The UDF05 Follow‐up of the Hubble Ultra Deep Field. I. The Faint‐End Slope of the Lyman Break Galaxy Population at<i>z</i>∼ 5

Oesch, Pascal; Stiavelli, M.; Carollo, C. M.; Bergeron, Louis; Koekemoer, Anton M.; Lucas, Ray A.; Pavlovsky, Cheryl; Trenti, Michele; Lilly, S. J.; Beckwith, S.; Dahlén, T.; Ferguson, Harry; Gardner, Jonathan P.; Lacey, Cedric G.; Mobasher, Bahram; Panagia, N.; Rix, H. W.

doi:10.1086/522423

Cited by 104 publications

(149 citation statements)

References 59 publications

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“…We see the same trend Oesch et al 2007,2010a,2010bArnouts et al 2005 Hathi et.al 2010Sawicki 2012Bradley et.al 2012Schenker et.al 2013 Figure 9. Evolution of the faint-end slope with redshift.…”

Section: Evolution Of Dust In Faint Star-forming Galaxiessupporting

confidence: 69%

ULTRA-FAINT ULTRAVIOLET GALAXIES ATz∼ 2 BEHIND THE LENSING CLUSTER A1689: THE LUMINOSITY FUNCTION, DUST EXTINCTION, AND STAR FORMATION RATE DENSITY

Alavi

Siana

Richard

et al. 2013

ApJ

134

183

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We have obtained deep ultraviolet imaging of the lensing cluster A1689 with the WFC3/UVIS camera onboard the Hubble Space Telescope in the F275W (30 orbits) and F336W (4 orbits) filters. These images are used to identify z ∼ 2 star-forming galaxies via their Lyman break, in the same manner that galaxies are typically selected at z 3. Because of the unprecedented depth of the images and the large magnification provided by the lensing cluster, we detect galaxies 100× fainter than previous surveys at this redshift. After removing all multiple images, we have 58 galaxies in our sample in the range −19.5 < M 1500 < −13 AB mag. Because the mass distribution of A1689 is well constrained, we are able to calculate the intrinsic sensitivity of the observations as a function of source plane position, allowing for accurate determinations of effective volume as a function of luminosity. We fit the faint-end slope of the luminosity function to be α = −1.74 ± 0.08, which is consistent with the values obtained for 2.5 < z < 6. Notably, there is no turnover in the luminosity function down to M 1500 = −13 AB mag. We fit the UV spectral slopes with photometry from existing Hubble optical imaging. The observed trend of increasingly redder slopes with luminosity at higher redshifts is observed in our sample, but with redder slopes at all luminosities and average reddening of E(B − V ) = 0.15 mag. We assume the stars in these galaxies are metal poor (0.2 Z ) compared to their brighter counterparts (Z ), resulting in bluer assumed intrinsic UV slopes and larger derived values for dust extinction. The total UV luminosity density at z ∼ 2 is 4.31 +0.68 −0.60 × 10 26 erg s −1 Hz −1 Mpc −3 , more than 70% of which is emitted by galaxies in the luminosity range of our sample. Finally, we determine the global star formation rate density from UV-selected galaxies at z ∼ 2 (assuming a constant dust extinction correction of 4.2 over all luminosities and a Kroupa initial mass function) of 0.148 +0.023 −0.020 M yr −1 Mpc −3 , significantly higher than previous determinations because of the additional population of fainter galaxies and the larger dust correction factors.

