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1. Dusty Starbursts Masquerading as Ultra-high Redshift Galaxies in JWST CEERS Observations

Author

Zavala, JA, Buat, V, Casey, CM, Finkelstein, SL, Burgarella, D, Bagley, MB, Ciesla, L, Daddi, E, Dickinson, M, Ferguson, HC, Franco, M, Jiménez-Andrade, EF, Kartaltepe, JS, Koekemoer, AM, Bail, AL, Murphy, EJ, Papovich, C, Tacchella, S, Wilkins, SM, Aretxaga, I, Behroozi, P, Champagne, JB, Fontana, A, Giavalisco, M, Grazian, A, Grogin, NA, Kewley, LJ, Kocevski, DD, Kirkpatrick, A, Lotz, JM, Pentericci, L, Pérez-González, PG, Pirzkal, N, Ravindranath, S, Somerville, RS, Trump, Yang, G, Aaron Yung, LY, Almaini, O, Amorín, RO, Annunziatella, M, Haro, PA, Backhaus, BE, Barro, G, Bell, EF, Bhatawdekar, R, Bisigello, L, Buitrago, F, Calabrò, A, Castellano, M, Chávez Ortiz, ÓA, Chworowsky, K, Cleri, NJ, Cohen, SH, Cole, JW, Cooke, KC, Cooper, MC, Cooray, AR, Costantin, L, Cox, IG, Croton, D, Davé, R, Vega, ADL, Dekel, A, Elbaz, D, Estrada-Carpenter, V, Fernández, V, Finkelstein, KD, Freundlich, J, Fujimoto, S, García-Argumánez, Á, Gardner, JP, Gawiser, E, Gómez-Guijarro, C, Guo, Y, Hamilton, TS, Hathi, NP, Holwerda, BW, Hirschmann, M, Huertas-Company, M, Hutchison, TA, Iyer, KG, Jaskot, AE, Jha, SW, Jogee, S, Juneau, S, Jung, I, Kassin, SA, Kurczynski, P, Larson, RL, Leung, GCK, Long, AS, Lucas, RA, Magnelli, B, Mantha, KB, Matharu, J, McGrath, EJ, McIntosh, DH, Medrano, A, Merlin, E, Zavala, JA [0000-0002-7051-1100], Buat, V [0000-0003-3441-903X], Casey, CM [0000-0002-0930-6466], Finkelstein, SL [0000-0001-8519-1130], Burgarella, D [0000-0002-4193-2539], Bagley, MB [0000-0002-9921-9218], Ciesla, L [0000-0003-0541-2891], Daddi, E [0000-0002-3331-9590], Dickinson, M [0000-0001-5414-5131], Ferguson, HC [0000-0001-7113-2738], Franco, M [0000-0002-3560-8599], Jiménez-Andrade, EF [0000-0002-2640-5917], Kartaltepe, JS [0000-0001-9187-3605], Koekemoer, AM [0000-0002-6610-2048], Bail, AL [0000-0002-9466-2763], Murphy, EJ [0000-0001-7089-7325], Papovich, C [0000-0001-7503-8482], Tacchella, S [0000-0002-8224-4505], Wilkins, SM [0000-0003-3903-6935], Aretxaga, I [0000-0002-6590-3994], Behroozi, P [0000-0002-2517-6446], Champagne, JB [0000-0002-6184-9097], Fontana, A [0000-0003-3820-2823], Giavalisco, M [0000-0002-7831-8751], Grazian, A [0000-0002-5688-0663], Grogin, NA [0000-0001-9440-8872], Kewley, LJ [0000-0001-8152-3943], Kocevski, DD [0000-0002-8360-3880], Kirkpatrick, A [0000-0002-5537-8110], Lotz, JM [0000-0003-3130-5643], Pentericci, L [0000-0001-8940-6768], Pérez-González, PG [0000-0003-4528-5639], Pirzkal, N [0000-0003-3382-5941], Ravindranath, S [0000-0002-5269-6527], Somerville, RS [0000-0002-6748-6821], Trump, JR [0000-0002-1410-0470], Yang, G [0000-0001-8835-7722], Aaron Yung, LY [0000-0003-3466-035X], Almaini, O [0000-0001-9328-3991], Amorín, RO [0000-0001-5758-1000], Annunziatella, M [0000-0002-8053-8040], Haro, PA [0000-0002-7959-8783], Backhaus, BE [0000-0001-8534-7502], Barro, G [0000-0001-6813-875X], Bell, EF [0000-0002-5564-9873], Bhatawdekar, R [0000-0003-0883-2226], Bisigello, L [0000-0003-0492-4924], Buitrago, F [0000-0002-2861-9812], Calabrò, A [0000-0003-2536-1614], Castellano, M [0000-0001-9875-8263], Chávez Ortiz, ÓA [0000-0003-2332-5505], Chworowsky, K [0000-0003-4922-0613], Cleri, NJ [0000-0001-7151-009X], Cohen, SH [0000-0003-3329-1337], Cole, JW [0000-0002-6348-1900], Cooke, KC [0000-0002-2200-9845], Cooper, MC [0000-0003-1371-6019], Cooray, AR [0000-0002-3892-0190], Costantin, L [0000-0001-6820-0015], Cox, IG [0000-0002-1803-794X], Croton, D [0000-0002-5009-512X], Davé, R [0000-0003-2842-9434], Vega, ADL [0000-0002-6219-5558], Dekel, A [0000-0003-4174-0374], Elbaz, D [0000-0002-7631-647X], Estrada-Carpenter, V [0000-0001-8489-2349], Fernández, V [0000-0003-0531-5450], Finkelstein, KD [0000-0003-0792-5877], Freundlich, J [0000-0002-5245-7796], Fujimoto, S [0000-0001-7201-5066], García-Argumánez, Á [0000-0002-8365-5525], Gardner, JP [0000-0003-2098-9568], Gawiser, E [0000-0003-1530-8713], Gómez-Guijarro, C [0000-0002-4085-9165], Guo, Y [0000-0002-4162-6523], Hamilton, TS [0000-0002-9753-1769], Hathi, NP [0000-0001-6145-5090], Holwerda, BW [0000-0002-4884-6756], Hirschmann, M [0000-0002-3301-3321], Huertas-Company, M [0000-0002-1416-8483], Hutchison, TA [0000-0001-6251-4988], Iyer, KG [0000-0001-9298-3523], Jaskot, AE [0000-0002-6790-5125], Jha, SW [0000-0001-8738-6011], Jogee, S [0000-0002-1590-0568], Juneau, S [0000-0002-0000-2394], Jung, I [0000-0003-1187-4240], Kassin, SA [0000-0002-3838-8093], Kurczynski, P [0000-0002-8816-5146], Larson, RL [0000-0003-2366-8858], Leung, GCK [0000-0002-9393-6507], Long, AS [0000-0002-7530-8857], Lucas, RA [0000-0003-1581-7825], Magnelli, B [0000-0002-6777-6490], Matharu, J [0000-0002-7547-3385], McGrath, EJ [0000-0001-8688-2443], Merlin, E [0000-0001-6870-8900], and Apollo - University of Cambridge Repository

