Submillimetre Photometry of 323 Nearby Galaxies from the HerschelHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. Reference Survey.

Submillimetre Photometry of 323 Nearby Galaxies from the Herschelthanks: Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. Reference Survey.

L. Ciesla Laboratoire d’Astrophysique de Marseille - LAM, Université d’Aix-Marseille & CNRS, UMR7326, 38 rue F. Joliot-Curie, 13388 Marseille Cedex 13, France    A.Boselli Laboratoire d’Astrophysique de Marseille - LAM, Université d’Aix-Marseille & CNRS, UMR7326, 38 rue F. Joliot-Curie, 13388 Marseille Cedex 13, France    M. W. L. Smith School of Physics and Astronomy, Cardiff University, Queens Buildings The Parade, Cardiff CF24 3AA, UK    G. J. Bendo UK ALMA Regional Centre Node, Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, United Kingdom    L. Cortese European Southern Observatory, Karl Schwarzschild Str. 2, 85748 Garching bei Muenchen, Germany    S. Eales School of Physics and Astronomy, Cardiff University, Queens Buildings The Parade, Cardiff CF24 3AA, UK    S. Bianchi INAF-Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125 Firenze, Italy    M. Boquien Laboratoire d’Astrophysique de Marseille - LAM, Université d’Aix-Marseille & CNRS, UMR7326, 38 rue F. Joliot-Curie, 13388 Marseille Cedex 13, France    V. Buat Laboratoire d’Astrophysique de Marseille - LAM, Université d’Aix-Marseille & CNRS, UMR7326, 38 rue F. Joliot-Curie, 13388 Marseille Cedex 13, France    J. Davies School of Physics and Astronomy, Cardiff University, Queens Buildings The Parade, Cardiff CF24 3AA, UK    M. Pohlen School of Physics and Astronomy, Cardiff University, Queens Buildings The Parade, Cardiff CF24 3AA, UK    S. Zibetti INAF-Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125 Firenze, Italy Dark Cosmology Centre, Niels Bohr Institute University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark    M. Baes Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, 9000, Gent, Belgium    A. Cooray Department of Physics & Astronomy, University of California, Irvine, CA 92697, USA 10 California Institute of Technology, 1200 E. California Blvd, Pasadena, CA 91125, USA    I. de Looze Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, 9000, Gent, Belgium    S. di Serego Alighieri INAF-Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125 Firenze, Italy    M. Galametz Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA    H. L. Gomez School of Physics and Astronomy, Cardiff University, Queens Buildings The Parade, Cardiff CF24 3AA, UK    V. Lebouteiller CEA/DSM/IRFU/Service d’Astrophysique, CEA, Saclay, Orme des Merisiers, Batiment 709, F-91191 Gif-sur-Yvette, France    S. C. Madden CEA/DSM/IRFU/Service d’Astrophysique, CEA, Saclay, Orme des Merisiers, Batiment 709, F-91191 Gif-sur-Yvette, France    C. Pappalardo INAF-Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125 Firenze, Italy    A. Remy CEA/DSM/IRFU/Service d’Astrophysique, CEA, Saclay, Orme des Merisiers, Batiment 709, F-91191 Gif-sur-Yvette, France    L. Spinoglio Istituto di Fisica dello Spazio Interplanetario, INAF, Via Fosso del Cavaliere 100, I-00133 Roma, Italy    M. Vaccari Dipartimento di Astronomia, Università di Padova, vicolo Osservatorio, 3, 35122 Padova, Italy Astrophysics Group, Physics Department, University of the Western Cape, Private Bag X17, 7535, Bellville, Cape Town, South Africa    R. Auld School of Physics and Astronomy, Cardiff University, Queens Buildings The Parade, Cardiff CF24 3AA, UK    D. L. Clements. Astrophysics Group, Imperial College, Blackett Laboratory, PrinceConsort Road, London SW7 2AZ, UK
Received; accepted
Key Words.:
Galaxies: ISM; Infrared: galaxies; Surveys; Catalogs

The Herschel Reference Survey (HRS) is a guaranteed time Herschel key project aimed at studying the physical properties of the interstellar medium in galaxies of the nearby universe. This volume limited, K-band selected sample is composed of galaxies spanning the whole range of morphological types (from ellipticals to late-type spirals) and environments (from the field to the centre of the Virgo Cluster). We present flux density measurements of the whole sample of 323 galaxies of the HRS in the three bands of the Spectral and Photometric Imaging Receiver (SPIRE), at 250 m, 350 m and 500 m. Aperture photometry is performed on extended galaxies and point spread function (PSF) fitting on timeline data for unresolved objects; we carefully estimate errors and upper limits. The flux densities are found to be in good agreement with those of the HeViCS and KINGFISH key projects in all SPIRE bands, and of the Planck consortium at 350 m and 550 m, for the galaxies in common. This submillimetre catalogue of nearby galaxies is a benchmark for the study of the dust properties in the local universe, giving the zero redshift reference for any cosmological survey.

1 Introduction

Dust grains in the interstellar medium (ISM) of galaxies profoundly affect our view of these systems by absorbing the ultra-violet (UV) and optical stellar emission and re-emitting it in the infrared, from m to 1 mm. Dust is produced by the aggregation of metals injected into the interstellar medium by massive stars, through stellar winds (Höfner 2009; Gomez et al. 2010b), supernovae (Clayton et al. 1997; Bianchi & Schneider 2007; Matsuura et al. 2011; Gomez et al. 2012), or less massive stars in their final evolution stages, such as asymptotic giant branch stars (Gehrz 1989; Dwek 1998; Galliano et al. 2008). Generally intermixed with gas in the ISM, dust is thus a good tracer of the cold molecular and atomic phases of the ISM and contains a significant fraction of metals. Dust plays an important role in the interstellar medium as it acts as a catalyst in the transformation process of the atomic to molecular hydrogen, shields the UV radiation field preventing the dissociation of molecular clouds, and contributes to the cooling and heating of the ISM in photodissociation regions (Wolfire et al. 1995). The 5-70 m spectral range corresponds to the emission of the hot dust generally associated with star formation whereas at longer wavelengths, up to 1mm, the submillimetre emission is generally dominated by the emission from the cold dust (e.g. Bendo et al. 2010, 2012a; Boquien et al. 2011). IRAS (Neugebauer et al. 1984), COBE (1989), ISO (Kessler et al. 1996), Spitzer (Werner et al. 2004), and AKARI (Murakami et al. 2007) allowed us to study the emission of the dust up to 240 m. However, most of the cold dust emission is drowned by warm dust at wavelengths shorter than 240 m. An accurate determination of dust masses requires submillimetre data (Devereux & Young 1990; Gordon et al. 2010; Galametz et al. 2011; Bendo et al. 2012a). Ground-based facilities, such as SCUBA on JCMT (Holland et al. 1999), reveal the submillimetre domain but observations of large samples of normal galaxies such as ours is still prohibitive due to the long integration times needed for these instruments. The Herschel Space Observatory (Pilbratt et al. 2010), launched in May 2009, opens a new window on the far-infrared/submillimetre spectral domain (55 to 672 m) and allows us to probe the cold dust component in large numbers of nearby galaxies.

To characterize the dust properties in the local universe, the Spectral and Photometric Imaging Receiver (SPIRE) (Griffin et al. 2010) Local Galaxies Working Group (SAG 2) has selected 323 galaxies to be observed as part of the Herschel Reference Survey (HRS) (Boselli et al. 2010b). The HRS is a guaranteed time key project and a benchmark study of dust in the nearby universe. The goals of the survey are to investigate (i) the dust content of galaxies as a function of Hubble type, stellar mass and environment, (ii) the connection between the dust content and composition and the other phases of the interstellar medium, and (iii) the origin and evolution of dust in galaxies. The HRS spans the whole range of morphological types including ellipticals to late-type spirals, with a few irregular dwarf galaxies, and environments (from relatively isolated field galaxies to members of the core of the Virgo Cluster). The sample is ideally defined also because of the availability of a large set of ancillary data. Multiwavelength data, from the literature, are available for about 90% of HRS galaxies from IRAS (Sanders et al. 2003; Moshir & et al. 1990; Thuan & Sauvage 1992; Soifer et al. 1989; Young et al. 1996); optical and near-infrared from SDSS (Abazajian et al. 2009) and 2MASS (Jarrett et al. 2003), and radio from NVSS (Condon et al. 1998) Êand FIRST (Becker et al. 1995). Most of these data are available on NED and GOLDMine (Gavazzi et al. 2003). Some of them are already released or currently analysed by our team such as UV data from GALEX (Boselli et al. 2011, Cortese et al., submitted), Spitzer/IRAC (Ciesla et al., in prep), and Spitzer/MIPS (Bendo et al. 2012b). H imaging (Boselli et al., in prep), CO(J=1-0) spectroscopy (Boselli et al., in prep), optical integrated spectroscopy (Boselli et al., submitted), CO(J=3-2) JCMT mapping (Smith et al. in prep), and gas metallicities (Hughes et al. 2012, submitted) will be soon available.

The first scientific results, based on a subsample of HRS data obtained during the Science Demonstration Phase (SDP) data, were presented in the A&A Herschel Special Issue (2010). Statistical studies based on this data set investigate the far-infrared/submillimetre colours (Boselli et al. 2012), the dust scaling relations as a function of environment and galaxy type (Cortese et al. 2012), and the properties of the early-type galaxies in the sample (Smith et al. 2012). A preliminary analysis of the spectral energy distributions (SEDs) was done as part of the SDP (Boselli et al. 2010a) while the complete analysis and modelling of the SEDs of the whole sample is in preparation (Ciesla et al., in prep). Thanks to the high angular resolution of Herschel (18 at 250 m, leading to a resolution of a few kpc at 20 Mpc), studies of large resolved HRS galaxies (with angular sizes between 2 and 10) within kiloparsec-sized subregions are also possible (Bendo et al. 2012a; Boquien et al. 2012).

The aim of this paper is to present the HRS catalogue of the flux densities at 250, 350 and 500 m. The paper is organised as follows. In Section 2, we briefly describe the HRS sample. Section 3 gives the description of the Herschel/SPIRE observations and data reduction. Section 4 details the techniques used for the flux extraction. In Section 5, we provide flux densities of the whole sample and in Section 6, we compare our results to those available in the literature.

2 The sample

The HRS galaxies are selected according to several criteria fully described in Boselli et al. (2010b). The HRS is a volume limited sample composed of galaxies at a distance between 15 and 25 Mpc. The galaxies are selected according to their K band magnitude, whose luminosity is a proxy for the total stellar mass (Gavazzi et al. 1996). Based on the optical extinction studies and far-infrared observations at wavelength shorter than 200 m, we expect late-type galaxies to have a larger content of dust than early-types (Sauvage & Thuan 1994). Thus, two different limits have been adopted: 12 for late-types and 8.7 for early-types (in Vega magnitudes). Finally, to limit any contamination from Galactic cirrus, we selected galaxies at high Galactic latitude () and with low Galactic extinction regions ( Schlegel et al. 1998). The final sample contains 323111With respect to the original sample given in Boselli et al. (2010b), the galaxy HRS 228 should be removed from the complete sample because its updated redshift on NED indicates it as a background object. galaxies, 62 early-types and 261 late-types.

