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% abbreviations used in this paper
\def\kms{~km~s$^{-1}$}
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\def\N_MIPSIRAC{71}

\begin {document}
%\slugcomment{\scriptsize \today \hskip 0.2in Version 3.4}

\title{The \Spitzer\ Local Volume Legacy: Infrared Imaging and Photometry for 258 Nearby Galaxies}
 
%\author {D.A.~Dale et al.}
\author {D.A.~Dale\altaffilmark{1}, S.A.~Cohen\altaffilmark{1}, L.C.~Johnson\altaffilmark{1}, M.D.~Schuster\altaffilmark{1}, M.~Block\altaffilmark{2}, C.W.~Engelbracht\altaffilmark{2}, A.~Begum\altaffilmark{3}, D.~Calzetti\altaffilmark{4}, J.J.~Dalconton\altaffilmark{5}, J.G.~Funes\altaffilmark{6}, A.~Gil~de~Paz\altaffilmark{7}, K.D.~Gordon\altaffilmark{8}, B.D.~Johnson\altaffilmark{9}, R.C.~Kennicutt\altaffilmark{3,2}, J.C.~Lee\altaffilmark{10}, S.~Sakai\altaffilmark{11}, E.D.~Skillman\altaffilmark{12}, L.~van~Zee\altaffilmark{13}, F.~Walter\altaffilmark{14}, D.R.~Weisz\altaffilmark{12}, B.~Williams\altaffilmark{5}, S.-Y.~Wu\altaffilmark{4}, Y.~Wu\altaffilmark{15}}
\altaffiltext{1}  {\scriptsize Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071; ddale@uwyo.edu}
\altaffiltext{2}  {\scriptsize Steward Observatory, University of Arizona, Tucson, AZ 85721}
\altaffiltext{3}  {\scriptsize Institute of Astronomy, University of Cambridge, Cambridge CB3 0HA, United Kingdom}
\altaffiltext{4}  {\scriptsize Astronomy Department, University of Massachusetts, Amherst, MA 01003}
\altaffiltext{5}  {\scriptsize Department of Astronomy, University of Washington, Seattle, WA 98195}
\altaffiltext{6}  {\scriptsize Vatican Observatory Research Group, Steward Observatory, University of Arizona, Tucson, AZ 85721}
\altaffiltext{7}  {\scriptsize Departamento de Astrofisica, Universidad Complutense, Madrid, E-28040, Spain}
\altaffiltext{8}  {\scriptsize Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218}
\altaffiltext{9}  {\scriptsize Department of Astronomy, Columbia University, New York, NY 10027}
\altaffiltext{10} {\scriptsize Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101}
\altaffiltext{11} {\scriptsize Division of Astronomy and Astrophysics, University of California, Los Angeles, CA 90095}
\altaffiltext{12} {\scriptsize Astronomy Department, University of Minnesota, Minneapolis, MN 55455}
\altaffiltext{13} {\scriptsize Department of Astronomy, Indiana University, Bloomington, IN 47405}
\altaffiltext{14} {\scriptsize Max Planck Institut f\"{u}r Astronomie, K\"{o}nigstuhl 17, 69117 Heidelberg, Germany}
\altaffiltext{15} {\scriptsize Astronomy Department, Cornell University, Ithaca, NY 14853}

\begin {abstract}
Near-, mid-, and far-infrared flux densities are presented for the Local Volume Legacy, a {\it Spitzer Space Telescope} legacy program built upon a foundation of ultraviolet, \hal, and infrared imaging for a volume-complete sample of 258 galaxies out to 11~Mpc.  
%Its broad goal is to provide critical insight into two of the primary processes that shape the growth of galaxies: star formation and its interaction with the interstellar medium.  This goal will be accomplished by investigating the spatially-resolved star-forming, dust, and red stellar populations of galaxies spanning the full local universe diversity of luminosities, surface brightnesses, metallicities, star formation, and dust properties.  
The Local Volume Legacy uniquely extends \GALEX\ and \Spitzer\ observations of galaxies to an unbiased, fully representative, and statistically robust sample of nearby galaxies, exploiting the faintest absolute depth and highest extragalactic spatial resolution achievable with the 
%{\it Galaxy Evolution Explorer} and 
{\it Spitzer Space Telescope}.  
%The tiered survey includes: {\it i}) all known galaxies inside a sub-volume bounded by 3.5~Mpc, and {\it ii}) an unbiased sample of spiral and irregular galaxies within the larger, and more representative, 11~Mpc sphere.  
%, to enhance the scientific return and provide an enduring core dataset on the Galactic neighborhood for the scientific community at large.
Compared to SINGS, another \Spitzer-based survey of the Local Universe, the sample of galaxies in the Local Volume Legacy contain a far higher fraction of dwarf and irregular galaxies, and no early-type galaxies.  There are several manifestations of these differences in local samples, including a much larger spread in mid-infrared colors for the Local Volume Legacy, likely due to the enhanced PAH-deficiency for low-metallicity galaxies.  Conversely, the Local Volume Legacy sample shows a tighter correlation in the infrared-to-ultraviolet ratio versus ultraviolet spectral slope, due in large part to the lack of early-type galaxies in the sample.
%The infrared data presented here leverage a rich suite of multi-wavelength ancillary data, including \hal\ imaging, optical broadband imaging and spectroscopy, stellar population mapping with the {\it Hubble Space Telescope}, and \HI\ mapping with the {\it Very Large Array} and the {\it Giant Metrewave Radio Telescope}.  Future studies based on the Local Volume Legacy sample will exploit further the multi-wavelength database...
\end {abstract}
 
\keywords{surveys --- galaxies: photometry --- infrared: galaxies}
 
\section {Introduction}

xx 2mass near-ir, 258 spitzer mid- and far-ir

Section~\ref{sec:sample} describes the sample, Section~\ref{sec:observations} reviews the observational and data processing programs, Section~\ref{sec:data} covers details of the integrated aperture photometry, Section~\ref{sec:results} presents initial results based on the photometry, and Section~\ref{sec:summary} summarizes our work.


