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Hubble Space Telescope WFC3/IR images of the promising z > 8.5 candidates from combined UDF12 and earlier data. Each panel is 2.4 arcsec on each side. Top two rows: summed (F125W+F140W+F160W) images for six sources with 8.5 < z
Source publication
We present the results of the deepest search to date for star-forming
galaxies beyond a redshift z~8.5 utilizing a new sequence of near-infrared Wide
Field Camera 3 images of the Hubble Ultra Deep Field. This `UDF12' campaign
completed in September 2012 doubles the earlier exposures with WFC3/IR in this
field and quadruples the exposure in the key...
Contexts in source publication
Context 1
... sources but one (see below) are detected in more than one filter and all are detected with an appropriately-reduced signal/noise in time-split subsets over the collective UDF09 and UDF12 campaigns. Figure 1 shows HST broad-band images for these 7 sources. Their SED fits and redshift probability distributions p(z) are given in Figure 2. Identifications, source photometry and optimum redshifts are summarized in Table 1. ...
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... of our 7 objects (UDF12-3921- 6322, UDF12-4265-7049, UDF12-4344-6547 & UDF12- 3947-8076) have low probabilities of being at z < 4 (1−4%). UDF12-4106-7304 has a ≃ 10% probability for z < 4 and lies close to the diffraction pattern of an adjacent source which may affect the F140W photometry ( Figure 1). UDF12-3895-7114 is the least secure with a 28% proba- bility of lying at z < 4. We discuss UDF-3954-6284 below. ...
Context 3
... is the case for all but one of our UDF12 candidates (Table 1). A major surprise is the non-detection in F140W of UDFj- 30546284 implying a redshift of z=11.90 (Figures 1 and 2). ...
Context 4
... we can use the same methodology to provide an upper limit of ρ UV (z ∼ 10.8) < 9.57 × 10 24 ergs s −1 Hz −1 Mpc −3 ( Figure 4, purple upper limit). Considering the putative z ∼ 12 source, both its mor- phology ( Figure 1) and its luminosity cause us to be cau- tious, particularly given the paucity of other detections beyond z ≃10.5. Nonetheless, since the emission line hy- pothesis is equally difficult to accept (Section 2.1), we es- timated the luminosity density using only the source lumi- nosity (M UV = −19.6AB ...
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Citations
... Over the past decade, deep surveys conducted by the Hubble Space Telescope (HST) discovered thousands of galaxies, significantly improving our understanding of the properties and demographics of ★ E-mail: priyanka.chakraborty@cfa.harvard.edu galaxies up to z ∼ 11 (Ellis et al. 2013;Ishigaki et al. 2015;Finkelstein et al. 2015;McLeod et al. 2016;Bhatawdekar et al. 2019;Bouwens et al. 2021). These surveys included the Hubble Ultra-Deep Field (HUDF, Beckwith et al. 2006), HUDF09 (Bouwens et al. 2011), HUDF12 (Ellis et al. 2013), the HST Great Observatories Origins Deep Survey (GOODS, Giavalisco et al. 2004), and many others (e.g., Scoville et al. 2007;Coe et al. 2019). ...
... galaxies up to z ∼ 11 (Ellis et al. 2013;Ishigaki et al. 2015;Finkelstein et al. 2015;McLeod et al. 2016;Bhatawdekar et al. 2019;Bouwens et al. 2021). These surveys included the Hubble Ultra-Deep Field (HUDF, Beckwith et al. 2006), HUDF09 (Bouwens et al. 2011), HUDF12 (Ellis et al. 2013), the HST Great Observatories Origins Deep Survey (GOODS, Giavalisco et al. 2004), and many others (e.g., Scoville et al. 2007;Coe et al. 2019). However, the limited near-infrared (NIR) coverage of the HST, along with its moderate light-collecting capacity, limited the exploration of the evolution of galaxies at earlier ( > 11) epochs. ...
