The star formation rate of the Universe at<i>z</i>≈ 6 from the<i>Hubble Ultra-Deep Field</i>

Bunker, Andrew J.; Stanway, Elizabeth R.; Ellis, Richard S.; McMahon, R. G.

doi:10.1111/j.1365-2966.2004.08326.x

Cited by 287 publications

(465 citation statements)

References 51 publications

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“…ies that are likely to be the primary driver of reionization (Madau, Haardt & Rees 1999;Bunker et al 2004;Yan & Windhorst 2004;Oesch et al 2009;Kuhlen & FaucherGiguère 2012;Robertson et al 2013). Other possible sources of reionization, such as quasars and annihilating DM, have little observational support and would in any case still require, at a minimum, a sizeable contribution from star-forming galaxies to maintain reionization (Haiman & Loeb 1998;Belikov & Hooper 2009;Willott et al 2010;Fontanot, Cristiani & Vanzella 2012).…”

Section: The Uv-luminosity Function and Reionizationmentioning

confidence: 99%

Galaxy UV-luminosity function and reionization constraints on axion dark matter

Bozek¹,

Marsh²,

Silk³

et al. 2015

Monthly Notices of the Royal Astronomical Society

172

208

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If the dark matter (DM) were composed of axions, then structure formation in the Universe would be suppressed below the axion Jeans scale. Using an analytic model for the halo mass function of a mixed DM model with axions and cold dark matter, combined with the abundance-matching technique, we construct the UV-luminosity function. Axions suppress high-z galaxy formation and the UV-luminosity function is truncated at a faintest limiting magnitude. From the UV-luminosity function, we predict the reionization history of the universe and find that axion DM causes reionization to occur at lower redshift. We search for evidence of axions using the Hubble Ultra Deep Field UV-luminosity function in the redshift range z = 6-10, and the optical depth to reionization, τ , as measured from cosmic microwave background polarization. All probes we consider consistently exclude m a 10 −23 eV from contributing more than half of the DM, with our strongest constraint ruling this model out at more than 8σ significance. In conservative models of reionization a dominant component of DM with m a = 10 −22 eV is in 3σ tension with the measured value of τ , putting pressure on an axion solution to the cusp-core problem. Tension is reduced to 2σ for the axion contributing only half of the DM. A future measurement of the UV-luminosity function in the range z = 10-13 by JWST would provide further evidence for or against m a = 10 −22 eV. Probing still higher masses of m a = 10 −21 eV will be possible using future measurements of the kinetic Sunyaev-Zel'dovich effect by Advanced ACTPol to constrain the time and duration of reionization.

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Section: The Uv-luminosity Function and Reionizationmentioning

confidence: 99%

Galaxy UV-luminosity function and reionization constraints on axion dark matter

Bozek¹,

Marsh²,

Silk³

et al. 2015

Monthly Notices of the Royal Astronomical Society

172

208

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“…Steidel et al 1995Steidel et al , 1999Bunker et al 2004;Dickinson et al 2004;Giavalisco et al 2004;Ouchi et al 2004;A&A 511, A20 (2010) Yoshida et al 2006;Bouwens et al 2003Bouwens et al , 2007McLure et al 2009) i.e. when the Universe was only less than 1 Gyr old.…”

Section: Introductionmentioning

confidence: 99%

Evidence of a fast evolution of the UV luminosity function beyond redshift 6 from a deep HAWK-I survey of the GOODS-S field

Castellano¹,

Fontana²,

Boutsia³

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 first results 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 two Hawk-I pointings on the GOODS South field for a total of ∼32 observing hours, covering ∼90 arcmin 2 . The images reach Y = 26.7 mag for the two fields. We used public ACS images in the z band to select z-dropout galaxies with the colour criteria Z − Y ≥ 1, Y − J < 1.5, and Y − K < 2. The other public data in the UBVRIJK bands are used to reject possible low redshift interlopers. The output has been compared with extensive Monte Carlo simulations to quantify the observational effects of our selection criteria, as well as the effects of photometric errors. Results. We detect 7 high-quality candidates in the magnitude range Y = 25.5−26.7. This interval samples the critical range for M * at z > 6 (M 1500 −19.5 to −21.5). After accounting for the expected incompleteness, we rule out a luminosity function constant from z = 6 to z = 7 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 +2.0 −0.9 × 10 25 erg s −1 Hz −1 Mpc −3 , implying a decrease by a factor 3.5 from z = 6 to z 6.8. On the basis of our findings, we make predictions for the surface densities expected in future surveys, based on ULTRA-VISTA, HST-WFC3, or JWST-NIRCam, evaluating the best observational strategy to maximise their impact.

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“…This is challenging; if the observed flux in the Lyα line is f α,17 (in units of 10 −17 erg s −1 cm −2 ) and its equivalent width is EW (in Å), then the AB-magnitude of the continuum is m AB = 30.4 − 2.5 log f α,17 + 2.5 log(EW/200). For comparison, the Hubble Ultra Deep Field reached an 8 − σ limiting magnitude in the z' filter of z ′ AB = 28.5 (Bunker et al 2004). Detecting both the Lyα line and the continuum is not only desirable for identifying primordial galaxies.…”

Section: Discussionmentioning

confidence: 99%

Continuum Emission by Cooling Clouds

Dijkstra

2008

ApJ

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The collapse of baryons into the center of a host dark matter halo is accompanied by radiation that may be detectable as compact ( < ∼ 10 kpc) UV-continuum and Lyα emission with Lyα luminosities as high as ∼ 10 42 − 10 43 erg s −1 in halos of mass M = 10 11 − 10 12 M ⊙ . We show that the observed equivalent width (EW) of the Lyα line emitted by these cooling clouds is EW < ∼ 400 Å (restframe). These luminosities and EWs are comparable to those detected in narrowband surveys for redshifted Lyα emission. The rest-frame ultraviolet of Lyα emitting cooling clouds radiation may be dominated by two-photon transitions from 2s→1s. The resulting spectrum can distinguish cooling clouds from a broad class of young star forming galaxies.

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The star formation rate of the Universe atz≈ 6 from theHubble Ultra-Deep Field

Cited by 287 publications

References 51 publications

Galaxy UV-luminosity function and reionization constraints on axion dark matter

Galaxy UV-luminosity function and reionization constraints on axion dark matter

Evidence of a fast evolution of the UV luminosity function beyond redshift 6 from a deep HAWK-I survey of the GOODS-S field

Continuum Emission by Cooling Clouds

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