\section{The Sample}
\label{sec:sample}
The sample of galaxies and its selection is described fully in the companion paper by Lee et al. (2008).  Briefly, the Local Volume Legacy sample includes {\it all} 69 known high Galactic latitude ($|b|>20$\degr) galaxies outside of the Local Group within 3.5~Mpc, with an extension to $\sim$4~Mpc in the direction of the M~81 group.  This inner tier of the Local Volume Legacy is the same set of galaxies found in the HST Treasury Survey ``ANGST'' (P.I. J. Dalcanton).  This volume out to 3.5~Mpc includes spiral, dIrr, dSph, and tidal dwarf galaxies, spanning a range of 6~magnitudes in luminosity, 10$^3$ in current star formation rate, and 1.5~dex in metallicity.  The outer tier of the Local Volume Legacy is drawn from 11HUGS, which began as an \hal+broadband optical imaging study of a volume-limited sample of 400 spiral and irregular galaxies within 11~Mpc (Kennicutt et al. 2008).  The survey was expanded to included \GALEX\ ultraviolet observations for 220 galaxies with $|b|>30$\degr\ and $B<15.5$~mag.  Statistical tests and comparisons with blind all-sky \HI\ surveys (Ryan-Weber et al. 2002; Lee 2006) show that the catalog completeness for spiral and irregular galaxies out to 11~Mpc is excellent ($>$95\%) within limits of $|b|\geq20$\degr\ and $B\leq15.5$~mag.  We have optimized our \Spitzer\ observations by restricting the sample to where we have high completeness and multi-wavelength coverage, and imposing limits of $B\leq15.5$~mag and $|b|\geq30$\degr.  Thirty-three of the Local Volume Legacy galaxies are also in the SINGS sample, another {\it Spitzer} Legacy program on nearby galaxies (Kennicutt et al. 2003).

The entire LVL sample includes 258 galaxies.  Approximately half (53\%) of the LVL galaxies have spiral morphology, 38\% are irregulars, 8\% are S0 galaxies, and there is a single elliptical.  For comparison, SINGS has larger fractions of non-spiral morphologies,
%is more evenly distributed by morphology, 
with 63\% spiral, 17\% irregular, 12\% S0, and 8\% elliptical morphologies.  Since the origination of this project, four LVL galaxies have new distances which place them outside of 11~Mpc: UGC~00521, UGC~06782, IC~2049, and UGC~7321.  Though the observations for these four systems are presented here, these galaxies will not be included in future, LVL sample-wide studies. % 11.32, 14.00, 16.73, 20.00 Mpc


\section {Observational Strategy and Data Processing}
\label{sec:observations}

%\subsection {Spitzer IRAC Near- and Mid-Infrared Data}
\subsection {New {\it Spitzer} IRAC 3.6, 4.5, 5.8, and 8.0\m\ Data}
\label{sec:irac_observations}

New {\it Spitzer} IRAC observations were obtained for 180 LVL galaxies.  The IRAC observing strategy follows that of SINGS, which shows that stellar and small grain dust emission is typically detected out to the optical radius at a surface brightness level of $\sim$0.04~MJy~sr$^{-1}$ (Regan et al. 2006; Dale et al 2000).  For galaxies smaller than the IRAC field of view ($D_{25}\leq300$\arcsec) the Astronomical Observing Requests (AORs) were constructed using four dithered 30~s integrations.  For larger galaxies a mosaicking strategy with $\sim$half-array spatial offsets was used, with the sizes of the mosaic `cores' tailored to the optical size of each galaxy.  Two sets of IRAC maps were obtained for each source to enable asteroid removal and to enhance map sensitivity and redundancy.  Combining all eight 30~s frames thus results in a net integration per pixel of 240~s (and 120~s around the $\sim$2\farcm5-wide mosaic peripheries).  Since each source was observed in all IRAC channels, ample sky coverage is automatically provided by the non-overlapping nature of the two IRAC imagers.

The BCD data used for post-pipeline processing are from the S18 pipeline version (update this sentence?).  The multi-epoch, multiple-pointing IRAC observations for each galaxy are combined into one single mosaic for each band using the MOPEX mosaicking software.  Additional post-BCD processing includes: distortion corrections, rotation of the individual frames (for multi-epoch observations), bias structure and bias drift corrections, image offset determinations via pointing refinements from the SSC pipeline (MOPEX's default), detector artifact removal, constant-level background subtraction, and image resampling to 0\farcs75 pixels using drizzling techniques.  The drizzling slightly improves the final PSF over the native one.  The final images are in units of MJy~sr$^{-1}$ and have the average sky level removed; sky values are estimated via several ``blank'' regions located near but beyond the target galaxy emission.

