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51. The Radio Galaxy Environment Reference Survey (RAGERS): a submillimetre study of the environments of massive radio-quiet galaxies at z = 1–3.

Author: Cornish, Thomas M, Wardlow, Julie L, Greve, Thomas R, Chapman, Scott, Chen, Chian-Chou, Dannerbauer, Helmut, Goto, Tomotsugu, Gullberg, Bitten, Ho, Luis C, Jiang, Xue-Jian, Lagos, Claudia, Lee, Minju, Serjeant, Stephen, Shim, Hyunjin, Smith, Daniel J B, Vijayan, Aswin, Wagg, Jeff, and Zhou, Dazhi
Subjects: RADIO galaxies, GALACTIC evolution, GALACTIC redshift, ACTIVE galactic nuclei, STAR formation, SUBMILLIMETER astronomy
Abstract: Measuring the environments of massive galaxies at high redshift is crucial to understanding galaxy evolution and the conditions that gave rise to the distribution of matter we see in the Universe today. While high- z radio galaxies (H z RGs) and quasars tend to reside in protocluster-like systems, the environments of their radio-quiet counterparts are relatively unexplored, particularly in the submillimetre, which traces dust-obscured star formation. In this study, we search for 850 μ m-selected submillimetre galaxies (SMGs) in the environments of massive (⁠|$M_{\star }$| |$\gt 10^{11}$| |${\rm M}_{\odot }$|⁠), radio-quiet (⁠|$L_{500 {\rm MHz}}$| |$\lesssim 10^{25}$| WHz |$^{-1}$|⁠) galaxies at |$z \sim 1\!-\!3$| using data from the SCUBA-2 COSMOS (S2COSMOS) survey. By constructing number counts in circular regions of radius 1–6 arcmin and comparing with blank-field measurements, we find no significant overdensities of SMGs around massive radio-quiet galaxies at any of these scales, despite being sensitive down to overdensities of |$\delta \sim 0.4$|⁠. To probe deeper than the catalogue we also examine the distribution of peaks in the SCUBA-2 signal-to-noise (SNR) map, which reveals only tentative signs of any difference in the SMG densities of the radio-quiet galaxy environments compared to the blank field, and only on smaller scales (1 arcmin radii, corresponding to |$\sim 0.5$| Mpc) and higher SNR thresholds. We conclude that massive, radio-quiet galaxies at cosmic noon are typically in environments with |$\delta \lesssim 0.4$|⁠ , which are either consistent with the blank field or contain only weak overdensities spanning sub-Mpc scales. The contrast between our results and studies of H z RGs with similar stellar masses and redshifts implies an intrinsic link between the wide-field environment and the radio luminosity of the active galactic nucleus at high redshift. [ABSTRACT FROM AUTHOR]
Published: 2024
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52. MIDIS: JWST NIRCam and MIRI Unveil the Stellar Population Properties of Lyα Emitters and Lyman-break Galaxies at z ≃ 3–7

Author: Iani, Edoardo, primary, Caputi, Karina I., additional, Rinaldi, Pierluigi, additional, Annunziatella, Marianna, additional, Boogaard, Leindert A., additional, Östlin, Göran, additional, Costantin, Luca, additional, Gillman, Steven, additional, Pérez-González, Pablo G., additional, Colina, Luis, additional, Greve, Thomas R., additional, Wright, Gillian, additional, Alonso-Herrero, Almudena, additional, Álvarez-Márquez, Javier, additional, Bik, Arjan, additional, Bosman, Sarah E. I., additional, Gómez, Alejandro Crespo, additional, Eckart, Andreas, additional, Hjorth, Jens, additional, Jermann, Iris, additional, Labiano, Alvaro, additional, Langeroodi, Danial, additional, Melinder, Jens, additional, Moutard, Thibaud, additional, Peißker, Florian, additional, Pye, John P., additional, Tikkanen, Tuomo V., additional, van der Werf, Paul P., additional, Walter, Fabian, additional, Henning, Thomas K., additional, Lagage, Pierre-Olivier, additional, and van Dishoeck, Ewine F., additional
Published: 2024
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53. Confirming the Quiescent Galaxy Population out to $z=3$: A Stacking Analysis of Mid-, Far-Infrared and Radio Data

Author: Man, Allison W. S., Greve, Thomas R., Toft, Sune, Magnelli, Benjamin, Karim, Alexander, Ilbert, Olivier, Salvato, Mara, Floc'h, Emeric Le, Bertoldi, Frank, Casey, Caitlin M., Lee, Nicholas, Li, Yanxia, Navarrete, Felipe, Sheth, Kartik, Smolcic, Vernesa, Sanders, David B., Schinnerer, Eva, and Zirm, Andrew W.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present stringent constraints on the average mid-, far-infrared and radio emissions of $\sim$14200 quiescent galaxies (QGs), identified out to $z=3$ in the COSMOS field via their rest-frame NUV$-$r and r$-$J colors, and with stellar masses $M_{\star}=10^{9.8-12.2} \,M_{\odot} $. Stacking in deep Spitzer (MIPS $24\,\mu$m), Herschel (PACS and SPIRE), and VLA (1.4 GHz) maps reveals extremely low dust-obscured star formation rates for QGs (SFR $<0.1-3\,M_{\odot}$yr$^{-1}$ at $z \leqslant 2$ and $<6-18\,M_{\odot}$yr$^{-1}$ at $z > 2$), consistent with the low unobscured SFRs ($<0.01-1.2\,M_{\odot}$yr$^{-1}$) inferred from modeling their ultraviolet-to-near-infrared photometry. The average SFRs of QGs are $>10\times$ below those of star-forming galaxies (SFGs) within the $M_{\star}$- and $z$-ranges considered. The stacked 1.4 GHz signals (S/N $> 5$) are, if attributed solely to star formation, in excess of the total (obscured plus unobscured) SFR limits, suggestive of a widespread presence of low-luminosity active galactic nuclei (AGN) among QGs. Our results reaffirm the existence of a significant population QGs out to $z = 3$, thus corroborating the need for powerful quenching mechanism(s) to terminate star formation in galaxies at earlier epochs., Comment: 7 pages, 3 color figures, 2 tables (including a landscape table). Submitted to ApJL. Comments welcome
Published: 2014
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54. Molecular gas heating mechanisms, and star formation feedback in merger/s tarbursts: NGC 6240 and Arp 193 as case studies

