Ultraviolet imaging of planetary nebulae with GALEX\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$\mathit{GALEX}$\end{document}

Over four hundred Galactic Planetary Nebulae (PNe) have been imaged by GALEX\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$\mathit{GALEX}$\end{document} in two ultraviolet (UV) bands, far-UV (FUV, 1344–1786 Å, λeff=1528Å\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$\lambda _{eff}= 1528~{\mathring{\mathrm{A}}}$\end{document}) and near-NUV (NUV, 1771–2831 Å, λeff=2271Å\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$\lambda _{eff} = 2271~{\mathring{\mathrm{A}}}$\end{document}). We present examples of extended PNe, for which UV spectroscopy is also available, to illustrate the variety in UV morphology and color, which reflects ionization conditions. The depth of the GALEX imaging varies from flux ≈0.4/5×10−18ergscm−2s−1Å−1□′′−1\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$\approx 0.4/5\times 10 ^{-18}~\mbox{ergs}\,\mbox{cm}^{-2}\,\mbox{s}^{-1}\,{\mathring{\mathrm{A}}}^{-1}\,\square ^{\prime\prime\,-1}$\end{document} (FUV/NUV\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$\mathit{FUV}/\mathit{NUV}$\end{document}) for exposures of the order of ∼100\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$\sim 100$\end{document} seconds, typical of the survey with the largest area coverage, to ∼0.3/8.3×10−19ergscm−2s−1Å−1□′′−1\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$\sim 0.3/8.3\times 10^{-19}~\mbox{ergs}\,\mbox{cm}^{-2}\,\mbox{s}^{-1}\,{\mathring{\mathrm{A}}}^{-1}\,\square ^{\prime\prime\,-1}$\end{document} (FUV/NUV\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$\mathit{FUV}/\mathit{NUV}$\end{document}) for ∼1500sec\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$\sim 1500~\mbox{sec}$\end{document} exposures, typical of the second largest survey (see Bianchi in Astrophys. Space Sci. 320:11, 2009; Bianchi et al. in Adv. Space Res. 53:900, 2014). GALEX\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$\mathit{GALEX}$\end{document} broad-band FUV and NUV fluxes include nebular emission lines and in some cases nebular continuum emission. The sensitivity of the GALEX\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$\mathit{GALEX}$\end{document} instrument and the low sky background, especially in FUV, enable detection and mapping of very faint ionization regions and fronts, including outermost wisps and bow shocks. The FUV-NUV\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$\mathit{FUV}\mbox{-}\mathit{NUV}$\end{document} color of the central star provides a good indication of its Teff\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$T_{eff}$\end{document}, because the GALEX\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$\mathit{GALEX}$\end{document} FUV-NUV color is almost reddening-free for Milky Way type dust (Bianchi et al. in Astrophys. J. Suppl. Ser. 230:24, 2017; Bianchi in Astrophys. Space Sci. 335:51, 2011, Bianchi in Astrophys. Space Sci. 354:103, 2014) and it is more sensitive to hot temperatures than optical colors.


Introduction
Planetary Nebulae (PN) are the evolved descendants of intermediate mass stars, the major providers of important chemical elements such as carbon and nitrogen. The expanding layers of gas, shed in the previous Red Giant phases and then ionized by the hot central star (CSPN), offer clues about the progenitor's evolution, in particular about the chemical elements produced by nucleosynthesis and brought up to outer layers, about the temperature and luminosity of the stellar remnant, through their ionization, and about massloss and wind momentum in subsequent phases, through their complex expansion kinematics and density structure. Studies of both the nebula and the central star benefit by observations in the Ultraviolet (UV), where crucial diagnostic transitions of important chemical elements, and trace elements, abound (e.g., Bianchi 2016Bianchi , 2012. CSPNe, the hottest stars known, emit most of their light at UV wavelengths or shortwards. IUE and HST spectrographs have collected UV spectra of a few hundred PNe, mostly of their central stars. FUSE has provided high resolution spectra at shorter UV wavelengths (905-1187 Å) for several objects. The FUSE observations, although difficult to obtain and limited to the brightest sources, have enabled major discoveries, such as highly ionized neon in the wind of CSPNe (Herald et al. 2005;Bianchi 2009, 2011;Keller et al. 2011, among others), whose lines are a crucial diagnostics for the hottest (T eff > 85000 K) CSPN; the brightest PNe in the Magellanic Clouds were also observed by FUSE (Her- Fig. 1 The "Helix" PN (NGC 7293, PK036-57.1) observed with GALEX. The color-composite image shows FUV in blue, NUV in yellow. Note that field stars, which are mostly of low temperature, appear yellow. At a distance of 219 pc (Harris et al. 2007), the GALEX ∼ 5 resolution corresponds to 0.005 pc. The lower panel shows a zoomed-in portion of the image, and a plot of archival IUE spectra taken in the bright part of the nebula, with the GALEX transmission bands overplotted, suggesting that the FUV flux mostly originates from HeII emission in the inner regions ald and Bianchi 2004Bianchi , 2007. For a review of the role of UV observations in the understanding of CSPNe see Bianchi (2012).
A completely different, new type of information has become available thanks to the deep sensitivity and wide field of view of the GALEX instrument. In this work we show examples of UV images of Planetary Nebulae, which uniquely complement ground-based and HST imaging in optical emission lines, and spectroscopic information.  . In most cases the central star is saturated, so the flux value at radius ∼ 0 is not meaningful. Images have different size (in arcsec), to optimally display the PN: the extent of each object in UV can be estimated from the X-axis scale of the flux profiles. Archival IUE spectra are shown with the GALEX FUV, NUV transmission curves overplotted described by Martin et al. (2005), and its performance by Morrissey et al. (2007). The characteristics of the data and the sky surveys are described by Bianchi (2009), Bianchi et al. (2011a, 2011b, 2014; in depth discussion of data quality and an updated version of science-enhanced catalogs of UV sources are presented in Bianchi et al. (2017Bianchi et al. ( , 2018.

