Galaxy clusters and groups in the ALHAMBRA survey

Ascaso, B.; Benı́tez, N.; Fernández-Soto, A.; Arnalte-Mur, P.; López-Sanjuan, C.; Molino, A.; Schoenell, W.; Jiménez-Teja, Y.; Merson, A.; Huertas-Company, M.; Díaz-García, L. A.; Martínez, V. J.; Cenarro, A. J.; Dupke, Renato A.; Márquez, I.; Masegosa, J.; Nieves-Seoane, L.; Pović, M.; Varela, J.; Viironen, K.; Aguerri, J. A. L.; Olmo, A. del; Moles, M.; Perea, J.; Alfaro, E. J.; Aparicio-Villegas, T.; Broadhurst, Tom; Cabrera-Caño, J.; Castander, F. J.; Cepa, J.; Cerviño, M.; Delgado, R. M. González; Cristóbal-Hornillos, D.; Hurtado-Gil, L.; Husillos, C.; Infante, L.; Prada, Francisco; Quintana, J. M.

doi:10.1093/mnras/stv1317

Cited by 21 publications

(28 citation statements)

References 78 publications

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“…Instead of color selections, that may rely on the type of stellar populations present in cluster galaxies as a function of redshift, a more complete selection of distant clusters can be made by searching for overdensities in redshift space, provided that accurate photometric redshifts over a large survey area are available (e.g., van Breukelen & Clewley, 2009;Eisenhardt et al, 2008;Chiaberge et al, 2010;Spitler et al, 2012;Castignani et al, 2014;Chiang et al, 2014;Ascaso et al, 2015;Wang et al, 2016). Strazzullo et al (2015) searched for overdensities of passive galaxies with photometric redshifts using nearest neighbor or fixed physical radius densities, finding several promising candidates in the range 1.5 < z < 2.5.…”

Section: High Redshift Cluster Surveysmentioning

confidence: 99%

The realm of the galaxy protoclusters

Overzier

2016

Astron Astrophys Rev

278

204

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The study of galaxy protoclusters is beginning to fill in unknown details of the important phase of the assembly of clusters and cluster galaxies. This review describes the current status of this field and highlights promising recent findings related to galaxy formation in the densest regions of the early universe. We discuss the main search techniques and the characteristic properties of protoclusters in observations and simulations, and show that protoclusters will have present-day masses similar to galaxy clusters when fully collapsed. We discuss the physical properties of galaxies in protoclusters, including (proto-)brightest cluster galaxies, and the forming red sequence. We highlight the fact that the most massive halos at high redshift are found in protoclusters, making these objects uniquely suited for testing important recent models of galaxy formation. We show that galaxies in protoclusters should be among the first galaxies at high redshift making the transition from a gas cooling regime dominated by cold streams to a regime dominated by hot intracluster gas, which could be tested observationally. We also discuss the possible connections between protoclusters and radio galaxies, quasars, and Ly-alpha blobs. Because of their early formation, large spatial sizes and high total star formation rates, protoclusters have also likely played a crucial role during the epoch of reionization, which can be tested with future experiments that will map the neutral and ionized cosmic web. Last, we review a number of promising observational projects that are expected to make significant impact in this growing, exciting field.Comment: Invited article for The Astronomy and Astrophysics Review (in press

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Section: High Redshift Cluster Surveysmentioning

confidence: 99%

The realm of the galaxy protoclusters

Overzier

2016

Astron Astrophys Rev

278

204

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“…This problem, known as the colour-redshift degeneracy, makes PDFs the only robust way to track the uncertainties in the observed photometry to the physical properties of interest. In this context, the ALHAMBRA photometric redshift PDFs have been successfully used to study high-redshift (z > 2) galaxies (Viironen et al 2015), to detect galaxy groups and clusters (Ascaso et al 2015), to estimate the merger fraction (López-Sanjuan et al 2015b), or to improve the estimation of stellar population parameters (Díaz-García et al 2015).…”

Section: Photometric Redshift Pdfmentioning

confidence: 99%

The ALHAMBRA survey:B-band luminosity function of quiescent and star-forming galaxies at 0.2 ≤ z < 1 by PDF analysis