Subjects
5101 Astronomical Sciences, 5109 Space Sciences, 51 Physical Sciences, Galaxies and Cosmology
Abstract

Lyman-break galaxy (LBG) candidates at z ≳ 10 are rapidly being identified in James Webb Space Telescope (JWST)/NIRCam observations. Due to the (redshifted) break produced by neutral hydrogen absorption of rest-frame UV photons, these sources are expected to drop out in the bluer filters while being well detected in redder filters. However, here we show that dust-enshrouded star-forming galaxies at lower redshifts (z ≲ 7) may also mimic the near-infrared (near-IR) colors of z > 10 LBGs, representing potential contaminants in LBG candidate samples. First, we analyze CEERS-DSFG-1, a NIRCam dropout undetected in the F115W and F150W filters but detected at longer wavelengths. Combining the JWST data with (sub)millimeter constraints, including deep NOEMA interferometric observations, we show that this source is a dusty star-forming galaxy (DSFG) at z ≈ 5.1. We also present a tentative 2.6σ SCUBA-2 detection at 850 μm around a recently identified z ≈ 16 LBG candidate in the same field and show that, if the emission is real and associated with this candidate, the available photometry is consistent with a z ∼ 5 dusty galaxy with strong nebular emission lines despite its blue near-IR colors. Further observations on this candidate are imperative to mitigate the low confidence of this tentative submillimeter emission and its positional uncertainty. Our analysis shows that robust (sub)millimeter detections of NIRCam dropout galaxies likely imply z ∼ 4–6 redshift solutions, where the observed near-IR break would be the result of a strong rest-frame optical Balmer break combined with high dust attenuation and strong nebular line emission, rather than the rest-frame UV Lyman break. This provides evidence that DSFGs may contaminate searches for ultra-high redshift LBG candidates from JWST observations.

