Galaxy protocluster candidates at 1.6  &lt;  <i>z</i>  ≲  2

Galametz, A.; Vernet, J.; Breuck, C. De; Hatch, N. A.; Miley, G. K.; Kodama, Tadayuki; Kurk, J.; Overzier, Roderik; Rettura, Alessandro; Röttgering, H. J. A.; Seymour, N.; Venemans, Bram; Zirm, A.

doi:10.1051/0004-6361/201015035

Cited by 28 publications

(27 citation statements)

References 85 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Towards that goal, literature that stretches back nearly 50 years shows that powerful radio-selected AGN preferentially reside in luminous red sequence galaxies (e.g., Matthews 1965;Best et al 1998;Venemans et al 2002;Hickox et al 2009;Griffith & Stern 2010). Indeed, targeted searches for high-redshift clusters and protoclusters around powerful high-redshift radio galaxies (HzRGs) have proven very successful and have a rich literature (e.g., Pentericci et al 2000;Stern et al 2003;Kurk et al 2004;Venemans et al 2007;Doherty et al 2010;Galametz et al 2009Galametz et al , 2010bHatch et al 2011;Matsuda et al 2011;Mayo et al 2012).…”

Section: Introductionmentioning

confidence: 99%

GALAXY CLUSTERS AROUND RADIO-LOUD ACTIVE GALACTIC NUCLEI AT 1.3 <z< 3.2 AS SEEN BYSPITZER

Wylezalek

Galametz

Stern

et al. 2013

ApJ

203

337

View full text Add to dashboard Cite

We report the first results from the Clusters Around Radio-Loud AGN (CARLA) program, a Cycle 7 and 8 Spitzer Space Telescope snapshot program to investigate the environments of a large sample of obscured and unobscured luminous radio-loud AGN at 1.2 < z < 3.2. These data, obtained for 387 fields, reach 3.6 and 4.5 µm depths of [3.6] AB = 22.6 and [4.5] AB = 22.9 at the 95% completeness level, which is two to three times fainter than L * in this redshift range. By using the color cut [3.6]-[4.5] > −0.1 (AB), which efficiently selects high-redshift (z > 1.3) galaxies of all types, we identify galaxy cluster member candidates in the fields of the radio-loud AGN. The local density of these IRAC-selected sources is compared to the density of similarly selected sources in blank fields. We find that 92% of the radio-loud AGN reside in environments richer than average. The majority (55%) of the radio-loud AGN fields are found to be overdense at a 2 σ level; 10% are overdense at a 5 σ level. A clear rise in surface density of IRAC-selected sources towards the position of the radio-loud AGN strongly supports an association of the majority of the IRAC-selected sources with the radioloud AGN. Our results provide solid statistical evidence that radio-loud AGN are likely beacons for finding high-redshift galaxy (proto-)clusters. We investigate how environment depends on AGN type (unobscured radio-loud quasars vs. obscured radio galaxies), radio luminosity and redshift, finding no correlation with either AGN type or radio luminosity. We find a decrease in density with redshift, consistent with galaxy evolution for this uniform, flux-limited survey. These results are consistent with expectations from the orientation-driven AGN unification model, at least for the high radio luminosity regimes considered in this sample.

show abstract

Section: Introductionmentioning

confidence: 99%

GALAXY CLUSTERS AROUND RADIO-LOUD ACTIVE GALACTIC NUCLEI AT 1.3 <z< 3.2 AS SEEN BYSPITZER

Wylezalek

Galametz

Stern

et al. 2013

ApJ

203

337

View full text Add to dashboard Cite

show abstract

“…It is particularly important for understanding how the morphologydensity relation (Dressler 1980) arose from the early z > 2 protoclusters, which were just beginning to form their red sequences (Kodama et al 2007;Tanaka et al 2013). Unlike lower redshift galaxy clusters, these protoclusters are usually rich in massive, star-forming galaxies (e.g., Overzier et al 2008;Galametz et al 2010;Hatch et al 2011aHatch et al , 2011bKuiper et al 2010;Koyama et al 2013a;Cooke et al 2014;Dannerbauer et al 2014;Shimakawa et al 2014;Umehata et al 2015). However, the galaxies in protoclusters are still affected by their environment.…”

Section: Introductionmentioning

confidence: 99%

Stellar mass function of cluster galaxies atz~ 1.5: evidence for reduced quenching efficiency at high redshift

Nantais

Burg

Lidman

et al. 2016

A&A

132

View full text Add to dashboard Cite

We present the stellar mass functions (SMFs) of passive and star-forming galaxies with a limiting mass of 10 10.1 M in four spectroscopically confirmed Spitzer Adaptation of the Red-sequence Cluster Survey (SpARCS) galaxy clusters at 1.37 < z < 1.63. The clusters have 113 spectroscopically confirmed members combined, with 8-45 confirmed members each. We construct Ks-bandselected photometric catalogs for each cluster with an average of 11 photometric bands ranging from u to 8 µm. We compare our cluster galaxies to a field sample derived from a similar Ks-band-selected catalog in the UltraVISTA/COSMOS field. The SMFs resemble those of the field, but with signs of environmental quenching. We find that 30 ± 20% of galaxies that would normally be forming stars in the field are quenched in the clusters. The environmental quenching efficiency shows little dependence on projected cluster-centric distance out to ∼4 Mpc, providing tentative evidence of pre-processing and/or galactic conformity in this redshift range. We also compile the available data on environmental quenching efficiencies from the literature, and find that the quenching efficiency in clusters and in groups appears to decline with increasing redshift in a manner consistent with previous results and expectations based on halo mass growth.

show abstract

“…The questions of when and how present-day galaxy clusters formed at high redshift have driven extensive searches for protoclusters of galaxies in the distant Universe in the past two decades (e.g., Le Fevre et al 1996;Steidel et al 1998;Pentericci et al 2000;Kurk et al 2000Kurk et al , 2004aBest et al 2003;Matsuda et al 2005;Daddi et al 2009a;Galametz et al 2010;Galametz et al 2012;Hatch et al 2011a,b;Mayo et al 2012;Walter et al 2012;Wylezalek et al 2013). Powerful high-redshift radio galaxies (HzRGs; see the review by Miley & De Breuck 2008) LABOCA and VLA images (FITS files) are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/570/A55 are considered to be the most promising signposts of the most massive clusters in formation.…”

Section: Introductionmentioning

confidence: 99%

An excess of dusty starbursts related to the Spiderweb galaxy

Dannerbauer

Kurk

Breuck

et al. 2014

A&A

Self Cite

141

208

View full text Add to dashboard Cite

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.

show abstract

Galaxy protocluster candidates at 1.6 < z ≲ 2

Cited by 28 publications

References 85 publications

GALAXY CLUSTERS AROUND RADIO-LOUD ACTIVE GALACTIC NUCLEI AT 1.3 <z< 3.2 AS SEEN BYSPITZER

GALAXY CLUSTERS AROUND RADIO-LOUD ACTIVE GALACTIC NUCLEI AT 1.3 <z< 3.2 AS SEEN BYSPITZER

Stellar mass function of cluster galaxies atz~ 1.5: evidence for reduced quenching efficiency at high redshift

An excess of dusty starbursts related to the Spiderweb galaxy

Contact Info

Product

Resources

About