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

Author

Finkelstein, Steven L., Bagley, Micaela B., Haro, Pablo Arrabal, Dickinson, Mark, Ferguson, Henry C., Kartaltepe, Jeyhan S., Papovich, Casey, Burgarella, Denis, Kocevski, Dale D., Huertas-Company, Marc, Iyer, Kartheik G., Koekemoer, Anton M., Larson, Rebecca L., Pérez-González, Pablo G., Rose, Caitlin, Tacchella, Sandro, Wilkins, Stephen M., Chworowsky, Katherine, Medrano, Aubrey, Morales, Alexa M., Somerville, Rachel S., Yung, L. Y. Aaron, Fontana, Adriano, Giavalisco, Mauro, Grazian, Andrea, Grogin, Norman A., Kewley, Lisa J., Kirkpatrick, Allison, Kurczynski, Peter, Lotz, Jennifer M., Pentericci, Laura, Pirzkal, Nor, Ravindranath, Swara, Ryan, Russell E., Jr., Trump, Jonathan R., Yang, Guang, and The CEERS Team, Almaini, Omar, Amorín, Ricardo O., Annunziatella, Marianna, Backhaus, Bren E., Barro, Guillermo, Behroozi, Peter, Bell, Eric F., Bhatawdekar, Rachana, Bisigello, Laura, Bromm, Volker, Buat, Véronique, Buitrago, Fernando, Calabrò, Antonello, Casey, Caitlin M., Castellano, Marco, Chávez Ortiz, Óscar A., Ciesla, Laure, Cleri, Nikko J., Cohen, Seth H., Cole, Justin W., Cooke, Kevin C., Cooper, M. C., Cooray, Asantha R., Costantin, Luca, Cox, Isabella G., Croton, Darren, Daddi, Emanuele, Davé, Romeel, de la Vega, Alexander, Dekel, Avishai, Elbaz, David, Estrada-Carpenter, Vicente, Faber, Sandra M., Fernández, Vital, Finkelstein, Keely D., Freundlich, Jonathan, Fujimoto, Seiji, García-Argumánez, Ángela, Gardner, Jonathan P., Gawiser, Eric, Gómez-Guijarro, Carlos, Guo, Yuchen, Hamblin, Kurt, Hamilton, Timothy S., Hathi, Nimish P., Holwerda, Benne W., Hirschmann, Michaela, Hutchison, Taylor A., Jaskot, Anne E., Jha, Saurabh W., Jogee, Shardha, Juneau, Stéphanie, Jung, Intae, Kassin, Susan A., Bail, Aurélien Le, Leung, Gene C. K., Lucas, Ray A., Magnelli, Benjamin, Mantha, Kameswara Bharadwaj, Matharu, Jasleen, McGrath, Elizabeth J., McIntosh, Daniel H., Merlin, Emiliano, Mobasher, Bahram, Newman, Jeffrey A., Nicholls, David C., Pandya, Viraj, Rafelski, Marc, Ronayne, Kaila, Santini, Paola, Seillé, Lise-Marie, Shah, Ekta A., Shen, Lu, Simons, Raymond C., Snyder, Gregory F., Stanway, Elizabeth R., Straughn, Amber N., Teplitz, Harry I., Vanderhoof, Brittany N., Vega-Ferrero, Jesús, Wang, Weichen, Weiner, Benjamin J., Willmer, Christopher N. A., Wuyts, Stijn, Zavala, Jorge A., Finkelstein, Steven L. [0000-0001-8519-1130], Bagley, Micaela B. [0000-0002-9921-9218], Haro, Pablo Arrabal [0000-0002-7959-8783], Dickinson, Mark [0000-0001-5414-5131], Ferguson, Henry C. [0000-0001-7113-2738], Kartaltepe, Jeyhan S. [0000-0001-9187-3605], Papovich, Casey [0000-0001-7503-8482], Burgarella, Denis [0000-0002-4193-2539], Kocevski, Dale D. [0000-0002-8360-3880], Huertas-Company, Marc [0000-0002-1416-8483], Iyer, Kartheik G. [0000-0001-9298-3523], Koekemoer, Anton M. [0000-0002-6610-2048], Larson, Rebecca L. [0000-0003-2366-8858], Pérez-González, Pablo G. [0000-0003-4528-5639], Rose, Caitlin [0000-0002-8018-3219], Tacchella, Sandro [0000-0002-8224-4505], Wilkins, Stephen M. [0000-0003-3903-6935], Chworowsky, Katherine [0000-0003-4922-0613], Morales, Alexa M. [0000-0003-4965-0402], Somerville, Rachel S. [0000-0002-6748-6821], Yung, L. Y. Aaron [0000-0003-3466-035X], Fontana, Adriano [0000-0003-3820-2823], Giavalisco, Mauro [0000-0002-7831-8751], Grazian, Andrea [0000-0002-5688-0663], Grogin, Norman A. [0000-0001-9440-8872], Kewley, Lisa J. [0000-0001-8152-3943], Kirkpatrick, Allison [0000-0002-1306-1545], Kurczynski, Peter [0000-0002-8816-5146], Lotz, Jennifer M. [0000-0003-3130-5643], Pentericci, Laura [0000-0001-8940-6768], Pirzkal, Nor [0000-0003-3382-5941], Ravindranath, Swara [0000-0002-5269-6527], Ryan, Russell E., Jr. [0000-0003-0894-1588], Trump, Jonathan R. [0000-0002-1410-0470], Yang, Guang [0000-0001-8835-7722], Almaini, Omar [0000-0001-9328-3991], Amorín, Ricardo O. [0000-0001-5758-1000], Annunziatella, Marianna [0000-0002-8053-8040], Backhaus, Bren E. [0000-0001-8534-7502], Behroozi, Peter [0000-0002-2517-6446], Bell, Eric F. [0000-0002-5564-9873], Bhatawdekar, Rachana [0000-0003-0883-2226], Bisigello, Laura [0000-0003-0492-4924], Bromm, Volker [0000-0003-0212-2979], Buat, Véronique [0000-0003-3441-903X], Buitrago, Fernando [0000-0002-2861-9812], Calabrò, Antonello [0000-0003-2536-1614], Casey, Caitlin M. [0000-0002-0930-6466], Castellano, Marco [0000-0001-9875-8263], Chávez Ortiz, Óscar A. [0000-0003-2332-5505], Ciesla, Laure [0000-0003-0541-2891], Cleri, Nikko J. [0000-0001-7151-009X], Cohen, Seth H. [0000-0003-3329-1337], Cole, Justin W. [0000-0002-6348-1900], Cooke, Kevin C. [0000-0002-2200-9845], Cooper, M. C. [0000-0003-1371-6019], Cooray, Asantha R. [0000-0002-3892-0190], Costantin, Luca [0000-0001-6820-0015], Cox, Isabella G. [0000-0002-1803-794X], Croton, Darren [0000-0002-5009-512X], Daddi, Emanuele [0000-0002-3331-9590], Davé, Romeel [0000-0003-2842-9434], de la Vega, Alexander [0000-0002-6219-5558], Dekel, Avishai [0000-0003-4174-0374], Elbaz, David [0000-0002-7631-647X], Estrada-Carpenter, Vicente [0000-0001-8489-2349], Fernández, Vital [0000-0003-0531-5450], Finkelstein, Keely D. [0000-0003-0792-5877], Freundlich, Jonathan [0000-0002-5245-7796], Fujimoto, Seiji [0000-0001-7201-5066], García-Argumánez, Ángela [0000-0002-8365-5525], Gardner, Jonathan P. [0000-0003-2098-9568], Gawiser, Eric [0000-0003-1530-8713], Gómez-Guijarro, Carlos [0000-0002-4085-9165], Guo, Yuchen [0000-0002-4162-6523], Hamblin, Kurt [0000-0002-6292-4589], Hamilton, Timothy S. [0000-0002-9753-1769], Hathi, Nimish P. [0000-0001-6145-5090], Holwerda, Benne W. [0000-0002-4884-6756], Hirschmann, Michaela [0000-0002-3301-3321], Hutchison, Taylor A. [0000-0001-6251-4988], Jaskot, Anne E. [0000-0002-6790-5125], Jha, Saurabh W. [0000-0001-8738-6011], Jogee, Shardha [0000-0002-1590-0568], Juneau, Stéphanie [0000-0002-0000-2394], Jung, Intae [0000-0003-1187-4240], Kassin, Susan A. [0000-0002-3838-8093], Bail, Aurélien Le [0000-0002-9466-2763], Leung, Gene C. K. [0000-0002-9393-6507], Lucas, Ray A. [0000-0003-1581-7825], Magnelli, Benjamin [0000-0002-6777-6490], Matharu, Jasleen [0000-0002-7547-3385], McGrath, Elizabeth J. [0000-0001-8688-2443], Merlin, Emiliano [0000-0001-6870-8900], Newman, Jeffrey A. [0000-0001-8684-2222], Nicholls, David C. [0000-0003-0892-5203], Pandya, Viraj [0000-0002-2499-9205], Rafelski, Marc [0000-0002-9946-4731], Ronayne, Kaila [0000-0001-5749-5452], Santini, Paola [0000-0002-9334-8705], Seillé, Lise-Marie [0000-0001-7755-4755], Shah, Ekta A. [0000-0001-7811-9042], Shen, Lu [0000-0001-9495-7759], Simons, Raymond C. [0000-0002-6386-7299], Snyder, Gregory F. [0000-0002-4226-304X], Stanway, Elizabeth R. [0000-0002-8770-809X], Straughn, Amber N. [0000-0002-4772-7878], Teplitz, Harry I. [0000-0002-7064-5424], Vanderhoof, Brittany N. [0000-0002-8163-0172], Vega-Ferrero, Jesús [0000-0003-2338-5567], Wang, Weichen [0000-0002-9593-8274], Weiner, Benjamin J. [0000-0001-6065-7483], Willmer, Christopher N. A. [0000-0001-9262-9997], Wuyts, Stijn [0000-0003-3735-1931], and Apollo - University of Cambridge Repository