3 Herschel/SPIRE observations and data reduction

3.1 Observations

We observed the 323 HRS galaxies with SPIRE (Griffin et al. 2010) in three wide bands at 250, 350 and 500 m. In order not to duplicate Herschel observations, 79 galaxies out of 323 were observed as part of the open time key project the Herschel Virgo Cluster Survey (HeViCS, Davies et al. 2010).

For the 239 galaxies outside the Virgo cluster plus 4 Virgo galaxies observed during the Science Demonstration Phase, the observations are carried out using the SPIRE scan-map mode with a nominal scan speed of 30″s. The sizes of the images depend on the optical extent of the targets and have been chosen to cover 1.5 times the optical diameter, 222The diameter at 25 mag arcsec., of the galaxies, which is the full area over which the infrared emission is expected. Previous observations of spiral discs indeed indicated that the infrared emission of late-type galaxies can be more extended than the optical disc (Bianchi et al. 2000). For galaxies with an optical diameter smaller than , the small scan-map mode is used to provide a homogeneous coverage of a circular area of diameter. For galaxies with an optical diameter larger than , the large scan-map mode is used to cover, at least, . The resulting sizes of the maps are thus , , and , depending on the optical size of the target. As early-type galaxies are known to contain less dust than late-types (Ferrarese et al. 2006), longer integration times were used on this subsample (Smith et al. 2012). For late-types, 3 pairs of cross-linked scan maps are made, while 8 pairs for early-types.

HeViCS covers at full depth ( in total), of the centre of the Virgo cluster at five wavelengths, from 100 to 500 m, using the PACS/SPIRE parallel mode, down to the confusion limit in the SPIRE bands (Davies et al. 2012). For the 79 HRS galaxies observed by HeViCS, the PACS/SPIRE parallel mode scan map is used with a scan speed of 60″ s done with 4 pairs of perpendicular scans. Regions around each of the 79 galaxies are cut off from the large fields to perform the aperture photometry. They are large enough to provide a good estimate of the background emission.

3.2 Data reduction

The complete description of the data reduction and map-making procedures will be presented in a dedicated paper by Smith et al. (in prep). Here, we just give a brief summary of the different steps carried out within the Herschel Interactive Pipeline Environment software (HIPE; Ott 2011). The SPIRE data are processed up to Level-1, the level where the pointed photometre timelines are derived, with a script adapted from the official scan map pipeline (Griffin et al. 2009; Dowell et al. 2010). The only difference to the Level-1 product is that we use the optimised deglitcher setting available for the observing mode. The typical SPIRE pipeline performs the following data processing steps on the timelines:

  1. Application of the glitch removal procedure to delete the cosmic rays that affect all detectors in an individual array, and then application of the wavelet glitch removal of cosmic rays from individual detectors (WaveletDeglitcher) for HRS data. For HeViCS data, the sigmaKappaDeglitcher is used.

  2. Application of an electrical low pass filter response correction, to correct for the delay in the data coming out of the electronics; this matches the detector timelines to the astrometric pointing timelines.

  3. Reapplication of the wavelet glitch removal for the HRS data; this additional step improves the removal of all glitches.

  4. Application of an additional time response correction.

  5. Flux calibration, which includes nonlinearity corrections.

  6. Removal of the temperature drift where all bolometers are brought to the same level using a custom method called BriGAdE (Smith et al. in prep).

  7. Corrections of the bolometer time response, which adjusts the bolometer detector timelines to account for the fact that the bolometers do not respond instantaneously to signal.

  8. Creation of the final maps using the naive map maker included in the standard pipeline.

The pipeline also performs some steps related to associating the astrometry with the bolometer timeline data and performs some minor time corrections before the mapmaking step.

[b]

Table 1: Summary of the properties of SPIRE image data.
250 m 350 m 500 m
Pixel size () 6″ 8″ 12″
Map FWHM 18.2″ 24.5″ 36.0″
Beam area () 423 arcsec 751 arcsec 1587 arcsec
Correction for extension ()
Correction for updated calibration 1. 1.
Total correction ()

The pixel sizes and FWHM values of the final maps are provided in Table LABEL:corr. By default, the pipeline applies a correction to the maps, called , that converts the flux densities weighted by the relative spectral response function (RSRF) in monochromatic flux densities, corresponding to spectra where is constant. In doing this, the pipeline considers all sources as point-like objects. However, the RSRF changes for extended sources, so we need to divide the data by the for point sources, automatically applied by the pipeline, and apply the for extended sources instead. For such extended sources, the resulting correction is thus , and their values are provided by the SPIRE Observer Manual333http://herschel.esac.esa.int/Docs/SPIRE/html/spire˙om.html. There are, in our sample, galaxies which are almost point-like that would not need this 444For simplicity, here we define =, for the exact definition refer to the SPIRE Observer Manual correction. Defining if a source is barely resolved can be subjective, thus for clarity, we defined two groups: one for point-like sources, one for extended sources using a quantitive criterion (see Section 4.1). We apply this correction for extended sources on all resolved galaxies of the HRS sample.

To update the maps product for the present work to the latest calibration (HIPE v8, SPIRE calibration tree v8.1), we multiply all 350 m measurements by 1.0067, the most recent flux calibration (SPIRE photometry cookbook555http://herschel.esac.esa.int/twiki/pub/Public/SpireCalibrationWeb/SPIREPhotometryCookbook˙jul2011˙2.pdf, Bendo et al. 2011). These corrections are listed in Table LABEL:corr, we define the total correction as the combination of correction for extension () and the correction for updated calibration.

3.3 Colour corrections

The SPIRE flux calibration assumes that the sources have a spectrum with constant across the filter. This assumption does not correspond to the SEDs of the objects observed (Boselli et al. 2010a). The observed SEDs of the target galaxies are close to a modified black body with a spectral index ranging from 1.0 to 2.0 (Boselli et al. 2012). Tuned colour corrections could thus be required. To quantify these colour corrections, we assume that the far-infrared spectrum can be farely well represented by a modified black body with a spectral index of 1.5 or 2.0 Table 2 lists the colour corrections that should be applied for different sets of and . They were obtained by integrating a modified blackbody of given and over the SPIRE spectral response function for each band. For extended sources, the spectral response functions have been weighted by (SPIRE Observer Manual) thus resulting in different sets of colour corrections for extended sources with respect to point sources. Indeed, for feedhorn bolometers in general and for the detectors in SPIRE specifically, the relative spectral responsivity function (RSRF) changes between point-like and extended sources as explained in Section 5.2.1 of the SPIRE Observers’ Manual. The colour corrections rely upon the integral of the product of the spectrum and the RSRF, then if the RSRF changes, the colour corrections will also change. We give the values for both point-like and extended sources. They are multiplicative corrections. Given the still poorly constrained shape of the SED of the target galaxies, these corrections listed in Table 2 are not applied to the set of data given in Table 9.

Extended Point like
250 m 350 m 500 m 250 m 350 m 500 m
1.026 1.025 1.044 1.023 0.995 0.959
1.019 1.009 1.021 0.984 0.959 0.917
1.005 0.996 1.007 0.955 0.938 0.896
0.994 0.988 0.999 0.937 0.925 0.884
0.985 0.983 0.994 0.924 0.917 0.876
1.021 1.025 1.049 1.026 1.004 0.977
1.022 1.014 1.031 0.995 0.972 0.940
1.011 1.004 1.020 0.970 0.953 0.920
1.002 0.998 1.014 0.953 0.942 0.909
0.995 0.993 1.009 0.941 0.934 0.902
0.990 0.990 1.006 0.933 0.929 0.897
0.986 0.987 1.003 0.926 0.925 0.893
0.983 0.985 1.001 0.922 0.922 0.890
0.981 0.984 1.000 0.918 0.919 0.888
666 Multiplicative factors to apply to correct values for galaxies with spectral energy distributions well represented by a modified black body with a grain emissivity parameter and a temperature in the given ranges. Color corrections for and , are consistent with those given in Davies et al. (2012); in that paper, however, the correction is included in the color correction for extended sources, while here it is included in the fluxes.
Table 2: The colour corrections for the SPIRE data for extended and point-like sources.

4 Flux extraction

As we chose long integration times in order to reach the confusion limit, the images include faint background sources. Furthermore, despite a high Galactic latitude selection, some images show the presence of Galactic cirrus. Our sample contains large extended galaxies, point-like sources and non-detected galaxies. These technical aspects, related to the nature of the emitting source and of the sky background emission around it, prevent us from performing an automatic photometry. Three methods are needed to accurately measure the flux for all of objects: a first method for point-like sources (PSF fitting on timeline data), a second for extended ones (aperture photometry) and the third for the determination of upper limits.

4.1 Point-like sources

SPIRE is calibrated using a timeline-based PSF fitting approach. It is then possible to extract the flux densities of point-like sources directly from the timeline data using a PSF fitting method. The PSF fitter fits a two-dimensional Gaussian function to the signal and position timeline data. For unresolved sources, the peak of the Gaussian function from the fit corresponds to the flux density of the source. For more information, see Bendo et al. (2012, in prep). Based on tests of aperture photometry versus timeline-based PSF fitting for SPIRE data, there is significantly worse accuracy and precision for aperture photometry on unresolved sources. Moreover, there are some systematic effects that are actually due to the mapping technique (related to where bolometers tend to cross over the unresolved sources). Timeline-based PSF fitting actually avoids those biases for point sources. The SPIRE-ICC (Instrument Control Center) strongly recommends the use of PSF fitting on timeline data for unresolved sources (SPIRE Observer’s Manual777http://herschel.esac.esa.int/Docs/SPIRE/html/spire˙om.html Section 5.2.11).

To identify point-like sources and measure their flux densities, we proceed with the following method. All of the images are inspected in order to make a list of point-like sources candidates. We run the timeline-based PSF fitter program and use the criterion given by the SPIRE photometry cookbook. For a given band, if the FWHM of the resulting gaussian fitted to the timeline data is smaller than 20″, 29″and 37″at 250, 350 and 500 m, respectively, then the source is considered as point-like. These limits for the FWHM were determined empirically by adding artificial randomly-placed sources to timeline data and then performing timeline-based PSF fits to those data. The resulting distribution of FWHM indicates that 20″, 29″and 37″are acceptable upper limits for the typical FWHM that will be measured for sources. According to this criterium, in the whole HRS sample, there are 10, 10 and 9 point-like sources at 250, 350 and 500 m, respectively. As the timeline data are calibrated in Jy/beam, the timeline fits for these data give amplitudes that correspond to the flux densities of the sources. These will be the most accurate flux densities that can be measured for these sources, as the measurement technique matches the method applied to the primary and secondary sources used for SPIRE flux calibration. As the pipeline is optimised for point sources, their flux densities do not need to be corrected with the correction described in Section 3.2 and provided in Table LABEL:corr. However, the 350 m measurements are corrected for the HIPE v8 updated calibration, thus they are multiplied by 1.0067.

4.2 Extended sources

The aperture photometry of extended sources is carried out using the DS9/Funtools program “Funcnts”. This task performs a basic aperture photometry, summing all pixels within a defined elliptical region. The mean value of the background is calculated in a given annulus and then subtracted from the counts of the aperture. With “Funcnts”, we can extract the counts in elliptical regions adapted to match the shape of the galaxies.