We report the detection of seven new galaxy candidates with redshift $z$ $>$ 11 within the JWST Advanced Deep Extragalactic Survey (JADES) GOODS-S and GOODS-N fields. These new candidates are detected through meticulous analysis of NIRCam photometry in eight filters spanning a wavelength range of 0.8-5.0 $\mu$m. Photometric redshifts of these galaxy candidates are independently measured utilizing spectral energy distribution (SED) fitting techniques using \texttt{EAZY} and \texttt{BAGPIPES} codes, followed by visual scrutiny. Two of these galaxy candidates are located in GOODS-S field, while the remaining five galaxies are located in GOODS-N field. Our analysis reveals that the stellar masses of these galaxies typically range from log $M_{\ast}$/$M_{\odot}$ = 7.75--8.75. Futhermore, these galaxies are typically young with their mass-weighted ages spanning from 80 to 240 Myr. Their specific star formation rates (sSFR), quantified as $\log (\text{sSFR}/\text{Gyr}$), are measured to vary between $\sim 0.95$ to 1.46. These new galaxy candidates offer a robust sample for probing the physical properties of galaxies within the first few hundred Myr of the history of the Universe. We also analyze the relationship between star formation rate (SFR) and stellar mass ($M_\ast$) within our sample. Using linear regression, our analysis yields a slope of $0.71 \pm 0.12$, which we then compare with results from previous studies. Continued investigation through spectroscopic analysis using JWST/NIRSpec is needed to spectroscopically confirm these high-redshift galaxy candidates and investigate further into their physical properties. We plan to follow up on these candidates with future NIRSpec observations.
... The HDF was later observed with HST's near-infrared (NIR) camera NICMOS (Thompson et al. 1998(Thompson et al. , 1999Dickinson et al. 2000), detecting redshifted optical rest-frame light from galaxies out to z ≈ 3 and extending the wavelength baseline for photometric redshift and spectral energy distribution (SED) analysis. The installation of a more sensitive Advanced Camera for Surveys (ACS; Clampin et al. 2000) during the second Hubble servicing mission motivated a Hubble Ultra Deep Field (HUDF; Beckwith et al. 2006), with subsequent infrared follow-up with NICMOS (Thompson et al. 2005), the HUDF parallel program (Oesch et al. 2007), and later with the more sensitive WFC3 (Kimble et al. 2008) infrared channel (Oesch et al. 2010;Ellis et al. 2013;Illingworth et al. 2013;Koekemoer et al. 2013). The deep infrared data were used to identify and study galaxies with photometric redshifts as high as z ≈ 12 (e.g., Bouwens et al. 2011a;Ellis et al. 2013;Oesch et al. 2013;Bouwens et al. 2016). ...
... The installation of a more sensitive Advanced Camera for Surveys (ACS; Clampin et al. 2000) during the second Hubble servicing mission motivated a Hubble Ultra Deep Field (HUDF; Beckwith et al. 2006), with subsequent infrared follow-up with NICMOS (Thompson et al. 2005), the HUDF parallel program (Oesch et al. 2007), and later with the more sensitive WFC3 (Kimble et al. 2008) infrared channel (Oesch et al. 2010;Ellis et al. 2013;Illingworth et al. 2013;Koekemoer et al. 2013). The deep infrared data were used to identify and study galaxies with photometric redshifts as high as z ≈ 12 (e.g., Bouwens et al. 2011a;Ellis et al. 2013;Oesch et al. 2013;Bouwens et al. 2016). ...
