The Herschel Reference Survey

By A. Boselli, S. Eales, L. Cortese, G. Bendo, P. Chanial, V. Buat, J. Davies, R. Auld, E. Rigby, M. Baes and 46 more. 2010

222 citations recorded by the source corpus.

The Herschel Reference Survey is a Herschel guaranteed time key project and will be a benchmark study of dust in the nearby universe. The survey will complement a number of other Herschel key projects including large cosmological surveys that trace dust in the distant universe. We will use Herschel to produce images of a statistically-complete sample of 323 galaxies at 250, 350, and 500 μm. The sample is volume-limited, containing sources with distances between 15 and 25 Mpc and flux limits in the K band to minimize the selection effects associated with dust and with young high-mass stars and to introduce a selection in stellar mass. The sample spans the whole range of morphological types (ellipticals to late-type spirals) and environments (from the field to the center of the Virgo Cluster) and as such will be useful for other purposes than our own. We plan to use the survey 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. In this article, we describe the goals of the survey, the details of the sample and some of the auxiliary observing programs that we have started to collect complementary data. We also use the available multifrequency data to carry out an analysis of the statistical properties of the sample.

Subfields: Astronomy and Astrophysics, Statistical and Nonlinear Physics, Statistics and Probability

View Paper: https://www.semanticscholar.org/paper/3a12dca0334026bdf9427e4466a4e738bf3c30b9

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Citations in the corpus

The dust scaling relations of the Herschel Reference Survey (2012, methodology): “Unfortunately, no homogeneous dataset for all the HRS galaxies is currently available forλ <200 µm (see Boselli et al. 2010b), making an accurate SED fitting of only the three SPIRE flux densities unfeasible in the case of d- tailed dust models and perhaps not ideal even in the case of a sin- gle…”
A z = 0 Multiwavelength Galaxy Synthesis. I. A WISE and GALEX Atlas of Local Galaxies (2019, unknown): “The Herschel Reference Survey (HRS, Boselli et al. 2010) built infrared maps of a volumelimited sample of ∼ 320 galaxies in the range d ≈ 15−25 Mpc.”
THE EMISSION BY DUST AND STARS OF NEARBY GALAXIES IN THE HERSCHEL KINGFISH SURVEY (2011, background): “‘Warmer’ far-IR colors are often associated with higher temperatures of small or large dust grain components, depending on the wavelengths (e.g., Li & Draine 2001; Boselli et al. 2010b).”
THE NEXT GENERATION VIRGO CLUSTER SURVEY (NGVS). I. INTRODUCTION TO THE SURVEY (2012, methodology): “Targeted observations include 250, 350, and 500 μm images for 82 Virgo galaxies obtained as part of the Herschel Reference Survey (HRS; Boselli et al. 2010) at an angular resolution of ∼30′′, and 6.75 μm (6′′ resolution) and 15.0 μm (8′′ resolution) images for 123 galaxies (mostly late-type…”
An ALMA survey of the SCUBA-2 CLS UDS field: physical properties of 707 sub-millimetre galaxies (2019, methodology): “This yields predicted SEDs of model galaxies covering the rest-frame UV-toradio wavelengths (e.g. Camps et al. 2018; McAlpine et al. 2019), and is calibrated against far-infrared observations from the Herschel Reference Survey (Boselli et al. 2010).”
Planck2015 results: XXVI. The SecondPlanckCatalogue of Compact Sources (2015, unknown): “If, however, the 17 sources in the HRS sample with flux densities greater than 10 Jy are excluded from the analysis, then the flux-density ratios for all flux-extraction methods are within 1σ of unity.”
THE HERSCHEL REFERENCE SURVEY: DUST IN EARLY-TYPE GALAXIES AND ACROSS THE HUBBLE SEQUENCE (2011, methodology): “We find that the temperatures of the early types are systematically higher (with U = 1638, n1 = 70, n2 = 30 and P > 99.99% 23), in agreement with the result that the ETGs in the HRS have warmer IR colors than late types (Boselli et al. 2010a; see also Bendo et al. 2003; Engelbracht et al. 2010).”
Cold gas properties of the Herschel Reference Survey - II. Molecular and total gas scaling relations (2014, methodology): “The calibration of the SSFR is significantly different from the one we used in our previous works (Boselli et al. 2010b; Boselli et al. 2012) based on Hα+[NII] and GALEX FUV imaging data, with the former corrected for dust extinction using the Balmer decrement and for [NII] contamination using the…”
HERSCHEL FAR-INFRARED AND SUBMILLIMETER PHOTOMETRY FOR THE KINGFISH SAMPLE OF NEARBY GALAXIES (2011, methodology): “SPIRE observations for six of our galaxies were obtained in the Herschel Reference Survey (Boselli et al. 2010): NGC 4254, NGC 4321, NGC 4536, NGC 4569, NGC 4579, and NGC 4725; those observations were not duplicated for KINGFISH.”
Gas-to-dust mass ratios in local galaxies over a 2 dex metallicity range (2013, background): “…the high-metallicity side, Smith et al. (2012) showed that the 30 elliptical galaxies detected with Herschel in the Herschel Reference Survey (HRS, Boselli et al. 2010) had a mean G/D of ∼120, which is slightly lower than what we find for our elliptical and spiral galaxies at moderate…”
The effect of the environment on the Hi scaling relations (2011, methodology): “As extensively discussed in Boselli et al. (2010), this sample is not only representative of the local universe but, spanning different density regimes 2 In this paper we will refer to the M(HI)/M∗ ratio as gas fraction.”
Planck2013 results. XXVIII. ThePlanckCatalogue of Compact Sources (2013, background): “Figure 14 shows the comparison between Planck flux densities at 545 and 857 GHz and four Herschel catalogues, HRS (Boselli et al. 2010), KINGFISH (Kennicutt et al. 2011), HeViCS (Davies et al. 2013), and H-ATLAS (Eales et al. 2010).”
xGASS: total cold gas scaling relations and molecular-to-atomic gas ratios of galaxies in the local Universe (2018, background): “…and extend to higher stellar mass the results of Boselli et al. (2014a), obtained for field late-type galaxies detected in both H I and CO lines in the Herschel Reference Survey (HRS; Boselli et al. 2010), assuming a luminosity-dependent XCO conversion factor to compute molecular gas masses.”
Hi-GAL, the Herschel infrared Galactic Plane Survey: Photometric maps and compact source catalogues: First data release for the inner Milky Way: +68° ≥ l ≥ -70° (2016, background): “Local universe galaxies have larger fluxes, but are also far from compact and have a very low spatial density (see Ciesla et al. (2012) and Boselli et al. 2010) Therefore, it is unlikely that they have been included in the present catalog.”
Dust spectral energy distributions of nearby galaxies: an insight from the Herschel Reference Survey (2014, methodology): “They are normalized to the observed 2MASS K-band flux densities as the galaxies of our sample were selected in this band (see Boselli et al. 2010b, for the description of the K band flux densities).”
The GALEX Arecibo SDSS Survey - VIII. Final data release. The effect of group environment on the gas content of massive galaxies (2013, methodology): “This approach was adopted by Cortese et al. (2011) to compare Virgo cluster and Hinormal galaxies, and was successful because the more nearby Herschel Reference Survey (HRS; Boselli et al. 2010) sample includes Hi detections and more stringent upper limits in the Hi-deficient regime.”
The role of cold gas and environment on the stellar mass-metallicity relation of nearby galaxies (2012, methodology): “In this study, we adopt a galaxy sample drawn from late-type galaxies in the Herschel Reference Survey (Boselli et al. 2010, A115, page 2 of 15 hereafter HRS).”