A submillimetre-bright z ∼ 3 overdensity behind a z ∼ 1 supercluster revealed by SCUBA-2 and Herschel

Noble, Allison; Engelen, A.J. van; Webb, Tracy; Coppin, K. E. K.; Delahaye, Anna; Gilbank, David; Gladders, Michael D.; Ivison, R. J.; Omori, Y.; Yee, H. K. C.

doi:10.1093/mnrasl/slt108

Cited by 8 publications

(13 citation statements)

References 44 publications

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“…Our observations of the region around HATLAS12-00 have uncovered a number of potentially associated sources at both submm wavelengths, as found by SCUBA2 and LABOCA, and in the Herschel data themselves. These results are not dissimilar to the submm source overdensities uncovered by Stevens et al (2010) around quasars, the Herschel source overdensities found by Rigby et al (2014) around some high redshift radio galaxies, the overdensity of Herschel and LABOCA sources associated with the Spiderweb galaxy (Dannerbauer et al, 2014), or the Herschel and SCUBA2 overdensity found behind the RCS 231953+00 supercluster by Noble et al (2013). We here quantitatively asses the source overdensities of both submm and Herschel sources around HATLAS12-00.…”

Section: Source Overdensities Around Hatlas12-00supporting

confidence: 81%

“…no other region in our 10000 comparison fields has a similar 350µm source density), < 10 −4 , 8 × 10 −4 , 3 × 10 −4 and 3 × 10 −4 levels, suggesting the possible presence of an overdensity on larger scales than the Planck beam, up to a radius of ∼10 arcmin. While this would certainly be a large structure in terms of physical size, amounting to about 10Mpc in diameter if it lies at the same redshift as HATLAS12-00, it is comparable to the scale of the z∼3 candidate supercluster identified by Noble et al (2013), through a combination of SPIRE and SCUBA2 data, and a number of other known protoclusters (Casey, 2016). Examination of the progenitors of z = 0 massive clusters in the Millennium Simulation (Diener et al, 2015) suggests that they can be as large as 20Mpc across at z ∼ 3, consistent with the sizes of these overdensities identified in the far-IR/submm.…”

Section: Spire Source Densitymentioning

confidence: 91%

“…The use of SPIRE colour-colour diagrams to constrain redshifts is well established (eg. Schulz et al, 2010;Amblard et al, 2010;Negrello et al, 2010;Wardlow et al, 2013;Her-ranz et al, 2013;Noble et al, 2013;Clements et al, 2014) though their interpretation can be uncertain. The observed colours of sources are compared to the colours, as a function of redshift, of the spectral energy distributions (SEDs) of known low redshift template objects, such as the starburst galaxy M82 or the nearest ULIRG, Arp220.…”

Section: Herschel-submm Coloursmentioning

confidence: 99%

“…Large area surveys with the Herschel Space Observatory (Pilbratt et al, 2010), SCUBA2 (Dempsey et al, 2013;Holland et al, 2013), or the Planck all sky survey (Planck Collaboration, 2011;Negrello et al, 2005) are capable of finding such objects. Several studies have been undertaken combining Planck and Herschel data to identify candidate high redshift clusters while others have used Herschel data (eg Valtchanov et al, 2013;Dannerbauer et al, 2014;Rigby et al, 2014) or SCUBA2 data (Ma et al, 2015;Casey et al, 2015) alone or in combination (Noble et al, 2013). Clements et al (2014) found a number of candidate objects in the Her-MES (Oliver at al., 2012) survey at z∼ 1 − 2, while Herschel followup observations of Planck all sky sources (Planck Collaboration, 2015) have identified at least one z∼1.7 cluster of dusty galaxies and large numbers of candidates.…”

Section: Introductionmentioning

confidence: 99%

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H-ATLAS: a candidate high redshift cluster/protocluster of star-forming galaxies

Clements¹,

Braglia²,

Petitpas³

et al. 2016

Mon. Not. R. Astron. Soc.

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We investigate the region around the Planck-detected z=3.26 gravitationally lensed galaxy HATLAS J114637.9-001132 (hereinafter HATLAS12-00) using both archival Herschel data from the H-ATLAS survey and using submm data obtained with both LABOCA and SCUBA2. The lensed source is found to be surrounded by a strong overdensity of both Herschel-SPIRE sources and submm sources. We detect 17 bright (S 870 >∼7 mJy) sources at >4σ closer than 5 arcmin to the lensed object at 850/870µm. Ten of these sources have good cross-identifications with objects detected by Herschel-SPIRE which have redder colours than other sources in the field, with 350µm flux > 250µm flux, suggesting that they lie at high redshift. Submillimeter Array (SMA) observations localise one of these companions to ∼1 arcsecond, allowing unambiguous cross identification with a 3.6 and 4.5 µm Spitzer source. The optical/near-IR spectral energy distribution (SED) of this source is measured by further observations and found to be consistent with z > 2, but incompatible with lower redshifts. We conclude that this system may be a galaxy cluster/protocluster or larger scale structure that contains a number of galaxies undergoing starbursts at the same time.