The data: UV imaging
GALEX imaged the field in two bands simultaneously: FUV (1344-1786 Å, λ eff = 1528 Å) and NUV (1771-2831 Å, λ eff = 2271 Å), with a field of view of 1.28/1.24 • [FUV/NUV] diameter, and resolution of ≈ 4.2/5.3 [FUV/ NUV]. The images, reconstructed from photon counting detector recordings, are sampled with virtual pixels of 1.5 size. GALEX sky coverage is fairly complete except for the Galactic plane, due to brightness safety limits (see Bianchi et al. 2017Bianchi et al. , 2014 which explains why the known PNe samples, mostly concentrated near the Galactic plane, are not entirely included in the UV surveys. Of the over 1000 known Galactic Planetary Nebulae, about 400 are included in the GALEX UV imaging surveys, out of the 1312 objects list of Kerber et al. (2003) with an additional ∼20 objects from the list of 111 new PN candidates of Acker (2016, Vizier online Table 1). Most are observed in the All-sky Imaging Survey (AIS), which has by far the largest sky coverage (see Bianchi et al. 2014Bianchi et al. , 2017, with a typical minimum exposure of ∼100 seconds (5 σ flux limit ∼ 0.4/5 × 10 −18 ergs cm −2 s −1 Å −1 −1 in FUV/NUV). Some objects have exposures up to several thousand seconds. Figures 1, 2 and 3 show seven PNe observed by GALEX, for which IUE archival spectra exist. The spectra are use- , but only about 100 of them were observed with both FUV and NUV detectors on (thick-lines, smaller histograms on the left panel). The magnitudes correspond to the best-fit of each source shape as determined by the pipeline; more details for extended objects resolved by GALEX will be provided in a forthcoming paper, where measurements of the central star will be isolated, and curve-of-growth provided for the nebula (Gómez-Muñoz et al. 2018). The vertical lines mark the flux limit above which non-linearity sets in (10% roll-off limit), for FUV and NUV (blue-dashed and red-dotted lines respectively) ful to interpret the nature of the UV emission in the broadband images of the nebula. There is little overlap between the GALEX sample and the PNe observed spectroscopically by IUE or HST, because the objects observed spectroscopically were mostly too bright for GALEX; on the other hand, interesting features such as faint outer shells, wisps and sharp cusps at the edges of the outer shells, seen clearly in some GALEX images, are beyond the reach of past spectroscopic capabilities, and mostly unaccessible also to current and forthcoming UV spectrographs. GALEX FUV and NUV images present a unique advantage, as they reveal outer features which are critical e.g., to interpret the dynamical co-evolution of the nebular shell within the surrounding medium (e.g., Villaver et al. 2018) as well as a challenge, because the broad-band filters may include several emission lines (Figs. 2 and 3) as well as stellar (in the PN center) and nebular continuum (Fig. 4). To help the interpretation of the GALEX broad-band fluxes, the scant IUE spectroscopic data and GALEX grism data (e.g., Bianchi et al. 2012) will be complemented by a grid of ionization models (Gómez-Muñoz et al. 2018); consistency with corollary data further helps the interpretation of the UV images. Figures 2 and 3 show for each PN the GALEX combined FUV and NUV image, and radially averaged flux profiles.

Discussion
For the objects with archival UV spectroscopy, some central stars exceed the brightness limit for GALEX non-linearity or saturation, therefore the flux profile is not meaningful at radius ∼ 0, and measurements of FUV and NUV magnitudes for such CSPNe are not reliable. For PNe with marked asymmetries a radially averaged flux profile is a simplified representation, nonetheless it gives a compact and homogeneous indication of the overall flux level and FUV-NUV color distribution, with good significance because of the integration over annuli areas.
The sample in Figs. 2 and 3 shows a wide variety in morphology and ionization structure, illustrating the rich information contained in the UV wavelength range. The radial profiles in this bright sample show that almost everywhere in the nebula the FUV flux is higher than the NUV flux, in spite of the NUV filter having a much wider wavelength window. In some cases the FUV and NUV profiles are similar, which may also indicate nebular continuum emission significantly contributing to the flux. Figure 4 shows that the nebular continuum is rather flat across the GALEX wavelength range, for a range of typical nebular conditions. It is computed adding the contributions of H and He recombination and two-photon continuum. In some cases (e.g., NGC 40) the FUV and NUV profiles are significantly dis-crepant, suggesting a complex ionization structure across the nebula. Figure 5 gives an overview of the distribution in magnitude and FUV-NUV color of the known objects included in the GALEX surveys. Because the FUV detector failed before the mission was completed, and most of the regions towards the Galactic plane were observed late in the mission (Bianchi et al. , 2017, about 400 objects have at least NUV measurements, and about 100 of them were observed with both NUV and FUV detectors on. Some PNe are included in more than one observation, amounting to a total of over 600 measurements of ∼400 objects. The magnitudes used for Fig. 5 are the best fit to the source shape performed by the GALEX pipeline, thus they may have a different meaning for extended (resolved) or compact objects, the relative contribution of the central star and nebular flux varying across the sample. A forthcoming work will extricate measurements of the central star and curves of growth for the PN flux for objects extended enough to be resolved by GALEX (Gómez-Muñoz et al. 2018).
More information on GALEX data, science catalogs and projects can be found at the author's UVSKY web site http:// dolomiti.pha.jhu.edu/uvsky.