The high dynamic range option (additional 1.2~s exposures) was incorporated into the observing program to allow recovery of information where exceptionally bright sources saturated, or at least pushed into the non-linear regime of, the detector in 30~s.  Pixels affected by these issues are identified by NaN-valued pixels created by the MOPEX processing to replace saturated pixels flagged by the SSC BCD processing pipeline or the appearance of the IRAC bandwidth effect artifact (see Section~4.3.3 of the IRAC Data Handbook).  The nuclear regions for several galaxies were affected by these saturation/artifact issues: NGC~0253 (5.8 \& 8.0\m), NGC~2903 (8.0\m), NGC~3031 (5.8 \& 8.0\m), NGC~3034 (all IRAC wavelengths), NGC~3351 (5.8 \& 8.0\m), NGC~3593 (5.8 \& 8.0\m), NGC~3627 (8.0\m), NGC~4258 (5.8 \& 8.0\m), and NGC~5195 (8.0\m).
% NGC2903 is the only 'new' IRAC galaxy that is saturated

To remedy the effects of saturation/non-linearity/bandwidth for an affected IRAC image, a mosaic of the high dynamic range 1.2~s frames is first created.  The short integration mosaic is interpolated to the same pixel grid as the longer integration mosaic.  A difference image is then created from the long and short integration mosaics, and any residual, systematic difference in the sky value is removed.  Pixels in the difference image valued at $\sim$1~MJy~sr$^{-1}$ or higher are flagged (routinely regions of ~400 pixels); flagged pixels from the short integration mosaic replace their counterparts in the long integration mosaic.

%\subsection {Spitzer MIPS Mid- and Far-Infrared Data}
\subsection {New {\it Spitzer} MIPS 24, 70, and 160\m\ Data}
\label{sec:mips_observations}

New {\it Spitzer} MIPS observations were obtained for 201 LVL galaxies.  Galaxies were imaged in all three MIPS bands centered at 24, 70, and 160\m, using the highly successful scan mapping strategy employed in the SINGS project.  The scan mode was used even on galaxies small enough to fit within the array field of view, because achieving adequate background measurements for extended targets in photometry mode is less efficient than the scan mode.  Each map was executed at the medium scan rate, and includes multiple scan legs tailored to the size of the galaxy and half-array offsets between scan legs.  Each galaxy was mapped twice, with the maps separated by 10-40 days to allow time for asteroids to move out of the field.  This second map was performed in the reverse direction (the ``backward mapping'' mode), with offsets in the cross-scan and in-scan directions.  Taken together, these mapping strategies ensure that each point on the galaxy is scanned over in two different directions, which aids reduction of array artifacts on both Si:As and Ge:Ga arrays.  The in-scan offset ensures that Ge:Ga stimflashes do no occur at the same point in both maps and thereby improves the calibration.  The integration time per point 
%and 1$\sigma$ low-background surface brightness sensitivity 
is 160, 80, and 16~s
% and 0.059, 0.32, and 0.85~MJy~sr$^{-1}$ 
at 24, 70, and 160\m, respectively.

The pixel scale of the MIPS mosaics is wavelength-dependent: 1\farcs5, 4\farcs5, and 9\farcs0 at 24, 70, and 160\m, respectively.  The MIPS images are processed with the MIPS Data Analysis Tool (DAT; Gordon et al. 2005), supplemented by custom scripts for the specific data reduction and mosaicking of extended sources.  The latter include: at 24\m, readout offset correction, array-averaged background subtraction, and exclusion of the first five images in each scan leg due to boost frame transients.  At 70 and 160\m, the custom scripts include a pixel-dependent background subtraction for each map to remove residual detector drifts and background cirrus and zodiacal emission.  This method of reduction was used for all the SINGS galaxies as well as very large MIPS/GTO galaxies (M~31, M~33, M~101, etc.).  

Finally, a correction for 70\m\ non-linearity effects is included in the data processing.  A correction of the form
\be
f^{\rm 70{\scriptsize \micron}}_{\rm true} = 0.581 (f^{\rm 70{\scriptsize \micron}}_{\rm measured})^{1.13},
\ee
derived from data presented by Gordon et al. (2008, in preparation), is applied to pixel values above a threshold of $\sim$66~MJy~sr$^{-1}$.  A small fraction of the pixels in a total of 40 LVL 70\m\ images require such a correction.  The median correction to the global 70\m\ flux density for these 40 galaxies is typically a few percent.
%a factor of 1.03, with the three largest corrections being factors of 1.124 (NGC~4826), 1.128 (NGC~1482), and 1.158 (NGC~7552).
% see arapaho:/data/lvl/mips_images/70.lincor.txt and the same file within without_70um_corr/cropped/ and arapaho:/data/lvl/mips_images/70.lincor.2.txt

\subsection {Archival {\it Spitzer} IRAC 3.6, 4.5, 5.8, and 8.0\m\ Data}

Archival IRAC data, with spatial coverage and sensitivity equal to or greater than that described in \S~\ref{sec:irac_observations}, are utilized for 78 LVL galaxies.  No new IRAC observations were obtained for this subset of the LVL sample.  The data processing procedures for the archival IRAC data are the same as those followed for the new observations described in \S~\ref{sec:irac_observations}.

\subsection {Archival {\it Spitzer} MIPS 24, 70, and 160\m\ Data}

Archival MIPS data, with spatial coverage and sensitivity equal to or greater than that described in \S~\ref{sec:mips_observations}, are utilized for 57 LVL galaxies.  No new MIPS observations were obtained for this subset of the LVL sample.  The data processing procedures for the archival MIPS data are the same as those followed for the new observations described in \S~\ref{sec:mips_observations}.


