The first release of data from the Herschel ATLAS: the SPIRE images★

Pascale, Enzo; Auld, Robbie Richard; Dariush, Aliakbar; Dunne, L.; Eales, Stephen Anthony; Maddox, S.; Panuzzo, P.; Pohlen, M.; Smith, Daniel; Buttiglione, S.; Cava, A.; Clements, D. L.; Cooray, Asantha; Dye, S.; Zotti, G. de; Fritz, J.; Hopwood, R.; Ibar, E.; Ivison, R. J.; Jarvis, M. J.; Leeuw, Lerothodi Leonard; López‐Caniego, M.; Rigby, E. E.; Rodighiero, G.; Scott, D.; Smith, Matthew W.; Temi, P.; Vaccari, M.; Valtchanov, I.

doi:10.1111/j.1365-2966.2011.18756.x

Cited by 107 publications

(109 citation statements)

References 25 publications

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“…This source, in particular, was found to be a 160 μm-peaker, suggesting z ∼ 1. The SPIRE data reduction is described in Pascale et al (2011), while source extraction and flux density estimation are described in Rigby et al (2011).…”

Section: Source Selection and Observationsmentioning

confidence: 99%

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Herschel-ATLAS and ALMA

Messias

Dye

Nagar

et al. 2014

A&A

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Context. The submillimetre-bright galaxy population is believed to comprise, aside from local galaxies and radio-loud sources, intrinsically active star-forming galaxies, the brightest of which are lensed gravitationally. The latter enable studies at a level of detail beyond what is usually possible by the observation facility. Aims. This work focuses on one of these lensed systems, HATLAS J142935.3−002836 (H1429−0028), selected in the Herschel-ATLAS field. Gathering a rich, multi-wavelength dataset, we aim to confirm the lensing hypothesis and model the background source's morphology and dynamics, as well as to provide a full physical characterisation. Methods. Multi-wavelength high-resolution data is utilised to assess the nature of the system. A lensing-analysis algorithm that simultaneously fits different wavebands is adopted to characterise the lens. The background galaxy dynamical information is studied by reconstructing the 3D source plane of the ALMA CO (J:4 → 3) transition. Near-IR imaging from HST and Keck-AO allows to constrain rest-frame optical photometry independently for the foreground and background systems. Physical parameters (such as stellar and dust masses) are estimated via modelling of the spectral energy distribution taking source blending, foreground obscuration, and differential magnification into account. Results. The system comprises a foreground edge-on disk galaxy (at z sp = 0.218) with an almost complete Einstein ring around it. The background source (at z sp = 1.027) is magnified by a factor of μ ∼ 8−10 depending on wavelength. It is comprised of two components and a tens-of-kpc-long tidal tail resembling the Antennae merger. As a whole, the background source is a massive stellar system (1.32 +0.63−0.41 × 10 11 M ) forming stars at a rate of 394 ± 90 M yr −1 , and it has a significant gas reservoir M ISM = 4.6 ± 1.7 × 10 10 M . Its depletion time due to star formation alone is thus expected to be τ SF = M ISM /SFR = 117 ± 51 Myr. The dynamical mass of one of the components is estimated to be 5.8 ± 1.7 × 10 10 M , and, together with the photometric total mass estimate, it implies that H1429−0028 is a major merger system (1:2.8 +1.8 −1.5).

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Section: Source Selection and Observationsmentioning

confidence: 99%

“…This procedure is described in detail in Rigby et al (2011). PACS and SPIRE data reduction are described, respectively, in Ibar et al (2010a) and Pascale et al (2011). 7 The SDSS magnitudes u and z have been converted to AB magnitudes by adding, respectively, −0.04 and 0.02.…”