Author: Papadopoulos, Padelis P., Zhang, Zhi-Yu, Xilouris, E. M., Weiss, Axel, van der Werf, Paul, Israel, Frank. P., Greve, Thomas. R., Isaak, Kate G., and Gao, Yu
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We used the SPIRE/FTS instrument aboard the Herschel Space Observatory (HSO) to obtain the Spectral Line Energy Distributions (SLEDs) of CO from J=4-3 to J=13-12 of Arp 193 and NGC 6240, two classical merger/starbursts selected from our molecular line survey of local Luminous Infrared Galaxies (LIRGs: L_{IR}>=10^{11} L_{sol}). The high-J CO SLEDs are then combined with ground-based low-J CO, {13}CO, HCN, HCO+, CS line data and used to probe the thermal and dynamical states of their large molecular gas reservoirs. We find the two CO SLEDs strongly diverging from J=4-3 onwards, with NGC6240 having a much higher CO line excitation than Arp193, despite their similar low-J CO SLEDs and L_{FIR}/L_{CO,1-0}, L_{HCN}/L_{CO} (J=1-0) ratios (proxies of star formation efficiency and dense gas mass fraction). In Arp193, one of the three most extreme starbursts in the local Universe, the molecular SLEDs indicate a small amount ~(5-15)% of dense gas (n>=10^{4}cm^{-3}) unlike NGC6240 where most of the molecular gas (~(60-70)%) is dense n~(10^4-10^5)cm^{-3}. Strong star-formation feedback can drive this disparity in their dense gas mass fractions, and also induce extreme thermal and dynamical states for the molecular gas.In NGC6240, and to a lesser degree in Arp193, we find large molecular gas masses whose thermal states cannot be maintained by FUV photons from Photon Dominated Regions (PDRs). We argue that this may happen often in metal-rich merger/starbursts, strongly altering the initial conditions of star formation. ALMA can now directly probe these conditions across cosmic epoch, and even probe their deeply dust-enshrouded outcome, the stellar IMF averaged over galactic evolution., Comment: 54 pages, 19 figures, accepted for publication in The Astrophysical Journal
Published: 2014
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55. DEIMOS spectroscopy of z=6 protocluster candidate in COSMOS - a massive protocluster embedded in a large-scale structure?

Author: Brinch, Malte, Greve, Thomas R, Sanders, David B, Mcpartland, Conor J R, Chartab, Nima, Gillman, Steven, Vijayan, Aswin P, Lee, Minju M, Brammer, Gabriel, Casey, Caitlin M, Ilbert, Olivier, Jin, Shuowen, Magdis, Georgios, Mccracken, H J, Sillassen, Nikolaj B, Toft, Sune, Zavala, Jorge A, Brinch, Malte, Greve, Thomas R, Sanders, David B, Mcpartland, Conor J R, Chartab, Nima, Gillman, Steven, Vijayan, Aswin P, Lee, Minju M, Brammer, Gabriel, Casey, Caitlin M, Ilbert, Olivier, Jin, Shuowen, Magdis, Georgios, Mccracken, H J, Sillassen, Nikolaj B, Toft, Sune, and Zavala, Jorge A
Published: 2024

56. The molecular gas in Luminous Infrared Galaxies: a new emergent picture

Author: Papadopoulos, Padelis P., Zhang, Zhi-Yu, Weiss, Axel, van der Werf, Paul, Isaak, Kate, Gao, Yu, Xilouris, Manolis, and Greve, Thomas R.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Results from a large, multi-J CO, {13}CO, and HCN line survey of Luminous Infrared Galaxies (L_{IR}>=10^{10} L_{\odot}) in the local Universe (z<=0.1), complemented by CO J=4--3 up to J=13--12 observations from the Herschel Space Observatory (HSO), paints a new picture for the average conditions of the molecular gas of the most luminous of these galaxies with turbulence and/or large cosmic ray (CR) energy densities U_{CR} rather than far-UV/optical photons from star-forming sites as the dominant heating sources. Especially in ULIRGs (L_{IR}>10^{12} L_{\odot}) the Photon Dominated Regions (PDRs) can encompass at most \sim few% of their molecular gas mass while the large U_{CR} and the strong turbulence in these merger/starbursts, can volumetrically heat much of their molecular gas to T_{kin}\sim(100-200)K, unhindered by the high dust extinctions. Moreover the strong supersonic turbulence in ULIRGs relocates much of their molecular gas at much higher average densities than in isolated spirals. This renders low-J CO lines incapable of constraining the properties of the bulk of the molecular gas in ULIRGs, with substantial and systematic underestimates of its mass possible when only such lines are used. A comparative study of multi-J HCN lines and CO SLEDs from J=1--0 up to J=13--12 of NGC 6240 and Arp 193 offers a clear example of two merger/starbursts whose similar low-J CO SLEDs, and L_{IR}/L_{CO,1-0}, L_{HCN, 1-0}/L_{CO,1-0} ratios, yield no indications about their strongly diverging CO SLEDs beyond J=4--3, and ultimately the different physical conditions in their molecular ISM. The much larger sensitivity of ALMA and its excellent site in the Atacama desert now allows the observations necessary to ...., Comment: 6 pages, 5 figures, invited talk at the IAU Symposium No 292, Beijing, China, 2013
Published: 2012
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57. Panchromatic Estimation of Star Formation Rates in BzK Galaxies at 1<z<3