Subjects
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

2. CEERS: MIRI deciphers the spatial distribution of dust-obscured star formation in galaxies at $0.1

Author

Magnelli, Benjamin, Gómez-Guijarro, Carlos, Elbaz, David, Daddi, Emanuele, Papovich, Casey, Shen, Lu, Haro, Pablo Arrabal, Bagley, Micaela B., Bell, Eric F., Buat, Véronique, Costantin, Luca, Dickinson, Mark, Finkelstein, Steven L., Gardner, Jonathan P., Jiménez-Andrade, Eric F., Kartaltepe, Jeyhan S., Koekemoer, Anton M., Lyu, Yipeng, Pérez-González, Pablo G., Pirzkal, Nor, Tacchella, Sandro, de la Vega, Alexander, Wuyts, Stijn, Yang, Guang, Yung, L. Y. Aaron, and Zavala, Jorge

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences
Abstract

[Abridged] We combine HST images from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey with JWST images from the Cosmic Evolution Early Release Science (CEERS) survey to measure the stellar and dust-obscured star formation distributions of a mass-complete ($>10^{10}M_\odot$) sample of 95 star-forming galaxies (SFGs) at $0.175$; 38 galaxies). At lower $S/N$, simulations show that simultaneous measurements of the size and Sérsic index become unreliable. We extend our study to fainter sources ($S/N>10$; 95 galaxies) by fixing their Sérsic index to unity. The Sérsic index of bright galaxies ($S/N>75$) has a median value of 0.7, which, together with their axis ratio distribution, suggests a disk-like morphology in the rest-MIR. Galaxies above the main sequence (MS; i.e., starbursts) have rest-MIR sizes that are a factor 2 smaller than their rest-optical sizes. The median rest-optical to rest-MIR size ratio of MS galaxies increases with stellar mass, from 1.1 at $10^{9.8}M_\odot$ to 1.6 at $10^{11}M_\odot$. This mass-dependent trend resembles the one found in the literature between the rest-optical and rest-near-infrared sizes of SFGs, suggesting that it is due to dust attenuation gradients affecting rest-optical sizes and that the sizes of the stellar and star-forming components of SFGs are, on average, consistent at all masses. There is, however, a small population of SFGs (15%) with a compact star-forming component embedded in a larger stellar structure. This could be the missing link between galaxies with an extended stellar component and those with a compact stellar component; the so-called blue nuggets., Submitted to A&A. 18 pages, 14 figures

Published
2023
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3. CEERS: Spatially Resolved UV and mid-IR Star Formation in Galaxies at 0.2 < z < 2.5: The Picture from the Hubble and James Webb Space Telescopes

Author

Shen, Lu, Papovich, Casey, Yang, Guang, Matharu, Jasleen, Wang, Xin, Magnelli, Benjamin, Elbaz, David, Jogee, Shardha, Alavi, Anahita, Haro, Pablo Arrabal, Backhaus, Bren E., Bagley, Micaela B., Bell, Eric F., Bisigello, Laura, Calabrò, Antonello, Cooper, M. C., Costantin, Luca, Daddi, Emanuele, Dickinson, Mark, Finkelstein, Steven L., Fujimoto, Seiji, Giavalisco, Mauro, Grogin, Norman A., Guo, Yuchen, Holwerda, Benne W., Kartaltepe, Jeyhan S., Koekemoer, Anton M., Kurczynski, Peter, Lucas, Ray A., Peŕez-Gonzaĺez, Pablo G., Pirzkal, Nor, Prichard, Laura, Rafelski, Marc, Ronayne, Kaila, Simons, Raymond C., Sunnquist, Ben, Teplitz, Harry I., Trump, Jonathan R., Weiner, Benjamin J., Windhorst, Rogier A., and Yung, L. Y. Aaron

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences
Abstract

We present the mid-IR (MIR) morphologies for 64 star-forming galaxies at $0.210^{9}~M_\odot}$ using JWST MIRI observations from the Cosmic Evolution Early Release Science survey (CEERS). The MIRI bands span the MIR (7.7--21~$μ$m), enabling us to measure the effective radii ($R_{\rm{eff}}$) and Sérsic indexes of these SFGs at rest-frame 6.2 and 7.7 $μ$m, which contains strong emission from Polycyclic aromatic hydrocarbon (PAH) features, a well-established tracer of star formation in galaxies. We define a ``PAH-band'' as the MIRI bandpass that contains these features at the redshift of the galaxy. We then compare the galaxy morphologies in the PAH-bands to those in rest-frame Near-UV (NUV) using HST ACS/F435W or ACS/F606W and optical/near-IR using HST WFC3/F160W imaging from UVCANDELS and CANDELS, where the NUV-band and F160W trace the profile of (unobscured) massive stars and the stellar continuum, respectively. The $R_{\rm{eff}}$ of galaxies in the PAH-band are slightly smaller ($\sim$10\%) than those in F160W for galaxies with $\rm{M_*\gtrsim10^{9.5}~M_\odot}$ at $z\leq1.2$, but the PAH-band and F160W have a similar fractions of light within 1 kpc. In contrast, the $R_{\rm{eff}}$ of galaxies in the NUV-band are larger, with lower fractions of light within 1 kpc compared to F160W for galaxies at $z\leq1.2$. Using the MIRI data to estimate the $\rm{SFR_{\rm{IR}}}$ surface density, we find the correlation between the $\rm{SFR_{\rm{IR}}}$ surface density and stellar mass has a steeper slope than that of the $\rm{SFR_{\rm{UV}}}$ surface density and stellar mass, suggesting more massive galaxies having increasing amounts of obscured fraction of star formation in their inner regions. This paper demonstrates how the high-angular resolution data from JWST/MIRI can reveal new information about the morphology of obscured-star formation., 28 pages, 11 figures, Accepted by ApJ

Published
2023
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4. Turbulent Gas in Lensed Planck-selected Starbursts at redshifts 1-3.5

Author

Harrington, Kevin C., Weiss, Axel, Yun, Min S., Magnelli, Benjamin, Sharon, C. E., Leung, T. K. D., Vishwas, A., Wang, Q. D., Jimenez-Andrade, E. F., Frayer, D. T., Liu, D., Garcia, P., Romano-Diaz, E., Frye, B. L., Jarugula, S., Badescu, T., Berman, D., Dannerbauer, H., Diaz-Sanchez, A., Grassitelli, L., Kamieneski, P., Kim, W. J., Kirkpatrick, A., Lowenthal, J. D., Messias, H., Puschnig, J., Stacey, G. J., Torne, P., and Bertoldi, F.

