PROBING VERY BRIGHT END OF GALAXY LUMINOSITY FUNCTION AT
                    <i>z</i>
                    ≳ 7 USING
                    <i>HUBBLE SPACE TELESCOPE</i>
                    PURE PARALLEL OBSERVATIONS

Yan, Haojing; Yan, Lin; Zamojski, Michel; Windhorst, Rogier A.; McCarthy, Patrick J.; Fan, Xiaohui; Röttgering, H. J. A.; Koekemoer, Anton M.; Robertson, Brant; Davé, Romeel; Cai, Zheng

doi:10.1088/2041-8205/728/1/l22

Cited by 96 publications

(108 citation statements)

References 34 publications

(39 reference statements)

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“…1 at Z − Y > 3.6). This relatively bright transient was also identified by McLure et al (2010) and Bunker et al (2010), while Yan et al (2011) showed its possible light curve. Tables 1 and 2 summarize the properties of the z-dropout candidates in the HUDF and ERS field, respectively.…”

Section: Selection Of Z = 7 Candidates: Color Criteriamentioning

confidence: 70%

A critical analysis of the UV luminosity function at redshift ~7 from deep WFC3 data

Grazian

Castellano

Koekemoer

et al. 2011

A&A

105

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Context. The study of the luminosity function (LF) of Lyman break galaxies (LBGs) at z = 7 is very important for ascertaining their role in the reionization of the Universe. These galaxies can be used also to investigate in detail the processes of formation and evolution of galactic structures in the infancy of our Universe. Aims. In this work we plan to perform a detailed and critical analysis of the statistical and systematic errors in the z ∼ 7 LF determination. Methods. To this aim, we have assembled a large sample of candidate LBGs at z ∼ 7 from different surveys, spanning a large variety of areas and depths. In particular, we have combined data from the deep (J < 27.4) and ultradeep (J < 29.2) surveys recently acquired with the new WFC3 NIR camera on HST, over the GOODS-ERS (∼40 sq. arcmin) and the HUDF (∼4 sq. arcmin) fields, with ground based surveys in wide and shallow areas from Hawk-I@VLT and HyperSuprimecam@Subaru. We have used public ACS images in the z band to select z-dropout galaxies, and other public data both in the blue (BVI) and in the red bands to reject possible low-redshift interlopers. We have compared our results with extensive Monte Carlo simulations to quantify the observational effects of our selection criteria as well as the effects of photometric scatter, color selections or the morphology of the candidates. Results. We have found that the number density of faint LBGs at z ∼ 7 is only marginally sensitive to the color selection adopted, but it is strongly dependent from the assumption made on the half light distributions of the simulated galaxies, used to correct the observed sample for incompleteness. The slope of the faint end of the LBGs LF has thus a rather large uncertainty, due to the unknown distribution of physical sizes of the z ∼ 7 LBGs. The implications of these uncertainties have been neglected by previous works. Conclusions. We conclude that galaxies at z ∼ 7 are unable to reionize the Universe unless there is a significant evolution in the clumpiness of the IGM or in the escape fraction of ionising photons or, alternatively, there is a large population of z ∼ 7 LBGs with large physical dimensions but still not detected by the present observations.

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Section: Selection Of Z = 7 Candidates: Color Criteriamentioning

confidence: 70%

A critical analysis of the UV luminosity function at redshift ~7 from deep WFC3 data

Grazian

Castellano

Koekemoer

et al. 2011

A&A

105

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show abstract

“…Some progress in this direction has come from the BoRG and HIPPIES programs (Trenti et al 2011;Yan et al 2011;Bernard et al 2016;Calvi et al 2016), which have uncovered galaxies up to z 8 10 -with M 22.5 UV~-mag (e.g., Calvi et al 2016). A complementary approach comes from ground-based surveys, which allow us to extend the surveyed area to ∼1-100 deg 2 , necessary to minimize the effects of cosmic variance in the systematic search for the brightest objects.…”

Section: = -+mentioning

confidence: 99%

HST Imaging of the Brightest z ∼ 8–9 Galaxies from UltraVISTA: The Extreme Bright End of the UV Luminosity Function

