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# Updated 34-band Photometry for the Sings/KINGFISH Samples of Nearby Galaxies

D. A. Dale, D. O. Cook, H. Roussel, J. A. Turner, L. Armus, A. D. Bolatto, M. Boquien, M. J. I. Brown, D. Calzetti, I. de Looze, et al.

► To cite this version:

D. A. Dale, D. O. Cook, H. Roussel, J. A. Turner, L. Armus, et al. Updated 34-band Photometry for the Sings/KINGFISH Samples of Nearby Galaxies. The Astrophysical Journal, 2017, 837, 10.3847/1538-4357/aa6032. insu-03746212

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https://insu.hal.science/insu-03746212v1

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Updated 34-band Photometry for the SINGS/KINGFISH Samples of Nearby Galaxies

D. A. Dale¹, D. O. Cook², H. Roussel³, J. A. Turner¹, L. Armus⁴, A. D. Bolatto⁵, M. Boquien⁶, M. J. I. Brown⁷, D. Calzetti⁸,
I. De Looze⁹, M. Galametz¹⁰,¹¹, K. D. Gordon¹², B. A. Groves¹³, T. H. Jarrett¹⁴, G. Helou⁴, R. Herrera-Camus¹⁵, J. L. Hinz¹⁶,
L. K. Hunt¹⁷, R. C. Kennicutt¹⁸, E. J. Murphy¹⁹, A. Rest¹², K. M. Sandstrom²⁰, J.-D. T. Smith²¹, F. S. Tabatabaei²², and
C. D. Wilson²³

¹ Department of Physics & Astronomy, University of Wyoming, Laramie WY, USA; ddale@uwyo.edu

² Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena CA, USA

³ Institut d'Astrophysique de Paris, Sorbonne Universités, Paris, France

⁴ Spitzer Science Center, California Institute of Technology, Pasadena, CA, USA

⁵ Department of Astronomy, University of Maryland, College Park, MD, USA

⁶ Unidad de Astronomía, Universidad de Antofagasta, Antofagasta, Chile

⁷ School of Physics & Astronomy, Monash University, Victoria 3800, Australia

⁸ Department of Astronomy, University of Massachusetts, Amherst MA, USA

⁹ Sterrenkundig Observatorium, Universiteit Gent, Gent, Belgium

¹⁰ European Southern Observatory, Garching, Germany

¹¹ Laboratoire AIM, CEA, Université Paris Diderot, IRFU/Service d'Astrophysique, Gif-sur-Yvette, France

¹² Space Telescope Science Institute, Baltimore MD, USA

¹³ Research School of Astronomy & Astrophysics, Australian National University, Canberra, Australia

¹⁴ Astronomy Department, University of Capetown, Rondebosch, South Africa

¹⁵ Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany

¹⁶ Steward Observatory, University of Arizona, Tucson AZ, USA

¹⁷ INAF—Osservatorio Astrofisico di Arcetri, Firenze, Italy

¹⁸ Institute of Astronomy, University of Cambridge, Cambridge, UK

¹⁹ National Radio Astronomy Observatory, Charlottesville, VA, USA

²⁰ Center for Astrophysics and Space Science, University of California, San Diego CA, USA

²¹ Department of Physics & Astronomy, University of Toledo, Toledo, OH, USA

²² Instituto de Astrofísica de Canarias, La Laguna, Spain

²³ Department of Physics & Astronomy, McMaster University, Hamilton, Ontario, Canada

Received 2016 December 5; revised 2017 February 8; accepted 2017 February 10; published 2017 March 7

Abstract

We present an update to the ultraviolet-to-radio database of global broadband photometry for the 79 nearby galaxies that comprise the union of the KINGFISH (Key Insights on Nearby Galaxies: A Far-Infrared Survey with Herschel) and SINGS (Spitzer Infrared Nearby Galaxies Survey) samples. The 34-band data set presented here includes contributions from observational work carried out with a variety of facilities including GALEX, SDSS, Pan-STARRS1, NOAO, 2MASS, Wide-Field Infrared Survey Explorer, Spitzer, Herschel, Planck, JCMT, and the VLA. Improvements of note include recalibrations of previously published SINGS $BVR_{Cl}$ and KINGFISH far-infrared/submillimeter photometry. Similar to previous results in the literature, an excess of submillimeter emission above model predictions is seen primarily for low-metallicity dwarf or irregular galaxies. This 33-band photometric data set for the combined KINGFISH+SINGS sample serves as an important multiwavelength reference for the variety of galaxies observed at low redshift. A thorough analysis of the observed spectral energy distributions is carried out in a companion paper.

**Key words:** galaxies: photometry – galaxies: ISM – infrared: ISM – ISM: general

**Supporting material:** extended figure

1. Introduction

Access to panchromatic broadband photometry for galaxies
is crucial to fully understanding the characteristics of, and
relative contributions to, galaxy spectra from the various
processes related to interstellar attenuation, star formation, and
the feeding of supermassive black holes (Silva et al. 1998; da
Cunha et al. 2008; M. Boquien 2016, in preparation). Although
a fairly complete multiwavelength data set has been published
for the SINGS (Spitzer Infrared Nearby Galaxies Survey)
sample of 75 nearby galaxies (Kennicutt et al. 2003; Dale et al.
2005, 2007), subsequent far-infrared/submillimeter Herschel
broadband data were later published for the KINGFISH (Key
Insights on Nearby Galaxies: A Far-Infrared Survey with
Herschel) sample of 61 nearby galaxies (Kennicutt et al. 2011;
Dale et al. 2012), a sample for which 57 of the 61 targets are
also SINGS targets. The photometric data sets from the

combined SINGS/KINGFISH surveys have served as impor-
tant references for studies seeking to understand the diverse
properties of galaxies in the Local Universe (da Cunha et al.
2008; Noll et al. 2009; Jonsson et al. 2010; Rémy-Ruyer et al.
2015), or to serve as redshift-zero comparison samples to
higher redshift galaxies (Kartaltepe et al. 2010; Maiolino et al.
2015; Scoville et al. 2016).

In this effort we present an update to the global (spatially
integrated) photometry for the 79 nearby galaxies that comprise
the union of the KINGFISH and SINGS samples. This update
includes a recalibration of the Dale et al. (2012) KINGFISH
far-infrared/submillimeter photometry, necessary since the
calibration of the Herschel photometers has undergone multiple
revisions since those data were first published. We also carry
out a Pan-STARRS1-based recalibration of the $BVR_{Cl}$ fluxes
previously published in Dale et al. (2007). A portion of these
ground-based broadband optical data is suspect, since the data were originally taken in non-photometric conditions, and the ensuing attempts to calibrate the non-photometric frames were insufficient. We also include new ugriz and 12 µm photometry from the Sloan Digital Sky Survey (SDSS) and the Wide-Field Infrared Survey Explorer (WISE) mission, respectively. In addition, the Herschel PACS photometry for KINGFISH galaxy NGC 0584 was not included in Dale et al. (2012) since these imaging data were not yet taken. Furthermore, we include new Herschel photometry for six SINGS galaxies from the Herschel Very Nearby Galaxy Survey (PI C. Wilson) that are not in the KINGFISH sample (NGC 2403, M81 = NGC 3031, M82 = NGC 3034, NGC 4125, M51a = NGC 5194, and M51b = NGC 5195). Finally, we complete the presentation of a multiwavelength database by including previously published global photometry from ultraviolet (GALEX), infrared/submillimeter (2MASS, Spitzer, SCUBA), and radio (VLA) wavelengths.

Section 2 provides a brief overview of the galaxy sample, Section 3 recapitulates the relevant observations and approaches to data processing, Section 4 describes the salient results, and Section 5 provides the summary. The companion paper (L.K. Hunt et al. 2017, in preparation) explores the observed spectral energy distributions (SEDs) by using and comparing fits employing three popular fitting tools: GRASIL, MAGPHYS, and CIGALE (Silva et al. 1998; da Cunha et al. 2008; Noll et al. 2009).

## 2. Galaxy Sample

Table 1 presents the full list of 79 galaxies that form the union of the SINGS and KINGFISH samples. The sample was chosen to be a representative sampling of the Local Universe; the sample is not volume limited and thus does not represent a statistical sampling of the Local Volume, but the sample is representative of the diversity of local galaxies. These galaxies were selected to span a range of morphologies, colors, and luminosities (e.g., Figures 5 and 3 of Kennicutt et al. 2003; Dale et al. 2012, respectively). Figure 1 demonstrates the sample’s range of optical colors and near-infrared luminosities; a few galaxies reside in the red sequence near the top of the diagram, but most of the sample spans the blue star-forming sequence. The sample is comprised of 8%, 11%, 63%, and 18% early-type, lenticular, spiral, and irregular galaxies, respectively, based on the optical morphologies provided in the NASA/IPAC Extragalactic Database (NED). This galaxy sample has no sources for which the optical luminosity is dominated by AGN emission, although one-third have signatures of Seyfert/LINER nuclei (Tajer et al. 2005; Dale et al. 2006; Moustakas et al. 2010; Grier et al. 2011). There are only a few galaxies that are undoubtedly interacting with neighboring galaxies, including NGC 5194 (with NGC 5195), NGC 1097 (with NGC 1097A), NGC 1316 (with NGC 1317), and NGC 3190 (with NGC 3187). The distances reach out to ~30 Mpc with a median value of ~10 Mpc.

## 3. Observations and Data Processing

Much of the photometry presented here has already been described in Dale et al. (2007, 2012), therefore we focus the following discussion on important differences from what is presented in those publications. The imaging bandpasses used here are listed in the heading of Table 2. The central

wavelengths and widths of the filters are computed via

$$ \bar{\lambda} = \frac{\int \lambda T(\lambda) d\lambda}{\int T(\lambda) d\lambda} \qquad (1) $$

and

$$ \Delta = \int \mathcal{T}(\lambda) d\lambda, \qquad (2) $$

where $\mathcal{T}$ represents the filter transmittance normalized to peak at unity, based on the filter profiles compiled by Noll et al. (2009) for use in the CIGALE software package (Noll et al. 2009).

### 3.1. Ground-based Optical

Some of the optical $BVR_{CIC}$ photometry from Dale et al. (2007) suffers from faulty calibration (Muñoz-Mateos et al. 2009). Sometimes insufficient numbers of standard star observations were taken, sometimes the standards were saturated, and some of the frames taken in non-photometric conditions were not successfully calibrated a posteriori. A recalibration is carried out here via comparison of photometry on foreground stars in Pan-STARRS1 (PS1) $g_{PS1}l_{PS1}i_{PS1}z_{PS1}$ and in our 2007-era $BVR_{CIC}$ imaging. The PS1 3$\pi$ Survey uses the 1.8 m telescope on Mount Haleakala to map the sky north of $\delta = -30^{\circ}$ with multiple passes of 30–60 s exposures in each of their five SDSS-like filters (Schlafly et al. 2012; Magnier et al. 2013).

Care was taken in the comparison to only use bright ($r_{PS1} < 19$ mag), unsaturated sources with point-spread functions (PSFs) that agree with the seeing profiles of each image (i.e., background galaxies are excluded). The median number of foreground stars per galaxy used for this purpose was 15. Aperture diameters for the foreground stellar photometry were typically 7"; increasing the aperture diameter by 50% results in a <1% difference in the calibration. The PS1 fluxes were converted from their measured values at 1.2 airmasses into 0 airmasses (Table 4 of Tonry et al. 2012), and the small (tens of millimag) corrections suggested by Scolnic et al. (2015) were incorporated (see their Table 3); the small calibration modifications of Scolnic et al. (2015) are based on a “super calibration” that combines flux measurements of secondary standards from several surveys including PS1 and SDSS.

We adopted the Tonry et al. (2012) quadratic filter transformations for stars between Pan-STARRS1 $g_{PS1}l_{PS1}i_{PS1}z_{PS1}$ and $BVR_{CIC}$, although very similar results are obtained when using linear transformations between SDSS and Johnson/Cousins filters (Jester et al. 2005; Lupton et al. 2005; Jordi et al. 2006; Chonis & Gaskell 2008; Tonry et al. 2012). The only significant outliers for any of these various stellar transformations are the Chonis & Gaskell (2008) V and Lupton et al. (2005) $R_C$ linear transformations, both of which yield calibrations that ultimately result in galaxy fluxes that are 25%–30% (~0.25–0.30 mag) brighter compared to when using other published transformations. The photometric calibrations are derived in practice from the error-weighted differences between the instrumental $BVR_{CIC}$ fluxes and the measured PS1 fluxes (transformed to $BVR_{CIC}$) for the suite of suitable foreground stars identified for each galaxy. The dispersions in these bootstrap calibrations range from 2% to 15% (with a median of 5%) and contribute to the overall photometric uncertainty estimates; the photometric uncertainties for the PS1-recalibrated fluxes are the sums in quadrature of these dispersions along with the uncertainties in the published
<table><caption>Table 1
Galaxy Sample</caption><thead><tr><th>Galaxy</th><th>Alternative Name</th><th>Optical Morph.</th><th>E(B-V) (mag.)</th><th>α<sub>0</sub> and δ<sub>0</sub> (J2000)</th><th>2a (")</th><th>2b (")</th><th>PA (°)</th><th>D (Mpc)</th><th>TIR (L<sub>☉</sub>)</th></tr></thead><tbody><tr><td>NGC 0024</td><td>UGC A002</td><td>SAc</td><td>0.017</td><td>000955.9-245755</td><td>301</td><td>216</td><td>45</td><td>8.20</td><td>8.8</td></tr><tr><td>NGC 0337</td><td>NGC 0337</td><td>SBd</td><td>0.096</td><td>005950.7-073444</td><td>253</td><td>194</td><td>140</td><td>19.30</td><td>10.1</td></tr><tr><td>NGC 0584</td><td>NGC 0584</td><td>E4</td><td>0.036</td><td>013120.6-065205</td><td>326</td><td>278</td><td>60</td><td>20.80</td><td>8.7</td></tr><tr><td>NGC 0628</td><td>Messier 074</td><td>SAc</td><td>0.060</td><td>013642.4+154711</td><td>879</td><td>808</td><td>90</td><td>7.20</td><td>9.9</td></tr><tr><td>NGC 0855</td><td>UGC 01718</td><td>E</td><td>0.061</td><td>021403.7+275237</td><td>259</td><td>169</td><td>60</td><td>9.73</td><td>8.6</td></tr><tr><td>NGC 0925</td><td>UGC 01913</td><td>SABd</td><td>0.065</td><td>022713.6+333504</td><td>735</td><td>486</td><td>105</td><td>9.12</td><td>9.7</td></tr><tr><td>NGC 1097</td><td>UGC A041</td><td>SBb</td><td>0.023</td><td>024618.0-301642</td><td>758</td><td>612</td><td>130</td><td>14.20</td><td>10.6</td></tr><tr><td>NGC 1266</td><td>NGC 1266</td><td>SB0</td><td>0.085</td><td>031600.6-022541</td><td>234</td><td>232</td><td>0</td><td>30.60</td><td>10.4</td></tr><tr><td>NGC 1291</td><td>NGC 1291</td><td>SB0/a</td><td>0.011</td><td>031717.9-410616</td><td>884</td><td>836</td><td>90</td><td>10.40</td><td>9.5</td></tr><tr><td>NGC 1316</td><td>FornaxA</td><td>SAB0</td><td>0.018</td><td>032241.2-371210</td><td>864</td><td>583</td><td>50</td><td>21.00</td><td>9.9</td></tr><tr><td>NGC 1377</td><td>NGC 1377</td><td>S0</td><td>0.024</td><td>033639.0-205408</td><td>181</td><td>162</td><td>90</td><td>24.60</td><td>10.1</td></tr><tr><td>NGC 1404</td><td>NGC 1404</td><td>E1</td><td>0.010</td><td>033852.3-353540</td><td>524</td><td>369</td><td>149</td><td>20.20</td><td>...</td></tr><tr><td>IC0342</td><td>UGC 02847</td><td>SABcd</td><td>0.480</td><td>034659.5+680539</td><td>1667</td><td>1439</td><td>100</td><td>3.28</td><td>10.1</td></tr><tr><td>NGC 1482</td><td>NGC 1482</td><td>SA0</td><td>0.034</td><td>035439.0-203009</td><td>349</td><td>310</td><td>119</td><td>22.60</td><td>10.6</td></tr><tr><td>NGC 1512</td><td>NGC 1512</td><td>SBab</td><td>0.009</td><td>040355.6-432149</td><td>1001</td><td>928</td><td>83</td><td>11.60</td><td>9.5</td></tr><tr><td>NGC 1566</td><td></td><td>SABbc</td><td>0.008</td><td>042000.4-545615</td><td>552</td><td>435</td><td>40</td><td>18.00</td><td>10.6</td></tr><tr><td>NGC 1705</td><td></td><td>SA0</td><td>0.007</td><td>045413.5-532137</td><td>167</td><td>120</td><td>40</td><td>5.80</td><td>8.0</td></tr><tr><td>NGC 2146</td><td>UGC 03429</td><td>SAb</td><td>0.082</td><td>061835.6+782129</td><td>236</td><td>235</td><td>120</td><td>17.20</td><td>11.0</td></tr><tr><td>NGC 2403</td><td>UGC 03918</td><td>SABcd</td><td>0.034</td><td>073655.1+653534</td><td>1512</td><td>929</td><td>124</td><td>3.50</td><td>9.6</td></tr><tr><td>HolmbergII</td><td>UGC 04305</td><td>Im</td><td>0.027</td><td>081910.8+704320</td><td>554</td><td>465</td><td>60</td><td>3.05</td><td>7.8</td></tr><tr><td>M081DwarfA</td><td></td><td>I?</td><td>0.018</td><td>082356.0+710145</td><td>78</td><td>78</td><td>90</td><td>3.50</td><td>...</td></tr><tr><td>DDO 053</td><td>UGC 04459</td><td>Im</td><td>0.033</td><td>083407.4+661043</td><td>155</td><td>142</td><td>90</td><td>3.61</td><td>7.0</td></tr><tr><td>NGC 2798</td><td>UGC 04905</td><td>SBa</td><td>0.017</td><td>091723.1+415957</td><td>235</td><td>232</td><td>90</td><td>25.80</td><td>10.6</td></tr><tr><td>NGC 2841</td><td>UGC 04966</td><td>SAb</td><td>0.013</td><td>092203.3+505837</td><td>629</td><td>334</td><td>150</td><td>14.10</td><td>10.1</td></tr><tr><td>NGC 2915</td><td></td><td>I0</td><td>0.236</td><td>092609.4-763736</td><td>183</td><td>132</td><td>110</td><td>3.78</td><td>7.6</td></tr><tr><td>HolmbergI</td><td>UGC 05139</td><td>IABm</td><td>0.044</td><td>094033.6+711120</td><td>264</td><td>219</td><td>63</td><td>3.90</td><td>7.1</td></tr><tr><td>NGC 2976</td><td>UGC 05221</td><td>SAc</td><td>0.062</td><td>094715.3+675509</td><td>541</td><td>353</td><td>144</td><td>3.55</td><td>8.9</td></tr><tr><td>NGC 3049</td><td>UGC 05325</td><td>SBab</td><td>0.033</td><td>095449.6+091614</td><td>218</td><td>160</td><td>29</td><td>19.20</td><td>9.5</td></tr><tr><td>NGC 3031</td><td>Messier 081</td><td>SAab</td><td>0.069</td><td>095531.8+690403</td><td>1628</td><td>1122</td><td>154</td><td>3.50</td><td>9.6</td></tr><tr><td>NGC 3034</td><td>Messier 082</td><td>I0</td><td>0.134</td><td>095552.1+694057</td><td>698</td><td>581</td><td>65</td><td>3.50</td><td>10.8</td></tr><tr><td>HolmbergIX</td><td>UGC 05336</td><td>Im</td><td>0.068</td><td>095729.2+690250</td><td>247</td><td>180</td><td>40</td><td>3.50</td><td>...</td></tr><tr><td>NGC 3077</td><td>UGC 05398</td><td>I0pec</td><td>0.058</td><td>100317.5+684354</td><td>488</td><td>436</td><td>64</td><td>3.83</td><td>8.9</td></tr><tr><td>M081DwarfB</td><td>UGC 05423</td><td>Im</td><td>0.068</td><td>100531.2+702151</td><td>134</td><td>90</td><td>139</td><td>3.60</td><td>6.5</td></tr><tr><td>NGC 3190</td><td>UGC 05559</td><td>SAap</td><td>0.022</td><td>101805.7+214957</td><td>334</td><td>196</td><td>117</td><td>19.30</td><td>9.8</td></tr><tr><td>NGC 3184</td><td>UGC 05557</td><td>SABcd</td><td>0.014</td><td>101815.6+412542</td><td>614</td><td>538</td><td>169</td><td>11.70</td><td>10.0</td></tr><tr><td>NGC 3198</td><td>UGC 05572</td><td>SBc</td><td>0.011</td><td>101954.8+453301</td><td>518</td><td>315</td><td>35</td><td>14.10</td><td>10.0</td></tr><tr><td>IC2574</td><td>UGC 05666</td><td>SABm</td><td>0.031</td><td>102823.9+682505</td><td>864</td><td>486</td><td>59</td><td>3.79</td><td>8.3</td></tr><tr><td>NGC 3265</td><td>UGC 05705</td><td>E</td><td>0.021</td><td>103106.8+284751</td><td>184</td><td>175</td><td>50</td><td>19.60</td><td>9.4</td></tr><tr><td>Mrk 33</td><td>UGC 05720</td><td>Im</td><td>0.010</td><td>103231.2+542359</td><td>181</td><td>177</td><td>90</td><td>21.70</td><td>9.8</td></tr><tr><td>NGC 3351</td><td>Messier 095</td><td>SBb</td><td>0.024</td><td>104358.1+114210</td><td>592</td><td>441</td><td>11</td><td>9.33</td><td>9.9</td></tr><tr><td>NGC 3521</td><td>UGC 06150</td><td>SABbc</td><td>0.049</td><td>110548.1-000127</td><td>926</td><td>455</td><td>165</td><td>11.20</td><td>10.5</td></tr><tr><td>NGC 3621</td><td>UGC A232</td><td>SAd</td><td>0.069</td><td>111818.3-324855</td><td>791</td><td>555</td><td>160</td><td>6.55</td><td>9.9</td></tr><tr><td>NGC 3627</td><td>Messier 066</td><td>SABb</td><td>0.029</td><td>112013.4+125927</td><td>745</td><td>486</td><td>167</td><td>9.38</td><td>10.4</td></tr><tr><td>NGC 3773</td><td>UGC 06605</td><td>SA0</td><td>0.023</td><td>113813.1+120644</td><td>118</td><td>116</td><td>0</td><td>12.40</td><td>8.8</td></tr><tr><td>NGC 3938</td><td>UGC 06856</td><td>SAc</td><td>0.018</td><td>115250.3+440715</td><td>504</td><td>468</td><td>0</td><td>17.90</td><td>10.3</td></tr><tr><td>NGC 4125</td><td>UGC 07118</td><td>E6p</td><td>0.016</td><td>120805.8+651024</td><td>228</td><td>151</td><td>90</td><td>21.40</td><td>9.1</td></tr><tr><td>NGC 4236</td><td>UGC 07306</td><td>SBdm</td><td>0.013</td><td>121643.2+692719</td><td>1240</td><td>369</td><td>162</td><td>4.45</td><td>8.7</td></tr><tr><td>NGC 4254</td><td>Messier 099</td><td>SAc</td><td>0.033</td><td>121849.7+142519</td><td>519</td><td>420</td><td>60</td><td>14.40</td><td>10.6</td></tr><tr><td>NGC 4321</td><td>Messier 100</td><td>SABbc</td><td>0.023</td><td>122254.8+154907</td><td>558</td><td>483</td><td>40</td><td>14.30</td><td>10.5</td></tr><tr><td>NGC 4450</td><td>UGC 07594</td><td>SAab</td><td>0.024</td><td>122830.1+170454</td><td>401</td><td>284</td><td>180</td><td>20.00</td><td>9.9</td></tr><tr><td>NGC 4536</td><td>UGC 07732</td><td>SABbc</td><td>0.016</td><td>123427.5+021113</td><td>454</td><td>376</td><td>120</td><td>14.50</td><td>10.3</td></tr><tr><td>NGC 4552</td><td>Messier 089</td><td>E</td><td>0.035</td><td>123539.8+123323</td><td>306</td><td>306</td><td>90</td><td>4.90</td><td>7.7</td></tr><tr><td>NGC 4559</td><td>UGC 07766</td><td>SABcd</td><td>0.015</td><td>123558.1+275752</td><td>576</td><td>327</td><td>140</td><td>6.98</td><td>9.5</td></tr><tr><td>NGC 4569</td><td>Messier 090</td><td>SABab</td><td>0.040</td><td>123650.2+131001</td><td>593</td><td>327</td><td>21</td><td>9.86</td><td>9.7</td></tr><tr><td>NGC 4579</td><td>Messier 058</td><td>SABb</td><td>0.035</td><td>123743.8+114858</td><td>325</td><td>271</td><td>90</td><td>16.40</td><td>10.1</td></tr><tr><td>NGC 4594</td><td>Messier 104</td><td>SAa</td><td>0.044</td><td>123959.6-113726</td><td>767</td><td>669</td><td>90</td><td>9.08</td><td>9.5</td></tr><tr><td>NGC 4625</td><td>UGC 07861</td><td>SABmp</td><td>0.016</td><td>124154.8+411623</td><td>298</td><td>214</td><td>100</td><td>9.30</td><td>8.8</td></tr><tr><td>NGC 4631</td><td>UGC 07865</td><td>SBd</td><td>0.015</td><td>124204.2+323219</td><td>901</td><td>240</td><td>85</td><td>7.62</td><td>10.4</td></tr><tr><td>NGC 4725</td><td>UGC 07989</td><td>SABab</td><td>0.010</td><td>125027.7+252948</td><td>689</td><td>523</td><td>30</td><td>11.90</td><td>9.9</td></tr><tr><td>NGC 4736</td><td>Messier 094</td><td>SAab</td><td>0.015</td><td>125055.2+410652</td><td>944</td><td>899</td><td>0</td><td>4.66</td><td>9.8</td></tr><tr><td>DDO 154</td><td>UGC 08024</td><td>IBm</td><td>0.008</td><td>125407.6+270916</td><td>216</td><td>126</td><td>50</td><td>4.30</td><td>...</td></tr><tr><td>NGC 4826</td><td>Messier 064</td><td>SAab</td><td>0.036</td><td>125643.3+214048</td><td>716</td><td>427</td><td>114</td><td>5.27</td><td>9.6</td></tr><tr><td>DDO 165</td><td>UGC 08201</td><td>Im</td><td>0.021</td><td>130625.9+674229</td><td>263</td><td>161</td><td>90</td><td>4.57</td><td>...</td></tr></tbody></table>
<table><caption>**Table 1**
(Continued)</caption><thead><tr><th>Galaxy</th><th>Alternative Name</th><th>Optical Morph.</th><th>E(B-V) (mag.)</th><th>α<sub>0</sub> and δ<sub>0</sub> (J2000)</th><th>2a (")</th><th>2b (")</th><th>PA (°)</th><th>D (Mpc)</th><th>TIR (L<sub>c</sub>)</th></tr></thead><tbody><tr><td>NGC 5033</td><td>UGC 08307</td><td>SAc</td><td>0.010</td><td>131328.2+363534</td><td>729</td><td>467</td><td>180</td><td>13.30</td><td>10.3</td></tr><tr><td>NGC 5055</td><td>Messier 063</td><td>SAbc</td><td>0.015</td><td>131549.2+420147</td><td>1097</td><td>711</td><td>80</td><td>7.94</td><td>10.3</td></tr><tr><td>NGC 5194</td><td>Messier 051a</td><td>SABbc</td><td>0.030</td><td>132950.6+471307</td><td>1699</td><td>1129</td><td>15</td><td>8.20</td><td>10.6</td></tr><tr><td>NGC 5195</td><td>Messier 051b</td><td>SB0p</td><td>0.031</td><td>132959.4+471556</td><td>202</td><td>191</td><td>0</td><td>8.20</td><td>9.3</td></tr><tr><td>NGC 5398</td><td>Tololo89</td><td>SBdm</td><td>0.056</td><td>140121.2-330402</td><td>198</td><td>146</td><td>0</td><td>7.66</td><td>8.6</td></tr><tr><td>NGC 5457</td><td>Messier 101</td><td>SABcd</td><td>0.007</td><td>140325.0+542429</td><td>1800</td><td>1446</td><td>37</td><td>6.70</td><td>10.3</td></tr><tr><td>NGC 5408</td><td></td><td>IBm</td><td>0.059</td><td>140321.1-412241</td><td>256</td><td>209</td><td>67</td><td>4.80</td><td>8.3</td></tr><tr><td>NGC 5474</td><td>UGC 09013</td><td>SAc</td><td>0.009</td><td>140500.8+533920</td><td>412</td><td>373</td><td>90</td><td>6.80</td><td>8.7</td></tr><tr><td>NGC 5713</td><td>UGC 09451</td><td>SABbcp</td><td>0.034</td><td>144011.4-001726</td><td>225</td><td>225</td><td>90</td><td>21.40</td><td>10.5</td></tr><tr><td>NGC 5866</td><td>UGC 09723</td><td>S0</td><td>0.012</td><td>150628.8+554551</td><td>500</td><td>306</td><td>129</td><td>15.30</td><td>9.7</td></tr><tr><td>IC4710</td><td></td><td>SBm</td><td>0.076</td><td>182838.9-665903</td><td>313</td><td>219</td><td>120</td><td>8.50</td><td>8.6</td></tr><tr><td>NGC 6822</td><td>DDO 229</td><td>IBm</td><td>0.199</td><td>194453.2-144811</td><td>1453</td><td>1100</td><td>150</td><td>0.60</td><td>7.9</td></tr><tr><td>NGC 6946</td><td>UGC 11597</td><td>SABcd</td><td>0.294</td><td>203449.2+600959</td><td>953</td><td>928</td><td>0</td><td>6.80</td><td>10.5</td></tr><tr><td>NGC 7331</td><td>UGC 12113</td><td>SAb</td><td>0.078</td><td>223704.3+342435</td><td>683</td><td>335</td><td>168</td><td>14.50</td><td>10.7</td></tr><tr><td>NGC 7552</td><td>IC5294</td><td>SAc</td><td>0.012</td><td>231610.8-423505</td><td>441</td><td>325</td><td>120</td><td>22.30</td><td>11.0</td></tr><tr><td>NGC 7793</td><td></td><td>SAd</td><td>0.017</td><td>235749.9-323525</td><td>716</td><td>526</td><td>98</td><td>3.91</td><td>9.3</td></tr></tbody></table>

