 Kpc = 15.2"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +32:10:17.59+32:10:55.59+32:11:33.60+32:12:11.60+32:12:49.60 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 22 of 209). 49
RAS F02208+4744 (UGC 01845) D ec li n a t i o n
10 Kpc = 31.7"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +47:55:33.23+47:56:52.56+47:58:11.90+47:59:31.23+48:00:50.56 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 23 of 209). 50
RAS F02281−0309 (NGC 958) D ec li n a t i o n
10 Kpc = 26.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −02:58:33.40−02:57:26.95−02:56:20.50−02:55:14.04−02:54:07.59 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 24 of 209). 51
RAS F02345+2053 (NGC 992) D ec li n a t i o n
10 Kpc = 36.6"FOV = 50 Kpc µ m µ m m s m s h m s m s m s +21:04:31.37+21:05:17.08+21:06:02.80+21:06:48.51+21:07:34.22 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 25 of 209). 52
RAS F02401−0013 (NGC 1068) D ec li n a t i o n
10 Kpc = 131"FOV = 50 Kpc µ m µ m m s m s h m s m s m s −00:06:14.26−00:03:31.08−00:00:47.90+00:01:55.28+00:04:38.46 µ m µ m Right Ascension µ m Fig. 3.— Continued (page 26 of 209). 53
RAS F02435+1253 (UGC 02238) D ec li n a t i o n
10 Kpc = 23.3"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +13:03:48.06+13:04:46.33+13:05:44.60+13:06:42.86+13:07:41.13 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 27 of 209). 54
RAS F02437+2122 D ec li n a t i o n
10 Kpc = 21.9"FOV = 50 Kpc µ m µ m m s m s h m s m s m s +21:34:15.77+21:34:43.08+21:35:10.40+21:35:37.71+21:36:05.02 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 28 of 209). 55
RAS F02437+2122 (2MASX J02464505+2133234) D ec li n a t i o n
10 Kpc = 21.9"FOV = 50 Kpc µ m µ m m s m s h m s m s m s +21:32:28.87+21:32:56.18+21:33:23.50+21:33:50.81+21:34:18.12 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 29 of 209). 56
RAS F02512+1446 (UGC 02369) D ec li n a t i o n
10 Kpc = 16.2"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +14:57:05.23+14:57:45.61+14:58:26.00+14:59:06.38+14:59:46.76 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 30 of 209). 57
RAS F03117+4151 (UGC 02608) D ec li n a t i o n
10 Kpc = 21.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +42:00:20.60+42:01:14.60+42:02:08.60+42:03:02.59+42:03:56.59 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 31 of 209). 58
RAS F03117+4151 (UGC 02612) D ec li n a t i o n
10 Kpc = 21.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +41:57:02.00+41:57:56.00+41:58:50.00+41:59:43.99+42:00:37.99 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 32 of 209). 59
RAS F03164+4119 (NGC 1275) D ec li n a t i o n
10 Kpc = 28.5"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +41:28:19.55+41:29:30.77+41:30:42.00+41:31:53.22+41:33:04.44 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 33 of 209). 60
RAS F03217+4022 D ec li n a t i o n
10 Kpc = 21.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +40:31:44.20+40:32:38.20+40:33:32.20+40:34:26.19+40:35:20.19 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 34 of 209). 61
RAS F03316−3618 (NGC 1365) D ec li n a t i o n
10 Kpc = 117"FOV = 65 Kpc µ m µ m m s m s h m s m s m s −36:14:44.63−36:11:35.26−36:08:25.90−36:05:16.53−36:02:07.16 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 35 of 209). 62
RAS F03359+1523 D ec li n a t i o n
10 Kpc = 14.5"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +15:31:41.36+15:32:17.73+15:32:54.10+15:33:30.46+15:34:06.83 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 36 of 209). 63
RAS F03514+1546 (CGCG 465−012) D ec li n a t i o n
10 Kpc = 22.9"FOV = 75 Kpc µ m µ m m s m s h m s m s m s +15:54:17.55+15:55:00.47+15:55:43.40+15:56:26.32+15:57:09.24 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 37 of 209). 64
RAS F03514+1546 (CGCG 465−011) D ec li n a t i o n
10 Kpc = 22.9"FOV = 75 Kpc µ m µ m m s m s h m s m s m s +15:57:58.45+15:58:41.37+15:59:24.30+16:00:07.22+16:00:50.14 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 38 of 209). 65
RAS 03582+6012 D ec li n a t i o n
10 Kpc = 16.7"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +60:19:16.49+60:19:58.24+60:20:40.00+60:21:21.75+60:22:03.50 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 39 of 209). 66
RAS F04097+0525 (UGC 02982) D ec li n a t i o n
10 Kpc = 28.5"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +05:30:26.45+05:31:37.77+05:32:49.10+05:34:00.42+05:35:11.74 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 40 of 209). 67
RAS F04118−3207 (ESO 420−G013) D ec li n a t i o n
10 Kpc = 41.4"FOV = 50 Kpc µ m µ m m s m s h m s m s m s −32:02:08.84−32:01:17.07−32:00:25.30−31:59:33.52−31:58:41.75 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 41 of 209). 68
RAS F04191−1855 (ESO 550−IG 025) D ec li n a t i o n
10 Kpc = 15.9"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −18:50:07.73−18:49:28.06−18:48:48.40−18:48:08.73−18:47:29.06 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 42 of 209). 69
RAS F04210−4042 (NGC 1572) D ec li n a t i o n
10 Kpc = 24.2"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −40:38:04.28−40:37:03.69−40:36:03.10−40:35:02.50−40:34:01.91 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 43 of 209). 70
RAS 04271+3849 D ec li n a t i o n
10 Kpc = 26.5"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +38:53:35.23+38:54:41.51+38:55:47.80+38:56:54.08+38:58:00.36 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 44 of 209). 71
RAS F04315−0840 (NGC 1614) D ec li n a t i o n
10 Kpc = 31.4"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −08:37:23.57−08:36:05.08−08:34:46.60−08:33:28.11−08:32:09.62 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 45 of 209). 72
RAS F04326+1904 (UGC 03094) D ec li n a t i o n
10 Kpc = 20.4"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +19:08:35.78+19:09:26.89+19:10:18.00+19:11:09.10+19:12:00.21 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 46 of 209). 73
RAS F04454−4838 (ESO 203−IG001) D ec li n a t i o n
10 Kpc = 9.73"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −48:34:19.24−48:33:54.92−48:33:30.60−48:33:06.27−48:32:41.95 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 47 of 209). 74
RAS F04502−3304 (MCG−05−12−006) D ec li n a t i o n
10 Kpc = 26.3"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −33:01:37.71−33:00:31.85−32:59:26.00−32:58:20.14−32:57:14.28 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 48 of 209). 75
RAS F05053−0805 (NGC 1797) D ec li n a t i o n
10 Kpc = 33.5"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −08:03:56.12−08:02:32.41−08:01:08.70−07:59:44.98−07:58:21.27 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 49 of 209). 76
RAS F05053−0805 (NGC 1799) D ec li n a t i o n
10 Kpc = 33.5"FOV = 80 Kpc µ m µ m m s m s h m s m s m s −08:00:22.93−07:59:15.96−07:58:09.00−07:57:02.03−07:55:55.06 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 50 of 209). 77
RAS F05054+1718 (CGCG 468−002) D ec li n a t i o n
10 Kpc = 27.5"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +17:19:40.47+17:20:49.13+17:21:57.80+17:23:06.46+17:24:15.12 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 51 of 209). 78
RAS 05083+2441 D ec li n a t i o n
10 Kpc = 21.8"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +24:43:52.31+24:44:46.70+24:45:41.10+24:46:35.49+24:47:29.88 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 52 of 209). 79
RAS F05081+7936 (VII Zw 031) D ec li n a t i o n
10 Kpc = 9.54"FOV = 200 Kpc µ m µ m m s m s h m s m s m s +79:38:37.49+79:39:25.19+79:40:12.90+79:41:00.60+79:41:48.30 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 53 of 209). 80
RAS 05129+5128 D ec li n a t i o n
10 Kpc = 18.1"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +51:30:26.19+51:31:11.54+51:31:56.90+51:32:42.25+51:33:27.60 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 54 of 209). 81
RAS F05189−2524 D ec li n a t i o n
10 Kpc = 12.0"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −25:22:46.16−25:22:16.18−25:21:46.20−25:21:16.21−25:20:46.23 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 55 of 209). 82
RAS F05187−1017 D ec li n a t i o n
10 Kpc = 17.9"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −10:16:15.56−10:15:30.88−10:14:46.20−10:14:01.51−10:13:16.83 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 56 of 209). 83
RAS 05368+4940 (MCG+08−11−002) D ec li n a t i o n
10 Kpc = 25.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +49:39:33.64+49:40:37.62+49:41:41.60+49:42:45.57+49:43:49.55 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 57 of 209). 84
RAS F05365+6921 (NGC 1961) D ec li n a t i o n
10 Kpc = 35.9"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +69:19:43.43+69:21:13.11+69:22:42.80+69:24:12.48+69:25:42.16 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 58 of 209). 85
RAS F05414+5840 (UGC 03351) D ec li n a t i o n
10 Kpc = 32.3"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +58:39:22.20+58:40:42.90+58:42:03.60+58:43:24.29+58:44:44.99 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 59 of 209). 86
RAS 05442+1732 D ec li n a t i o n
10 Kpc = 26.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +17:31:15.85+17:32:22.47+17:33:29.10+17:34:35.72+17:35:42.34 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 60 of 209). 87
RAS F06076−2139 D ec li n a t i o n
10 Kpc = 13.5"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −21:41:35.57−21:41:01.93−21:40:28.30−21:39:54.66−21:39:21.02 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 61 of 209). 88
RAS F06052+8027 (UGC 03410) D ec li n a t i o n
10 Kpc = 36.3"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +80:24:45.84+80:26:16.47+80:27:47.10+80:29:17.72+80:30:48.35 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 62 of 209). 89
RAS F06107+7822 (NGC 2146) D ec li n a t i o n
10 Kpc = 119"FOV = 50 Kpc µ m µ m m s m s h m s m s m s +78:16:27.64+78:18:55.82+78:21:24.00+78:23:52.17+78:26:20.35 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 63 of 209). 90
RAS F06259−4708 (ESO 255−IG007) D ec li n a t i o n
10 Kpc = 12.9"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −47:11:53.73−47:11:21.56−47:10:49.40−47:10:17.23−47:09:45.06 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 64 of 209). 91
RAS F06295−1735 (ESO 557−G002) D ec li n a t i o n
10 Kpc = 23.0"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −17:39:55.93−17:38:58.31−17:38:00.70−17:37:03.08−17:36:05.46 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 65 of 209). 92
RAS F06538+4628 (UGC 03608) D ec li n a t i o n
10 Kpc = 22.8"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +46:22:16.51+46:23:13.55+46:24:10.60+46:25:07.64+46:26:04.68 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 66 of 209). 93
RAS F06592−6313 D ec li n a t i o n
10 Kpc = 20.8"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −63:19:36.15−63:18:44.27−63:17:52.40−63:17:00.52−63:16:08.64 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 67 of 209). 94
RAS F07027−6011 (AM 0702−601) D ec li n a t i o n
10 Kpc = 15.6"FOV = 150 Kpc µ m µ m m s m s h m s m s m s −60:17:59.36−60:17:01.03−60:16:02.70−60:15:04.36−60:14:06.03 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 68 of 209). 95
RAS 07063+2043 (NGC 2342) D ec li n a t i o n
10 Kpc = 27.5"FOV = 110 Kpc µ m µ m m s m s h m s m s m s +20:34:39.43+20:35:55.06+20:37:10.70+20:38:26.33+20:39:41.96 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 69 of 209). 96
RAS F07160−6215 (NGC 2369) D ec li n a t i o n
10 Kpc = 44.3"FOV = 70 Kpc µ m µ m m s m s h m s m s m s −62:23:11.31−62:21:53.85−62:20:36.40−62:19:18.94−62:18:01.48 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 70 of 209). 97
RAS 07251−0248 D ec li n a t i o n
10 Kpc = 6.10"FOV = 200 Kpc µ m µ m m s m s h m s m s m s −02:55:55.78−02:55:25.29−02:54:54.80−02:54:24.30−02:53:53.81 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 71 of 209). 98
RAS F07256+3355 (NGC 2388) D ec li n a t i o n
10 Kpc = 34.6"FOV = 220 Kpc µ m µ m m s m s h m s m s m s +33:44:02.84+33:47:12.87+33:50:22.90+33:53:32.92+33:56:42.95 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 72 of 209). 99
RAS F07329+1149 (MCG+02−20−003) D ec li n a t i o n
10 Kpc = 28.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +11:40:11.56+11:41:23.18+11:42:34.80+11:43:46.41+11:44:58.03 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 73 of 209). 100
RAS F07329+1149 (NGC 2416) D ec li n a t i o n
10 Kpc = 28.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +11:34:18.86+11:35:30.48+11:36:42.10+11:37:53.71+11:39:05.33 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 74 of 209). 101
RAS 08355−4944 D ec li n a t i o n
10 Kpc = 18.4"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −49:56:02.00−49:55:16.00−49:54:30.00−49:53:43.99−49:52:57.99 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 75 of 209). 102
RAS F08339+6517 D ec li n a t i o n
10 Kpc = 24.8"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +65:05:11.09+65:06:13.14+65:07:15.20+65:08:17.25+65:09:19.30 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 76 of 209). 103
RAS F08354+2555 (NGC 2623) D ec li n a t i o n
10 Kpc = 25.4"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +25:43:09.33+25:44:12.91+25:45:16.50+25:46:20.08+25:47:23.66 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 77 of 209). 104
RAS 08424−3130 (ESO 432−IG006) D ec li n a t i o n
10 Kpc = 28.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −31:44:03.54−31:42:52.02−31:41:40.50−31:40:28.97−31:39:17.45 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 78 of 209). 105
RAS F08520−6850 (ESO 060−IG016) D ec li n a t i o n
10 Kpc = 10.8"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −69:02:50.77−69:02:23.88−69:01:57.00−69:01:30.11−69:01:03.22 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 79 of 209). 106
RAS F08572+3915 D ec li n a t i o n
10 Kpc = 8.75"FOV = 200 Kpc µ m µ m m s m s h m s m s m s +39:02:26.48+39:03:10.24+39:03:54.00+39:04:37.75+39:05:21.51 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 80 of 209). 107
RAS 09022−3615 D ec li n a t i o n
10 Kpc = 8.54"FOV = 200 Kpc µ m µ m m s m s h m s m s m s −36:28:26.94−36:27:44.22−36:27:01.50−36:26:18.77−36:25:36.05 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 81 of 209). 108
RAS F09111−1007 D ec li n a t i o n
10 Kpc = 9.32"FOV = 200 Kpc µ m µ m m s m s h m s m s m s −10:20:57.76−10:20:11.18−10:19:24.60−10:18:38.01−10:17:51.43 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 82 of 209). 109
RAS F09126+4432 (UGC 04881) D ec li n a t i o n
10 Kpc = 12.5"FOV = 150 Kpc µ m µ m m s m s h m s m s m s +44:18:20.07+44:19:07.03+44:19:54.00+44:20:40.96+44:21:27.92 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 83 of 209). 110
RAS F09320+6134 (UGC 05101) D ec li n a t i o n
10 Kpc = 12.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +61:20:08.93+61:20:40.41+61:21:11.90+61:21:43.38+61:22:14.86 µ m µ m Right Ascension µ m Fig. 3.— Continued (page 84 of 209). 111
RAS F09333+4841 (MCG+08−18−013) D ec li n a t i o n
10 Kpc = 18.8"FOV = 150 Kpc µ m µ m m s m s h m s m s m s +48:25:57.90+48:27:08.35+48:28:18.80+48:29:29.24+48:30:39.69 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 85 of 209). 112
RAS F09437+0317 (Arp 303) D ec li n a t i o n
10 Kpc = 23.1"FOV = 150 Kpc µ m µ m m s m s h m s m s m s +03:00:37.16+03:02:03.78+03:03:30.40+03:04:57.01+03:06:23.63 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 86 of 209). 113
RAS F10015−0614 (NGC 3110) D ec li n a t i o n
10 Kpc = 27.4"FOV = 95 Kpc µ m µ m m s m s h m s m s m s −06:31:18.78−06:30:13.64−06:29:08.50−06:28:03.35−06:26:58.21 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 87 of 209). 114
RAS F10038−3338 (ESO 374−IG 032) D ec li n a t i o n
10 Kpc = 14.1"FOV = 130 Kpc µ m µ m m s m s h m s m s m s −33:54:37.99−33:53:52.04−33:53:06.10−33:52:20.15−33:51:34.20 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 88 of 209). 115
RAS F10173+0828 D ec li n a t i o n
10 Kpc = 10.1"FOV = 200 Kpc µ m µ m m s m s h m s m s m s +08:11:51.44+08:12:42.12+08:13:32.80+08:14:23.47+08:15:14.15 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 89 of 209). 116
RAS F10196+2149 (NGC 3221) D ec li n a t i o n
10 Kpc = 32.3"FOV = 80 Kpc µ m µ m m s m s h m s m s m s +21:32:01.48+21:33:06.04+21:34:10.60+21:35:15.15+21:36:19.71 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 90 of 209). 117
RAS F10257−4339 (NGC 3256) D ec li n a t i o n
10 Kpc = 54.0"FOV = 50 Kpc µ m µ m m s m s h m s m s m s −43:56:28.99−43:55:21.49−43:54:14.00−43:53:06.50−43:51:59.00 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 91 of 209). 118
RAS F10409−4556 (ESO 264−G036) D ec li n a t i o n