Author: Kurczynski, Peter, Gawiser, Eric, Huynh, Minh, Ivison, Rob J., Treister, Ezequiel, Smail, Ian, Blanc, Guillermo A., Cardamone, Carolin N., Greve, Thomas R., Schinnerer, Eva, Urry, Meg, and van der Werf, Paul
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We determine star formation rates (SFRs) in a sample of color-selected, star-forming (sBzK) galaxies (K(AB)<21.8) in the Extended Chandra Deep Field - South. To identify and avoid active galactic nuclei, we use X-ray, IRAC color, and IR/radio flux ratio selection methods. Photometric redshift-binned, average flux densities are measured with stacking analyses in Spitzer-MIPS IR, BLAST and APEX/LABOCA submillimeter, VLA and GMRT radio and Chandra X-ray data. We include averages of aperture fluxes in MUSYC UBVRIz'JHK images to determine UV-through-radio spectral energy distributions. We determine the total IR luminosities and compare SFR calibrations from FIR, 24 micron, UV, radio and X-ray wavebands. We find consistency with our best estimator, SFR(IR+UV), to within errors for the preferred radio SFR calibration. Our results imply that 24 micron only and X-ray SFR estimates should be applied to high redshift galaxies with caution. Average IR luminosities are consistent with luminous infrared galaxies. We find SFR(IR+UV) for our stacked sBzKs at median redshifts 1.4, 1.8, and 2.2 to be 55+/-6 (random error), 74+/-8 and 154+/-17 Msun yr^-1 respectively, with additional systematic uncertainty of a factor of ~2., Comment: 27 pages, 6 figures, 8 tables. Accepted for publication in The Astrophysical Journal
Published: 2010
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58. Origins of the extragalactic background at 1mm from a combined analysis of the AzTEC and MAMBO data in GOODS-N

Author: Penner, Kyle, Pope, Alexandra, Chapin, Edward L., Greve, Thomas R., Bertoldi, Frank, Brodwin, Mark, Chary, Ranga-Ram, Conselice, Christopher J., Coppin, Kristen, Giavalisco, Mauro, Hughes, David H., Ivison, Rob J., Perera, Thushara, Scott, Douglas, Scott, Kimberly, and Wilson, Grant
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a study of the cosmic infrared background, which is a measure of the dust obscured activity in all galaxies in the Universe. We venture to isolate the galaxies responsible for the background at 1mm; with spectroscopic and photometric redshifts we constrain the redshift distribution of these galaxies. We create a deep 1.16mm map (sigma ~ 0.5mJy) by combining the AzTEC 1.1mm and MAMBO 1.2mm datasets in GOODS-N. This combined map contains 41 secure detections, 13 of which are new. By averaging the 1.16mm flux densities of individually undetected galaxies with 24um flux densities > 25uJy, we resolve 31--45 per cent of the 1.16mm background. Repeating our analysis on the SCUBA 850um map, we resolve a higher percentage (40--64 per cent) of the 850um background. A majority of the background resolved (attributed to individual galaxies) at both wavelengths comes from galaxies at z > 1.3. If the ratio of the resolved submillimeter to millimeter background is applied to a reasonable scenario for the origins of the unresolved submillimeter background, 60--88 per cent of the total 1.16mm background comes from galaxies at z > 1.3., Comment: 12 pages, 10 figures. Accepted by MNRAS. The combined map is publicly available at http://www.astro.umass.edu/~pope/goodsn_mm/
Published: 2010
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59. A joint analysis of BLAST 250--500um and LABOCA 870um observations in the Extended Chandra Deep Field South

Author: Chapin, Edward L., Chapman, Scott C., Coppin, Kristen E., Devlin, Mark J., Dunlop, James S., Greve, Thomas R., Halpern, Mark, Hasselfield, Matthew F., Hughes, David H., Ivison, Rob J., Marsden, Gaelen, Moncelsi, Lorenzo, Netterfield, Calvin B., Pascale, Enzo, Scott, Douglas, Smail, Ian, Viero, Marco, Walter, Fabian, Weiss, Axel, and van der Werf, Paul
Subjects: Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract: We present a joint analysis of the overlapping BLAST 250, 350, 500um, and LABOCA 870um observations (from the LESS survey) of the ECDF-S. Out to z~3, the BLAST filters sample near the peak wavelength of far-infrared (FIR) emission from galaxies (rest-frame wavelengths ~60--200um), primarily produced by dust heated through absorption in star-forming clouds. However, identifying counterparts to individual BLAST peaks is very challenging, given the large beams (FWHM 36--60"). In contrast, the 870um observations have a significantly smaller 19" FWHM beam, and are sensitive to higher redshifts (z~1--5, and potentially beyond) due to the more favourable negative K-correction. We use the LESS data, as well as deep Spitzer and VLA imaging, to identify 118 individual sources that produce significant emission in the BLAST bands. We characterize the temperatures and FIR luminosities for a subset of 69 sources which have well-measured submm SEDs and redshift measurements out to z~3. For flux-limited sub-samples in each BLAST band, and a dust emissivity index \beta=2.0, we find a median temperature T=30K (all bands) as well as median redshifts: z=1.1 (interquartile range 0.2--1.9) for S250 > 40mJy; z=1.3 (interquartile range 0.6--2.1) for S350 > 30mJy; and z=1.6 (interquartile range 1.3--2.3) for S500 > 20mJy. Taking into account selection effects for our survey (a bias toward detecting lower-temperature galaxies), we find no evidence for evolution in the local FIR-temperature correlation out to z~2.5. Comparing with star-forming galaxy SED templates, about 8% of our sample appears to exhibit significant excesses in the radio and/or mid-IR, consistent with those sources harbouring an AGN. We describe the following techniques in two appendices: our `matched filter' for identifying sources in the presence of point-source confusion; and our approach for identifying counterparts using likelihood ratios., Comment: 54 pages, 16 figures, 10 tables. Accepted by MNRAS. This revision matches the accepted version: source list reduced from 125 to 118 objects; additional tests for matching catalogue, flux bias, and clustering; and simulation of SPIRE data. Data (maps, catalogues) are available at http://www.blastexperiment.info/results.php
Published: 2010
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60. A high-redshift calibration of the [O I]-to-H I conversion factor in star-forming galaxies.