Note. Foreground extinctions derive from Schlafly & Finkbeiner (2011). 2a and 2b are the lengths of the major and minor axes used in the elliptical aperture photometry described herein; the position angle of the aperture's major axis is measured east of north. The total infrared luminosity listed in the last column is derived from Equation (5) of Dale et al. (2014) and the *Spitzer* 8, 24, 70, and 160 µm fluxes in Table 2 and assumes the distances provided in this table. *WISE* 22 µm and *Herschel* PACS 70 and 160 µm fluxes are used for NGC 3034 since its MIPS data suffer from saturation.

<figure><img src="image_4.png" /><figcaption>**Figure 1.** Comparison of global *g-r* colors and absolute 2MASS *Ks* magnitudes for the KINGFISH/SINGS (large circles) and SDSS low-redshift samples (10 < *d* < 150 Mpc *h*⁻¹; Blanton et al. 2005). The values are corrected for foreground Milky Way extinction.</figcaption></figure>

*g*<sub>PS1</sub>*r*<sub>PS1</sub>*i*<sub>PS1</sub>*z*<sub>PS1</sub> → *BVR*<sub>CIC</sub> transformations and the instrumental galaxy flux measurements.

The Pan-STARRS1 survey does not encompass regions of the sky south of Galactic latitude $\delta = -30^\circ$, and thus PS1 calibration is not possible for 18 SINGS/KINGFISH objects. Table 3 indicates for which targets the *BVR*<sub>CIC</sub> photometry has been recalibrated via PS1. Additional broadband optical photometry is possible via other ground-based efforts. SDSS *ugriz* imaging (Data Release 12) is used to provide optical fluxes for 51 of the 79 SINGS/KINGFISH galaxies. The union of the SDSS *ugriz* and PS1-recalibrated *BVR*<sub>CIC</sub>

samples comprises 63 galaxies, hence 80% of the full sample. The fraction of the sample for which we have reliable optical photometry approaches 100% after inclusion of *BVR*<sub>CIC</sub> photometry from other global photometric data sets (see Table 3 and de Vaucouleurs et al. 1991; Muñoz-Mateos et al. 2009; Tully et al. 2009; Cook et al. 2014).

Other differences between our *BVR*<sub>CIC</sub> photometry and those appearing in Dale et al. (2007) include the use of SINGS Data Release 5 (DR5) images (DR2 imaging was used in the previous publication), more robust sky level determinations (i.e., a significantly larger number of sky pixels are now used—38% more on average), and a fresh take on the editing of foreground stars and background galaxies (see Section 3.5). In some instances the DR5 images are noticeably flatter than their DR2 counterparts (e.g., NGC 0628 *VR*<sub>CIC</sub>). Otherwise, the data-processing procedures are essentially identical to those already described in Dale et al. (2007).