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Section: Source Overdensities Around Hatlas12-00supporting

confidence: 81%

Section: Spire Source Densitymentioning

confidence: 91%

Section: Herschel-submm Coloursmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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H-ATLAS: a candidate high redshift cluster/protocluster of star-forming galaxies

Clements¹,

Braglia²,

Petitpas³

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The use of Herschel -SPIRE colour-colour diagrams to separate sources of different redshifts is well established (e.g. Herranz et al 2013;Noble et al 2013;Clements et al 2014;Ivison et al 2016;Negrello et al 2016), though the precise interpretation of the results are uncertain. Typically, sources whose SED peak at longer wavelengths tend to lie at higher redshifts ( 2016; Ivison et al 2016), and therefore sources whose SED peak at 250, 350 and 500 µm likely indicate progressively higher redshifts.…”

Section: Herschel Coloursmentioning

confidence: 99%

Candidate high-z protoclusters among the Planck compact sources, as revealed by Herschel–SPIRE

Greenslade

Clements

Cheng

et al. 2018

Monthly Notices of the Royal Astronomical Society

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By determining the nature of all the Planck compact sources within 808.4 deg 2 of large Herschel surveys, we have identified 27 candidate proto-clusters of dusty star forming galaxies (DSFGs) that are at least 3σ overdense in either 250, 350 or 500 µm sources. We find roughly half of all the Planck compact sources are resolved by Herschel into multiple discrete objects, with the other half remaining unresolved by Herschel. We find a significant difference between versions of the Planck catalogues, with earlier releases hosting a larger fraction of candidate proto-clusters and Galactic Cirrus than later releases, which we ascribe to a difference in the filters used in the creation of the three catalogues. We find a surface density of DSFG candidate protoclusters of (3.3 ± 0.7) × 10 −2 sources deg −2 , in good agreement with previous similar studies. We find that a Planck colour selection of S 857 /S 545 < 2 works well to select candidate proto-clusters, but can miss proto-clusters at z < 2. The Herschel colours of individual candidate proto-cluster members indicate our candidate proto-clusters all likely all lie at z > 1. Our candidate proto-clusters are a factor of 5 times brighter at 353 GHz than expected from simulations, even in the most conservative estimates. Further observations are needed to confirm whether these candidate proto-clusters are physical clusters, multiple proto-clusters along the line of sight, or chance alignments of unassociated sources.

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An excess of dusty starbursts related to the Spiderweb galaxy

Dannerbauer

Kurk

Breuck

et al. 2014

A&A

158

208

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We present APEX LABOCA 870 μm observations of the field around the high-redshift radio galaxy MRC1138−262 at z = 2.16. We detect 16 submillimeter galaxies (SMGs) in this ∼140 arcmin 2 bolometer map with flux densities in the range 3-11 mJy. The raw number counts indicate a density of SMGs that is up to four times that of blank field surveys. Based on an exquisite multiwavelength database, including VLA 1.4 GHz radio and infrared observations, we investigate whether these sources are members of the protocluster structure at z ≈ 2.2. Using Herschel PACS and SPIRE and Spitzer MIPS photometry, we derive reliable far-infrared (FIR) photometric redshifts for all sources. Follow-up VLT ISAAC and SINFONI NIR spectra confirm that four of these SMGs have redshifts of z ≈ 2.2. We also present evidence that another SMG in this field, detected earlier at 850 μm, has a counterpart that exhibits Hα and CO(1-0) emission at z = 2.15. Including the radio galaxy and two SMGs with FIR photometric redshifts at z = 2.2, we conclude that at least eight submm sources are part of the protocluster at z = 2.16 associated with the radio galaxy MRC1138−262. We measure a star formation rate density SFRD ∼1500 M yr −1 Mpc −3 , four magnitudes higher than the global SFRD of blank fields at this redshift. Strikingly, these eight sources are concentrated within a region of 2 Mpc (the typical size of clusters in the local universe) and are distributed within the filaments traced by the HAEs at z ≈ 2.2. This concentration of massive, dusty starbursts is not centered on the submillimeter-bright radio galaxy which could support the infalling of these sources into the cluster center. Approximately half (6/11) of the SMGs that are covered by the Hα imaging data are associated with HAEs, demonstrating the potential of tracing SMG counterparts with this population. To summarize, our results demonstrate that submillimeter observations may enable us to study (proto)clusters of massive, dusty starbursts.

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A submillimetre-bright z ∼ 3 overdensity behind a z ∼ 1 supercluster revealed by SCUBA-2 and Herschel

Cited by 8 publications

References 44 publications

H-ATLAS: a candidate high redshift cluster/protocluster of star-forming galaxies

H-ATLAS: a candidate high redshift cluster/protocluster of star-forming galaxies

Candidate high-z protoclusters among the Planck compact sources, as revealed by Herschel–SPIRE

An excess of dusty starbursts related to the Spiderweb galaxy

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