The Herschel ATLAS

Eales, Stephen Anthony; Dunne, L.; Clements, D. L.; Cooray, A.; Zotti, G. de; Dye, S.; Ivison, R. J.; Jarvis, M. J.; Lagache, G.; Maddox, S.; Negrello, M.; Serjeant, S.; Thompson, M. A.; Kampen, E. van; Amblard, A.; Andreani, P.; Baes, M.; Beelen, A.; Bendo, G. J.; Benford, Dominic J.; Bertoldi, F.; Bock, J. J.; Bonfield, D. G.; Boselli, A.; Bridge, Carrie; Buat, V.; Burgarella, D.; Carlberg, R.; Cava, A.; Chanial, P.; Charlot, S.; Christopher, N.; Coles, Peter; Cortese, Luca; Dariush, Aliakbar; Cunha, Elisabete da; Dalton, Gavin; Danese, L.; Dannerbauer, H.; Driver, Simon P.; Dunlop, James; Fan, Lulu; Farrah, D.; Frayer, D. T.; Frenk, Carlos S.; Geach, J. E.; Gardner, Jonathan P.; Gomez, Haley Louise; González‐Nuevo, J.; González-Solares, E.; Griffin, Matthew Joseph; Hardcastle, M. J.; Hatziminaoglou, E.; Herranz, D.; Hughes, D. H.; Ibar, E.; Jeong, Wooju; Lacey, Cedric G.; Lapi, A.; Lawrence, A.; Lee, M.; Leeuw, Lerothodi Leonard; Liske, J.; López‐Caniego, M.; Müller, Thomas; Nandra, K.; Panuzzo, P.; Παπαγεωργίου, Ανδρέας; Patanchon, G.; Peacock, J. A.; Pearson, Chris; Phillipps, S.; Pohlen, M.; Popescu, C. C.; Rawlings, Steve; Rigby, E.; Rigopoulou, M.; Robotham, Aaron S. G.; Rodighiero, G.; Sansom, A. E.; Schulz, B.; Scott, D.; Smith, D. J. B.; Sibthorpe, B.; Smail, Ian; Stevens, J. A.; Sutherland, William J.; Takeuchi, Tsutomu T.; Tedds, J. A.; Temi, P.; Tuffs, R.; Trichas, M.; Vaccari, M.; Valtchanov, I.; Werf, P. van der; Verma, Aprajita; Vieria, J.; Vlahakis, C.; White, G. J.

doi:10.1086/653086

Cited by 565 publications

(386 citation statements)

References 56 publications

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“…The H-ATLAS survey (Herschel Astrophysical Terahertz Large Area Survey - Eales et al 2010;Valiante et al 2016) is one of the largest legacies of Herschel. This survey observed a total of 616.4 square degrees over five fields in five wavebands.…”

Section: Introductionmentioning

confidence: 99%

The Herschel Bright Sources (HerBS): sample definition and SCUBA-2 observations

Bakx

Eales

Negrello

et al. 2017

Monthly Notices of the Royal Astronomical Society

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101

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We present the Herschel Bright Sources (HerBS) sample, a sample of bright, high-redshift Herschel sources detected in the 616.4 square degree H-ATLAS survey. The HerBS sample contains 209 galaxies, selected with a 500 µm flux density greater than 80 mJy and an estimated redshift greater than 2. The sample consists of a combination of HyLIRGs and lensed ULIRGs during the epoch of peak cosmic star formation. In this paper, we present SCUBA-2 observations at 850 µm of 189 galaxies of the HerBS sample, 152 of these sources were detected. We fit a spectral template to the Herschel-SPIRE and 850 µm SCUBA-2 flux densities of 22 sources with spectroscopically determined redshifts, using a two-component modified blackbody spectrum as a template. We find a cold-and hot-dust temperature of 21.29 +1.35 −1.66 K and 45.80 +2.88 −3.48 K, a cold-to-hot dust mass ratio of 26.62 +5.61 −6.74 and a β of 1.83 +0.14 −0.28 . The poor quality of the fit suggests that the sample of galaxies is too diverse to be explained by our simple model. Comparison of our sample to a galaxy evolution model indicates that the fraction of lenses is high. Out of the 152 SCUBA-2 detected galaxies, the model predicts 128.4 ± 2.1 of those galaxies to be lensed (84.5%). The SPIRE 500 µm flux suggests that out of all 209 HerBS sources, we expect 158.1 ± 1.7 lensed sources, giving a total lensing fraction of 76 per cent.

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Section: Introductionmentioning

confidence: 99%

The Herschel Bright Sources (HerBS): sample definition and SCUBA-2 observations

Bakx

Eales

Negrello

et al. 2017

Monthly Notices of the Royal Astronomical Society

Self Cite

101

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“…The search includes AGNs observed with SPIRE in a "Small Scan" mode and sources that are located in relatively large fields observed by various key projects. We searched for such sources in the following extragalactic fields: H-ATLAS (Eales et al 2010), COSMOS (Scoville et al 2007), Extended Groth Strip (EGS; Davis et al 2007), ELAIS (Rowan-Robinson et al 1999), Lockman Hole (Lonsdale et al 2003), Strip-82 (Adelman-McCarthy et al 2007), and Böotes (Jannuzi et al 2004). This list does not cover every field observed with SPIRE and reflects the publicly available Herschel data that was correct to late 2014.…”