## 3.2. Herschel Infrared

Fluxes based on *Herschel* PACS and SPIRE imaging are presented here for 67 of the 79 SINGS/KINGFISH galaxies. The *Herschel* PACS and SPIRE imaging observations are described in Dale et al. (2012) for the 61 KINGFISH galaxies, except for the PACS observations of NGC 0584, which were taken too late to appear in that publication. Another minor difference from Dale et al. (2012) is that the PACS maps used here are deeper for five KINGFISH objects since we have now incorporated additional data from other observing programs: Holmberg II, IC 2574, NGC 2798, NGC 4236, and NGC 4631. Deeper observations allow for more robust measurements, e.g., the 70 and 100 µm flux-to-uncertainty ratios for Holmberg II are a factor of two larger than published in Dale et al. (2012) (see Section 4). We also incorporate here new *Herschel* imaging observations for 6 SINGS galaxies from the *Herschel* Very Nearby Galaxy Survey (VNGS; PI C. Wilson) that are not in the KINGFISH sample: NGC 2403, M81 = NGC 3031, M82 = NGC 3034, NGC 4125, M51a = NGC 5194, and M51b = NGC 5195. The observing
<table><caption>Table 2
Global Flux Densities in Jansky's Corrected for neither Galactic nor Intrinsic Extinction</caption><thead><tr><th>Filter</th><th>GALEX<br>FUV</th><th>GALEX<br>NUV</th><th>B</th><th>V</th><th>R<sub>C</sub></th><th>I<sub>C</sub></th><th>SDSS<br>u</th><th>SDSS<br>g</th><th>SDSS<br>r</th><th>SDSS<br>i</th></tr></thead><tbody><tr><td>λ&#773;(μm)</td><td>0.154</td><td>0.231</td><td>0.441</td><td>0.551</td><td>0.659</td><td>0.806</td><td>0.356</td><td>0.482</td><td>0.626</td><td>0.767</td></tr><tr><td>Δλ(μm)</td><td>0.025</td><td>0.073</td><td>0.096</td><td>0.089</td><td>0.159</td><td>0.150</td><td>0.056</td><td>0.127</td><td>0.133</td><td>0.135</td></tr><tr><td>A<sub>λ</sub>/A<sub>V</sub></td><td>2.586</td><td>2.994</td><td>1.310</td><td>1.0</td><td>0.788</td><td>0.577</td><td>1.642</td><td>1.219</td><td>0.849</td><td>0.641</td></tr><tr><td>NGC 0024</td><td>772 ± 121E-3</td><td>981 ± 149E-3</td><td>817 ± 021E-2</td><td>108 ± 002E-1</td><td>138 ± 007E-1</td><td>183 ± 007E-1</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 0337</td><td>463 ± 064E-3</td><td>819 ± 113E-3</td><td>786 ± 046E-2</td><td>908 ± 044E-2</td><td>108 ± 006E-1</td><td>139 ± 015E-1</td><td>249 ± 006E-2</td><td>664 ± 014E-2</td><td>100 ± 002E-1</td><td>121 ± 002E-1</td></tr><tr><td>NGC 0584</td><td>274 ± 039E-4</td><td>146 ± 020E-3</td><td>130 ± 014E-1</td><td>264 ± 020E-1</td><td>346 ± 039E-1</td><td>519 ± 048E-1</td><td>292 ± 007E-2</td><td>143 ± 002E-1</td><td>296 ± 006E-1</td><td>433 ± 008E-1</td></tr><tr><td>NGC 0628</td><td>469 ± 073E-2</td><td>591 ± 091E-2</td><td>528 ± 033E-1</td><td>721 ± 033E-1</td><td>921 ± 042E-1</td><td>118 ± 006E+0</td><td>179 ± 003E-1</td><td>492 ± 009E-1</td><td>804 ± 016E-1</td><td>108 ± 002E+0</td></tr><tr><td>NGC 0855</td><td>920 ± 144E-4</td><td>178 ± 027E-3</td><td>204 ± 020E-2</td><td>335 ± 033E-2</td><td>457 ± 012E-2</td><td>...</td><td>840 ± 029E-3</td><td>268 ± 006E-2</td><td>468 ± 010E-2</td><td>633 ± 013E-2</td></tr><tr><td>NGC 0925</td><td>293 ± 040E-2</td><td>357 ± 049E-2</td><td>265 ± 013E-1</td><td>456 ± 123E-1</td><td>465 ± 039E-1</td><td>601 ± 049E-1</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 1097</td><td>298 ± 042E-2</td><td>418 ± 058E-2</td><td>373 ± 013E-1</td><td>641 ± 023E-1</td><td>898 ± 033E-1</td><td>124 ± 004E+0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 1266</td><td>024 ± 003E-4</td><td>141 ± 019E-4</td><td>146 ± 010E-2</td><td>289 ± 015E-2</td><td>404 ± 031E-2</td><td>638 ± 047E-2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 1291</td><td>698 ± 109E-3</td><td>151 ± 023E-2</td><td>579 ± 021E-1</td><td>118 ± 004E+0</td><td>172 ± 006E+0</td><td>241 ± 008E+0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 1316</td><td>268 ± 037E-3</td><td>142 ± 019E-2</td><td>...</td><td>782 ± 028E-1</td><td>155 ± 005E+0</td><td>290 ± 010E+0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 1377</td><td>...</td><td>...</td><td>210 ± 011E-2</td><td>350 ± 014E-2</td><td>453 ± 032E-2</td><td>732 ± 023E-2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 1404</td><td>889 ± 123E-4</td><td>253 ± 035E-3</td><td>172 ± 006E-1</td><td>355 ± 013E-1</td><td>513 ± 018E-1</td><td>764 ± 028E-1</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>IC0342</td><td>233 ± 034E-2</td><td>513 ± 077E-2</td><td>975 ± 134E-1</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 1482</td><td>303 ± 047E-4</td><td>106 ± 015E-3</td><td>499 ± 028E-2</td><td>692 ± 045E-2</td><td>976 ± 095E-2</td><td>150 ± 013E-1</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 1512</td><td>158 ± 024E-2</td><td>165 ± 028E-2</td><td>146 ± 005E-1</td><td>252 ± 009E-1</td><td>351 ± 012E-1</td><td>489 ± 018E-1</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 1566</td><td>509 ± 071E-2</td><td>612 ± 084E-2</td><td>348 ± 012E-1</td><td>593 ± 021E-1</td><td>697 ± 025E-1</td><td>864 ± 031E-1</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 1705</td><td>158 ± 024E-2</td><td>148 ± 022E-2</td><td>267 ± 009E-2</td><td>366 ± 013E-2</td><td>399 ± 014E-2</td><td>537 ± 019E-2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 2146</td><td>188 ± 028E-3</td><td>485 ± 072E-3</td><td>119 ± 015E-1</td><td>210 ± 027E-1</td><td>...</td><td>537 ± 014E-1</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 2403</td><td>185 ± 029E-1</td><td>220 ± 034E-1</td><td>129 ± 012E+0</td><td>205 ± 029E+0</td><td>227 ± 008E+0</td><td>301 ± 007E+0</td><td>751 ± 015E-1</td><td>153 ± 003E+0</td><td>225 ± 004E+0</td><td>287 ± 005E+0</td></tr><tr><td>HoII</td><td>340 ± 053E-2</td><td>369 ± 056E-2</td><td>127 ± 009E-1</td><td>149 ± 007E-1</td><td>201 ± 022E-1</td><td>303 ± 049E-1</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>M81dwA</td><td>418 ± 057E-4</td><td>488 ± 067E-4</td><td>100 ± 040E-3</td><td>900 ± 400E-4</td><td>110 ± 040E-3</td><td>140 ± 060E-3</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>DDO 053</td><td>214 ± 033E-3</td><td>207 ± 032E-3</td><td>660 ± 160E-3</td><td>820 ± 200E-3</td><td>550 ± 180E-3</td><td>800 ± 260E-3</td><td>271 ± 014E-3</td><td>507 ± 017E-3</td><td>602 ± 020E-3</td><td>624 ± 021E-3</td></tr><tr><td>NGC 2798</td><td>965 ± 133E-4</td><td>201 ± 027E-3</td><td>298 ± 027E-2</td><td>545 ± 033E-2</td><td>645 ± 033E-2</td><td>110 ± 010E-1</td><td>839 ± 028E-3</td><td>310 ± 007E-2</td><td>598 ± 012E-2</td><td>825 ± 017E-2</td></tr><tr><td>NGC 2841</td><td>116 ± 016E-2</td><td>183 ± 025E-2</td><td>435 ± 020E-1</td><td>765 ± 027E-1</td><td>101 ± 007E+0</td><td>176 ± 009E+0</td><td>111 ± 002E-1</td><td>459 ± 009E-1</td><td>941 ± 018E-1</td><td>140 ± 002E+0</td></tr><tr><td>NGC 2915</td><td>218 ± 030E-3</td><td>216 ± 030E-3</td><td>214 ± 021E-2</td><td>308 ± 011E-2</td><td>508 ± 018E-2</td><td>500 ± 050E-2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>HoI</td><td>369 ± 058E-3</td><td>401 ± 061E-3</td><td>116 ± 029E-2</td><td>153 ± 038E-2</td><td>147 ± 043E-2</td><td>211 ± 053E-2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 2976</td><td>125 ± 019E-2</td><td>173 ± 026E-2</td><td>220 ± 014E-1</td><td>357 ± 011E-1</td><td>464 ± 029E-1</td><td>676 ± 045E-1</td><td>753 ± 016E-2</td><td>225 ± 004E-1</td><td>400 ± 008E-1</td><td>539 ± 010E-1</td></tr><tr><td>NGC 3049</td><td>228 ± 034E-3</td><td>339 ± 046E-3</td><td>246 ± 020E-2</td><td>359 ± 018E-2</td><td>397 ± 028E-2</td><td>532 ± 051E-2</td><td>923 ± 027E-3</td><td>234 ± 005E-2</td><td>390 ± 008E-2</td><td>499 ± 010E-2</td></tr><tr><td>NGC 3031</td><td>100 ± 015E-1</td><td>133 ± 020E-1</td><td>297 ± 029E+0</td><td>610 ± 061E+0</td><td>...</td><td>141 ± 003E+1</td><td>884 ± 017E-1</td><td>362 ± 007E+0</td><td>778 ± 015E+0</td><td>116 ± 002E+1</td></tr><tr><td>NGC 3034</td><td>101 ± 015E-2</td><td>288 ± 043E-2</td><td>111 ± 018E+0</td><td>164 ± 016E+0</td><td>243 ± 033E+0</td><td>376 ± 045E+0</td><td>323 ± 006E-1</td><td>105 ± 002E+0</td><td>231 ± 004E+0</td><td>345 ± 006E+0</td></tr><tr><td>HoIX</td><td>226 ± 031E-3</td><td>280 ± 038E-3</td><td>570 ± 090E-3</td><td>550 ± 110E-3</td><td>590 ± 120E-3</td><td>900 ± 300E-3</td><td>375 ± 019E-3</td><td>635 ± 020E-3</td><td>807 ± 024E-3</td><td>930 ± 028E-3</td></tr><tr><td>NGC 3077</td><td>...</td><td>...</td><td>183 ± 005E-1</td><td>...</td><td>539 ± 014E-1</td><td>...</td><td>694 ± 015E-2</td><td>264 ± 005E-1</td><td>496 ± 010E-1</td><td>688 ± 013E-1</td></tr><tr><td>M81dwB</td><td>469 ± 073E-4</td><td>586 ± 090E-4</td><td>480 ± 160E-3</td><td>650 ± 210E-3</td><td>800 ± 270E-3</td><td>830 ± 230E-3</td><td>175 ± 011E-3</td><td>447 ± 016E-3</td><td>682 ± 021E-3</td><td>842 ± 025E-3</td></tr><tr><td>NGC 3190</td><td>334 ± 046E-4</td><td>149 ± 020E-3</td><td>997 ± 040E-2</td><td>180 ± 005E-1</td><td>253 ± 008E-1</td><td>400 ± 015E-1</td><td>216 ± 005E-2</td><td>102 ± 002E-1</td><td>211 ± 004E-1</td><td>317 ± 006E-1</td></tr><tr><td>NGC 3184</td><td>373 ± 051E-2</td><td>492 ± 068E-2</td><td>336 ± 029E-1</td><td>478 ± 020E-1</td><td>566 ± 039E-1</td><td>740 ± 041E-1</td><td>106 ± 002E-1</td><td>316 ± 006E-1</td><td>509 ± 010E-1</td><td>667 ± 013E-1</td></tr><tr><td>NGC 3198</td><td>215 ± 029E-2</td><td>259 ± 035E-2</td><td>200 ± 008E-1</td><td>251 ± 013E-1</td><td>296 ± 024E-1</td><td>398 ± 033E-1</td><td>628 ± 013E-2</td><td>171 ± 003E-1</td><td>270 ± 005E-1</td><td>350 ± 007E-1</td></tr><tr><td>IC2574</td><td>390 ± 061E-2</td><td>405 ± 061E-2</td><td>140 ± 019E-1</td><td>184 ± 025E-1</td><td>182 ± 029E-1</td><td>264 ± 035E-1</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 3265</td><td>474 ± 065E-4</td><td>807 ± 111E-4</td><td>112 ± 014E-2</td><td>170 ± 008E-2</td><td>218 ± 020E-2</td><td>352 ± 051E-2</td><td>365 ± 016E-3</td><td>113 ± 003E-2</td><td>209 ± 005E-2</td><td>289 ± 006E-2</td></tr><tr><td>Mrk 33</td><td>378 ± 052E-3</td><td>475 ± 065E-3</td><td>196 ± 014E-2</td><td>283 ± 055E-2</td><td>336 ± 073E-2</td><td>392 ± 078E-2</td><td>937 ± 027E-3</td><td>197 ± 004E-2</td><td>299 ± 006E-2</td><td>342 ± 007E-2</td></tr><tr><td>NGC 3351</td><td>147 ± 023E-2</td><td>242 ± 036E-2</td><td>302 ± 037E-1</td><td>533 ± 039E-1</td><td>700 ± 050E-1</td><td>107 ± 006E+0</td><td>876 ± 018E-2</td><td>328 ± 006E-1</td><td>620 ± 012E-1</td><td>878 ± 017E-1</td></tr><tr><td>NGC 3521</td><td>144 ± 023E-2</td><td>296 ± 045E-2</td><td>629 ± 024E-1</td><td>107 ± 002E+0</td><td>147 ± 002E+0</td><td>225 ± 006E+0</td><td>170 ± 003E-1</td><td>664 ± 013E-1</td><td>129 ± 002E+0</td><td>180 ± 003E+0</td></tr><tr><td>NGC 3621</td><td>427 ± 062E-2</td><td>608 ± 086E-2</td><td>428 ± 015E-1</td><td>651 ± 024E-1</td><td>780 ± 028E-1</td><td>104 ± 003E+0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 3627</td><td>246 ± 038E-2</td><td>452 ± 069E-2</td><td>742 ± 042E-1</td><td>115 ± 002E+0</td><td>141 ± 012E+0</td><td>215 ± 011E+0</td><td>214 ± 004E-1</td><td>760 ± 015E-1</td><td>136 ± 002E+0</td><td>190 ± 003E+0</td></tr><tr><td>NGC 3773</td><td>345 ± 047E-3</td><td>454 ± 062E-3</td><td>166 ± 009E-2</td><td>226 ± 008E-2</td><td>259 ± 021E-2</td><td>327 ± 026E-2</td><td>754 ± 023E-3</td><td>163 ± 004E-2</td><td>253 ± 005E-2</td><td>307 ± 007E-2</td></tr></tbody></table>
<table><caption>Table 2
(Continued)</caption><thead><tr><th>Filter</th><th>GALEX</th><th>GALEX</th><th>B</th><th>V</th><th>R<sub>C</sub></th><th>I<sub>C</sub></th><th>SDSS</th><th>SDSS</th><th>SDSS</th><th>SDSS</th></tr><tr><th></th><th>FUV</th><th>NUV</th><th></th><th></th><th></th><th></th><th>u</th><th>g</th><th>r</th><th>i</th></tr></thead><tbody><tr><td>λ&#773;(μm)</td><td>0.154</td><td>0.231</td><td>0.441</td><td>0.551</td><td>0.659</td><td>0.806</td><td>0.356</td><td>0.482</td><td>0.626</td><td>0.767</td></tr><tr><td>Δλ(μm)</td><td>0.025</td><td>0.073</td><td>0.096</td><td>0.089</td><td>0.159</td><td>0.150</td><td>0.056</td><td>0.127</td><td>0.133</td><td>0.135</td></tr><tr><td>Λ<sub>λ</sub>/Λ<sub>V</sub></td><td>2.586</td><td>2.994</td><td>1.310</td><td>1.0</td><td>0.788</td><td>0.577</td><td>1.642</td><td>1.219</td><td>0.849</td><td>0.641</td></tr><tr><td>NGC 3938</td><td>...</td><td>311 ± 043E-2</td><td>218 ± 008E-1</td><td>308 ± 005E-1</td><td>347 ± 019E-1</td><td>486 ± 017E-1</td><td>724 ± 015E-2</td><td>203 ± 004E-1</td><td>314 ± 006E-1</td><td>407 ± 008E-1</td></tr><tr><td>NGC 4125</td><td>...</td><td>193 ± 028E-3</td><td>202 ± 003E-1</td><td>369 ± 007E-1</td><td>504 ± 011E-1</td><td>764 ± 048E-1</td><td>391 ± 008E-2</td><td>204 ± 004E-1</td><td>419 ± 008E-1</td><td>619 ± 012E-1</td></tr><tr><td>NGC 4236</td><td>625 ± 098E-2</td><td>744 ± 113E-2</td><td>343 ± 029E-1</td><td>395 ± 031E-1</td><td>479 ± 038E-1</td><td>560 ± 054E-1</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 4254</td><td>259 ± 038E-2</td><td>464 ± 064E-2</td><td>344 ± 021E-1</td><td>486 ± 014E-1</td><td>614 ± 022E-1</td><td>765 ± 026E-1</td><td>128 ± 002E-1</td><td>339 ± 006E-1</td><td>543 ± 010E-1</td><td>697 ± 014E-1</td></tr><tr><td>NGC 4321</td><td>262 ± 039E-2</td><td>445 ± 061E-2</td><td>442 ± 020E-1</td><td>670 ± 017E-1</td><td>889 ± 041E-1</td><td>132 ± 007E+0</td><td>152 ± 003E-1</td><td>442 ± 008E-1</td><td>755 ± 015E-1</td><td>103 ± 002E+0</td></tr><tr><td>NGC 4450</td><td>...</td><td>438 ± 060E-3</td><td>201 ± 010E-1</td><td>368 ± 010E-1</td><td>505 ± 017E-1</td><td>768 ± 032E-1</td><td>513 ± 011E-2</td><td>213 ± 004E-1</td><td>432 ± 008E-1</td><td>629 ± 012E-1</td></tr><tr><td>NGC 4536</td><td>148 ± 020E-2</td><td>191 ± 026E-2</td><td>185 ± 012E-1</td><td>273 ± 023E-1</td><td>343 ± 035E-1</td><td>520 ± 100E-1</td><td>561 ± 012E-2</td><td>172 ± 003E-1</td><td>292 ± 005E-1</td><td>393 ± 007E-1</td></tr><tr><td>NGC 4552</td><td>140 ± 019E-3</td><td>344 ± 047E-3</td><td>230 ± 009E-1</td><td>425 ± 010E-1</td><td>603 ± 016E-1</td><td>942 ± 051E-1</td><td>440 ± 009E-2</td><td>239 ± 004E-1</td><td>501 ± 010E-1</td><td>749 ± 015E-1</td></tr><tr><td>NGC 4559</td><td>473 ± 065E-2</td><td>568 ± 078E-2</td><td>305 ± 019E-1</td><td>396 ± 011E-1</td><td>452 ± 033E-1</td><td>570 ± 039E-1</td><td>108 ± 002E-1</td><td>277 ± 005E-1</td><td>402 ± 008E-1</td><td>502 ± 010E-1</td></tr><tr><td>NGC 4569</td><td>427 ± 059E-3</td><td>139 ± 019E-2</td><td>335 ± 033E-1</td><td>555 ± 055E-1</td><td>...</td><td>...</td><td>909 ± 019E-2</td><td>361 ± 007E-1</td><td>624 ± 012E-1</td><td>900 ± 018E-1</td></tr><tr><td>NGC 4579</td><td>434 ± 060E-3</td><td>897 ± 124E-3</td><td>293 ± 012E-1</td><td>535 ± 020E-1</td><td>694 ± 043E-1</td><td>105 ± 006E+0</td><td>661 ± 014E-2</td><td>299 ± 006E-1</td><td>602 ± 012E-1</td><td>883 ± 017E-1</td></tr><tr><td>NGC 4594</td><td>376 ± 059E-3</td><td>111 ± 017E-2</td><td>103 ± 006E+0</td><td>242 ± 032E+0</td><td>292 ± 009E+0</td><td>453 ± 028E+0</td><td>242 ± 005E-1</td><td>123 ± 002E+0</td><td>265 ± 005E+0</td><td>401 ± 008E+0</td></tr><tr><td>NGC 4625</td><td>549 ± 087E-3</td><td>698 ± 107E-3</td><td>364 ± 028E-2</td><td>527 ± 047E-2</td><td>617 ± 086E-2</td><td>805 ± 058E-2</td><td>126 ± 003E-2</td><td>341 ± 007E-2</td><td>534 ± 011E-2</td><td>686 ± 014E-2</td></tr><tr><td>NGC 4631</td><td>963 ± 151E-2</td><td>118 ± 018E-1</td><td>616 ± 048E-1</td><td>812 ± 030E-1</td><td>944 ± 048E-1</td><td>119 ± 005E+0</td><td>249 ± 005E-1</td><td>579 ± 011E-1</td><td>854 ± 017E-1</td><td>108 ± 002E+0</td></tr><tr><td>NGC 4725</td><td>202 ± 028E-2</td><td>271 ± 037E-2</td><td>466 ± 024E-1</td><td>825 ± 022E-1</td><td>104 ± 003E+0</td><td>163 ± 007E+0</td><td>123 ± 002E-1</td><td>478 ± 009E-1</td><td>910 ± 018E-1</td><td>131 ± 002E+0</td></tr><tr><td>NGC 4736</td><td>625 ± 098E-2</td><td>809 ± 123E-2</td><td>141 ± 009E+0</td><td>215 ± 006E+0</td><td>292 ± 010E+0</td><td>431 ± 024E+0</td><td>415 ± 008E-1</td><td>162 ± 003E+0</td><td>300 ± 006E+0</td><td>421 ± 008E+0</td></tr><tr><td>DDO 154</td><td>413 ± 064E-3</td><td>401 ± 062E-3</td><td>105 ± 029E-2</td><td>113 ± 035E-2</td><td>121 ± 030E-2</td><td>127 ± 032E-2</td><td>450 ± 017E-3</td><td>892 ± 026E-3</td><td>102 ± 002E-2</td><td>102 ± 002E-2</td></tr><tr><td>NGC 4826</td><td>100 ± 015E-2</td><td>258 ± 039E-2</td><td>957 ± 078E-1</td><td>149 ± 008E+0</td><td>190 ± 017E+0</td><td>303 ± 017E+0</td><td>228 ± 004E-1</td><td>966 ± 019E-1</td><td>184 ± 003E+0</td><td>268 ± 005E+0</td></tr><tr><td>DDO 165</td><td>483 ± 075E-3</td><td>660 ± 100E-3</td><td>285 ± 071E-2</td><td>277 ± 028E-2</td><td>254 ± 055E-2</td><td>339 ± 125E-2</td><td>929 ± 028E-3</td><td>220 ± 005E-2</td><td>255 ± 006E-2</td><td>284 ± 006E-2</td></tr><tr><td>NGC 5033</td><td>181 ± 025E-2</td><td>235 ± 032E-2</td><td>241 ± 012E-1</td><td>392 ± 021E-1</td><td>...</td><td>636 ± 041E-1</td><td>734 ± 015E-2</td><td>235 ± 004E-1</td><td>422 ± 008E-1</td><td>581 ± 011E-1</td></tr><tr><td>NGC 5055</td><td>369 ± 058E-2</td><td>586 ± 090E-2</td><td>804 ± 080E-1</td><td>133 ± 013E+0</td><td>181 ± 005E+0</td><td>274 ± 007E+0</td><td>280 ± 005E-1</td><td>934 ± 018E-1</td><td>171 ± 003E+0</td><td>245 ± 004E+0</td></tr><tr><td>NGC 5194</td><td>107 ± 016E-1</td><td>165 ± 025E-1</td><td>133 ± 015E+0</td><td>182 ± 012E+0</td><td>215 ± 020E+0</td><td>323 ± 029E+0</td><td>568 ± 011E-1</td><td>149 ± 003E+0</td><td>249 ± 005E+0</td><td>335 ± 006E+0</td></tr><tr><td>NGC 5195</td><td>155 ± 025E-3</td><td>420 ± 066E-3</td><td>373 ± 042E-1</td><td>612 ± 041E-1</td><td>806 ± 076E-1</td><td>150 ± 013E+0</td><td>675 ± 014E-2</td><td>261 ± 005E-1</td><td>562 ± 011E-1</td><td>852 ± 017E-1</td></tr><tr><td>NGC 5398</td><td>469 ± 064E-3</td><td>699 ± 096E-3</td><td>481 ± 048E-2</td><td>506 ± 050E-2</td><td>403 ± 040E-2</td><td>520 ± 052E-2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 5457</td><td>346 ± 054E-1</td><td>387 ± 059E-1</td><td>202 ± 017E+0</td><td>261 ± 024E+0</td><td>285 ± 007E+0</td><td>431 ± 011E+0</td><td>755 ± 015E-1</td><td>189 ± 003E+0</td><td>275 ± 005E+0</td><td>352 ± 007E+0</td></tr><tr><td>NGC 5408</td><td>...</td><td>...</td><td>562 ± 056E-2</td><td>804 ± 080E-2</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 5474</td><td>231 ± 036E-2</td><td>251 ± 038E-2</td><td>124 ± 007E-1</td><td>165 ± 006E-1</td><td>180 ± 012E-1</td><td>215 ± 019E-1</td><td>488 ± 011E-2</td><td>116 ± 002E-1</td><td>166 ± 003E-1</td><td>199 ± 004E-1</td></tr><tr><td>NGC 5713</td><td>387 ± 053E-3</td><td>750 ± 103E-3</td><td>920 ± 062E-2</td><td>134 ± 006E-1</td><td>174 ± 006E-1</td><td>237 ± 025E-1</td><td>285 ± 006E-2</td><td>884 ± 018E-2</td><td>151 ± 003E-1</td><td>197 ± 004E-1</td></tr><tr><td>NGC 5866</td><td>584 ± 081E-4</td><td>375 ± 051E-3</td><td>235 ± 010E-1</td><td>429 ± 015E-1</td><td>542 ± 037E-1</td><td>849 ± 049E-1</td><td>556 ± 012E-2</td><td>255 ± 005E-1</td><td>493 ± 009E-1</td><td>731 ± 014E-1</td></tr><tr><td>IC4710</td><td>118 ± 016E-2</td><td>157 ± 021E-2</td><td>566 ± 056E-2</td><td>797 ± 079E-2</td><td>704 ± 070E-2</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 6822</td><td>573 ± 079E-2</td><td>739 ± 103E-2</td><td>658 ± 034E-1</td><td>973 ± 037E-1</td><td>121 ± 004E+0</td><td>977 ± 085E-1</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 6946</td><td>183 ± 025E-2</td><td>335 ± 046E-2</td><td>610 ± 060E-1</td><td>127 ± 005E+0</td><td>...</td><td>349 ± 034E+0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 7331</td><td>802 ± 111E-3</td><td>151 ± 020E-2</td><td>452 ± 026E-1</td><td>715 ± 013E-1</td><td>101 ± 002E+0</td><td>168 ± 007E+0</td><td>905 ± 019E-2</td><td>386 ± 007E-1</td><td>814 ± 016E-1</td><td>124 ± 002E+0</td></tr><tr><td>NGC 7552</td><td>697 ± 096E-3</td><td>136 ± 019E-2</td><td>127 ± 004E-1</td><td>216 ± 007E-1</td><td>226 ± 022E-1</td><td>214 ± 021E-1</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 7793</td><td>111 ± 017E-1</td><td>129 ± 019E-1</td><td>550 ± 055E-1</td><td>766 ± 076E-1</td><td>745 ± 074E-1</td><td>661 ± 066E-1</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>Filter</td><td>SDSS</td><td>2MASS</td><td>2MASS</td><td>2MASS</td><td>Spitzer</td><td>Spitzer</td><td>Spitzer</td><td>Spitzer</td><td>WISE</td><td>Spitzer</td></tr><tr><td>λ&#773;(μm)</td><td>z</td><td>J</td><td>H</td><td>K<sub>s</sub></td><td>IRAC</td><td>IRAC</td><td>IRAC</td><td>IRAC</td><td>W3</td><td>MIPS</td></tr><tr><td>Δλ(μm)</td><td>0.910</td><td>1.24</td><td>1.65</td><td>2.17</td><td>3.56</td><td>4.51</td><td>5.76</td><td>7.96</td><td>12.8</td><td>23.8</td></tr><tr><td>Δλ(μm)</td><td>0.131</td><td>0.163</td><td>0.252</td><td>0.264</td><td>0.687</td><td>0.872</td><td>1.25</td><td>2.55</td><td>5.51</td><td>5.32</td></tr><tr><td>Λ<sub>λ</sub>/Λ<sub>V</sub></td><td>0.488</td><td>0.296</td><td>0.187</td><td>0.116</td><td>0.0451</td><td>0.0288</td><td>0.0193</td><td>0.0296</td><td>0.0355</td><td>0.0193</td></tr><tr><td>NGC 0024</td><td>...</td><td>228 ± 012E-1</td><td>246 ± 013E-1</td><td>188 ± 012E-1</td><td>101 ± 013E-1</td><td>682 ± 101E-2</td><td>821 ± 116E-2</td><td>117 ± 016E-1</td><td>924 ± 064E-2</td><td>120 ± 004E-1</td></tr><tr><td>NGC 0337</td><td>136 ± 002E-1</td><td>178 ± 009E-1</td><td>190 ± 009E-1</td><td>164 ± 008E-1</td><td>958 ± 126E-2</td><td>659 ± 090E-2</td><td>141 ± 018E-1</td><td>376 ± 047E-1</td><td>291 ± 020E-1</td><td>673 ± 028E-1</td></tr><tr><td>NGC 0584</td><td>562 ± 011E-1</td><td>880 ± 044E-1</td><td>109 ± 005E+0</td><td>860 ± 043E-1</td><td>365 ± 049E-1</td><td>219 ± 029E-1</td><td>174 ± 022E-1</td><td>114 ± 014E-1</td><td>700 ± 049E-2</td><td>480 ± 020E-2</td></tr></tbody></table>