To understand and quantify the contribution of background features in the measurements, we choose three different objects as representative examples, as illustrated in Figure 1. There are three extreme cases. The first one is M99 (HRS 102) which is a bright resolved face-on spiral. The second one is NGC 3945 (HRS 71), a nearly face-on barred spiral, lying in a region polluted by a strong cirrus emission. The last one is NGC 4550 (HRS 210), an unresolved faint early-type galaxy. This source is treated as all point-like sources, but we choose to include it as a comparison with the two previous extended galaxies. Different growth curves are obtained when the background is estimated in different regions, as depicted in Figure 1. Here the different growth curves (colored lines) are obtained when the sky background is estimated in annuli of constant width of 60″ but of 30″ increasing radii. M99 (HRS 102) is a prototypical case with no particular problems since its growth curve reaches a plateau. Indeed, M99 is very bright, thus its flux density is not affected by faint background sources at large radii. On the contrary, the presence of Galactic cirrus strongly affects the flux density measurements, as for NGC 3945 (HRS 71). In this case, the growth curves do not saturate after a given radius. The curves of NGC 4550 (HRS 210) clearly show the contribution of background features at radii greater than , where is the optical semi major axis taken from NED. Furthermore, as NGC 4550 (HRS 210) is in a crowded field, several background sources contribute to any background region chosen. The HRS sample is composed of galaxies of different properties such as those shown in Figure 1. It is thus clear that a standard, automatic procedure cannot be blindly applied for the extraction of the flux densities of all the sources. We thus need to define appropriate apertures for each object.

To define the apertures, we apply two different methods, one for the extended sources, mainly late-type galaxies, and another one for resolved but compact object, generally early-types. We inspect the infrared images and compare them with the optical ones. For most of the late-types, the infrared disk is more extended than its optical counterpart. We find that taking an elliptical diameter of 1.4 times the optical one is large enough to contain all the infrared emission of these galaxies. However, in some particular cases, this standard aperture needs to be adapted, especially for galaxies which are interacting, galaxies with a companion or a strong background source within the standard aperture. For instance, HI-deficient888The HI-deficiency is defined as the difference, in logarithmic units, between the HI mass expected from an isolated galaxy with the same morphological type and optical diameter and the observed HI mass (Haynes et al. 1984). spiral galaxies of the Virgo cluster have truncated dust disks (Cortese et al. 2010). Furthermore, edge-on spirals have an optical semi-minor axis very small and is not large enough to include the extended structure due to the side-lobes of the SPIRE beams (a typical example is NGC 4565-HRS 213 in Figure 14). We thus modify the ellipticity of edge-on galaxies of the aperture to include all the infrared emission.

Elliptical galaxies, even if resolved, have a faint compact infrared emission concentrated in the center. Lenticulars are the intermediate type between ellipticals and spirals. They contain extended dust but generally not beyond the optical emission. For all of these galaxies, the apertures are adapted to match the emission and avoid any major background contamination.

For all galaxies, the background contribution is measured in a region defined as a circular annulus of inner radius , with a 60″ width. This choice is dictated by the fact that we want to quantify any possible contribution of large scale fluctuations in the sky background on source, but at the same time extract flux densities sufficiently far from the target to avoid any contamination of the galaxy to the sky background estimate. The width of the annulus is taken as a good compromise between the will of having a reliable statistic to estimate the background, and the will of avoiding as much as possible contamination from background sources and images features. We performed a detailed check on every background region to avoid or minimize any kind of source contamination (companion galaxy, strong background sources, etc).

Figure 1: Growth curves at 250 m of the galaxies M 99 (HRS 102), NGC 3945 (HRS 71), and NGC 4550 (HRS 210). The different colored curves are obtained by changing the background estimate region as described in the text. The vertical red dashed lines correspond to the FWHM of the SPIRE beam at 250 m. The right panels show the 250 m images of the three galaxies, the black ellipses indicate the optical shapes of the galaxies.

The ellipses used for the aperture photometry and the circular annuli used for the background estimation are listed in Table 8, organized as follows:

  • Column 1: Herschel Reference Survey name (HRS).

  • Column 2: Zwicky name, from the Catalogue of Galaxies and of Cluster of Galaxies, (Zwicky et al. 1968, CGCG).

  • Column 3: Virgo Cluster Catalogue name, (Binggeli et al. 1985, VCC).

  • Column 4: Uppsala General Catalogue name, (Nilson 1973, UGC).

  • Column 5: New General Catalogue name, (Dreyer 1888, NGC).

  • Column 6: Index Catalogue name, (Dreyer 1895, IC).

  • Column 7: Right Ascension J2000 (RA).

  • Column 8: Declination J2000 (Dec).

  • Column 9: Semi major axis of the aperture, in arcseconds ().

  • Column 10: Semi minor axis of the aperture, in arcseconds ().

  • Column 11: Position Angle, in degree (PA) (from North to East).

  • Column 12: Inner radius of the background circular annulus, in arcseconds ().

  • Column 13: Outer radius of the background circular annulus, in arcseconds ().

Figure 14 shows the optical and infrared images of the HRS galaxies, along with the apertures used. Table LABEL:apratios gives the mean and median infrared to optical aperture diameter ratios for elliptical, lenticular and late-type galaxies respectively, where the infrared diameter is the one listed in Table 8.

Median ratio Mean ratio Chosen ratio
E 0.38 0.29 0.30
S0, S0a, S0/Sa 0.76 0.88 0.80
Late-types 1.40 1.41 1.40
999The chosen ratios are used to calculate upper limits of sources not detected with SPIRE.
Table 3: Median, mean and chosen infrared to optical aperture ratios of detected galaxies according to their morphological type.

4.3 Aperture correction

Figure 2: Simulation of the photometry of an extended face-on spiral galaxy at 500 m. Upper panel: a flat extended source. In red, the integrated radial profile of the original source, and in blue of the convolved source. In orange, the convolved to original source flux density ratios. The dashed line marks the size of the original source. Lower panel: an extended galaxy with a linear surface brightness profile.

As defined in Section 4.2, these apertures have been expressly chosen to include all of the infrared emission of the galaxies. Studying the emission of extended galaxies observed with Herschel, Dale et al. (2012) have shown that, at low surface brightness, the shape of the PSF can affect the emission at the edge of any object. They empirically defined the aperture correction as the ratio between the flux density measured on the IRAC 8.0 m unsmoothed image, and the flux density measured on the same image smoothed to a Herschel band PSF. They found a median value of 1.0 at all wavelengths, with maximum corrections between 7% and 13% for SPIRE. To quantify the effect of the wings of the PSF on our measurements, and understand whether a specific correction is required, we do the following exercise. The maximal effect is expected for an extended galaxy with a flat radial profile and a sharp edge at 500 m. We create a mock galaxy on an image with the Herschel 500 m resolution, and with a constant surface brightness of 1 Jy beam dropping to 0 at a radius of 204″. Using the 500 m PSF provided by Sibthorpe et al.101010ftp://ftp.sciops.esa.int/pub/hsc-calibration/SPIRE/PHOT/Beams/, we convolve the mock galaxy with the SPIRE 500 m PSF. We carry out the photometry using circular apertures from to in steps of on both the original and convolved images (Figure 2). The largest aperture correction is at the radius of the original source (204″). For a linear decreasing surface brightness profile, more physical but still extreme, the correction drops to . These 2-5 corrections can be considered as an upper limit for our data because: i) a flat radial profile is quite unphysical and ii) our apertures have been expressly chosen larger than the infrared size of the galaxies. As we always choose the aperture greater than the infrared emission of the galaxy (except for galaxies in particular configurations like NGC 4567-HRS 215 and NGC 4568-HRS 216), the aperture correction is thus much smaller than . As the calibration errors (7%) are greater than the aperture corrections, we choose not to apply them on our measurements and consider our flux densities as integrated values.

4.4 Photometric uncertainties

There are two sources of uncertainty when carrying out photometry on SPIRE images, the systematic errors due to the absolute flux calibration and the stochastic errors related to the flux extraction technique. The calibration errors are (1) the uncertainty on the models used to determine the flux density of Neptune (5), (2) a 2 random uncertainty that is measured from the standard deviation in the ratio of the measured Neptune flux density to the model Neptune flux density. The resulting calibration error is 7 in all bands (Swinyard et al. 2010; SPIRE Observer’s Manual). Technically, the errors should add together quadratically, but the SPIRE team decided to use 7 as a conservative upper limit on the flux calibration. As the methods used for point-like and extended source photometry are different, the stochastic error estimation is computed in different ways.

4.4.1 Point-like sources

The uncertainty for point-like sources is calculated by performing tests in which artificial point sources with the same flux density as the target were added to the timeline data at random locations within a box centered on each source. The artificial sources were then fit with the timeline-based source fitter using the same settings as were applied to each target galaxy. A hundred iterations of adding artificial sources to the fields around each galaxy were performed, and the standard deviation of the flux densities of the artificial sources was used as the uncertainty in the flux density measurement of the target galaxy. The highest value of the point-like source errors is 5 mJy for sources with a flux density less than 200 mJy.

4.4.2 Extended sources

For aperture photometry of extended sources, the stochastic total error, , depends mainly on (1) the instrumental error, , (2) the confusion error, and (3) the error on the determination of the sky background, . We calculate the errors on our flux density measurements according to the formula:

(1)

The instrumental error:

The instrumental error is due to the noise of the instrument which depends on the number of scans crossing a pixel. Assuming it independent from pixel to pixel, the instrumental error is:

(2)

where is the number of pixels within the aperture and is the pixel per pixel uncertainty measured in the aperture on the error map provided by the pipeline. Mean values of are 1.2, 1.4 and 2.4 of the total flux density at 250, 350 and 500 m, respectively.

The confusion error:

The confusion error is due to the presence of background sources (i.e. faint point-like sources) within the aperture. As the beam size is larger than the pixel size, this uncertainty is correlated between neighboring pixels. A point-like background source will then affect several pixels. The confusion error is:

(3)

where is the confusion noise. Here, we assume the values estimated by Nguyen et al. (2010), i.e. , and mJy/beam at 250, 350 and 500 m respectively. The pixel size of the images and the beam area are given in Table LABEL:corr. Mean values of are 4.2, 5.8 and 9.2 of the total flux density at 250, 350 and 500 m, respectively. They are thus dominant with respect to the instrument noise.

The background error:

The uncertainty on the sky background comes from large scale structures not removed during the map-making procedure. These large scale structures, for instance, can be due to Galactic cirrus, as those evident in Figure 1 of Davies et al. (2012) in the Virgo Cluster. Indeed, despite the fact that the galaxies are selected at high Galactic latitude, some images are contaminated by cirrus (see Figure 1). They contribute to the galaxy emission and/or to the background determination. To determine , the uncertainty on the background, we take pixel boxes around the galaxy in the image map for all of the three bands, we calculate the standard deviation of the mean values of the same boxes, as described in Boselli et al. (2003). Ideally we would estimate from boxes with a similar number of pixels to the apertures used for the photometry. This was not possible due to the sizes of the images. The effect of using smaller boxes will be to give us a conservative estimate of . The number of boxes depends on the size of the galaxy and on the size of the image; the mean numbers of boxes are 16, 14 and 11 at 250, 350 and 500 m. The error on the sky determination is:

(4)

where is the uncertainty of the background. Mean values of are 8.0, 9.6 and 10.3 of the total flux density at 250, 350 and 500 m, respectively. is thus the dominant error for extended galaxies.