We present the Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey, a deep slitless spectroscopic and imaging Cycle 1 JWST treasury survey designed to constrain feedback mechanisms in low-mass galaxies across cosmic time. NGDEEP targets the Hubble Ultra Deep Field (HUDF) with NIRISS slitless spectroscopy ( f lim , line , 5 σ ≈ 1.2 × 10 ⁻¹⁸ erg s ⁻¹ cm ⁻² ) to measure metallicities and star formation rates (SFRs) for low-mass galaxies through the peak of the cosmic SFR density (0.5 < z < 4). In parallel, NGDEEP targets the HUDF-Par2 parallel field with NIRCam ( m lim , 5 σ = 30.6 − 30.9 ) to discover galaxies to z > 12, constraining the slope of the faint end of the rest-ultraviolet luminosity function. NGDEEP overlaps with the deepest HST Advanced Camera for Surveys optical imaging in the sky, F435W in the HUDF ( m lim , F 435 W = 29.6 ) and F814W in HUDF-Par2 ( m lim , F 814 W = 30 ), making this a premier HST+JWST deep field. As a treasury survey, NGDEEP data are public immediately, and we will rapidly release data products and catalogs in the spirit of previous deep-field initiatives. In this paper we present the NGDEEP survey design, summarize the science goals, and detail plans for the public release of NGDEEP reduced data products.
... Studying early systems in the "Epoch of Reionization" (EoR; z 6) is key to understanding fundamental cosmological questions such as the development of large-scale structure, the processes of cosmic reionization, and the first galaxy formation in the Universe. In the last decades, deep Hubble Space Telescope (HST) surveys provided thousands of EoR galaxies and initial characterization of their stellar component, in terms of unobscured star formation and sizes at rest-frame ultraviolet (UV) wavelengths (e.g., Ellis et al. 2013;Bouwens et al. 2015;Finkelstein et al. 2015;Oesch et al. 2016). ...
We present Atacama Large Millimeter/submillimeter Array (ALMA) deep spectroscopy for a lensed galaxy at z spec = 8.496 with log ( M star / M ⊙ ) ∼ 7.8 whose optical nebular lines and stellar continuum are detected by JWST/NIRSpec and NIRCam Early Release Observations in the field of SMACS J0723.3–7327. Our ALMA spectrum shows [O iii ] 88 μ m and [C ii ] 158 μ m line detections at 4.0 σ and 4.5 σ , respectively. The redshift and position of the [O iii ] line coincide with those of the JWST source, while the [C ii ] line is blueshifted by 90 km s ⁻¹ with a spatial offset of 0.″5 (≈0.5 kpc in the source plane) from the centroid of the JWST source. The NIRCam F444W image, including [O iii ] λ 5007 and H β line emission, spatially extends beyond the stellar components by a factor of >8. This indicates that the z = 8.5 galaxy has already experienced strong outflows as traced by extended [O iii ] λ 5007 and offset [C ii ] emission, which would promote ionizing photon escape and facilitate reionization. With careful slit-loss corrections and the removal of emission spatially outside the galaxy, we evaluate the [O iii ] 88 μ m/ λ 5007 line ratio, and derive the electron density n e by photoionization modeling to be 220 − 130 + 230 cm ⁻³ , which is comparable with those of z ∼ 2–3 galaxies. We estimate an [O iii ] 88 μ m/[C ii ] 158 μ m line ratio in the galaxy of >4, as high as those of known z ∼ 6–9 galaxies. This high [O iii ] 88 μ m/[C ii ] 158 μ m line ratio is generally explained by the high n e as well as the low metallicity ( Z gas / Z ⊙ = 0.04 − 0.02 + 0.02 ), high ionization parameter ( log U > − 2.27 ), and low carbon-to-oxygen abundance ratio (log(C/O) = [−0.52: −0.24]) obtained from the JWST/NIRSpec data; further [C ii ] follow-up observations will constrain the covering fraction of photodissociation regions.
... It has therefore been exciting to see the fruits of these observations: the discovery of many thousands of galaxies at z > 4 ( Bunker et al. 2004Bouwens et al. 2011aBouwens et al. , 2015Bouwens et al. , 2022Lorenzoni et al. 2011;Ellis et al. 2013;McLure et al. 2013;Oesch et al. 2013Oesch et al. , 2014Oesch et al. , 2018Schenker et al. 2013;Finkelstein et al. 2015Finkelstein et al. , 2023Ishigaki et al. 2015;Harikane et al. 2016;McLeod et al. 2016;Morishita et al. 2018;Bridge et al. 2019;Rojas-Ruiz et al. 2020;Bagley et al. 2024). While these sources have been found through multiple methods, the primary method of high-redshift galaxy selection relies on photometry alone. ...