<table><caption>Table 2
(Continued)</caption><thead><tr><th>Filter</th><th>SDSS<br>z</th><th>2MASS<br>J</th><th>2MASS<br>H</th><th>2MASS<br>K<sub>s</sub></th><th>Spitzer<br>IRAC</th><th>Spitzer<br>IRAC</th><th>Spitzer<br>IRAC</th><th>Spitzer<br>IRAC</th><th>WISE<br>W3</th><th>Spitzer<br>MIPS</th></tr></thead><tbody><tr><td>λ&#773;(μm)</td><td>0.910</td><td>1.24</td><td>1.65</td><td>2.17</td><td>3.56</td><td>4.51</td><td>5.76</td><td>7.96</td><td>12.8</td><td>23.8</td></tr><tr><td>Δλ(μm)</td><td>0.131</td><td>0.163</td><td>0.252</td><td>0.264</td><td>0.687</td><td>0.872</td><td>1.25</td><td>2.55</td><td>5.51</td><td>5.32</td></tr><tr><td>Δλ/Δν</td><td>0.488</td><td>0.296</td><td>0.187</td><td>0.116</td><td>0.0451</td><td>0.0288</td><td>0.0193</td><td>0.0296</td><td>0.0355</td><td>0.0193</td></tr></tbody></table><table><tbody><tr><td>NGC 0628</td><td>123 ± 002E+0</td><td>156 ± 007E+0</td><td>160 ± 008E+0</td><td>128 ± 006E+0</td><td>839 ± 117E-1</td><td>544 ± 075E-1</td><td>116 ± 014E+0</td><td>259 ± 033E+0</td><td>235 ± 016E+0</td><td>323 ± 012E+0</td></tr><tr><td>NGC 0855</td><td>766 ± 017E-2</td><td>853 ± 051E-2</td><td>940 ± 064E-2</td><td>778 ± 066E-2</td><td>428 ± 060E-2</td><td>280 ± 039E-2</td><td>359 ± 030E-2</td><td>474 ± 057E-2</td><td>354 ± 024E-2</td><td>851 ± 034E-2</td></tr><tr><td>NGC 0925</td><td>...</td><td>561 ± 028E-1</td><td>621 ± 031E-1</td><td>500 ± 026E-1</td><td>307 ± 041E-1</td><td>210 ± 028E-1</td><td>349 ± 044E-1</td><td>606 ± 075E-1</td><td>545 ± 038E-1</td><td>943 ± 040E-1</td></tr><tr><td>NGC 1097</td><td>...</td><td>234 ± 011E+0</td><td>270 ± 013E+0</td><td>226 ± 011E+0</td><td>123 ± 016E+0</td><td>800 ± 109E-1</td><td>146 ± 018E+0</td><td>317 ± 039E+0</td><td>298 ± 020E+0</td><td>661 ± 027E+0</td></tr><tr><td>NGC 1266</td><td>...</td><td>112 ± 005E-1</td><td>120 ± 006E-1</td><td>116 ± 006E-1</td><td>538 ± 073E-2</td><td>414 ± 054E-2</td><td>542 ± 072E-2</td><td>878 ± 111E-2</td><td>111 ± 007E-1</td><td>872 ± 036E-1</td></tr><tr><td>NGC 1291</td><td>...</td><td>432 ± 021E+0</td><td>453 ± 022E+0</td><td>396 ± 019E+0</td><td>207 ± 028E+0</td><td>127 ± 017E+0</td><td>906 ± 121E-1</td><td>639 ± 079E-1</td><td>592 ± 041E-1</td><td>480 ± 019E-1</td></tr><tr><td>NGC 1316</td><td>...</td><td>461 ± 023E+0</td><td>484 ± 024E+0</td><td>417 ± 020E+0</td><td>247 ± 033E+0</td><td>153 ± 021E+0</td><td>112 ± 014E+0</td><td>553 ± 069E-1</td><td>605 ± 042E-1</td><td>428 ± 021E-1</td></tr><tr><td>NGC 1377</td><td>...</td><td>986 ± 051E-2</td><td>113 ± 006E-1</td><td>936 ± 053E-2</td><td>567 ± 075E-2</td><td>850 ± 116E-2</td><td>267 ± 035E-1</td><td>419 ± 052E-1</td><td>397 ± 027E-1</td><td>182 ± 007E+0</td></tr><tr><td>NGC 1404</td><td>...</td><td>136 ± 006E+0</td><td>158 ± 007E+0</td><td>134 ± 006E+0</td><td>727 ± 098E-1</td><td>434 ± 059E-1</td><td>331 ± 042E-1</td><td>158 ± 020E-1</td><td>137 ± 009E-1</td><td>880 ± 040E-2</td></tr><tr><td>IC0342</td><td>...</td><td>952 ± 047E+0</td><td>106 ± 005E+1</td><td>107 ± 005E+1</td><td>125 ± 016E+1</td><td>701 ± 096E+0</td><td>113 ± 014E+1</td><td>251 ± 031E+1</td><td>233 ± 016E+1</td><td>362 ± 014E+1</td></tr><tr><td>NGC 1482</td><td>...</td><td>225 ± 011E-1</td><td>294 ± 015E-1</td><td>290 ± 015E-1</td><td>204 ± 028E-1</td><td>151 ± 020E-1</td><td>592 ± 076E-1</td><td>155 ± 019E+0</td><td>123 ± 008E+0</td><td>367 ± 014E+0</td></tr><tr><td>NGC 1512</td><td>...</td><td>804 ± 043E-1</td><td>851 ± 048E-1</td><td>727 ± 046E-1</td><td>438 ± 052E-1</td><td>294 ± 033E-1</td><td>260 ± 034E-1</td><td>456 ± 054E-1</td><td>448 ± 031E-1</td><td>486 ± 019E-1</td></tr><tr><td>NGC 1566</td><td>...</td><td>138 ± 006E+0</td><td>140 ± 007E+0</td><td>126 ± 006E+0</td><td>750 ± 101E-1</td><td>479 ± 065E-1</td><td>907 ± 115E-1</td><td>211 ± 026E+0</td><td>188 ± 013E+0</td><td>282 ± 012E+0</td></tr><tr><td>NGC 1705</td><td>...</td><td>570 ± 036E-2</td><td>537 ± 044E-2</td><td>442 ± 047E-2</td><td>266 ± 036E-2</td><td>192 ± 025E-2</td><td>183 ± 019E-2</td><td>192 ± 020E-2</td><td>194 ± 013E-2</td><td>538 ± 022E-2</td></tr><tr><td>NGC 2146</td><td>...</td><td>892 ± 044E-1</td><td>117 ± 005E+0</td><td>107 ± 005E+0</td><td>835 ± 113E-1</td><td>629 ± 086E-1</td><td>250 ± 032E+0</td><td>676 ± 084E+0</td><td>495 ± 034E+0</td><td>123 ± 004E+1</td></tr><tr><td>NGC 2403</td><td>329 ± 006E+0</td><td>283 ± 014E+0</td><td>284 ± 014E+0</td><td>235 ± 012E+0</td><td>149 ± 025E+0</td><td>101 ± 017E+0</td><td>197 ± 026E+0</td><td>386 ± 051E+0</td><td>395 ± 027E+0</td><td>587 ± 023E+0</td></tr><tr><td>HoII</td><td>...</td><td>275 ± 016E-1</td><td>294 ± 019E-1</td><td>226 ± 018E-1</td><td>771 ± 098E-2</td><td>644 ± 078E-2</td><td>399 ± 047E-2</td><td>440 ± 048E-2</td><td>417 ± 030E-2</td><td>177 ± 007E-1</td></tr><tr><td>M81dwA</td><td>...</td><td>370 ± 066E-3</td><td>384 ± 098E-3</td><td>290 ± 117E-3</td><td>185 ± 094E-3</td><td>960 ± 960E-4</td><td>&lt;376E-3</td><td>&lt;236E-3</td><td>&lt;630E-4</td><td>&lt;173E-2</td></tr><tr><td>DDO 053</td><td>583 ± 033E-3</td><td>730 ± 200E-3</td><td>134 ± 030E-2</td><td>783 ± 366E-3</td><td>425 ± 100E-3</td><td>309 ± 100E-3</td><td>264 ± 090E-3</td><td>437 ± 100E-3</td><td>642 ± 047E-3</td><td>239 ± 010E-2</td></tr><tr><td>NGC 2798</td><td>106 ± 002E-1</td><td>160 ± 008E-1</td><td>184 ± 009E-1</td><td>172 ± 009E-1</td><td>114 ± 015E-1</td><td>810 ± 114E-2</td><td>265 ± 034E-1</td><td>632 ± 078E-1</td><td>587 ± 041E-1</td><td>261 ± 010E+0</td></tr><tr><td>NGC 2841</td><td>179 ± 003E+0</td><td>277 ± 013E+0</td><td>319 ± 015E+0</td><td>265 ± 013E+0</td><td>126 ± 017E+0</td><td>750 ± 103E-1</td><td>669 ± 085E-1</td><td>115 ± 014E+0</td><td>100 ± 007E+0</td><td>908 ± 037E-1</td></tr><tr><td>NGC 2915</td><td>...</td><td>103 ± 005E-1</td><td>127 ± 006E-1</td><td>839 ± 048E-2</td><td>521 ± 072E-2</td><td>340 ± 049E-2</td><td>321 ± 043E-2</td><td>304 ± 038E-2</td><td>180 ± 012E-2</td><td>620 ± 026E-2</td></tr><tr><td>HoI</td><td>...</td><td>296 ± 041E-2</td><td>385 ± 062E-2</td><td>157 ± 072E-2</td><td>959 ± 140E-3</td><td>595 ± 120E-3</td><td>373 ± 180E-3</td><td>362 ± 160E-3</td><td>163 ± 082E-3</td><td>654 ± 073E-3</td></tr><tr><td>NGC 2976</td><td>647 ± 013E-1</td><td>808 ± 040E-1</td><td>858 ± 043E-1</td><td>689 ± 036E-1</td><td>405 ± 058E-1</td><td>281 ± 039E-1</td><td>513 ± 065E-1</td><td>101 ± 012E+0</td><td>835 ± 058E-1</td><td>139 ± 005E+0</td></tr><tr><td>NGC 3049</td><td>601 ± 013E-2</td><td>751 ± 040E-2</td><td>802 ± 046E-2</td><td>729 ± 045E-2</td><td>402 ± 051E-2</td><td>273 ± 038E-2</td><td>651 ± 086E-2</td><td>134 ± 016E-1</td><td>112 ± 007E-1</td><td>426 ± 017E-1</td></tr><tr><td>NGC 3031</td><td>153 ± 003E+1</td><td>219 ± 010E+1</td><td>243 ± 012E+1</td><td>207 ± 010E+1</td><td>105 ± 014E+1</td><td>652 ± 089E+0</td><td>556 ± 074E+0</td><td>759 ± 099E+0</td><td>580 ± 040E+0</td><td>521 ± 020E+0</td></tr><tr><td>NGC 3034</td><td>461 ± 009E+0</td><td>811 ± 040E+0</td><td>992 ± 049E+0</td><td>960 ± 048E+0</td><td>712 ± 223E+0</td><td>567 ± 178E+0</td><td>234 ± 072E+1</td><td>613 ± 189E+1</td><td>713 ± 050E+1</td><td>322 ± 096E+2<sup>a</sup></td></tr><tr><td>HoIX</td><td>902 ± 060E-3</td><td>231 ± 020E-2</td><td>196 ± 027E-2</td><td>142 ± 032E-2</td><td>730 ± 113E-3</td><td>377 ± 101E-3</td><td>&lt;130E-2</td><td>&lt;119E-2</td><td>526 ± 050E-3</td><td>&lt;362E-2</td></tr><tr><td>NGC 3077</td><td>821 ± 016E-1</td><td>993 ± 050E-1</td><td>100 ± 005E+0</td><td>850 ± 044E-1</td><td>533 ± 072E-1</td><td>360 ± 049E-1</td><td>430 ± 054E-1</td><td>808 ± 100E-1</td><td>748 ± 052E-1</td><td>129 ± 005E+0</td></tr><tr><td>M81dwB</td><td>997 ± 037E-3</td><td>111 ± 014E-2</td><td>130 ± 022E-2</td><td>132 ± 026E-2</td><td>534 ± 100E-3</td><td>360 ± 100E-3</td><td>321 ± 090E-3</td><td>307 ± 080E-3</td><td>373 ± 124E-3</td><td>332 ± 034E-3</td></tr><tr><td>NGC 3190</td><td>423 ± 008E-1</td><td>697 ± 034E-1</td><td>824 ± 041E-1</td><td>734 ± 036E-1</td><td>371 ± 050E-1</td><td>234 ± 032E-1</td><td>246 ± 031E-1</td><td>327 ± 041E-1</td><td>277 ± 019E-1</td><td>266 ± 011E-1</td></tr><tr><td>NGC 3184</td><td>754 ± 015E-1</td><td>103 ± 005E+0</td><td>112 ± 005E+0</td><td>908 ± 046E-1</td><td>556 ± 075E-1</td><td>356 ± 048E-1</td><td>666 ± 084E-1</td><td>143 ± 017E+0</td><td>115 ± 008E+0</td><td>142 ± 005E+0</td></tr><tr><td>NGC 3198</td><td>417 ± 008E-1</td><td>568 ± 028E-1</td><td>627 ± 031E-1</td><td>545 ± 027E-1</td><td>273 ± 036E-1</td><td>173 ± 023E-1</td><td>335 ± 042E-1</td><td>682 ± 085E-1</td><td>605 ± 042E-1</td><td>105 ± 004E+0</td></tr><tr><td>IC2574</td><td>...</td><td>360 ± 020E-1</td><td>232 ± 019E-1</td><td>172 ± 021E-1</td><td>124 ± 020E-1</td><td>906 ± 127E-2</td><td>642 ± 087E-2</td><td>688 ± 089E-2</td><td>442 ± 032E-2</td><td>281 ± 011E-1</td></tr><tr><td>NGC 3265</td><td>361 ± 008E-2</td><td>497 ± 028E-2</td><td>565 ± 035E-2</td><td>476 ± 035E-2</td><td>283 ± 037E-2</td><td>198 ± 026E-2</td><td>410 ± 054E-2</td><td>101 ± 012E-1</td><td>855 ± 059E-2</td><td>294 ± 012E-1</td></tr><tr><td>Mrk 33</td><td>384 ± 008E-2</td><td>486 ± 028E-2</td><td>555 ± 035E-2</td><td>476 ± 035E-2</td><td>265 ± 036E-2</td><td>188 ± 026E-2</td><td>528 ± 067E-2</td><td>127 ± 016E-1</td><td>157 ± 010E-1</td><td>861 ± 035E-1</td></tr><tr><td>NGC 3351</td><td>110 ± 002E+0</td><td>164 ± 008E+0</td><td>174 ± 008E+0</td><td>152 ± 007E+0</td><td>770 ± 109E-1</td><td>500 ± 070E-1</td><td>658 ± 092E-1</td><td>126 ± 016E+0</td><td>115 ± 008E+0</td><td>253 ± 010E+0</td></tr><tr><td>NGC 3521</td><td>235 ± 004E+0</td><td>355 ± 017E+0</td><td>408 ± 020E+0</td><td>342 ± 017E+0</td><td>195 ± 027E+0</td><td>129 ± 018E+0</td><td>235 ± 032E+0</td><td>559 ± 075E+0</td><td>483 ± 033E+0</td><td>548 ± 021E+0</td></tr><tr><td>NGC 3621</td><td>...</td><td>181 ± 009E+0</td><td>205 ± 010E+0</td><td>164 ± 008E+0</td><td>983 ± 132E-1</td><td>664 ± 091E-1</td><td>160 ± 020E+0</td><td>347 ± 043E+0</td><td>293 ± 020E+0</td><td>368 ± 018E+0</td></tr><tr><td>NGC 3627</td><td>236 ± 004E+0</td><td>324 ± 016E+0</td><td>366 ± 018E+0</td><td>313 ± 015E+0</td><td>177 ± 025E+0</td><td>115 ± 017E+0</td><td>219 ± 030E+0</td><td>520 ± 069E+0</td><td>460 ± 032E+0</td><td>750 ± 029E+0</td></tr><tr><td>NGC 3773</td><td>345 ± 008E-2</td><td>442 ± 023E-2</td><td>380 ± 022E-2</td><td>370 ± 023E-2</td><td>221 ± 027E-2</td><td>143 ± 023E-2</td><td>255 ± 034E-2</td><td>474 ± 059E-2</td><td>409 ± 028E-2</td><td>144 ± 005E-1</td></tr><tr><td>NGC 3938</td><td>464 ± 009E-1</td><td>625 ± 031E-1</td><td>570 ± 029E-1</td><td>531 ± 027E-1</td><td>320 ± 043E-1</td><td>211 ± 029E-1</td><td>410 ± 052E-1</td><td>980 ± 122E-1</td><td>846 ± 059E-1</td><td>108 ± 004E+0</td></tr><tr><td>NGC 4125</td><td>795 ± 016E-1</td><td>136 ± 006E+0</td><td>151 ± 007E+0</td><td>127 ± 006E+0</td><td>639 ± 086E-1</td><td>371 ± 050E-1</td><td>247 ± 032E-1</td><td>143 ± 017E-1</td><td>104 ± 007E-1</td><td>784 ± 042E-2</td></tr><tr><td>NGC 4236</td><td>...</td><td>626 ± 033E-1</td><td>824 ± 044E-1</td><td>566 ± 034E-1</td><td>245 ± 033E-1</td><td>185 ± 028E-1</td><td>184 ± 014E-1</td><td>215 ± 027E-1</td><td>138 ± 009E-1</td><td>513 ± 020E-1</td></tr></tbody></table>
<table><caption>Table 2
(Continued)</caption><thead><tr><th>Filter</th><th>SDSS<br>z</th><th>2MASS<br>J</th><th>2MASS<br>H</th><th>2MASS<br>K<sub>s</sub></th><th>Spitzer<br>IRAC</th><th>Spitzer<br>IRAC</th><th>Spitzer<br>IRAC</th><th>Spitzer<br>IRAC</th><th>WISE<br>W3</th><th>Spitzer<br>MIPS</th></tr></thead><tbody><tr><td>λ&#773;(μm)</td><td>0.910</td><td>1.24</td><td>1.65</td><td>2.17</td><td>3.56</td><td>4.51</td><td>5.76</td><td>7.96</td><td>12.8</td><td>23.8</td></tr><tr><td>Δλ(μm)</td><td>0.131</td><td>0.163</td><td>0.252</td><td>0.264</td><td>0.687</td><td>0.872</td><td>1.25</td><td>2.55</td><td>5.51</td><td>5.32</td></tr><tr><td>Δλ/Δν</td><td>0.488</td><td>0.296</td><td>0.187</td><td>0.116</td><td>0.0451</td><td>0.0288</td><td>0.0193</td><td>0.0296</td><td>0.0355</td><td>0.0193</td></tr><tr><td>NGC 4254</td><td>842 ± 017E-1</td><td>122 ± 006E+0</td><td>132 ± 006E+0</td><td>119 ± 006E+0</td><td>697 ± 094E-1</td><td>468 ± 064E-1</td><td>149 ± 018E+0</td><td>392 ± 048E+0</td><td>331 ± 023E+0</td><td>419 ± 016E+0</td></tr><tr><td>NGC 4321</td><td>122 ± 002E+0</td><td>182 ± 009E+0</td><td>197 ± 009E+0</td><td>163 ± 008E+0</td><td>950 ± 128E-1</td><td>637 ± 087E-1</td><td>121 ± 015E+0</td><td>287 ± 035E+0</td><td>257 ± 018E+0</td><td>333 ± 013E+0</td></tr><tr><td>NGC 4450</td><td>789 ± 015E-1</td><td>117 ± 005E+0</td><td>136 ± 006E+0</td><td>106 ± 005E+0</td><td>527 ± 071E-1</td><td>324 ± 044E-1</td><td>260 ± 033E-1</td><td>267 ± 033E-1</td><td>246 ± 017E-1</td><td>209 ± 011E-1</td></tr><tr><td>NGC 4536</td><td>491 ± 010E-1</td><td>702 ± 035E-1</td><td>742 ± 037E-1</td><td>694 ± 035E-1</td><td>394 ± 053E-1</td><td>285 ± 038E-1</td><td>620 ± 079E-1</td><td>165 ± 020E+0</td><td>131 ± 009E+0</td><td>345 ± 013E+0</td></tr><tr><td>NGC 4552</td><td>988 ± 019E-1</td><td>157 ± 007E+0</td><td>175 ± 008E+0</td><td>143 ± 007E+0</td><td>824 ± 111E-1</td><td>480 ± 065E-1</td><td>299 ± 038E-1</td><td>170 ± 021E-1</td><td>100 ± 007E-1</td><td>940 ± 041E-2</td></tr><tr><td>NGC 4559</td><td>545 ± 011E-1</td><td>760 ± 038E-1</td><td>777 ± 039E-1</td><td>652 ± 033E-1</td><td>353 ± 047E-1</td><td>233 ± 032E-1</td><td>420 ± 053E-1</td><td>837 ± 104E-1</td><td>629 ± 044E-1</td><td>111 ± 004E+0</td></tr><tr><td>NGC 4569</td><td>108 ± 002E+0</td><td>175 ± 008E+0</td><td>203 ± 010E+0</td><td>164 ± 008E+0</td><td>759 ± 102E-1</td><td>472 ± 064E-1</td><td>590 ± 075E-1</td><td>101 ± 012E+0</td><td>931 ± 065E-1</td><td>143 ± 005E+0</td></tr><tr><td>NGC 4579</td><td>111 ± 002E+0</td><td>198 ± 009E+0</td><td>218 ± 010E+0</td><td>179 ± 008E+0</td><td>863 ± 117E-1</td><td>520 ± 071E-1</td><td>541 ± 069E-1</td><td>726 ± 090E-1</td><td>706 ± 049E-1</td><td>759 ± 031E-1</td></tr><tr><td>NGC 4594</td><td>523 ± 010E+0</td><td>771 ± 038E+0</td><td>894 ± 044E+0</td><td>743 ± 037E+0</td><td>389 ± 053E+0</td><td>235 ± 031E+0</td><td>179 ± 022E+0</td><td>144 ± 016E+0</td><td>109 ± 007E+0</td><td>771 ± 030E-1</td></tr><tr><td>NGC 4625</td><td>795 ± 017E-2</td><td>966 ± 063E-2</td><td>112 ± 008E-1</td><td>892 ± 087E-2</td><td>486 ± 064E-2</td><td>307 ± 040E-2</td><td>605 ± 076E-2</td><td>134 ± 016E-1</td><td>112 ± 007E-1</td><td>128 ± 005E-1</td></tr><tr><td>NGC 4631</td><td>121 ± 002E+0</td><td>172 ± 008E+0</td><td>196 ± 009E+0</td><td>182 ± 009E+0</td><td>119 ± 017E+0</td><td>845 ± 114E-1</td><td>247 ± 031E+0</td><td>584 ± 072E+0</td><td>463 ± 032E+0</td><td>812 ± 032E+0</td></tr><tr><td>NGC 4725</td><td>159 ± 003E+0</td><td>240 ± 012E+0</td><td>315 ± 015E+0</td><td>239 ± 012E+0</td><td>113 ± 015E+0</td><td>704 ± 096E-1</td><td>753 ± 095E-1</td><td>120 ± 015E+0</td><td>875 ± 061E-1</td><td>859 ± 037E-1</td></tr><tr><td>NGC 4736</td><td>518 ± 010E+0</td><td>684 ± 034E+0</td><td>760 ± 038E+0</td><td>639 ± 032E+0</td><td>344 ± 048E+0</td><td>229 ± 031E+0</td><td>256 ± 034E+0</td><td>481 ± 064E+0</td><td>454 ± 031E+0</td><td>552 ± 022E+0</td></tr><tr><td>DDO 154</td><td>126 ± 004E-2</td><td>984 ± 260E-3</td><td>123 ± 039E-2</td><td>119 ± 047E-2</td><td>510 ± 100E-3</td><td>350 ± 100E-3</td><td>&lt;403E-3</td><td>&lt;399E-3</td><td>&lt;124E-3</td><td>&lt;438E-3</td></tr><tr><td>NGC 4826</td><td>336 ± 006E+0</td><td>547 ± 027E+0</td><td>616 ± 030E+0</td><td>520 ± 026E+0</td><td>239 ± 034E+0</td><td>151 ± 021E+0</td><td>159 ± 021E+0</td><td>223 ± 029E+0</td><td>185 ± 012E+0</td><td>254 ± 010E+0</td></tr><tr><td>DDO 165</td><td>306 ± 008E-2</td><td>313 ± 035E-2</td><td>463 ± 054E-2</td><td>370 ± 062E-2</td><td>127 ± 023E-2</td><td>907 ± 150E-3</td><td>587 ± 170E-3</td><td>407 ± 080E-3</td><td>&lt;168E-3</td><td>&lt;448E-3</td></tr><tr><td>NGC 5033</td><td>720 ± 014E-1</td><td>119 ± 006E+0</td><td>133 ± 006E+0</td><td>116 ± 005E+0</td><td>639 ± 086E-1</td><td>470 ± 064E-1</td><td>815 ± 103E-1</td><td>192 ± 023E+0</td><td>172 ± 012E+0</td><td>196 ± 007E+0</td></tr><tr><td>NGC 5055</td><td>309 ± 006E+0</td><td>414 ± 020E+0</td><td>491 ± 024E+0</td><td>402 ± 020E+0</td><td>236 ± 032E+0</td><td>155 ± 021E+0</td><td>259 ± 033E+0</td><td>558 ± 070E+0</td><td>524 ± 036E+0</td><td>558 ± 022E+0</td></tr><tr><td>NGC 5194</td><td>414 ± 008E+0</td><td>484 ± 024E+0</td><td>577 ± 029E+0</td><td>446 ± 022E+0</td><td>265 ± 035E+0</td><td>178 ± 025E+0</td><td>422 ± 053E+0</td><td>106 ± 013E+1</td><td>101 ± 007E+1</td><td>124 ± 004E+1</td></tr><tr><td>NGC 5195</td><td>112 ± 002E+0</td><td>229 ± 011E+0</td><td>274 ± 013E+0</td><td>222 ± 011E+0</td><td>830 ± 113E-1</td><td>509 ± 070E-1</td><td>461 ± 060E-1</td><td>644 ± 080E-1</td><td>997 ± 069E-1</td><td>146 ± 005E+0</td></tr><tr><td>NGC 5398</td><td>...</td><td>767 ± 040E-2</td><td>644 ± 037E-2</td><td>527 ± 035E-2</td><td>375 ± 050E-2</td><td>245 ± 036E-2</td><td>143 ± 020E-2</td><td>585 ± 075E-2</td><td>641 ± 044E-2</td><td>278 ± 013E-1</td></tr><tr><td>NGC 5457</td><td>386 ± 007E+0</td><td>435 ± 021E+0</td><td>501 ± 025E+0</td><td>440 ± 022E+0</td><td>281 ± 038E+0</td><td>189 ± 025E+0</td><td>338 ± 042E+0</td><td>761 ± 094E+0</td><td>687 ± 048E+0</td><td>105 ± 004E+1</td></tr><tr><td>NGC 5408</td><td>...</td><td>124 ± 006E-1</td><td>116 ± 006E-1</td><td>742 ± 050E-2</td><td>376 ± 071E-2</td><td>214 ± 051E-2</td><td>284 ± 053E-2</td><td>254 ± 047E-2</td><td>645 ± 045E-2</td><td>427 ± 017E-1</td></tr><tr><td>NGC 5474</td><td>222 ± 004E-1</td><td>262 ± 014E-1</td><td>305 ± 018E-1</td><td>193 ± 015E-1</td><td>108 ± 013E-1</td><td>730 ± 102E-2</td><td>555 ± 101E-2</td><td>114 ± 014E-1</td><td>100 ± 007E-1</td><td>156 ± 006E-1</td></tr><tr><td>NGC 5713</td><td>230 ± 004E-1</td><td>362 ± 018E-1</td><td>379 ± 019E-1</td><td>327 ± 016E-1</td><td>200 ± 027E-1</td><td>137 ± 019E-1</td><td>288 ± 037E-1</td><td>114 ± 014E+0</td><td>982 ± 068E-1</td><td>234 ± 009E+0</td></tr><tr><td>NGC 5866</td><td>889 ± 017E-1</td><td>129 ± 006E+0</td><td>147 ± 007E+0</td><td>125 ± 006E+0</td><td>662 ± 089E-1</td><td>420 ± 057E-1</td><td>311 ± 039E-1</td><td>314 ± 039E-1</td><td>260 ± 018E-1</td><td>213 ± 008E+0</td></tr><tr><td>IC4710</td><td>...</td><td>997 ± 054E-2</td><td>951 ± 057E-2</td><td>753 ± 054E-2</td><td>693 ± 096E-2</td><td>461 ± 064E-2</td><td>448 ± 061E-2</td><td>644 ± 082E-2</td><td>362 ± 025E-2</td><td>118 ± 005E-1</td></tr><tr><td>NGC 6822</td><td>...</td><td>177 ± 008E+0</td><td>184 ± 009E+0</td><td>146 ± 007E+0</td><td>157 ± 027E+0</td><td>973 ± 185E-1</td><td>988 ± 179E-1</td><td>122 ± 017E+0</td><td>110 ± 007E+0</td><td>313 ± 012E+0</td></tr><tr><td>NGC 6946</td><td>...</td><td>546 ± 027E+0</td><td>454 ± 022E+0</td><td>502 ± 025E+0</td><td>315 ± 042E+0</td><td>212 ± 029E+0</td><td>576 ± 072E+0</td><td>137 ± 017E+1</td><td>127 ± 008E+1</td><td>199 ± 007E+1</td></tr><tr><td>NGC 7331</td><td>169 ± 003E+0</td><td>264 ± 013E+0</td><td>320 ± 016E+0</td><td>273 ± 013E+0</td><td>158 ± 021E+0</td><td>101 ± 013E+0</td><td>185 ± 023E+0</td><td>401 ± 049E+0</td><td>335 ± 023E+0</td><td>434 ± 024E+0</td></tr><tr><td>NGC 7552</td><td>...</td><td>699 ± 035E-1</td><td>791 ± 039E-1</td><td>694 ± 035E-1</td><td>452 ± 061E-1</td><td>360 ± 049E-1</td><td>106 ± 013E+0</td><td>270 ± 033E+0</td><td>266 ± 018E+0</td><td>106 ± 004E+1</td></tr><tr><td>NGC 7793</td><td>...</td><td>164 ± 008E+0</td><td>168 ± 008E+0</td><td>130 ± 006E+0</td><td>744 ± 103E-1</td><td>481 ± 064E-1</td><td>104 ± 013E+0</td><td>189 ± 023E+0</td><td>147 ± 010E+0</td><td>209 ± 008E+0</td></tr><tr><td>Filter</td><td>Spitzer<br>MIPS</td><td>Herschel<br>PACS</td><td>Herschel<br>PACS</td><td>Spitzer<br>MIPS</td><td>Herschel<br>PACS</td><td>Herschel<br>SPIRE</td><td>Herschel<br>SPIRE</td><td>Herschel<br>SPIRE</td><td>JCMT<br>SCUBA</td><td>Planck<br>HFI</td></tr><tr><td>λ&#773;(μm)</td><td>72.5</td><td>71.8</td><td>103</td><td>157</td><td>167</td><td>252</td><td>353</td><td>511</td><td>850</td><td>850</td></tr><tr><td>Δλ (μm)</td><td>21.3</td><td>21.3</td><td>30.6</td><td>35.8</td><td>68.5</td><td>67.3</td><td>95.2</td><td>184</td><td>247</td><td>238</td></tr><tr><td>Δλ/Δν</td><td>0.00231</td><td>0.00231</td><td>0.00104</td><td>0.000388</td><td>0.000388</td><td>0.000152</td><td>0.0000725</td><td>0.0000361</td><td>0.0000146</td><td>0.0</td></tr><tr><td>NGC 0024</td><td>222 ± 015E+0</td><td>...</td><td>...</td><td>712 ± 085E+0</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>457 ± 091E-1</td></tr><tr><td>NGC 0337</td><td>111 ± 007E+1</td><td>139 ± 006E+1</td><td>210 ± 010E+1</td><td>200 ± 024E+1</td><td>197 ± 009E+1</td><td>894 ± 063E+0</td><td>405 ± 028E+0</td><td>158 ± 011E+0</td><td>349 ± 052E-1</td><td>573 ± 234E-1</td></tr><tr><td>NGC 0584</td><td>175 ± 045E-1</td><td>180 ± 025E-1</td><td>300 ± 033E-1</td><td>118 ± 030E+0</td><td>610 ± 038E-1</td><td>&lt;838E-1</td><td>&lt;603E-1</td><td>&lt;419E-1</td><td>...</td><td>...</td></tr><tr><td>NGC 0628</td><td>338 ± 023E+1</td><td>420 ± 021E+1</td><td>836 ± 041E+1</td><td>111 ± 013E+2</td><td>114 ± 005E+2</td><td>621 ± 044E+1</td><td>298 ± 021E+1</td><td>114 ± 008E+1</td><td>...</td><td>198 ± 015E+0</td></tr><tr><td>NGC 0855</td><td>168 ± 011E+0</td><td>208 ± 010E+0</td><td>253 ± 013E+0</td><td>222 ± 026E+0</td><td>206 ± 010E+0</td><td>135 ± 009E+0</td><td>726 ± 052E-1</td><td>222 ± 018E-1</td><td>...</td><td>...</td></tr><tr><td>NGC 0925</td><td>143 ± 010E+1</td><td>136 ± 006E+1</td><td>289 ± 014E+1</td><td>433 ± 052E+1</td><td>372 ± 018E+1</td><td>251 ± 017E+1</td><td>138 ± 009E+1</td><td>652 ± 046E+0</td><td>...</td><td>...</td></tr></tbody></table>