Figure 3 shows the influence of each error component as a function of the number of pixels of the aperture, assuming mean values of and ( is constant at a given band). The background error is the dominant source of uncertainty for extended galaxies of size larger than 80 pixels, which is the case for more than 90 of the galaxies of our sample.

Figure 3: Error components versus the number of pixels of the aperture and the histogram of the number of pixels.

Independent measurements

As part of the Science Demonstration Phase, 15 extended galaxies were observed in both the HRS and HeViCS projects. To test the reproducibility of our measurements and the accuracy of our errors, we compare the flux densities of the two sets of data. Indeed, we have two sets of independent images of the same galaxies produced by two different SPIRE scan modes. We perform the photometry on these two sets and compare the flux densities measured in exactly the same conditions (same apertures, same background regions and same photometric procedure). The names and flux densities of these sources from both HRS and HeViCS data are listed in Table LABEL:sdp. Figure 4 shows the ratio between the flux densities from HRS images and the flux densities from HeViCS images in the three bands. The median differences between the flux densities are 1.6, 1.9 and 3.0 at 250, 350 and 500 m, respectively. We can consider these values as a lower limits to the photometric uncertainty on the flux densities measured in this work.

HRS Name HRS HeViCS
250 m 350 m 500 m 250 m 350 m 500 m
mJy mJy mJy mJy mJy mJy
102 NGC 4254
106 NGC 4276
122 NGC 4321
152 NGC 4412
158 NGC 4423
160 NGC 4430
162 NGC 4435
163 NGC 4438
165 UGC 7579
182 NGC 4480
190 NGC 4501
206 IC 3521
217 NGC 4569
220 NGC 4579
223 UGC 7802
Table 4: The 15 extended galaxies observed in both HRS and HeViCS projects for the Herschel Science Demonstration Phase.
Figure 4: Ratio between flux density measurements of 15 galaxies from HRS images and measurements of the same 15 galaxies from HeViCS images. Blue diamonds are for 250 m flux densities, green triangles are for 350 m and red squares are for 500 m.

Table LABEL:err indicates the mean total stochastic error for the extended sources within the HRS, for early-types and late-types galaxies separately, and for different flux density ranges. Calibration errors are not included. Adding the calibration errors, the mean total errors are 9, 11 and 13 at 250, 350 and 500 m, respectively, which is consistent with the 10, 10 and 15 estimated by Davies et al. (2012).

250 m 350 m 500 m
All 6.2 8.2 11.1
E 20.2 25.8 20.9
S0, S0a, S0/Sa 9.0 13.2 19.1
Late-types 5.9 7.6 10.5
mJy 21.8 24.6 21.6
mJy mJy 10.2 10.9 10.2
mJy 4.6 5.9 5.9
Table 5: Mean stochastic errors () on the HRS flux densities for extended galaxies.

4.5 Undetected sources

Bona fide detected galaxies are identified through a visual inspection of the images rather than following strict signal to noise criteria. This choice is dictated by the fact that, given the different nature of the sky background and of the emitting source, we might have strong detections but with a very low signal to noise (this is for instance the case of HRS 71 which has an uncertain flux density measurement since lying in a cirrus dominated region) or very high signal to noise sources with uncertain values (point like sources which can be easily confused with background objects). If we limit our sample to extended sources with no cirrus contamination nor nearby companions, our detection threshold is S/N 3, 2 and 2 at 250, 350 and 500 m, respectively, where the S/N is defined as the ratio of the flux density over the total uncertainty .

For the undetected galaxies (39, 42 and 47 galaxies at 250, 350 and 500 m, respectively), an upper limit is determined as:

(5)

where is estimated as in Equation 1. The measure of requires the adoption of a representative aperture, , for each undetected source. We make three different assumptions according to the morphology of the undetected galaxies. We form 3 groups: (a) type E, (b) type S0, S0a, S0/Sa and (c) late-types. For both group (a) and (b), we calculate the ratio between the semi-major axis of the infrared elliptical aperture and the semi-major axis of the optical diameter of the detected galaxies of the same morphological type (Table LABEL:apratios). Given the mean values measured for detected sources, we decided to adopt for ellipticals and for S0 and S0/Sa. We take for late-type galaxies, as we do for detected late-types. The radii of the circular region used for the calculation of upper limits are then 0.3, 0.8 or 1.4 times the optical semi-major axis for ellipticals, lenticular and spiral galaxies, respectively. For galaxies detected only in one or two bands, but not in the others, we use the aperture defined at these bands and take as the radius of the circular aperture to calculate the upper limit in the other bands. A minimum conservative and independent of radius for upper limit apertures has been set to not to have apertures smaller than the SPIRE resolution.

250 m 350 m 500 m
E 32 32 23
S0, S0a, S0/Sa 60 58 55
Late-types 97 96 95
Table 6: Detection rates in each band for different morphology classes.
Figure 5: The surface brightness versus the stellar mass at 250 (top panel), 350 (middle panel) and 500 m (bottom panel). Filled triangles are for detections, empty triangles for non-detections. Red, orange and blue colors are for elliptical, lenticular and late-type galaxies, respectively. Triangles with a green contour are point-like sources.

To test whether these upper limits are realistic, we plot in Figure 5 the surface brightness of the galaxies versus their stellar mass calculated as in Boselli et al. (2009) (for details, see Boselli et al. 2012). The surface brightness is calculated by dividing flux densities by the infrared size of galaxies, i.e. the aperture size. The detection limit in surface brightness of our survey is 0.03, 0.02 and 0.008 mJy arcsec at 250, 350 and 500 m, respectively. The only extended galaxy with a surface brightness below this threshold is M86 (HRS150) whose dust emission comes from a peculiar feature probably stripped from a nearby star forming system (Gomez et al. 2010a). At 350 m, the other detected galaxy with a low surface brightness is NGC4636 (HRS241) which is a faint, clearly detected, compact source. Few sources have a relatively high surface brightness at 250 m but are non detected at 350 and 500 m. These sources are close to point-like and are well detected at 250 m. However, at 350 and 500 m, they become as faint as the background sources, with a comparable surface brightness. To be conservative, we thus consider them as undetected sources. These two galaxies are particular cases, thus we consider that our upper limits are realistic as they lie at the lower limit of the detections.

Table LABEL:detectrate gives the detection rate in each band for the 3 groups: ellipticals (E), lenticulars (S0, S0a, S0/Sa) and late types.

5 Flux densities calculation

SPIRE maps are in Jy/beam. Flux densities, upper limits and errors of extended sources are thus converted into mJy using Equation 6.

(6)

where the pixel size of the images, , the beam area, , and the correction, (latest HIPE v8 calibration111111http://herschel.esac.esa.int/twiki/bin/genpdf/Public/HipeWhatsNew8x?pdforientation=portrait&pdftoclevels=3 and extended sources corrections) are given in Table LABEL:corr.

5.1 The data table

The flux densities of the 323 HRS galaxies in the three SPIRE bands (without colour corrections applied) are given in Table 9, organized as follows:

  • Column 1: HRS name.

  • Column 2: Flag of the 250 m flux density (); 0: Non-detection, 1: Detection (extended source), 2: Detection (point-like source), 3: Overestimation of the flux density due to the presence of a strong background source or a companion galaxy, 4: Presence of Galactic cirrus.

  • Column 3: Flux density at 250 m () in mJy.

  • Column 4: Flag of the 350 m flux density (); see Column 2.

  • Column 5: Flux density at 350 m ( ) in mJy.

  • Column 6: Flag of the 500 m flux density (); see Column 2.

  • Column 7: Flux density at 500 m () in mJy.

  • Column 8: Number of pixels in the 250 m aperture ().

  • Column 9: Number of pixels in the 350 m aperture ().

  • Column 10: Number of pixels in the 500 m aperture ().

  • Column 11: Instrumental error at 250 m, determined as in Equation 2 ().

  • Column 12: Instrumental error at 350 m, determined as in Equation 2 ().

  • Column 13: Instrumental error at 500 m, determined as in Equation 2 ().

  • Column 14: Confusion error at 250 m, determined as in Equation 3 ().

  • Column 15: Confusion error at 350 m, determined as in Equation 3 ().

  • Column 16: Confusion error at 500 m, determined as in Equation 3 ().

  • Column 17: Sky error at 250 m, determined as in Equation 4 ().

  • Column 18: Sky error at 350 m, determined as in Equation 4 ().

  • Column 19: Sky error at 500 m, determined as in Equation 4 ().

The , and are not provided for point-like galaxies (i.e. flag 2) as their errors are calculated with a different method (see Section 4.4.1). The total errors provided in Table 9 do not contain the calibration error of 7 which can be added in quadrature.

6 Comparison with the literature

Submillimetre photometry in the 250-550 m spectral domain is available for some HRS galaxies from Davies et al. (2012), Auld et al. (submitted), Dale et al. (2012) and Planck Collaboration et al. (2011).

Comparison with the HeViCS Bright Galaxy Catalogue

Figure 6: A comparison of the flux densities of the 59 sources common to both the HRS sample and the HeViCS Virgo bright galaxy sample (Davies et al. 2012) at 250, 350 and 500 m. Red triangles are for early type galaxies, blue triangles for late type galaxies. The dashed line indicates the linear fit.

We compare our results with those of Davies et al. (2012) (Figure 6) who used a different method to perform the photometry. They carried out a study on 78 bright Virgo galaxies as part of the HeViCS. Before extracting flux densities, they smoothed and re-gridded the 250 m and 350 m images to the 500 m resolution and pixel scale. They defined “by eye” elliptical apertures and a concentric annulus (for background estimation) on the 500 m image and used them at all bands. For consistency with our work, we apply the corrections to their measurements, using the values given in Table LABEL:corr. For the 59 galaxies in common to both the HRS and HeViCS surveys, mean values of the flux density ratios between their measurements on HeViCS fields and in this work are , and at 250, 350 and 500 m. Thus our fluxes and those of Davies et al. (2012) are consistent with each other. Auld et al. (2012, submitted) present a comparison between the flux densities of the optically selected Virgo galaxies, from the Virgo Cluster Catalogue (VCC), and HRS ones, for galaxies in common. Despite the different techniques used (automatic for Auld et al. 2012), the measurements are in good agreement.

Comparison with KINGFISH

KINGFISH (Key Insights on Nearby Galaxies: A Far-Infrared Survey with Herschel; Kennicutt et al. 2011) is a survey of 61 nearby galaxies observed in PACS and SPIRE bands. Dale et al. (2012) provide the flux densities of this sample in which six galaxies are in common with the HRS. The comparison is important as the images of the targets are the same but the data reduction, map-making, and flux extraction use different methods. They carried out aperture photometry using ellipses and applied aperture correction, which are of the order of a few percents (Dale, private communication). They also applied Galactic extinction corrections to their measurements. These corrections are however very small since they do not exceed 0.4, where this value has been determined for an object . The background is estimated by taking the mean value of several regions circumscribing the galaxy. The correction is applied to their flux densities to have consistency between their and our measurements.

