THE NEWFIRM MEDIUM-BAND SURVEY: PHOTOMETRIC CATALOGS, REDSHIFTS, AND THE BIMODAL COLOR DISTRIBUTION OF GALAXIES OUT TO<i>z</i>∼ 3

Whitaker, Katherine E.; Labbé, Ivo; Dokkum, Pieter van; Brammer, Gabriel; Kriek, Mariska; Marchesini, Danilo; Quadri, Ryan; Franx, Marijn; Muzzin, Adam; Williams, R.; Bezanson, Rachel; Illingworth, G. D.; Lee, Kyoung-Soo; Lundgren, Britt; Nelson, Erica J.; Rudnick, Gregory; Tal, Tomer; Wake, David A.

doi:10.1088/0004-637x/735/2/86

Cited by 402 publications

(437 citation statements)

References 68 publications

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“…1). This precision is similar to that achieved by the NEWFIRM Medium-Band Survey (NMBS; Whitaker et al 2011) which augmented the optical and near-infrared photometry on the COSMOS and AEGIS fields with five medium band images that ranged across the wavelength range typically spanned by Y , J and H. Here we show that a similar precision can be achieved for the galaxies in the protocluster with a smaller number of images because the filters were optimally chosen to span across the important Balmer and 4000Å breaks.…”

Section: Photometric Redshiftssupporting

confidence: 81%

The structure and evolution of a forming galaxy cluster atz= 1.62

Hatch

Muldrew

Cooke

et al. 2016

Mon. Not. R. Astron. Soc.

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We present a comprehensive picture of the Cl 0218.3−0510 protocluster at z = 1.623 across 10 co-moving Mpc. Using filters that tightly bracket the Balmer and 4000Å breaks of the protocluster galaxies we obtain precise photometric redshifts resulting in a protocluster galaxy sample that is 89 ± 5% complete and has a contamination of only 12 ± 5%. Both star forming and quiescent protocluster galaxies are located allowing us to map the structure of the forming cluster for the first time. The protocluster contains 6 galaxy groups, the largest of which is the nascent cluster. Only a small minority of the protocluster galaxies are in the nascent cluster (11%) or in the other galaxy groups (22%), as most protocluster galaxies reside between the groups. Unobscured star forming galaxies predominantly reside between the protocluster's groups, whereas red galaxies make up a large fraction of the groups' galactic content, so observing the protocluster through only one of these types of galaxies results in a biased view of the protocluster's structure. The structure of the protocluster reveals how much mass is available for the future growth of the cluster and we use the Millennium Simulation, scaled to a Planck cosmology, to predict that Cl 0218.3−0510 will evolve into a 2.7 +3.9 −1.7 × 10 14 M ⊙ cluster by the present day.

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Section: Photometric Redshiftssupporting

confidence: 81%

The structure and evolution of a forming galaxy cluster atz= 1.62

Hatch

Muldrew

Cooke

et al. 2016

Mon. Not. R. Astron. Soc.

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“…In addition, the effects of these variations are relatively degenerate on the colour -M * /L plane (almost parallel to the relation, Bell & de Jong 2001;Bell et al 2003;Szomoru et al 2013), which makes this colour a useful proxy for the M * /L. We derive the relation using the NEWFIRM medium band survey (NMBS) catalogue, which combines existing ground-based and space-based UV to mid-IR data, and new near-IR medium band NEWFIRM data in the AEGIS and COSMOS fields (Whitaker et al 2011). The entire catalogue comprises photometries in 37 (20) bands, high accuracy photometric redshifts derived with EAZY (Brammer, van Dokkum & Coppi 2008) and spectroscopic redshifts for a subset of the sample in COSMOS (AEGIS).…”

Section: Stellar Mass-to-light Ratio -Colour Relationmentioning

confidence: 99%

Sizes, colour gradients and resolved stellar mass distributions for the massive cluster galaxies in XMMUJ2235-2557 atz= 1.39

Chan

Beifiori

Mendel

et al. 2016

Mon. Not. R. Astron. Soc.

137

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(2016) 'Sizes, colour gradients and resolved stellar mass distributions for the massive cluster galaxies in XMMUJ2235-2557 at z = 1.39.', Monthly notices of the Royal Astronomical Society., 458 (3). pp. 3181-3209. Further information on publisher's website: Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTWe analyse the sizes, colour gradients, and resolved stellar mass distributions for 36 massive and passive galaxies in the cluster XMMUJ2235-2557 at z = 1.39 using optical and nearinfrared Hubble Space Telescope imaging. We derive light-weighted Sérsic fits in five HST bands (i 775 , z 850 ,Y 105 , J 125 , H 160 ), and find that the size decreases by ∼ 20% going from i 775 to H 160 band, consistent with recent studies. We then generate spatially resolved stellar mass maps using an empirical relationship between M * /L H 160 and (z 850 − H 160 ) and use these to derive mass-weighted Sérsic fits: the mass-weighted sizes are ∼ 41% smaller than their restframe r-band counterparts compared with an average of ∼ 12% at z ∼ 0. We attribute this evolution to the evolution in the M * /L H 160 and colour gradient. Indeed, as expected, the ratio of mass-weighted to light-weighted size is correlated with the M * /L gradient, but is also mildly correlated with the mass surface density and mass-weighted size. The colour gradients (∇ z−H ) are mostly negative, with a median value of ∼ 0.45 mag dex −1 , twice the local value. The evolution is caused by an evolution in age gradients along the semi-major axis (a), with ∇ age = d log(age)/d log(a) ∼ −0.33, while the survival of weaker colour gradients in old, local galaxies implies that metallicity gradients are also required, with ∇ Z = d log(Z)/d log(a) ∼ −0.2. This is consistent with recent observational evidence for the inside-out growth of passive galaxies at high redshift, and favours a gradual mass growth mechanism, such as minor mergers.