Subjects
Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

Dusty star-forming galaxies at high redshift (1 < z < 3) represent the most intense star-forming regions in the Universe. Key aspects to these processes are the gas heating and cooling mechanisms. Although it is well known that these galaxies are gas-rich, little is known about the gas excitation conditions. Here we examine these processes in a sample of 24 strongly lensed star-forming galaxies identified by the \textit{Planck} satellite (LPs) at z ~ 1.1 - 3.5. We analyze 162 CO rotational transitions (ranging from Jupper = 1 - 12) and 37 atomic carbon fine-structure lines ([CI]) in order to characterize the physical conditions of the gas in sample of LPs. We simultaneously fit the CO and [CI] lines, and the dust continuum emission, using two different non-LTE, radiative transfer models. The first model represents a two component gas density, while the second assumes a turbulence driven log-normal gas density distribution. These LPs are among the most gas-rich, infrared (IR) luminous galaxies ever observed ($\mu_{\rm L}$L$_{\rm IR(8-1000\mu m) } \sim 10^{13-14.6} $\Lsun; $< \mu_{\rm L}$M$_{\rm ISM}> = 2.7 \pm 1.2 \times 10^{12}$ \Msun, with $\mu_{\rm L} \sim 10-30$ the average lens magnification factor). Our results suggest that the turbulent ISM present in the LPs can be well-characterized by a high turbulent velocity dispersion ($ \sim 100 $ \kms) and gas kinetic temperature to dust temperature ratios $ \sim 2.5$, sustained on scales larger than a few kpc. We speculate that the average surface density of the molecular gas mass and IR luminosity $\Sigma_{\rm M_{\rm ISM}}$ $\sim 10^{3 - 4}$ \Msun pc$^{-2}$ and $\Sigma_{\rm L_{\rm IR}}$ $\sim 10^{11 - 12}$ \Lsun kpc$^{-2}$, arise from both stellar mechanical feedback and a steady momentum injection from the accretion of intergalactic gas., Comment: 54 pages, 18 figures. Accepted for publication in The Astrophysical Journal (as of Oct. 30, 2020). Please feel free to view the supplementary figures here (which can later be found online in the ApJ after the full publication procedure): https://drive.google.com/drive/folders/1CN3rqlUDcNi5JSDH2GhFk_SLSlo10han?usp=sharing

Published
2020
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5. 'SZ spectroscopy' in the coming decade: Galaxy cluster cosmology and astrophysics in the submillimeter

Author

Basu, Kaustuv, Erler, Jens, Chluba, Jens, Delabrouille, Jacques, Hill, J. Colin, Mroczkowski, Tony, Niemack, Michael D., Remazeilles, Mathieu, Sayers, Jack, Scott, Douglas, Vavagiakis, Eve M., Zemcov, Michael, Aravena, Manuel, Bartlett, James G., Battaglia, Nicholas, Bertoldi, Frank, Charmetant, Maude, Golwala, Sunil, Herter, Terry L., Klaassen, Pamela, Komatsu, Eiichiro, Magnelli, Benjamin, Mantz, Adam B., Meerburg, P. Daniel, Melin, Jean-Baptiste, Nagai, Daisuke, Parshley, Stephen C., Pointecouteau, Etienne, Ramos-Ceja, Miriam E., Ruszkowski, Mateusz, Sehgal, Neelima, Stacey, Gordon G., and Sunyaev, Rashid

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Sunyaev-Zeldovich (SZ) effects were first proposed in the 1970s as tools to identify the X-ray emitting hot gas inside massive clusters of galaxies and obtain their velocities relative to the cosmic microwave background (CMB). Yet it is only within the last decade that they have begun to significantly impact astronomical research. Thanks to the rapid developments in CMB instrumentation, measurement of the dominant thermal signature of the SZ effects has become a routine tool to find and characterize large samples of galaxy clusters and to seek deeper understanding of several important astrophysical processes via high-resolution imaging studies of many targets. With the notable exception of the Planck satellite and a few combinations of ground-based observatories, much of this "SZ revolution" has happened in the photometric mode, where observations are made at one or two frequencies in the millimeter regime to maximize the cluster detection significance and minimize the foregrounds. Still, there is much more to learn from detailed and systematic analyses of the SZ spectra across multiple wavelengths, specifically in the submillimeter (>300 GHz) domain. The goal of this Science White Paper is to highlight this particular aspect of SZ research, point out what new and potentially groundbreaking insights can be obtained from these studies, and emphasize why the coming decade can be a golden era for SZ spectral measurements., Science white paper submitted for the Astro2020 decadal review, 5 pages + references

Published
2019
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6. The case for a 'sub-millimeter SDSS': a 3D map of galaxy evolution to z~10

Author

Geach, James E., Banerji, Manda, Bertoldi, Frank, Bethermin, Matthieu, Casey, Caitlin M., Chen, Chian-Chou, Clements, David L., Cicone, Claudia, Combes, Francoise, Conselice, Christopher, Cooray, Asantha, Coppin, Kristen, Daddi, Emanuele, Dannerbauer, Helmut, Dave, Romeel, Doherty, Matthew, Dunlop, James S., Edge, Alastair, Farrah, Duncan, Franco, Maximilien, Fuller, Gary, Garratt, Tracy, Gear, Walter, Greve, Thomas R., Hatziminaoglou, Evanthia, Hayward, Christopher C., Ivison, Rob J., Kawabe, Ryohei, Klaassen, Pamela, Knudsen, Kirsten K., Kohno, Kotaro, Koprowski, Maciej, Lagos, Claudia D. P., Magdis, Georgios E., Magnelli, Benjamin, McGee, Sean L., Michalowski, Michal, Mroczkowski, Tony, Noroozian, Omid, Oliver, Seb, Riechers, Dominik, Rujopakarn, Wiphu, Scott, Douglas, Serjeant, Stephen, Smith, Matthew W. L., Swinbank, Mark, Tamura, Yoichi, van der Werf, Paul, van Kampen, Eelco, Verma, Aprajita, Vieira, Joaquin, Wagg, Jeff, Walter, Fabian, Wang, Lingyu, Wootten, Al, and Yun, Min S.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Sloan Digital Sky Survey (SDSS) was revolutionary because of the extraordinary breadth and ambition of its optical imaging and spectroscopy. We argue that a 'sub-millimeter SDSS' - a sensitive large-area imaging+spectroscopic survey in the sub-mm window - will revolutionize our understanding of galaxy evolution in the early Universe. By detecting the thermal dust continuum emission and atomic and molecular line emission of galaxies out to z~10 it will be possible to measure the redshifts, star formation rates, dust and gas content of hundreds of thousands of high-z galaxies down to ~L*. Many of these galaxies will have counterparts visible in the deep optical imaging of the Large Synoptic Survey Telescope. This 3D map of galaxy evolution will span the peak epoch of galaxy formation all the way back to cosmic dawn, measuring the co-evolution of the star formation rate density and molecular gas content of galaxies, tracking the production of metals and charting the growth of large-scale structure., Comment: Science White paper submitted to the Astro2020 Decadal Survey