Flux densities are compared in Figure 7 (left panel). Mean HRS to KINGFISH flux density ratios are , and at 250, 350, and 500 m. At 250 and 350 m the results are in very good agreement but not at 500 m. This 7% discrepancy can be due to the differences in the data reduction and map-making or in the flux extraction procedures. To understand if its origin comes from the method used to perform the photometry, we apply our flux extraction technique on the public KINGFISH images. On Figure 7 (right panel), we show the flux density ratio of the measurements obtained in this work to those given by Dale et al. (2012) (crosses), as well as to those that we have extracted using our own procedure on the public KINGFISH images (diamonds). At 250 m, all sets of data are consistent. At 350 m, the flux densities measured on KINGFISH images with our procedure are higher than ours. As the same method to extract fluxes is employed, this difference is due to the data reduction and map-making procedure applied by the SAG2 and the KINGFISH team. We note also a systematic difference between Dale et al. (2012) measurements and ours on the same images. This is due to the different flux extraction methods. At 500 m, the flux densities measured on KINGFISH images with our procedure are lower than our measurements, this discrepancy comes from the different production of the images. As at 350 m, we note the systematic error due to the different methods used to perform the photometry. The discrepancies observed between HRS and KINGFISH flux densities is thus a combination between differences in the production of the images and differences in the way the photometry is performed.

Figure 7: Left panel: Comparison between KINGFISH (Dale et al. 2012) and HRS flux densities of six common galaxies: NGC 4254 (HRS 102), NGC 4321 (HRS 122), NGC 4536 (HRS 205), NGC 4569 (HRS 217), NGC 4579 (HRS 220) and NGC 4725 (HRS 263) in the three SPIRE bands. Blue diamonds, green triangles and red squares are for the 250, 350 and 500 m measurements respectively. The dashed lines give the linear fits. Right panel: the flux density ratio obtained in this work to those given by Dale et al. (2012) (crosses), as well as to those that we have extracted using our own procedure from the public KINGFISH images (diamonds).

Comparison with Planck

We also compare our measurements with the Planck Early Release Compact Source Catalog (ERCSC) of the Planck Collaboration (Planck Collaboration et al. 2011). The catalogue contains flux densities derived from several method. To be consistent with this work, we use the measurements determined from aperture photometry. Cross-matching the two catalogues, we find 155 galaxies in common at 350 m and 76 galaxies in common at 550 m. The Planck FWHM are at 350 m and at 550 m. The photometry on the Planck compact sources was carried out using the FWHM of the band as the radius of the aperture. After visually inspecting each HRS galaxy with a corresponding Planck source, we excluded 11 sources because the Planck measurements may have potentially included other bright sources that lie within  5′of the galaxies.

The comparison between the data taken from the Planck catalogues and those presented here in Table 9 is shown in Figure 8. Mean Herschel to Planck flux density ratios are 0.91 and 1.13 at 350 and 500 m, respectively. At 500 m, Herschel flux densities are on average higher than those of Planck at 550 m. The discrepancy at 500 m is in part due to the difference of wavelength. If we assume a modified black body with a of 1.5, 20K, and assuming the relative colour corrections (1.02 for the SPIRE data, 0.91 for the Planck one, as indicated by the ERCSC Explanatory Supplement), we expect a flux density ratio of . Once correcting the Planck data for this difference, the same ratio drops to 0.98 at 500 m and 0.96 at 350 m. Colour corrections thus explain the mean differences between the two independent sets of data. They do not however explain other systematic differences such as those related to aperture effects. The major differences between the Planck measurements and ours are due to the different aperture sizes. Higher ratios correspond to galaxies that have a size larger than the Planck 350 m FWHM. Lower ratios can be explained by the contribution of background sources, visible on Herschel images, present in the Planck beam (Figure 9). At low flux densities, Planck data are systematically higher than those of Herschel, probably due to the important contamination of background sources (Figure 8). Davies et al. (2012) also compared their results with those of the Planck Collaboration at 350 m. The result of their linear fit is given in Figure 8, upper left panel (flux densities are not color corrected).

To understand this strong systematic difference between Planck measurements and ours, we carried out the photometric method used for the Planck catalogue on HRS images of the galaxies in common but using the aperture and sky annulus defined by the Planck consortium. A circular aperture with a radius of 4.23′(4.47′) at 350 m (500 m) is used, and the background region is defined as a circular annulus with an inner radius of 4.23′(4.47′) at 350 m (500 m) and outer radius of 24.23′(24.47′) at 350 m (500 m). This is a rough approximation, and a more precise work would require a convolution of the Herschel images to the resolution of Planck which is beyond the purpose of the present paper. We rejected flux densities of galaxies with sizes bigger than the Planck beam, or faint galaxies contaminated by strong background sources within the Planck beam. Figure 8 (lower panels) shows the Planck photometry versus HRS photometry measured in Planck apertures only for galaxies with good flux density measurements, the associated flux densities are in Table LABEL:4galpl. The results of the linear least squares fits show the consistency of the two sets of measurements. The HRS photometry in the beam of Planck is in good agreement with the flux densities of the Planck catalogue. Furthermore, the calibration error of Planck at 350 and 550 m Planck is 7% (Planck HFI Core Team et al. 2011), associated with the calibration error of Herschel, we obtain 10%. We can conclude that, despite differences due to the choice of the aperture, our measurements are consistent with the Planck data. However, because of the various photometry issues but particularly the source blending issues, Herschel measurements should be used instead of Planck measurements for these galaxies whenever possible.

Figure 8: Upper panels: the HRS versus Planck flux densities of 144 bright galaxies at 350 m and 76 bright galaxies at 500 m. The black lines are the one to one relationship in log scale. The red lines are the results of the linear fit; the orange line, on the 350 m plot, is the result of Davies et al. (2012) linear least squares fit. Middle panels: the HRS/Planck flux density ratio versus the HRS flux densities at 350 m and 500 m. The black line corresponds to the mean ratio, the dashed lines correspond to the standard deviation of the ratios. Lower panels: Planck flux densities versus HRS flux densities measured in the aperture used by the Planck Consortium at 350 m and 500 m.
Figure 9: Comparison between Planck and Herschel aperture photometry on 350 m SPIRE images, with in white, the apertures used for Herschel photometry and in dashed white for the background estimation, in magenta the aperture used by the Planck consortium on Planck images.
HRS Planck HRS in Planck beam
mJy mJy mJy
HRS 64
HRS 213
HRS 263
HRS 276
Table 7: Flux densities from different sources for the 4 galaxies shown in Figure 9, at 350 m.

7 Data access

The table is available on the SAG2 Herschel Database in Marseille (HeDaM; Roehlly et al. in preparation) at http://hedam.oamp.fr/HRS/. An electronic version of the catalogue and a README file can be downloaded there. The README describes how the photometry is performed for both extended and point-like sources. Through this database, we plan in the next future to give access to the community to all Herschel and ancillary data of the HRS galaxies.

8 Conclusion

We present the flux densities of the 323 galaxies of the Herschel Reference Survey in the three SPIRE bands. For extended galaxies, aperture photometry on elliptical regions is performed using the ”Funcnts” DS9/Funtools task. The background contribution is estimated calculating the mean value of the pixels within a concentric circular annulus. A different technique is used for point-like sources, where a PSF fitting is directly performed on timeline data. We compare our results with those of Davies et al. (2012), KINGFISH (Dale et al. 2012) and the Planck Early Science Compact Source Catalog (Planck Collaboration et al. 2011). Our measurements and those of Davies et al. (2012) and Dale et al. (2012) are consistent. Despite the different size of PSF between SPIRE and Planck, our flux densities and those of the Planck Consortium are in a good agreement. The catalogue is publicly available on the HeDaM database.

Acknowledgements.
We thank the referee for precious comments and suggestions which helped improving the quality of the manuscript. LC thanks Daniel Dale for enlightening discussions about the photometry of extended galaxies. LC although thanks Samuel Boissier and Sébastien Heinis for useful discussions. AB thanks the ESO visiting program committee for inviting him at the Garching headquarters for a two months staying. SB, SdiSA and CP acknowledge financial support by ASI through the ASI-INAF grants I/016/07/0 and I/009/10/0. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHS C, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). This research has made use of the NASA/IPAC ExtraGalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The research leading to these results has received funding from the European CommunityÕs Seventh Framework Programme (/FP7/2007-2013/) under grant agreement No 229517. This research has made use of the NASA/IPAC ExtraGalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration and of the GOLDMine database (http://goldmine.mib.infn.it/). The Dark Cosmology Centre is funded by the Danish National Research Foundation.