<table><caption>Table 2
(Continued)</caption><thead><tr><th>Filter</th><th>Spitzer<br>MIPS</th><th>Herschel<br>PACS</th><th>Herschel<br>PACS</th><th>Spitzer<br>MIPS</th><th>Herschel<br>PACS</th><th>Herschel<br>SPIRE</th><th>Herschel<br>SPIRE</th><th>Herschel<br>SPIRE</th><th>JCMT<br>SCUBA</th><th>Planck<br>HFI</th></tr></thead><tbody><tr><td>λ&#773;(μm)</td><td>72.5</td><td>71.8</td><td>103</td><td>157</td><td>167</td><td>252</td><td>353</td><td>511</td><td>850</td><td>850</td></tr><tr><td>Δλ (μm)</td><td>21.3</td><td>21.3</td><td>30.6</td><td>35.8</td><td>68.5</td><td>67.3</td><td>95.2</td><td>184</td><td>247</td><td>238</td></tr><tr><td>Δλ/Δν</td><td>0.00231</td><td>0.00231</td><td>0.00104</td><td>0.000388</td><td>0.000388</td><td>0.000152</td><td>0.0000725</td><td>0.0000361</td><td>0.0000146</td><td>0.0</td></tr><tr><td>NGC 1097</td><td>598 ± 046E+1</td><td>787 ± 039E+1</td><td>123 ± 006E+2</td><td>153 ± 018E+2</td><td>132 ± 006E+2</td><td>669 ± 047E+1</td><td>293 ± 020E+1</td><td>106 ± 007E+1</td><td>144 ± 078E+0</td><td>212 ± 012E+0</td></tr><tr><td>NGC 1266</td><td>126 ± 009E+1</td><td>148 ± 007E+1</td><td>171 ± 008E+1</td><td>102 ± 012E+1</td><td>113 ± 005E+1</td><td>404 ± 028E+0</td><td>145 ± 010E+0</td><td>402 ± 030E+1</td><td>...</td><td>...</td></tr><tr><td>NGC 1291</td><td>527 ± 037E+0</td><td>439 ± 027E+0</td><td>135 ± 007E+1</td><td>262 ± 031E+1</td><td>226 ± 011E+1</td><td>151 ± 010E+1</td><td>757 ± 054E+0</td><td>309 ± 022E+0</td><td>...</td><td>...</td></tr><tr><td>NGC 1316</td><td>543 ± 040E+0</td><td>568 ± 029E+0</td><td>997 ± 050E+0</td><td>126 ± 017E+1</td><td>123 ± 006E+1</td><td>494 ± 035E+0</td><td>204 ± 015E+0</td><td>707 ± 058E+1</td><td>...</td><td>...</td></tr><tr><td>NGC 1377</td><td>634 ± 046E+0</td><td>725 ± 036E+0</td><td>651 ± 032E+0</td><td>338 ± 042E+0</td><td>337 ± 016E+0</td><td>122 ± 008E+0</td><td>469 ± 034E+1</td><td>163 ± 013E+1</td><td>...</td><td>...</td></tr><tr><td>NGC 1404</td><td>&lt;165E-1</td><td>&lt;214E-1</td><td>&lt;252E-1</td><td>&lt;286E-1</td><td>&lt;204E-1</td><td>&lt;154E-1</td><td>&lt;134E-1</td><td>&lt;909E-2</td><td>...</td><td>...</td></tr><tr><td>IC0342</td><td>351 ± 024E+2</td><td>470 ± 023E+2</td><td>894 ± 044E+2</td><td>914 ± 109E+2</td><td>107 ± 005E+3</td><td>564 ± 040E+2</td><td>251 ± 017E+2</td><td>922 ± 065E+1</td><td>...</td><td>...</td></tr><tr><td>NGC 1482</td><td>324 ± 028E+1</td><td>419 ± 020E+1</td><td>522 ± 026E+1</td><td>387 ± 046E+1</td><td>419 ± 021E+1</td><td>154 ± 010E+1</td><td>582 ± 041E+0</td><td>176 ± 012E+0</td><td>330 ± 050E-1</td><td>...</td></tr><tr><td>NGC 1512</td><td>682 ± 048E+0</td><td>752 ± 039E+0</td><td>150 ± 007E+1</td><td>196 ± 023E+1</td><td>191 ± 009E+1</td><td>147 ± 010E+1</td><td>866 ± 062E+0</td><td>363 ± 026E+0</td><td>...</td><td>551 ± 090E-1</td></tr><tr><td>NGC 1566</td><td>343 ± 025E+1</td><td>...</td><td>...</td><td>102 ± 012E+2</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>142 ± 010E+0</td></tr><tr><td>NGC 1705</td><td>124 ± 008E+0</td><td>...</td><td>...</td><td>139 ± 016E+0</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 2146</td><td>215 ± 015E+2</td><td>198 ± 009E+2</td><td>236 ± 011E+2</td><td>119 ± 014E+2</td><td>174 ± 008E+2</td><td>613 ± 043E+1</td><td>221 ± 015E+1</td><td>681 ± 048E+0</td><td>...</td><td>...</td></tr><tr><td>NGC 2403</td><td>857 ± 060E+1</td><td>994 ± 049E+1</td><td>...</td><td>225 ± 027E+2</td><td>192 ± 009E+2</td><td>119 ± 008E+2</td><td>627 ± 048E+1</td><td>279 ± 024E+1</td><td>...</td><td>422 ± 032E+0</td></tr><tr><td>HoII</td><td>318 ± 022E+0</td><td>438 ± 022E+0</td><td>574 ± 028E+0</td><td>346 ± 042E+0</td><td>363 ± 018E+0</td><td>152 ± 011E+0</td><td>771 ± 067E-1</td><td>284 ± 142E-1</td><td>...</td><td>...</td></tr><tr><td>M81dwA</td><td>&lt;149E-1</td><td>...</td><td>...</td><td>&lt;143E-1</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>DDO 053</td><td>315 ± 025E-1</td><td>400 ± 025E-1</td><td>519 ± 031E-1</td><td>357 ± 050E-1</td><td>300 ± 020E-1</td><td>138 ± 014E-1</td><td>989 ± 106E-2</td><td>&lt;389E-2</td><td>...</td><td>...</td></tr><tr><td>NGC 2798</td><td>217 ± 017E+1</td><td>250 ± 012E+1</td><td>287 ± 014E+1</td><td>206 ± 024E+1</td><td>202 ± 010E+1</td><td>740 ± 052E+0</td><td>272 ± 019E+0</td><td>853 ± 061E-1</td><td>194 ± 032E-1</td><td>...</td></tr><tr><td>NGC 2841</td><td>102 ± 007E+1</td><td>110 ± 005E+1</td><td>286 ± 014E+1</td><td>622 ± 075E+1</td><td>488 ± 024E+1</td><td>321 ± 022E+1</td><td>152 ± 010E+1</td><td>589 ± 041E+0</td><td>...</td><td>122 ± 010E+0</td></tr><tr><td>NGC 2915</td><td>140 ± 010E+0</td><td>107 ± 005E+0</td><td>180 ± 009E+0</td><td>145 ± 026E+0</td><td>162 ± 008E+0</td><td>816 ± 059E-1</td><td>463 ± 034E-1</td><td>204 ± 016E-1</td><td>...</td><td>...</td></tr><tr><td>HoI</td><td>292 ± 028E-1</td><td>280 ± 031E-1</td><td>441 ± 039E-1</td><td>526 ± 075E-1</td><td>552 ± 039E-1</td><td>369 ± 031E-1</td><td>229 ± 020E-1</td><td>108 ± 012E-1</td><td>...</td><td>...</td></tr><tr><td>NGC 2976</td><td>199 ± 013E+1</td><td>209 ± 010E+1</td><td>372 ± 018E+1</td><td>426 ± 051E+1</td><td>459 ± 022E+1</td><td>242 ± 017E+1</td><td>113 ± 008E+1</td><td>442 ± 031E+0</td><td>609 ± 236E-1</td><td>110 ± 022E+0</td></tr><tr><td>NGC 3049</td><td>289 ± 021E+0</td><td>382 ± 019E+0</td><td>529 ± 026E+0</td><td>486 ± 059E+0</td><td>493 ± 024E+0</td><td>259 ± 018E+0</td><td>131 ± 009E+0</td><td>644 ± 046E-1</td><td>...</td><td>...</td></tr><tr><td>NGC 3031</td><td>852 ± 059E+1</td><td>997 ± 049E+1</td><td>...</td><td>308 ± 037E+2</td><td>281 ± 014E+2</td><td>176 ± 013E+2</td><td>876 ± 070E+1</td><td>364 ± 034E+1</td><td>...</td><td>...</td></tr><tr><td>NGC 3034</td><td>162 ± 048E+3<sup>a</sup></td><td>209 ± 010E+3</td><td>...</td><td>857 ± 257E+2<sup>a</sup></td><td>142 ± 007E+3</td><td>442 ± 031E+2</td><td>151 ± 010E+2</td><td>456 ± 033E+1</td><td>551 ± 082E+0</td><td>900 ± 018E+0</td></tr><tr><td>HoIX</td><td>&lt;228E-1</td><td>...</td><td>...</td><td>&lt;457E-1</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 3077</td><td>196 ± 013E+1</td><td>213 ± 010E+1</td><td>292 ± 014E+1</td><td>281 ± 033E+1</td><td>278 ± 013E+1</td><td>132 ± 009E+1</td><td>613 ± 043E+0</td><td>237 ± 017E+0</td><td>...</td><td>...</td></tr><tr><td>M81dwB</td><td>114 ± 012E-1</td><td>903 ± 116E-2</td><td>270 ± 018E-1</td><td>161 ± 027E-1</td><td>292 ± 018E-1</td><td>176 ± 014E-1</td><td>104 ± 010E-1</td><td>426 ± 213E-2</td><td>...</td><td>...</td></tr><tr><td>NGC 3190</td><td>565 ± 040E+0</td><td>629 ± 031E+0</td><td>109 ± 005E+1</td><td>150 ± 018E+1</td><td>153 ± 007E+1</td><td>819 ± 058E+0</td><td>348 ± 024E+0</td><td>118 ± 008E+0</td><td>189 ± 035E-1</td><td>...</td></tr><tr><td>NGC 3184</td><td>157 ± 011E+1</td><td>180 ± 009E+1</td><td>392 ± 019E+1</td><td>704 ± 084E+1</td><td>537 ± 026E+1</td><td>314 ± 022E+1</td><td>146 ± 010E+1</td><td>577 ± 041E+0</td><td>...</td><td>126 ± 009E+0</td></tr><tr><td>NGC 3198</td><td>102 ± 007E+1</td><td>109 ± 005E+1</td><td>224 ± 011E+1</td><td>389 ± 049E+1</td><td>296 ± 014E+1</td><td>182 ± 012E+1</td><td>955 ± 067E+0</td><td>403 ± 028E+0</td><td>...</td><td>105 ± 010E+0</td></tr><tr><td>IC2574</td><td>483 ± 034E+0</td><td>578 ± 029E+0</td><td>937 ± 047E+0</td><td>105 ± 012E+1</td><td>986 ± 049E+0</td><td>569 ± 040E+0</td><td>412 ± 029E+0</td><td>165 ± 012E+0</td><td>...</td><td>...</td></tr><tr><td>NGC 3265</td><td>270 ± 019E+0</td><td>292 ± 014E+0</td><td>322 ± 016E+0</td><td>270 ± 034E+0</td><td>285 ± 014E+0</td><td>115 ± 008E+0</td><td>509 ± 037E-1</td><td>194 ± 015E-1</td><td>...</td><td>...</td></tr><tr><td>Mrk 33</td><td>434 ± 031E+0</td><td>...</td><td>...</td><td>386 ± 047E+0</td><td>...</td><td>...</td><td>...</td><td>...</td><td>400 ± 060E-2</td><td>...</td></tr><tr><td>NGC 3351</td><td>218 ± 015E+1</td><td>270 ± 013E+1</td><td>486 ± 024E+1</td><td>569 ± 068E+1</td><td>538 ± 026E+1</td><td>313 ± 022E+1</td><td>138 ± 009E+1</td><td>480 ± 034E+0</td><td>...</td><td>102 ± 009E+0</td></tr><tr><td>NGC 3521</td><td>644 ± 045E+1</td><td>800 ± 040E+1</td><td>163 ± 008E+2</td><td>195 ± 023E+2</td><td>203 ± 010E+2</td><td>106 ± 007E+2</td><td>459 ± 032E+1</td><td>164 ± 011E+1</td><td>210 ± 082E+0</td><td>312 ± 014E+0</td></tr><tr><td>NGC 3621</td><td>501 ± 039E+1</td><td>504 ± 025E+1</td><td>101 ± 005E+2</td><td>139 ± 017E+2</td><td>124 ± 006E+2</td><td>649 ± 046E+1</td><td>305 ± 021E+1</td><td>123 ± 008E+1</td><td>...</td><td>...</td></tr><tr><td>NGC 3627</td><td>918 ± 070E+1</td><td>107 ± 005E+2</td><td>188 ± 009E+2</td><td>215 ± 027E+2</td><td>196 ± 009E+2</td><td>904 ± 064E+1</td><td>360 ± 025E+1</td><td>120 ± 008E+1</td><td>186 ± 070E+0</td><td>228 ± 011E+0</td></tr><tr><td>NGC 3773</td><td>157 ± 012E+0</td><td>139 ± 029E+0</td><td>214 ± 010E+0</td><td>238 ± 033E+0</td><td>206 ± 010E+0</td><td>945 ± 067E-1</td><td>414 ± 030E-1</td><td>155 ± 011E-1</td><td>...</td><td>...</td></tr><tr><td>NGC 3938</td><td>142 ± 010E+1</td><td>164 ± 008E+1</td><td>307 ± 015E+1</td><td>519 ± 062E+1</td><td>392 ± 019E+1</td><td>219 ± 015E+1</td><td>983 ± 069E+0</td><td>365 ± 026E+0</td><td>...</td><td>883 ± 083E-1</td></tr><tr><td>NGC 4125</td><td>111 ± 010E+0</td><td>740 ± 041E-1</td><td>...</td><td>176 ± 027E+0</td><td>183 ± 009E+0</td><td>895 ± 286E-1</td><td>509 ± 210E-1</td><td>239 ± 159E-1</td><td>...</td><td>...</td></tr><tr><td>NGC 4236</td><td>801 ± 056E+0</td><td>803 ± 041E+0</td><td>113 ± 005E+1</td><td>161 ± 019E+1</td><td>172 ± 008E+1</td><td>107 ± 007E+1</td><td>694 ± 049E+0</td><td>356 ± 025E+0</td><td>...</td><td>727 ± 101E-1</td></tr><tr><td>NGC 4254</td><td>502 ± 036E+1</td><td>596 ± 029E+1</td><td>110 ± 005E+2</td><td>142 ± 017E+2</td><td>126 ± 006E+2</td><td>618 ± 043E+1</td><td>249 ± 017E+1</td><td>833 ± 059E+0</td><td>100 ± 054E+0</td><td>159 ± 009E+0</td></tr><tr><td>NGC 4321</td><td>405 ± 028E+1</td><td>440 ± 022E+1</td><td>907 ± 045E+1</td><td>139 ± 016E+2</td><td>116 ± 005E+2</td><td>627 ± 044E+1</td><td>265 ± 018E+1</td><td>901 ± 064E+0</td><td>875 ± 493E-1</td><td>165 ± 008E+0</td></tr><tr><td>NGC 4450</td><td>342 ± 028E+0</td><td>...</td><td>...</td><td>169 ± 021E+1</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr></tbody></table>
<table><caption>**Table 2**
(Continued)</caption><thead><tr><th>Filter</th><th>Spitzer<br>MIPS</th><th>Herschel<br>PACS</th><th>Herschel<br>PACS</th><th>Spitzer<br>MIPS</th><th>Herschel<br>PACS</th><th>Herschel<br>SPIRE</th><th>Herschel<br>SPIRE</th><th>Herschel<br>SPIRE</th><th>JCMT<br>SCUBA</th><th>Planck<br>HFI</th></tr></thead><tbody><tr><td>λ(μm)</td><td>72.5</td><td>71.8</td><td>103</td><td>157</td><td>167</td><td>252</td><td>353</td><td>511</td><td>850</td><td>850</td></tr><tr><td>Δλ (μm)</td><td>21.3</td><td>21.3</td><td>30.6</td><td>35.8</td><td>68.5</td><td>67.3</td><td>95.2</td><td>184</td><td>247</td><td>238</td></tr><tr><td>A<sub>λ</sub>/A<sub>V</sub></td><td>0.00231</td><td>0.00231</td><td>0.00104</td><td>0.000388</td><td>0.000388</td><td>0.000152</td><td>0.0000725</td><td>0.0000361</td><td>0.0000146</td><td>0.0</td></tr><tr><td>NGC 4536</td><td>319 ± 024E+1</td><td>419 ± 020E+1</td><td>567 ± 028E+1</td><td>580 ± 070E+1</td><td>555 ± 027E+1</td><td>268 ± 019E+1</td><td>121 ± 008E+1</td><td>462 ± 032E+0</td><td>414 ± 112E-1</td><td>967 ± 078E-1</td></tr><tr><td>NGC 4552</td><td>537 ± 110E-1</td><td>...</td><td>...</td><td>142 ± 073E+0</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 4559</td><td>168 ± 011E+1</td><td>180 ± 009E+1</td><td>337 ± 016E+1</td><td>541 ± 065E+1</td><td>405 ± 020E+1</td><td>236 ± 016E+1</td><td>122 ± 008E+1</td><td>529 ± 037E+0</td><td>...</td><td>148 ± 011E+0</td></tr><tr><td>NGC 4569</td><td>123 ± 008E+1</td><td>148 ± 007E+1</td><td>325 ± 016E+1</td><td>412 ± 051E+1</td><td>400 ± 020E+1</td><td>209 ± 014E+1</td><td>900 ± 063E+0</td><td>309 ± 022E+0</td><td>464 ± 082E-1</td><td>615 ± 081E-1</td></tr><tr><td>NGC 4579</td><td>952 ± 075E+0</td><td>999 ± 050E+0</td><td>254 ± 012E+1</td><td>410 ± 049E+1</td><td>345 ± 017E+1</td><td>194 ± 013E+1</td><td>844 ± 059E+0</td><td>297 ± 021E+0</td><td>439 ± 066E-1</td><td>625 ± 112E-1</td></tr><tr><td>NGC 4594</td><td>730 ± 051E+0</td><td>808 ± 041E+0</td><td>259 ± 013E+1</td><td>406 ± 048E+1</td><td>380 ± 019E+1</td><td>238 ± 016E+1</td><td>116 ± 008E+1</td><td>477 ± 034E+0</td><td>372 ± 108E-1</td><td>122 ± 014E+0</td></tr><tr><td>NGC 4625</td><td>185 ± 013E+0</td><td>151 ± 008E+0</td><td>376 ± 019E+0</td><td>508 ± 061E+0</td><td>469 ± 023E+0</td><td>256 ± 018E+0</td><td>130 ± 009E+0</td><td>549 ± 040E-1</td><td>...</td><td>...</td></tr><tr><td>NGC 4631</td><td>138 ± 009E+2</td><td>140 ± 007E+2</td><td>233 ± 011E+2</td><td>269 ± 032E+2</td><td>238 ± 011E+2</td><td>114 ± 008E+2</td><td>523 ± 037E+1</td><td>201 ± 014E+1</td><td>573 ± 120E+0</td><td>421 ± 017E+0</td></tr><tr><td>NGC 4725</td><td>885 ± 066E+0</td><td>103 ± 005E+1</td><td>260 ± 013E+1</td><td>599 ± 073E+1</td><td>466 ± 023E+1</td><td>302 ± 021E+1</td><td>160 ± 011E+1</td><td>648 ± 046E+0</td><td>...</td><td>128 ± 011E+0</td></tr><tr><td>NGC 4736</td><td>100 ± 007E+2</td><td>107 ± 005E+2</td><td>165 ± 008E+2</td><td>164 ± 019E+2</td><td>141 ± 007E+2</td><td>635 ± 045E+1</td><td>260 ± 018E+1</td><td>901 ± 064E+0</td><td>153 ± 065E+0</td><td>169 ± 011E+0</td></tr><tr><td>DDO 154</td><td>&lt;591E-2</td><td>&lt;775E-2</td><td>&lt;912E-2</td><td>&lt;223E-1</td><td>&lt;801E-2</td><td>&lt;514E-2</td><td>&lt;483E-2</td><td>&lt;349E-2</td><td>...</td><td>...</td></tr><tr><td>NGC 4826</td><td>528 ± 037E+1</td><td>563 ± 028E+1</td><td>975 ± 048E+1</td><td>857 ± 102E+1</td><td>906 ± 045E+1</td><td>393 ± 027E+1</td><td>156 ± 011E+1</td><td>516 ± 036E+0</td><td>123 ± 030E+0</td><td>101 ± 008E+0</td></tr><tr><td>DDO 165</td><td>&lt;141E-1</td><td>&lt;976E-2</td><td>&lt;119E-1</td><td>&lt;205E-1</td><td>&lt;101E-1</td><td>&lt;762E-2</td><td>&lt;713E-2</td><td>&lt;484E-2</td><td>...</td><td>...</td></tr><tr><td>NGC 5033</td><td>288 ± 020E+1</td><td>...</td><td>...</td><td>910 ± 111E+1</td><td>...</td><td>...</td><td>...</td><td>...</td><td>109 ± 055E+0</td><td>137 ± 010E+0</td></tr><tr><td>NGC 5055</td><td>744 ± 052E+1</td><td>764 ± 038E+1</td><td>175 ± 008E+2</td><td>273 ± 032E+2</td><td>241 ± 012E+2</td><td>138 ± 009E+2</td><td>611 ± 043E+1</td><td>221 ± 015E+1</td><td>...</td><td>397 ± 015E+0</td></tr><tr><td>NGC 5194</td><td>156 ± 010E+2</td><td>180 ± 009E+2</td><td>...</td><td>477 ± 057E+2</td><td>409 ± 020E+2</td><td>203 ± 014E+2</td><td>831 ± 064E+1</td><td>294 ± 029E+1</td><td>261 ± 039E+0</td><td>512 ± 022E+0</td></tr><tr><td>NGC 5195</td><td>971 ± 068E+0</td><td>217 ± 010E+1</td><td>...</td><td>129 ± 015E+1</td><td>279 ± 013E+1</td><td>123 ± 009E+1</td><td>446 ± 040E+0</td><td>152 ± 022E+0</td><td>259 ± 039E-1</td><td>...</td></tr><tr><td>NGC 5398</td><td>203 ± 015E+0</td><td>245 ± 012E+0</td><td>333 ± 016E+0</td><td>351 ± 050E+0</td><td>283 ± 014E+0</td><td>186 ± 013E+0</td><td>101 ± 007E+0</td><td>489 ± 035E-1</td><td>...</td><td>...</td></tr><tr><td>NGC 5457</td><td>118 ± 008E+2</td><td>135 ± 006E+2</td><td>262 ± 013E+2</td><td>399 ± 047E+2</td><td>336 ± 016E+2</td><td>194 ± 013E+2</td><td>942 ± 066E+1</td><td>388 ± 027E+1</td><td>...</td><td>...</td></tr><tr><td>NGC 5408</td><td>358 ± 026E+0</td><td>369 ± 018E+0</td><td>275 ± 014E+0</td><td>256 ± 037E+0</td><td>231 ± 011E+0</td><td>822 ± 060E-1</td><td>416 ± 032E-1</td><td>147 ± 014E-1</td><td>...</td><td>...</td></tr><tr><td>NGC 5474</td><td>347 ± 024E+0</td><td>354 ± 018E+0</td><td>604 ± 031E+0</td><td>913 ± 109E+0</td><td>853 ± 043E+0</td><td>482 ± 034E+0</td><td>280 ± 020E+0</td><td>134 ± 009E+0</td><td>...</td><td>377 ± 085E-1</td></tr><tr><td>NGC 5713</td><td>236 ± 018E+1</td><td>295 ± 014E+1</td><td>421 ± 021E+1</td><td>396 ± 047E+1</td><td>385 ± 019E+1</td><td>156 ± 011E+1</td><td>608 ± 043E+0</td><td>193 ± 013E+0</td><td>572 ± 119E-1</td><td>500 ± 116E-1</td></tr><tr><td>NGC 5866</td><td>870 ± 063E+0</td><td>880 ± 044E+0</td><td>180 ± 009E+1</td><td>177 ± 021E+1</td><td>178 ± 008E+1</td><td>757 ± 053E+0</td><td>305 ± 021E+0</td><td>965 ± 072E-1</td><td>140 ± 020E-1</td><td>192 ± 067E-1</td></tr><tr><td>IC4710</td><td>237 ± 018E+0</td><td>...</td><td>...</td><td>356 ± 048E+0</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 6822</td><td>636 ± 044E+1</td><td>...</td><td>...</td><td>143 ± 017E+2</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 6946</td><td>206 ± 016E+2</td><td>252 ± 012E+2</td><td>457 ± 022E+2</td><td>502 ± 060E+2</td><td>525 ± 026E+2</td><td>256 ± 018E+2</td><td>106 ± 007E+2</td><td>362 ± 025E+1</td><td>298 ± 044E+0</td><td>...</td></tr><tr><td>NGC 7331</td><td>749 ± 066E+1</td><td>688 ± 034E+1</td><td>135 ± 006E+2</td><td>189 ± 024E+2</td><td>171 ± 008E+2</td><td>882 ± 062E+1</td><td>385 ± 027E+1</td><td>139 ± 009E+1</td><td>211 ± 038E+0</td><td>...</td></tr><tr><td>NGC 7552</td><td>675 ± 110E+1</td><td>...</td><td>...</td><td>933 ± 112E+1</td><td>...</td><td>...</td><td>...</td><td>...</td><td>795 ± 166E-1</td><td>921 ± 085E-1</td></tr><tr><td>NGC 7793</td><td>329 ± 023E+1</td><td>350 ± 017E+1</td><td>695 ± 034E+1</td><td>107 ± 012E+2</td><td>901 ± 045E+1</td><td>526 ± 037E+1</td><td>276 ± 019E+1</td><td>117 ± 008E+1</td><td>...</td><td>283 ± 013E+0</td></tr></tbody></table>

