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The Great Observatories All-Sky LIRG Survey: Herschel Image Atlas and Aperture Photometry1

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The Great Observatories All-Sky LIRG Survey: Herschel Image Atlas and Aperture Photometry1 The Great Observatories All-Sky LIRG Survey: Herschel Image Atlas and Aperture Photometry1 Jason K. Chu1, D. B. Sanders1, K. L. Larson1;2, J. M. Mazzarella2, J. H. Howell2, T. D´ıaz-Santos2;3, K. C. Xu4, R. Paladini4, B. Schulz4, D. Shupe4, P. Appleton4, L. Armus2, N. Billot5, B. H. P. Chan2, A. S. Evans6;7, D. Fadda2, D. T. Frayer7, S. Haan7, C. M. Ishida8, K. Iwasawa9, D.-C. Kim7, S. Lord10, E. Murphy7, A. Petric11, G. C. Privon12, J. A. Surace13, E. Treister12 ABSTRACT Far-infrared (FIR) images and photometry are presented for 201 Luminous and Ultraluminous In- frared Galaxies [LIRGs: log (LIR=L ) = 11:00 − 11:99, ULIRGs: log (LIR=L ) = 12:00 − 12:99], in the Great Observatories All-Sky LIRG Survey (GOALS) based on observations with the Herschel Space Observatory Photodetector Array Camera and Spectrometer (PACS) and the Spectral and Photometric Imaging Receiver (SPIRE) instruments. The image atlas displays each GOALS target in the three PACS bands (70, 100, and 160 µm) and the three SPIRE bands (250, 350, and 500 µm), optimized to reveal structures at both high and low surface brightness levels, with images scaled to simplify comparison of structures in the same physical areas of ∼100 × 100 kpc2. Flux densities of companion galaxies in merg- ing systems are provided where possible, depending on their angular separation and the spatial resolution in each passband, along with integrated system fluxes (sum of components). This dataset constitutes the imaging and photometric component of the GOALS Herschel OT1 observing program, and is comple- mentary to atlases presented for the Hubble Space Telescope (Evans et al: 2017, in prep.), Spitzer Space Telescope (Mazzarella et al: 2017, in prep.), and Chandra X-ray Observatory (Iwasawa et al: 2011, 2017, in prep.). Collectively these data will enable a wide range of detailed studies of AGN and starburst activity within the most luminous infrared galaxies in the local Universe. Subject headings: atlases — galaxies: active — galaxies: interactions — galaxies: starburst — galaxies: structure — infrared: galaxies 1. Introduction 1Institute for Astronomy, University of Hawaii, 2680 Wood- lawn Drive, Honolulu, HI 96822; [email protected], The Great Observatories All-Sky LIRG Survey [email protected] (GOALS, Armus et al. 2009), combines both imag- 2 Infrared Processing & Analysis Center, MS 100-22, California ing and spectroscopic data for the complete sam- Institute of Technology, Pasadena, CA 91125; bchan, jhhowell, klar- son, lee, [email protected], [email protected] ple of 201 Luminous Infrared Galaxies (LIRGs: 3Nucleo de Astronom´ıa de la Facultad de Ingenier´ıa, Universi- dad Diego Portales, Av. Ejercito Libertador 441, Santiago, Chile; tat de Barcelona (IEEC-UB), Mart´ı i Franques` 1, 08028 Barcelona, arXiv:1702.01756v1 [astro-ph.GA] 6 Feb 2017 [email protected] Spain; [email protected] 4NASA Herschel Science Center, MS 100-22, California Insti- 10SETI Institute; [email protected] tute of Technology, Pasadena, CA 91125; apple, bschulz, cxu, pala- 11Canada France Hawaii Telescope Corp., Concepcion,´ Chile; dini, [email protected] [email protected] 5 Observatoire de l’Universite´ de Geneve,´ 51 chemin des Mail- 12Instituto de Astrof´ısica, Facultad de F´ısica, Pontificia Univer- lettes, 1290 Versoix, Switzerland; [email protected] sidad Catolica´ de Chile, Casilla 306, Santiago 22, Chile; gprivon, 6Department of Astronomy, University of Virginia, Char- [email protected] lottesville, VA 22904-4325; [email protected] 13Spitzer Science Center, MS 314-6, California Institute of Tech- 7National Radio Astronomy Observatory, 520 Edgemont nology, Pasadena, CA 91125; [email protected] Road, Charlottesville, VA 22903-2475; dfrayer, dkim, emur- 1Based on Herschel Space Observatory observations. Herschel [email protected], [email protected] is an ESA space observatory with science instruments provided by 8Department of Physics and Astronomy, University of Hawaii at European-led Principal Investigator consortia and with important Hilo, Hilo, HI, 96720; [email protected] participation from NASA. 9ICREA and Institut del Ciencies` del Cosmos (ICC), Universi- 1 log (LIR=L ) > 11:0) selected from the IRAS Re- ric measurements are given in x6. Section 7 contains vised Bright Galaxy Sample (RBGS, Sanders et al. a discussion of basic results, including comparisons 2003). The full RBGS contains 629 objects, represent- with prior measurements, and a summary is given in ing a complete sample of extragalactic sources with x8. A reference cosmology of ΩΛ = 0:72; Ωm = 0:28 −1 −1 IRAS 60 µm flux density, S60 > 5:24 Jy, covering and H0 = 70 km sec. Mpc is adopted, however the