Published
2023

2. A Long Time Ago in a Galaxy Far, Far Away: A Candidate z ~ 12 Galaxy in Early JWST CEERS Imaging

Author

Finkelstein, SL, Bagley, MB, Haro, PA, Dickinson, M, Ferguson, HC, Kartaltepe, JS, Papovich, C, Burgarella, D, Kocevski, DD, Huertas-Company, M, Iyer, KG, Koekemoer, AM, Larson, RL, Pérez-González, PG, Rose, C, Tacchella, S, Wilkins, SM, Chworowsky, K, Medrano, A, Morales, AM, Somerville, RS, Aaron Yung, LY, Fontana, A, Giavalisco, M, Grazian, A, Grogin, NA, Kewley, LJ, Kirkpatrick, A, Kurczynski, P, Lotz, JM, Pentericci, L, Pirzkal, N, Ravindranath, S, Ryan, RE, Trump, Yang, G, Almaini, O, Amorín, RO, Annunziatella, M, Backhaus, BE, Barro, G, Behroozi, P, Bell, EF, Bhatawdekar, R, Bisigello, L, Bromm, V, Buat, V, Buitrago, F, Calabrò, A, Casey, CM, Castellano, M, Chávez Ortiz, ÓA, Ciesla, L, Cleri, NJ, Cohen, SH, Cole, JW, Cooke, KC, Cooper, MC, Cooray, AR, Costantin, L, Cox, IG, Croton, D, Daddi, E, Davé, R, De La Vega, A, Dekel, A, Elbaz, D, Estrada-Carpenter, V, Faber, SM, Fernández, V, Finkelstein, KD, Freundlich, J, Fujimoto, S, García-Argumánez, Á, Gardner, JP, Gawiser, E, Gómez-Guijarro, C, Guo, Y, Hamblin, K, Hamilton, TS, Hathi, NP, Holwerda, BW, Hirschmann, M, Hutchison, TA, Jaskot, AE, Jha, SW, Jogee, S, Juneau, S, Jung, I, Kassin, SA, Le Bail, A, Leung, GCK, Lucas, RA, Magnelli, B, Mantha, KB, Matharu, J, McGrath, EJ, McIntosh, DH, Merlin, E, Mobasher, B, Finkelstein, SL [0000-0001-8519-1130], Bagley, MB [0000-0002-9921-9218], Haro, PA [0000-0002-7959-8783], Dickinson, M [0000-0001-5414-5131], Ferguson, HC [0000-0001-7113-2738], Kartaltepe, JS [0000-0001-9187-3605], Papovich, C [0000-0001-7503-8482], Burgarella, D [0000-0002-4193-2539], Kocevski, DD [0000-0002-8360-3880], Huertas-Company, M [0000-0002-1416-8483], Iyer, KG [0000-0001-9298-3523], Koekemoer, AM [0000-0002-6610-2048], Larson, RL [0000-0003-2366-8858], Pérez-González, PG [0000-0003-4528-5639], Rose, C [0000-0002-8018-3219], Tacchella, S [0000-0002-8224-4505], Wilkins, SM [0000-0003-3903-6935], Chworowsky, K [0000-0003-4922-0613], Morales, AM [0000-0003-4965-0402], Somerville, RS [0000-0002-6748-6821], Aaron Yung, LY [0000-0003-3466-035X], Fontana, A [0000-0003-3820-2823], Giavalisco, M [0000-0002-7831-8751], Grazian, A [0000-0002-5688-0663], Grogin, NA [0000-0001-9440-8872], Kewley, LJ [0000-0001-8152-3943], Kirkpatrick, A [0000-0002-1306-1545], Kurczynski, P [0000-0002-8816-5146], Lotz, JM [0000-0003-3130-5643], Pentericci, L [0000-0001-8940-6768], Pirzkal, N [0000-0003-3382-5941], Ravindranath, S [0000-0002-5269-6527], Ryan, RE [0000-0003-0894-1588], Trump, JR [0000-0002-1410-0470], Yang, G [0000-0001-8835-7722], Almaini, O [0000-0001-9328-3991], Amorín, RO [0000-0001-5758-1000], Annunziatella, M [0000-0002-8053-8040], Backhaus, BE [0000-0001-8534-7502], Behroozi, P [0000-0002-2517-6446], Bell, EF [0000-0002-5564-9873], Bhatawdekar, R [0000-0003-0883-2226], Bisigello, L [0000-0003-0492-4924], Bromm, V [0000-0003-0212-2979], Buat, V [0000-0003-3441-903X], Buitrago, F [0000-0002-2861-9812], Calabrò, A [0000-0003-2536-1614], Casey, CM [0000-0002-0930-6466], Castellano, M [0000-0001-9875-8263], Chávez Ortiz, ÓA [0000-0003-2332-5505], Ciesla, L [0000-0003-0541-2891], Cleri, NJ [0000-0001-7151-009X], Cohen, SH [0000-0003-3329-1337], Cole, JW [0000-0002-6348-1900], Cooke, KC [0000-0002-2200-9845], Cooper, MC [0000-0003-1371-6019], Cooray, AR [0000-0002-3892-0190], Costantin, L [0000-0001-6820-0015], Cox, IG [0000-0002-1803-794X], Croton, D [0000-0002-5009-512X], Daddi, E [0000-0002-3331-9590], Davé, R [0000-0003-2842-9434], De La Vega, A [0000-0002-6219-5558], Dekel, A [0000-0003-4174-0374], Elbaz, D [0000-0002-7631-647X], Estrada-Carpenter, V [0000-0001-8489-2349], Fernández, V [0000-0003-0531-5450], Finkelstein, KD [0000-0003-0792-5877], Freundlich, J [0000-0002-5245-7796], Fujimoto, S [0000-0001-7201-5066], García-Argumánez, Á [0000-0002-8365-5525], Gardner, JP [0000-0003-2098-9568], Gawiser, E [0000-0003-1530-8713], Gómez-Guijarro, C [0000-0002-4085-9165], Guo, Y [0000-0002-4162-6523], Hamblin, K [0000-0002-6292-4589], Hamilton, TS [0000-0002-9753-1769], Hathi, NP [0000-0001-6145-5090], Holwerda, BW [0000-0002-4884-6756], Hirschmann, M [0000-0002-3301-3321], Hutchison, TA [0000-0001-6251-4988], Jaskot, AE [0000-0002-6790-5125], Jha, SW [0000-0001-8738-6011], Jogee, S [0000-0002-1590-0568], Juneau, S [0000-0002-0000-2394], Jung, I [0000-0003-1187-4240], Kassin, SA [0000-0002-3838-8093], Le Bail, A [0000-0002-9466-2763], Leung, GCK [0000-0002-9393-6507], Lucas, RA [0000-0003-1581-7825], Magnelli, B [0000-0002-6777-6490], Matharu, J [0000-0002-7547-3385], McGrath, EJ [0000-0001-8688-2443], Merlin, E [0000-0001-6870-8900], and Apollo - University of Cambridge Repository

