The Herschel Multi-tiered Extragalactic Survey: HerMES

By H. Oliver, J. Bock, B. Altieri, A. Amblard, V. Arumugam, H. Aussel, T. Babbedge, A. Beelen, M. B'ethermin, A. Blain and 221 more. 2012

638 citations recorded by the source corpus.

The Herschel Multi-tiered Extragalactic Survey (HerMES) is a legacy programme designed to map a set of nested fields totalling ∼380 deg^2. Fields range in size from 0.01 to ∼20 deg^2, using the Herschel-Spectral and Photometric Imaging Receiver (SPIRE) (at 250, 350 and 500 μm) and the Herschel-Photodetector Array Camera and Spectrometer (PACS) (at 100 and 160 μm), with an additional wider component of 270 deg^2 with SPIRE alone. These bands cover the peak of the redshifted thermal spectral energy distribution from interstellar dust and thus capture the reprocessed optical and ultraviolet radiation from star formation that has been absorbed by dust, and are critical for forming a complete multiwavelength understanding of galaxy formation and evolution. The survey will detect of the order of 100 000 galaxies at 5σ in some of the best-studied fields in the sky. Additionally, HerMES is closely coordinated with the PACS Evolutionary Probe survey. Making maximum use of the full spectrum of ancillary data, from radio to X-ray wavelengths, it is designed to facilitate redshift determination, rapidly identify unusual objects and understand the relationships between thermal emission from dust and other processes. Scientific questions HerMES will be used to answer include the total infrared emission of galaxies, the evolution of the luminosity function, the clustering properties of dusty galaxies and the properties of populations of galaxies which lie below the confusion limit through lensing and statistical techniques. This paper defines the survey observations and data products, outlines the primary scientific goals of the HerMES team, and reviews some of the early results.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/950d09d3de169a96c45e4002c8ab4f23864e24ad