entire sky above a Galactic latitude of jbj > 5◦. we also take into account local non-cosmological ef- The median redshift of objects in the GOALS sam- fects by using the three-attractor model of Mould et al. ple is hzi = 0:021, with a maximum redshift of (2000). zmax = 0:0876. As the nearest and brightest 60 µm extragalactic objects, they represent a sample that 2. The GOALS Sample is the most amenable for study at all wavelengths. The primary objective of the GOALS multi-wavelength The IRAS RBGS contains a total of 179 LIRGs survey is to fully characterize the diversity of proper- (log (LIR=L ) = 11:0−11:99), and 22 ultra-luminous ties observed in a large, statistically significant sample infrared galaxies (ULIRGs: log (LIR=L ) ≥ 12:0); of the nearest LIRGs. This allows us to probe the full these 201 objects comprise the GOALS sample (Ar- range of phenomena such as normal star formation, mus et al. 2009), a statistically complete flux-limited starbursts, and active galactic nuclei (AGN) that power sample of infrared-luminous galaxies in the local uni- the observed far-infrared emission, as well as to bet- verse. In addition to the Herschel observations re- ter characterize the range of galaxy types (i. e. normal ported here, the GOALS objects have been the subject disks, major and minor interactions/mergers, etc.) that of an intense multi-wavelength observing campaign, are associated with the LIRG phase. A secondary ob- including VLA 20 cm (Condon et al. 1990, 1996), mil- jective is to provide a data set that is ideally suited for limeter wave spectral line observations of CO(1!0) comparison with LIRGs observed at high redshifts. emission (Sanders et al. 1991), sub-millimeter imag- ing at 450 µm and 850 µm (Dunne et al. 2000), near- GOALS currently includes imaging and spec- infrared images from 2MASS (Skrutskie et al. 2006), troscopy from the Spitzer, Hubble, GALEX, Chandra, optical and K-band imaging (Ishida 2004), as well as XMM-Newton, and now Herschel space-borne obser- space-based imaging from the Spitzer Space Telescope vatories, along with complementary ground-based ob- (IRAC and MIPS, Mazzarella et al: 2017, in prep), servations from ALMA, Keck, and other telescopes. Hubble Space Telescope (ACS, Evans et al: 2017, in The GOALS project is described in more detail at prep.), GALEX (NUV and FUV, Howell et al. 2010), http://goals.ipac.caltech.edu/. and the Chandra X-ray Observatory (ACIS, Iwasawa Due to limitations in angular resolution, wavelength et al. 2011, 2017 in prep). Extensive spectroscopy data coverage, and sensitivity of pre-Herschel (IRAS, ISO, also exist on the GOALS sample, such as in the op- Spitzer, AKARI) far-infrared (FIR) data, the spatial dis- tical (Kim et al. 1995) and with Spitzer IRS in the tribution of FIR emission within the GOALS sources, mid-infrared (Stierwalt et al. 2013). Herschel PACS and the total amount of gas and dust in these sys- spectroscopy was obtained in Cycles 1 and 2 target- tems, are poorly determined. The Herschel data will ing the [C II] 157.7 µm, [O I] 63.2 µm, and [O III] allow us for the first time to directly probe the critical 88 µm emission lines and the OH 79 µm absorption FIR and submillimeter wavelength regime of these in- feature for the entire sample, as well as the [N II] 122 frared luminous systems, enabling us to accurately de- µm line in 122 GOALS galaxies (D´ıaz-Santos et al. termine the bolometric luminosities, infrared surface 2013, 2014, 2017 in prep). In addition, Herschel brightnesses, star formation rates, and dust masses and SPIRE FTS spectroscopy were obtained to probe the temperatures on spatial scales of 2 – 5 kpc within the CO spectral line energy distribution from J = 4 ! 3 GOALS sample. up to J = 13 ! 12 for 93 of the GOALS objects This paper presents imaging and photometry for all (Lu et al. 2014, 2015, 2017, submitted), as well as the 201 LIRGs and LIRG systems in the IRAS RBGS that [N II] 205 µm emission line for 122 objects Zhao et al. were observed during our GOALS Herschel OT1 pro- (2013, 2016). gram. A more complete description of the GOALS Out of the original list of 203 GOALS systems, sample is given in x2. The data acquisition is described two were omitted from our Herschel sample, making in x3 and data reduction procedures are discussed in for a final tally of 201 objects. IRAS F13097–1531 x4. The image atlas is presented in x5, and photomet- 2 (NGC 5010) was part of the original RBGS sample of Sanders et al. (2003), however due to a revision in the redshift of the object it was much closer than thought. This caused the resulting far-IR luminosity to drop sig- 11 nificantly below the LIRG threshold of 10 L . The other object we excluded from our sample is IRAS 05223+1908, which we believe is a young stellar ob- ject (YSO), due to the fact that its spectral energy dis- tribution (SED) peaks in the submillimeter part of the spectrum.
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