References

  • Abazajian et al. (2009) Abazajian, K. N., Adelman-McCarthy, J. K., Agüeros, M. A., et al. 2009, ApJS, 182, 543
  • Baes et al. (2010) Baes, M., Clemens, M., Xilouris, E. M., et al. 2010, A&A, 518, L53
  • Becker et al. (1995) Becker, R. H., White, R. L., & Helfand, D. J. 1995, ApJ, 450, 559
  • Bendo et al. (2012a) Bendo, G. J., Boselli, A., Dariush, A., et al. 2012a, MNRAS, 419, 1833
  • Bendo et al. (2012b) Bendo, G. J., Galliano, F., & Madden, S. C. 2012b, ArXiv e-prints, 1202.4629
  • Bendo et al. (2010) Bendo, G. J., Wilson, C. D., Warren, B. E., et al. 2010, MNRAS, 402, 1409
  • Bianchi et al. (2000) Bianchi, S., Alton, P. B., & Davies, J. I. 2000, in ESA Special Publication, Vol. 455, ISO Beyond Point Sources: Studies of Extended Infrared Emission, ed. R. J. Laureijs, K. Leech, & M. F. Kessler, 149
  • Bianchi & Schneider (2007) Bianchi, S. & Schneider, R. 2007, MNRAS, 378, 973
  • Binggeli et al. (1985) Binggeli, B., Sandage, A., & Tammann, G. A. 1985, AJ, 90, 1681
  • Boquien et al. (2012) Boquien, M., Buat, V., Boselli, A., et al. 2012, ArXiv e-prints, 1201.2405
  • Boquien et al. (2011) Boquien, M., Calzetti, D., Combes, F., et al. 2011, AJ, 142, 111
  • Boselli et al. (2009) Boselli, A., Boissier, S., Cortese, L., et al. 2009, ApJ, 706, 1527
  • Boselli et al. (2011) Boselli, A., Boissier, S., Heinis, S., et al. 2011, A&A, 528, A107
  • Boselli et al. (2010a) Boselli, A., Ciesla, L., Buat, V., et al. 2010a, A&A, 518, L61
  • Boselli et al. (2012) Boselli, A., Ciesla, L., Cortese, L., et al. 2012, ArXiv e-prints, 1201.2305
  • Boselli et al. (2010b) Boselli, A., Eales, S., Cortese, L., et al. 2010b, PASP, 122, 261
  • Boselli et al. (2003) Boselli, A., Sauvage, M., Lequeux, J., Donati, A., & Gavazzi, G. 2003, A&A, 406, 867
  • Clayton et al. (1997) Clayton, D. D., Arnett, D., Kane, J., & Meyer, B. S. 1997, ApJ, 486, 824
  • Condon et al. (1998) Condon, J. J., Cotton, W. D., Greisen, E. W., et al. 1998, AJ, 115, 1693
  • Cortese et al. (2012) Cortese, L., Ciesla, L., Boselli, A., et al. 2012, ArXiv e-prints, 1201.2762
  • Cortese et al. (2010) Cortese, L., Davies, J. I., Pohlen, M., et al. 2010, A&A, 518, L49
  • Dale et al. (2012) Dale, D. A., Aniano, G., Engelbracht, C. W., et al. 2012, ApJ, 745, 95
  • Davies et al. (2012) Davies, J. I., Bianchi, S., Cortese, L., et al. 2012, MNRAS, 419, 3505
  • Devereux & Young (1990) Devereux, N. A. & Young, J. S. 1990, in NASA Conference Publication, Vol. 3084, NASA Conference Publication, ed. D. J. Hollenbach & H. A. Thronson Jr., 92
  • Dowell et al. (2010) Dowell, C. D., Pohlen, M., Pearson, C., et al. 2010, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 7731, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series
  • Dreyer (1888) Dreyer, J. L. E. 1888, MNRAS, 49, 1
  • Dreyer (1895) Dreyer, J. L. E. 1895, MNRAS, 51, 185
  • Dwek (1998) Dwek, E. 1998, ApJ, 501, 643
  • Ferrarese et al. (2006) Ferrarese, L., Côté, P., Jordán, A., et al. 2006, ApJS, 164, 334
  • Galametz et al. (2011) Galametz, M., Madden, S. C., Galliano, F., et al. 2011, A&A, 532, A56
  • Galliano et al. (2008) Galliano, F., Dwek, E., & Chanial, P. 2008, ApJ, 672, 214
  • Gavazzi et al. (2003) Gavazzi, G., Boselli, A., Donati, A., Franzetti, P., & Scodeggio, M. 2003, A&A, 400, 451
  • Gavazzi et al. (1996) Gavazzi, G., Pierini, D., & Boselli, A. 1996, A&A, 312, 397
  • Gehrz (1989) Gehrz, R. 1989, in IAU Symposium, Vol. 135, Interstellar Dust, ed. L. J. Allamandola & A. G. G. M. Tielens, 445
  • Gomez et al. (2010a) Gomez, H. L., Baes, M., Cortese, L., et al. 2010a, A&A, 518, L45
  • Gomez et al. (2012) Gomez, H. L., Clark, C. J. R., Nozawa, T., et al. 2012, MNRAS, 2206
  • Gomez et al. (2010b) Gomez, H. L., Vlahakis, C., Stretch, C. M., et al. 2010b, MNRAS, 401, L48
  • Gordon et al. (2010) Gordon, K. D., Galliano, F., Hony, S., et al. 2010, A&A, 518, L89
  • Griffin et al. (2009) Griffin, M., Ade, P., André, P., et al. 2009, in EAS Publications Series, Vol. 34, EAS Publications Series, ed. L. Pagani & M. Gerin, 33–42
  • Griffin et al. (2010) Griffin, M. J., Abergel, A., Abreu, A., et al. 2010, A&A, 518, L3
  • Haynes et al. (1984) Haynes, M. P., Magri, C. A., & Giovanelli, R. 1984, in Bulletin of the American Astronomical Society, Vol. 16, Bulletin of the American Astronomical Society, 882
  • Höfner (2009) Höfner, S. 2009, in Astronomical Society of the Pacific Conference Series, Vol. 414, Cosmic Dust - Near and Far, ed. T. Henning, E. Grün, & J. Steinacker, 3
  • Holland et al. (1999) Holland, W. S., Robson, E. I., Gear, W. K., et al. 1999, MNRAS, 303, 659
  • Jarrett et al. (2003) Jarrett, T. H., Chester, T., Cutri, R., Schneider, S. E., & Huchra, J. P. 2003, AJ, 125, 525
  • Kennicutt et al. (2011) Kennicutt, R. C., Calzetti, D., Aniano, G., et al. 2011, PASP, 123, 1347
  • Matsuura et al. (2011) Matsuura, M., Dwek, E., Meixner, M., et al. 2011, Science, 333, 1258
  • Moshir & et al. (1990) Moshir, M. & et al. 1990, in IRAS Faint Source Catalogue, version 2.0 (1990)
  • Murakami et al. (2007) Murakami, H., Baba, H., Barthel, P., et al. 2007, PASJ, 59, 369
  • Nguyen et al. (2010) Nguyen, H. T., Schulz, B., Levenson, L., et al. 2010, A&A, 518, L5
  • Nilson (1973) Nilson, P. 1973, Uppsala general catalogue of galaxies, ed. Nilson, P.
  • Ott (2011) Ott, S. 2011, in Astronomical Society of the Pacific Conference Series, Vol. 442, Astronomical Data Analysis Software and Systems XX, ed. I. N. Evans, A. Accomazzi, D. J. Mink, & A. H. Rots, 347
  • Planck Collaboration et al. (2011) Planck Collaboration, Ade, P. A. R., Aghanim, N., et al. 2011, A&A, 536, A7
  • Planck HFI Core Team et al. (2011) Planck HFI Core Team, Ade, P. A. R., Aghanim, N., et al. 2011, A&A, 536, A6
  • Sanders et al. (2003) Sanders, D. B., Mazzarella, J. M., Kim, D.-C., Surace, J. A., & Soifer, B. T. 2003, AJ, 126, 1607
  • Sauvage & Thuan (1994) Sauvage, M. & Thuan, T. X. 1994, ApJ, 429, 153
  • Schlegel et al. (1998) Schlegel, D. J., Finkbeiner, D. P., & Davis, M. 1998, ApJ, 500, 525
  • Smith et al. (2012) Smith, M. W. L., Gomez, H. L., Eales, S. A., et al. 2012, ArXiv e-prints, 1112.1408
  • Soifer et al. (1989) Soifer, B. T., Boehmer, L., Neugebauer, G., & Sanders, D. B. 1989, AJ, 98, 766
  • Swinyard et al. (2010) Swinyard, B. M., Ade, P., Baluteau, J.-P., et al. 2010, A&A, 518, L4
  • Thuan & Sauvage (1992) Thuan, T. X. & Sauvage, M. 1992, A&AS, 92, 749
  • Wolfire et al. (1995) Wolfire, M. G., Hollenbach, D., McKee, C. F., Tielens, A. G. G. M., & Bakes, E. L. O. 1995, ApJ, 443, 152
  • Young et al. (1996) Young, J. S., Allen, L., Kenney, J. D. P., Lesser, A., & Rownd, B. 1996, AJ, 112, 1903
  • Zwicky et al. (1968) Zwicky, F., Herzog, E., & Wild, P. 1968, Catalogue of galaxies and of clusters of galaxies, ed. Zwicky, F., Herzog, E., & Wild, P.