Author: Wilson, Sophia N., Heintz, Kasper E., Jakobsson, Páll, Madden, Suzanne C., Watson, Darach, Magdis, Georgios, Valentino, Francesco, Greve, Thomas R., and Vizgan, David
Subjects: GAMMA ray bursts, GALAXIES, GALACTIC evolution, INTERSTELLAR medium, GALACTIC redshift, GAS reservoirs
Abstract: The assembly and build-up of neutral atomic hydrogen (H I) in galaxies is one of the most fundamental processes in galaxy formation and evolution. Studying this process directly in the early universe is hindered by the weakness of the hyperfine 21-cm H I line transition, impeding direct detections and measurements of the H I gas masses (MHI). Here we present a new method to infer MHI of high-redshift galaxies using neutral, atomic oxygen as a proxy. Specifically, we derive metallicity-dependent conversion factors relating the far-infrared [O I]-63 μm and [O I]-145 μm emission line luminosities and MHI in star-forming galaxies at z ≈ 2 − 6 using gamma-ray bursts (GRBs) as probes. We calibrate the [O I]-to-H I conversion factor relying on a sample of local galaxies with direct measurements of MHI and [O I]-63 μm and [O I]-145 μm line luminosities in addition to the SIGAME hydrodynamical simulation framework at similar epochs (z ≈ 0). We find that the [O I]63 μm-to-H I and [O I]145 μm-to-H I conversion factors, here denoted β[OI]−63 μm and β[OI]−145 μm, respectively, universally appear to be anti-correlated with the gas-phase metallicity. The GRB measurements further predict a mean ratio of L[OI]−63 μm/L[OI]−145 μm = 1.55 ± 0.12 and reveal generally less excited [C II] over [O I] compared to the local galaxy sample. The z ≈ 0 galaxy sample also shows systematically higher β[OI]−63 μm and β[OI]−145 μm conversion factors than the GRB sample, indicating either suppressed [O I] emission in local galaxies likely due to their lower hydrogen densities or more extended, diffuse H I gas reservoirs traced by the H I 21-cm. Finally, we apply these empirical calibrations to the few detections of [O I]-63 μm and [O I]-145 μm line transitions at z ≈ 2 from the literature and further discuss the applicability of these conversion factors to probe the H I gas content in the dense, star-forming interstellar medium (ISM) of galaxies well into the epoch of reionization. [ABSTRACT FROM AUTHOR]
Published: 2024
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61. First Light And Reionisation Epoch Simulations (FLARES) XII: The consequences of star-dust geometry on galaxies in the EoR

Author: Vijayan, Aswin P, primary, Thomas, Peter A, additional, Lovell, Christopher C, additional, Wilkins, Stephen M, additional, Greve, Thomas R, additional, Irodotou, Dimitrios, additional, Roper, William J, additional, and Seeyave, Louise T C, additional
Published: 2023
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62. DEIMOS spectroscopy of z = 6 protocluster candidate in COSMOS – a massive protocluster embedded in a large-scale structure?

Author: Brinch, Malte, primary, Greve, Thomas R, additional, Sanders, David B, additional, McPartland, Conor J R, additional, Chartab, Nima, additional, Gillman, Steven, additional, Vijayan, Aswin P, additional, Lee, Minju M, additional, Brammer, Gabriel, additional, Casey, Caitlin M, additional, Ilbert, Olivier, additional, Jin, Shuowen, additional, Magdis, Georgios, additional, McCracken, H J, additional, Sillassen, Nikolaj B, additional, Toft, Sune, additional, and Zavala, Jorge A, additional
Published: 2023
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63. MINDS

Author: Gasman, Danny, primary, van Dishoeck, Ewine F., additional, Grant, Sierra L., additional, Temmink, Milou, additional, Tabone, Benoît, additional, Henning, Thomas, additional, Kamp, Inga, additional, Güdel, Manuel, additional, Lagage, Pierre-Olivier, additional, Perotti, Giulia, additional, Christiaens, Valentin, additional, Samland, Matthias, additional, Arabhavi, Aditya M., additional, Argyriou, Ioannis, additional, Abergel, Alain, additional, Absil, Olivier, additional, Barrado, David, additional, Boccaletti, Anthony, additional, Bouwman, Jeroen, additional, Caratti o Garatti, Alessio, additional, Geers, Vincent, additional, Glauser, Adrian M., additional, Guadarrama, Rodrigo, additional, Jang, Hyerin, additional, Kanwar, Jayatee, additional, Lahuis, Fred, additional, Morales-Calderón, Maria, additional, Mueller, Michael, additional, Nehmé, Cyrine, additional, Olofsson, Göran, additional, Pantin, Éric, additional, Pawellek, Nicole, additional, Ray, Tom P., additional, Rodgers-Lee, Donna, additional, Scheithauer, Silvia, additional, Schreiber, Jürgen, additional, Schwarz, Kamber, additional, Vandenbussche, Bart, additional, Vlasblom, Marissa, additional, Waters, Rens L. B. F. M., additional, Wright, Gillian, additional, Colina, Luis, additional, Greve, Thomas R., additional, and Östlin, Göran, additional
Published: 2023
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64. The nature of faint Spitzer-selected dust-obscured galaxies

