Economic Analysis

Kuiper, Edward

doi:10.1007/978-1-4899-6281-2_11

Cited by 13 publications

(13 citation statements)

References 1 publication

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“…The literature provides further supporting evidence for this interpretation. Steidel et al (2003) also found that the stellar masses of galaxies in a z = 2.3 protocluster are twice as massive as similarly selected galaxies in the field, and Kuiper et al (2010) found a similar result for Lyman break galaxies in a z = 3.1 protocluster. Furthermore, Tanaka et al (2010) found the ages of galaxies in the MRC 1138−262 protocluster were similar to those in the field.…”

Section: Stellar Massesmentioning

confidence: 84%

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Hα emitters in z∼ 2 protoclusters: evidence for faster evolution in dense environments

Hatch

Kurk

Pentericci³

et al. 2011

Monthly Notices of the Royal Astronomical Society

110

112

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This is a study of Hα emitters in two dense galaxy protoclusters surrounding radio galaxies at z∼ 2. We show that the protocluster surrounding MRC 1138−262 contains 14 ± 2 times more Hα candidates than the average field (9σ significance), and the z= 2.35 radio galaxy 4C +10.48 is surrounded by 12 ± 2 times more emitters than the field (5σ), so it is also likely to reside in a dense protocluster environment. We compared these Hα emitters, situated in dense environments, to a control field sample selected from three separate fields forming a total area of 172 arcmin2. We constructed and compared Hα and rest‐frame R continuum luminosity functions of the emitters in both environments. The star formation density is on average 13 times greater in the protoclusters than the field at z∼ 2, so the total star formation rate within the central 1.5 Mpc of the protoclusters exceeds 3000 M⊙ yr−1. However, we found no significant difference in the shape of the Hα luminosity functions, implying that environment does not substantially affect the strength of the Hα line from strongly star‐forming galaxies. The protocluster emitters are typically 0.8 mag brighter in rest‐frame R continuum than field emitters, implying they are twice as massive as their field counterparts at the same redshift. We also show the protocluster galaxies have lower specific star formation rates than field galaxies, meaning the emitters in the dense environments formed more of their stars earlier than the field galaxies. We conclude that galaxy growth in the early Universe was accelerated in dense environments, and that cluster galaxies differed from field galaxies even before the cluster had fully formed.

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Section: Stellar Massesmentioning

confidence: 84%

“…Protocluster studies that use broad‐band photometric redshifts are plagued by sample contamination (e.g. Kuiper et al 2010; Tanaka et al 2010), and any signature of environmental dependance may be washed out.…”

Section: Introductionmentioning

confidence: 99%

Hα emitters in z∼ 2 protoclusters: evidence for faster evolution in dense environments

Hatch

Kurk

Pentericci³

et al. 2011

Monthly Notices of the Royal Astronomical Society

110

112

View full text Add to dashboard Cite

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“…The other detections (e.g., less massive objects) can only currently be identified as significant red galaxy overdensities, without confirmation of virialization by the detection of hot gas. Depending on the presence, or not, of the red sequence and their richness, these objects have been identified as clusters or proto-clusters (e.g., Pentericci et al 2000;Miley et al 2004Miley et al , 2006Venemans 2007;Kuiper et al 2010;.…”

Section: Discussionmentioning

confidence: 99%

STAR-FORMING BLUE ETGS IN TWO NEWLY DISCOVERED GALAXY OVERDENSITIES IN THE HUDF ATz= 1.84 AND 1.9: UNVEILING THE PROGENITORS OF PASSIVE ETGS IN CLUSTER CORES