Appendix A Tables

HRS CGCG VCC UGC NGC IC RA Dec
(arcsec) (arcsec) (degree) (arcsec) (arcsec)
1 123035 - - - - 154.415 22.8100 47 40 170 46 106
2 124004 - 5588 - - 155.238 25.3650 46 45 40 62 103
3 94026 - 5617 3226 - 155.863 19.8980 39 38 15 300 354
4 94028 - 5620 3227 - 155.877 19.8650 117 97 155 249 309
5 94052 - - - 610 156.618 20.2280 80 47 28 86 146
6 154016 - 5662 3245 - 156.755 28.6390 125 45 150 153 213
7 154017 - 5663 3245 - 156.827 28.5070 20 20 - 150 210
8 154020 - 5685 3254 - 157.333 29.4910 210 66 46 232 292
9 154026 - 5731 3277 - 158.231 28.5120 81 73 25 90 150
10 183028 - 5738 - - 158.624 35.2570 55 43 30 74 148
11 124038 - 5742 3287 - 158.697 21.6480 87 41 20 97 157
12 124041 - - - - 158.925 26.1260 28 22 20 31 91
13 183030 - 5753 3294 - 159.068 37.3250 149 76 115 165 225
14 124045 - 5767 3301 - 159.234 21.8820 42 42 55 165 225
15 65087 - 5826 3338 - 160.531 13.7470 247 152 100 273 333
16 94116 - 5842 3346 - 160.912 14.8720 112 98 108 125 185
17 95019 - 5887 3370 - 161.767 17.2740 132 74 150 146 206
18 155015 - 5906 3380 - 162.051 28.6020 71 56 20 79 139
19 184016 - 5909 3381 - 162.103 34.7110 85 78 55 94 154
20 184018 - 5931 3395 2613 162.459 32.9830 83 62 50 125 192
21 155028 - 5958 - - 162.816 27.8490 78 45 180 86 127
22 155029 - 5959 3414 - 162.818 27.9750 81 71 10 165 225
23 184028 - 5972 3424 - 162.943 32.9010 108 59 110 131 191
24 184029 - 5982 3430 - 163.048 32.9500 167 94 35 185 245
25 125013 - 5995 3437 - 163.149 22.9340 101 67 117 116 176
26 184031 - 5990 - - 163.160 34.4830 58 34 15 62 122
27 184034 - 6001 3442 - 163.284 33.9100 55 47 178 79 143
28 155035 - 6023 3451 - 163.587 27.2400 79 48 50 79 139
29 95060 - 6026 3454 - 163.623 17.3440 90 51 115 91 144
30 95062 - 6028 3455 - 163.630 17.2850 99 61 70 110 170
31 267027 - 6024 3448 - 163.663 54.3050 236 74 65 261 321
32 95065 - 6030 3457 - 163.703 17.6210 38 38 - 167 217
33 95085 - 6077 3485 - 165.010 14.8420 88 76 60 97 157
34 95097 - 6116 3501 - 165.697 17.9890 166 52 30 180 240
35 267037 - 6115 3499 - 165.796 56.2220 34 30 20 37 97
36 155049 - 6118 3504 - 165.797 27.9730 112 87 150 125 185
37 155051 - 6128 3512 - 166.012 28.0370 68 63 138 75 135
38 38129 - 6167 3526 - 166.736 7.1740 82 44 55 88 148
39 66115 - 6169 - - 166.764 12.0600 80 39 180 86 146
40 67019 - 6209 3547 - 167.483 10.7210 80 39 7 107 148
41 96011 - 6267 3592 - 168.613 17.2600 73 41 117 82 142
42 96013 - 6277 3596 - 168.776 14.7870 170 162 180 188 248
43 96022 - 6299 3608 - 169.246 18.1490 28 28 - 146 206
44 96026 - 6320 - - 169.572 18.8470 54 51 107 65 117
45 291054 - 6330 3619 - 169.840 57.7580 78 75 115 125 185
46 96029 - 6343 3626 - 170.016 18.3570 58 54 160 125 185
47 156064 - 6352 3629 - 170.133 26.9630 96 68 65 106 166
48 268021 - 6360 3631 - 170.262 53.1700 210 200 118 232 292
49 39130 - 6368 3640 - 170.279 3.2350 35 35 - 185 245
50 96037 - 6396 3655 - 170.728 16.5900 76 52 30 92 149
51 96038 - 6405 3659 - 170.939 17.8190 86 61 55 97 157
52 268030 - 6406 3657 - 170.982 52.9210 60 54 160 67 127
53 67071 - 6420 3666 - 171.109 11.3420 183 50 95 203 263
54 96045 - 6445 3681 - 171.624 16.8630 94 75 165 104 164
55 96047 - 6453 3684 - 171.797 17.0300 121 84 125 134 194
56 291072 - 6458 3683 - 171.883 56.8770 82 64 128 86 146
57 96049 - 6460 3686 - 171.933 17.2240 133 104 25 148 208
58 96050 - 6464 3691 - 172.039 16.9210 52 41 30 78 140
59 67084 - 6474 3692 - 172.100 9.4080 132 48 95 135 186
60 268051 - 6547 3729 - 173.456 53.1260 118 80 15 131 191
61 292009 - 6575 - - 174.110 58.1910 82 24 171 186 245
62 186012 - 6577 3755 - 174.139 36.4100 132 57 115 146 206
63 268063 - 6579 3756 - 174.200 54.2940 175 87 179 193 253
64 292017 - 6629 3795 - 175.029 58.6130 92 48 53 99 142
65 292019 - 6640 3794 - 175.223 56.2020 94 60 120 104 164
66 186024 - 6651 3813 - 175.328 36.5470 94 46 85 104 164
67 268076 - 6706 3846 - 176.062 55.0350 83 55 60 107 158
68 186045 - - - - 176.608 34.8530 20 20 - 75 113
69 268088 - 6787 3898 - 177.314 56.0840 183 107 108 203 263
70 - - - - 2969 178.130 -3.8720 61 51 105 229 278
71 292042 - 6860 3945 - 178.307 60.6760 220 145 165 244 304
72 - - - 3952 2972 178.419 -3.9970 81 48 79 85 142
73 269013 - 6870 3953 - 178.454 52.3270 243 129 13 321 381
74 269019 - 6918 3982 - 179.117 55.1250 98 85 38 108 168
75 269020 - 6919 - - 179.156 55.6330 51 40 90 70 131
76 269022 - 6923 - - 179.206 53.1600 84 34 170 93 153
77 13033 - 6993 4030 - 180.098 -1.1000 175 126 31 193 253
78 98019 - 6995 4032 - 180.137 20.0740 78 76 176 175 252
79 69024 - 7001 4019 755 180.293 14.1040 107 52 145 147 195
80 69027 - 7002 4037 - 180.349 13.4010 105 85 15 203 267
81 13046 - 7021 4045 - 180.676 1.9770 126 93 5 139 199
82 98037 - - - - 180.900 16.0560 57 54 105 63 109
83 41031 - 7035 - - 180.917 2.6410 47 45 150 51 111
84 69036 - 7048 4067 - 181.048 10.8540 50 37 45 55 115
85 243044 - 7095 4100 - 181.536 49.5820 225 74 163 249 309
86 41041 - 7111 4116 - 181.903 2.6920 159 100 163 176 236
87 69058 - 7117 4119 - 182.040 10.3790 68 50 150 190 250
88 41042 - 7116 4123 - 182.046 2.8780 210 162 105 232 292
89 69088 66 7215 4178 - 183.193 10.8660 224 78 30 248 308
90 13104 - 7214 4179 - 183.217 1.3000 91 91 - 176 236
91 98108 92 7231 4192 - 183.451 14.9000 410 109 155 454 514
92 69101 131 7255 - 3061 183.768 14.0290 101 51 120 120 180
93 187029 - 7256 4203 - 183.771 33.1970 103 84 180 157 217
94 69104 145 7260 4206 - 183.820 13.0240 205 51 180 237 297
95 69107 152 7268 4207 - 183.877 9.5850 82 37 120 91 151
96 69110 157 7275 4212 - 183.914 13.9020 151 84 75 167 227
97 69112 167 7284 4216 - 183.977 13.1490 383 90 19 424 484
98 69119 187 7291 4222 - 184.094 13.3070 144 47 55 163 223
99 69123 213 7305 - 3094 184.233 13.6250 39 29 92 61 111
100 98130 226 7315 4237 - 184.298 15.3240 84 48 105 93 153
101 158060 - 7338 4251 - 184.535 28.1750 87 87 - 168 228
102 98144 307 7345 4254 - 184.707 14.4160 258 235 60 285 345
103 42015 341 7361 4260 - 184.843 6.0990 68 35 45 83 128
104 99015 - 7366 - - 184.869 17.2300 50 50 - 55 115
105 99014 355 7365 4262 - 184.877 14.8780 44 44 - 52 146
106 42032 393 7385 4276 - 185.031 7.6920 88 88 - 97 157
107 42033 404 7387 - - 185.072 4.2010 81 39 15 86 136
108 42037 434 - 4287 - 185.202 5.6400 76 34 70 77 131
109 42038 449 7403 4289 - 185.259 3.7220 180 37 1 201 261
110 70024 465 7407 4294 - 185.324 11.5110 165 52 160 183 243
111 99024 483 7412 4298 - 185.387 14.6060 101 75 140 287 402
112 42044 492 7413 4300 - 185.423 5.3850 90 29 40 147 189
113 99027 497 7418 4302 - 185.427 14.5980 270 59 177 313 373
114 42045 508 7420 4303 - 185.479 4.4740 276 224 162 306 366
115 42047 517 7422 - - 185.505 5.1000 57 36 170 65 125
116 70031 522 7432 4305 - 185.515 12.7410 109 109 - 120 180
117 70029 524 7431 4307 - 185.523 9.0440 160 46 25 159 219
118 42053 552 7439 - - 185.613 4.5660 79 60 170 80 98
119 99029 559 7442 4312 - 185.631 15.5380 214 52 170 237 297
120 70034 570 7445 4313 - 185.661 11.8010 214 48 143 237 297
121 70035 576 7447 4316 - 185.676 9.3320 107 46 110 107 160
122 99030 596 7450 4321 - 185.729 15.8220 383 340 30 424 484
123 42063 613 7451 4324 - 185.776 5.2500 147 42 53 149 223
124 70039 630 7456 4330 - 185.822 11.3680 246 60 64 345 422
125 42068 648 7461 4339 - 185.896 6.0820 22 22 - 107 167
126 99036 654 7467 4340 - 185.897 16.7220 86 86 - 167 227
127 42070 656 7465 4343 - 185.911 6.9540 108 43 130 109 160
128 42072 667 7469 - 3259 185.952 7.1870 79 39 15 87 147
129 99038 685 7473 4350 - 185.991 16.6930 20 20 - 148 208
130 70045 692 7476 4351 - 186.007 12.2050 83 62 70 100 178
131 42079 697 7474 - 3267 186.023 7.0410 65 65 - 72 132
132 42080 699 7477 - 3268 186.031 6.6070 81 57 22 90 150
133 158099 - 7483 4359 - 186.046 31.5220 149 48 105 219 295
134 70048 713 7482 4356 - 186.061 8.5360 135 36 40 148 208
135 42083 731 7488 4365 - 186.118 7.3170 78 78 - 405 465
136 42089 758 7492 4370 - 186.229 7.4450 73 36 80 81 141
137 70057 759 7493 4371 - 186.231 11.7040 122 122 - 237 297
138 70058 763 7494 4374 - 186.266 12.8870 20 20 - 139 265
139 42093 787 7498 4376 - 186.325 5.7410 77 44 135 85 145
140 42092 785 7497 4378 - 186.325 4.9250 128 104 160 142 202
141 70061 792 7503 4380 - 186.342 10.0170 147 73 155 163 223
142 99044 801 7507 4383 - 186.356 16.4700 109 54 20 120 180
143 42095 827 7513 - - 186.428 7.2170 156 43 155 167 227
144 70068 836 7520 4388 - 186.445 12.6620 214 52 90 237 297
145 70067 849 7519 4390 - 186.461 10.4590 91 76 125 101 161
146 42098 851 7518 - 3322 186.475 7.5550 91 38 160 100 160
147 42099 859 7522 - - 186.493 3.4300 121 40 130 135 195
148 99049 865 7526 4396 - 186.495 15.6720 141 57 125 156 216
149 70071 873 7528 4402 - 186.531 13.1130 165 48 90 183 243
150 70072 881 7532 4406 - 186.549 12.9460 129 113 130 430 495
151 70076 912 7538 4413 - 186.634 12.6110 122 73 15 135 195
152 42104 921 7536 4412 - 186.650 3.9650 79 65 76 87 147
153 42105 938 7541 4416 - 186.695 7.9190 91 85 145 111 157
154 70082 939 7546 - - 186.697 8.8850 103 98 165 152 213
155 70080 944 7542 4417 - 186.711 9.5840 86 86 - 167 227
156 99054 958 7551 4419 - 186.735 15.0470 147 58 133 163 223
157 42106 957 7549 4420 - 186.744 2.4940 86 50 8 93 153
158 42107 971 7556 4423 - 186.787 5.8800 128 50 20 142 202
159 70090 979 7561 4424 - 186.798 9.4210 85 80 100 201 261
160 42111 1002 7566 4430 - 186.860 6.2630 93 89 120 225 316
161 70093 1003 7568 4429 - 186.861 11.1070 20 20 - 377 437
162 70098 1030 7575 4435 - 186.919 13.0790 83 77 10 96 148
163 70097 1043 7574 4438 - 186.940 13.0090 134 118 27 327 404
164 70099 1047 7581 4440 - 186.973 12.2930 84 84 - 93 153