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Citations in the corpus

Characterization of Scuba-2 450 μm and 850 μm selected galaxies in the COSMOS field (2013, background): “Herschel has mapped hundreds of square degrees at 250–500µm(Eales et al. 2010; Oliver et al. 2012).”
THE EVOLVING INTERSTELLAR MEDIUM OF STAR-FORMING GALAXIES SINCE z = 2 AS PROBED BY THEIR INFRARED SPECTRAL ENERGY DISTRIBUTIONS (2012, methodology): “The source was discovered in Science Demonstration Phase Herschel/SPIRE observations of the Lockman-SWIRE field as part of the Herschel Multi-tiered Extragalactic Survey (HerMES; S. Oliver et al. 2012).”
Panchromatic spectral energy distributions of Herschel sources (2013, methodology): “…carried out in the framework of the PACS Evolutionary Probe (PEP, Lutz et al. 2011) and theHerschel Multi-tiered Extragalactic Survey (HerMES, Oliver et al. 2012) in three of the most popular extragalactic “blank fields”: GOODS-N, GOODS-S, and COSMOS (Dickinson et al. 2001; Scoville et al.…”
The Herschel census of infrared SEDs through cosmic time (2013, background): “…carried out during the Science Demonstration Phase of the largest extragalactic surveys, the Herschel Multi-tiered Extragalactic Survey (HerMES; Oliver et al. 2012), the PACS Evolutionary Probe (PEP; Lutz et al. 2011) and the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS; Eales…”
The evolution of the dust and gas content in galaxies (2013, methodology): “…work we use the data collected by two extragalactic surveys, PACS Evolutionary Probe (PEP, Lutz et al. 2011) and Herschel Multi-tiered Extra-galactic Survey (HerMES, Oliver et al. 2012), to investigate the evolution of the dust and gas content in galaxies from the local Universe out to z ∼ 2.5.”
The VISTA deep extragalactic observations (VIDEO) survey (2012, methodology): “…by the need to cover the wealth of ancillary data available in these fields, including Spitzer (Lonsdale et al. 2004; Mauduit et al. 2012) and Herschel (Oliver et al. 2012), in addition to future ground-based optical data from both the Very Large Telescope (VLT) Survey Telescope (VST) and the DES.”
A CORRELATION BETWEEN STAR FORMATION RATE AND AVERAGE BLACK HOLE ACCRETION IN STAR-FORMING GALAXIES (2013, methodology): “The far-IR data in this work is based on the publicly availableH rschel SPIRE 250µm observations from theHerschel Multi-tiered Extragalactic Survey (HerMES, Oliver et al. 2012).”
Herschel PEP/HerMES: the redshift evolution (0 ≤ z ≤ 4) of dust attenuation and of the total (UV+IR) star formation rate density (2013, background): “1 From two Herschel Large Programmes: PACS Evolutionary Probe (Lutz et al.(2011)) and the Herschel Multi-tiered Extragalactic Survey (HerMES, Oliver et al.(2012))”
The evolution of the dust temperatures of galaxies in the SFR–M∗ plane up to z ~ 2 (2013, methodology): “PACS observations were taken as part of the PEP (Lutz et al. 2011) guaranteed time key programme, while the SPIRE observations were taken as part of the Herschel Multi-tiered Extragalactic Survey (HerMES; Oliver et al. 2012).”
HerMES: CANDIDATE GRAVITATIONALLY LENSED GALAXIES AND LENSING STATISTICS AT SUBMILLIMETER WAVELENGTHS (2012, methodology): “HerMES is described in Oliver et al. (2012).”
An ALMA survey of sub-millimetre Galaxies in the Extended Chandra Deep Field South: the far-infrared properties of SMGs (2013, methodology): “Herschel / SPIRE 250, 350 and 500µm observations covering ECDFS were taken as part of theHerschel Multi-tiered Extra-galactic Survey (HerMES) guaranteed time program (as described in Oliver et al. 2012).”
CANDELS MULTI-WAVELENGTH CATALOGS: SOURCE DETECTION AND PHOTOMETRY IN THE GOODS-SOUTH FIELD (2013, methodology): “…field also has very deep far-IR to submillimeter data from Herschel Space Observatory from the PEP survey (Lutz et al. 2011) and the HerMes survey (Oliver et al. 2012), deep submillimeter (1.1 mm) observation with AzTEC/ASTE (Scott et al. 2010), and radio imaging from the VLA (Kellermann et al.…”
The Atacama Cosmology Telescope: CMB polarization at 200 < ℓ < 9000 (2014, neutral): “Overlapping surveys include SDSS [77], BOSS [15], CFHTLS [21], XMMXXL [93], Herschel (HerMES & HeLMS, [65, 90]), HSC [83], DES [30], GAMA [32], and KiDS [29].”
The Herschel view of the dominant mode of galaxy growth from z = 4 to the present day (2014, methodology): “The PACS images are the result of the combined observation of both GOODS–Herschel and PACS evolutionary probe (PEP; Lutz et al. 2011), while SPIRE images were obtained as part of the HerMES program (Oliver et al. 2012).”
A deep ALMA image of the Hubble Ultra Deep Field (2016, methodology): “…PACS Evolutionary Probe (PEP; Lutz et al. 2011) surveys, while SPIRE (Griffin et al. 2010) images at 250µm, 350µm and 500µm, reaching 5.86, 6.34 and 6.88 mJy respectively (including confusion noise) are provided by the Herschel Multi-tiered Extragalactic Survey (HerMES; Oliver et al. 2010, 2012).”
THE COSMOS2015 CATALOG: EXPLORING THE 1 < z < 6 UNIVERSE WITH HALF A MILLION GALAXIES (2016, methodology): “Flux density measurements with a signal to noise smaller than 3 in the initial SPIRE COSMOS catalog published by Oliver et al. (2012) are not considered in our present work.”
COMBINED CO AND DUST SCALING RELATIONS OF DEPLETION TIME AND MOLECULAR GAS FRACTIONS WITH COSMIC TIME, SPECIFIC STAR-FORMATION RATE, AND STELLAR MASS (2014, positive): “2.2 Dust observations As part of the Herschel-PEP (Lutz et al. 2011) and Herschel-HERMES (Oliver et al. 2012) far-IR continuum surveys, Magnelli et al. (2014) have established 100 to 500µm far-IR SEDs from stacking PACS and SPIRE photometry in 8846, 4753 and 254 749 Kand I-selected SFGs in the…”
AN ALMA SURVEY OF SUB-MILLIMETER GALAXIES IN THE EXTENDED CHANDRA DEEP FIELD SOUTH: PHYSICAL PROPERTIES DERIVED FROM ULTRAVIOLET-TO-RADIO MODELING (2015, methodology): “Herschel/SPIRE imaging at 250, 350, and 500 μm is available from the Herschel Multitiered Extragalactic Survey (HerMES; Oliver et al. 2012).”
GRAVITATIONAL LENS MODELS BASED ON SUBMILLIMETER ARRAY IMAGING OF HERSCHEL-SELECTED STRONGLY LENSED SUB-MILLIMETER GALAXIES AT z > 1.5 (2013, methodology): “The total area considered for the candidate selection is ≈ 300 deg2 in H-ATLAS (comprising the full equatorial fields and ≈ 75% of the northern galactic pole field) and 94.8 deg2 in nine independent fields in HerMES (for details of the fields, see Oliver et al. 2012).”