We present a catalog of 717 candidate galaxies at z > 8 selected from 125 square arcmin of NIRCam imaging as part of the JWST Advanced Deep Extragalactic Survey (JADES). We combine the full JADES imaging data set with data from the JWST Extragalactic Medium Survey and First Reionization Epoch Spectroscopic COmplete Survey (FRESCO) along with extremely deep existing observations from Hubble Space Telescope (HST)/Advanced Camera for Surveys (ACS) for a final filter set that includes 15 JWST/NIRCam filters and five HST/ACS filters. The high-redshift galaxy candidates were selected from their estimated photometric redshifts calculated using a template-fitting approach, followed by visual inspection from seven independent reviewers. We explore these candidates in detail, highlighting interesting resolved or extended sources, sources with very red long-wavelength slopes, and our highest-redshift candidates, which extend to z phot ∼ 18. Over 93% of the sources are newly identified from our deep JADES imaging, including 31 new galaxy candidates at z phot > 12. We also investigate potential contamination by stellar objects, and do not find strong evidence from spectral energy distribution fitting that these faint high-redshift galaxy candidates are low-mass stars. Using 42 sources in our sample with measured spectroscopic redshifts from NIRSpec and FRESCO, we find excellent agreement to our photometric redshift estimates, with no catastrophic outliers and an average difference of 〈Δ z = z phot − z spec 〉 = 0.26. These sources comprise one of the most robust samples for probing the early buildup of galaxies within the first few hundred million years of the Universe’s history.
... To accomplish the goal, observations of present galaxies to first galaxies are key to revealing the entire process of galaxy formation. Before the operation of the James Webb Space Telescope (JWST), large telescopes such as the Hubble Space Telescope (HST) have driven observational studies of galaxy formation with millions of high-redshift galaxies and revealed the evolution of the ultraviolet (UV) luminosity function and the cosmic star formation rate (SFR) density at 2 z 10 (e.g., Madau & Dickinson 2014;Bouwens et al. 2015Bouwens et al. , 2021Finkelstein et al. 2015;Ishigaki et al. 2018;Ono et al. 2018;Harikane et al. 2022b), possibly up to z ∼ 11-13 (e.g., Coe et al. 2013;Ellis et al. 2013;Harikane et al. 2022a). Several studies discuss the evolution of the cosmic SFR density at high redshifts being well reproduced by models assuming constant star formation efficiencies (e.g., Bouché et al. 2010;Mason et al. 2015;Harikane et al. 2018Harikane et al. , 2022bOesch et al. 2018;Tacchella et al. 2018;Bouwens et al. 2021), which is motivated by the clustering analysis of galaxies at z ∼ 2-7 (Harikane et al. 2016(Harikane et al. , 2022b and by the abundance matching studies (e.g., Behroozi et al. 2013;Mason et al. 2015;Moster et al. 2018). ...
... Such models predict a rapid decline of the cosmic SFR density at z > 10 due to the decline of the halo number density (Harikane et al. , 2022bOesch et al. 2018). However, some studies using photometric galaxy candidates at z ∼ 10-12 indicate that SFR densities at z > 10 are higher than these models' predictions (Coe et al. 2013;Ellis et al. 2013;McLeod et al. 2016). Such high SFR densities at z > 10 are also suggested by mature stellar populations in galaxies at z ∼ 6-9 (Hashimoto et al. 2018;Mawatari et al. 2020). ...
