Observational Searches for Star-Forming Galaxies at <i>z</i> &gt; 6

Finkelstein, Steven L.

doi:10.1017/pasa.2016.26

Cited by 151 publications

(125 citation statements)

References 300 publications

(723 reference statements)

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“…JWST should extend our knowledge of high-z LFs by pushing one to two magnitudes deeper than current observations with Hubble (e.g. Salvaterra et al 2011;Dayal et al 2013;Shimizu et al 2014;O'Shea et al 2015;Finkelstein 2016;Wilkins et al 2017;Cowley et al 2018;Tacchella et al 2018;Williams et al 2018;Yung et al 2019). This will allow us to push blank field LFs to magnitudes fainter than M UV ∼ > −17; such faint magnitudes are currently accessible only through cluster lensing, and are thus susceptible to large systematic uncertainties including lens modeling and completeness corrections (e.g.…”

Section: Introductionmentioning

confidence: 80%

Properties of reionization-era galaxies from JWST luminosity functions and 21-cm interferometry

Park

Gillet

Mesinger

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Next generation observatories will enable us to study the first billion years of our Universe in unprecedented detail. Foremost among these are 21-cm interferometry with the Hydrogen Epoch of Reionization Arrays (HERA) and the Square Kilometre Array (SKA), and high-z galaxy observations with the James Webb Space Telescope (JWST). Taking a basic galaxy model, in which we allow the star formation rates and ionizing escape fractions to have a power-law dependence on halo mass with an exponential turnover below some threshold, we quantify how observations from these instruments can be used to constrain the astrophysics of high-z galaxies. For this purpose, we generate mock JWST LFs, based on two different hydrodynamical cosmological simulations; these have intrinsic luminosity functions (LFs) which turn over at different scales and yet are fully consistent with present-day observations. We also generate mock 21-cm power spectrum observations, using 1000h observations with SKA1 and a moderate foreground model. Using only JWST data, we predict up to a factor of 2-3 improvement (compared with HST) in the fractional uncertainty of the star formation rate to halo mass relation and the scales at which the LFs peak (i.e. turnover). Most parameters regulating the UV galaxy properties can be constrained at the level of ∼ 10% or better, if either (i) we are able to better characterize systematic lensing uncertainties than currently possible; or (ii) the intrinsic LFs peak at magnitudes brighter than M UV ∼ < −13. Otherwise, improvement over HST-based inference is modest. When combining with upcoming 21-cm observations, we are able to significantly mitigate degeneracies, and constrain all of our astrophysical parameters, even for our most pessimistic assumptions about upcoming JWST LFs. The 21-cm observations also result in an order of magnitude improvement in constraints on the EoR history.

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Section: Introductionmentioning

confidence: 80%

Properties of reionization-era galaxies from JWST luminosity functions and 21-cm interferometry

Park

Gillet

Mesinger

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…This has left luminosity functions highly uncertain at these redshifts, while also hinting at accelerated evolution in the first 600 Myr (Bouwens et al 2012;Oesch et al 2018). Luminosity functions are fairly well constrained at z ∼ 4 − 8 (Bouwens et al 2015;Finkelstein 2016;Kawamata et al 2018). Only recently were constraints placed on all three parameters (φ * , M * , α) of the z ∼ 9 luminosity function (Morishita et al 2018); these results are consistent with either accelerated or smoother (non-accelerated) evolution at z > 8.…”

Section: Luminosity Functions Of Galaxies At the Epoch Of Reionizationmentioning

confidence: 99%

“…But lensing more than compensates for the lost volume by magnifying many more faint galaxies into view whenever luminosity function number counts are steeper than φ ∝ L −2 (Broadhurst et al 1995). This is especially true brightward of L * , for example, AB mag ∼28 at z ∼ 8 (Bradley et al 2012;Finkelstein 2016).…”

Section: Introductionmentioning

confidence: 99%

“…The Grism Lens-Amplified Survey from Space (GLASS; Treu et al 2015) delivered spectroscopic properties and high-redshift confirmations (e.g., Schmidt et al 2016Schmidt et al , 2017. The high-redshift searches in lensing programs complement searches in blank field surveys such as the UDF, CANDELS, and BoRG, constraining luminosity functions from z ∼ 4 − 10 (Bouwens et al 2015;Finkelstein 2016;Oesch et al 2018;Morishita et al 2018).…”