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“…The HAWK-I observations were made between November 2013 and February 2014 as part of the ESO program 092.A-0472 (PI: G. Brammer). The raw HAWK-I images were processed using a custom pipeline, which was originally developed for the NEWFIRM Medium Band Survey (NMBS; Whitaker et al 2011) and later adapted for the ZFOURGE (Spitler et al 2014) and HAWK-I HFF surveys (Brammer, in prep.). The final reduced HAWK-I mosaic has excellent image quality (0.…”

Section: Vlt Imagementioning

confidence: 99%

Frontier Fields: Combining HST, VLT, andSpitzerdata to explore thez~ 8 Universe behind the lensing cluster MACSJ0416.1−2403

Laporte

Streblyanska

Kim

et al. 2015

A&A

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Context. The Hubble Space Telescope (HST) Frontier Fields (HFFs) project started at the end of 2013 with the aim of providing extremely deep images of six massive galaxy clusters. One of the main goals of this program is to push several telescopes to their limits to provide the best current view of the earliest stages of the Universe. The analysis of the initial data has already demonstrated the huge capabilities of the program. Aims. We present a detailed analysis of z ∼ 8 objects behind the HFFs lensing cluster, MACSJ0416.1-2403, combining 0.3−1.6 µm imaging from HST, ground-based K s imaging from VLT HAWK-I, and 3.6 µm and 4.5 µm Spitzer Space Telescope. The images probe to 5σ depths of ≈29 AB for HST, 25.6 AB for HAWK-I, and ≈0.310 and 0.391 µJy at 3.6 and 4.5 µm, respectively. With these datasets, we assess the photometric properties of z ∼ 8 galaxies in this field, as well as their distribution in luminosity, to unprecedented sensitivity. Methods. We applied the classical Lyman break (LB) technique, which combines non detection criteria in bands blueward of the Lyman break at z ∼ 8 and color-selection in bands redward of the break. To avoid contamination by mid-z interlopers, we required a strong break between optical and near-infrared data. We determined the photometric properties of z ∼ 8 selected candidates using spectral energy distribution (SED)-fitting with standard library templates. The luminosity function at z ∼ 8 is computed using a Monte-Carlo method taking advantage of the SED-fitting results. A piece of cautionary information is gleaned from new deep optical photometry of a previously identified z ∼ 8 galaxy in this cluster, which is now firmly detected as a mid-z interloper with a strong ≈1.5 mag Balmer break (between F606W and F125W). Using the SED of this interloper, we estimated the contamination rate of our MACSJ0416.1−2403 sample, and that of previous samples in Abell 2744 that were based on HFF data, we highlight the dangers of pushing the LB technique too close to the photometry limits. Results. Our selection reliably recovers four objects with m F160W ranging from 26.0 to 27.9 AB that are located in modestamplification regions (µ < 2.4). Two of the objects display a secondary break between the IRAC 3.6 µm and 4.5 µm bands, which could be associated to the Balmer break or emission lines at z ∼ 8. The SED-fitting analysis suggests that all of these objects favor high-z solutions with no reliable secondary solutions. The candidates generally have star formation rates around ∼10 M /yr and sizes ranging from 0.2 to 0.5 kpc, which agrees well with previous observations and expectations for objects in the early Universe. The sample size and luminosity distribution are consistent with previous findings.

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THE NEWFIRM MEDIUM-BAND SURVEY: PHOTOMETRIC CATALOGS, REDSHIFTS, AND THE BIMODAL COLOR DISTRIBUTION OF GALAXIES OUT TOz∼ 3

Abstract: The Open University's repository of research publications and other research outputs The newfirm medium-band survey: photometric catalogs, redshifts, and the bimodal color distribution of galaxies out to z 3

Cited by 402 publications

References 68 publications

The structure and evolution of a forming galaxy cluster atz= 1.62

The structure and evolution of a forming galaxy cluster atz= 1.62

Sizes, colour gradients and resolved stellar mass distributions for the massive cluster galaxies in XMMUJ2235-2557 atz= 1.39

Frontier Fields: Combining HST, VLT, andSpitzerdata to explore thez~ 8 Universe behind the lensing cluster MACSJ0416.1−2403

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