Luminous Lyman Break Galaxies at<i>z</i> &gt; 5 and the Source of Reionization

Lehnert, M. D.; Bremer, M. N.

doi:10.1086/376729

Cited by 124 publications

(202 citation statements)

References 35 publications

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“…The g-dropout number counts are compared to Steidel et al (1999) being consistent for i < 24.5 and suggesting some incompleteness of the older survey for fainter magnitudes. The 13 R-dropouts reported in Lehnert & Bremer (2003) show a similar number density as the r-dropouts in the current study.…”

Section: Redshift Distributionssupporting

confidence: 80%

“…From the simulated catalogues described above we find that the contamination from stars and low-z interlopers can be kept below the 10% level in each magnitude bin (bin-size Δmag = 0.5) by applying a bright cutoff of r > 23 for the u-, i > 23.5 for the g-, and z > 24 for the r-dropouts (for a discussion on how to avoid contaminants in an R-dropout survey by a bright cutoff see also Lehnert & Bremer 2003). These magnitude cuts define our high-quality samples which consist of 17 338 u-, 17 281 g-, and 7038 r-dropouts.…”

Section: Propertiesmentioning

confidence: 90%

See 1 more Smart Citation

CARS: the CFHTLS-Archive-Research Survey

Hildebrandt¹,

Pielorz²,

Erben³

et al. 2009

A&A

170

266

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Aims. We measure the clustering properties for a large samples of u-(z ∼ 3), g-(z ∼ 4), and r-(z ∼ 5) dropouts from the CanadaFrance-Hawaii Telescope Legacy Survey (CFHTLS) Deep fields. Methods. Photometric redshift distributions along with simulations allow us to de-project the angular correlation measurements and estimate physical quantities such as the correlation length, halo mass, galaxy bias, and halo occupation as a function of UV luminosity. Results. For the first time we detect a significant one-halo term in the correlation function at z ∼ 5. The comoving correlation lengths and halo masses of LBGs are found to decrease with decreasing rest-frame UV-luminosity. No significant redshift evolution is found in either quantity. The typical halo mass hosting an LBG is M > ∼ 10 12 h −1 M and the halos are typically occupied by less than one galaxy. Clustering segregation with UV luminosity is clearly observed in the dropout samples, however redshift evolution cannot clearly be disentangled from systematic uncertainties introduced by the redshift distributions. We study a range of possible redshift distributions to illustrate the effect of this choice. Spectroscopy of representative subsamples is required to make high-accuracy absolute measurements of high-z halo masses.

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Section: Redshift Distributionssupporting

confidence: 80%

Section: Propertiesmentioning

confidence: 90%

CARS: the CFHTLS-Archive-Research Survey

Hildebrandt¹,

Pielorz²,

Erben³

et al. 2009

A&A

170

266

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show abstract

“…The expected colors of stars from Pickles (1998) are overplotted as stars. The downward facing triangles at VÀI = 6 are objects which were not detected in V. Lehnert & Bremer (2003) and the dashed line at IÀZ = 1.5 is the selection criteria of Stanway et al (2003). The light solid lines show the expected evolution of Coleman et al (1980) galaxy templates and the Kinney et al (1996) SB2 and SB3 galaxy templates.…”

Section: Number Countsmentioning

confidence: 99%

“…These results suggest that a combination of z ' 1 galaxies and late-type stars are contaminating the z > 5.5 selection. Figure 25 shows that the selection criteria of Lehnert & Bremer (2003) is very likely selecting low-redshift galaxies or stars. We find that 95% of the objects selecting using this Fig.…”

Section: Number Countsmentioning

confidence: 99%

A Deep Wide-Field, Optical, and Near-Infrared Catalog of a Large Area around the Hubble Deep Field North