Published
2019
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7. Discovery of a Proto-cluster Associated with a Ly-$��$ Blob Pair at z=2.3

Author

B��descu, Toma, Yang, Yujin, Bertoldi, Frank, Zabludoff, Ann, Karim, Alexander, and Magnelli, Benjamin

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Bright Ly-$��$ blobs (LABs) --- extended nebulae with sizes of $\sim$100kpc and Ly-$��$ luminosities of $\sim$10$^{44}$erg s$^{-1}$ --- often reside in overdensities of compact Ly-$��$ emitters (LAEs) that may be galaxy protoclusters. The number density, variance, and internal kinematics of LABs suggest that they themselves trace group-like halos. Here we test this hierarchical picture, presenting deep, wide-field Ly-$��$ narrowband imaging of a 1$^\circ$ $\times$ 0.5$^\circ$ region around a LAB pair at $z$ = 2.3 discovered previously by a blind survey. We find 183 Ly-$��$ emitters, including the original LAB pair and three new LABs with Ly-$��$ luminosities of (0.9--1.3)$\times$10$^{43}$erg s$^{-1}$ and isophotal areas of 16--24 arcsec$^2$. Using the LAEs as tracers and a new kernel density estimation method, we discover a large-scale overdensity (Bo{��}tes J1430+3522) with a surface density contrast of $��_��$ = 2.7, a volume density contrast of $��$ $\sim$ 10.4, and a projected diameter of $\approx$ 20 comoving Mpc. Comparing with cosmological simulations, we conclude that this LAE overdensity will evolve into a present-day Coma-like cluster with $\log{(M/M_\odot)}$ $\sim$ $15.1\pm0.2$. In this and three other wide-field LAE surveys re-analyzed here, the extents and peak amplitudes of the largest LAE overdensities are similar, not increasing with survey size, implying that they were indeed the largest structures then and do evolve into rich clusters today. Intriguingly, LABs favor the outskirts of the densest LAE concentrations, i.e., intermediate LAE overdensities of $��_��= 1 - 2$. We speculate that these LABs mark infalling proto-groups being accreted by the more massive protocluster.

Published
2017
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8. Evidence for a wide range of UV obscuration in z ~ 2 dusty galaxies from the GOODS-Herschel survey

Author

Penner, Kyle, Dickinson, Mark, Pope, Alexandra, Dey, Arjun, Magnelli, Benjamin, Pannella, Maurilio, Altieri, Bruno, Aussel, Herve, Buat, Veronique, Bussmann, Shane, Charmandaris, Vassilis, Coia, Daniela, Daddi, Emanuele, Dannerbauer, Helmut, Elbaz, David, Hwang, Ho Seong, Kartaltepe, Jeyhan, Lin, Lihwai, Magdis, Georgios, Morrison, Glenn, Popesso, Paola, Scott, Douglas, and Valtchanov, Ivan

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Dusty galaxies at z ~ 2 span a wide range of relative brightness between rest-frame mid-infrared (8um) and ultraviolet wavelengths. We attempt to determine the physical mechanism responsible for this diversity. Dust-obscured galaxies (DOGs), which have rest-frame mid-IR to UV flux density ratios > 1000, might be abnormally bright in the mid-IR, perhaps due to prominent AGN and/or PAH emission, or abnormally faint in the UV. We use far-infrared data from the GOODS-Herschel survey to show that most DOGs with 10^12 L_Sun < L_IR < 10^13 L_Sun are not abnormally bright in the mid-IR when compared to other dusty galaxies with similar IR (8--1000um) luminosities. We observe a relation between the median IR to UV luminosity ratios and the median UV continuum power-law indices for these galaxies, and we find that only 24% have specific star formation rates which indicate the dominance of compact star-forming regions. This circumstantial evidence supports the idea that the UV- and IR-emitting regions in these galaxies are spatially coincident, which implies a connection between the abnormal UV faintness of DOGs and dust obscuration. We conclude that the range in rest-frame mid-IR to UV flux density ratios spanned by dusty galaxies at z ~ 2 is due to differing amounts of UV obscuration. Of galaxies with these IR luminosities, DOGs are the most obscured. We attribute differences in UV obscuration to either: 1) differences in the degree of alignment between the spatial distributions of dust and massive stars, or 2) differences in the total dust content., 9 pages, 9 figures. Accepted by ApJ

Published
2012
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9. Widespread and Hidden Active Galactic Nuclei in Star-Forming Galaxies at Redshift > 0.3

Author

Juneau, St��phanie, Dickinson, Mark, Bournaud, Fr��d��ric, Alexander, David M., Daddi, Emanuele, Mullaney, James R., Magnelli, Benjamin, Kartaltepe, Jeyhan S., Hwang, Ho Seong, Willner, S. P., Coil, Alison L., Rosario, David J., Trump, Jonathan R., Weiner, Benjamin J., Willmer, Christopher N. A., Cooper, Michael C., Elbaz, David, Faber, S. M., Frayer, David T., Kocevski, Dale D., Laird, Elise S., Monkiewicz, Jacqueline A., Nandra, Kirpal, Newman, Jeffrey, Salim, Samir, and Symeonidis, Myrto