10 Kpc = 21.5"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −46:14:31.64−46:13:37.87−46:12:44.10−46:11:50.32−46:10:56.55 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 92 of 209). 119
RAS F10567−4310 (ESO 264−G057) D ec li n a t i o n
10 Kpc = 25.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −43:28:33.31−43:27:29.25−43:26:25.20−43:25:21.14−43:24:17.08 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 93 of 209). 120
RAS F10565+2448 D ec li n a t i o n
10 Kpc = 14.0"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +24:31:24.32+24:31:59.26+24:32:34.20+24:33:09.13+24:33:44.07 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 94 of 209). 121
RAS F11011+4107 (MCG+07−23−019) D ec li n a t i o n
10 Kpc = 14.0"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +40:49:50.52+40:50:25.46+40:51:00.40+40:51:35.33+40:52:10.27 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 95 of 209). 122
RAS F11186−0242 (CGCG 011−076) D ec li n a t i o n
10 Kpc = 18.7"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −03:00:54.13−03:00:07.46−02:59:20.80−02:58:34.13−02:57:47.46 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 96 of 209). 123
RAS F11231+1456 (IC 2810) D ec li n a t i o n
10 Kpc = 14.1"FOV = 200 Kpc µ m µ m m s m s h m s m s m s +14:37:59.92+14:39:10.56+14:40:21.20+14:41:31.83+14:42:42.47 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 97 of 209). 124
RAS F11255−4120 (ESO 319−G022) D ec li n a t i o n
10 Kpc = 26.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −41:39:04.94−41:37:58.32−41:36:51.70−41:35:45.07−41:34:38.45 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 98 of 209). 125
RAS F11257+5850 (NGC 3690) D ec li n a t i o n
10 Kpc = 41.5"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +58:30:15.79+58:31:59.54+58:33:43.30+58:35:27.05+58:37:10.80 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 99 of 209). 126
RAS F11506−3851 (ESO 320−G030) D ec li n a t i o n
10 Kpc = 51.2"FOV = 50 Kpc µ m µ m m s m s h m s m s m s −39:09:56.95−39:08:52.97−39:07:49.00−39:06:45.02−39:05:41.04 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 100 of 209). 127
RAS F12043−3140 (ESO 440−IG058) D ec li n a t i o n
10 Kpc = 19.3"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −31:58:29.18−31:57:40.99−31:56:52.80−31:56:04.60−31:55:16.41 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 101 of 209). 128
RAS F12112+0305 D ec li n a t i o n
10 Kpc = 6.99"FOV = 200 Kpc µ m µ m m s m s h m s m s m s +02:47:32.30+02:48:07.25+02:48:42.20+02:49:17.14+02:49:52.09 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 102 of 209). 129
RAS F12116+5448 (NGC 4194) D ec li n a t i o n
10 Kpc = 48.8"FOV = 50 Kpc µ m µ m m s m s h m s m s m s +54:29:33.59+54:30:34.54+54:31:35.50+54:32:36.45+54:33:37.40 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 103 of 209). 130
RAS F12115−4656 (ESO 267−G030) D ec li n a t i o n
10 Kpc = 22.2"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −47:15:33.39−47:14:37.94−47:13:42.50−47:12:47.05−47:11:51.60 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 104 of 209). 131
RAS F12115−4656 (ESO 267−G029) D ec li n a t i o n
10 Kpc = 22.2"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −47:18:16.29−47:17:20.84−47:16:25.40−47:15:29.95−47:14:34.50 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 105 of 209). 132
RAS 12116−5615 D ec li n a t i o n
10 Kpc = 17.0"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −56:33:57.72−56:33:15.21−56:32:32.70−56:31:50.18−56:31:07.67 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 106 of 209). 133
RAS F12224−0624 D ec li n a t i o n
10 Kpc = 17.4"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −06:42:18.98−06:41:35.54−06:40:52.10−06:40:08.65−06:39:25.21 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 107 of 209). 134
RAS F12243−0036 (NGC 4418) D ec li n a t i o n
10 Kpc = 56.8"FOV = 60 Kpc µ m µ m m s m s h m s m s m s −00:56:22.56−00:54:57.33−00:53:32.10−00:52:06.86−00:50:41.63 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 108 of 209). 135
RAS F12540+5708 (Mrk 231/UGC 08058) D ec li n a t i o n
10 Kpc = 11.7"FOV = 150 Kpc µ m µ m m s m s h m s m s m s +56:50:57.30+56:51:41.05+56:52:24.80+56:53:08.54+56:53:52.29 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 109 of 209). 136
RAS F12590+2934 (NGC 4922) D ec li n a t i o n
10 Kpc = 19.5"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +29:17:02.21+29:17:50.90+29:18:39.60+29:19:28.29+29:20:16.98 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 110 of 209). 137
RAS F12592+0436 (CGCG 043−099) D ec li n a t i o n
10 Kpc = 12.7"FOV = 150 Kpc µ m µ m m s m s h m s m s m s +04:18:25.65+04:19:13.22+04:20:00.80+04:20:48.37+04:21:35.94 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 111 of 209). 138
RAS F12596−1529 (MCG−02−33−098) D ec li n a t i o n
10 Kpc = 27.0"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −15:48:16.96−15:47:09.38−15:46:01.80−15:44:54.21−15:43:46.63 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 112 of 209). 139
RAS F13001−2339 (ESO 507−G070) D ec li n a t i o n
10 Kpc = 20.3"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −23:56:59.40−23:56:08.60−23:55:17.80−23:54:26.99−23:53:36.19 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 113 of 209). 140
RAS 13052−5711 D ec li n a t i o n
10 Kpc = 20.3"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −57:29:11.80−57:28:21.05−57:27:30.30−57:26:39.54−57:25:48.79 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 114 of 209). 141
RAS F13126+2453 (IC 0860) D ec li n a t i o n
10 Kpc = 37.1"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +24:34:02.11+24:35:34.85+24:37:07.60+24:38:40.34+24:40:13.08 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 115 of 209). 142
RAS 13120−5453 D ec li n a t i o n
10 Kpc = 15.2"FOV = 120 Kpc µ m µ m m s m s h m s m s m s −55:10:53.83−55:10:08.16−55:09:22.50−55:08:36.83−55:07:51.16 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 116 of 209). 143
RAS F13136+6223 (VV 250a) D ec li n a t i o n
10 Kpc = 15.5"FOV = 150 Kpc µ m µ m m s m s h m s m s m s +62:05:41.17+62:06:39.28+62:07:37.40+62:08:35.51+62:09:33.62 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 117 of 209). 144
RAS F13182+3424 (UGC 08387) D ec li n a t i o n
10 Kpc = 19.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +34:06:43.97+34:07:33.08+34:08:22.20+34:09:11.31+34:10:00.42 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 118 of 209). 145
RAS F13188+0036 (NGC 5104) D ec li n a t i o n
10 Kpc = 23.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +00:18:35.33+00:19:34.26+00:20:33.20+00:21:32.13+00:22:31.06 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 119 of 209). 146
RAS F13197−1627 (MCG−03−34−064) D ec li n a t i o n
10 Kpc = 25.9"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −16:45:15.92−16:44:11.06−16:43:06.20−16:42:01.33−16:40:56.47 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 120 of 209). 147
RAS F13229−2934 (NGC 5135) D ec li n a t i o n
10 Kpc = 34.8"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −29:52:54.31−29:51:27.35−29:50:00.40−29:48:33.44−29:47:06.48 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 121 of 209). 148
RAS 13242−5713 (ESO 173−G015) D ec li n a t i o n
10 Kpc = 61.9"FOV = 50 Kpc µ m µ m m s m s h m s m s m s −57:31:56.65−57:30:39.22−57:29:21.80−57:28:04.37−57:26:46.94 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 122 of 209). 149
RAS F13301−2356 (IC 4280) D ec li n a t i o n
10 Kpc = 25.8"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −24:14:34.73−24:13:30.11−24:12:25.50−24:11:20.88−24:10:16.26 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 123 of 209). 150
RAS F13362+4831 (NGC 5256) D ec li n a t i o n
10 Kpc = 16.9"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +48:15:12.73+48:15:54.96+48:16:37.20+48:17:19.43+48:18:01.66 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 124 of 209). 151
RAS F13373+0105 (Arp 240) D ec li n a t i o n
10 Kpc = 19.9"FOV = 150 Kpc µ m µ m m s m s h m s m s m s +00:47:40.46+00:48:54.98+00:50:09.50+00:51:24.01+00:52:38.53 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 125 of 209). 152
RAS F13428+5608 (Mrk 273/UGC 08696) D ec li n a t i o n
10 Kpc = 12.8"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +55:52:08.88+55:52:40.99+55:53:13.10+55:53:45.20+55:54:17.31 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 126 of 209). 153
RAS F13470+3530 (UGC 08739) D ec li n a t i o n
10 Kpc = 26.2"FOV = 90 Kpc µ m µ m m s m s h m s m s m s +35:13:28.25+35:14:27.22+35:15:26.20+35:16:25.17+35:17:24.14 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 127 of 209). 154
RAS F13478−4848 (ESO 221−IG010) D ec li n a t i o n
10 Kpc = 33.5"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −49:06:06.22−49:04:42.51−49:03:18.80−49:01:55.08−49:00:31.37 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 128 of 209). 155
RAS F13497+0220 (NGC 5331) D ec li n a t i o n
10 Kpc = 14.2"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +02:05:06.97+02:05:42.48+02:06:18.00+02:06:53.51+02:07:29.02 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 129 of 209). 156
RAS F13564+3741 (Arp 84) D ec li n a t i o n
10 Kpc = 36.0"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +37:23:20.51+37:24:50.50+37:26:20.50+37:27:50.49+37:29:20.48 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 130 of 209). 157
RAS F14179+4927 (CGCG 247−020) D ec li n a t i o n
10 Kpc = 18.1"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +49:12:41.51+49:13:26.70+49:14:11.90+49:14:57.09+49:15:42.28 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 131 of 209). 158
RAS F14280+3126 (NGC 5653) D ec li n a t i o n
10 Kpc = 35.1"FOV = 70 Kpc µ m µ m m s m s h m s m s m s +31:10:53.02+31:11:54.41+31:12:55.80+31:13:57.18+31:14:58.57 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 132 of 209). 159
RAS F14348−1447 D ec li n a t i o n
10 Kpc = 6.24"FOV = 300 Kpc µ m µ m m s m s h m s m s m s −15:01:57.87−15:01:11.03−15:00:24.20−14:59:37.36−14:58:50.52 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 133 of 209). 160
RAS F14378−3651 D ec li n a t i o n
10 Kpc = 7.46"FOV = 200 Kpc µ m µ m m s m s h m s m s m s −37:05:46.62−37:05:09.31−37:04:32.00−37:03:54.68−37:03:17.37 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 134 of 209). 161
RAS F14423−2039 (NGC 5734) D ec li n a t i o n
10 Kpc = 31.6"FOV = 110 Kpc µ m µ m m s m s h m s m s m s −20:56:24.89−20:54:57.89−20:53:30.90−20:52:03.90−20:50:36.90 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 135 of 209). 162
RAS F14547+2449 (VV 340a/Arp 302) D ec li n a t i o n
10 Kpc = 14.1"FOV = 155 Kpc µ m µ m m s m s h m s m s m s +24:34:56.08+24:35:50.64+24:36:45.20+24:37:39.75+24:38:34.31 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 136 of 209). 163
RAS F14544−4255 (IC 4518A/B) D ec li n a t i o n
10 Kpc = 26.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −43:10:09.37−43:09:02.83−43:07:56.30−43:06:49.76−43:05:43.22 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 137 of 209). 164
RAS F15107+0724 (CGCG 049−057) D ec li n a t i o n
10 Kpc = 32.4"FOV = 80 Kpc µ m µ m m s m s h m s m s m s +07:11:22.57+07:12:27.33+07:13:32.10+07:14:36.86+07:15:41.62 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 138 of 209). 165
RAS F15163+4255 (VV 705) D ec li n a t i o n
10 Kpc = 12.2"FOV = 200 Kpc µ m µ m m s m s h m s m s m s +42:42:39.59+42:43:40.54+42:44:41.50+42:45:42.45+42:46:43.40 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 139 of 209). 166
RAS 15206−6256 (ESO 099−G004) D ec li n a t i o n
10 Kpc = 16.0"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −63:08:49.16−63:08:09.28−63:07:29.40−63:06:49.51−63:06:09.63 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 140 of 209). 167
RAS F15250+3608 D ec li n a t i o n
10 Kpc = 9.04"FOV = 150 Kpc µ m µ m m s m s h m s m s m s +35:57:29.97+35:58:03.88+35:58:37.80+35:59:11.71+35:59:45.62 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 141 of 209). 168
RAS F15276+1309 (NGC 5936) D ec li n a t i o n
10 Kpc = 31.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +12:56:44.16+12:58:03.13+12:59:22.10+13:00:41.06+13:02:00.03 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 142 of 209). 169
RAS F15327+2340 (Arp 220/UGC 09913) D ec li n a t i o n
10 Kpc = 24.3"FOV = 140 Kpc µ m µ m m s m s h m s m s m s +23:27:21.03+23:28:46.16+23:30:11.30+23:31:36.43+23:33:01.56 µ m µ m Right Ascension µ m Fig. 3.— Continued (page 143 of 209). 170
RAS F15437+0234 (NGC 5990) D ec li n a t i o n
10 Kpc = 32.8"FOV = 80 Kpc µ m µ m m s m s h m s m s m s +02:22:44.22+02:23:49.91+02:24:55.60+02:26:01.28+02:27:06.97 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 144 of 209). 171
RAS F16030+2040 (NGC 6052) D ec li n a t i o n
10 Kpc = 27.4"FOV = 90 Kpc µ m µ m m s m s h m s m s m s +20:30:29.57+20:31:31.28+20:32:33.00+20:33:34.71+20:34:36.42 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 145 of 209). 172
RAS F16104+5235 (NGC 6090) D ec li n a t i o n
10 Kpc = 16.0"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +52:26:07.37+52:26:47.28+52:27:27.20+52:28:07.11+52:28:47.02 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 146 of 209). 173
RAS F16164−0746 D ec li n a t i o n
10 Kpc = 17.0"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −07:55:28.02−07:54:45.51−07:54:03.00−07:53:20.48−07:52:37.97 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 147 of 209). 174
RAS F16284+0411 (CGCG 052−037) D ec li n a t i o n
10 Kpc = 18.3"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +04:03:09.87+04:03:55.58+04:04:41.30+04:05:27.01+04:06:12.72 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 148 of 209). 175
RAS 16304−6030 (NGC 6156) D ec li n a t i o n
10 Kpc = 43.9"FOV = 75 Kpc µ m µ m m s m s h m s m s m s −60:39:52.57−60:38:30.28−60:37:08.00−60:35:45.71−60:34:23.42 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 149 of 209). 176
RAS F16330−6820 (ESO 069−IG006) D ec li n a t i o n
10 Kpc = 10.7"FOV = 200 Kpc µ m µ m m s m s h m s m s m s −68:28:28.84−68:27:35.57−68:26:42.30−68:25:49.02−68:24:55.75 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 150 of 209). 177
RAS F16399−0937 D ec li n a t i o n
10 Kpc = 17.0"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −09:44:38.65−09:43:56.17−09:43:13.70−09:42:31.22−09:41:48.74 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 151 of 209). 178
RAS F16443−2915 (ESO 453−G005) D ec li n a t i o n
10 Kpc = 21.4"FOV = 140 Kpc µ m µ m m s m s h m s m s m s −29:22:43.97−29:21:29.08−29:20:14.20−29:18:59.31−29:17:44.42 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 152 of 209). 179
RAS F16504+0228 (NGC 6240) D ec li n a t i o n
10 Kpc = 18.7"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +02:22:29.96+02:23:16.63+02:24:03.30+02:24:49.96+02:25:36.63 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 153 of 209). 180
RAS F16516−0948 D ec li n a t i o n
10 Kpc = 20.2"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −09:55:01.71−09:54:11.30−09:53:20.90−09:52:30.49−09:51:40.08 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 154 of 209). 181
RAS F16577+5900 (Arp 293) D ec li n a t i o n
10 Kpc = 24.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +58:54:44.57+58:55:46.03+58:56:47.50+58:57:48.96+58:58:50.42 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 155 of 209). 182
RAS F17132+5313 D ec li n a t i o n
10 Kpc = 9.82"FOV = 200 Kpc µ m µ m m s m s h m s m s m s +53:08:53.42+53:09:42.51+53:10:31.60+53:11:20.68+53:12:09.77 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 156 of 209). 183
RAS F17138−1017 D ec li n a t i o n
10 Kpc = 25.4"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −10:22:47.51−10:21:44.00−10:20:40.50−10:19:36.99−10:18:33.48 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 157 of 209). 184
RAS F17207−0014 D ec li n a t i o n
10 Kpc = 11.3"FOV = 175 Kpc µ m µ m m s m s h m s m s m s −00:18:39.81−00:17:50.25−00:17:00.70−00:16:11.14−00:15:21.58 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 158 of 209). 185
RAS F17222−5953 (ESO 138−G027) D ec li n a t i o n
10 Kpc = 21.9"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −59:57:44.56−59:56:49.88−59:55:55.20−59:55:00.51−59:54:05.83 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 159 of 209). 186
RAS F17530+3447 (UGC 11041) D ec li n a t i o n
10 Kpc = 27.5"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +34:44:16.69+34:45:25.44+34:46:34.20+34:47:42.95+34:48:51.70 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 160 of 209). 187
RAS F17548+2401 (CGCG 141−034) D ec li n a t i o n
10 Kpc = 23.0"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +23:59:07.15+24:00:04.57+24:01:02.00+24:01:59.42+24:02:56.84 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 161 of 209). 188