López-Sanjuan

Tempel

Benı́tez

et al. 2017

A&A

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Aims. Our goal is to study the evolution of the B-band luminosity function (LF) since z ∼ 1 using ALHAMBRA data. Methods. We used the photometric redshift and the I-band selection magnitude probability distribution functions (PDFs) of those ALHAMBRA galaxies with I ≤ 24 mag to compute the posterior LF. We statistically studied quiescent and star-forming galaxies using the template information encoded in the PDFs. The LF covariance matrix in redshift -magnitude -galaxy type space was computed, including the cosmic variance. That was estimated from the intrinsic dispersion of the LF measurements in the 48 ALHAMBRA sub-fields. The uncertainty due to the photometric redshift prior is also included in our analysis. Results. We modelled the LF with a redshift-dependent Schechter function affected by the same selection effects than the data. The measured ALHAMBRA LF at 0.2 ≤ z < 1 and the evolving Schechter parameters both for quiescent and star-forming galaxies agree with previous results in the literature. The estimated redshift evolution of M * B ∝ Qz is Q SF = −1.03 ± 0.08 and Q Q = −0.80 ± 0.08, and of log 10 φ * ∝ Pz is P SF = −0.01 ± 0.03 and P Q = −0.41 ± 0.05. The measured faint-end slopes are α SF = −1.29 ± 0.02 and α Q = −0.53 ± 0.04. We find a significant population of faint quiescent galaxies with M B −18, modelled by a second Schechter function with slope β = −1.31 ± 0.11. Conclusions. We present a robust methodology to compute LFs using multi-filter photometric data. The application to ALHAMBRA shows a factor 2.55 ± 0.14 decrease in the luminosity density j B of star-forming galaxies, and a factor 1.25 ± 0.16 increase in the j B of quiescent ones since z = 1, confirming the continuous build-up of the quiescent population with cosmic time. The contribution of the faint quiescent population to j B increases from 3% at z = 1 to 6% at z = 0. The developed methodology will be applied to future multi-filter surveys such as J-PAS.

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“…Fernández-Soto et al 2002;Cunha et al 2009;Wittman 2009;Myers et al 2009;Schmidt & Thorman 2013;Carrasco Kind & Brunner 2014). The ALHAMBRA PDFs have been successfully used to study high-redshift (z > 2) galaxies (Viironen et al 2015), to detect galaxy groups and clusters (Ascaso et al 2015), to estimate the merger fraction , or to improve the estimation of stellar population parameters (Díaz-García et al 2015). The probability that a galaxy i is located at redshift z and has a spectral type T is PDF i (z, T ).…”

Section: Probability Distribution Functions In Alhambramentioning

confidence: 99%

The ALHAMBRA survey: Estimation of the clustering signal encoded in the cosmic variance

López-Sanjuan

Cenarro

Hernández-Monteagudo

et al. 2015

A&A

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Aims. The relative cosmic variance (σ v ) is a fundamental source of uncertainty in pencil-beam surveys and, as a particular case of count-in-cell statistics, can be used to estimate the bias between galaxies and their underlying dark-matter distribution. Our goal is to test the significance of the clustering information encoded in the σ v measured in the ALHAMBRA survey. Methods. We measure the cosmic variance of several galaxy populations selected with B-band luminosity at 0.35 ≤ z < 1.05 as the intrinsic dispersion in the number density distribution derived from the 48 ALHAMBRA subfields. We compare the observational σ v with the cosmic variance of the dark matter expected from the theory, σ v,dm . This provides an estimation of the galaxy bias b. Results. The galaxy bias from the cosmic variance is in excellent agreement with the bias estimated by two-point correlation function analysis in ALHAMBRA. This holds for different redshift bins, for red and blue subsamples, and for several B-band luminosity selections. We find that b increases with the B-band luminosity and the redshift, as expected from previous work. Moreover, red galaxies have a larger bias than blue galaxies, with a relative bias of b rel = 1.4 ± 0.2.Conclusions. Our results demonstrate that the cosmic variance measured in ALHAMBRA is due to the clustering of galaxies and can be used to characterise the σ v affecting pencil-beam surveys. In addition, it can also be used to estimate the galaxy bias b from a method independent of correlation functions.

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Galaxy clusters and groups in the ALHAMBRA survey

Cited by 21 publications

References 78 publications

The realm of the galaxy protoclusters

The realm of the galaxy protoclusters

The ALHAMBRA survey:B-band luminosity function of quiescent and star-forming galaxies at 0.2 ≤ z < 1 by PDF analysis

The ALHAMBRA survey: Estimation of the clustering signal encoded in the cosmic variance

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