Subjects
5101 Astronomical Sciences, 5109 Space Sciences, 51 Physical Sciences, Galaxies and Cosmology
Abstract

We report the discovery of a candidate galaxy with a photo-z of z ∼ 12 in the first epoch of the James Webb Space Telescope (JWST) Cosmic Evolution Early Release Science Survey. Following conservative selection criteria, we identify a source with a robust z phot = 11.8 − 0.2 + 0.3 (1σ uncertainty) with m F200W = 27.3 and ≳7σ detections in five filters. The source is not detected at λ < 1.4 μm in deep imaging from both Hubble Space Telescope (HST) and JWST and has faint ∼3σ detections in JWST F150W and HST F160W, which signal a Lyα break near the red edge of both filters, implying z ∼ 12. This object (Maisie’s Galaxy) exhibits F115W − F200W > 1.9 mag (2σ lower limit) with a blue continuum slope, resulting in 99.6% of the photo-z probability distribution function favoring z > 11. All data-quality images show no artifacts at the candidate’s position, and independent analyses consistently find a strong preference for z > 11. Its colors are inconsistent with Galactic stars, and it is resolved (r h = 340 ± 14 pc). Maisie’s Galaxy has log M */M ⊙ ∼ 8.5 and is highly star-forming (log sSFR ∼ −8.2 yr−1), with a blue rest-UV color (β ∼ −2.5) indicating little dust, though not extremely low metallicity. While the presence of this source is in tension with most predictions, it agrees with empirical extrapolations assuming UV luminosity functions that smoothly decline with increasing redshift. Should follow-up spectroscopy validate this redshift, our universe was already aglow with galaxies less than 400 Myr after the Big Bang.

Published
2022
Full Text
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3. Changes in Pluto's atmosphere: 1988-2006

Author

Elliott, JL, Pasachoff, JM, Pike, RE, Zuluaga, CA, Bosh, AS, Dieters, S, Francis, PJ, Giles, AB, Greenhill, JG, Lade, B, Lucas, R, Person, MJ, Ramm, DJ, Gulbis, AAS, Souza, SP, Adams, ER, Babcock, BA, Gangestad, JW, Jaskot, AE, Kramer, EA, Elliott, JL, Pasachoff, JM, Pike, RE, Zuluaga, CA, Bosh, AS, Dieters, S, Francis, PJ, Giles, AB, Greenhill, JG, Lade, B, Lucas, R, Person, MJ, Ramm, DJ, Gulbis, AAS, Souza, SP, Adams, ER, Babcock, BA, Gangestad, JW, Jaskot, AE, and Kramer, EA

Abstract

The 2006 June 12 occultation of the star P384.2 (2UCAC 26039859) by Pluto was observed from five sites in southeastern Australia with high-speed imaging photometers that produced time-series CCD images. Light curves were constructed from the image time series and fit by least-squares methods with model light curves. A new modeling procedure is presented that allows a simultaneous fit of the atmospheric parameters for Pluto and the astrometric parameters for the occultation to all of the light curves. Under the assumption of a clear atmosphere and using this modeling procedure to establish the upper atmosphere boundary condition, immersion and emersion temperature profiles were derived by inversion of the Siding Spring light curve, which had our best signal-to-noise ratio. Above 1230 km radius, atmospheric temperatures are100K and decrease slightly with altitude—the same as observed in 1988 and 2002. Below 1210 km, the temperature abruptly decreases with altitude (gradients 2.2 K km1), which would reach the expected N2 surface-ice temperature of 40 K in the 1158Y1184 km radius range. This structure is similar to that observed in 2002, but a much stronger thermal gradient (or stronger extinction) is implied by the 1988 light curve (which shows a ‘‘kink’’ or ‘‘knee’’ at 1210 km). The temperature profiles derived from inversion of the present data show good agreement with a physical model for Pluto’s atmosphere selected from those presented by Strobel et al. (1996). Constraints derived from the temperature profiles (and considering the possibility of a deep troposphere) yield a value of 1152 32 km for Pluto’s surface radius. This value is compared with surface-radius values derived from the series of mutual occultations and eclipses that occurred in 1985Y1989, and the limitations of both types of measurements for determining Pluto’s surface radius are discussed. The radius of Pluto’s atmospheric shadow at the half-intensity point is 1207:9 8:5 km, the same as obtained i