... mag, corresponding to the SFR of SFR UV = 0.8 M e yr −1 . We also plot estimates based on the photometric samples in the literature (Coe et al. 2013;Ellis et al. 2013;Finkelstein et al. 2015;Bouwens et al. 2020Bouwens et al. , 2023aBouwens et al. , 2023bHarikane et al. 2023a;Donnan et al. 2023a;Pérez-González et al. 2023b). Since some of these studies calculate the SFR densities with different ). ...
We present pure spectroscopic constraints on the UV luminosity functions and cosmic star formation rate (SFR) densities from 25 galaxies at z spec = 8.61–13.20. By reducing the JWST/NIRSpec spectra taken in multiple programs of Early Release Observation, Early Release Science, General Observer, and Director’s Discretionary Time observations with our analysis technique, we independently confirm 16 galaxies at z spec = 8.61–11.40, including new redshift determinations, and a bright interloper at z spec = 4.91 that was claimed as a photometric candidate at z ∼ 16. In conjunction with nine galaxies at redshifts up to z spec = 13.20 in the literature, we make a sample of 25 spectroscopically confirmed galaxies in total and carefully derive the best estimates and lower limits of the UV luminosity functions. These UV luminosity function constraints are consistent with the previous photometric estimates within the uncertainties and indicate mild redshift evolution toward z ∼ 12, showing tensions with some theoretical models of rapid evolution. With these spectroscopic constraints, we obtain firm lower limits of the cosmic SFR densities and spectroscopically confirm a high SFR density at z ∼ 12 beyond the constant star formation efficiency models, which supports earlier claims from the photometric studies. While there are no spectroscopically confirmed galaxies with very large stellar masses violating the ΛCDM model due to the removal of the bright interloper, we confirm star-forming galaxies at z spec = 11–13 with stellar masses much higher than model predictions. Our results indicate possibilities of high star formation efficiency (>5%), a hidden active galactic nucleus, a top-heavy initial mass function (possibly with Population III), and large scatter/variance. Having these successful and unsuccessful spectroscopy results, we suggest observational strategies for efficiently removing low-redshift interlopers for future JWST programs.
... Ho we ver, this search for the highest redshift galaxies in the Hubble Space Telescope ( HST ) + Spitzer era hit a natural redshift frontier (see e.g. Bouwens et al. 2011Bouwens et al. , 2019 MNRAS 527, 11627-11650 (2024) Oesch et al. 2012Oesch et al. , 2018Coe et al. 2013 ;Ellis et al. 2013 ). And this frontier was not because we had already reached the formation epoch of the very first galaxies in the Universe (which we hope to achieve in the JWST era), but rather simply due to running out of sensitive NIR HST filters with which to actually detect these highredshift dropout galaxies (as well as the low resolution of Spitzer ). ...
The presence of evolved stars in high-redshift galaxies can place valuable indirect constraints on the onset of star formation in the Universe. Thus we use PEARLS GTO and public NIRCam photometric data to search for Balmer-break candidate galaxies at 7 < z < 12. We find that our Balmer-break candidates at z ∼ 10.5 tend to be older (115 Myr), have lower inferred [O iii] + Hβ equivalent widths (120 Å), have lower specific star formation rates (6 Gyr−1) and redder UV slopes (β = −1.8) than our control sample of galaxies. However, these trends all become less strong at z ∼ 8, where the F444W filter now probes the strong rest-frame optical emission lines, thus providing additional constraints on the current star formation activity of these galaxies. Indeed, the bursty nature of Epoch of Reionisation galaxies can lead to a disconnect between their current SED profiles and their more extended star formation histories. We discuss how strong emission lines, the cumulative effect of weak emission lines, dusty continua, and AGN can all contribute to the photometric excess seen in the rest-frame optical, thus mimicking the signature of a Balmer break. Additional medium-band imaging will thus be essential to more robustly identify Balmer-break galaxies. However, the Balmer break alone cannot serve as a definitive proxy for the stellar age of galaxies, being complexly dependent on the star-formation history. Ultimately, deep NIRSpec continuum spectroscopy and MIRI imaging will provide the strongest indirect constraints on the formation era of the first galaxies in the Universe, thereby revealing when cosmic dawn breaks.