\section {Aperture Photometry}
Table~\ref{tab:data} presents the global flux densities for the entire LVL sample, for wavelengths spanning the near- to far-infrared.  The data are corrected for Galactic extinction (Schlegel, Finkbeiner, \& Davis 1998) assuming $A_V/E(B-V)\approx3.1$ and the reddening curve of Li \& Draine (2001).  The effect of airmass has been removed from the ground-based near-infrared fluxes.  Below follows a description of the infrared data collected for the LVL program.
\label{sec:data}

\subsection {2MASS Near-Infrared JHK$_{\rm s}$}
The Two Micron All Sky Survey (2MASS) obtained data for the entire sky at 1.25, 1.65, and 2.17\m\ using two automated, ground-based 1.3~m telescopes (Skrutskie et al. 2006).  Integrated flux densities for several LVL galaxies were adopted from the 2MASS Large Galaxy Atlas (Jarrett et al. 2003); near-infrared fluxes from the Large Galaxy Atlas are consistent with expectations based on IRAC 3.6 and 4.5\m\ fluxes and simple stellar model extrapolations to 2MASS wavelengths.  However, many of the fluxes from the 2MASS All-Sky Extended Source Catalog are 0.5--2~mag low based on similar extrapolations from IRAC 3.5 and 4.5\m\ data; when Extended Source Catalog fluxes appear unexpectedly faint, it is typically due to the comparatively small apertures used in the automated 2MASS extraction.  Hence we have extracted 2MASS flux densities for the vast majority of the LVL sample using the same apertures and foreground star removals used to determine IRAC and MIPS fluxes, as discussed in the following section.

\subsection {{\it Spitzer} 3.6, 4.5, 5.8, 8.0, 24, 70, and 160\m}

\subsubsection {Foreground Star and Background Galaxy Removal}

The presence of foreground stars and background galaxies can significantly affect the global infrared fluxes for some galaxies, particularly the fainter dwarfs and galaxies at how Galactic latitudes.  Once identified, the foreground stars and background galaxies are removed through a simple interpolation of the local sky from the images using the IRAF task {\tt IMEDIT}.  Our procedure for identifying these sources relies on a multi-wavelength analysis (3.6, 8.0, 24\m, and \hal), looking for objects especially blue (foreground stars; $f_\nu(3.6)/f_\nu(8.0)>8$) or small red systems that have galaxy morphologies and lie outside the main target galaxy profile yet still within the global aperture.  Archival {\it Hubble Space Telescope} imaging was also inspected for obvious background galaxy or foreground stellar identifications, when available.  When uncertain about the identification of a particular source, we opted to err on the conservative side and allow such sources to remain in the global flux extraction.  However, these sources of uncertain origin are typically very faint and negligibly impact global flux extractions.  
%Table~\ref{tab:data} includes the amplitude of the correction for foreground star/background galaxie -- the number in parentheses following each flux is the ratio of the flux corrected for foreground stars/background galaxies to the flux extracted from the unedited images.  
The median ratios of edited-to-unedited fluxes is [0.854,0.846,0.939,0.971,0.980,1.00,1.00] at [3.6,4.5,5.8,8.0,24,70,160]\m; very few significant corrections are made at 24, 70, and 160\m.
%particularly for the longer two wavelengths.
% see /d/lvl/flux/no_star_edits/compare_star_no_star.f

The uncertainties provided in Table~\ref{tab:data} include both calibration and statistical uncertainties.  Calibration uncertainties are 5-10\% for IRAC 3.6 and 4.5\m\ data, and 10-15\% for IRAC 5.8 and 8.0\m\ data; 10\% IRAC calibration uncertainties are used in Table~\ref{tab:data}.  MIPS calibration uncertainties are 4\%, 7\%, and 12\% respectively at 24, 70, and 160\m.

\subsubsection {Aperture Corrections}

For a given galaxy, the same aperture was used for extracting all IRAC and MIPS fluxes.  Elliptical apertures for IRAC and MIPS photometry were based on capturing all the galaxy emission visible for all IRAC and MIPS images.  Typically this means that the 3.6\m\ image was used to create the aperture, since the IRAC images are more sensitive than the MIPS images and 3.6\m\ is the {\it Spitzer} wavelength at which stars are brightest.

Since the IRAC flux calibration is based on point source photometry for a 12\arcsec\ radius aperture, the fluxes for all extended sources and aperture radii $\neq$ 12\arcsec\ need to have an additional correction applied.  These corrections account for the ``extended'' emission due to the wings of the PSF and also for the scattering of the diffuse emisssion across the IRAC focal plane.  As described in Dale et al. (2007), the IRAC extended source correction has been derived for a variety of source morphologies and extents.  For an effective aperture radius $r=\sqrt{ab}$ in arcseconds derived from the semi-major $a$ and semi-minor $b$ ellipse axes provided in Table~\ref{tab:data}, 
the IRAC extended source aperture correction is
\be
f^{\rm IRAC}_{\rm true} / f^{\rm IRAC}_{\rm measured} = A {\rm e}^{-r^B} + C,
\label{eqn:irac}
\ee
where $A$, $B,$ and $C$ are listed in Table~\ref{tab:IRAC_ap}
\footnote{See http://ssc.spitzer.caltech.edu/irac/calib/extcal/}.
%Equation of Dale et al. (2007) is used in this work to correct the IRAC fluxes.  
The median IRAC extended source aperture corrections are [0.914,0.941,0.826,0.756] at [3.6,4.5,5.8,8.0]\m\ and the largest corrections are [0.949,0.966,0.940,0.831] for BK03N.  