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We characterize the incidence of active galactic nuclei (AGNs) is 0.3 < z < 1 star-forming galaxies by applying multi-wavelength AGN diagnostics (X-ray, optical, mid-infrared, radio) to a sample of galaxies selected at 70-micron from the Far-Infrared Deep Extragalactic Legacy survey (FIDEL). Given the depth of FIDEL, we detect "normal" galaxies on the specific star formation rate (sSFR) sequence as well as starbursting systems with elevated sSFR. We find an overall high occurrence of AGN of 37+/-3%, more than twice as high as in previous studies of galaxies with comparable infrared luminosities and redshifts but in good agreement with the AGN fraction of nearby (0.05 < z < 0.1) galaxies of similar infrared luminosities. The more complete census of AGNs comes from using the recently developed Mass-Excitation (MEx) diagnostic diagram. This optical diagnostic is also sensitive to X-ray weak AGNs and X-ray absorbed AGNs, and reveals that absorbed active nuclei reside almost exclusively in infrared-luminous hosts. The fraction of galaxies hosting an AGN appears to be independent of sSFR and remains elevated both on the sSFR sequence and above. In contrast, the fraction of AGNs that are X-ray absorbed increases substantially with increasing sSFR, possibly due to an increased gas fraction and/or gas density in the host galaxies., 21 pages, 15 figures. Accepted for publication in the Astrophysical Journal. Subject headings updated; otherwise identical to previous version

Published
2012
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10. A Long Time Ago in a Galaxy Far, Far Away: A Candidate z similar to 12 Galaxy in Early JWST CEERS Imaging

Author

Finkelstein, Steven L., Bagley, Micaela B., Haro, Pablo Arrabal, Dickinson, Mark, Ferguson, Henry C., Kartaltepe, Jeyhan S., Papovich, Casey, Burgarella, Denis, Kocevski, Dale D., Huertas-Company, Marc, Iyer, Kartheik G., Koekemoer, Anton M., Larson, Rebecca L., Perez-Gonzalez, Pablo G., Rose, Caitlin, Tacchella, Sandro, Wilkins, Stephen M., Chworowsky, Katherine, Medrano, Aubrey, Morales, Alexa M., Somerville, Rachel S., Yung, L. Y. Aaron, Fontana, Adriano, Giavalisco, Mauro, Grazian, Andrea, Grogin, Norman A., Kewley, Lisa J., Kirkpatrick, Allison, Kurczynski, Peter, Lotz, Jennifer M., Pentericci, Laura, Pirzkal, Nor, Ravindranath, Swara, Ryan, Russell E., Jr., Trump, Jonathan R., Yang, Guang, Almaini, Omar, Amorin, Ricardo O., Annunziatella, Marianna, Backhaus, Bren E., Barro, Guillermo, Behroozi, Peter, Bell, Eric F., Bhatawdekar, Rachana, Bisigello, Laura, Bromm, Volker, Buat, Veronique, Buitrago, Fernando, Calabro, Antonello, Casey, Caitlin M., Castellano, Marco, Ortiz, Oscar A. Chavez, Ciesla, Laure, Cleri, Nikko J., Cohen, Seth H., Cole, Justin W., Cooke, Kevin C., Cooper, M. C., Cooray, Asantha R., Costantin, Luca, Cox, Isabella G., Croton, Darren, Daddi, Emanuele, Dave, Romeel, de la Vega, Alexander, Dekel, Avishai, Elbaz, David, Estrada-Carpenter, Vicente, Faber, Sandra M., Fernandez, Vital, Finkelstein, Keely D., Freundlich, Jonathan, Fujimoto, Seiji, Garcia-Argumanez, Angela, Gardner, Jonathan P., Gawiser, Eric, Gomez-Guijarro, Carlos, Guo, Yuchen, Hamblin, Kurt, Hamilton, Timothy S., Hathi, Nimish P., Holwerda, Benne W., Hirschmann, Michaela, Hutchison, Taylor A., Jaskot, Anne E., Jha, Saurabh W., Jogee, Shardha, Juneau, Stephanie, Jung, Intae, Kassin, Susan A., Le Bail, Aurelien, Leung, Gene C. K., Lucas, Ray A., Magnelli, Benjamin, Mantha, Kameswara Bharadwaj, Matharu, Jasleen, McGrath, Elizabeth J., McIntosh, Daniel H., Merlin, Emiliano, Mobasher, Bahram, Newman, Jeffrey A., Nicholls, David C., Pandya, Viraj, Rafelski, Marc, Ronayne, Kaila, Santini, Paola, Seille, Lise-Marie, Shah, Ekta A., Shen, Lu, Simons, Raymond C., Snyder, Gregory F., Stanway, Elizabeth R., Straughn, Amber N., Teplitz, Harry, I, Vanderhoof, Brittany N., Vega-Ferrero, Jesus, Wang, Weichen, Weiner, Benjamin J., Willmer, Christopher N. A., Wuyts, Stijn, and Zavala, Jorge A.

Subjects
epoch simulations flares, semianalytic forecasts, space-telescope, 1st galaxies, star-formation histories, light-cones, mass, luminosity function, l-dwarf, stellar
Abstract

We report the discovery of a candidate galaxy with a photo -z of z similar to 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 zphot = 11.8(+0.3) (-0.2) (1 sigma uncertainty) with m(F200W) = 27.3 and > 7 sigma detections in five filters. The source is not detected at lambda < 1.4 mu m in deep imaging from both Hubble Space Telescope (HST) and JWST and has faint similar to 3 sigma detections in JWST F150W and HST F160W, which signal a Ly alpha break near the red edge of both filters, implying z similar to 12. This object (Maisie's Galaxy) exhibits F115W - F200W > 1.9 mag (2 sigma 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-?similar to 8.5 and is highly star-forming (log sSFR similar to -8.2 yr(-1)), with a blue rest-UV color (beta similar to -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.