Section: Multi-wavelength Photometrymentioning

confidence: 99%

Herschel-ATLAS and ALMA

Messias

Dye

Nagar

et al. 2014

A&A

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“…Our adopted procedure for the determination of the photometric uncertainties in the SPIRE maps is fully described by Leipski et al (2013), which in turn follows the procedures presented by Elbaz et al (2011) and Pascale et al (2011). Initially, an artificial source free map was created by removing the extracted sources in a SPIRE map from the map itself.…”

Section: Spirementioning

confidence: 99%

Star formation inz> 1 3CR host galaxies as seen byHerschel

Podigachoski

Barthel

Haas

et al. 2015

A&A

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We present Herschel (PACS and SPIRE) far-infrared (FIR) photometry of a complete sample of z > 1 3CR sources, from the Herschel guaranteed time project The Herschel Legacy of distant radio-loud AGN. Combining these with existing Spitzer photometric data, we perform an infrared (IR) spectral energy distribution (SED) analysis of these landmark objects in extragalactic research to study the star formation in the hosts of some of the brightest active galactic nuclei (AGN) known at any epoch. Accounting for the contribution from an AGN-powered warm dust component to the IR SED, about 40% of our objects undergo episodes of prodigious, ULIRGstrength star formation, with rates of hundreds of solar masses per year, coeval with the growth of the central supermassive black hole. Median SEDs imply that the quasar and radio galaxy hosts have similar FIR properties, in agreement with the orientationbased unification for radio-loud AGN. The star-forming properties of the AGN hosts are similar to those of the general population of equally massive non-AGN galaxies at comparable redshifts, thus there is no strong evidence of universal quenching of star formation (negative feedback) within this sample. Massive galaxies at high redshift may be forming stars prodigiously, regardless of whether their supermassive black holes are accreting or not.

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“…It was allocated 600 hr of observing time and covers about 600 deg 2 of sky in five photometric bands (100, 160, 250, 350 and 500 μm) with the Photodetector Array Camera and Spectrometer (PACS; Poglitsch et al 2010) and the Spectral and Photometric Imaging Receiver (SPIRE; Griffin et al 2010). H-ATLAS map making is described by Pascale et al (2011) for SPIRE and by Ibar et al (2010) for PACS. The procedures for source extraction and catalog generation can be found in Rigby et al (2011) andE.…”

Section: Planck Datamentioning

confidence: 99%

Toward a Tomographic Analysis of the Cross-Correlation Between Planck CMB Lensing and H-Atlas Galaxies

Bianchini

Lapi

Calabrese

et al. 2016

ApJ

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We present an improved and extended analysis of the cross-correlation between the map of the cosmic microwave background (CMB) lensing potential derived from the Planck mission data and the high-redshift galaxies detected by the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) in the photometric redshift range  z 1.5 ph . We compare the results based on the 2013 and 2015 Planck datasets, and investigate the impact of different selections of the H-ATLAS galaxy samples. Significant improvements over our previous analysis have been achieved thanks to the higher signal-to-noise ratio of the new CMB lensing map recently released by the Planck collaboration. The effective galaxy bias parameter, b, for the full galaxy sample, derived from a joint analysis of the cross-power spectrum and of the galaxy auto-power spectrum is found to be = -+ b 3.54 0.14 0.15 . Furthermore, a first tomographic analysis of the cross-correlation signal is implemented by splitting the galaxy sample into two redshift intervals: 0.24 for the higher redshift bin. Consistent with our previous analysis, we find that the amplitude of the cross-correlation signal is a factor of -+ 1.45 0.13 0.14 higher than expected from the standard ΛCDM model for the assumed redshift distribution. The robustness of our results against possible systematic effects has been extensively discussed, although the tension is mitigated by passing from 4 to 3σ.

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The first release of data from the Herschel ATLAS: the SPIRE images★

Cited by 107 publications

References 25 publications

Herschel-ATLAS and ALMA

Herschel-ATLAS and ALMA

Star formation inz> 1 3CR host galaxies as seen byHerschel

Toward a Tomographic Analysis of the Cross-Correlation Between Planck CMB Lensing and H-Atlas Galaxies

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