Author: Pope, Alexandra, Bussmann, R. Shane, Dey, Arjun, Meger, Nicole, Alexander, David M., Brodwin, Mark, Chary, Ranga-Ram, Dickinson, Mark E., Frayer, David T., Greve, Thomas R., Huynh, Minh, Lin, Lihwai, Morrison, Glenn, Scott, Douglas, and Yan, Chi-Hung
Subjects: Astrophysics
Abstract: We use deep far-IR, submm, radio and X-ray imaging and mid-IR spectroscopy to explore the nature of a sample of Spitzer-selected dust-obscured galaxies (DOGs) in GOODS-N. A sample of 79 galaxies satisfy the criteria R-[24]>14 (Vega) down to S24>100 microJy. Twelve of these galaxies have IRS spectra available which we use to measure redshifts and classify these objects as being dominated by star formation or active galactic nuclei (AGN) activity in the mid-IR. The IRS spectra and Spitzer photometric redshifts confirm that the DOGs lie in a tight redshift distribution around z~2. Based on mid-IR colors, 80% of DOGs are likely dominated by star formation; the stacked X-ray emission from this sub-sample of DOGs is also consistent with star formation. Since only a small number of DOGs are individually detected at far-IR and submm wavelengths, we use a stacking analysis to determine the average flux from these objects and plot a composite IR (8-1000 microns) spectral energy distribution (SED). The average luminosity of these star forming DOGs is LIR~1e12 Lsun. We compare the average star forming DOG to the average bright (S850>5 mJy) submillimeter galaxy (SMG); the S24>100 microJy DOGs are 3 times more numerous but 8 times less luminous in the IR. The far-IR SED shape of DOGs is similar to that of SMGs (average dust temperature of around 30 K) but DOGs have a higher mid-IR to far-IR flux ratio. The average star formation-dominated DOG has a star formation rate of 200 Msun/yr which, given their space density, amounts to a contribution of 0.01 Msun/yr/Mpc3 (or 5-10%) to the star formation rate density at z~2. We use the composite SED to predict the average flux of DOGs in future Herschel/PACS 100 micron and SCUBA-2 450 micron surveys and show that the majority of them will be detected., Comment: 7 pages, 5 figures; accepted for publication in ApJ
Published: 2008
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65. A large CO and HCN line survey of Luminous Infrared Galaxies

Author: Papadopoulos, Padelis P., Greve, Thomas R., van der Werf, Paul, Müehle, Stefanie, Isaak, Kate, and Gao, Yu
Subjects: Astrophysics
Abstract: A large CO, HCN multi-transition survey of 30 Luminous Infrared Galaxies ($\rm L_{IR}>10^{11} L_{\odot}$) is nearing completion with the James Clerk Maxwell Telescope (JCMT) on Mauna Kea (Hawaii), and the IRAM 30-meter telescope at Pico Veleta (Spain). The CO J=1--0, 2--1, 3--2, 4--3,6--5, $ ^{13}$CO J=2--1, HCN J=1--0, 3--2, 4--3 observations, resulting from $\sim 250$ hours of JCMT, $\sim 100$ hours of 30-m observing time and data from the literature constitute {\it the largest extragalactic molecular line survey to date}, and can be used to address a wide range of issues and eventually allow the construction of reliable Spectral Line Energy Distributions (SLEDs) for the molecular gas in local starbursts. First results suggest that: a) HCN and HCO$^+$ J=1--0 line luminosities can be poor mass estimators of dense molecular gas ($\rm n\geq 10^4 cm^{-3}$) unless their excitation is accounted for, b) CO cooling of such gas in ULIRGs may be comparable to that of the CII line at $\rm 158 \mu m$, and c) low excitation of the {\it global} molecular gas reservoir remains possible in such systems. In such cases the expected low CO $\rm J+1\to J$ line luminosities for $\rm J+1\geq 4$ can lead to a strong bias against their detection from ULIRGs at high redshifts., Comment: 4 pages, to appear in Astrophysics and Space Science (special issue for 2006 conference "Science with ALMA: a new era for Astrophysics")
Published: 2007

66. CI emission in Ultra Luminous Infrared Galaxies as a molecular gas mass tracer

Author: Papadopoulos, Padeli P. and Greve, Thomas R.
Subjects: Astrophysics
Abstract: We present new sensitive wide-band measurements of the fine structure line 3^P_1 -> 3^P_0 (J=1-0, 492GHz) of neutral atomic carbon (CI) in the two typical Ultra Luminous Infrared Galaxies NGC6240 and Arp220. We then use them along with several other CI measurements in similar objects found in the literature to estimate their global molecular gas content under the assumption of a full CI-H_2 concomitance. We find excellent agreement between the H_2 gas mass estimated with this method and the standard methods using 12^CO. This may provide a new way to measure H_2 gas mass in galaxies, and one which may be very valuable in ULIRGs since in such systems the bright 12^CO emission is known to systematically overestimate the gas mass while their 13^CO emission is usually very weak. At redshifts z>=1 the CI J=1-0 line shifts to much more favorable atmospheric windows and can become a viable alternative tracer of the H_2 gas fueling starburst events in the distant Universe., Comment: 11 pages, 2 figures. Accepted for publication in ApJ Letters
Published: 2004
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67. Dust and gas in the early universe : an observational perspective on galaxy formation and evolution