RAS 17578−0400 D ec li n a t i o n
10 Kpc = 30.8"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −04:03:50.22−04:02:33.26−04:01:16.30−03:59:59.33−03:58:42.37 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 162 of 209). 189
RAS 18090+0130 D ec li n a t i o n
10 Kpc = 16.3"FOV = 125 Kpc µ m µ m m s m s h m s m s m s +01:29:59.47+01:30:50.38+01:31:41.30+01:32:32.21+01:33:23.12 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 163 of 209). 190
RAS F18131+6820 (NGC 6621) D ec li n a t i o n
10 Kpc = 22.3"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +68:19:47.08+68:20:42.89+68:21:38.70+68:22:34.50+68:23:30.31 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 164 of 209). 191
RAS F18093−5744 (IC 4687) D ec li n a t i o n
10 Kpc = 26.9"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −57:46:15.36−57:45:08.13−57:44:00.90−57:42:53.66−57:41:46.43 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 165 of 209). 192
RAS F18145+2205 (CGCG 142−034) D ec li n a t i o n
10 Kpc = 24.8"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +22:04:38.64+22:05:40.62+22:06:42.60+22:07:44.57+22:08:46.55 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 166 of 209). 193
RAS F18293−3413 D ec li n a t i o n
10 Kpc = 24.9"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −34:13:31.25−34:12:29.12−34:11:27.00−34:10:24.87−34:09:22.74 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 167 of 209). 194
RAS F18329+5950 (NGC 6670A/B) D ec li n a t i o n
10 Kpc = 16.9"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +59:51:56.04+59:52:38.17+59:53:20.30+59:54:02.42+59:54:44.55 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 168 of 209). 195
RAS F18341−5732 (IC 4734) D ec li n a t i o n
10 Kpc = 29.0"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −57:31:50.24−57:30:37.82−57:29:25.40−57:28:12.97−57:27:00.55 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 169 of 209). 196
RAS F18425+6036 (NGC 6701) D ec li n a t i o n
10 Kpc = 33.9"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +60:36:21.97+60:37:46.78+60:39:11.60+60:40:36.41+60:42:01.22 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 170 of 209). 197
RAS F19120+7320 (VV 414/NGC 6786/UGC 11415) D ec li n a t i o n
10 Kpc = 19.2"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +73:23:28.26+73:24:16.23+73:25:04.20+73:25:52.16+73:26:40.13 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 171 of 209). 198
RAS F19115−2124 (ESO 593−IG008) D ec li n a t i o n
10 Kpc = 10.2"FOV = 150 Kpc µ m µ m m s m s h m s m s m s −21:20:22.95−21:19:44.62−21:19:06.30−21:18:27.97−21:17:49.64 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 172 of 209). 199
RAS F19297−0406 D ec li n a t i o n
10 Kpc = 6.16"FOV = 200 Kpc µ m µ m m s m s h m s m s m s −04:01:02.65−04:00:31.87−04:00:01.10−03:59:30.32−03:58:59.54 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 173 of 209). 200
RAS 19542+1110 D ec li n a t i o n
10 Kpc = 7.93"FOV = 200 Kpc µ m µ m m s m s h m s m s m s +11:17:45.59+11:18:25.24+11:19:04.90+11:19:44.55+11:20:24.20 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 174 of 209). 201
RAS F19542−3804 (ESO 339−G011) D ec li n a t i o n
10 Kpc = 24.2"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −37:58:09.30−37:57:08.85−37:56:08.40−37:55:07.94−37:54:07.49 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 175 of 209). 202
RAS F20221−2458 (NGC 6907) D ec li n a t i o n
10 Kpc = 42.0"FOV = 60 Kpc µ m µ m m s m s h m s m s m s −24:50:38.92−24:49:35.91−24:48:32.90−24:47:29.88−24:46:26.87 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 176 of 209). 203
RAS 20264+2533 (MCG+04−48−002) D ec li n a t i o n
10 Kpc = 32.4"FOV = 75 Kpc µ m µ m m s m s h m s m s m s +25:41:40.68+25:42:41.49+25:43:42.30+25:44:43.10+25:45:43.91 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 177 of 209). 204
RAS F20304−0211 (NGC 6926) D ec li n a t i o n
10 Kpc = 24.1"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −02:03:39.24−02:02:39.07−02:01:38.90−02:00:38.72−01:59:38.55 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 178 of 209). 205
RAS 20351+2521 D ec li n a t i o n
10 Kpc = 14.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +25:30:24.51+25:31:01.00+25:31:37.50+25:32:13.99+25:32:50.48 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 179 of 209). 206
RAS F20550+1655 (CGCG 448−020/II Zw 096) D ec li n a t i o n
10 Kpc = 13.8"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +17:06:32.84+17:07:07.22+17:07:41.60+17:08:15.97+17:08:50.35 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 180 of 209). 207
RAS F20551−4250 (ESO 286−IG019) D ec li n a t i o n
10 Kpc = 11.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −42:39:58.63−42:39:29.56−42:39:00.50−42:38:31.43−42:38:02.36 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 181 of 209). 208
RAS F21008−4347 (ESO 286−G035) D ec li n a t i o n
10 Kpc = 27.0"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −43:37:51.09−43:36:43.59−43:35:36.10−43:34:28.60−43:33:21.10 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 182 of 209). 209
RAS 21101+5810 D ec li n a t i o n
10 Kpc = 12.8"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +58:22:03.92+58:22:35.91+58:23:07.90+58:23:39.88+58:24:11.87 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 183 of 209). 210
RAS F21330−3846 (ESO 343−IG013) D ec li n a t i o n
10 Kpc = 25.0"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −38:34:42.65−38:33:40.22−38:32:37.80−38:31:35.37−38:30:32.94 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 184 of 209). 211
RAS F21453−3511 (NGC 7130) D ec li n a t i o n
10 Kpc = 29.3"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −34:59:31.19−34:58:17.94−34:57:04.70−34:55:51.45−34:54:38.20 µ m µ m Right Ascension µ m Fig. 3.— Continued (page 185 of 209). 212
RAS F22118−2742 (ESO 467−G027) D ec li n a t i o n
10 Kpc = 27.6"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −27:30:08.36−27:28:59.33−27:27:50.30−27:26:41.26−27:25:32.23 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 186 of 209). 213
RAS F22132−3705 (IC 5179) D ec li n a t i o n
10 Kpc = 41.1"FOV = 50 Kpc µ m µ m m s m s h m s m s m s −36:52:19.92−36:51:28.56−36:50:37.20−36:49:45.83−36:48:54.47 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 187 of 209). 214
RAS F22287−1917 (ESO 602−G025) D ec li n a t i o n
10 Kpc = 19.7"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −19:03:42.50−19:02:53.25−19:02:04.00−19:01:14.74−19:00:25.49 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 188 of 209). 215
RAS F22389+3359 (UGC 12150) D ec li n a t i o n
10 Kpc = 23.0"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +34:13:01.69+34:13:59.24+34:14:56.80+34:15:54.35+34:16:51.90 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 189 of 209). 216
RAS F22467−4906 (ESO 239−IG002) D ec li n a t i o n
10 Kpc = 11.7"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −48:51:57.03−48:51:27.66−48:50:58.30−48:50:28.93−48:49:59.56 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 190 of 209). 217
RAS F22491−1808 D ec li n a t i o n
10 Kpc = 6.83"FOV = 200 Kpc µ m µ m m s m s h m s m s m s −17:53:33.15−17:52:59.02−17:52:24.90−17:51:50.77−17:51:16.64 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 191 of 209). 218
RAS F23007+0836 (NGC 7469/IC 5283/Arp 298) D ec li n a t i o n
10 Kpc = 30.3"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +08:50:29.23+08:51:45.06+08:53:00.90+08:54:16.73+08:55:32.56 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 192 of 209). 219
RAS F23024+1916 (CGCG 453−062) D ec li n a t i o n
10 Kpc = 19.9"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +19:31:27.64+19:32:17.37+19:33:07.10+19:33:56.82+19:34:46.55 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 193 of 209). 220
RAS F23128−5919 (ESO 148−IG002) D ec li n a t i o n
10 Kpc = 11.3"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −59:04:12.34−59:03:44.07−59:03:15.80−59:02:47.52−59:02:19.25 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 194 of 209). 221
RAS F23135+2517 (IC 5298) D ec li n a t i o n
10 Kpc = 18.3"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +25:31:52.78+25:32:38.54+25:33:24.30+25:34:10.05+25:34:55.81 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 195 of 209). 222
RAS F23133−4251 (NGC 7552) D ec li n a t i o n
10 Kpc = 88.9"FOV = 50 Kpc µ m µ m m s m s h m s m s m s −42:38:47.76−42:36:56.63−42:35:05.50−42:33:14.36−42:31:23.23 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 196 of 209). 223
RAS F23157+0618 (NGC 7591) D ec li n a t i o n
10 Kpc = 29.9"FOV = 90 Kpc µ m µ m m s m s h m s m s m s +06:32:03.47+06:33:10.63+06:34:17.80+06:35:24.96+06:36:32.12 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 197 of 209). 224
RAS F23157−0441 (NGC 7592) D ec li n a t i o n
10 Kpc = 20.4"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −04:26:39.51−04:25:48.45−04:24:57.40−04:24:06.34−04:23:15.28 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 198 of 209). 225
RAS F23180−6929 (ESO 077−IG014) D ec li n a t i o n
10 Kpc = 12.0"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −69:13:54.23−69:13:24.16−69:12:54.10−69:12:24.03−69:11:53.96 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 199 of 209). 226
RAS F23254+0830 (NGC 7674) D ec li n a t i o n
10 Kpc = 17.3"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +08:45:24.62+08:46:07.81+08:46:51.00+08:47:34.18+08:48:17.37 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 200 of 209). 227
RAS 23262+0314 (NGC 7679) D ec li n a t i o n
10 Kpc = 28.9"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +03:28:16.75+03:29:29.07+03:30:41.40+03:31:53.72+03:33:06.04 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 201 of 209). 228
RAS 23262+0314 (NGC 7682) D ec li n a t i o n
10 Kpc = 28.9"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +03:29:35.25+03:30:47.57+03:31:59.90+03:33:12.22+03:34:24.54 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 202 of 209). 229
RAS F23365+3604 D ec li n a t i o n
10 Kpc = 8.14"FOV = 200 Kpc µ m µ m m s m s h m s m s m s +36:19:46.76+36:20:27.48+36:21:08.20+36:21:48.91+36:22:29.63 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 203 of 209). 230
RAS F23394−0353 (MCG−01−60−022) D ec li n a t i o n
10 Kpc = 22.3"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −03:38:46.01−03:37:50.20−03:36:54.40−03:35:58.59−03:35:02.78 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 204 of 209). 231
RAS F23394−0353 (MCG−01−60−021) D ec li n a t i o n
10 Kpc = 22.3"FOV = 100 Kpc µ m µ m m s m s h m s m s m s −03:41:33.91−03:40:38.10−03:39:42.30−03:38:46.49−03:37:50.68 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 205 of 209). 232
RAS 23436+5257 D ec li n a t i o n
10 Kpc = 14.8"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +53:12:47.66+53:13:24.68+53:14:01.70+53:14:38.71+53:15:15.73 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 206 of 209). 233
RAS F23444+2911 (Arp 86) D ec li n a t i o n
10 Kpc = 29.0"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +29:25:51.14+29:27:03.67+29:28:16.20+29:29:28.72+29:30:41.25 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 207 of 209). 234
RAS F23488+1949 (NGC 7771) D ec li n a t i o n
10 Kpc = 35.3"FOV = 200 Kpc µ m µ m m s m s h m s m s m s +20:01:48.61+20:04:44.90+20:07:41.20+20:10:37.49+20:13:33.78 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 208 of 209). 235
RAS F23488+2018 (Mrk 331) D ec li n a t i o n
10 Kpc = 27.9"FOV = 100 Kpc µ m µ m m s m s h m s m s m s +20:32:35.65+20:33:45.52+20:34:55.40+20:36:05.27+20:37:15.14 µ m µ m Right Ascension µ m µ m Fig. 3.— Continued (page 209 of 209). 236 . Herschel -GOALS Aperture Photometry
In this section we discuss the manner in which thebroadband photometry were determined for our sam-ple. Both PACS and SPIRE photometry were obtainedusing the annularSkyAperturePhotometry routine found in HIPE. At first we attempted to mea-sure fluxes by using an automated routine to determinethe appropriate circular aperture sizes for each galaxy,based on data from the MIPS instrument on
Spitzer .Unfortunately this approach does not work well for oursample, due to the extended nature of some GOALSsystems and galaxies.Instead we concluded that the best approach was todetermine apertures by visual inspection, and subse-quently check that we included all of the flux by plot-ting a curve of growth. We found that after subtract-ing any offset in the background levels, the curve ofgrowth almost always flattens out at large radii, indi-cating a background flux contribution of zero. Thereare only a few small cases in the PACS data where thecurve of growth does not flatten out, and in all casesthis occurs when the object is very faint ( F λ (cid:46) . Jy)and the background noise is more dominant. Curveof growth plots for the SPIRE data are also flat atlarge radii even for faint fluxes, again indicating ro-bust background subtractions. In Figure 4 we show aset of representative curve-of-growth plots and aper-tures for IRAS F09111–1007 at different wavelengths.The photometry aperture is represented by the bluecircle in the image and the blue line in the curve ofgrowth plot below it. In order to facilitate compari-son of matched aperture fluxes, all PACS aperture sizesare identical, while all SPIRE apertures are also iden-tical, but larger than that of PACS. The aperture ra-dius is typically set by the band with the largest beamsize in which we can make a measurement for eachinstrument, which is usually the 160 µ m channel forPACS and the 500 µ m channel for SPIRE. We foundthat aperture radii encompassing approximately 95%of the total light gave the best tradeoff between includ-ing all of the flux but at the same time keeping thebackground error from getting too high. Although itis possible to use the same aperture size across all sixbands (i. e. the SPIRE aperture size), the larger SPIREaperture would encompass a significant amount of skybackground for the higher resolution images (i. e. at 70 µ m) and would introduce additional noise in our mea-surements. We therefore decided it was best to matchthe apertures for each instrument. To accurately measure the flux of each galaxy thesky background must be subtracted from the measuredflux. To do this we estimate the sky background in theannulus represented by the red circles in the image,which corresponds to the two red lines in the curveof growth plot. These background annuli were cho-sen to be as free from any source emission as possible.Within the annularSkyAperturePhotometry routine we used the sky estimation algorithm from DAOPhot to estimate the sky level, with the “frac-tional pixel” setting enabled. The background cor-rected flux density is then the total flux minus the prod-uct of the measured background level and the numberof pixels within the target aperture.We note that in some cases both component and to-tal fluxes are measured for close pairs. These galaxiescan be easily resolved and separated at shorter wave-lengths, but become unresolved at longer wavelengths.In order to choose the best flux aperture, we care-fully selected the radius at which the curve of growthwas flattest. This is apparent in Figure 4 in the firsttwo columns where the galaxy pair is easily resolvedat 70 µ m, but becomes marginally resolved at 160 µ m. The third column in Figure 4 shows the curveof growth from a single large aperture encompassingthe entire system, which includes faint extended fluxmissed by the individual component apertures. Fi-nally since the galaxy pair is unresolved in the 350 µ m and 500 µ m SPIRE bands, we do not measure anycomponent fluxes at those wavelengths. At 250 µ m,component fluxes are still computed since they pair isstill resolved. Every effort was made to measure asmany marginally resolved systems as possible, whilealso providing a total flux measurement from one largeaperture when necessary. We believe separately mea-suring component and total fluxes in cases such as thiswill be useful when the fractional flux contribution ofeach component is desired.In Table 3 we present the table of monochromatictotal flux density for each GOALS system in units ofJansky. Depending on the number of galaxies withina system, their apparent separation on the sky, and thebeam size at that particular wavelength, the total Her-schel flux for each system is calculated using one ofthree methods. In the simple case of single galaxy,the system flux is just the flux of that galaxy. In caseswhere there are two or more galaxies that are widelyseparated, the total flux is the sum of the component Adapted from the IDL AstroLib mmm.pro routine.