11. The Physical Conditions of Emission-line Galaxies at Cosmic Dawn from JWST/NIRSpec Spectroscopy in the SMACS 0723 Early Release Observations

Author

Jonathan R. Trump, Pablo Arrabal Haro, Raymond C. Simons, Bren E. Backhaus, Ricardo O. Amorín, Mark Dickinson, Vital Fernández, Casey Papovich, David C. Nicholls, Lisa J. Kewley, Samantha W. Brunker, John J. Salzer, Stephen M. Wilkins, Omar Almaini, Micaela B. Bagley, Danielle A. Berg, Rachana Bhatawdekar, Laura Bisigello, Véronique Buat, Denis Burgarella, Antonello Calabrò, Caitlin M. Casey, Laure Ciesla, Nikko J. Cleri, Justin W. Cole, M. C. Cooper, Asantha R. Cooray, Luca Costantin, Darren Croton, Henry C. Ferguson, Steven L. Finkelstein, Seiji Fujimoto, Jonathan P. Gardner, Eric Gawiser, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Marc Huertas-Company, Taylor A. Hutchison, Shardha Jogee, Stéphanie Juneau, Intae Jung, Jeyhan S. Kartaltepe, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Jennifer M. Lotz, Ray A. Lucas, Benjamin Magnelli, Jasleen Matharu, Pablo G. Pérez-González, Nor Pirzkal, Marc Rafelski, Caitlin Rose, Lise-Marie Seillé, Rachel S. Somerville, Amber N. Straughn, Sandro Tacchella, Brittany N. Vanderhoof, Benjamin J. Weiner, Stijn Wuyts, L. Y. Aaron Yung, Jorge A. Zavala, Trump, Jonathan R [0000-0002-1410-0470], Haro, Pablo Arrabal [0000-0002-7959-8783], Simons, Raymond C [0000-0002-6386-7299], Backhaus, Bren E [0000-0001-8534-7502], Amorín, Ricardo O [0000-0001-5758-1000], Dickinson, Mark [0000-0001-5414-5131], Fernández, Vital [0000-0003-0531-5450], Papovich, Casey [0000-0001-7503-8482], Nicholls, David C [0000-0003-0892-5203], Kewley, Lisa J [0000-0001-8152-3943], Brunker, Samantha W [0000-0001-6776-2550], Salzer, John J [0000-0001-8483-603X], Wilkins, Stephen M [0000-0003-3903-6935], Almaini, Omar [0000-0001-9328-3991], Bagley, Micaela B [0000-0002-9921-9218], Berg, Danielle A [0000-0002-4153-053X], Bhatawdekar, Rachana [0000-0003-0883-2226], Bisigello, Laura [0000-0003-0492-4924], Buat, Véronique [0000-0003-3441-903X], Burgarella, Denis [0000-0002-4193-2539], Calabrò, Antonello [0000-0003-2536-1614], Casey, Caitlin M [0000-0002-0930-6466], Ciesla, Laure [0000-0003-0541-2891], Cleri, Nikko J [0000-0001-7151-009X], Cole, Justin W [0000-0002-6348-1900], Cooper, MC [0000-0003-1371-6019], Cooray, Asantha R [0000-0002-3892-0190], Costantin, Luca [0000-0001-6820-0015], Croton, Darren [0000-0002-5009-512X], Ferguson, Henry C [0000-0001-7113-2738], Finkelstein, Steven L [0000-0001-8519-1130], Fujimoto, Seiji [0000-0001-7201-5066], Gardner, Jonathan P [0000-0003-2098-9568], Gawiser, Eric [0000-0003-1530-8713], Giavalisco, Mauro [0000-0002-7831-8751], Grazian, Andrea [0000-0002-5688-0663], Grogin, Norman A [0000-0001-9440-8872], Hathi, Nimish P [0000-0001-6145-5090], Hirschmann, Michaela [0000-0002-3301-3321], Holwerda, Benne W [0000-0002-4884-6756], Huertas-Company, Marc [0000-0002-1416-8483], Hutchison, Taylor A [0000-0001-6251-4988], Jogee, Shardha [0000-0002-1590-0568], Juneau, Stéphanie [0000-0002-0000-2394], Jung, Intae [0000-0003-1187-4240], Kartaltepe, Jeyhan S [0000-0001-9187-3605], Kirkpatrick, Allison [0000-0002-1306-1545], Kocevski, Dale D [0000-0002-8360-3880], Koekemoer, Anton M [0000-0002-6610-2048], Lotz, Jennifer M [0000-0003-3130-5643], Lucas, Ray A [0000-0003-1581-7825], Magnelli, Benjamin [0000-0002-6777-6490], Matharu, Jasleen [0000-0002-7547-3385], Pérez-González, Pablo G [0000-0003-4528-5639], Pirzkal, Nor [0000-0003-3382-5941], Rafelski, Marc [0000-0002-9946-4731], Rose, Caitlin [0000-0002-8018-3219], Seillé, Lise-Marie [0000-0001-7755-4755], Somerville, Rachel S [0000-0002-6748-6821], Straughn, Amber N [0000-0002-4772-7878], Tacchella, Sandro [0000-0002-8224-4505], Vanderhoof, Brittany N [0000-0002-8163-0172], Weiner, Benjamin J [0000-0001-6065-7483], Wuyts, Stijn [0000-0003-3735-1931], Aaron Yung, LY [0000-0003-3466-035X], Zavala, Jorge A [0000-0002-7051-1100], Apollo - University of Cambridge Repository, Trump, JR [0000-0002-1410-0470], Haro, PA [0000-0002-7959-8783], Simons, RC [0000-0002-6386-7299], Backhaus, BE [0000-0001-8534-7502], Amorín, RO [0000-0001-5758-1000], Dickinson, M [0000-0001-5414-5131], Fernández, V [0000-0003-0531-5450], Papovich, C [0000-0001-7503-8482], Nicholls, DC [0000-0003-0892-5203], Kewley, LJ [0000-0001-8152-3943], Brunker, SW [0000-0001-6776-2550], Salzer, JJ [0000-0001-8483-603X], Wilkins, SM [0000-0003-3903-6935], Almaini, O [0000-0001-9328-3991], Bagley, MB [0000-0002-9921-9218], Berg, DA [0000-0002-4153-053X], Bhatawdekar, R [0000-0003-0883-2226], Bisigello, L [0000-0003-0492-4924], Buat, V [0000-0003-3441-903X], Burgarella, D [0000-0002-4193-2539], Calabrò, A [0000-0003-2536-1614], Casey, CM [0000-0002-0930-6466], Ciesla, L [0000-0003-0541-2891], Cleri, NJ [0000-0001-7151-009X], Cole, JW [0000-0002-6348-1900], Cooray, AR [0000-0002-3892-0190], Costantin, L [0000-0001-6820-0015], Croton, D [0000-0002-5009-512X], Ferguson, HC [0000-0001-7113-2738], Finkelstein, SL [0000-0001-8519-1130], Fujimoto, S [0000-0001-7201-5066], Gardner, JP [0000-0003-2098-9568], Gawiser, E [0000-0003-1530-8713], Giavalisco, M [0000-0002-7831-8751], Grazian, A [0000-0002-5688-0663], Grogin, NA [0000-0001-9440-8872], Hathi, NP [0000-0001-6145-5090], Hirschmann, M [0000-0002-3301-3321], Holwerda, BW [0000-0002-4884-6756], Huertas-Company, M [0000-0002-1416-8483], Hutchison, TA [0000-0001-6251-4988], Jogee, S [0000-0002-1590-0568], Juneau, S [0000-0002-0000-2394], Jung, I [0000-0003-1187-4240], Kartaltepe, JS [0000-0001-9187-3605], Kirkpatrick, A [0000-0002-1306-1545], Kocevski, DD [0000-0002-8360-3880], Koekemoer, AM [0000-0002-6610-2048], Lotz, JM [0000-0003-3130-5643], Lucas, RA [0000-0003-1581-7825], Magnelli, B [0000-0002-6777-6490], Matharu, J [0000-0002-7547-3385], Pérez-González, PG [0000-0003-4528-5639], Pirzkal, N [0000-0003-3382-5941], Rafelski, M [0000-0002-9946-4731], Rose, C [0000-0002-8018-3219], Seillé, LM [0000-0001-7755-4755], Somerville, RS [0000-0002-6748-6821], Straughn, AN [0000-0002-4772-7878], Tacchella, S [0000-0002-8224-4505], Vanderhoof, BN [0000-0002-8163-0172], Weiner, BJ [0000-0001-6065-7483], Wuyts, S [0000-0003-3735-1931], and Zavala, JA [0000-0002-7051-1100]