Author: Greve, Thomas R.
Subjects: 520
Abstract: The first part of the thesis presents the results from unbiased surveys at millimetre (1200 μm) and radio (1.4 GHz) wavelengths of the ELAIS N2 and Lockman Hole East fields both of which have previously been mapped at 850 μm. From the first survey the most accurate number counts at 1200 μm to date are derived and are found to match simple parametric models of galaxy evolution remarkably well. Exploiting the well-matched data in all three wavebands we address the issue of the stability of low signal-to-noise (sub)mm surveys and extract an extremely robust sample of sources detected in the radio and both of the (sub)mm bands. Constraints are also imposed on the redshift distribution of submm sources using spectral templates representative of local starburst galaxies. The radio data is used in conjunction with optical/near-infrared imaging to obtain robust radio counterparts and thereby pinpoint the location of the optical/near-infrared host galaxies for an unprecedented large sample of submm sources. The optical/near-infrared colours and morphologies are summarised revealing that about 60 per cent of the host galaxies display highly structured or complex morphology, suggestive of merging or interacting systems. In the second part of the thesis the potential of the molecule carbonmonoxide (CO) to trace gas and the properties of the interstellar medium of galaxies at high redshifts is explored. A simple numerical code which simulates the non-LTE excitation conditions of CO in a spherical molecular cloud of H2 is constructed and is subsequently used to constrain the density and kinetic temperature in two case-studies of high redshift galaxies. Finally, the results from a first systematic interferometric CO survey of luminous submm galaxies are presented. The bulk properties such as gas mass and CO linewidths of an unprecedented large sample of bright submm galaxies are derived and compared with local starburst galaxies as well with other galaxy populations at high redshifts. Based on the average dynamical and total baryonic masses as well as the typical gas exhaustion time of submm galaxies an evolutionary scenario is proposed which attempts to link them to massive evolved galaxies at z ~1 and old giant ellipticals at the present day. Lower limits are imposed on the co-moving number density of massive galaxies at high redshifts and a comparison with predictions from semi-analytical models of galaxy formation reveals the shortcomings of current models to explain the rapid assembly of massive galaxies in the early Universe.
Published: 2005

68. Sub-millimetre galaxies with Webb

Author: Gillman, Steven, primary, Gullberg, Bitten, additional, Brammer, Gabe, additional, Vijayan, Aswin P., additional, Lee, Minju, additional, Blánquez, David, additional, Brinch, Malte, additional, Greve, Thomas R., additional, Jermann, Iris, additional, Jin, Shuowen, additional, Kokorev, Vasily, additional, Liu, Lijie, additional, Magdis, Georgios, additional, Rizzo, Francesca, additional, and Valentino, Francesco, additional
Published: 2023
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69. Life beyond 30: Probing the −20 < M UV < −17 Luminosity Function at 8 < z < 13 with the NIRCam Parallel Field of the MIRI Deep Survey

Author: Pérez-González, Pablo G., primary, Costantin, Luca, additional, Langeroodi, Danial, additional, Rinaldi, Pierluigi, additional, Annunziatella, Marianna, additional, Ilbert, Olivier, additional, Colina, Luis, additional, Nørgaard-Nielsen, Hans Ulrik, additional, Greve, Thomas R., additional, Östlin, Göran, additional, Wright, Gillian, additional, Alonso-Herrero, Almudena, additional, Álvarez-Márquez, Javier, additional, Caputi, Karina I., additional, Eckart, Andreas, additional, Le Fèvre, Olivier, additional, Labiano, Álvaro, additional, García-Marín, Macarena, additional, Hjorth, Jens, additional, Kendrew, Sarah, additional, Pye, John P., additional, Tikkanen, Tuomo, additional, van der Werf, Paul, additional, Walter, Fabian, additional, Ward, Martin, additional, Bik, Arjan, additional, Boogaard, Leindert, additional, Bosman, Sarah E. I., additional, Gómez, Alejandro Crespo, additional, Gillman, Steven, additional, Iani, Edoardo, additional, Jermann, Iris, additional, Melinder, Jens, additional, Meyer, Romain A., additional, Moutard, Thibaud, additional, van Dishoek, Ewine, additional, Henning, Thomas, additional, Lagage, Pierre-Olivier, additional, Guedel, Manuel, additional, Peissker, Florian, additional, Ray, Tom, additional, Vandenbussche, Bart, additional, García-Argumánez, Ángela, additional, and María Mérida, Rosa, additional
Published: 2023
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70. The James Webb Space Telescope Mission