Section: Introductionmentioning

confidence: 99%

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RELICS: Reionization Lensing Cluster Survey

Coe

Salmon

Bradač

et al. 2019

ApJ

192

159

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Large surveys of galaxy clusters with the Hubble and Spitzer Space Telescopes, including CLASH and the Frontier Fields, have demonstrated the power of strong gravitational lensing to efficiently deliver large samples of high-redshift galaxies. We extend this strategy through a wider, shallower survey named RELICS, the Reionization Lensing Cluster Survey. This survey, described here, was designed primarily to deliver the best and brightest high-redshift candidates from the first billion years after the Big Bang. RELICS observed 41 massive galaxy clusters with Hubble and Spitzer at 0.4-1.7µm and 3.0-5.0µm, respectively. We selected 21 clusters based on Planck PSZ2 mass estimates and the other 20 based on observed or inferred lensing strength. Our 188-orbit Hubble Treasury Program obtained the first high-resolution near-infrared images of these clusters to efficiently search for lensed highredshift galaxies. We observed 46 WFC3/IR pointings (∼200 arcmin 2 ) with two orbits divided among four filters (F105W, F125W, F140W, and F160W) and ACS imaging as needed to achieve single-orbit depth in each of three filters (F435W, F606W, and F814W). As previously reported by Salmon et al., we discovered 322 z ∼ 6 − 10 candidates, including the brightest known at z ∼ 6, and the most spatially-resolved distant lensed arc known at z ∼ 10. Spitzer IRAC imaging (945 hours awarded, plus 100 archival) has crucially enabled us to distinguish z ∼ 10 candidates from z ∼ 2 interlopers. For each cluster, two HST observing epochs were staggered by about a month, enabling us to discover 11 supernovae, including 3 lensed supernovae, which we followed up with 20 orbits from our program. We delivered reduced HST images and catalogs of all clusters to the public via MAST and reduced Spitzer images via IRSA. We have also begun delivering lens models of all clusters, to be completed before the JWST GO Cycle 1 call for proposals.

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“…The luminosity functions determined from the XDF galaxies show an exponential decay with increasing redshift until approximately z = 8 (e.g. Koekemoer et al 2013;Bouwens et al 2014;Finkelstein 2016) followed by steeper drop off subject to great uncertainty due to the limited number of observations and difficulty confirming their redshifts. Specifically at both the brightest end (M 1600 ≤ −22) and the faint end (M 1600 ≥ −17), the uncertainties between and within fits grow to a several orders of magnitude differences in the number density of objects (Bowler et al 2015).…”

Section: Eor Galaxy Observationsmentioning

confidence: 99%

First light: exploring the spectra of high-redshift galaxies in the Renaissance Simulations

Barrow

Wise

Norman

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present synthetic observations for the first generations of galaxies in the Universe and make predictions for future deep field observations for redshifts greater than 6. Due to the strong impact of nebular emission lines and the relatively compact scale of H ii regions, high resolution cosmological simulations and a robust suite of analysis tools are required to properly simulate spectra. We created a software pipeline consisting of FSPS, Hyperion, Cloudy and our own tools to generate synthetic IR observations from a fully three-dimensional arrangement of gas, dust, and stars. Our prescription allows us to include emission lines for a complete chemical network and tackle the effect of dust extinction and scattering in the various lines of sight. We provide spectra, 2-D binned photon imagery for both HST and JWST IR filters, luminosity relationships, and emission line strengths for a large sample of high redshift galaxies in the Renaissance Simulations. Our resulting synthetic spectra show high variability between galactic halos with a strong dependence on stellar mass, metallicity, gas mass fraction, and formation history. haloes with the lowest stellar mass have the greatest variability in [O iii]/Hβ, [O iii] and C iii] while haloes with higher masses are seen to show consistency in their spectra and [O iii] equivalent widths (EW) between 1Å and 10Å. Viewing angle accounted for three-fold difference in flux due to the presence of ionized gas channels in a halo. Furthermore, JWST colour plots show a discernible relationship between redshift, colour, and mean stellar age.

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Observational Searches for Star-Forming Galaxies at z > 6

Cited by 151 publications

References 300 publications

Properties of reionization-era galaxies from JWST luminosity functions and 21-cm interferometry

Properties of reionization-era galaxies from JWST luminosity functions and 21-cm interferometry

RELICS: Reionization Lensing Cluster Survey

First light: exploring the spectra of high-redshift galaxies in the Renaissance Simulations

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