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Section: Evolution Of Dust In Faint Star-forming Galaxiessupporting

confidence: 69%

ULTRA-FAINT ULTRAVIOLET GALAXIES ATz∼ 2 BEHIND THE LENSING CLUSTER A1689: THE LUMINOSITY FUNCTION, DUST EXTINCTION, AND STAR FORMATION RATE DENSITY

Alavi

Siana

Richard

et al. 2013

ApJ

134

183

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“…These six new "blank fields" are comparable in depth to the HUDF parallel fields (Oesch et al 2007), and triple the area of unlensed fields observed by HST to a depth of ∼29th ABmag. The background volumes lensed by the clusters are much smaller than those probed by unlensed fields.…”

Section: Science Goals and Strategysupporting

confidence: 53%

The Frontier Fields: Survey Design and Initial Results

Lotz

Koekemoer

Coe

et al. 2017

ApJ

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611

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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“…These fields include the HUDF (Beckwith et al 2006) and two HUDF05 flanking fields (Oesch et al 2007). These observations are primarily of use in establishing the distribution of UV-continuum slopes β for very faint z ∼ 4-7 galaxies.…”

Section: Hudf09 Observationsmentioning

confidence: 99%

UV-CONTINUUM SLOPES ATz∼ 4-7 FROM THE HUDF09+ERS+CANDELS OBSERVATIONS: DISCOVERY OF A WELL-DEFINED UV COLOR-MAGNITUDE RELATIONSHIP FORz⩾ 4 STAR-FORMING GALAXIES

Bouwens¹,

Illingworth²,

Oesch³

et al. 2012

ApJ

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448

601

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Ultra-deep Advanced Camera for Surveys (ACS) and WFC3/IR HUDF+HUDF09 data, along with the wide-area GOODS+ERS+CANDELS data over the CDF-S GOODS field, are used to measure UV colors, expressed as the UV-continuum slope β, of star-forming galaxies over a wide range of luminosity (0.1L * z=3 to 2L * z=3 ) at high redshift (z ∼ 7 to z ∼ 4). β is measured using all ACS and WFC3/IR passbands uncontaminated by Lyα and spectral breaks. Extensive tests show that our β measurements are only subject to minimal biases. Using a different selection procedure, Dunlop et al. recently found large biases in their β measurements. To reconcile these different results, we simulated both approaches and found that β measurements for faint sources are subject to large biases if the same passbands are used both to select the sources and to measure β. High-redshift galaxies show a well-defined restframe UV color-magnitude (CM) relationship that becomes systematically bluer toward fainter UV luminosities. No evolution is seen in the slope of the UV CM relationship in the first 1.5 Gyr, though there is a small evolution in the zero point to redder colors from z ∼ 7 to z ∼ 4. This suggests that galaxies are evolving along a well-defined sequence in the L UV -color (β) plane (a "star-forming sequence"?). Dust appears to be the principal factor driving changes in the UV color β with luminosity. These new larger β samples lead to improved dust extinction estimates at z ∼ 4-7 and confirm that the extinction is essentially zero at low luminosities and high redshifts. Inclusion of the new dust extinction results leads to (1) excellent agreement between the star formation rate (SFR) density at z ∼ 4-8 and that inferred from the stellar mass density; and (2) to higher specific star formation rates (SSFRs) at z 4, suggesting that the SSFR may evolve modestly (by factors of ∼2) from z ∼ 4-7 to z ∼ 2.

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The UDF05 Follow‐up of the Hubble Ultra Deep Field. I. The Faint‐End Slope of the Lyman Break Galaxy Population atz∼ 5

Cited by 104 publications

References 59 publications

ULTRA-FAINT ULTRAVIOLET GALAXIES ATz∼ 2 BEHIND THE LENSING CLUSTER A1689: THE LUMINOSITY FUNCTION, DUST EXTINCTION, AND STAR FORMATION RATE DENSITY

ULTRA-FAINT ULTRAVIOLET GALAXIES ATz∼ 2 BEHIND THE LENSING CLUSTER A1689: THE LUMINOSITY FUNCTION, DUST EXTINCTION, AND STAR FORMATION RATE DENSITY

The Frontier Fields: Survey Design and Initial Results

UV-CONTINUUM SLOPES ATz∼ 4-7 FROM THE HUDF09+ERS+CANDELS OBSERVATIONS: DISCOVERY OF A WELL-DEFINED UV COLOR-MAGNITUDE RELATIONSHIP FORz⩾ 4 STAR-FORMING GALAXIES

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