Capak¹,

Cowie²,

Hu³

et al. 2004

289

223

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We have conducted a deep multicolor imaging survey of 0.2 deg 2 centered on the Hubble Deep Field North (HDF-N). We shall refer to this region as the Hawaii HDF-N. Deep data were collected in U, B, V, R, I, and z 0 bands over the central 0.2 deg 2 and in HK 0 over a smaller region covering the Chandra Deep Field North. The data were reduced to have accurate relative photometry and astrometry across the entire field to facilitate photometric redshifts and spectroscopic follow-up. We have compiled a catalog of 48,858 objects in the central 0.2 deg 2 detected at 5 significance in a 3 00 aperture in either R or z 0 band. Number counts and color-magnitude diagrams are presented and shown to be consistent with previous observations. Using color selection we have measured the density of objects at 3 < z < 7. Our multicolor data indicates that samples selected at z > 5.5 using the Lyman break technique suffer from more contamination by low-redshift objects than suggested by previous studies.

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“…Here we present the analysis of two other pointings ( Fig. 1), chosen for the wealth of deep, public observations previously exploited by other authors to search for z ∼ 4−6 LBGs: the BDF field at RA = 336.98 • , Dec = −35.17 • (Lehnert & Bremer 2003), and the New Technology Telescope Deep Field (NTTDF) at RA = 181.36 • , Dec = −7.72 • (Arnouts et al 1999;Fontana et al 2000Fontana et al , 2003. The total exposure time is 15h49m for BDF and 15h03m for the NTTDF in the Y band.…”

Section: Observationsmentioning

confidence: 99%

The bright end of thez ~ 7UVluminosity function from a wide and deep HAWK-I survey

Castellano

Fontana

Paris

et al. 2010

A&A

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Aims. We perform a deep search for galaxies in the redshift range 6.5 ≤ z ≤ 7.5 to measure the evolution of the number density of luminous galaxies in this redshift range and derive useful constraints on the evolution of their luminosity function. Methods. We present here the second half of an ESO Large Programme, which exploits the unique combination of area and sensitivity provided in the near-IR by the camera Hawk-I at the VLT. We have obtained ∼30 observing hours with Hawk-I in the Y-band of two high galactic latitude fields. We combined the Y-band data with deep J and K Hawk-I observations, as well as FORS1/FORS2 U, B, V, R, I, and Z observations to select z-drop galaxies with Z − Y > 1, no optical detection, and flat Y − J and Y − K colour terms. Results. We detect eight high-quality candidates in the magnitude range Y = 25.5−26.5 that we add to the z-drop candidates selected in two Hawk-I pointings over the GOODS-South field. We use this full sample of 15 objects found in ∼161 arcmin 2 of our survey to constrain the average physical properties and the evolution of the number density of z ∼ 7 LBGs. A stacking analysis yields a best-fit SED with photometric redshift z = 6.85 +0.20 −0.15 and an E(B − V) = 0.05 +0.15 −0.05 . We compute a binned estimate of the z ∼ 7 LF and explore the effects of photometric scatter and model uncertainties on the statistical constraints. After accounting for the expected incompleteness through MonteCarlo simulations, we strengthen our previous finding that a Schechter luminosity function constant from z = 6 to z = 7 is ruled out at a > ∼ 99% confidence level, even including the effects of cosmic variance. For galaxies brighter than M 1500 = −19.0, we derive a luminosity density ρ UV = 1.5 +2.1 −0.8 × 10 25 erg s −1 Hz −1 Mpc −3 , implying a decrease by a factor 3.5 from z = 6 to z 6.8. We find that under standard assumptions, the emission rate of ionizing photons coming from UV bright galaxies is lower by at least a factor of two than the value required for reionization. Finally, we exploit deep Hawk-I J and K band observations to derive an upper limit on the number density of M 1500 < ∼ −22.0 LBGs at z ∼ 8 (Y-dropouts).

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Luminous Lyman Break Galaxies atz > 5 and the Source of Reionization

Cited by 124 publications

References 35 publications

CARS: the CFHTLS-Archive-Research Survey

CARS: the CFHTLS-Archive-Research Survey

A Deep Wide-Field, Optical, and Near-Infrared Catalog of a Large Area around the Hubble Deep Field North

The bright end of thez ~ 7UVluminosity function from a wide and deep HAWK-I survey

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