Note. The compact table entry format TUV ± WXYEZ implies (T.UV ± W.XY) × 10$^2$ in Jy. Corrections for neither Galactic nor intrinsic extinction have been applied (see Section 3). The uncertainties include both statistical and systematic effects. 5σ upper limits are provided for non-detections. No color corrections have been applied. The filter central wavelengths and widths are computed via Equations (1) and (2).

a The Spitzer MIPS data for NGC 3034 suffer from saturation, and thus the tabulated values are lower limits.
<table><caption>**Table 3**
BVR<sub>C</sub>I<sub>C</sub> Photometry/Calibration Source</caption><thead><tr><th>Galaxy</th><th>B</th><th>V</th><th>R<sub>C</sub></th><th>I<sub>C</sub></th></tr></thead><tbody><tr><td>NGC 0024</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 0337</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 0584</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 0628</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 0855</td><td>RC3</td><td>RC3</td><td>C14</td><td>...</td></tr><tr><td>NGC 0925</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 1097</td><td>MM09</td><td>MM09</td><td>MM09</td><td>MM09</td></tr><tr><td>NGC 1266</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 1291</td><td>MM09</td><td>MM09</td><td>MM09</td><td>MM09</td></tr><tr><td>NGC 1316</td><td>MM09</td><td>MM09</td><td>MM09</td><td>MM09</td></tr><tr><td>NGC 1377</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 1404</td><td>MM09</td><td>MM09</td><td>MM09</td><td>MM09</td></tr><tr><td>IC0342</td><td>RC3</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 1482</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 1512</td><td>MM09</td><td>MM09</td><td>MM09</td><td>MM09</td></tr><tr><td>NGC 1566</td><td>MM09</td><td>MM09</td><td>MM09</td><td>MM09</td></tr><tr><td>NGC 1705</td><td>MM09</td><td>MM09</td><td>MM09</td><td>MM09</td></tr><tr><td>NGC 2403</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 2146</td><td>RC3</td><td>RC3</td><td>...</td><td>T09</td></tr><tr><td>HolmbII</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>M81dwA</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>DDO 053</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 2798</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 2841</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 2915</td><td>RC3</td><td>MM09</td><td>MM09</td><td>D07</td></tr><tr><td>HolmbI</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 2976</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 3049</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 3031</td><td>RC3</td><td>RC3</td><td>...</td><td>T09</td></tr><tr><td>NGC 3034</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>HolmbIX</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 3077</td><td>C14</td><td>...</td><td>RC3</td><td>...</td></tr><tr><td>M81dwB</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 3190</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 3184</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 3198</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>IC2574</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 3265</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>Mrk 33</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 3351</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 3521</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 3621</td><td>MM09</td><td>MM09</td><td>MM09</td><td>MM09</td></tr><tr><td>NGC 3627</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 3773</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 3938</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 4125</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 4236</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 4254</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 4321</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 4450</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 4536</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 4552</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 4559</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 4569</td><td>RC3</td><td>RC3</td><td>...</td><td>...</td></tr><tr><td>NGC 4579</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 4594</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 4625</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 4631</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 4725</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 4736</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>DDO 154</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 4826</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>DDO 165</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 5033</td><td>PS1</td><td>PS1</td><td>...</td><td>PS1</td></tr></tbody></table>

<table><caption>**Table 3**
(Continued)</caption><thead><tr><th>Galaxy</th><th>B</th><th>V</th><th>R<sub>C</sub></th><th>I<sub>C</sub></th></tr></thead><tbody><tr><td>NGC 5055</td><td>RC3</td><td>RC3</td><td>C14</td><td>T09</td></tr><tr><td>NGC 5194</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 5195</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 5398</td><td>D07</td><td>D07</td><td>D07</td><td>D07</td></tr><tr><td>NGC 5457</td><td>RC3</td><td>RC3</td><td>C14</td><td>T09</td></tr><tr><td>NGC 5408</td><td>RC3</td><td>RC3</td><td>...</td><td>...</td></tr><tr><td>NGC 5474</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 5713</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 5866</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>IC4710</td><td>D07</td><td>D07</td><td>D07</td><td>...</td></tr><tr><td>NGC 6822</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 6946</td><td>RC3</td><td>PS1</td><td>...</td><td>PS1</td></tr><tr><td>NGC 7331</td><td>PS1</td><td>PS1</td><td>PS1</td><td>PS1</td></tr><tr><td>NGC 7552</td><td>MM09</td><td>MM09</td><td>D07</td><td>D07</td></tr><tr><td>NGC 7793</td><td>D07</td><td>D07</td><td>D07</td><td>D07</td></tr></tbody></table>

Note. PS1: recalibration of Dale et al. (2007) photometry using Pan-STARRS1 (Section 3.1); D07: Dale et al. (2007); MM09: Muñoz-Mateos et al. (2009); C14: Cook et al. (2014); T09: unpublished photometry from M. Pierce via the Extragalactic Distance Database (Tully et al. 2009); RC3: de Vaucouleurs et al. (1991).

procedures for these 6 galaxies are described in Bendo et al. (2010).

The Herschel PACS and SPIRE imaging data for these 61 + 6 = 67 KINGFISH + VNGS galaxies for this publication were processed from Level 0 to Level 1 using HIPE Version 11.0.24 and the Level 1 to Level 2 post-pipeline processing used Scanamorphos Version 24.0 (Roussel 2013); the data published in Dale et al. (2012) were processed using HIPE Version 5.0 and Scanamorphos Version 12.5. With this newer version of Scanamorphos, the PACS distortion flatfield is now properly incorporated. In practice, this has decreased the noise levels in the PACS maps and slightly modified the PACS flux calibration (~1%). Moreover, the destriping of PACS observations of large and diffuse fields is substantially improved, and the subtraction of the average drift on short timescales no longer introduces low-level noise. These changes allow for more secure detections of diffuse emission and more robust estimates of sky levels.