IRAS
Faint Source Catalog, and galaxies with no“F” prefix are from the Point Source Catalog. Col-umn (3) lists common optical counterpart names to thegalaxy systems. Columns (4) – (6) are the total fluxesfrom the PACS instrument in units of Jy. Note thatthe four galaxies which lack µ m measurements areIRAS F02401-0013 (NGC 1068), IRAS F09320+6134(UGC 05101), IRAS F15327+2340 (Arp 220), andIRAS F21453-3511 (NGC 7130). Columns (7) – (9)are the total fluxes from the SPIRE instrument in unitsof Jy.In Table 4 we present the table of monochromaticflux density in units of Jansky for each componentmeasurable within each system, with the total systemflux from Table 3 included for completeness on thelast line for each system. For total fluxes that do nothave an aperture size listed, the totals were calculatedas the sum of the components. Likewise the RA anddeclination for these systems (on the totals line) rep-resent the geometric midpoint between the companiongalaxies. The column descriptions are (1) the row ref-erence number, which corresponds to the same indicesused in Tables 1–3. Column (2) is the IRAS name ofthe galaxy, ordered by ascending RA. Column (3) isthe individual name to that galaxy component. Notethat galaxies prefixed by IRGP are from the catalogof newly defined infrared galaxy pairs defined in thecompanion Spitzer -GOALS paper by Mazzarella et al . (2017). Columns (4) – (5) are the coordinates of theaperture centers used. Lines where coordinates arelisted but have no aperture radii are cases where thetotal flux is the sum of two widely separated compo-nents. These are the same 8 µ m coordinates adopted in Mazzarella et al . (2017), however a few were slightlyadjusted for the Herschel data. Columns (6) – (7) arethe aperture radii used for PACS photometry, in arc-sec and kpc respectively. Columns (8) – (10) are thefluxes from the PACS instrument in units of Jy. Galaxycomponents that do not have flux measurements aretoo close to a companion galaxy to be resolved byPACS. Columns (11) – (12) are the aperture radii usedfor SPIRE photometry, in arcsec and kpc respectively.Finally columns (13) – (15) are the fluxes from theSPIRE instrument in units of Jy. Galaxy componentsthat do not have flux measurements are too close to acompanion galaxy to be resolved by SPIRE.
In addition to measuring the flux, we must applyan aperture correction to account for flux outside ofthe aperture. The PACS aperture corrections are deter-mined from observations of bright celestial standards,and the correction factors are included in the PACS cal-ibration files distributed from the HSA. Within HIPE,the photApertureCorrectionPointSource task performs the aperture correction, where the in-put is the output product from the aperture photom-etry task. In addition a responsivity version must bespecified, which for our data we used the most recentversion (FM 7 ). Since these aperture corrections areonly applicable to point sources at each wavelength,we only apply the aperture correction to point sourceswithin our sample. To identify the point sources, weperformed PSF fitting of each source in our sample,and selected the objects with FWHM consistent withthe corresponding point source FWHM in each PACSband. In Table 4 we denote the fluxes in which anaperture correction was applied by the superscript c.Typical (average) aperture correction values for the70, 100, and 160 µ m bands are 11.7%, 12.8%, and15.5% of the uncorrected flux, respectively. The me-dian values of the aperture correction values are lessthan a percent away from the averages. We do not flagaperture-corrected fluxes in Table 3 since many of thetotal fluxes are a combination of aperture-correctedand uncorrected fluxes.We also experimented with applying these correc-tions to marginally resolved systems and systems with For a description, see section 2.3 ofthe PACS calibration framework document:http://herschel.esac.esa.int/twiki/pub/Pacs/PacsCalibration/The PACS Calibration Framework - issue 0.13.pdf
238 point source and extended flux, however we foundthat the aperture corrections artificially boosted theflux by approximately 6% on average. This is becausemany of our objects have varying levels of flux contri-bution from the point source and extended component.Furthermore, the PACS team performed a careful sur-face brightness comparison of PACS data with thatof IRAS and
Spitzer
MIPS data on the same fields. Byconvolving, converting, and re-gridding the higher res-olution PACS 70 µ m to that of IRAS µ m and MIPS70 µ m, and the PACS 100 µ m maps to that of IRAS µ m it was shown that there is no need to apply anypixel-to-pixel gain corrections to the PACS data. Theyalso conclude that their point-source based calibrationscheme is applicable in the case for extended sources.A similar conclusion is reached for the PACS red ar-ray . Mel´endez et al. (2014) also found in their Her-schel
PACS observations of the
Swift
BAT sample thataperture corrections on extended sources were negligi-ble (less than 3%). Therefore we leave sources appear-ing extended or semi-extended in our sample unalteredby any aperture correction.The absolute flux calibration of PACS uses mod-els of five different late type standard stars with fluxesranging between 0.6–15 Jy in the three photometricbands (Balog et al. 2014). In addition, ten differentasteroids are also used to establish the flux calibrationover the range of 0.1–300 Jy (M¨uller et al. 2014). Forthe standard stars, the absolute flux accuracy is within3% at 70 µ m and 100 µ m, and within 5% at 160 µ m.In addition, Uranus and Neptune were also observedfor validation purposes with fluxes of up to severalhundred Jy, however a 10% reduction due to nonlin-earity in the detector response was observed. Takenaltogether, the error in flux calibration is consistentto within 5% of the measured flux and takes into ac-count flat-fielding, responsivity correction which in-cludes the conversion of engineering units from voltsto Jy pixel − , and gain drift correction which correctsfor small drifts in gain with time (PACS Observer’sManual, and references therein). Since PACS did notperform absolute measurements over the course of themission, the fluxes are only measured relative to thezero level calculated by the mappers which is arbitrary.In addition to the flux calibration uncertainty, wemust also take into account the error from the back- For more details see the
Herschel technical note PICC-NHSC-TN-029. See technical note PICC-NHSC-TR-034. ground subtraction as well as the instrumental error.The error from the background subtraction is calcu-lated in the following manner: first using the HIPE im-plementation of
DAOPhot the 1- σ dispersion is calcu-lated from all the pixels within the background annulussurrounding the target aperture. This is then multipliedby the square root of the total number of pixels withinphotometry aperture, under the assumption that the er-ror in background subtraction of individual pixels arenot correlated. On the other hand the instrumental er-ror is calculated as the quadrature sum of all error pix-els within the target aperture, using the error maps pro-duced by the mapmaker. The total flux uncertainty isthen calculated as the quadrature sum of all three errorcomponents.We note that only two of the three galaxies in IRASF07256+3355 (NGC 2388) were observed by PACSdue to the smaller field of view, while SPIRE observedall three. Consequently the total fluxes in Table 3 forthis system is the sum of only the two galaxies ob-served by both instruments, however SPIRE photom-etry of the third galaxy to the west is provided in thecomponent flux table (Table 4). The same is also truefor IRAS F23488+1949, with the third galaxy to theNNW of the closer pair. 239ig. 4.— Twelve curve of growth plots for IRAS F09111–1007, which are representative for the entire GOALSsample. The blue circle in each image is the photometry aperture, while the red circles are the annuli from which thebackground is measured. These circles are represented in the curve of growth plot immediately below each image.The first column shows the PACS 70 µ m, 100 µ m, and 160 µ m photometry apertures for the western component of thesystem. The second column shows the PACS photometry apertures for the eastern nucleus. The third column shows thePACS photometry apertures encompassing both galaxies which includes flux not in the component apertures, givingthe total flux from this system. In the SPIRE bands, we only computed component fluxes at 250 µ m since the galaxypair is still resolved, however since the galaxies are essentially unresolved in the other two SPIRE bands, we onlycompute total fluxes at those two wavelengths. Note the fourth column only shows the total SPIRE apertures of bothgalaxies, and the individual 250 µ m plots were omitted to keep the figure manageable. 240 A B LE P A C S AND SP I R ET O T A L F L UX E S O F GOA L SS Y S TE M S P A C SSP I R E I R A S N a m e O p ti ca l N a m e F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) J y J y J y J y J y J y ( )( )( )( )( )( )( )( )( ) F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F - NG C , M r k938 . ± . . ± . . ± . . ± . . ± . . ± . F - A r p256 , M C G - - - / . ± . . ± . . ± . . ± . . ± . . ± . F - E S O -I G , H a r o11 . ± . . ± . . ± . . ± . . ± . . ± . F - NG C . ± . . ± . . ± . . ± . . ± . . ± . F + M C G + - - . ± . . ± . . ± . . ± . . ± . . ± . F + NG C B . ± . . ± . . ± . . ± . . ± . . ± . F - I C , A r p236 . ± . . ± . . ± . . ± . . ± . . ± . F - M C G - - - . ± . . ± . . ± . . ± . . ± . . ± . F - E S O - G . ± . . ± . . ± . . ± . . ± . . ± . F + C G C G - . ± . . ± . . ± . . ± . . ± . . ± . F - E S O - G . ± . . ± . . ± . . ± . . ± . . ± . F - RR , E S O - G / . ± . . ± . . ± . . ± . . ± . . ± . F - . ± . . ± . . ± . . ± . . ± . . ± . F + III Z w . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F + UG C . ± . . ± . . ± . . ± . . ± . . ± . F - NG C . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F + I C . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F + M C G + - - . ± . . ± . . ± . . ± . . ± . . ± . F + UG C . ± . . ± . . ± . . ± . . ± . . ± . F - NG C . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F - NG C . ± . ··· . ± . . ± . . ± . . ± . F + UG C . ± . . ± . . ± . . ± . . ± . . ± . F + . ± . . ± . . ± . . ± . . ± . . ± . F + a M A S X J + . ± . . ± . . ± . . ± . . ± . . ± . F + UG C . ± . . ± . . ± . . ± . . ± . . ± . F + UG C . ± . . ± . . ± . . ± . . ± . . ± . F + a UG C . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F + . ± . . ± . . ± . . ± . . ± . . ± . F - NG C . ± . . ± . . ± . . ± . . ± . . ± . A B LE — C on ti nu e d P A C SSP I R E I R A S N a m e O p ti ca l N a m e F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) J y J y J y J y J y J y ( )( )( )( )( )( )( )( )( ) F + . ± . . ± . . ± . . ± . . ± . . ± . F + C G C G - . ± . . ± . . ± . . ± . . ± . . ± . F + a C G C G - . ± . . ± . . ± . . ± . . ± . . ± . + . ± . . ± . . ± . . ± . . ± . . ± . F + UG C . ± . . ± . . ± . . ± . . ± . . ± . F - E S O - G . ± . . ± . . ± . . ± . . ± . . ± . F - E S O -I G . ± . . ± . . ± . . ± . . ± . . ± . F - NG C . ± . . ± . . ± . . ± . . ± . . ± . + . ± . . ± . . ± . . ± . . ± . . ± . F - NG C . ± . . ± . . ± . . ± . . ± . . ± . F + UG C . ± . . ± . . ± . . ± . . ± . . ± . F - E S O -I G . ± . . ± . . ± . . ± . . ± . . ± . F - M C G - - - . ± . . ± . . ± . . ± . . ± . . ± . F - NG C . ± . . ± . . ± . . ± . . ± . . ± . F - a NG C . ± . . ± . . ± . . ± . . ± . . ± . F + C G C G - . ± . . ± . . ± . . ± . . ± . . ± . + . ± . . ± . . ± . . ± . . ± . . ± . F + V II Z w . ± . . ± . . ± . . ± . . ± . . ± . + . ± . . ± . . ± . . ± . . ± . . ± . F - . ± . . ± . . ± . . ± . . ± . . ± . F - . ± . . ± . . ± . . ± . . ± . . ± . + M C G + - - . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F + UG C . ± . . ± . . ± . . ± . . ± . . ± . + . ± . . ± . . ± . . ± . . ± . . ± . F - . ± . . ± . . ± . . ± . . ± . . ± . F + UG C . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F - E S O -I G . ± . . ± . . ± . . ± . . ± . . ± . F - E S O - G . ± . . ± . . ± . . ± . . ± . . ± . F + UG C . ± . . ± . . ± . . ± . . ± . . ± . F - . ± . . ± . . ± . . ± . . ± . . ± . F - A M - . ± . . ± . . ± . . ± . . ± . . ± . + NG C . ± . . ± . . ± . . ± . . ± . . ± . F - NG C . ± . . ± . . ± . . ± . . ± . . ± . A B LE — C on ti nu e d P A C SSP I R E I R A S N a m e O p ti ca l N a m e F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) J y J y J y J y J y J y ( )( )( )( )( )( )( )( )( ) - . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . b . ± . b . ± . b . ± . b . ± . b . ± . b F + M C G + - - . ± . . ± . . ± . . ± . . ± . . ± . F + a NG C . ± . . ± . . ± . . ± . . ± . . ± . - . ± . . ± . . ± . . ± . . ± . . ± . F + . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . - E S O -I G . ± . . ± . . ± . . ± . . ± . . ± . F - E S O -I G . ± . . ± . . ± . . ± . . ± . . ± . F + . ± . . ± . . ± . . ± . . ± . . ± . - . ± . . ± . . ± . . ± . . ± . . ± . F - . ± . . ± . . ± . . ± . . ± . . ± . F + UG C . ± . . ± . . ± . . ± . . ± . . ± . F + UG C . ± . ··· . ± . . ± . . ± . . ± . F + M C G + - - . ± . . ± . . ± . . ± . . ± . . ± . F + A r p303 , I C / . ± . . ± . . ± . . ± . . ± . . ± . F - NG C . ± . . ± . . ± . . ± . . ± . . ± . F - E S O -I G . ± . . ± . . ± . . ± . . ± . . ± . F + . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F - NG C . ± . . ± . . ± . . ± . . ± . . ± . F - E S O - G . ± . . ± . . ± . . ± . . ± . . ± . F - E S O - G . ± . . ± . . ± . . ± . . ± . . ± . F + . ± . . ± . . ± . . ± . . ± . . ± . F + M C G + - - . ± . . ± . . ± . . ± . . ± . . ± . F - C G C G - . ± . . ± . . ± . . ± . . ± . . ± . F + I C . ± . . ± . . ± . . ± . . ± . . ± . F - E S O - G . ± . . ± . . ± . . ± . . ± . . ± . F + NG C , A r p299 . ± . . ± . . ± . . ± . . ± . . ± . F - E S O - G . ± . . ± . . ± . . ± . . ± . . ± . F - E S O -I G . ± . . ± . . ± . . ± . . ± . . ± . F + . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F - E S O - G . ± . . ± . . ± . . ± . . ± . . ± . F - a E S O - G . ± . . ± . . ± . . ± . . ± . . ± . A B LE — C on ti nu e d P A C SSP I R E I R A S N a m e O p ti ca l N a m e F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) J y J y J y J y J y J y ( )( )( )( )( )( )( )( )( ) - . ± . . ± . . ± . . ± . . ± . . ± . F - . ± . . ± . . ± . . ± . . ± . . ± . F - NG C . ± . . ± . . ± . . ± . . ± . . ± . F + UG C , M r k231 . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F + C G C G - . ± . . ± . . ± . . ± . . ± . . ± . F - M C G - - - . ± . . ± . . ± . . ± . . ± . . ± . F - E S O - G . ± . . ± . . ± . . ± . . ± . . ± . - . ± . . ± . . ± . . ± . . ± . . ± . F + I C . ± . . ± . . ± . . ± . . ± . . ± . - . ± . . ± . . ± . . ± . . ± . . ± . F + VV a . ± . . ± . . ± . . ± . . ± . . ± . F + UG C . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F - M C G - - - . ± . . ± . . ± . . ± . . ± . . ± . F - NG C . ± . . ± . . ± . . ± . . ± . . ± . - E S O - G . ± . . ± . . ± . . ± . . ± . . ± . F - I C . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F + A r p240 , NG C / . ± . . ± . . ± . . ± . . ± . . ± . F + UG C , M r k273 . ± . . ± . . ± . . ± . . ± . . ± . F + UG C . ± . . ± . . ± . . ± . . ± . . ± . F - E S O -I G . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F + A r p84 , NG C / . ± . . ± . . ± . . ± . . ± . . ± . F + C G C G - . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F - . ± . . ± . . ± . . ± . . ± . . ± . F - . ± . . ± . . ± . . ± . . ± . . ± . F - NG C . ± . . ± . . ± . . ± . . ± . . ± . F + VV a , A r p302 . ± . . ± . . ± . . ± . . ± . . ± . F - I C A / B . ± . . ± . . ± . . ± . . ± . . ± . F + C G C G - . ± . . ± . . ± . . ± . . ± . . ± . F + VV . ± . . ± . . ± . . ± . . ± . . ± . - E S O - G . ± . . ± . . ± . . ± . . ± . . ± . A B LE — C on ti nu e d P A C SSP I R E I R A S N a m e O p ti ca l N a m e F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) J y J y J y J y J y J y ( )( )( )( )( )( )( )( )( ) F + . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F + A r p220 , UG C . ± . ··· . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F - . ± . . ± . . ± . . ± . . ± . . ± . F + C G C G - . ± . . ± . . ± . . ± . . ± . . ± . - NG C . ± . . ± . . ± . . ± . . ± . . ± . F - E S O -I G . ± . . ± . . ± . . ± . . ± . . ± . F - . ± . . ± . . ± . . ± . . ± . . ± . F - E S O - G . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F - . ± . . ± . . ± . . ± . . ± . . ± . F + NG C , A r p293 . ± . . ± . . ± . . ± . . ± . . ± . F + . ± . . ± . . ± . . ± . . ± . . ± . F - . ± . . ± . . ± . . ± . . ± . . ± . F - . ± . . ± . . ± . . ± . . ± . . ± . F - E S O - G . ± . . ± . . ± . . ± . . ± . . ± . F + UG C . ± . . ± . . ± . . ± . . ± . . ± . F + C G C G - . ± . . ± . . ± . . ± . . ± . . ± . - . ± . . ± . . ± . . ± . . ± . . ± . + . ± . . ± . . ± . . ± . . ± . . ± . F + NG C , A r p81 . ± . . ± . . ± . . ± . . ± . . ± . F - I C . ± . . ± . . ± . . ± . . ± . . ± . F + C G C G - . ± . . ± . . ± . . ± . . ± . . ± . F - . ± . . ± . . ± . . ± . . ± . . ± . F + NG C A / B . ± . . ± . . ± . . ± . . ± . . ± . F - I C . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F + VV , NG C , UG C . ± . . ± . . ± . . ± . . ± . . ± . F - E S O -I G . ± . . ± . . ± . . ± . . ± . . ± . F - . ± . . ± . . ± . . ± . . ± . . ± . + . ± . . ± . . ± . . ± . . ± . . ± . F - E S O - G . ± . . ± . . ± . . ± . . ± . . ± . A B LE — C on ti nu e d P A C SSP I R E I R A S N a m e O p ti ca l N a m e F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) J y J y J y J y J y J y ( )( )( )( )( )( )( )( )( ) F - NG C . ± . . ± . . ± . . ± . . ± . . ± . + M C G + - - . ± . . ± . . ± . . ± . . ± . . ± . F - NG C . ± . . ± . . ± . . ± . . ± . . ± . + . ± . . ± . . ± . . ± . . ± . . ± . F + C G C G - , II Z w . ± . . ± . . ± . . ± . . ± . . ± . F - E S O -I G . ± . . ± . . ± . . ± . . ± . . ± . F - E S O - G . ± . . ± . . ± . . ± . . ± . . ± . + . ± . . ± . . ± . . ± . . ± . . ± . F - E S O -I G . ± . . ± . . ± . . ± . . ± . . ± . F - NG C . ± . ··· . ± . . ± . . ± . . ± . F - E S O - G . ± . . ± . . ± . . ± . . ± . . ± . F - I C . ± . . ± . . ± . . ± . . ± . . ± . F - E S O - G . ± . . ± . . ± . . ± . . ± . . ± . F + UG C . ± . . ± . . ± . . ± . . ± . . ± . F - E S O -I G . ± . . ± . . ± . . ± . . ± . . ± . F - . ± . . ± . . ± . . ± . . ± . . ± . F + NG C , I C , A r p298 . ± . . ± . . ± . . ± . . ± . . ± . F + C G C G - . ± . . ± . . ± . . ± . . ± . . ± . F - E S O -I G . ± . . ± . . ± . . ± . . ± . . ± . F + I C . ± . . ± . . ± . . ± . . ± . . ± . F - NG C . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . . ± . . ± . . ± . . ± . . ± . F - NG C . ± . . ± . . ± . . ± . . ± . . ± . F - E S O -I G . ± . . ± . . ± . . ± . . ± . . ± . F + NG C , H C G . ± . . ± . . ± . . ± . . ± . . ± . + NG C . ± . . ± . . ± . . ± . . ± . . ± . + a NG C . ± . . ± . . ± . . ± . . ± . . ± . F + . ± . . ± . . ± . . ± . . ± . . ± . F - M C G - - - . ± . . ± . . ± . . ± . . ± . . ± . F - a M C G - - - , M r k933 . ± . . ± . . ± . . ± . . ± . . ± . + . ± . . ± . . ± . . ± . . ± . . ± . F + A r p86 , NG C / . ± . . ± . . ± . . ± . . ± . . ± . F + NG C . ± . b . ± . b . ± . b . ± . b . ± . b . ± . b F + M r k331 . ± . . ± . . ± . . ± . . ± . . ± . O TE . — T h e m ono c h r o m a ti c fl uxd e n s it y i nun it s o f J a n s ky f o r eac ho f t h e t h r ee P A C S a nd t h r ee SP I R E b r o a db a nd fi lt e r s . T h e s ea r e t h e t o t a l fl ux e s f o r eac h GOA L S s y s t e m . T h ec o l u m nd e s c r i p ti on s a r e ( ) t h e r o w r e f e r e n ce nu m b e r . ( ) T h e I R A S n a m e o f t h e g a l a xy , o r d e r e dby a s ce nd i ng R A . G a l a x i e s w it h t h e“ F ” p r e fi xo r i g i n a t e fr o m t h e I RA S F a i n t S ou r ce C a t a l og , a ndg a l a x i e s w it hno “ F ” p r e fi x a r e fr o m t h e P o i n t S ou r ce C a t a l og . ( ) C o mm onop ti ca l c oun t e r p a r t n a m e s t o t h e g a l a xy s y s t e m s . C o l u m n s ( ) – ( ) a r e t h e fl ux e s fr o m t h e P A C S i n s t r u m e n ti nun it s o f J y . N o t e t h a tt h e f ou r g a l a x i e s w h i c h l ac k µ mm ea s u r e m e n t s a r e I R A SF - ( NG C ) , I R A SF + ( UG C ) , I R A SF + ( A r p220 ) , a nd I R A SF - ( NG C ) . C o l u m n s ( ) – ( ) a r e t h e fl ux e s fr o m t h e SP I R E i n s t r u m e n ti nun it s o f J y . a T h e s ea r e v e r y w i d e l y s e p a r a t e dg a l a xyp a i r s t h a t r e qu i r e d t w o H e rs c h e l P A C S ob s e r v a ti on s . b T h i s i s a t r i p l e s y s t e m , ho w e v e r on l y t w o c o m pon e n t g a l a x i e s a r e v i s i b l e i n P A C S du e t o it ss m a ll e r fi e l do f v i e w . T h e t o t a l fl ux f o r t h i ss y s t e m do e s no t i n c l ud e t h e t h i r dg a l a xyno t v i s i b l e i n P A C S . .2. SPIRE Aperture Photometry The SPIRE 2-pass pipeline (see § Planck -HFI maps (see § annularSkyAperturePhotometry task in HIPE in order to keep our measurements asuniform as possible. However this method results inthe loss of flux outside the finite-sized aperture, forwhich an aperture correction is needed to fully ac-count for all the flux. In the case of point sources, we applied the aperture correction by dividing our fluxesby the encircled energy fraction (EEF) amount corre-sponding to the aperture radius and SPIRE channel.The EEFs can be found in the SPIRE calibration files(accessible from within HIPE), and represents the ra-tio of flux (energy) inside the aperture divided by thetrue flux of the point source. As with the PACS aper-ture corrections, SPIRE fluxes in which an aperturecorrection was applied are denoted by a superscript cin Table 4, with average corrections of 10.1%, 10.3%,and 14.8% for the 250, 350, and 500 µ m channels re-spectively. Similarly the median correction values areless than a percent difference from the averages.In order to check the validity of our point sourcefluxes, we measured our fluxes a second time using thetimeline source fitter on a subset of 65 objects that arepoint sources in all three SPIRE bands. The timelinefitter is the preferred method of obtaining point sourcefluxes on the SPIRE maps, since it works on the base-line subtracted, destriped, and deglitched Level 1 time-lines of the data (which are calibrated in Jy/beam ).By using a Levenberg-Marquardt algorithm to fit a twodimensional circular or elliptical Gaussian function tothe 2-D timeline data, the source can be modeled andthe point source flux can be calculated from the 2-Dfit. The advantage is it avoids any potential artifactsarising from the map-making process, such as smear-ing effects from pixelization. Because it does not usethe Level 2 maps, source extraction is not necessary(i. e. aperture photometry), and there are no aperturecorrections needed since the 2-D fit in principle takesinto accounts all of the flux from the point source.When we compared the aperture photometry resultsto the timeline fitter results, we found that they bothagree very well at 250 µ m and 350 µ m with an aver-age aperture/timeline flux ratio of 1.030 and 0.995 re-spectively, however the 500 µ m channel had a slightlylower ratio of 0.93. To further check our results, weplotted the aperture/timeline flux ratio against the aper-ture photometry flux for all three bands, and foundno statistically significant correlation in the flux ra-tio as a function of flux. However we do note inthe 500 µ m case, fluxes less than approximately 150mJy appear to have a lower aperture/timeline flux ra-tio, whereas fluxes above that value have an averageratio close to unity. We believe this underestimationat faint fluxes is due to confusion noise, which wasalso observed in the SPIRE Map Making Test Report. See Dowell et al. (2010), § µ m fluxes are still consistent within the typical fluxerrors ( ∼ %). As a final check we also plotted theaperture/timeline ratio against the aperture photometryradius, and we again found no statistically significantcorrelation. From these tests our point source aperturephotometry fluxes appear to be in good agreement withthe results from the timeline fitter.In the case of semi-extended to extended sources,aperture corrections become more complex since theflux originates not from an unresolved source, but isseen instead as surface brightness distributed within anaperture. Although an aperture correction is needed forreasons similar to the point source case, Shimizu et al.(2016) found that their extended SPIRE fluxes for their Swift
BAT sample did not need aperture corrections be-cause they were negligible. To test this, they first con-volved their 160 µ m PACS data to the resolution of thethree SPIRE bands, and then measured the fluxes onboth the convolved and unconvolved images using thesame SPIRE aperture sizes. Aperture corrections werethen calculated as the ratio of the flux on the originalPACS image divided by the flux obtained on the con-volved image, with resulting median aperture correc-tions of 1.01, 0.98, and 0.98 for the 250 µ m, 350 µ m,and 500 µ m channels respectively. This makes the as-sumption that the 160 µ m and SPIRE fluxes originatefrom the same material within their galaxies. We alsonote that their aperture sizes are similar to ours, sincetheir galaxy sample lies in the same redshift range.Ciesla et al. (2012) also showed by simulating in theworst-case scenario, a maximum aperture correctionof 5% is needed at 500 µ m. However this was done onan (intentionally) unphysical source that has a flat con-stant surface brightness, with a sharp drop to zero fluxat a set radius. On more realistic sources they calcu-lated aperture corrections of approximately (cid:46) σ dispersion of the flux in each pixel within theannular area used for our background measurements.This is then multiplied by the square root of the num-ber of pixels within the photometry aperture (whichcan be a fractional amount) to obtain the error in back-ground measurement. The instrumental error is calcu-lated by summing in quadrature the pixels within theaperture on the error map generated by the pipeline.We note this underestimates the error because the noiseis correlated between pixels. Our final SPIRE flux un-certainties are then computed as the quadrature sumof all three sources of error. In the case where thetotal system flux is the sum of two (or more) com-ponents, the flux uncertainty is the quadrature sum ofeach galaxy component’s flux error. Due to the large radiative contribution of
Herschel ’soptical components (230 Jy, 250 Jy, 270 Jy for thePSW, PMW, PLW channels respectively), SPIRE canonly measure the relative flux on the sky, i. e. the fluxof the target minus the background level. During datareduction the SPIRE maps are generated such thatthe background is approximately normalized to zero,which makes it impossible to determine the absoluteflux of the target. However to recover the absoluteflux we used the all-sky maps from the
Planck mission(modified to have a spatial resolution of 8 (cid:48)
FWHM),since the Planck-HFI 857 GHz and 545 GHz filtersmatch fairly well to the
Herschel µ m and 500 µ m band passes respectively (see Fig. 5.16 in theSPIRE handbook). These corrections become moreimportant in sources with very extended flux, sincesome of the diffuse low surface-brightness flux maybe subtracted out. 249ertincourt et al. (2016) performed an in-depthanalysis of SPIRE and HFI data on the same fields,and found a very high degree of linearity between thetwo datasets, as well as a good agreement in the rel-ative calibrations between the two instruments. Thezero-points of the Planck maps are derived assumingthat the zero-point of the Galactic emission can be de-fined as zero dust emission for a null HI column den-sity . The final step is to apply a slight gain cor-rection to the Planck maps, which for our data weused the NHSC recommended gain factors of 0.989and 1.02 for the 857 GHz and 545 GHz channels, re-spectively. The
Planck calibration uncertainty for bothchannels is 10%. Using the all-sky
Planck data, zero-point corrections are applied as flux offsets over the en-tire SPIRE map, and do not affect the SPIRE flux cal-ibrations (which is background subtracted). We notethat these zero point corrections were only applied tothe 350 µ m and 500 µ m channels only, and the 250 µ m maps were not corrected since there is no overlapwith Planck . See the Explanatory Supplement to the Planck 2013 results: http://wiki.cosmos.esa.int/planckpla/index.php/CMBand astrophysical component maps A B LE P A C S AND SP I R ET O T A L AND C O M P ON E N T F L UX E S O F GOA L SS Y S TE M S A p e r t u r e C e n t e r C oo r d i n a t e P A C SSP I R E I R A S N a m e I nd i v i du a l N a m e R AD ec . A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) ——— HH : MM : SS DD : MM : SS (cid:48)(cid:48) kp c J y J y J y (cid:48)(cid:48) kp c J y J y J y ( )( )( )( )( )( )( )( )( )( )( )( )( )( )( ) F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . c F - NG C : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - NG C : : . − : : . ······························ F - I R G P J . - : : . − : : . ······ . ± . c . ± . c . ± . c ······ . ± . c . ± . c . ± . c F - M C G - - - : : . − : : . . . ± . c . ± . c . ± . c ··············· F - M C G - - - : : . − : : . . . ± . . ± . . ± . ··············· F - A r p256 : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F - E S O -I G : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - NG C : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - NG C : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - R S C G : : . − : : . ······ . ± . c . ± . c . ± . c ······ . ± . c . ± . c . ± . c F + M C G + - - : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F + NG C B : : . + : : . . . ± . c . ± . c ·················· F + NG C A : : . + : : . . . ± . . ± . ·················· F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F - I C A : : . − : : . ······························ F - I C B : : . − : : . ······························ F - I C : : . − : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F - M C G - - - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - M C G - - - : : . − : : . ······························ F - M C G - - - : : . − : : . ······························ F - E S O - G : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + C G C G - : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - E S O - G : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - E S O - G : : . − : : . . . ± . c . ± . c . ± . c . . ± . c ······ F - E S O - G : : . − : : . . . ± . c . ± . c . ± . c . . ± . c ······ F - RR : : . − : : . ······ . ± . c . ± . c . ± . c . . ± . . ± . . ± . F - I R A SF - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + III Z w : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F + UG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + KUG + : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + I R G P J . + : : . + : : . ······ . ± . c . ± . c . ± . c ······ . ± . c . ± . c . ± . c A B LE — C on ti nu e d A p e r t u r e C e n t e r C oo r d i n a t e P A C SSP I R E I R A S N a m e I nd i v i du a l N a m e R AD ec . A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) ——— HH : MM : SS DD : MM : SS (cid:48)(cid:48) kp c J y J y J y (cid:48)(cid:48) kp c J y J y J y ( )( )( )( )( )( )( )( )( )( )( )( )( )( )( ) F - NG C : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - NG C : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - NG C : : . − : : . . . ± . . ± . . ± . . . ± . c . ± . c ··· F - NG C : : . − : : . . . ± . . ± . . ± . . . ± . . ± . ··· F - NG C / : : . − : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F - H C G : : . − : : . ······ . ± . c . ± . c . ± . c ······ . ± . c . ± . c . ± . c F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F + I C : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F + M A S X J + : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F + I R G P J . + : : . + : : . ······ . ± . . ± . . ± . ······ . ± . c . ± . c . ± . c F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + I R G P J . + : : . + : : . ······ . ± . . ± . . ± . . . ± . . ± . . ± . F + M C G + - - : : . + : : . . . ± . c . ± . c . ± . c . . ± . c ······ F + M C G + - - : : . + : : . . . ± . c . ± . c . ± . c . . ± . c ······ F + K P G : : . + : : . ······ . ± . c . ± . c . ± . c . . ± . . ± . . ± . F + UG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - NG C : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F - NG C : : . − : : . . . ± . ··· . ± . . . ± . . ± . . ± . F + UG C : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F + I R A SF + : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + a M