Stefanon

Labbé

Bouwens

et al. 2017

ApJ

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We report on the discovery of three especially bright candidate z 8 phot  galaxies. Five sources were targeted for follow-up with the mag, 5s) NIR data from the UltraVISTA DR3 release, deep ground-based optical imaging from the CFHTLS and Suprime-Cam programs, and Spitzer/IRAC mosaics combining observations from the SMUVS and SPLASH programs. Through the refined spectral energy distributions, which now also include new HyperSuprimeCam g-, r-, i-, z-, and Y-band data, we confirm that 3/5 galaxies have robust z 8.0 8.7phot~-, consistent with the initial selection. The remaining 2/5 galaxies have a nominal z 2 phot~. However, with HST data alone, these objects have increased probability of being at z 9 . We measure mean UV continuum slopes 1.74 0.35 b = - for the three z 8 9 -galaxies, marginally bluer than similarly luminous z 4 6 -in CANDELS but consistent with previous measurements of similarly luminous galaxies at z 7 . The circularized effective radius for our brightest source is 0.9±0.3kpc, similar to previous measurements for a bright z 11 galaxy and bright z 7 galaxies. Finally, enlarging our sample to include the six brightest z 8 LBGs identified over UltraVISTA (i.e., including three other sources from Labbé et al.) we estimate for the first time the volume density of galaxies at the extreme bright end (M 22 UV~-mag) of the z 8 UV luminosity function. Despite this exceptional result, the still large statistical uncertainties do not allow us to discriminate between a Schechter and a double-power-law form.

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“…Wider field near-infrared imaging with the HST Multi-Cycle Treasury Cosmic Assembly Near-infrared Deep Extra-galactic Legacy Survey (CANDELS; Grogin et al 2012;Koekemoer et al 2011) built upon the previous HST ACS/WFC and Spitzer observations of the GOODS, GEMS (Rix et al 2004), COSMOS (Scoville et al 2007), EGS (Davis et al 2007), and UDS (Lawrence et al 2007) extragalactic legacy fields. Thanks to WFC3, detections of z∼8 candidates are now relatively commonplace (e.g., Finkelstein et al 2010;Labbé et al 2010;McLure et al 2011;Yan et al 2011;Bradley et al 2012). The current measurement of the cosmic star formation history extends to less than 500 Myr after the Big Bang (e.g., Ellis et al 2013;Oesch et al 2013Oesch et al , 2016Bouwens et al 2015a;Finkelstein et al 2015; but see Brammer et al 2013;Pirzkal et al 2013), albeit with very small numbers of candidates at z>9.…”

Section: Introductionmentioning

confidence: 99%

The Frontier Fields: Survey Design and Initial Results

Lotz

Koekemoer

Coe

et al. 2017

ApJ

594

574

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What are the faintest distant galaxies we can see with the Hubble Space Telescope (HST) now, before the launch of the James Webb Space Telescope? This is the challenge taken up by the Frontier Fields, a Director's discretionary time campaign with HST and the Spitzer Space Telescope to see deeper into the universe than ever before. The Frontier Fields combines the power of HST and Spitzer with the natural gravitational telescopes of massive highmagnification clusters of galaxies to produce the deepest observations of clusters and their lensed galaxies ever obtained. Six clusters-Abell 2744, MACSJ0416.1-2403, MACSJ0717.5+3745, MACSJ1149.5+2223, Abell S1063, and Abell 370-have been targeted by the HST ACS/WFC and WFC3/IR cameras with coordinated parallel fields for over 840 HST orbits. The parallel fields are the second-deepest observations thus far by HST with 5σ point-source depths of ∼29th ABmag. Galaxies behind the clusters experience typical magnification factors of a few, with small regions magnified by factors of 10-100. Therefore, the Frontier Field cluster HST images achieve intrinsic depths of ∼30-33 mag over very small volumes. Spitzer has obtained over 1000 hr of Director's discretionary imaging of the Frontier Field cluster and parallels in IRAC 3.6 and 4.5 μm bands to 5σ point-source depths of ∼26.5, 26.0 ABmag. We demonstrate the exceptional sensitivity of the HST Frontier Field images to faint high-redshift galaxies, and review the initial results related to the primary science goals.

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PROBING VERY BRIGHT END OF GALAXY LUMINOSITY FUNCTION AT z ≳ 7 USING HUBBLE SPACE TELESCOPE PURE PARALLEL OBSERVATIONS

Cited by 96 publications

References 34 publications

A critical analysis of the UV luminosity function at redshift ~7 from deep WFC3 data

A critical analysis of the UV luminosity function at redshift ~7 from deep WFC3 data

HST Imaging of the Brightest z ∼ 8–9 Galaxies from UltraVISTA: The Extreme Bright End of the UV Luminosity Function

The Frontier Fields: Survey Design and Initial Results

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