... Despite its many achievements, the Hubble Space Telescope ( HST ) was unable to advance the search for early galaxies significantly beyond redshifts z 10, due to its limited near -infrared wa velength co v erage ( λ < 1.6 μm; e.g. Coe et al. 2013 ;Ellis et al. 2013 ;Oesch et al. 2016 ). By contrast, the exquisite near/mid-infrared imaging now being provided by the NIRCam instrument on-board the larger and colder JWST has already pushed the redshift frontier out to z 13 (Finkelstein et al. 2022b ;Naidu et al. 2022 ;Robertson et al. 2023 ), with candidate high-redshift galaxies already being unco v ered at redshifts as extreme as z = 16-17 (Harikane et al. 2023b ). ...
... For most of the deep extragalactic imaging surveys performed with HST only F125W and F160W imaging are available for this purpose, at least for the majority of the CANDELS (Grogin et al. 2011 ) area. The addition of the F140W filter for such surv e ys as the HUDF (Beckwith et al. 2006 ;Ellis et al. 2013 ), CLASH (Postman et al. 2012 ), and the Frontier Fields (Lotz et al. 2017 ) w as k ey for selecting z = 9 galaxies in McLeod et al. ( 2015 ), MNRAS 527, 5004-5022 (2024) McLeod, McLure & Dunlop ( 2016 ) as it provided a third filter with high-resolution imaging that probes beyond the Lyman break. The Spitzer space telescope (e.g. ...
... Using this data set, Donnan et al. ( 2023b ) unco v ered a sample of six high-redshift candidates, including three spectroscopically confirmed z > 10 galaxies (Curtis-Lake et al. 2023 ;Robertson et al. 2023 ). Among these is UDFj-39546284, a z 12 galaxy first disco v ered a decade previously with HST imaging (Bouwens et al. 2011 ;Ellis et al. 2013 ). Although we do not search the JEMS data set in this study, we include the six candidates found in Donnan et al. ( 2023b ) in our LF analysis in Section 5 . ...
We present a new determination of the evolving galaxy UV luminosity function (LF) over the redshift range 9.5 < z < 12.5 based on a wide-area (>250 arcmin2) data set of JWST NIRCam near-infrared imaging assembled from thirteen public JWST surveys. Our relatively large-area search allows us to uncover a sample of 61 robust z > 9.5 candidates detected at ≥8σ, and hence place new constraints on the intermediate-to-bright end of the UV LF. When combined with our previous JWST+UltraVISTA results, this allows us to measure the form of the LF over a luminosity range corresponding to four magnitudes (M1500). At these early times we find that the galaxy UV LF is best described by a double power-law function, consistent with results obtained from recent ground-based and early JWST studies at similar redshifts. Our measurements provide further evidence for a relative lack of evolution at the bright-end of the UV LF at z = 9 − 11, but do favour a steep faint-end slope (α ≤ −2). The luminosity-weighted integral of our evolving UV LF provides further evidence for a gradual, smooth (exponential) decline in co-moving star-formation rate density (ρSFR) at least out to z ≃ 12, with our determination of ρSFR(z = 11) lying significantly above the predictions of many theoretical models of galaxy evolution.
... The HUDF has remained the premier field, with contributions too numerous to list but hosting the deepest general-purpose extragalactic images at nearly all common wavelengths. Key examples include very deep HST infrared images, such as from the HUDF09 and HUDF12 program (Ellis et al. 2013;Illingworth et al. 2013), the continued investment of Chandra imaging (e.g., Xue et al. 2016), deep Atacama Large Millimeter/ submillimeter Array observations Walter et al. 2016;Dunlop et al. 2017;Hatsukade et al. 2018), deep Very Large Array imaging (e.g., Rujopakarn et al. 2016), and large investments of spectroscopy, such as with the Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope (e.g., Bacon et al. 2017Bacon et al. , 2021. ...