A S X J + : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F + M C G + - - : : . + : : . ······························ F + M C G + - - : : . + : : . ······························ F + UG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . c F + UG C : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F + a UG C : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F + I R A SF + : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - NG C : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + I R A SF + : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c A B LE — C on ti nu e d A p e r t u r e C e n t e r C oo r d i n a t e P A C SSP I R E I R A S N a m e I nd i v i du a l N a m e R AD ec . A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) ——— HH : MM : SS DD : MM : SS (cid:48)(cid:48) kp c J y J y J y (cid:48)(cid:48) kp c J y J y J y ( )( )( )( )( )( )( )( )( )( )( )( )( )( )( ) F + a C G C G - : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F + C G C G - : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c + I R A S + N E : : . + : : . ······························ + I R A S + S W : : . + : : . ······························ + I R A S + : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F + UG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c F - E S O - G : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - E S O -I G N E D : : . − : : . . . ± . c . ± . c . ± . c ··············· F - E S O -I G N E D : : . − : : . . . ± . c . ± . c . ± . c ··············· F - E S O -I G : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . c F - NG C : : . − : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c + I R A S + : : . + : : . . . ± . . ± . c . ± . c . . ± . c . ± . c . ± . c F - NG C : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + UG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F - E S O -I G : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - M C G - - - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - NG C : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - a NG C : : . − : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c F + C G C G - N E D : : . + : : . . . ± . c . ± . c . ± . c ··············· F + C G C G - N E D : : . + : : . . . ± . c . ± . c . ± . c ··············· F + C G C G - : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . + I R A S + : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c + M A S X J + : : . + : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c + I R G P J . + : : . + : : . ······ . ± . c . ± . c . ± . c . . ± . . ± . . ± . F + V II Z w : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c + I R A S + : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - I R A SF - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - I R A SF - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c + M C G + - - : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . A B LE — C on ti nu e d A p e r t u r e C e n t e r C oo r d i n a t e P A C SSP I R E I R A S N a m e I nd i v i du a l N a m e R AD ec . A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) ——— HH : MM : SS DD : MM : SS (cid:48)(cid:48) kp c J y J y J y (cid:48)(cid:48) kp c J y J y J y ( )( )( )( )( )( )( )( )( )( )( )( )( )( )( ) F + UG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c + I R A S + : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c + UG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . + H I P A SS J + : : . + : : . ······ . ± . c . ± . c . ± . c . . ± . . ± . . ± . F - I R A SF - N W : : . − : : . ······························ F - I R A SF - S E : : . − : : . ······························ F - I R A SF - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + UG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . c F + UG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + K P G : : . + : : . ······ . ± . . ± . . ± . ······ . ± . . ± . . ± . c F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F - E S O -I G N E D : : . − : : . ······························ F - E S O -I G N E D : : . − : : . ······························ F - E S O -I G N E D : : . − : : . ······························ F - E S O -I G : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F - E S O - G : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - E S O - G : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F - I R G P J . - : : . − : : . ······ . ± . c . ± . c . ± . c ······ . ± . c . ± . c . ± . c F + UG C : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F - I R A SF - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - A M - N E D : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - A M - N E D : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - A M - : : . − : : . ······ . ± . c . ± . c . ± . c . . ± . . ± . . ± . + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c + K P G : : . + : : . ······ . ± . . ± . . ± . ······ . ± . . ± . c . ± . c F - NG C : : . − : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c - I R A S - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + NG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + NG C : : . + : : . ········· b ··· b ··· b . . ± . b . ± . b , c . ± . b , c F + W B L : : . + : : . ······ . ± . c . ± . c . ± . c ······ . ± . c . ± . c . ± . c F + M C G + - - : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c A B LE — C on ti nu e d A p e r t u r e C e n t e r C oo r d i n a t e P A C SSP I R E I R A S N a m e I nd i v i du a l N a m e R AD ec . A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) ——— HH : MM : SS DD : MM : SS (cid:48)(cid:48) kp c J y J y J y (cid:48)(cid:48) kp c J y J y J y ( )( )( )( )( )( )( )( )( )( )( )( )( )( )( ) F + a NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . c - I R A S - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + I R A SF + : : . + : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c F + NG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c - E S O -I G S W : : . − : : . . . ± . c . ± . c . ± . c ··············· - E S O -I G N E : : . − : : . . . ± . c . ± . c . ± . c ··············· - E S O -I G : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F - E S O -I G N E D : : . − : : . ······························ F - E S O -I G N E D : : . − : : . ······························ F - E S O -I G : : . − : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c F + I R A SF + : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c - I R A S - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - M A S X J - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c ······ F - M A S X J - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c ······ F - I R A SF - : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + C G C G - : : . + : : . ······························ F + UG C N E D : : . + : : . ······························ F + UG C N E D : : . + : : . ······························ F + UG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . c F + UG C : : . + : : . . . ± . c ··· . ± . c . . ± . c . ± . c . ± . c F + M C G + - - : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c ··· F + M C G + - - : : . + : : . . . ± . . ± . . ± . . . ± . . ± . ··· F + C G C G - : : . + : : . ······ . ± . c . ± . c . ± . c . . ± . . ± . . ± . F + I C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + I C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + A r p303 : : . + : : . ······ . ± . . ± . . ± . . . ± . . ± . . ± . F - NG C : : . − : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c F - M C G - - - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - I R G P J . - : : . − : : . ······ . ± . c . ± . c . ± . c . . ± . . ± . . ± . F - E S O -I G : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + I R A SF + : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . A B LE — C on ti nu e d A p e r t u r e C e n t e r C oo r d i n a t e P A C SSP I R E I R A S N a m e I nd i v i du a l N a m e R AD ec . A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) ——— HH : MM : SS DD : MM : SS (cid:48)(cid:48) kp c J y J y J y (cid:48)(cid:48) kp c J y J y J y ( )( )( )( )( )( )( )( )( )( )( )( )( )( )( ) F - NG C : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . c F - E S O - G : : . − : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c F - E S O - G : : . − : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c F + I R A SF + : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + M C G + - - : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - C G C G - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c ··· F - M A S X J - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c ··· F - I R G P J . - : : . − : : . ······ . ± . c . ± . c . ± . c . . ± . . ± . . ± . F + I C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c ··· F + M C G + - - : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c ··· F + I R A SF + : : . + : : . ······ . ± . c . ± . c . ± . c . . ± . . ± . . ± . F - E S O - G : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + UG C : : . + : : . ······························ F + UG C : : . + : : . ······························ F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F - E S O - G : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - M C G - - - : : . − : : . ······························ F - M C G - - - : : . − : : . ······························ F - E S O -I G : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + I R A SF + : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + NG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - E S O - G : : . − : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F - a E S O - G : : . − : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c - I R A S - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - I R A SF - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - NG C : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - M C G + - - : : . − : : . . . ± . . ± . . ± . c . . ± . c . ± . c . ± . c F - K P G : : . − : : . ······ . ± . c . ± . c . ± . c ······ . ± . c . ± . c . ± . c F + UG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + M A S X J + : : . + : : . ······························ F + F I R S T J . + : : . + : : . ······························ A B LE — C on ti nu e d A p e r t u r e C e n t e r C oo r d i n a t e P A C SSP I R E I R A S N a m e I nd i v i du a l N a m e R AD ec . A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) ——— HH : MM : SS DD : MM : SS (cid:48)(cid:48) kp c J y J y J y (cid:48)(cid:48) kp c J y J y J y ( )( )( )( )( )( )( )( )( )( )( )( )( )( )( ) F + NG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + C G C G - : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - M C G - - - S W : : . − : : . ······························ F - M C G - - - N E : : . − : : . ······························ F - M C G - - - : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F - E S O - G : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c - I R A S - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + I C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c - I R A S - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + VV a : : . + : : . . . ± . c . ± . c . ± . c ··············· F + VV : : . + : : . . . ± . c . ± . c . ± . c ··············· F + VV : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + UG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + NG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - M C G - - - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - M C G - - - : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . c F - I R A SF - : : . − : : . ······ . ± . c . ± . c . ± . c ······ . ± . c . ± . c . ± . c F - NG C : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . - E S O - G : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . c F - I C : : . − : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c F + K P G A : : . + : : . ······························ F + K P G B : : . + : : . ······························ F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . c F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . c F + A r p240 : : . + : : . ······ . ± . . ± . . ± . . . ± . . ± . . ± . F + UG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + UG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . c F - E S O -I G : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + NG C S : : . + : : . . . ± . c . ± . c ·················· F + NG C N : : . + : : . . . ± . c . ± . c ·················· A B LE — C on ti nu e d A p e r t u r e C e n t e r C oo r d i n a t e P A C SSP I R E I R A S N a m e I nd i v i du a l N a m e R AD ec . A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) ——— HH : MM : SS DD : MM : SS (cid:48)(cid:48) kp c J y J y J y (cid:48)(cid:48) kp c J y J y J y ( )( )( )( )( )( )( )( )( )( )( )( )( )( )( ) F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . c F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + NG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + A r p84 : : . + : : . ······ . ± . c . ± . c . ± . c . . ± . . ± . . ± . F + C G C G - : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + NG C W : : . + : : . ······························ F + NG C E : : . + : : . ······························ F + NG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - I R A SF - S W : : . − : : . ······························ F - I R A SF - N E : : . − : : . ······························ F - I R A SF - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - I R A SF - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - NG C : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . c F - NG C : : . − : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c F - I R G P J . - : : . − : : . ······ . ± . . ± . . ± . ······ . ± . . ± . c . ± . c F + VV a : : . + : : . . . ± . . ± . . ± . ··············· F + VV : : . + : : . . . ± . . ± . . ± . ··············· F + VV : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F - I C A : : . − : : . . . ± . . ± . ·················· F - I C B : : . − : : . . . ± . c . ± . c ·················· F - I C : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + C G C G - : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + VV N E D : : . + : : . ······························ F + VV N E D : : . + : : . ······························ F + VV : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c - E S O - G : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + I R A SF + : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c F + UG C : : . + : : . . . ± . c ··· . ± . c . . ± . c . ± . c . ± . c F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c F + NG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c A B LE — C on ti nu e d A p e r t u r e C e n t e r C oo r d i n a t e P A C SSP I R E I R A S N a m e I nd i v i du a l N a m e R AD ec . A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) ——— HH : MM : SS DD : MM : SS (cid:48)(cid:48) kp c J y J y J y (cid:48)(cid:48) kp c J y J y J y ( )( )( )( )( )( )( )( )( )( )( )( )( )( )( ) F - I R A SF - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + C G C G - : : . + : : . . . ± . c . ± . c . ± . c . . ± . c ······ F + M A S X J + : : . + : : . . . ± . c . ± . c . ± . c . . ± . c ······ F + I R G P J . + : : . + : : . ······ . ± . c . ± . c . ± . c . . ± . . ± . . ± . - NG C : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F - M A S X J - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - M A S X J - : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F - E S O -I G : : . − : : . ······ . ± . c . ± . c . ± . c ······ . ± . c . ± . c . ± . c F - I R A SF - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - E S O - G : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - M A S X J - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - I R G P J . - : : . − : : . ······ . ± . c . ± . c . ± . c ······ . ± . c . ± . c . ± . c F + NG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - I R A SF - : : . − : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c F + NG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + A r p293 : : . + : : . ······ . ± . c . ± . c . ± . c . . ± . . ± . . ± . F + : : . + : : . ······························ F + : : . + : : . ······························ F + I R A SF + : : . + : : . . . ± . . ± . . ± . c . . ± . c . ± . c . ± . c F - I R A SF - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - I R A SF - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - E S O - G : : . − : : . . . ± . . ± . . ± . c . . ± . c . ± . c . ± . c F + UG C : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F + C G C G - : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c - I R A S - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c - M A S X J - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c - M A S X J - : : . − : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c - M A S X J - : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . - I R G P J - : : . − : : . ······ . ± . . ± . . ± . ······ . ± . c . ± . c . ± . c + M A S X J + : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c + M A S X J + : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c + I R A S + : : . + : : . ······ . ± . c . ± . c . ± . c ······ . ± . c . ± . c . ± . c A B LE — C on ti nu e d A p e r t u r e C e n t e r C oo r d i n a t e P A C SSP I R E I R A S N a m e I nd i v i du a l N a m e R AD ec . A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) ——— HH : MM : SS DD : MM : SS (cid:48)(cid:48) kp c J y J y J y (cid:48)(cid:48) kp c J y J y J y ( )( )( )( )( )( )( )( )( )( )( )( )( )( )( ) F + NG C : : . + : : . . . ± . c . ± . c ·················· F + NG C S E : : . + : : . . . ± . c . ± . c ·················· F + NG C : : . + : : . . . ± . c . ± . c ·················· F + A r p81 : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F - I C : : . − : : . . . ± . c . ± . c ·················· F - I C : : . − : : . . . ± . c . ± . c ·················· F - I C : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - K T S : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F - I R A SF - : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + C G C G - : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F + C G C G - : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + I R G P J + : : . + : : . ······ . ± . c . ± . c . ± . c ······ . ± . c . ± . c . ± . c F - I R A SF - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + NG C B : : . + : : . . . ± . . ± . . ± . ··············· F + NG C A : : . + : : . . . ± . . ± . . ± . ··············· F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F - I C : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . c F + NG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + UG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + VV : : . + : : . ······ . ± . c . ± . c . ± . c . . ± . . ± . . ± . F - E S O -I G : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - I R A SF - : : . − : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c + I R A S + : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - E S O - G : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - NG C : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . + M C G + - - : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c + NG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c + I R G P J + : : . + : : . ······ . ± . c . ± . c . ± . c ······ . ± . c . ± . c . ± . c F - NG C : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . + I R A S + : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F + C G C G - N W : : . + : : . ······························ F + C G C G - S E s w : : . + : : . ······························ A B LE — C on ti nu e d A p e r t u r e C e n t e r C oo r d i n a t e P A C SSP I R E I R A S N a m e I nd i v i du a l N a m e R AD ec . A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) ——— HH : MM : SS DD : MM : SS (cid:48)(cid:48) kp c J y J y J y (cid:48)(cid:48) kp c J y J y J y ( )( )( )( )( )( )( )( )( )( )( )( )( )( )( ) F + C G C G - S E n e : : . + : : . ······························ F + C G C G - : : . + : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c F - E S O -I G : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - E S O - G : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c + I R A S + : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - E S O -I G N E D : : . − : : . ······························ F - E S O -I G N E D : : . − : : . ······························ F - E S O -I G : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . c F - NG C : : . − : : . . . ± . ··· . ± . . . ± . c . ± . c . ± . c F - E S O - G : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . c F - I C : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F - E S O - G : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + UG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - E S O -I G : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - I R A SF - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + NG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + I C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + A r p298 : : . + : : . ······ . ± . c . ± . c . ± . c . . ± . . ± . . ± . F + C G C G - : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - E S O -I G : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + I C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - NG C : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + NG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + F + : : . + : : . ······ . ± . c . ± . c . ± . c ······ . ± . c . ± . c . ± . c F - NG C E : : . − : : . ······························ F - NG C W : : . − : : . ······························ F - NG C : : . − : : . . . ± . . ± . . ± . . . ± . . ± . c . ± . c F - E S O -I G N E D : : . − : : . . . ± . c . ± . c ·················· F - E S O -I G N E D : : . − : : . . . ± . c . ± . c ·················· F - E S O -I G : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . c A B LE — C on ti nu e d A p e r t u r e C e n t e r C oo r d i n a t e P A C SSP I R E I R A S N a m e I nd i v i du a l N a m e R AD ec . A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) A ng . A p . P hy s . A p . F λ ( µ m ) F λ ( µ m ) F λ ( µ m ) ——— HH : MM : SS DD : MM : SS (cid:48)(cid:48) kp c J y J y J y (cid:48)(cid:48) kp c J y J y J y ( )( )( )( )( )( )( )( )( )( )( )( )( )( )( ) F + NG C : : . + : : . . . ± . c . ± . c ·················· F + NG C A : : . + : : . . . ± . c . ± . c ·················· F + A R P : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . + NG C : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c + a NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + I R A SF + : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - M C G - - - : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - a M C G - - - : : . − : : . . . ± . . ± . . ± . . . ± . . ± . . ± . c F - a M R K : : . − : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F - M C G - - - / M R K : : . − : : . ··············· . . ± . . ± . . ± . + I R A S + : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c . ± . c F + A r p86 : : . + : : . ······ . ± . . ± . . ± . . . ± . . ± . . ± . F + NG C : : . + : : . ········· b ··· b ··· b . . ± . b . ± . b . ± . b , c F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . ··· F + NG C : : . + : : . . . ± . . ± . . ± . . . ± . c . ± . c ··· F + K T G : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . F + M R K : : . + : : . . . ± . c . ± . c . ± . c . . ± . c . ± . c . ± . c F + UG C : : . + : : . . . ± . . ± . . ± . . . ± . . ± . . ± . c F + K P G : : . + : : . ······ . ± . c . ± . c . ± . c ······ . ± . c . ± . c . ± . c N O TE . — W e p r e s e n tt h e t a b l e o f m ono c h r o m a ti c fl uxd e n s it y i nun it s o f J a n s ky f o r eac ho f t h e t h r ee P A C S a nd t h r ee SP I R E b r o a db a nd fi lt e r s . T h e s ea r e t h ec o m pon e n t fl ux e s m ea s u r a b l e f o r eac h s y s t e m , w it h t h e t o t a l s y s t e m fl ux fr o m T a b l e i n c l ud e d f o r c o m p l e t e n e ss on t h e l a s tli n e f o r eac h s y s t e m . F o r t o t a l fl ux e s t h a t dono t h a v ea n a p e r t u r e s i ze li s t e d , t h e t o t a l s w e r eca l c u l a t e d a s t h e s u m o f t h ec o m pon e n t s . L i k e w i s e t h e R A a ndd ec . f o r t h e s e s y s t e m s r e p r e s e n tt h e m i dpo i n t b e t w ee n t h ec o m p a n i ong a l a x i e s . T h ec o l u m nd e s c r i p ti on s a r e ( ) t h e r o w r e f e r e n ce nu m b e r , w h i c h c o rr e s pond s t o t h e s a m e i nd i ce s u s e d i n T a b l e s . ( ) T h e I R A S n a m e o f t h e g a l a xy , o r d e r e dby a s ce nd i ng R A . G a l a x i e s w it h t h e“ F ” p r e fi xo r i g i n a t e fr o m t h e I RA S F a i n t S ou r ce C a t a l og , a ndg a l a x i e s w it hno “ F ” p r e fi x a r e fr o m t h e P o i n t S ou r ce C a t a l og . ( ) T h e i nd i v i du a l g a l a xyn a m e o f t h a t c o m pon e n t . G a l a x i e s p r e fi x e dby I R G P ( i n fr a r e dg a l a xyp a i r) a r e d e fi n e d i n t h ec o m p a n i on Sp it z e r - GOA L S p a p e r by M azza r e ll ae t a l . ( ) . C o l u m n s ( ) – ( ) a r e t h ec oo r d i n a t e s o f t h ea p e r t u r ece n t e r s u s e d . T h e s ea r e t h e s a m e µ m c oo r d i n a t e s a dop t e d i n M azza r e ll ae t a l . ( ) . C o l u m n s ( ) – ( ) a r e t h ea p e r t u r e r a d ii u s e d f o r P A C S pho t o m e t r y , i n a r c s eca ndkp c r e s p ec ti v e l y . C o l u m n s ( ) – ( ) a r e t h e fl ux e s fr o m t h e P A C S i n s t r u m e n ti nun it s o f J y . N o t e t h a tt h e f ou r g a l a x i e s w h i c h l ac k µ mm ea s u r e m e n t s a r e I R A SF - ( NG C ) , I R A SF + ( UG C ) , I R A SF + ( A r p220 ) , a nd I R A SF - ( NG C ) . G a l a xy c o m pon e n t s t h a t dono t h a v e fl ux m ea s u r e m e n t s a r e t oo c l o s e t o ac o m p a n i ong a l a xy t ob e r e s o l v e dby P A C S . C o l u m n s ( ) – ( ) a r e t h ea p e r t u r e r a d ii u s e d f o r SP I R E pho t o m e t r y , i n a r c s eca ndkp c r e s p ec ti v e l y . C o l u m n s ( ) – ( ) a r e t h e fl ux e s fr o m t h e P A C S i n s t r u m e n ti nun it s o f J y . G a l a xy c o m pon e n t s t h a t dono t h a v e fl ux m ea s u r e m e n t s a r e t oo c l o s e t o ac o m p a n i ong a l a xy t ob e r e s o l v e dby SP I R E . a T h e s ea r e v e r y w i d e l y s e p a r a t e dg a l a xyp a i r s t h a t r e qu i r e d t w o H e rs c h e l P A C S ob s e r v a ti on s . b T h i s g a l a xy i s p a r t o f a t r i p l e s y s t e m , bu ti s on l yv i s i b l e i n t h e SP I R E i m a g e s . T h e t o t a l fl ux f o r t h i ss y s t e m do e s no t i n c l ud e t h i s g a l a xy . c T h e s e fl ux e s h a v ea n a p e r t u r ec o rr ec ti on f ac t o r a pp li e d . .3. Distribution of Herschel
Fluxes
In Figure 5 we show the distribution of fluxes fromour
Herschel program in each of the three PACS andSPIRE photometer bands. The histogram x -axis rangeand binning for each band was selected in order tomeaningfully show the data. The fluxes shown hereare all 1657 measured fluxes, comprising both compo-nent and total fluxes, and do not include total systemfluxes that are the sum of the component fluxes. The x -axis of each panel is shown in units of log(Jy) to en-compass the wide dynamic range of fluxes measuredwithin the data.As expected the fluxes are generally higher in thethree PACS bands, while they are lower in the SPIREbands due to the Rayleigh-Jeans tail of the galaxy’sSED. The number of measured fluxes and bin sizesare indicated for each band, as well as the minimumand maximum fluxes. The galaxies with the high-est fluxes are all nearby (IRAS F02401–0013/NGC1068, IRAS F03316–3618/NGC 1365, and IRASF06107+7822/NGC 2146) and tend to be quite ex-tended in the Herschel maps, with the exception ofNGC 2146 which appears to be more concentratedthan the other two in the PACS 70 µ m and 100 µ m channels. On the other hand the faintest measuredfluxes in the PACS bands are well within the “faint”flux regime for PACS data reduction (see §
7. Discussion7.1. Comparison of PACS Fluxes to Previous Mis-sions
One important check is to compare our new PACS100 µ m fluxes to the legacy IRAS µ m fluxes pub-lished in Sanders et al. (2003), since the central wave-lengths of both instruments are the same. In Figure 6we show the filter transmission curves for PACS and IRAS in blue and red respectively. Before comparingthe fluxes measured from each telescope, several con-straints must be used to ensure a meaningful compar-ison. Importantly, we only selected objects that eitherappear as single galaxies in the PACS 100 µ m maps,or have component galaxies close enough such that itis only marginally resolved (or not at all) by PACS.We note that the IRAS µ m channel has a FWHMbeamsize of ∼ (cid:48) , which is significantly larger than thePACS 100 µ m beamsize of 6 . (cid:48)(cid:48)
8, therefore any unre-solved system in PACS would certainly appear unre-solved to
IRAS . Second, we also applied an aperture correction for point source objects in the PACS 100 µ m maps, however we did not apply a color correctionto any of our fluxes (see § IRAS
RBGS fluxes (see alsoSoifer et al. 1989), to ensure as accurate of a compar-ison as possible . Importantly, these objects span theentire range of 100 µ m fluxes within the GOALS sam-ple, and represent the entire spectrum of source mor-phology from point source to very extended objects.In the upper panel of Figure 7 we plot the 100 µ m PACS/IRAS flux ratio as a function of the IRAS µ m flux for 128 GOALS objects satisfying ourcriteria (corresponding to 64% of our sample). Thered line represents the unweighted average of the ra-tio which is 1.012, with dashed lines representing the - σ scatter of 0.09. On the other hand the median ofthe PACS/IRAS ratio is 1.006. Additionally we see novariation in the flux ratio except for fluxes above ∼ . (cid:48) × . (cid:48) and . (cid:48) × . (cid:48) .Their fluxes could be underestimated by IRAS sincethey were computed assuming point source photome-try, however once we exclude these two systems, theredoesn’t appear to be any PACS excess left in the brightsources. Overall, there is a broad agreement in fluxesbetween our Herschel data and the
IRAS data, to withinmeasurement errors ( ∼ µ m fluxes to the IRAS µ m fluxes, however becauseof the difference in wavelength, we first had to inter-polate the IRAS µ m measurement to 70 µ m. Todo this, we first estimated the power law index to thenearest whole number on the short-wavelength side ofthe SED bump using the IRAS µ m and PACS 70 µ m fluxes . To interpolate the IRAS µ m flux to70 µ m, we divided the IRAS µ m fluxes by mul-tiplicative factors corresponding to each power lawindex found in Table 2 of the Herschel technical notePICC-ME-TN-038. These factors were calculated by The
IRAS data reduction pipeline also assumes a power law spectralindex of − , which is the same as PACS and SPIRE. We did not use the
IRAS µ m flux as that is right on the peak ofthe SED, which would systematically underestimate the power lawindex. µ m flux to theinterpolated IRAS µ m flux as a function of the IRAS flux, shown in the bottom panel of Figure 7. The aver-age flux ratio represented by the red line is 1.001 witha - σ scatter of 0.04 (dashed lines), and the medianratio is 1.00. The agreement between the PACS and IRAS data in this case is exquisite, with an even tighterrelation than the 100 µ m comparison throughout theentire flux range.Another comparison is to perform a similar analysisusing GOALS data from the Spitzer
MIPS instrumentat 70 and 160 µ m (Mazzarella et al . µ m data will completely supersede the corre-sponding MIPS data.The results here are also similar to the analysis donein the Herschel technical note SAp-PACS-MS-0718-11, where extended source fluxes were compared be-tween PACS to
Spitzer -MIPS and
IRAS . Although theyfound an average PACS/IRAS 100 µ m flux ratio of1.32, their dispersion in the flux ratio is very similarto our results in Figure 7. We note that their analy-sis was done on HIPE 6, where the PACS responsivitywas not well understood resulting in much higher fluxratios than our result. Herschel PACS 100 µ m and IRAS 100 µ m Transmission Curve
60 80 100 120 140Wavelength ( µ m)0.00.20.40.60.81.0 N o r m a li ze d R e s p o n s e Fig. 6.— The normalized transmission curves of the100 µ m band passes for Herschel -PACS in blue and
IRAS in red.