Subjects
similar-to 2, SIMILAR-TO 2, NEAR-INFRARED SPECTROSCOPY, COLLISION STRENGTHS, near-infrared spectroscopy, MASS-METALLICITY RELATION, FOS: Physical sciences, CHEMICAL-COMPOSITION, Galaxies and Cosmology, collision strengths, LY-ALPHA, atomic database, STAR-FORMING GALAXIES, MOSDEF SURVEY, mosdef survey, NEBULAR EMISSION, Astronomy and Astrophysics, mass-metallicity relation, star-forming galaxies, Astrophysics - Astrophysics of Galaxies, ATOMIC DATABASE, ly-alpha, nebular emission, Space and Planetary Science, 5101 Astronomical Sciences, Astrophysics of Galaxies (astro-ph.GA), chemical-composition, 51 Physical Sciences
Abstract

We present rest-frame optical emission-line flux ratio measurements for five $z>5$ galaxies observed by the JWST Near-Infared Spectrograph (NIRSpec) in the SMACS 0723 Early Release Observations. We add several quality-control and post-processing steps to the NIRSpec pipeline reduction products in order to ensure reliable relative flux calibration of emission lines that are closely separated in wavelength, despite the uncertain \textit{absolute} spectrophotometry of the current version of the reductions. Compared to $z\sim3$ galaxies in the literature, the $z>5$ galaxies have similar [OIII]$\lambda$5008/H$\beta$ ratios, similar [OIII]$\lambda$4364/H$\gamma$ ratios, and higher ($\sim$0.5 dex) [NeIII]$\lambda$3870/[OII]$\lambda$3728 ratios. We compare the observations to MAPPINGS V photoionization models and find that the measured [NeIII]$\lambda$3870/[OII]$\lambda$3728, [OIII]$\lambda$4364/H$\gamma$, and [OIII]$\lambda$5008/H$\beta$ emission-line ratios are consistent with an interstellar medium that has very high ionization ($\log(Q) \simeq 8-9$, units of cm~s$^{-1}$), low metallicity ($Z/Z_\odot \lesssim 0.2$), and very high pressure ($\log(P/k) \simeq 8-9$, units of cm$^{-3}$). The combination of [OIII]$\lambda$4364/H$\gamma$ and [OIII]$\lambda$(4960+5008)/H$\beta$ line ratios indicate very high electron temperatures of $4.1, Comment: Accepted for publication in AAS Journals. 14 pages, 6 figures, 3 tables

Published
2023
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