Somewhat different from the situation for IRAC imaging, the main reason MIPS aperture corrections are needed is due to the smearing of light outside the aperture.  MIPS aperture corrections are based on simulations carried out on the higher resolution 3.6\m\ images edited for foreground stars and background galaxies.  MIPS aperture corrections are empirically determined from a comparison of fluxes from smoothed and unsmoothed 3.6\m\ imaging, an approximate proxy for tracing the MIPS galaxy morphologies.  The aperture correction for a given MIPS flux is the ratio of the fluxs from the unsmoothed 3.6\m\ image to the flux from the 3.6\m\ image smoothed to the same PSF as the MIPS image in question.  
%See Table~XXX.  
The median MIPS aperture corrections are [1.01,1.01,1.02,] at [24,70,160]\m, and the most significant corrections are [1.09,1.12,1.42].  
%The uncertainties in the aperture corrections are typically a few percent, and are based on the differences between the canonical and ``minimum'' corrections.  Minimum MIPS aperture corrections are computed assuming point source light distributions.

\subsection {Upper Limits}
Many of the optically-faint galaxies in the sample are frequently undetected in the infrared, particularly at wavelengths of 5.8\m\ and longer; upper limits are included in Table~\ref{tab:data} for sources undetected by infrared imaging.  The 3$\sigma$ upper limits for {\it Spitzer} imaging are derived according to
\be
f_\nu(3\sigma~{\rm upper~limit}) ~ = ~ 3 ~ \sigma_{\rm sky} \Omega_{\rm pix} ~ \sqrt{N_{\rm pix}+{N_{\rm pix}}^2/N_{\rm sky}} ~ \approx ~ 3 ~ \sigma_{\rm sky} \Omega_{\rm pix} ~ \sqrt{2 N_{\rm pix}}
\ee
where $\sigma_{\rm sky}$ is the sky surface brightness fluctuation per pixel (MJy~sr$^{-1}$), $\Omega_{\rm pix}$ the solid angle subtended per pixel, $N_{\rm pix}$ the number of pixels in the galaxy aperture, and $N_{\rm sky}$ the number of pixels in the sky aperture.  The parameter $\sigma_{\rm sky}$ is approximately 0.02, 0.03, 0.11, 0.12, 0.2, 0.9, 1.7~MJy~sr$^{-1}$ at 3.6, 4.5, 5.8, 8.0, 24, 70, and 160\m, respectively (Lee et al. 2008).  A similar computation for 2MASS near-infrared upper limits is carried out after converting that survey's mean 10$\sigma$ point source sensitivities ($\sim$ 16.4, 15.5, and 14.8~mag for $J$, $H$, and $K_{\rm s}$, respectively; Skrutskie et al. 2006) to 3$\sigma$ values and accounting for the difference in the 4\arcsec\ radius 2MASS point source aperture and the LVL galaxy apertures.


\section{Results}
\label{sec:results}

\subsection{Detection Rate}
The bottom panel of Figure~\ref{fig:detection_rate} displays the detection rate as a function of $B$ band apparent magnitude for the different \Spitzer\ imaging channels.  Nearly all galaxies are detected at all \Spitzer\ wavelengths down to $B\approx14$~mag.  Interestingly, the $B\sim15.5$~mag cut-off for the outer tier of the sample that extends to 11~Mpc (see \S~\ref{sec:sample}) proved to be a useful sample selection criterion, as very few MIPS detections are available fainter than this magnitude limit.  The inner tier/ANGST portion of the sample extends the sample to much fainter levels, as faint as $B\approx19$~mag in the cases of BK03N and M~81~Dwarf~A.  As expected for the optically-faint galaxies, the highest detection rates are found for the stellar-dominated 3.6 and 4.5\m\ channels, while the 70 and 160\m\ imaging proved to be far more challenging to convincingly detect cold dust emission.  

%For reference all 75 SINGS galaxies, including several M~81 dwarfs, were detected in the stellar-dominated 3.6 and 4.5\m\ bands (the faintest galaxy, M~81~Dwarf~A with $B=16.5$~mag and no star formation at any wavelength, was a 2$\sigma$ detection; Dale et al. 2007). 

%With our MIPS observing strategy, we expected to detect most galaxies brighter than $B=15-16$~mag.  Fainter than $B\sim14.3$~mag, every galaxy in the SINGS sample and every galaxy in the MIPS starburst GTO sample is detected in all three bands.  For fainter objects ($B=14.5-18$~mag), the detection rate in those combined samples falls to 50\% (3 of 6).    We estimated that up to 25 of the 204 MIPS targets may be undetected by MIPS in at least the 10um band

\subsection{Multi-Wavelength Spectral Energy Distributions}
\label{sec:seds}
Figure~\ref{fig:seds1} provides the ultraviolet-infrared spectral energy distributions for all 258 galaxies.  The ultraviolet data are from Lee, Gil de Paz et al. (2008).  The solid curve is the sum of a dust (dashed) and a stellar (dotted) model.  The dust curve is a Dale \& Helou (2002) model (least squares) fitted to ratios of the observed 24, 70, and 160\m\ fluxes, and then scaled to match the overall infrared brightness.  The $\alpha_{\rm SED}$ listed within each panel parametrizes the distribution of dust mass as a function of heating intensity, as described in Dale \& Helou (2002).  To quantify the uncertainty on $\alpha_{\rm SED}$ displayed within each panel of Figure~\ref{fig:seds1}, 1,000 Monte Carlo simulations of the fit to each galaxy's far-infrared fluxes are performed, utilizing the tabulated flux uncertainties to add a random (Gaussian deviate) flux offset at each MIPS wavelength.  The $\alpha_{\rm SED}$ uncertainties reflect the standard deviations in the simulations. 
%Broadly speaking, smaller values of $\alpha_{\rm SED}$ (more heating from stronger interstellar radiation fields) correspond to later Hubble types and larger infrared-to-ultraviolet ratios.
The stellar curve is a 1~Gyr continuous star formation, solar metallicity curve from Vazquez \& Leitherer (2005) fitted to the 2MASS data.  The initial mass function for this curve utilizes a double power law form, with $\alpha_{\rm 1,IMF}=1.3$ for $0.1<m/M_\odot<0.5$ and $\alpha_{\rm 2,IMF}=2.3$ for $0.5<m/M_\odot<100$ (e.g., Kroupa 2002).  Though this stellar curve (not adjusted for internal extinction) may not be applicable to many galaxies, it is included as a ``standard'' reference against which deviations in the ultraviolet can be compared from galaxy to galaxy.  %The stellar curve also serves to highlight the relative importance of stars and dust in each galaxy, particularly in the transition from stellar to dust emission in the mid-infrared (e.g. NGC~1404 versus NGC~1482).