4. CEERS Key Paper I: An Early Look into the First 500 Myr of Galaxy Formation with JWST

Author

Steven L. Finkelstein, Micaela B. Bagley, Henry C. Ferguson, Stephen M. Wilkins, Jeyhan S. Kartaltepe, Casey Papovich, L. Y. Aaron Yung, Pablo Arrabal Haro, Peter Behroozi, Mark Dickinson, Dale D. Kocevski, Anton M. Koekemoer, Rebecca L. Larson, Aurélien Le Bail, Alexa M. Morales, Pablo G. Pérez-González, Denis Burgarella, Romeel Davé, Michaela Hirschmann, Rachel S. Somerville, Stijn Wuyts, Volker Bromm, Caitlin M. Casey, Adriano Fontana, Seiji Fujimoto, Jonathan P. Gardner, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Taylor A. Hutchison, Saurabh W. Jha, Shardha Jogee, Lisa J. Kewley, Allison Kirkpatrick, Arianna S. Long, Jennifer M. Lotz, Laura Pentericci, Justin D. R. Pierel, Nor Pirzkal, Swara Ravindranath, Russell E. Ryan, Jonathan R. Trump, Guang Yang, Rachana Bhatawdekar, Laura Bisigello, Véronique Buat, Antonello Calabrò, Marco Castellano, Nikko J. Cleri, M. C. Cooper, Darren Croton, Emanuele Daddi, Avishai Dekel, David Elbaz, Maximilien Franco, Eric Gawiser, Benne W. Holwerda, Marc Huertas-Company, Anne E. Jaskot, Gene C. K. Leung, Ray A. Lucas, Bahram Mobasher, Viraj Pandya, Sandro Tacchella, Benjamin J. Weiner, Jorge A. Zavala, Finkelstein, SL [0000-0001-8519-1130], Bagley, MB [0000-0002-9921-9218], Ferguson, HC [0000-0001-7113-2738], Wilkins, SM [0000-0003-3903-6935], Kartaltepe, JS [0000-0001-9187-3605], Papovich, C [0000-0001-7503-8482], Yung, LY [0000-0003-3466-035X], Haro, PA [0000-0002-7959-8783], Behroozi, P [0000-0002-2517-6446], Dickinson, M [0000-0001-5414-5131], Kocevski, DD [0000-0002-8360-3880], Koekemoer, AM [0000-0002-6610-2048], Larson, RL [0000-0003-2366-8858], Le Bail, A [0000-0002-9466-2763], Morales, AM [0000-0003-4965-0402], Pérez-González, PG [0000-0003-4528-5639], Burgarella, D [0000-0002-4193-2539], Davé, R [0000-0003-2842-9434], Hirschmann, M [0000-0002-3301-3321], Somerville, RS [0000-0002-6748-6821], Wuyts, S [0000-0003-3735-1931], Bromm, V [0000-0003-0212-2979], Casey, CM [0000-0002-0930-6466], Fontana, A [0000-0003-3820-2823], Fujimoto, S [0000-0001-7201-5066], Gardner, JP [0000-0003-2098-9568], Giavalisco, M [0000-0002-7831-8751], Grazian, A [0000-0002-5688-0663], Grogin, NA [0000-0001-9440-8872], Hathi, NP [0000-0001-6145-5090], Hutchison, TA [0000-0001-6251-4988], Jha, SW [0000-0001-8738-6011], Jogee, S [0000-0002-1590-0568], Kewley, LJ [0000-0001-8152-3943], Kirkpatrick, A [0000-0002-1306-1545], Long, AS [0000-0002-7530-8857], Lotz, JM [0000-0003-3130-5643], Pentericci, L [0000-0001-8940-6768], Pierel, JDR [0000-0002-2361-7201], Pirzkal, N [0000-0003-3382-5941], Ravindranath, S [0000-0002-5269-6527], Ryan, RE [0000-0003-0894-1588], Trump, JR [0000-0002-1410-0470], Yang, G [0000-0001-8835-7722], Bhatawdekar, R [0000-0003-0883-2226], Bisigello, L [0000-0003-0492-4924], Buat, V [0000-0003-3441-903X], Calabrò, A [0000-0003-2536-1614], Castellano, M [0000-0001-9875-8263], Cleri, NJ [0000-0001-7151-009X], Cooper, MC [0000-0003-1371-6019], Croton, D [0000-0002-5009-512X], Daddi, E [0000-0002-3331-9590], Dekel, A [0000-0003-4174-0374], Elbaz, D [0000-0002-7631-647X], Franco, M [0000-0002-3560-8599], Gawiser, E [0000-0003-1530-8713], Holwerda, BW [0000-0002-4884-6756], Huertas-Company, M [0000-0002-1416-8483], Jaskot, AE [0000-0002-6790-5125], Leung, GCK [0000-0002-9393-6507], Lucas, RA [0000-0003-1581-7825], Mobasher, B [0000-0001-5846-4404], Pandya, V [0000-0002-2499-9205], Tacchella, S [0000-0002-8224-4505], Weiner, BJ [0000-0001-6065-7483], Zavala, JA [0000-0002-7051-1100], and Apollo - University of Cambridge Repository