... With the JWST Advanced Deep Extragalactic Survey (JADES), we aim to continue the legacy of the GOODS-S/ HUDF and GOODS-N/HDF fields, bringing extremely deep high-quality JWST near-infrared imaging and spectroscopy to the field. JADES is a collaboration of the JWST Near-Infrared Camera (NIRCam) and Near-Infrared Spectrograph instrument development teams, pooling about 770 hr of guaranteed time of the mission to the purpose of executing a carefully crafted survey of the fields (Eisenstein et al. 2023). ...
... These are half of the Deep Prime mosaic, covering the HUDF, and a log of the observations is presented in Table 1, which tabulates several parameters used in the Astronomer's Proposal Tool, used to identify the observation, namely, the pointing name, the observation number, the name associated with pointing (TARGPROP), the visit identification, and the starting and ending UT dates of the observation. As described in Eisenstein et al. (2023), observations 7, 10, 15, and 18 form a 2 × 2 overlapping mosaic of pointings, each a nine-point dither of five filter pairs. Observations 11 and 17 add another eight-point dither, building depth in three of the filter pairs in two of the pointings. ...
JWST has revolutionized the field of extragalactic astronomy with its sensitive and high-resolution infrared view of the distant Universe. Adding to the new legacy of JWST observations, we present the first NIRCam imaging data release from the JWST Advanced Deep Extragalactic Survey (JADES), providing nine filters of infrared imaging of ∼25 arcmin ² covering the Hubble Ultra Deep Field and portions of Great Observatories Origins Deep Survey South. Utilizing 87 on-sky dual-filter hours of exposure time, these images reveal the deepest ever near-infrared view of this iconic field. We supply carefully constructed nine-band mosaics of the JADES bands, as well as matching reductions of five additional bands from the JWST Extragalactic Medium-band Survey. Combining with existing Hubble Space Telescope imaging, we provide 23-band space-based photometric catalogs and photometric redshifts for ≈47,500 sources. To promote broad engagement with JADES, we have created an interactive FitsMap website to provide an interface for professional researchers and the public to experience these JWST data sets. Combined with the first JADES NIRSpec data release, these public JADES imaging and spectroscopic data sets provide a new foundation for discoveries of the infrared Universe by the worldwide scientific community.
... The classic Lyman break technique has been effective at assembling large samples of LBGs in the range z ∼ 3 − 5 where the Lyman limit falls at optical wavelengths (e.g., Steidel et al. 2003;Ouchi et al. 2004;Giavalisco et al. 2004;Verma et al. 2007;Iwata et al. 2007;Pentericci et al. 2010;Bielby et al. 2011;Oteo et al. 2013a;Álvarez-Márquez et al. 2016;Malkan et al. 2017), and the use of space-based observatories has extended the Lyman limit detection window as low as z ∼ 1 (e.g., Burgarella et al. 2006;Ly et al. 2009;Basu-Zych et al. 2011;Haberzettl et al. 2012;Oteo et al. 2013bOteo et al. , 2014Hathi et al. 2013). Modified selection methods exploiting the Lyman-α break that dominates the rest-frame UV at redshifts z 5 have successfully isolated large samples of LBGs at redshifts up to z ∼ 10 (e.g., Bouwens et al. 2006Bouwens et al. , 2010Bouwens et al. , 2015McLure et al. 2011;Ellis et al. 2013;Finkelstein 2016;Harikane et al. 2018Harikane et al. , 2022b, and the redshift-dependent line blanketing by the Lyα forest, in combination with the relatively flat rest-frame UV continuum, has been used to select LBGs in the range 1.4 < z < 2.7 at which redshifts the Lyman limit is not observable from the ground (Adelberger et al. 2004;Steidel et al. 2004). ...