Mention anything about 8\m\ values falling below the SEDs?  Could be a prelude to the low 8-to-TIR discussion in the next section. 

\subsection{SEDs binned by TIR/UV?}

\subsection{Infrared Colors}
\label{sec:colors}
The IRAC-MIPS infrared colors for the LVL sample are displayed in panel a of Figure~\ref{fig:global_colors}.  The $f_\nu(70\micron)/f_\nu(160\micron)$ ratio typically traces the temperature of large interstellar grains, while the $f_\nu(8.0\micron)/f_\nu(24\micron)$ ratio has several influences.  The flux at 24\m\ mostly represents emission from very small grains (grains with effective radii of 15--40\AA; Draine \& Li 2007), and the flux at 8.0\m\ can have contributions from stars, hot dust, PAHs, and AGN.  Perhaps due to the diversity of emission mechanisms responsible for 8.0 and 24\m\ flux levels, the $f_\nu(8.0\micron)/f_\nu(24\micron)$ ratio spans two orders of magnitude compared to the single factor of $\sim$10 stretch in the the $f_\nu(70\micron)/f_\nu(160\micron)$ ratio.  Since the LVL sample largely lacks ``strong'' AGN, loosely defined here as AGN that dominate a galaxy's emission over substantial portions of the electromagnetic spectrum, it is unlikely that AGN contribute much to the scatter in Figure~\ref{fig:global_colors}.

The far-infrared or total infrared, respectively commonly defined as the emission from 42--122\m\ ({\it FIR}) and 8--1000\m\ or 3--1100\m\ ({\it TIR}), are frequently used as indications of the star formation rate in galaxies (Kennicutt 1998; Bell 2003).  However, in many instances the far-infrared continuum is unavailable or not detected, so monochromatic infrared proxies for ({\it FIR}) or ({\it TIR}) are occasionally employed (e.g., Bavouzet et al. 2008).  Hence, the tightness (dispersion) in monochromatic-to-bolometric ratios are of general interest.  Five flavors of these ratios are displayed in the remaining panels of Figure~\ref{fig:global_colors}, and a tabulation of median LVL infrared colors and monochromatic-to-bolometric infrared ratios can be found in Table~\ref{tab:ratios} along with their dispersions.  Panel b of Figure~\ref{fig:global_colors} shows the distribution of the 8.0\m\ emission with respect to the 3-1100\m\ total infrared, a distribution which 
%also displays a two order of magnitude stretch along with 
exhibits
a dispersion of 0.23~dex, similar to that for $f_\nu(70\micron)/f_\nu(160\micron)$ and $f_\nu(8.0\micron)/f_\nu(24\micron)$.  
%Many of the irregular systems in the SINGS sample of nearby galaxies have elevated $f_\nu(70\micron)/f_\nu(160\micron)$ ratios (e.g., Walter et al. 2006; Dale et al. 2007), indicating strong overall heating of the dust grain population.  
While it is evident that the LVL sample is distributed fairly evenly by morphology across $f_\nu(70\micron)/f_\nu(160\micron)$ ratios, the bulk of the systems exhibiting relatively low $f_\nu(8.0\micron)/f_\nu(24\micron)$ and $\nu f_\nu(8.0\micron$)/{\it TIR} ratios are from late-type spirals and irregulars.  

The preponderance of late-type spirals and irregulars showing relatively low 8.0\m\ emission is amplified when ``dust-only'' 8.0\m\ emission is considered.  Panel c of Figure~\ref{fig:global_colors} shows a plot similar to that in Panel b but with the stellar emission removed using the expression presented in Helou et al. (2004): 
\begin{equation}
\label{eq:fnu8*}
  \nu f_\nu(8.0\mu {\rm m})_{\rm dust} = \nu f_\nu(8.0\mu {\rm m}) - \eta^{8*} \nu f_\nu(3.6\mu {\rm m})
\end{equation}
where $\eta^{8*}=0.232 \times 3.6/8.0$.  The dispersion (0.44~dex) and overall range are significantly larger when the dust-only 8.0\m\ emission is normalized to the total infrared.  It is possible that a portion of these increases in dispersion and range are due to the inapplicability of Equation~\ref{eq:fnu8*} to late-type spirals, but it should be noted that Equation~\ref{eq:fnu8*} is based on a detailed analysis of NGC~300, a local system with an Sd morphological classification.  Another possibility is that the late-type spirals and irregulars within LVL are on average less abundant in heavy metals, and thus either the formation of PAH molecules is starved or the relatively fragile PAHs are photo-dissociated in the hard radiation fields typically associated with low-metallicity environments (Madden et al 2006; Dale et al. 2008).  Additional data and detailed follow-up utilizing LVL metallicities would be required to address this issue.