Section: Sample Selectionmentioning

confidence: 99%

Star Formation Black Hole Growth and Dusty Tori in the Most Luminous Agns at Z = 2–3.5

Netzer

Lani

Nordon

et al. 2016

ApJ

136

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We report Herschel/SPIRE observations of 100 very luminous, optically selected active galactic nuclei (AGNs) at z 2 3.5 -= with log L 1350 (ergs −1 ) 46.5 , where L 1350 is λL λ at 1350 Å. The distribution in L 1350 is similar to the general distribution of Sloan Digital Sky Survey AGNs in this redshift and luminosity interval. We measured starformation (SF) luminosity, L SF , and SF rate (SFR) in 34 detected sources by fitting combined SF and torus templates, where the torus emission is based on Wide Field Infrared Survey Explorer observations. We also obtained statistically significant stacks for the undetected sources in two luminosity groups. The sample properties are compared with those of very luminous AGNs at z 4. M e yr −1 , respectively. The mean SFR of the undetected sources is 148 M e yr −1 . The ratio of SFR to the black hole accretion rate is ≈80 for the detected sources and less than 10 for the undetected sources. Unlike a sample of sources at z ; 4.8 that we studied recently, there is no difference in L AGN and only a very small difference in L torus between the detected and undetected sources. (2) The redshift distribution of L SF and L AGN for the most luminous, redshift 2-7 AGNs are different. Similar to previous studies, the highest L AGN are found at z ≈ 3. However, the L SF of such sources peaks at z ≈ 5. Assuming the objects in our sample are hosted by the most massive galaxies at those redshifts, we find that approximately 2/3 of the hosts are already below the main sequence of SF galaxies at z = 2−3.5. (3) The spectral energy distributions (SEDs) of dusty tori at high redshift are similar to the shapes found in low redshift, low luminosity AGNs. Herschel upper limits put strong constraints on the long wavelength shape of the SED, ruling out several earlier suggested torus templates as applicable for this sample. (4) We find no evidence for a luminosity dependence of the torus covering factor in sources with log L AGN (ergs −1 ) = 44−47.5. This conclusion is based on the recognition that the estimated L AGN in several earlier studies is highly uncertain and non-uniformally treated. The median covering factors over this range are 0.68 for isotropic dust emission and 0.4 for anisotropic emission.

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“…In the short term, SCUBA-2 on the JCMT will be mapping ∼10 deg 2 S 850 ∼1.2 mJy (1σ ) depths, although this limit still corresponds to rather luminous (∼ULIRG-class) systems at z ∼ 2. Similarly, Herschel has recently mapped large areas of sky in the 250-500 μm submm bands (Eales et al 2010;Oliver et al 2010), but these are relatively shallow surveys suffering from significant confusion issues that, at redshifts beyond z ∼ 1, are generally only tracing the most luminous galaxies, and not probing into the L regime. Finally, powerful radio galaxies at high redshifts provide excellent beacons for such molecular line semi-blind redshift surveys as they mark the centers of deep potential wells where multiple gas-rich systems converge, forming the massive galaxy clusters found in the present cosmic epoch (e.g., De Breuck et al 2004;Miley & De Breuck 2008).…”

Section: Semi-blind Redshift Surveysmentioning

confidence: 99%

Molecular and Atomic Line Surveys of Galaxies. I. The Dense, Star-Forming Gas Phase as a Beacon

Geach

Papadopoulos

2012

ApJ

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We predict the space density of molecular gas reservoirs in the universe and place a lower limit on the number counts of carbon monoxide (CO), hydrogen cyanide (HCN) molecular, and [C ii] atomic emission lines in blind redshift surveys in the submillimeter-centimeter spectral regime. Our model uses (1) recently available HCN spectral line energy distributions (SLEDs) of local luminous infrared galaxies (LIRGs, L IR > 10 11 L ), (2) a value for = SFR/M dense (H 2 ) provided by new developments in the study of star formation feedback on the interstellar medium, and (3) a model for the evolution of the infrared luminosity density. Minimal "emergent" CO SLEDs from the dense gas reservoirs expected in all star-forming systems in the universe are then computed from the HCN SLEDs since warm, HCN-bright gas will necessarily be CO-bright, with the dense star-forming gas phase setting an obvious minimum to the total molecular gas mass of any star-forming galaxy. We include [C ii] as the most important of the far-infrared cooling lines. Optimal blind surveys with the Atacama Large Millimeter Array (ALMA) could potentially detect very distant (z ∼ 10-12) [C ii] emitters in the ULIRG galaxy class at a rate of ∼0.1-1 hr −1 (although this prediction is strongly dependent on the star formation and enrichment history at this early epoch), whereas the (high-frequency) Square Kilometer Array will be capable of blindly detecting z > 3 low-J CO emitters at a rate of ∼40-70 hr −1 . The [C ii] line holds special promise for detecting metal-poor systems with extensive reservoirs of CO-dark molecular gas where detection rates with ALMA can reach up to 2-7 hr −1 in Bands 4-6.

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The Herschel ATLAS

Cited by 565 publications

References 56 publications

The Herschel Bright Sources (HerBS): sample definition and SCUBA-2 observations

The Herschel Bright Sources (HerBS): sample definition and SCUBA-2 observations

Star Formation Black Hole Growth and Dusty Tori in the Most Luminous Agns at Z = 2–3.5

Molecular and Atomic Line Surveys of Galaxies. I. The Dense, Star-Forming Gas Phase as a Beacon

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