THE CLOWES-CAMPUSANO LARGE QUASAR GROUP SURVEY. I.<i>GALEX</i>SELECTED SAMPLE OF LYMAN BREAK GALAXIES AT<i>z</i>∼ 1

Haberzettl, L.; Williger, G. M.; Lauroesch, J. T.; Haines, C. P.; Valls–Gabaud, D.; Harris, Kathryn A.; Koekemoer, Anton M.; Loveday, Jon; Campusano, Luis E.; Clowes, R. G.; Davé, Romeel; Graham, M. J.; Söchting, Ilona K.

doi:10.1088/0004-637x/702/1/506

Cited by 14 publications

(12 citation statements)

References 72 publications

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“…There is evidence for general sheet‐like enhancements of red galaxies with embedded clusters associated with this LQG (Haines et al 2004). Haberzettl et al (2009) similarly find evidence for enhancements of candidates for Lyman‐break galaxies associated with it. A direct association (i.e.…”

Section: Introductionmentioning

confidence: 58%

Two close large quasar groups of size ∼ 350 Mpc at

Clowes¹,

Campusano

Graham

et al. 2011

Monthly Notices of the Royal Astronomical Society

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The Clowes & Campusano large quasar group (LQG) atz = 1.28 has been re-examined using the quasar data from the DR7QSO catalogue of the Sloan Digital Sky Survey. In the 1991 discovery, the LQG impinged on the northern, southern and eastern limits of the survey. In the DR7QSO data, the western, northern and southern boundaries of the LQG remain essentially the same, but an extension eastwards of ∼2 • is indicated. In the DR7QSO data, the LQG has 34 members, withz = 1.28. A new group of 38 members is indicated atz = 1.11 and within ∼2. • 0 of the Clowes & Campusano LQG. The characteristic sizes of these two LQGs, ∼350-400 Mpc, appear to be only marginally consistent with the scale of homogeneity in the concordance cosmology. In addition to their intrinsic interest, these two LQGs provide locations in which to investigate early large-scale structure in galaxies and to identify high-z clusters. A method is presented for assessing the statistical significance and overdensity of groups found by linkage of points.

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Section: Introductionmentioning

confidence: 58%

Two close large quasar groups of size ∼ 350 Mpc at

Clowes¹,

Campusano

Graham

et al. 2011

Monthly Notices of the Royal Astronomical Society

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“…In addition, the UV LF is one of the few galaxy observables which is directly measurable at all epochs using current telescopes. Over the past 20 years, many studies have been devoted to UV LF measurements at high redshifts with z > 3 (Steidel et al 1999;Adelberger & Steidel 2000;Bunker et al 2004;Dickinson et al 2004;Ouchi et al 2004;Yan & Windhorst 2004;Beckwith et al 2006;Yoshida et al 2006;Sawicki & Thompson 2006;Bouwens et al 2007;Iwata et al 2007;McLure et al 2009;Ouchi et al 2009;van der Burg et al 2010;Bradley et al 2012;Cucciati et al 2012;McLure et al 2013;Schenker et al 2013;Atek et al 2014;Schmidt et al 2014a;Atek et al 2015b,a;Bouwens et al 2015;Bowler et al 2015;Finkelstein et al 2015;Ishigaki et al 2015), intermediate redshifts with 1 < z < 3 (Dahlen et al 2007;Reddy et al 2008;Hathi et al 2010;Oesch et al 2010a;Cucciati et al 2012;Sawicki 2012;Parsa et al 2016) including our previous work (Alavi et al 2014, hereafter A14), as well as low redshifts with z < 1 Budavári et al 2005;Wyder et al 2005;Haberzettl et al 2009;Ly et al 2009;…”

Section: Introductionmentioning

confidence: 99%

The Evolution of the Faint End of the Uv Luminosity Function During the Peak Epoch of Star Formation *