Author: Gardner, Jonathan P., primary, Mather, John C., additional, Abbott, Randy, additional, Abell, James S., additional, Abernathy, Mark, additional, Abney, Faith E., additional, Abraham, John G., additional, Abraham, Roberto, additional, Abul-Huda, Yasin M., additional, Acton, Scott, additional, Adams, Cynthia K., additional, Adams, Evan, additional, Adler, David S., additional, Adriaensen, Maarten, additional, Aguilar, Jonathan Albert, additional, Ahmed, Mansoor, additional, Ahmed, Nasif S., additional, Ahmed, Tanjira, additional, Albat, Rüdeger, additional, Albert, Loïc, additional, Alberts, Stacey, additional, Aldridge, David, additional, Allen, Mary Marsha, additional, Allen, Shaune S., additional, Altenburg, Martin, additional, Altunc, Serhat, additional, Alvarez, Jose Lorenzo, additional, Álvarez-Márquez, Javier, additional, de Oliveira, Catarina Alves, additional, Ambrose, Leslie L., additional, Anandakrishnan, Satya M., additional, Andersen, Gregory C., additional, Anderson, Harry James, additional, Anderson, Jay, additional, Anderson, Kristen, additional, Anderson, Sara M., additional, Aprea, Julio, additional, Archer, Benita J., additional, Arenberg, Jonathan W., additional, Argyriou, Ioannis, additional, Arribas, Santiago, additional, Artigau, Étienne, additional, Arvai, Amanda Rose, additional, Atcheson, Paul, additional, Atkinson, Charles B., additional, Averbukh, Jesse, additional, Aymergen, Cagatay, additional, Bacinski, John J., additional, Baggett, Wayne E., additional, Bagnasco, Giorgio, additional, Baker, Lynn L., additional, Balzano, Vicki Ann, additional, Banks, Kimberly A., additional, Baran, David A., additional, Barker, Elizabeth A., additional, Barrett, Larry K., additional, Barringer, Bruce O., additional, Barto, Allison, additional, Bast, William, additional, Baudoz, Pierre, additional, Baum, Stefi, additional, Beatty, Thomas G., additional, Beaulieu, Mathilde, additional, Bechtold, Kathryn, additional, Beck, Tracy, additional, Beddard, Megan M., additional, Beichman, Charles, additional, Bellagama, Larry, additional, Bely, Pierre, additional, Berger, Timothy W., additional, Bergeron, Louis E., additional, Bernier, Antoine-Darveau, additional, Bertch, Maria D., additional, Beskow, Charlotte, additional, Betz, Laura E., additional, Biagetti, Carl P., additional, Birkmann, Stephan, additional, Bjorklund, Kurt F., additional, Blackwood, James D., additional, Blazek, Ronald Paul, additional, Blossfeld, Stephen, additional, Bluth, Marcel, additional, Boccaletti, Anthony, additional, Boegner Jr, Martin E., additional, Bohlin, Ralph C., additional, Boia, John Joseph, additional, Böker, Torsten, additional, Bonaventura, N., additional, Bond, Nicholas A., additional, Bosley, Kari Ann, additional, Boucarut, Rene A., additional, Bouchet, Patrice, additional, Bouwman, Jeroen, additional, Bower, Gary, additional, Bowers, Ariel S., additional, Bowers, Charles W., additional, Boyce, Leslye A., additional, Boyer, Christine T., additional, Boyer, Martha L., additional, Boyer, Michael, additional, Boyer, Robert, additional, Bradley, Larry D., additional, Brady, Gregory R., additional, Brandl, Bernhard R., additional, Brannen, Judith L., additional, Breda, David, additional, Bremmer, Harold G., additional, Brennan, David, additional, Bresnahan, Pamela A., additional, Bright, Stacey N., additional, Broiles, Brian J., additional, Bromenschenkel, Asa, additional, Brooks, Brian H., additional, Brooks, Keira J., additional, Brown, Bob, additional, Brown, Bruce, additional, Brown, Thomas M., additional, Bruce, Barry W., additional, Bryson, Jonathan G., additional, Bujanda, Edwin D., additional, Bullock, Blake M., additional, Bunker, A. J., additional, Bureo, Rafael, additional, Burt, Irving J., additional, Bush, James Aaron, additional, Bushouse, Howard A., additional, Bussman, Marie C., additional, Cabaud, Olivier, additional, Cale, Steven, additional, Calhoon, Charles D., additional, Calvani, Humberto, additional, Canipe, Alicia M., additional, Caputo, Francis M., additional, Cara, Mihai, additional, Carey, Larkin, additional, Case, Michael Eli, additional, Cesari, Thaddeus, additional, Cetorelli, Lee D., additional, Chance, Don R., additional, Chandler, Lynn, additional, Chaney, Dave, additional, Chapman, George N., additional, Charlot, S., additional, Chayer, Pierre, additional, Cheezum, Jeffrey I., additional, Chen, Bin, additional, Chen, Christine H., additional, Cherinka, Brian, additional, Chichester, Sarah C., additional, Chilton, Zachary S., additional, Chittiraibalan, Dharini, additional, Clampin, Mark, additional, Clark, Charles R., additional, Clark, Kerry W., additional, Clark, Stephanie M., additional, Claybrooks, Edward E., additional, Cleveland, Keith A., additional, Cohen, Andrew L., additional, Cohen, Lester M., additional, Colón, Knicole D., additional, Coleman, Benee L., additional, Colina, Luis, additional, Comber, Brian J., additional, Comeau, Thomas M., additional, Comer, Thomas, additional, Reis, Alain Conde, additional, Connolly, Dennis C., additional, Conroy, Kyle E., additional, Contos, Adam R., additional, Contreras, James, additional, Cook, Neil J., additional, Cooper, James L., additional, Cooper, Rachel Aviva, additional, Correia, Michael F., additional, Correnti, Matteo, additional, Cossou, Christophe, additional, Costanza, Brian F., additional, Coulais, Alain, additional, Cox, Colin R., additional, Coyle, Ray T., additional, Cracraft, Misty M., additional, Crew, Keith A., additional, Curtis, Gary J., additional, Cusveller, Bianca, additional, Maciel, Cleyciane Da Costa, additional, Dailey, Christopher T., additional, Daugeron, Frédéric, additional, Davidson, Greg S., additional, Davies, James E., additional, Davis, Katherine Anne, additional, Davis, Michael S., additional, Day, Ratna, additional, de Chambure, Daniel, additional, de Jong, Pauline, additional, De Marchi, Guido, additional, Dean, Bruce H., additional, Decker, John