To check the consistency of our SPIRE fluxes wecompared the measured fluxes of our SPIRE datareduced using three different SPIRE calibrations:
SPIRECAL 10 1 , SPIRECAL 13 1 , and the latestversion
SPIRECAL 14 2 . In Figure 8 we show sixhistograms of the fractional percentage change in fluxbetween each calibration version for each of the bands.In order to facilitate as direct of a comparison as pos-sible, we use the uncorrected fluxes computed directlyby the annularSkyAperturePhotometry taskin HIPE, which are not aperture or color corrected.The histograms show as a general trend towards longerwavelengths, a larger variance in the percent changein flux. This is again due to the long wavelengthRayleigh-Jeans tail of the galaxy’s SED, where thefainter fluxes are affected more by instrument uncer-tainties.In the histogram comparing
SPIRECAL 10 1 and
SPIRECAL 13 1 (Fig. 8, first column), the generaltrend is an increase in the measured flux by an un-weighted average of approximately 1.45%, 0.91%, and1.19% of the
SPIRECAL 13 1 flux, for the 250 µ m,350 µ m, and 500 µ m channels. The shape of the his-togram distribution is very close to Gaussian in eachcase, however the 250 µ m channel shows a slight pos-itive skewness. The main updates in the calibrationand data reduction pipeline are improved absolute fluxcalibrations of Neptune, and a better algorithm in de-striping the data and removal of image artifacts.In the second column of Figure 8 we show the his-togram of measured fluxes between SPIRECAL 13 1 ,and the latest version
SPIRECAL 14 2 . The onlychange was an update to the absolute flux calibrationof the instrument, which resulted in an even smallerchange in the average flux: 0.24%, –0.19%, and 0.25%for the 250 µ m, 350 µ m, and 500 µ m channels respec-tively. SPIRE maps reduced using the two previouscalibration versions are available upon request. In this section we detail several cautionary notes onusing the data presented in this paper.
By convention both of the PACS and SPIRE datareduction packages consider a flux calibration of theform νF ν = constant (i. e. a spectral index of − ). 264ince the Herschel photometry for the GOALS sam-ple covers a wide range of wavelengths, and thereforedifferent parts of the galaxy’s SED, the color correc-tion factor changes as a function of wavelength, as wellas weaker dependence on infrared luminosity (due to achange in the dust temperature). This is because the ef-fective beam area of each instrument changes slightlyfor different spectral indices. For PACS the color cor-rection factors are listed on the NHSC website , andare applied to the fluxes by dividing the factor for theappropriate power law exponent. The SPIRE colorcorrection factors are listed in the online SPIRE datareduction guide in Table 6.16 and are to be multi-plied .For this paper, we have decided to forego applying acolor correction for both PACS and SPIRE fluxes. Thiswould otherwise require a detailed analysis involving amulti-component SED fit for each galaxy to derive thespectral slope at each observed Herschel band, whichis outside the current scope of this paper. This deci-sion was agreed upon for both the
Herschel and
Spitzer (Mazzarella et al . ∼ , and for SPIRE bands up to ∼ for ex-tended sources, which is less than or equal to the abso-lute calibration uncertainty of both instruments. How-ever we note for point sources, the SPIRE color correc-tion can be higher, which we estimate to be ∼ fora spectral index of α = 4 . If a photometric precisionof within a few percent is desired, we strongly recom-mend users of the Herschel -GOALS data to includecolor corrections to the aperture photometry presentedin this paper.
Since galaxies within GOALS sample are verybright in the far-infrared, there is a small chance thatsome of our images exhibit saturation issues in a few ofour
Herschel maps. For the PACS photometer there aretwo types of saturations. Hard saturation occurs whenthe signal after the readout electronics are outside thedynamic range of the analog-to-digital converter. Onthe other hand soft saturation arises from saturation ofthe readout electronics itself. Taking into account botheffects, the point source saturation limits are 220 Jy, https://nhscsci.ipac.caltech.edu/pacs/docs/PACS photometer colorcorrectionfactors.txt http://herschel.esac.esa.int/hcss-doc-14.0/print/spire drg/spire drg.pdf
510 Jy, and 1125 Jy for the 70 µ m, 100 µ m, and 160 µ m passbands respectively.Fortunately for our sample, the latter two pass-bands have saturation limits well above our maximummeasured fluxes of 248 Jy and 301 Jy for the 100 µ m and 160 µ m channels. For the 70 µ m channel,the nearby galaxy F02401–0013 has a total measuredflux of 290 Jy which is above the saturation limit, andF06107+7822 which has a flux of 205 Jy and is closeto the saturation limit. However both appear very ex-tended at 70 µ m, and in checking the saturation masksin the time-ordered data cubes we found no significantnumber of pixels were masked due to saturation. Nine of our PACS maps exhibit residual correlatednoise resembling low-level ripples in both the scanand cross-scan directions for only the blue camera (70 µ m and 100 µ m). Of these maps three of them onlyhave this effect on the edges of the map, and do not af-fect the photometry or map quality. Unfortunately forthe other six maps the current processing techniquesin Jscanam, Unimap, and MADMap fail to remove it.One example of this is the 100 µ m map of F03316–3618. However we emphasize that these are very low-level effects, and do not significantly affect the qualityof the photometry , which we estimate to be on thefew percent level. This was calculated by first placingten random apertures on empty sky on each map, thenmeasuring the standard deviation in the flux per pixelon the affected maps. This is then multiplied by thenumber of pixels within the photometry aperture.
8. Summary
In this paper we have presented broad band
Her-schel imaging for the entire GOALS sample in Figure3. Total system fluxes, and component fluxes (wherepossible) are also computed in all six
Herschel bandsin Tables 3 and 4 respectively. Particular care wastaken in producing archival quality atlas maps usingthe best data reduction codes and algorithms availableat the time. The data presented here are thus far thehighest resolution, most sensitive and comprehensivefar-infrared imaging survey of the nearest luminous in-frared galaxies. For many of these objects, this paperpresents the first imaging data and reliable photometry These image artifacts are taken into account when calculating theuncertainty in flux. ∼ µ m in the submillimeterregime.1) All 201 GOALS objects were detected in allthree Herschel
PACS (70, 100, and 160 µ m) and allthree SPIRE (250, 350, 500 µ m) bands. The FOVof the PACS and SPIRE images are sufficient andsensitive enough to detect the full extent of the far-infrared emission for even the widest pair separations.Only two GOALS systems have full SPIRE cover-age but lack PACS coverage of a third distant com-ponent (NGC 2385 in F07256+3355, and NGC 7769in F23488+1949). In addition, four galaxies observedoutside of our Herschel program lack 100 µ m datasince they were not observed by those programs.2) The image quality of the data are superb andwere cleaned using the most up to date reduction rou-tines and calibration files from the Herschel
ScienceCenter. None of the images suffer from any saturationeffects, major striping, or other image quality issuesthat may arise from scan-based observations. Aperturecorrections were applied only to point sources, whileno color corrections were applied to any objects. Fur-thermore the SPIRE 350 µ m and 500 µ m maps werezero-point corrected using data from the Planck obser-vations.3) The resolution is sufficient to resolve individ-ual components of many pairs and interacting/mergingsystems in our sample, particularly at the shorter wave-lengths where the PACS 70 µ m FWHM band has abeamsize of . (cid:48)(cid:48) . On the other hand wider pairs canstill be resolved even at the longer wavelength SPIREbands.4) Comparing our PACS 70 and 100 µ m fluxes tothe legacy IRAS
60 and 100 µ m measurements respec-tively, we found an excellent agreement (to within er-ror) across our flux range as well as object morpholo-gies ranging from point sources to extended systems.5) The PACS 70 µ m and 160 µ m data within thispaper supersede the reported fluxes and maps fromthe MIPS instrument on Spitzer (see Mazzarella et al . Herschel data.In conjunction with datasets from other infraredtelescopes (i. e.
Spitzer , WISE), the
Herschel data fromthis paper will allow us for the first time to constructaccurate spectral energy distributions in the infrared( ∼ µ m) for the entire GOALS sample, whichwill be presented in several forthcoming papers. TheFITS files for the image mosaics constructed and pre- sented in this atlas are being made available in the In-frared Science Archive (IRSA) . Metadata for the im-ages are also being folded into the NASA/IPAC Ex-tragalactic Database (NED) to simplify searches incontext with other data in NED, including links to theFITS files at IRSA.
9. Acknowledgments
J. Chu gratefully acknowledges Laurie Chu forproofreading the manuscript, and Thomas Shimizu fordiscussions on reducing the
Herschel data. D.S. ac-knowledges the hospitality of the Aspen Center forPhysics, which is supported by the National Sci-ence Foundation Grant No. PHY-1066293. D.S. andK.L. also acknowledge the Distinguished Visitor Pro-gram at the Research School for Astronomy and As-trophysics, Australian National University for theirgenerous support while they were in residence at theMount Stromlo Observatory, Weston Creek, NSW.J.B., J.C., K.L. and D.S. gratefully acknowledge fund-ing support from NASA grant NNX11AB02G. G.C.P.was supported by a FONDECYT Postdoctoral Fellow-ship (No. 3150361). Support for this research was pro-vided by NASA through a GO Cycle 1 award issuedby JPL/Caltech. We thank the Observer Support groupof the NASA
Herschel
Science Center for patientlyhandling revisions and refinements of our AORs be-fore execution of the observations, and for their expertassistance in reducing the data. This paper has useddata from the
Planck mission, which is a project of theEuropean Space Agency in cooperation with the sci-entific community. ESA led the project, developed thesatellite, integrated the payload into it, and launchedand operated the satellite. This research has made ex-tensive use of the NASA/IPAC Extragalactic Database(NED) which is operated by the Jet Propulsion Labora-tory, California Institute of Technology, under contractwith the National Aeronautics and Space Administra-tion. We thank the anonymous referee whose com-ments helped us further improve our manuscript.Facilities:
Herschel (PACS),
Herschel (SPIRE),
Planck (HFI). http://irsa.ipac.caltech.edu/data/Herschel/GOALS/ http://ned.ipac.caltech.edu/ ) [Jy]0102030405060 G a l ax i e s N = 287Bin Size = 0.1S min = 0.0369 JyS max = 286 Jy −1 0 1 2 3log(S ) [Jy]0102030405060
N = 283Bin Size = 0.1S min = 0.0846 JyS max = 237 Jy −1 0 1 2 3log(S ) [Jy]01020304050 G a l ax i e s N = 272Bin Size = 0.1S min = 0.125 JyS max = 291 Jy −1 0 1 2 3log(S ) [Jy]010203040
N = 279Bin Size = 0.1S min = 0.111 JyS max = 118 Jy −1 0 1 2 3log(S ) [Jy]010203040 G a l ax i e s N = 271Bin Size = 0.1S min = 0.0583 JyS max = 45.7 Jy −2.0 −1.5 −1.0 −0.5 0.0 0.5 1.0log(S ) [Jy]01020304050
N = 261Bin Size = 0.1S min = 0.0230 JyS max = 15.6 Jy
Fig. 5.— Histogram plot of the
Herschel
PACS and SPIRE fluxes from our sample. The histogram range for eachband was fine tuned in order to meaningfully show the data. The fluxes shown here are all the actual measured fluxes,consisting of component and total fluxes. The x -axis of each panel is shown in units of log(Jy) to encompass the widedynamic range of fluxes measured within the data. 267 erschel−PACS to IRAS 100 µ m Flux Ratio µ m Flux0.60.81.01.21.4 H er s c h e l/ I RA S µ m F l u x R a t i o Herschel−PACS 70 µ m to IRAS 70 µ m interp. Flux Ratio µ m interp. Flux0.60.81.01.21.4 H er s c h e l / I RA S i n t er p . F l u x R a t i o Fig. 7.—
Upper panel : The
Herschel -PACS 100 µ m to IRAS µ m flux ratio plotted as a function of the IRAS µ m flux for 128 of our galaxies carefully chosen to be single objects, or if the system has multiple components theyare too close to be distinguishable by PACS at 100 µ m. These galaxies represent the entire spectrum of very extendedemission, to point sources as seen by PACS. The mean ratio represented by the red line is 1.012, with the dashed redlines representing the - σ scatter of 0.09. The median ratio is 1.006. There appears to be no significant systematicoffset, nor is there any evidence of a slope signifying a change in the flux ratio at different IRAS µ m flux. Errorbars were omitted to keep the plot readable. Lower panel : Same as the upper panel but for the
Herschel -PACS 70 µ m data compared to the interpolated IRAS 70 µ m flux. The mean ratio is 1.001 with a - σ scatter of 0.04, and amedian ratio of 1.00. The agreement between the PACS 70 µ m and interpolated IRAS µ m fluxes is excellent. 268 PIRE 250: 13_1 vs. 10_1SPIRE 250: 13_1 vs. 10_1 −30 −20 −10 0 10 20 30(S[13_1] − S[10_1]) / S[13_1] %01020304050 G a l ax i e s ∆ =1.45 % SPIRE 350: 13_1 vs. 10_1SPIRE 350: 13_1 vs. 10_1 −30 −20 −10 0 10 20 30(S[13_1] − S[10_1]) / S[13_1] %010203040 G a l ax i e s ∆ =0.91 % SPIRE 500: 13_1 vs. 10_1SPIRE 500: 13_1 vs. 10_1 −30 −20 −10 0 10 20 30(S[13_1] − S[10_1]) / S[13_1] %051015202530 G a l ax i e s ∆ =1.19 % SPIRE 250: 14_2 vs. 13_1SPIRE 250: 14_2 vs. 13_1 −30 −20 −10 0 10 20 30(S[14_2] − S[13_1]) / S[14_2] %01020304050 ∆ =0.24 % SPIRE 350: 14_2 vs. 13_1SPIRE 350: 14_2 vs. 13_1 −30 −20 −10 0 10 20 30(S[14_2] − S[13_1]) / S[14_2] %010203040 ∆ =−0.19 % SPIRE 500: 14_2 vs. 13_1SPIRE 500: 14_2 vs. 13_1 −30 −20 −10 0 10 20 30(S[14_2] − S[13_1]) / S[14_2] %051015202530 ∆ =0.25 % Fig. 8.— Histogram plots comparing the percent change in flux between
SPIRECAL 10 1 vs.
SPIRECAL 13 1 in the first column, and
SPIRECAL 13 1 vs.
SPIRECAL 14 2 in the second column. The values in each panelrepresent the unweighted average percent change between each calibration version. 269
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