One important factor involved in the SPIRE flux calibration is the SPIRE beam size, since the SPIRE images are converted into surface brightness units by dividing by the estimated beam areas. The updated beam sizes used for this work at [250, 350, 500] µm are [469.35, 831.27, 1804.31] arcsec², representing percentage increases of [11.0, 10.7, 13.7]% compared to the previous values of [423, 751, 1587] arcsec² used by Dale et al. (2012). These updated values are the recommended beam sizes in Version 3.0 (2016 June 03) of the SPIRE Handbook.

The PACS fractional calibration uncertainties are of order $\epsilon_{cal}/f_{\nu} \sim 5\%$, according to Version 2.5.1 (2013 July 09) of the PACS Observer's Manual. Calibration uncertainties for SPIRE data are estimated at $\epsilon_{cal}/f_{\nu} \sim 7\%$, also taken from Version 3.0 of the SPIRE Observer's Manual. This level of uncertainty in the SPIRE calibration is a sum in quadrature of the uncertainties in the absolute and relative calibrations (~5.5%) along with the uncertainties in the extended source calibration (~4%).

<footnote n="24">24 Version 14.0.0 was used for the six VNGS galaxies. This version provides better deglitched SPIRE maps and a slightly improved extended source calibration for PACS.</footnote>
### 3.3. WISE 12 µm

WISE 12 µm imaging (Wright et al. 2010) is used here to help bridge the gap in wavelength coverage in our broadband SEDs between the Spitzer 8 and 24 µm bandpasses. The 12 µm bandpass is an important tracer of the PAH complexes centered near (restframe) wavelengths of 11.3, 12.7, and 17 µm (Smith et al. 2007). At 12 µm, the (single-frame) WISE PSF full-width at half maximum (FWHM) is 6.5 and the photometric calibration ~7%.<fnref n="25" /> A full suite of WISE W1, W2, W3, and W4 (3.4, 4.6, 12, and 22 µm) “total” flux densities is provided in Table 4 (see the Appendix). We use native resolution imaging (not the drizzled Atlas release imaging), which provides superior resolution and minimizes the need for aperture corrections.

### 3.4. Planck 850 µm

There are SCUBA 850 µm flux densities available for only 27 galaxies in the SINGS/KINGFISH sample, and we therefore supplement these data with Planck 850 µm flux densities for 36 galaxies; the total number of 850 µm detections for the combined Planck/SCUBA SINGS/KINGFISH sample is 43. We use cataloged Planck 850 µm flux densities derived from the APERFLUX technique, a technique that employs circular apertures plus concentric sky annuli. Of the different flavors of Planck flux density extractions, APERFLUX is the simplest method and relies on the fewest assumptions; the Planck team recommends APERFLUX for wavelengths 850 µm and shorter (Planck Collaboration et al. 2016a). Although some of the SCUBA 850 µm data suffer from relatively small maps and spatial filtering issues, the lower resolution Planck data may be affected by foreground or background sources.

### 3.5. Sky Estimation and Elimination of Spatial Interlopers

The “sky” in the direction of any galaxy is a superposition of emission from faint foreground stars and background galaxies, interstellar emission, and in the case of ground-based observations, the Earth’s atmosphere. To determine the sky level for each image, a set of sky apertures has been defined (by eye) that collectively circumscribe the galaxy, projected on the sky close enough to the galaxy to measure the “local” sky, but far enough away to avoid any galaxy emission (the process is unchanged from Dale et al. 2012, see their Figure 1).

Before estimating the sky levels and executing aperture photometry, any emission from obvious foreground stars or from neighboring or background galaxies is identified and removed from the areas covered by each galaxy’s aperture and collection of sky apertures. The identification is assisted by ancillary data at shorter wavelengths and higher spatial resolution (e.g., Spitzer/IRAC 3.6 and 8.0 µm, HST optical, and ground-based Hα imaging). The removal is accomplished via IRAF/IMEDIT by replacing the values of contaminated pixels via a 2D surface fit to a nearby sky annulus of width 2 pixels, with noise added that matches the noise statistics of the sky annulus. These annuli only sample the local sky around each spatial interloper and thus do not capture the full sky variations across the image. Fortunately, the spatial interlopers

are much smaller than our target galaxies, a fact that limits the effect of any shortcomings in the contaminant-removal procedure.

The total sky area, derived from the sum of the areas from all sky apertures, is typically significantly greater than the area covered by the galaxy aperture itself, thereby limiting the contribution of uncertainty in the sky level to the overall error budget. The mean sky level per pixel is computed from the collection of these sky apertures, the value is scaled to the number of pixels in the galaxy aperture, and the result is subtracted from the overall galaxy aperture counts.

### 3.6. Aperture Photometry

The elliptical apertures used for global photometry are listed in Table 1, and the same aperture is used to extract the flux at each wavelength. The apertures were chosen to encompass essentially all of the detectable emission at every wavelength (see also Dale et al. 2005, 2007, 2012). The average ratio of aperture major axis length 2a to the de Vaucouleurs $D_{25}$ optical major axis is 1.45 (with a $1\sigma$ dispersion in this ratio of 0.45).

At the longest wavelengths where the imaging resolution is typically coarsest, a small portion of the galaxy emission may appear beyond the chosen apertures. Thus, for the Spitzer and Herschel photometry we use the aperture corrections described in Dale et al. (2007, 2012). No aperture corrections were applied to the WISE photometry as they are negligible for the large apertures used here on native resolution imaging.

The uncertainties in the integrated photometry $\epsilon_{total}$ are computed as a combination in quadrature of the calibration uncertainty $\epsilon_{cal}$ and the measurement uncertainty $\epsilon_{sky}$ based on the measured sky fluctuations and the areas covered by the galaxy and the sum of the sky apertures, i.e.,

$$ \epsilon_{\text{total}} = \sqrt{\epsilon_{\text{cal}}^2 + \epsilon_{\text{sky}}^2} \qquad (3) $$

with

$$ \epsilon_{\text{sky}} = \sigma_{\text{sky}} \Omega_{\text{pix}} \sqrt{N_{\text{pix}} + N_{\text{pix}}^2 / N_{\text{sky}}} \qquad (4) $$

where $\sigma_{sky}$ is the standard deviation of the sky surface brightness fluctuations, $\Omega_{pix}$ is the solid angle subtended per pixel, and $N_{pix}$ and $N_{sky}$ are the number of pixels in the galaxy and (the sum of) the sky apertures, respectively. For the few sources undetected by Spitzer, Herschel, or WISE imaging, $5\sigma$ upper limits are derived assuming a galaxy spans all $N_{pix}$ pixels in the aperture,

$$ f_{\nu} (5\sigma \text{ upper limit}) = 5 \epsilon_{\text{sky}} \qquad (5) $$

Based on our visual scrutiny of the imaging data sets from a given telescope, any images redward of a non-detection are also considered to yield non-detections.

The galaxy apertures, the sky apertures, and the foreground stellar masks are provided with the electronic version of the journal article.

<footnote n="25">²⁵ Explanatory Supplement to the WISE All-Sky Data Release Products; 2015 February 19.</footnote>
<table><caption>**Table 4**

WISE and VLA 20 cm Total Flux Densities in Janskys Corrected for neither Galactic nor Intrinsic Extinction</caption><thead><tr><th></th><th>WISE</th><th>WISE</th><th>WISE</th><th>WISE</th><th>NRAO</th></tr></thead><tbody><tr><td>Filter</td><td>W1</td><td>W2</td><td>W3</td><td>W4</td><td>VLA</td></tr><tr><td>λ&#773;(μm)</td><td>3.40</td><td>4.65</td><td>12.8</td><td>22.4</td><td>20 cm</td></tr><tr><td>Δλ(μm)</td><td>0.663</td><td>1.04</td><td>5.51</td><td>4.11</td><td></td></tr><tr><td>A<sub>λ</sub>/A<sub>V</sub></td><td>0.0523</td><td>0.0287</td><td>0.0285</td><td>0.0225</td><td>0.0</td></tr><tr><td>NGC0024</td><td>108 ± 007E-1</td><td>544 ± 038E-2</td><td>895 ± 068E-2</td><td>109 ± 009E-1</td><td>...</td></tr><tr><td>NGC0337</td><td>981 ± 069E-2</td><td>693 ± 050E-2</td><td>310 ± 022E-1</td><td>733 ± 053E-1</td><td>109 ± 010E-1</td></tr><tr><td>NGC0584</td><td>420 ± 029E-1</td><td>208 ± 014E-1</td><td>661 ± 055E-2</td><td>335 ± 040E-2</td><td>&lt;500E-2</td></tr><tr><td>NGC0628</td><td>842 ± 059E-1</td><td>513 ± 036E-1</td><td>233 ± 016E+0</td><td>329 ± 023E+0</td><td>172 ± 017E-1</td></tr><tr><td>NGC0855</td><td>442 ± 031E-2</td><td>243 ± 018E-2</td><td>391 ± 034E-2</td><td>710 ± 056E-2</td><td>490 ± 050E-3</td></tr><tr><td>NGC0925</td><td>304 ± 021E-1</td><td>177 ± 013E-1</td><td>535 ± 040E-1</td><td>864 ± 076E-1</td><td>460 ± 050E-2</td></tr><tr><td>NGC1097</td><td>126 ± 008E+0</td><td>765 ± 054E-1</td><td>293 ± 020E+0</td><td>685 ± 048E+0</td><td>414 ± 041E-1</td></tr><tr><td>NGC1266</td><td>559 ± 039E-2</td><td>399 ± 028E-2</td><td>932 ± 067E-2</td><td>740 ± 053E-1</td><td>116 ± 012E-1</td></tr><tr><td>NGC1291</td><td>226 ± 016E+0</td><td>119 ± 008E+0</td><td>563 ± 050E-1</td><td>594 ± 069E-1</td><td>...</td></tr><tr><td>NGC1316</td><td>293 ± 020E+0</td><td>151 ± 010E+0</td><td>527 ± 039E-1</td><td>419 ± 034E-1</td><td>255 ± 026E-1</td></tr><tr><td>NGC1377</td><td>503 ± 035E-2</td><td>948 ± 067E-2</td><td>390 ± 027E-1</td><td>163 ± 011E+0</td><td>&lt;100E-3</td></tr><tr><td>NGC1404</td><td>721 ± 051E-1</td><td>370 ± 026E-1</td><td>166 ± 017E-1</td><td>740 ± 073E-2</td><td>390 ± 060E-3</td></tr><tr><td>IC0342</td><td>828 ± 058E+0</td><td>486 ± 034E+0</td><td>237 ± 018E+1</td><td>418 ± 029E+1</td><td>240 ± 024E+0</td></tr><tr><td>NGC1482</td><td>205 ± 014E-1</td><td>150 ± 010E-1</td><td>119 ± 008E+0</td><td>353 ± 025E+0</td><td>238 ± 024E-1</td></tr><tr><td>NGC1512</td><td>400 ± 028E-1</td><td>208 ± 014E-1</td><td>386 ± 028E-1</td><td>468 ± 035E-1</td><td>700 ± 100E-3</td></tr><tr><td>NGC1566</td><td>740 ± 052E-1</td><td>446 ± 031E-1</td><td>188 ± 013E+0</td><td>292 ± 020E+0</td><td>400 ± 000E-1</td></tr><tr><td>NGC1705</td><td>301 ± 021E-2</td><td>162 ± 011E-2</td><td>193 ± 015E-2</td><td>562 ± 052E-2</td><td>...</td></tr><tr><td>NGC2146</td><td>873 ± 061E-1</td><td>659 ± 046E-1</td><td>546 ± 038E+0</td><td>160 ± 011E+1</td><td>107 ± 010E+0</td></tr><tr><td>NGC2403</td><td>169 ± 011E+0</td><td>101 ± 007E+0</td><td>365 ± 026E+0</td><td>614 ± 045E+0</td><td>330 ± 033E-1</td></tr><tr><td>HoII</td><td>...</td><td>...</td><td>...</td><td>...</td><td>197 ± 028E-2</td></tr><tr><td>M81dwA</td><td>080 ± 010E-4</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>DDO053</td><td>460 ± 045E-3</td><td>297 ± 037E-3</td><td>...</td><td>338 ± 047E-2</td><td>...</td></tr><tr><td>NGC2798</td><td>107 ± 007E-1</td><td>762 ± 054E-2</td><td>564 ± 040E-1</td><td>238 ± 016E+0</td><td>829 ± 085E-2</td></tr><tr><td>NGC2841</td><td>139 ± 009E+0</td><td>759 ± 054E-1</td><td>895 ± 063E-1</td><td>112 ± 008E+0</td><td>840 ± 086E-2</td></tr><tr><td>NGC2915</td><td>537 ± 038E-2</td><td>296 ± 021E-2</td><td>218 ± 017E-2</td><td>513 ± 040E-2</td><td>...</td></tr><tr><td>HoI</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC2976</td><td>433 ± 030E-1</td><td>255 ± 018E-1</td><td>854 ± 061E-1</td><td>140 ± 010E+0</td><td>508 ± 054E-2</td></tr><tr><td>NGC3049</td><td>399 ± 028E-2</td><td>223 ± 016E-2</td><td>107 ± 007E-1</td><td>385 ± 028E-1</td><td>120 ± 023E-2</td></tr><tr><td>NGC3031</td><td>112 ± 007E+1</td><td>618 ± 043E+0</td><td>527 ± 037E+0</td><td>490 ± 035E+0</td><td>379 ± 037E-1</td></tr><tr><td>NGC3034</td><td>733 ± 051E+0</td><td>614 ± 043E+0</td><td>713 ± 050E+1</td><td>356 ± 025E+2</td><td>765 ± 077E+0</td></tr><tr><td>HoIX</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC3077</td><td>615 ± 043E-1</td><td>356 ± 025E-1</td><td>732 ± 053E-1</td><td>182 ± 013E+0</td><td>...</td></tr><tr><td>M81dwB</td><td>559 ± 043E-3</td><td>327 ± 029E-3</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC3190</td><td>377 ± 026E-1</td><td>214 ± 015E-1</td><td>267 ± 019E-1</td><td>259 ± 019E-1</td><td>430 ± 047E-2</td></tr><tr><td>NGC3184</td><td>504 ± 035E-1</td><td>290 ± 020E-1</td><td>114 ± 008E+0</td><td>146 ± 010E+0</td><td>559 ± 059E-2</td></tr><tr><td>NGC3198</td><td>288 ± 020E-1</td><td>171 ± 012E-1</td><td>596 ± 043E-1</td><td>105 ± 007E+0</td><td>270 ± 034E-2</td></tr><tr><td>IC2574</td><td>121 ± 009E-1</td><td>688 ± 059E-2</td><td>354 ± 037E-2</td><td>...</td><td>107 ± 023E-2</td></tr><tr><td>NGC3265</td><td>262 ± 018E-2</td><td>156 ± 011E-2</td><td>786 ± 056E-2</td><td>261 ± 018E-1</td><td>111 ± 023E-2</td></tr><tr><td>Mrk33</td><td>259 ± 018E-2</td><td>173 ± 012E-2</td><td>144 ± 010E-1</td><td>788 ± 056E-1</td><td>172 ± 026E-2</td></tr><tr><td>NGC3351</td><td>813 ± 057E-1</td><td>433 ± 030E-1</td><td>114 ± 008E+0</td><td>246 ± 017E+0</td><td>438 ± 048E-2</td></tr><tr><td>NGC3521</td><td>208 ± 014E+0</td><td>121 ± 008E+0</td><td>486 ± 034E+0</td><td>597 ± 042E+0</td><td>356 ± 035E-1</td></tr><tr><td>NGC3621</td><td>889 ± 064E-1</td><td>612 ± 045E-1</td><td>276 ± 019E+0</td><td>366 ± 026E+0</td><td>197 ± 019E-1</td></tr><tr><td>NGC3627</td><td>187 ± 013E+0</td><td>112 ± 008E+0</td><td>458 ± 032E+0</td><td>788 ± 056E+0</td><td>457 ± 045E-1</td></tr><tr><td>NGC3773</td><td>210 ± 015E-2</td><td>121 ± 008E-2</td><td>399 ± 030E-2</td><td>124 ± 009E-1</td><td>580 ± 050E-3</td></tr><tr><td>NGC3938</td><td>315 ± 022E-1</td><td>197 ± 014E-1</td><td>848 ± 060E-1</td><td>112 ± 008E+0</td><td>617 ± 065E-2</td></tr><tr><td>NGC4125</td><td>794 ± 056E-1</td><td>399 ± 028E-1</td><td>120 ± 010E-1</td><td>670 ± 062E-2</td><td>&lt;500E-2</td></tr><tr><td>NGC4236</td><td>229 ± 016E-1</td><td>124 ± 010E-1</td><td>134 ± 014E-1</td><td>...</td><td>281 ± 034E-2</td></tr><tr><td>NGC4254</td><td>683 ± 048E-1</td><td>445 ± 031E-1</td><td>332 ± 023E+0</td><td>448 ± 031E+0</td><td>421 ± 041E-1</td></tr><tr><td>NGC4321</td><td>100 ± 007E+0</td><td>625 ± 045E-1</td><td>258 ± 018E+0</td><td>378 ± 027E+0</td><td>340 ± 034E-1</td></tr><tr><td>NGC4450</td><td>552 ± 039E-1</td><td>297 ± 021E-1</td><td>221 ± 016E-1</td><td>223 ± 020E-1</td><td>940 ± 100E-3</td></tr><tr><td>NGC4536</td><td>422 ± 029E-1</td><td>267 ± 019E-1</td><td>132 ± 009E+0</td><td>349 ± 025E+0</td><td>194 ± 018E-1</td></tr><tr><td>NGC4552</td><td>918 ± 065E-1</td><td>447 ± 036E-1</td><td>256 ± 034E-1</td><td>999 ± 138E-2</td><td>100 ± 003E-1</td></tr><tr><td>NGC4559</td><td>352 ± 024E-1</td><td>230 ± 016E-1</td><td>677 ± 048E-1</td><td>114 ± 008E+0</td><td>654 ± 068E-2</td></tr><tr><td>NGC4569</td><td>793 ± 056E-1</td><td>448 ± 031E-1</td><td>894 ± 063E-1</td><td>139 ± 009E+0</td><td>834 ± 086E-2</td></tr><tr><td>NGC4579</td><td>929 ± 065E-1</td><td>498 ± 035E-1</td><td>610 ± 043E-1</td><td>687 ± 049E-1</td><td>984 ± 100E-2</td></tr><tr><td>NGC4594</td><td>444 ± 031E+0</td><td>236 ± 016E+0</td><td>113 ± 008E+0</td><td>893 ± 070E-1</td><td>136 ± 014E-1</td></tr><tr><td>NGC4625</td><td>477 ± 033E-2</td><td>275 ± 019E-2</td><td>100 ± 007E-1</td><td>127 ± 011E-1</td><td>710 ± 210E-3</td></tr><tr><td>NGC4631</td><td>124 ± 008E+0</td><td>804 ± 056E-1</td><td>469 ± 033E+0</td><td>839 ± 059E+0</td><td>120 ± 012E+0</td></tr><tr><td>NGC4725</td><td>116 ± 008E+0</td><td>598 ± 042E-1</td><td>740 ± 053E-1</td><td>721 ± 053E-1</td><td>280 ± 034E-2</td></tr><tr><td>NGC4736</td><td>389 ± 027E+0</td><td>221 ± 015E+0</td><td>447 ± 031E+0</td><td>586 ± 042E+0</td><td>270 ± 027E-1</td></tr><tr><td>DDO154</td><td>443 ± 038E-3</td><td>...</td><td>...</td><td>...</td><td>...</td></tr></tbody></table>
<table><caption>**Table 4**
(Continued)</caption><thead><tr><th></th><th>WISE</th><th>WISE</th><th>WISE</th><th>WISE</th><th>NRAO</th></tr></thead><tbody><tr><td>Filter</td><td>W1</td><td>W2</td><td>W3</td><td>W4</td><td>VLA</td></tr><tr><td>λ(μm)</td><td>3.40</td><td>4.65</td><td>12.8</td><td>22.4</td><td>20 cm</td></tr><tr><td>Δλ(μm)</td><td>0.663</td><td>1.04</td><td>5.51</td><td>4.11</td><td></td></tr><tr><td>A<sub>λ</sub>/A<sub>V</sub></td><td>0.0523</td><td>0.0287</td><td>0.0285</td><td>0.0225</td><td>0.0</td></tr><tr><td>NGC4826</td><td>265 ± 018E+0</td><td>145 ± 010E+0</td><td>197 ± 014E+0</td><td>265 ± 019E+0</td><td>101 ± 009E-1</td></tr><tr><td>DDO165</td><td>124 ± 009E-2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC5033</td><td>642 ± 045E-1</td><td>389 ± 027E-1</td><td>169 ± 012E+0</td><td>210 ± 015E+0</td><td>178 ± 017E-1</td></tr><tr><td>NGC5055</td><td>247 ± 017E+0</td><td>140 ± 009E+0</td><td>516 ± 036E+0</td><td>628 ± 044E+0</td><td>389 ± 039E-1</td></tr><tr><td>NGC5194</td><td>288 ± 020E+0</td><td>177 ± 012E+0</td><td>977 ± 069E+0</td><td>...</td><td>149 ± 015E+0</td></tr><tr><td>NGC5195</td><td>814 ± 057E-1</td><td>456 ± 032E-1</td><td>582 ± 041E-1</td><td>122 ± 008E+0</td><td>495 ± 053E-2</td></tr><tr><td>NGC5398</td><td>394 ± 028E-2</td><td>211 ± 015E-2</td><td>823 ± 060E-2</td><td>263 ± 019E-1</td><td>420 ± 080E-3</td></tr><tr><td>NGC5457</td><td>254 ± 018E+0</td><td>155 ± 011E+0</td><td>655 ± 046E+0</td><td>102 ± 007E+1</td><td>749 ± 075E-1</td></tr><tr><td>NGC5408</td><td>333 ± 024E-2</td><td>194 ± 014E-2</td><td>...</td><td>433 ± 031E-1</td><td>...</td></tr><tr><td>NGC5474</td><td>113 ± 008E-1</td><td>638 ± 046E-2</td><td>979 ± 084E-2</td><td>134 ± 014E-1</td><td>120 ± 023E-2</td></tr><tr><td>NGC5713</td><td>205 ± 014E-1</td><td>136 ± 009E-1</td><td>100 ± 007E+0</td><td>235 ± 016E+0</td><td>159 ± 016E-1</td></tr><tr><td>NGC5866</td><td>704 ± 049E-1</td><td>384 ± 027E-1</td><td>240 ± 017E-1</td><td>222 ± 017E-1</td><td>227 ± 030E-2</td></tr><tr><td>IC4710</td><td>602 ± 043E-2</td><td>349 ± 027E-2</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC6822</td><td>160 ± 011E+0</td><td>873 ± 065E-1</td><td>139 ± 015E+0</td><td>286 ± 034E+0</td><td>694 ± 140E-2</td></tr><tr><td>NGC6946</td><td>310 ± 022E+0</td><td>202 ± 014E+0</td><td>122 ± 008E+1</td><td>205 ± 014E+1</td><td>139 ± 014E+0</td></tr><tr><td>NGC7331</td><td>163 ± 011E+0</td><td>984 ± 069E-1</td><td>335 ± 023E+0</td><td>429 ± 030E+0</td><td>372 ± 037E-1</td></tr><tr><td>NGC7552</td><td>440 ± 031E-1</td><td>347 ± 024E-1</td><td>270 ± 019E+0</td><td>114 ± 008E+1</td><td>275 ± 028E-1</td></tr><tr><td>NGC7793</td><td>775 ± 054E-1</td><td>468 ± 033E-1</td><td>150 ± 010E+0</td><td>188 ± 013E+0</td><td>102 ± 009E-1</td></tr></tbody></table>

Note. The compact table entry format TUV ± WXYEZ implies (T.UV ± W.XY) × 10<sup>7</sup> in Jy. Corrections for neither Galactic nor intrinsic extinction has been applied. The uncertainties include both statistical and systematic effects. No color corrections have been applied. The filter central wavelengths and widths are computed via Equations (1) and (2).