165 42117 1048 7579 - - 186.981 5.7210 77 35 130 87 147
166 70100 1062 7583 4442 - 187.016 9.8040 121 121 - 234 294
167 70104 1086 7587 4445 - 187.066 9.4360 93 33 105 103 208
168 70108 1091 7590 - - 187.078 8.7290 57 37 175 127 174
169 99063 - 7595 - 3391 187.114 18.4150 63 50 95 66 125
170 99062 1110 7594 4450 - 187.124 17.0850 258 169 171 285 345
171 70111 1118 7600 4451 - 187.169 9.2590 82 40 170 91 151
172 99065 1126 7602 - 3392 187.180 14.9990 122 48 40 135 195
173 42124 1145 7609 4457 - 187.246 3.5710 95 94 165 135 195
174 70116 1154 7614 4459 - 187.250 13.9790 20 20 - 156 216
175 70115 1158 7613 4461 - 187.262 13.1840 84 84 - 163 223
176 70121 1190 7622 4469 - 187.367 8.7500 84 48 85 201 261
177 42132 1205 7627 4470 - 187.407 7.8240 77 48 180 85 145
178 42134 1226 7629 4472 - 187.445 8.0010 92 92 - 476 536
179 70125 1231 7631 4473 - 187.454 13.4290 36 36 - 187 247
180 70129 1253 7638 4477 - 187.509 13.6360 55 44 35 95 148
181 70133 1279 7645 4478 - 187.573 12.3290 22 22 - 87 147
182 42139 1290 7647 4480 - 187.612 4.2470 83 60 170 93 153
183 70139 1316 7654 4486 - 187.706 12.3910 58 57 159 374 470
184 70140 1326 7657 4491 - 187.738 11.4840 79 39 148 87 147
185 42141 1330 7656 4492 - 187.749 8.0780 82 82 - 91 151
186 129005 - 7662 4494 - 187.850 25.7750 26 25 180 222 282
187 42144 1375 7668 4505 - 187.913 3.9390 199 158 70 221 281
188 99075 1379 7669 4498 - 187.915 16.8530 119 64 125 132 192
189 99077 1393 7676 - 797 187.978 15.1240 70 46 108 78 138
190 99076 1401 7675 4501 - 187.997 14.4200 303 162 140 336 396
191 99078 1410 7677 4502 - 188.014 16.6880 62 32 40 94 177
192 70152 1419 7682 4506 - 188.044 13.4200 36 29 105 100 160
193 70157 1450 7695 - 3476 188.174 14.0500 94 72 30 120 180
194 14063 - 7694 4517 - 188.190 0.1150 462 86 80 511 571
195 99087 1479 7703 4516 - 188.281 14.5750 90 90 - 100 160
196 70167 1508 7709 4519 - 188.376 8.6550 151 109 152 167 227
197 70168 1516 7711 4522 - 188.415 9.1750 169 42 33 187 247
198 159016 - 7714 4525 - 188.463 30.2770 126 67 65 159 214
199 99090 1532 7716 - 800 188.486 15.3550 82 59 150 91 151
200 42155 1535 7718 4526 - 188.513 7.6990 71 68 163 325 385
201 42156 1540 7721 4527 - 188.535 2.6540 246 78 67 272 332
202 70173 1549 7728 - 3510 188.562 11.0720 22 22 - 51 111
203 42158 1554 7726 4532 - 188.581 6.4680 112 51 166 120 180
204 42159 1555 7727 4535 - 188.585 8.1980 270 232 180 308 397
205 14068 1562 7732 4536 - 188.613 2.1880 303 137 140 336 396
206 42162 1575 7736 - 3521 188.664 7.1600 84 59 18 167 234
207 99093 1588 7742 4540 - 188.712 15.5510 79 66 145 132 202
208 99096 1615 7753 4548 - 188.860 14.4960 252 209 150 279 339
209 - - - 4546 - 188.873 -3.7930 104 75 80 135 188
210 70182 1619 7757 4550 - 188.878 12.2210 20 20 - 108 159
211 70184 1632 7760 4552 - 188.916 12.5560 65 65 - 336 396
212 99098 - 7768 4561 - 189.034 19.3230 77 62 110 87 147
213 129010 - 7772 4565 - 189.087 25.9880 595 80 135 659 719
214 70186 1664 7773 4564 - 189.113 11.4390 38 38 - 201 261
215 70189 1673 7777 4567 - 189.136 11.2580 86 41 75 204 265
216 70188 1676 7776 4568 - 189.143 11.2390 93 53 33 206 266
217 70192 1690 7786 4569 - 189.208 13.1630 258 157 23 498 558
218 42178 1692 7785 4570 - 189.223 7.2470 84 84 - 163 223
219 70195 1720 7793 4578 - 189.377 9.5550 90 90 - 175 235
220 70197 1727 7796 4579 - 189.431 11.8180 264 204 100 292 352
221 42183 1730 7794 4580 - 189.452 5.3680 83 73 160 100 160
222 70199 1757 7803 4584 - 189.574 13.1100 82 44 20 91 151
223 42186 1758 7802 - - 189.587 7.8910 76 40 55 87 147
224 42187 1760 7804 4586 - 189.618 4.3190 181 48 115 201 261
225 70202 1778 7817 - 3611 189.767 13.3640 33 30 115 81 141
226 42191 1780 7821 4591 - 189.802 6.0120 82 37 40 91 151
227 14091 - 7819 4592 - 189.828 -0.5320 241 63 95 267 327
228 - - - - - 189.843 -5.6650 22 22 - 39 79
229 70204 1809 7825 - 3631 189.950 12.9740 46 46 - 51 111
230 99106 1811 7826 4595 - 189.966 15.2980 90 59 110 100 160
231 70206 1813 7828 4596 - 189.983 10.1760 20 20 - 221 281
232 70213 1859 7839 4606 - 190.240 11.9120 66 56 33 308 412
233 70216 1868 7843 4607 - 190.302 11.8870 163 56 4 280 376
234 70214 1869 7842 4608 - 190.305 10.1560 103 103 - 199 259
235 42205 1883 7850 4612 - 190.387 7.3150 51 51 - 100 160
236 70223 1903 7858 4621 - 190.510 11.6470 69 69 - 356 416
237 42208 1923 7871 4630 - 190.630 3.9600 97 67 10 102 147
238 14109 - 7869 4629 - 190.636 -1.3510 57 51 80 64 124
239 99112 1932 7875 4634 - 190.671 14.2960 119 51 156 309 390
240 70229 1938 7880 4638 - 190.698 11.4430 48 48 - 93 153
241 43002 1939 7878 4636 - 190.708 2.6880 36 35 90 447 507
242 70230 1943 7884 4639 - 190.718 13.2580 134 84 123 148 208
243 15008 - 7895 4643 - 190.834 1.9780 130 126 135 213 265
244 71015 1972 7896 4647 - 190.885 11.5830 109 90 105 120 180
245 71016 1978 7898 4649 - 190.917 11.5530 45 45 - 237 297
246 100004 - 7901 4651 - 190.928 16.3930 163 115 80 181 241
247 71019 1987 7902 4654 - 190.986 13.1270 209 109 128 232 292
248 71023 2000 7914 4660 - 191.133 11.1910 22 22 - 87 147
249 71026 2006 7920 - 3718 191.192 12.3510 38 30 72 120 180
250 43018 - 7924 4665 - 191.275 3.0560 108 108 - 209 269
251 15015 - 7926 4666 - 191.286 -0.4620 189 189 44 198 262
252 15016 - 7931 4668 - 191.384 -0.5350 99 51 5 120 186
253 15019 - 7951 4684 - 191.823 -2.7270 49 46 20 133 193
254 71043 2058 7965 4689 - 191.940 13.7630 246 186 164 272 332
255 43028 - 7961 4688 - 191.944 4.3360 150 137 35 204 264
256 15023 - - 4691 - 192.057 -3.3330 83 74 105 131 191
257 71045 2070 7970 4698 - 192.096 8.4870 238 119 165 263 323
258 - - - 4697 - 192.150 -5.8010 20 20 - 260 314
259 43034 - 7975 4701 - 192.298 3.3890 151 125 40 167 227
260 100011 - 7980 4710 - 192.412 15.1650 103 60 27 199 259
261 43040 - 7982 - - 192.459 2.8530 147 53 180 157 217
262 43041 - 7985 4713 - 192.491 5.3110 134 90 110 148 208
263 129027 - 7989 4725 - 192.611 25.5010 440 404 35 449 509
264 15027 - 7991 - - 192.662 1.4640 93 34 170 101 170
265 - - - 4720 - 192.678 -4.1560 57 44 115 92 143
266 - - - 4731 - 192.755 -6.3930 277 136 90 307 367
267 129028 - 8005 4747 - 192.941 25.7770 165 76 30 183 243
268 71060 - 8007 4746 - 192.981 12.0830 92 51 120 102 162
269 71062 2092 8010 4754 - 193.073 11.3140 120 120 - 233 293
270 15029 - 8009 4753 - 193.092 -1.2000 202 120 105 280 340
271 100015 - 8014 4758 - 193.184 15.8490 129 58 160 139 199
272 71065 2095 8016 4762 - 193.234 11.2310 208 208 - 404 464
273 15031 - 8020 4771 - 193.339 1.2690 171 65 135 186 246
274 15032 - 8021 4772 - 193.372 2.1680 117 44 145 188 254
275 - - - 4775 - 193.440 -6.6220 89 84 50 99 159
276 71068 - 8022 4779 - 193.462 9.7100 88 76 10 97 157
277 43060 - - 4791 - 193.683 8.0530 50 33 65 55 115
278 71071 - 8032 - - 193.684 13.2370 115 39 165 127 187
279 15037 - 8041 - - 193.803 0.1170 130 79 157 144 204
280 43066 - 8043 4799 - 193.815 2.8970 72 38 90 74 134
281 43068 - 8045 - - 193.848 7.9090 38 30 105 42 102
282 43069 - - 4803 - 193.890 8.2410 22 22 - 23 83
283 43071 - 8054 4808 - 193.954 4.3040 110 70 127 120 180
284 - - - - 3908 194.169 -7.5630 90 43 170 84 144
285 15049 - 8078 4845 - 194.505 1.5760 218 68 100 241 301
286 71092 - 8102 4866 - 194.863 14.1710 294 54 87 415 521
287 15055 - 8121 4904 - 195.245 -0.0270 115 103 145 120 185
288 - - - 4941 - 196.055 -5.5520 152 81 15 168 228
289 - - - 4981 - 197.203 -6.7770 115 85 149 127 187
290 189037 - 8271 5014 - 197.880 36.2820 64 52 102 79 139
291 217031 - 8388 5103 - 200.125 43.0840 60 60 - 67 127
292 218010 - 8439 5145 - 201.308 43.2670 84 74 85 93 153
293 16069 - 8443 5147 - 201.582 2.1010 92 77 125 103 169
294 246017 - 8593 - 902 204.005 49.9610 93 46 160 101 161
295 73054 - 8616 5248 - 204.384 8.8850 260 187 140 288 348
296 190041 - 8675 5273 - 205.535 35.6540 56 56 95 94 149
297 246023 - 8711 5301 - 206.602 46.1070 181 71 150 193 253
298 218047 - 8725 5303 - 206.937 38.3050 65 53 85 42 102
299 45108 - 8727 5300 - 207.067 3.9510 163 107 140 180 240
300 218058 - 8756 - - 207.650 42.5410 75 42 85 79 139
301 17088 - 8790 5334 4338 208.227 -1.1150 175 126 40 193 253
302 45137 - 8821 5348 - 208.547 5.2270 154 39 177 237 305
303 295024 - 8843 5372 - 208.692 58.6660 62 58 40 92 162
304 46001 - 8831 5356 - 208.744 5.3340 133 51 12 143 203
305 46003 - 8838 5360 958 208.911 4.9850 83 28 70 101 161
306 46007 - 8847 5363 - 209.030 5.2550 170 110 130 189 249
307 46009 - 8853 5364 - 209.050 5.0140 283 183 30 314 374
308 46011 - 8857 - - 209.111 4.3970 20 20 - 42 102
309 272031 - 9036 5486 - 211.854 55.1030 44 43 125 150 195
310 47010 - 9172 5560 - 215.023 3.9910 149 50 115 172 232
311 47012 - 9175 5566 - 215.083 3.9340 197 103 35 449 525
312 47020 - 9183 5576 - 215.265 3.2710 31 31 - 165 225
313 47022 - 9187 5577 - 215.305 3.4360 154 64 55 157 217
314 19012 - 9215 - - 215.863 1.7260 95 62 165 101 161
315 220015 - 9242 - - 216.338 39.5400 211 34 71 382 451
316 47063 - 9308 5638 - 217.418 3.2330 24 24 - 125 185
317 47066 - 9311 - 1022 217.508 3.7730 51 41 165 51 111
318 47070 - 9328 5645 - 217.664 7.2750 100 63 105 111 171
319 75064 - 9353 5669 - 218.183 9.8920 167 118 61 185 245
320 47090 - 9363 5668 - 218.351 4.4500 152 144 17 198 276
321 47123 - 9427 5692 - 219.576 3.4100 49 33 40 62 124
322 47127 - 9436 5701 - 219.796 5.3640 153 148 90 293 382
323 48004 - 9483 - 1048 220.741 4.8900 100 47 163 104 164
Table 8: continued.
HRS footnotemark: footnotemark: footnotemark:
(mJy) (mJy) (mJy) (mJy) (mJy) (mJy) (mJy) (mJy) (mJy) (mJy) (mJy) (mJy)
1 163 92 41
2 185 102 45
3 135 75 32
4 993 560 251
5 340 192 86
6 501 281 127
7 456 256 114
8 1216 685 301
9