Alavi

Siana

Richard

et al. 2016

ApJ

147

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We present a robust measurement of the rest-frame UV luminosity function (LF) and its evolution during the peak epoch of cosmic star formation at 1 < z < 3. We use our deep near ultraviolet imaging from WFC3/UVIS on the Hubble Space Telescope (HST) and existing ACS/WFC and WFC3/IR imaging of three lensing galaxy clusters, Abell 2744 and MACSJ0717 from the Hubble Frontier Field survey and Abell 1689. Combining deep UV imaging and high magnification from strong gravitational lensing, we use photometric redshifts to identify 780 ultra-faint galaxies with M UV < −12.5 AB mag at 1 < z < 3. From these samples, we identified 5 new, faint, multiply imaged systems in A1689. We run a Monte Carlo simulation to estimate the completeness correction and effective volume for each cluster using the latest published lensing models. We compute the rest-frame UV LF and find the best-fit faint-end slopes of α = −1.56 ± 0.04, α = −1.72 ± 0.04 and α = −1.94 ± 0.06 at 1.0 < z < 1.6, 1.6 < z < 2.2 and 2.2 < z < 3.0, respectively. Our results demonstrate that the UV LF becomes steeper from z ∼ 1.3 to z ∼ 2.6 with no sign of a turnover down to M UV = −14 AB mag. We further derive the UV LFs using the Lyman break "dropout" selection and confirm the robustness of our conclusions against different selection methodologies. Because the sample sizes are so large, and extend to such faint luminosities, the statistical uncertainties are quite small, and systematic uncertainties (due to the assumed size distribution, for example), likely dominate. If we restrict our analysis to galaxies and volumes above > 50% completeness in order to minimize these systematics, we still find that the faint-end slope is steep and getting steeper with redshift, though with slightly shallower (less negative) values (α = −1.55 ± 0.06, −1.69 ± 0.07 and −1.79 ± 0.08 for z ∼ 1.3, 1.9 and 2.6, respectively). Finally, we conclude that the faint star-forming galaxies with UV magnitudes of −18.5 < M UV < −12.5 covered in this study, produce the majority (55%-60%) of the unobscured UV luminosity density at 1 < z < 3.

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“…At this redshift, the Lyman break occurs in the UV, which can only be observed from space. First studies using deep images observed by the GALEX satellite obtained samples of LBGs at z ∼ 1 using FUV dropouts (Burgarella et al 2006(Burgarella et al , 2007Haberzettl et al 2009). The majority of LBGs (∼ 75%) at this redshift are disk-dominated, while the rest consist of interacting/merging galaxies (Burgarella et al 2006).…”

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confidence: 99%

GALEX-SELECTED LYMAN BREAK GALAXIES ATz∼ 2: COMPARISON WITH OTHER POPULATIONS

Haberzettl¹,

Williger²,

Lehnert³

et al. 2012

ApJ

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We present results of a search for bright Lyman break galaxies at 1.5 ≤ z ≤ 2.5 in the GOODS-S field using a NUV-dropout technique in combination with color-selection. We derived a sample of 73 LBG candidates. We compare our selection efficiencies to BM/BX-and BzK methods (techniques solely based on ground-based data sets), and find the NUV data to provide greater efficiency for selecting star-forming galaxies. We estimate LBG candidate ages, masses, star formation rates, and extinction from fitting PEGASE synthesis evolution models. We find about 20% of our LBG candidates are comparable to infrared luminous LBGs or sub-millimeter galaxies which are thought to be precursors of massive elliptical galaxies today. Overall, we can show that although BM/BX and BzK methods do identify star-forming galaxies at z ∼ 2, the sample they provide biases against those star-forming galaxies which are more massive and contain sizeable red stellar populations. A true Lyman break criterion at z ∼ 2 is therefore more directly comparable to the populations found at z ∼ 3, which does contain a red fraction.

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THE CLOWES-CAMPUSANO LARGE QUASAR GROUP SURVEY. I.GALEXSELECTED SAMPLE OF LYMAN BREAK GALAXIES ATz∼ 1

Cited by 14 publications

References 72 publications

Two close large quasar groups of size ∼ 350 Mpc at

Two close large quasar groups of size ∼ 350 Mpc at

The Evolution of the Faint End of the Uv Luminosity Function During the Peak Epoch of Star Formation *

GALEX-SELECTED LYMAN BREAK GALAXIES ATz∼ 2: COMPARISON WITH OTHER POPULATIONS

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