# 4. Results

## 4.1. Flux Densities

Table 2 presents the spatially integrated flux densities for all 79 SINGS+KINGFISH galaxies for 30 photometric bands. In Table 5 we also supply global aperture photometry for the few cases where upper limits are provided in Table 2. The tabulated flux densities include aperture corrections (Section 3.6) and are *not* corrected for Galactic extinction. No color corrections have been applied to the data in Table 2. Some of the fluxes presented here remain unchanged from the values published elsewhere, for example, 2MASS JHK<sub>s</sub> Spitzer IRAC and MIPS, SCUBA 850 µm, and VLA 20 cm photometry. However, if any differences exist between values published in multiple publications, precedence is given to the more recent published values, e.g., 2MASS and Spitzer photometry from the Local Volume Legacy publication of Dale et al. (2009) is given priority over the 2MASS and Spitzer photometry appearing in Dale et al. (2007).

Figure 2 provides a comparison of our updated optical fluxes with those presented in previous publications. The updated $VR_C I_C$ optical fluxes are generally in agreement, on average, with previously published values, and the $1\sigma$ scatters in the differences for these filters are ~0.2–0.3 mag. The differences with published B filter fluxes, however, show a locus of points indicating that the literature data are typically 0.2 mag fainter than what we obtain after calibrating via Pan-STARRS1. There is also a second grouping of B data points, comprising nearly one-third of the total sample, that indicates the Dale et al. (2007) data are ~0.4 mag *brighter*; these may be cases where the B standard star calibration images for Dale et al. (2007) were either saturated or obtained in non-photometric conditions, both of

which would lead to artificially fainter standard star counts/s and thus artificially bright galaxy fluxes.

Figure 3 provides a similar comparison for the Herschel far-infrared/submillimeter photometry. The updated SPIRE beam sizes are larger than those used in Dale et al. (2012) by [11, 11, 14]% at [250, 350, 500] µm, which naturally leads to fainter SPIRE fluxes. This decrease is evident in Figure 3, where the average SPIRE flux is ~[8, 5, 16]% fainter at [250, 350, 500] µm than what appeared in Dale et al. (2012). For the five galaxies where we incorporated additional PACS data from other observing programs (Holmberg II, IC 2574, NGC 2798, NGC 4236, and NGC 4631; see Section 3), the resulting PACS maps are deeper and thus allow for some diffuse flux to be additionally detected. For faint Holmberg II it makes an appreciable difference: the 70 and 100 µm global fluxes are now 40%–50% larger.

## 4.2. The Spectral Energy Distributions

Figure 4 shows the observed infrared/submillimeter SEDs for the KINGFISH sample. Included in each panel, when available, are the GALEX far- and near-ultraviolet, $BVR_C I_C$ and ugriz optical, 2MASS JHK<sub>s</sub> near-infrared, Spitzer 3.6, 4.5, 5.8, 8.0, 24, 70, and 160 µm, WISE 12 µm, Herschel 70, 100, 160, 250, 350, and 500 µm, and Planck and SCUBA 850 µm fluxes.

The broadband SEDs displayed in Figure 4 are fitted with the models of Draine & Li (2007) over the wavelength range 3.6–500 µm, models based on mixtures of amorphous silicate and graphitic dust grains that effectively reproduce the average Milky Way extinction curve and are consistent with observations of PAH features and the variety of infrared continua in local galaxies. A total of four free parameters are used in the fits: the fraction $q_{PAH}$ of the dust mass residing in polycyclic
<table><caption>**Table 5**
Aperture Photometry for Cases of Upper Limits in Table 2</caption><thead><tr><th>Filter</th><th>Spitzer</th><th>Spitzer</th><th>WISE</th><th>Spitzer</th><th>Spitzer</th><th>Herschel</th><th>Herschel</th><th>Spitzer</th><th>Herschel</th><th>Herschel</th><th>Herschel</th><th>Herschel</th></tr><tr><th>λ(μm)</th><th>IRAC</th><th>IRAC</th><th>W3</th><th>MIPS</th><th>MIPS</th><th>PACS</th><th>PACS</th><th>MIPS</th><th>PACS</th><th>SPIRE</th><th>SPIRE</th><th>SPIRE</th></tr></thead><tbody><tr><td>NGC0584</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>281 ± 158E-1</td><td>110 ± 106E-1</td><td>099 ± 684E-2</td></tr><tr><td>NGC1404</td><td>...</td><td>...</td><td>...</td><td>...</td><td>110 ± 080E-1</td><td>330 ± 062E-1</td><td>-111 ± 009E+0</td><td>130 ± 120E-1</td><td>630 ± 066E-1</td><td>-149 ± 030E-1</td><td>-139 ± 025E-1</td><td>295 ± 166E-2</td></tr><tr><td>M81dwA</td><td>-010 ± 520E-3</td><td>034 ± 640E-3</td><td>-420 ± 090E-4</td><td>050 ± 330E-3</td><td>029 ± 146E-1</td><td>330 ± 090E-2</td><td>...</td><td>020 ± 473E-1</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>DDO053</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>980 ± 578E-3</td></tr><tr><td>HoIX</td><td>-400 ± 200E-4</td><td>771 ± 100E-3</td><td>526 ± 050E-3</td><td>128 ± 040E-3</td><td>068 ± 120E-2</td><td>...</td><td>...</td><td>-251 ± 260E-2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>DDO154</td><td>560 ± 080E-3</td><td>180 ± 200E-4</td><td>422 ± 035E-3</td><td>145 ± 050E-3</td><td>338 ± 140E-2</td><td>-270 ± 019E-1</td><td>500 ± 029E-1</td><td>-009 ± 280E-2</td><td>600 ± 136E-2</td><td>109 ± 011E-1</td><td>693 ± 093E-2</td><td>294 ± 061E-2</td></tr><tr><td>DDO165</td><td>...</td><td>...</td><td>800 ± 280E-4</td><td>449 ± 060E-3</td><td>141 ± 020E-1</td><td>-240 ± 021E-1</td><td>150 ± 022E-1</td><td>206 ± 043E-1</td><td>400 ± 178E-2</td><td>101 ± 133E-2</td><td>100 ± 124E-2</td><td>501 ± 092E-2</td></tr></tbody></table>

Note. The compact table entry format TUV ± WXYEZ implies (T.UV ± W.XY) × 10² in Jy. Corrections for neither Galactic nor intrinsic extinction has been applied (see Section 3). The uncertainties include both statistical and systematic effects. No color corrections have been applied.
<figure><img src="image_5.png" /><figcaption>**Figure 2.** Comparison of global *BVRc*<sub>IC</sub> galaxy photometry from the literature with those measured here that are calibrated based on Pan-STARRS1 *g*<sub>P1</sub>*r*<sub>P1</sub>*i*<sub>P1</sub>*z*<sub>P1</sub> photometry on field stars (see Section 3.1).</figcaption></figure>

aromatic hydrocarbons (PAHs), the intensity $U_{\min}$ of the interstellar radiation field that heats the general diffuse interstellar medium, and the fraction $\gamma$ of the dust mass heated by more intense starlight distributions such as those arising from photodissociation regions (PDRs) in star-forming regions, the ratio of the stellar mass to the dust mass ($M_{\text{dust}}$ is determined by the normalization of the SED model with the observed photometric data). The parameter $q_{\text{PAH}}$ ranges between 0% and 12%, and $U_{\min}$ can have values between 0.01 and 30. As was done for Draine et al. (2007) and Dale et al. (2012), we minimize the number of free parameters by fixing the maximum value of the interstellar radiation field ($U_{\max} = 10^6$) as well as the power-law exponent that governs the distribution of starlight intensities heating the dust ($\alpha = 2$). More details of these models may be found in Draine & Li (2007) and Draine et al. (2007).

The new SED fits here can be compared to what was obtained previously for the KINGFISH sample in Dale et al. (2012) with the outdated SPIRE photometric calibration. Figure 5 provides such a comparison for dust mass, PAH fraction, and the properties of the radiation field that is heating the dust. The two systematic differences, in the inferred dust mass and the diffuse radiation field intensity $U_{\min}$, are the result of the changes in the PACS and SPIRE calibrations—brighter at 70 and 100 µm and fainter at 250, 350, and 500 µm result in warmer interstellar dust and smaller overall dust masses. We

note that while recent results indicate a necessary change in the DL07 dust opacities (Dalcanton et al. 2015; Planck Collaboration et al. 2016b), we are consistently using the same (original) dust models from Draine & Li (2007) in the Figure 5 comparisons. The two outliers in $q_{\text{PAH}}$ are the result of the inclusion of new PACS photometry for NGC 0584 and an improved sky estimate for NGC 1291's PACS 70 µm map, which led to a factor of ~2 smaller flux that is now in much better agreement with the *Spitzer* 70 µm flux.

As was mentioned in Dale et al. (2012), the faintest targets pose the most challenges to SED fitting. Spatial variations in the foreground cirrus amplify the relative uncertainty in the extracted fluxes for these targets. Even with our updated data processing and analysis, this situation remains essentially unchanged for galaxies like NGC 0584, DDO 053, M81 dwarf B, and Holmberg I. However, the addition of *WISE* fluxes to the SED fitting incrementally improves our confidence in the SED fits. A more detailed analysis of theoretical fits to these SEDs is presented in the companion paper (L.K. Hunt et al. 2017, in preparation) and in B.T. Draine et al. (2017, in preparation).

### 4.3. Submillimeter Excess

Dale et al. (2012) found an excess of submillimeter emission for several galaxies in the KINGFISH sample, where the observed 500 µm emission was measured to lie significantly
<figure><img src="image_6.png" /><figcaption>**Figure 3.** Comparison of updated global Herschel photometry with those presented in Dale et al. (2012). The error bars are relatively constant since they are primarily dominated by systematics for the brighter sources.</figcaption></figure>

above the model predictions based on Draine & Li (2007) fits to the observed 3.6–500 µm SEDs. The submillimeter excess ξ (500 µm) was quantitatively defined in Dale et al. (2012) as

$$ \xi(500 \mu\text{m}) = \frac{f_{\nu}(500 \mu\text{m})_{\text{observed}} - f_{\nu}(500 \mu\text{m})_{\text{model}}}{f_{\nu}(500 \mu\text{m})_{\text{model}}}. \quad (6) $$

This excess was primarily found in low-metallicity galaxies: 9 of the 10 dwarf/irregular/Magellanic galaxies in the KINGFISH sample with 500 µm detections exhibited ξ(500 µm) > 0.60. This result echoed similar claims of submillimeter excess in studies of M33, the Magellanic Clouds, and other low-metallicity star-forming galaxies (Galliano et al. 2005; Galametz et al. 2011; Planck Collaboration et al. 2011; Gordon et al. 2014; Izotov et al. 2014; Hermelo et al. 2016). With the updated calibrations for our present data set, including SPIRE calibration changes that result in 500 µm fluxes lower by an average of 16% (Figure 3), we still see submillimeter excesses in the sample, but at lower significance. The average excess for dwarf/ irregular/Magellanic galaxies in Dale et al. (2012) was 〈ξ(500 µm)〉$_{T=\text{Im,10,Sm}} \sim 0.70$, whereas in the current work the average value is 〈ξ(500 µm)〉$_{T=\text{Im,10,Sm}} \sim 0.53$ for the 11 SINGS/KINGFISH dwarf/irregular/Magellanic galaxies with secure 500 µm detections. Note that an alternative signal-to-noise-ratio-like definition of the submillimeter excess may be defined by normalizing via the model and observational

uncertainties, namely

$$ S/N(500 \mu\text{m excess}) = \frac{f_{\nu}(500 \mu\text{m})_{\text{observed}} - f_{\nu}(500 \mu\text{m})_{\text{model}}}{\sqrt{\epsilon_{\text{obs}}^2 + \epsilon_{\text{mod}}^2}}. \quad (7) $$

In this case, the average value is 〈S/N(500 µm excess)〉 ∼ 4.3 for ε<sub>mod</sub> = 0 and ∼3.3 for ε<sub>mod</sub> = 0.1 f<sub>ν</sub> (500 µm)<sub>model</sub> for the 11 SINGS/KINGFISH dwarf galaxies. We caution that our results may be biased since we restrict our analysis to securely detected sources.

Although the left-hand panel of Figure 6 shows no dependence for submillimeter excess on far-infrared color, there is a clear trend in the right-hand panel, with higher submillimeter excesses for lower gas-phase metallicity. This persistency of a submillimeter excess in primarily low-metallicity galaxies contradicts the analysis of Kirkpatrick et al. (2013), who found no significant submillimeter excesses for a subset of 20 galaxies from the KINGFISH sample with robust (and updated) far-infrared photometry that span a range in metallicity. However, there are three main differences between the analysis carried out here and by Kirkpatrick et al. (2013). First, Kirkpatrick et al. (2013) only fit data spanning 24–350 µm. Our SED fitting employs the full infrared continuum over 3.6–500 µm, and therefore our approach must balance contributions from stellar and PAH emission in addition to that from larger dust grains. Second, Kirkpatrick et al. (2013) employ the superposition of two modified blackbodies,
<figure><img src="image_7.png" /><figcaption>**Figure 4.** Globally integrated infrared/submillimeter spectral energy distributions for all the galaxies in the KINGFISH/SINGS sample, sorted by R.A. The following symbols are used: filled circles (Herschel), triangles (GALEX, 2MASS, and WISE), open circles (Spitzer and Planck), and squares (BVR<sub>C</sub>I<sub>C</sub> and ugriz and SCUBA). Arrows indicate 5σ upper limits (and lower limits in the case of NGC 3034). The solid curve is the sum of a 5000 K stellar blackbody (short dashed) along with models of dust emission from PDRs (dotted; *U* > *U*<sub>min</sub>) and the diffuse interstellar medium (long dashed; *U* = *U*<sub>min</sub>). The fitted parameters from these Draine & Li (2007) 3.6–500 µm model fits are listed within each panel along with the reduced χ<sup>2</sup> (see Section 4.2 for details). While the plotted data are corrected for Galactic extinction, the fluxes tabulated in Table 2 are not corrected. The uncertainties are smaller than the symbols plotted. There are no SED fits in cases where the far-infrared photometry provides only limits.

*(An extended version of this figure is available.)*</figcaption></figure>

whereas our fits use a more sophisticated dust model (Draine & Li 2007); we have four free parameters in our SED fitting, whereas Kirkpatrick et al. (2013) have only three free parameters: the temperature and emissivity of the cold dust component, and the ratio of the amplitudes of the two modified blackbodies. Third, while we normalize our submillimeter excesses by the predicted model value at 500 µm, Kirkpatrick et al. (2013) normalize via the observed 500 µm value. Normalizing by the observed flux is an approach that naturally depresses the excess measure. For example, the average submillimeter excess for the 11 SINGS/KINGFISH dwarf/irregular/Magellanic galaxies with 500 µm detections is 0.33 if the normalization is via the observed flux, a factor of 1.6 times smaller than when normalizing by the predicted model flux.

**5. Summary**

We present an update to the full panchromatic photometric database for the 79 galaxies in the combined SINGS/KINGFISH sample of nearby galaxies, for ultraviolet through radio wavelengths. Updates include incorporating recent improvements in the calibration of the *Herschel* photometers and a recalibration of BVR<sub>C</sub>I<sub>C</sub> photometry using broadband data from the Pan-STARRS1 survey. On average, the updated *Herschel* fluxes differ

by [+5, +8, 0, -8, -5, -16]% at [70, 100, 160, 250, 350, 500] µm compared to what was published in the original KINGFISH photometry paper of Dale et al. (2012). The average updated fluxes for the VR<sub>C</sub>I<sub>C</sub> filters are essentially unchanged from the SINGS photometry presented in Dale et al. (2007), but with a scatter of 0.2–0.3 mag. The updated collection of B fluxes are about ~0.2 mag brighter than what appears in the literature. Finally, theoretical Draine & Li (2007) SED models are fit to each galaxy’s 3.6–500 µm data set. Two of the fitted parameters show small but systematic differences with the results published previously: the total dust masses are about 20% lower, and the typical value of the radiation field that is heating the diffuse ISM is about 10% higher. Both of these results naturally arise from the changes in the calibrations of the *Herschel* imagers since 2012. We confirm our previous finding of an excess of submillimeter emission (500 µm) in primarily low-metallicity dwarf/irregular galaxies, but at a smaller amplitude due to the updated calibration of the *Herschel* SPIRE beams. A full exploration of this panchromatic data set is carried out in a companion paper by L. K. Hunt et al. (2017, in preparation).

We thank the referee for excellent suggestions that improved this work. *Herschel* is an ESA space observatory with science
<figure><img src="image_8.png" /><figcaption>**Figure 5.** Comparison of DL07 output fit parameters from Dale et al. (2012) with those measured here. The dispersions in the ordinate (y-axis) values are inset.</figcaption></figure>

<figure><img src="image_9.png" /><figcaption>**Figure 6.** The submillimeter excess parameter $\xi(500~\mu\text{m})$ (see Equation (7)) as a function of far-infrared color and characteristic oxygen abundance as derived from Moustakas et al. (2010). Red circles indicate irregular galaxies ($T = \text{Sm, Im, or I0}$).</figcaption></figure>

instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This work is based on observations made with the *Spitzer Space Telescope* and utilizes the NASA/IPAC Infrared Science Archive, both operated by JPL/Caltech under a contract with NASA. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the *GALEX* mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. Funding for the Sloan Digital Sky Survey and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the NSF, the U.S. Department of Energy, NASA, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding

Council for England. This publication makes use of data products from the *Wide-field Infrared Survey Explorer*, which is a joint project of the University of California, Los Angeles, and the JPL/Caltech, funded by NASA. The Pan-STARRS1 Surveys have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extra-terrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of
<figure><img src="image_10.png" /><figcaption>**Figure 7.** Comparison of Spitzer- and aperture-based global photometry with total WISE photometry. The dotted lines for the top two panels indicate the expected flux density ratios after convolving a 5000 K blackbody with the respective filter bandpass profiles. The average ratio and its uncertainty ($\sigma/\sqrt{N}$) are inset.</figcaption></figure>

Taiwan, the Space Telescope Science Institute, the NSF, the University of Maryland, and Eotvos Lorand University and the Los Alamos National Laboratory.

## Appendix
WISE Fluxes

Table 2 presents WISE W3 (12 µm) flux densities based on the same apertures used for the other flux densities presented in Table 2. We additionally present here “total” flux densities for all four WISE bands using zero-points of [309.666, 170.623, 29.043, 7.875] Jy for [W1, W2, W3, W4] at central wavelengths of [3.4, 4.6, 12, 22] µm.<fnref n="26" /> The process for extracting “total” flux densities follows that described in Jarrett et al. (2013), whereby azimuthally averaged elliptical surface brightness profiles are extrapolated to three disk scale lengths beyond the 1σ (sky rms) isophotal radii. For WISE, the 1σ isophotes are at surface brightness levels of approximately [23.0, 21.8, 18.1, 15.8] mag arcsec⁻² (Vega) for [W1, W2, W3, W4] (Jarrett et al. 2013). This particular WISE database

provides an excellent opportunity to check our Spitzer- and aperture-based global fluxes at 3.6, 4.5, and 24 µm. Figure 7 presents such a comparison. The agreement between Spitzer and WISE flux densities is close to expectations. The dotted lines in the top two panels indicate the expected flux density ratios after convolving the filter bandpasses with a 5000 K stellar blackbody; the observed ratios match the expected ratios to within the observed 1σ scatters. There is perhaps a weak trend for the ratio of Spitzer 24 µm and WISE W3, with the ratio decreasing with increasing brightness.

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<footnote n="26">²⁶ Brown et al. (2014) suggest W4 has an effective central wavelength of 22.8 µm.</footnote>