Mei

Scarlata

Pentericci

et al. 2015

ApJ

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We present the discovery of two galaxy overdensities in the Hubble Space Telescope UDF: a proto-cluster, HUDFJ0332.4-2746.6 at z = 1.84 ± 0.01, and a group, HUDFJ0332.5-2747.3 at z = 1.90 ± 0.01. Assuming viralization, the velocity dispersion of HUDFJ0332.4-2746.6 implies a mass of M 200 = (2.2±1.8)×10 14 M , consistent with the lack of extended X-ray emission. Neither overdensity shows evidence of a red sequence. About 50% of their members show interactions and/or disturbed morphologies, which are signatures of merger remnants or disk instability. Most of their ETGs have blue colors and show recent star-formation. These observations reveal for the first time large fractions of spectroscopically confirmed star-forming blue ETGs in proto-clusters at z ≈ 2. These star-forming ETGs are most likely among the progenitors of the quiescent population in clusters at more recent epochs. Their mass-size relation is consistent with that of passive ETGs in clusters at z ∼ 0.7 − 1.5. If these galaxies are the progenitors of cluster ETGs at these lower redshifts, their size would evolve according to a similar mass-size relation. It is noteworthy that quiescent ETGs in clusters at z = 1.8 − 2 also do not show any significant size evolution over this redshift range, contrary to field ETGs. The ETG fraction is 50%, compared to the typical quiescent ETG fraction of ≈ 80% in cluster cores at z < 1. The fraction, masses, and colors of the newly discovered ETGs imply that other cluster ETGs will be formed/accreted at a later time.

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“…A study by Maschietto et al (, hereafter M08) has found tentative evidence for a similar overdensity of [O iii ] emitters. In an attempt to obtain a complete galaxy census of the overdensity, Kuiper et al (, hereafter K10) assembled photometry of the field in 18 bands ranging from U band to Spitzer 8 μm. K10 selected LBGs in the 40 arcmin 2 field around the radio galaxy and detected a small surface overdensity.…”

Section: Introductionmentioning

confidence: 99%

A z ∼ 3 radio galaxy and its protocluster: evidence for a superstructure?

Kuiper

Venemans

Hatch

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present spectroscopic follow‐up observations of Lyman‐break galaxies (LBGs) selected in the field surrounding the radio galaxy MRC 0316−257 at z ∼ 3.13 (0316). Robust spectroscopic redshifts are determined for 20 out of 24 objects. Three of the spectroscopically confirmed galaxies have 3.12 < z < 3.13 indicating that these objects reside in a protocluster structure previously found around the radio galaxy. An additional five objects are found 1600 km s−1 blue shifted with respect to the main protocluster structure. This is in addition to three [O iii] emitters found at this redshift in a previous study. This is further evidence that a structure exists directly in front of the 0316 protocluster. We estimate that the foreground structure is responsible for half of the surface overdensity of LBGs found in the field as a whole. The foreground structure is associated with a strong surface density peak 1.4 Mpc to the north‐west of the radio galaxy, and a 2D Kolmogorov–Smirnov test indicates that the spatial distributions of the 0316 and foreground galaxies differ at the 3σ level. In addition, we compare the properties of protocluster, foreground structure and field galaxies, but we find no significant differences. In terms of the nature of the two structures, a merger scenario is a possible option. Simple merger dynamics indicates that the observed relative velocity of 1600 km s−1 can be reproduced if the two structures have masses of ∼5 × 1014 M⊙ and have starting separations of around 2.5–3 Mpc. It is also possible that the foreground structure is unrelated to the 0316 protocluster in which case the two structures will not interact before z = 0.

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Economic Analysis

Cited by 13 publications

References 1 publication

Hα emitters in z∼ 2 protoclusters: evidence for faster evolution in dense environments

Hα emitters in z∼ 2 protoclusters: evidence for faster evolution in dense environments

STAR-FORMING BLUE ETGS IN TWO NEWLY DISCOVERED GALAXY OVERDENSITIES IN THE HUDF ATz= 1.84 AND 1.9: UNVEILING THE PROGENITORS OF PASSIVE ETGS IN CLUSTER CORES

A z ∼ 3 radio galaxy and its protocluster: evidence for a superstructure?

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