In contrast to the 8.0\m-to-{\it TIR} measures, the $\nu f_\nu(24\micron$)/{\it TIR} ratio (panel d of Figure~\ref{fig:global_colors}) shows a range less than an order of magnitude and a dispersion of 0.15~dex; the 70\m-to-{\it TIR} and 160\m-to-{\it TIR} ratios have even smaller dispersions (panels e \& f and Table~\ref{tab:ratios}).  The implication is that, compared to the 8.0\m\ emission from galaxies, the infrared emission from very small grains at 24\m\ and from large grains at 70 and 160\m\ are far more tightly coupled to the bolometric infrared emission.  This result conceptually follows work by Calzetti et al. (2007) and Kennicutt et al. (2007), who show that the 24\m\ flux is an effective tracer of a galaxy's current star formation rate, much more effective than is 8.0\m, particularly when the 24\m\ emission is coupled with \hal\ to capture the unobscured portion of star formation.


\section {Summary}
\label{sec:summary}

\acknowledgements 
Support for this work, part of the {\it Spitzer Space Telescope} Legacy Science Program, was provided by NASA through Contract Number XXX issued by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407.  This research has made use of the NASA/IPAC Extragalactic Database which is operated by JPL/Caltech, under contract with NASA.  This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.  IRAF, the Image Reduction and Analysis Facility, has been developed by the National Optical Astronomy Observatories and the Space Telescope Science Institute.

\begin {thebibliography}{dum}
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\bibitem{Dal02} Dale, D.A. \& Helou, G. 2002, \apj, 576, 159
%\bibitem{Dal05} Dale, D.A. et al. 2005, \apj, 633, 857
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\bibitem{Gil08} Gil de Paz, A. et al. 2008, in preparation
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\end {thebibliography}

%TABLES
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\begin{deluxetable}{lrcrrr}
\def\a{\tablenotemark{a}}
\def\b{\tablenotemark{b}}
\def\c{\tablenotemark{c}}
\def\d{$^\dagger$}
\def\p{$\pm$}
\tabletypesize{\scriptsize}
\tablenum{1}
\tablecaption{Infrared Photometry Apertures \label{tab:additional_data}}
\tablewidth{0pc}
\tablehead{
\colhead{Galaxy} &
\colhead{Optical} &
\colhead{$\alpha_0$~\&~$\delta_0$} &
\colhead{2$a$} &
\colhead{2$b$} &
\colhead{PA} 
\\
\colhead{} &
\colhead{Morphology} &
\colhead{(J2000)} &
\colhead{($\arcsec$)} &
\colhead{($\arcsec$)} &
\colhead{($\degr$)} 
}
\startdata
%\input /d/lvl/flux/aps.tex
\enddata     
\tablecomments{\footnotesize The position angles in the above ellipse parameters are measured east of north.}
\tablenotetext{a}{\footnotesize Infrared photometry for the Large and Small Magellanic Clouds will be provided by the SAGE (P.I. M. Meixner) and SAGE-SMC (P.I. K. Gordon) projects.}
\tablenotetext{b}{\footnotesize NGC~1800 and MCG-05-13-004 spatially overlap so separate photometry for MCG-05-13-004 is not provided.}
\tablenotetext{c}{\footnotesize The bright core of NGC~3034 (M~82) has rendered the {\it Spitzer} data extremely difficult to process; saturation effects severely limit our ability to extract reliable flux densities.}
%\tablenotetext{d}{\footnotesize}
\end{deluxetable}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\begin{deluxetable}{lcrrrrrrrrrr}
%\rotate
\def\a{\tablenotemark{a}}
\def\b{\tablenotemark{b}}
\def\c{\tablenotemark{c}}
\def\d{\tablenotemark{d}}
\def\e{\tablenotemark{e}}
\def\f{\tablenotemark{f}}
\def\p{$\pm$}
\tabletypesize{\scriptsize}
\tablenum{2}
\label{tab:data}
\tablecaption{Infrared Flux Densities}
\tablewidth{0pc}
\tablehead{
\colhead{Galaxy} &
\colhead{E(B-V)} &
\colhead{2MASS J} &
\colhead{2MASS H} &
\colhead{2MASS K$_{\rm s}$} &
\colhead{IRAC} &
\colhead{IRAC} &
\colhead{IRAC} &
\colhead{IRAC} &
\colhead{MIPS} &
\colhead{MIPS} &
\colhead{MIPS} 
\\
\colhead{} &
\colhead{} &
\colhead{1.25\m} &
\colhead{1.65\m} &
\colhead{2.17\m} &
\colhead{3.6\m} &
\colhead{4.5\m} &
\colhead{5.8\m} &
\colhead{8.0\m} &
\colhead{24\m} &
\colhead{70\m} &
\colhead{160\m} 
\\
\colhead{} & 
\colhead{(mag)} &
\colhead{(Jy)} &
\colhead{(Jy)} &
\colhead{(Jy)} &
\colhead{(Jy)} &
\colhead{(Jy)} &
\colhead{(Jy)} &
\colhead{(Jy)} &
\colhead{(Jy)} &
\colhead{(Jy)} &
\colhead{(Jy)} 
}
\startdata
%\input table1.tex
\enddata     
\vskip-0.3in
\tablecomments{\footnotesize See \S~\ref{sec:data} for corrections that have been applied to the data.  The uncertainties include both statistical and systematic effects ($\lesssim10$\% for the optical and near-infrared data).}
\tablenotetext{a}{\footnotesize Infrared photometry for the Large and Small Magellanic Clouds will be provided by the SAGE (P.I. M. Meixner) and SAGE-SMC (P.I. K. Gordon) projects.}
\tablenotetext{b}{\footnotesize NGC~1800 and MCG-05-13-004 spatially overlap so separate photometry for MCG-05-13-004 is not provided.}
\tablenotetext{c}{\footnotesize The bright core of NGC~3034 (M~82) has rendered the {\it Spitzer} data extremely difficult to process; saturation effects severely limit our ability to extract reliable flux densities.}
\tablenotetext{d}{\footnotesize Only 4.5 and 8.0\m\ data were obtained for IC~5152.}
\tablenotetext{e}{\footnotesize IRAC data taken from the archives.}
\tablenotetext{f}{\footnotesize MIPS data taken from the archives.}
\end{deluxetable}
%\clearpage
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\begin{deluxetable}{cccc}
\tabletypesize{\scriptsize}
\tablenum{3}
\label{tab:IRAC_ap}
%\tablecaption{IRAC Aperture Correction Parameters \label{tab:IRAC_ap}}
\tablecaption{IRAC Aperture Correction Parameters}
\tablewidth{0pc}
\tablehead{
\colhead{$\lambda$} &
\colhead{A} &
\colhead{B} &
\colhead{C} 
}
\startdata
3.5\m&   0.82&    0.370&   0.910\\
4.5\m&   1.16&    0.443&   0.940\\
5.8\m&   1.49&    0.207&   0.710\\
8.0\m&   1.37&    0.330&   0.740\\
\enddata
\tablecomments{\footnotesize See \S~\ref{sec:data} and http://ssc.spitzer.caltech.edu/irac/calib/extcal/}
\end{deluxetable}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\begin{deluxetable}{llc}
\tabletypesize{\scriptsize}
\tablenum{4}
\label{tab:ratios}
\tablecaption{LVL Infrared Ratios and Dispersions}
\tablewidth{0pc}
\tablehead{
\colhead{Ratio} &
\colhead{Median} &
\colhead{Dispersion} 
\\
\colhead{} &
\colhead{} &
\colhead{(dex)} 
}
\startdata
$f_\nu(70\micron)/f_\nu(160\micron$)        &   0.84~&0.22\\
$f_\nu(8.0\micron)/f_\nu(24\micron$)        &   0.41~&0.27\\
$\nu f_\nu(8.0\micron$)/{\it TIR}           &   0.098&0.23\\
$\nu f_\nu(8.0\micron)_{\rm dust}$/{\it TIR}&   0.19~&0.44\\
$\nu f_\nu(24\micron$)/{\it TIR}            &   0.080&0.15\\
$\nu f_\nu(70\micron$)/{\it TIR}            &   0.60~&0.11\\
$\nu f_\nu(160\micron$)/{\it TIR}           &   0.31~&0.12\\
\enddata
%\tablecomments{\footnotesize See \S~\ref{sec:data} and http://ssc.spitzer.caltech.edu/irac/calib/extcal/}
\end{deluxetable}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%FIGURES
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\begin{figure}
 \plotone{f4}
 \caption{Top: The distribution of LVL galaxies as a function of apparent $B$-band magnitude.  The shaded portion portrays the subsample that falls within 3.5~Mpc.  Bottom: The imaging detection rate for different \Spitzer\ wavelengths.}
 \label{fig:detection_rate}
\end{figure}