High-redshift Lyman break galaxies (LBGs) are efficiently selected in deep images using as few as three broadband filters, and have been shown to have multiple intrinsic and small- to large-scale environmental properties related to Lyman-α. In this paper we demonstrate a statistical relationship between net Lyman-α equivalent width (net Lyα EW) and the optical broadband photometric properties of LBGs at z ∼ 2. We show that LBGs with the strongest net Lyα EWin absorption (aLBGs) and strongest net Lyα EWin emission (eLBGs) separate into overlapping but discrete distributions in (Un – ${\mathcal R}$) colour and ${\mathcal R}$-band magnitude space, and use this segregation behaviour to determine photometric selection criteria by which sub-samples with a desired Lyα spectral type can be selected using data from as few as three broadband optical filters. We propose application of our result to current and future large-area and all-sky photometric surveys that will select hundreds of millions of LBGs across many hundreds to thousands of Mpc, and for which spectroscopic follow-up to obtain Lyα spectral information is prohibitive. To this end, we use spectrophotometry of composite spectra derived from a sample of 798 LBGs divided into quartiles on the basis of net Lyα EWto calculate selection criteria for the isolation of Lyα-absorbing and Lyα-emitting populations of z ∼ 3 LBGs using ugri broadband photometric data from the Vera Rubin Observatory Legacy Survey of Space and Time (LSST).
... The iconic Hubble Deep Field (Williams et al. 1996; Thompson et al. 1999;Dickinson 2000) resulted in the detection of galaxies out to z ∼ 3 using its deep near-infrared (NIR) imaging, while the succeeding Hubble Ultra Deep Field (HUDF) Advanced Camera for Surveys (ACS) imaging (Beckwith et al. 2006) and its WFC3 NIR addition (HUDF09; Oesch et al. 2010) led to the discovery of hundreds of galaxies at z > 6 ( Bouwens et al. 2004Bouwens et al. , 2006Bouwens et al. , 2010Bunker et al. 2004Bunker et al. , 2010Finkelstein et al. 2010;McLure et al. 2010;Oesch et al. 2010). The combination of various legacy HST deep-field data has enabled constraints of galaxy evolution up to z ; 10 (e.g., Ellis et al. 2013;Bouwens et al. 2015Bouwens et al. , 2021Finkelstein et al. 2015). While early public JWST imaging data sets from Early Release Science programs Finkelstein et al. 2023) have probed higher redshifts than HST due to their redder wavelength coverage, they have yet to exceed the depths reached by the HST HUDF. ...
We present a robust sample of very high redshift galaxy candidates from the first epoch of JWST/NIRCam imaging from the Next Generation Deep Extragalactic Exploratory Public (NGDEEP) survey. The NGDEEP NIRCam imaging, spanning 9.7 arcmin ² in the Hubble Ultra Deep Field Parallel Field 2, reaches m = 30.4 (5 σ , point-source, 2″ diameter apertures corrected to total) in F277W, making it the deepest public JWST GO imaging data set to date. We describe our detailed data reduction process of the six-filter broadband JWST/NIRCam imaging, incorporating custom corrections for systematic effects to produce high-quality calibrated images. Using robust photometric redshift selection criteria, we identify a sample of 38 z ≳ 9 galaxy candidates. These objects span a redshift range of z = 8.5–15.8 and apparent magnitudes of m F277W = 27–30.5 AB mag, reaching ∼1.5 mag deeper than previous public JWST imaging surveys. We calculate the rest-frame ultraviolet luminosity function at z ∼ 9 and 11 and present a new measurement of the luminosity function faint-end slope at z ∼ 11. We find a faint-end slope of α = −2.5 ± 0.4 and −2.2 ± 0.2 at z ∼ 9 and 11, respectively. This is consistent with no significant evolution in the faint-end slope and number density from z = 9 to 11. Comparing our results with theoretical predictions, we find that some models produce better agreement at the faint end than the bright end. These results will help to constrain how stellar feedback impacts star formation at these early epochs.