Subjects
epoch simulations flares, cosmology legacy survey, deblended dust emission, uv luminosity functions, ultra-deep field, hubble frontier fields, FOS: Physical sciences, Astronomy and Astrophysics, initial mass function, 5109 Space Sciences, space-telescope observations, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, similar-to 10, Astrophysics of Galaxies (astro-ph.GA), 51 Physical Sciences, high-redshift galaxies
Abstract

We present an investigation into the first 500 Myr of galaxy evolution from the Cosmic Evolution Early Release Science (CEERS) survey. CEERS, one of 13 JWST ERS programs, targets galaxy formation from z~0.5 to z>10 using several imaging and spectroscopic modes. We make use of the first epoch of CEERS NIRCam imaging, spanning 35.5 sq. arcmin, to search for candidate galaxies at z>9. Following a detailed data reduction process implementing several custom steps to produce high-quality reduced images, we perform multi-band photometry across seven NIRCam broad and medium-band (and six Hubble broadband) filters focusing on robust colors and accurate total fluxes. We measure photometric redshifts and devise a robust set of selection criteria to identify a sample of 26 galaxy candidates at z~9-16. These objects are compact with a median half-light radius of ~0.5 kpc. We present an early estimate of the z~11 rest-frame ultraviolet (UV) luminosity function, finding that the number density of galaxies at M_UV ~ -20 appears to evolve very little from z~9 to z~11. We also find that the abundance (surface density [arcmin^-2]) of our candidates exceeds nearly all theoretical predictions. We explore potential implications, including that at z>10 star formation may be dominated by top-heavy initial mass functions, which would result in an increased ratio of UV light per unit halo mass, though a complete lack of dust attenuation and/or changing star-formation physics may also play a role. While spectroscopic confirmation of these sources is urgently required, our results suggest that the deeper views to come with JWST should yield prolific samples of ultra-high-redshift galaxies with which to further explore these conclusions., 41 pages, 20 figures, 6 tables, submitted to ApJL. Key results in Figures 13-15, discussed in Sections 7 and 8

Published
2022
Full Text
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