\begin{figure}
 \plotone{/d/lvl/flux/p01.ps}
 \caption{Globally-integrated 0.15-160\m\ spectral energy distributions for the LVL sample.  {\it GALEX}, 2MASS, and {\it Spitzer} data are represented by open triangles, filled squares, and filled circles, respectively.  Downward-pointing arrows, if present, indicate 3$\sigma$ upper limits.  The solid curve is the sum of a dust (dashed) and a stellar (dotted) model.  The dust curve is a Dale \& Helou (2002) model fitted to the amplitude and ratios of the observed 24, 70, and 160\m\ fluxes; the $\alpha_{\rm SED}$ listed within each panel parametrizes the distribution of dust mass as a function of heating intensity, as described in Dale \& Helou (2002).  The stellar curve is a 1~Gyr continuous star formation, solar metallicity curve from Vazquez \& Leitherer (2005) fitted to the 2MASS data (see \S~\ref{sec:seds} for details).}
 \label{fig:seds1}
\end{figure}

\begin{figure}
 \plotone{f3}
 \caption{Top: The {\it Spitzer} infrared colors and monochromatic-to-bolometric infrared ratios for globally-integrated LVL data.  The solid and dotted lines indicate the SED models of Dale \& Helou (2002) and Dale et al. (2001), respectively, derived from the average global trends for a sample of normal star-forming galaxies observed by \ISO\ and \IRAS.}
 \label{fig:global_colors}
\end{figure}

%\begin{figure}
% \plotone{f1}
% \caption{The infrared-to-far-ultraviolet ratio as a function of ultraviolet spectral slope.  Normal star-forming and starbursting galaxies from Kong et al. (2004) and Calzetti et al. (1995) are plotted in addition to the SINGS data points.  The dotted curve is that for starbursting galaxies from Kong et al. (2004) and the solid curve is applicable to normal star-forming galaxies (Cortese et al. 2006).}
% \label{fig:beta}
%\end{figure}
%
%\begin{figure}
% \plotone{f2}
% \caption{The infrared-to-ultraviolet ratio as a function of the specific star formation rate (Equation~\ref{eqn:ssfr}).  The error bars derive from the observational uncertainties plus a 30\% factor assumed for converting the $K_{\rm s}$ luminosity to a stellar mass (see Section~\ref{sec:ssfr}).}
% \label{fig:ssfr}
%\end{figure}

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\end{document}