E., additional, Delisa, Amy S., additional, Dell, Lawrence C., additional, Dellagatta, Gail, additional, Dembinska, Franciszka, additional, Demosthenes, Sandor, additional, Dencheva, Nadezhda M., additional, Deneu, Philippe, additional, DePriest, William W., additional, Deschenes, Jeremy, additional, Dethienne, Nathalie, additional, Detre, Örs Hunor, additional, Diaz, Rosa Izela, additional, Dicken, Daniel, additional, DiFelice, Audrey S., additional, Dillman, Matthew, additional, Disharoon, Maureen O., additional, Dixon, William V., additional, Doggett, Jesse B., additional, Dominguez, Keisha L., additional, Donaldson, Thomas S., additional, Doria-Warner, Cristina M., additional, Santos, Tony Dos, additional, Doty, Heather, additional, Douglas, Jr, Robert E., additional, Doyon, René, additional, Dressler, Alan, additional, Driggers, Jennifer, additional, Driggers, Phillip A., additional, Dunn, Jamie L., additional, DuPrie, Kimberly C., additional, Dupuis, Jean, additional, Durning, John, additional, Dutta, Sanghamitra B., additional, Earl, Nicholas M., additional, Eccleston, Paul, additional, Ecobichon, Pascal, additional, Egami, Eiichi, additional, Ehrenwinkler, Ralf, additional, Eisenhamer, Jonathan D., additional, Eisenhower, Michael, additional, Eisenstein, Daniel J., additional, El Hamel, Zaky, additional, Elie, Michelle L., additional, Elliott, James, additional, Elliott, Kyle Wesley, additional, Engesser, Michael, additional, Espinoza, Néstor, additional, Etienne, Odessa, additional, Etxaluze, Mireya, additional, Evans, Leah, additional, Fabreguettes, Luce, additional, Falcolini, Massimo, additional, Falini, Patrick R., additional, Fatig, Curtis, additional, Feeney, Matthew, additional, Feinberg, Lee D., additional, Fels, Raymond, additional, Ferdous, Nazma, additional, Ferguson, Henry C., additional, Ferrarese, Laura, additional, Ferreira, Marie-Héléne, additional, Ferruit, Pierre, additional, Ferry, Malcolm, additional, Filippazzo, Joseph Charles, additional, Firre, Daniel, additional, Fix, Mees, additional, Flagey, Nicolas, additional, Flanagan, Kathryn A., additional, Fleming, Scott W., additional, Florian, Michael, additional, Flynn, James R., additional, Foiadelli, Luca, additional, Fontaine, Mark R., additional, Fontanella, Erin Marie, additional, Forshay, Peter Randolph, additional, Fortner, Elizabeth A., additional, Fox, Ori D., additional, Framarini, Alexandro P., additional, Francisco, John I., additional, Franck, Randy, additional, Franx, Marijn, additional, Franz, David E., additional, Friedman, Scott D., additional, Friend, Katheryn E., additional, Frost, James R., additional, Fu, Henry, additional, Fullerton, Alexander W., additional, Gaillard, Lionel, additional, Galkin, Sergey, additional, Gallagher, Ben, additional, Galyer, Anthony D., additional, García Marín, Macarena, additional, Gardner, Lisa E., additional, Garland, Dennis, additional, Garrett, Bruce Albert, additional, Gasman, Danny, additional, Gáspár, András, additional, Gastaud, René, additional, Gaudreau, Daniel, additional, Gauthier, Peter Timothy, additional, Geers, Vincent, additional, Geithner, Paul H., additional, Gennaro, Mario, additional, Gerber, John, additional, Gereau, John C., additional, Giampaoli, Robert, additional, Giardino, Giovanna, additional, Gibbons, Paul C., additional, Gilbert, Karoline, additional, Gilman, Larry, additional, Girard, Julien H., additional, Giuliano, Mark E., additional, Gkountis, Konstantinos, additional, Glasse, Alistair, additional, Glassmire, Kirk Zachary, additional, Glauser, Adrian Michael, additional, Glazer, Stuart D., additional, Goldberg, Joshua, additional, Golimowski, David A., additional, Gonzaga, Shireen P., additional, Gordon, Karl D., additional, Gordon, Shawn J., additional, Goudfrooij, Paul, additional, Gough, Michael J., additional, Graham, Adrian J., additional, Grau, Christopher M., additional, Green, Joel David, additional, Greene, Gretchen R., additional, Greene, Thomas P., additional, Greenfield, Perry E., additional, Greenhouse, Matthew A., additional, Greve, Thomas R., additional, Greville, Edgar M., additional, Grimaldi, Stefano, additional, Groe, Frank E., additional, Groebner, Andrew, additional, Grumm, David M., additional, Grundy, Timothy, additional, Güdel, Manuel, additional, Guillard, Pierre, additional, Guldalian, John, additional, Gunn, Christopher A., additional, Gurule, Anthony, additional, Gutman, Irvin Meyer, additional, Guy, Paul D., additional, Guyot, Benjamin, additional, Hack, Warren J., additional, Haderlein, Peter, additional, Hagan, James B., additional, Hagedorn, Andria, additional, Hainline, Kevin, additional, Haley, Craig, additional, Hami, Maryam, additional, Hamilton, Forrest Clifford, additional, Hammann, Jeffrey, additional, Hammel, Heidi B., additional, Hanley, Christopher J., additional, Hansen, Carl August, additional, Hardy, Bruce, additional, Harnisch, Bernd, additional, Harr, Michael Hunter, additional, Harris, Pamela, additional, Hart, Jessica Ann, additional, Hartig, George F., additional, Hasan, Hashima, additional, Hashim, Kathleen Marie, additional, Hashimoto, Ryan, additional, Haskins, Sujee J., additional, Hawkins, Robert Edward, additional, Hayden, Brian, additional, Hayden, William L., additional, Healy, Mike, additional, Hecht, Karen, additional, Heeg, Vince J., additional, Hejal, Reem, additional, Helm, Kristopher A., additional, Hengemihle, Nicholas J., additional, Henning, Thomas, additional, Henry, Alaina, additional, Henry, Ronald L., additional, Henshaw, Katherine, additional, Hernandez, Scarlin, additional, Herrington, Donald C., additional, Heske, Astrid, additional, Hesman, Brigette Emily, additional, Hickey, David L., additional, Hilbert, Bryan N., additional, Hines, Dean C., additional, Hinz, Michael R., additional, Hirsch, Michael, additional, Hitcho, Robert S., additional, Hodapp, Klaus, additional, Hodge, Philip E., additional, Hoffman, Melissa, additional, Holfeltz, Sherie T., additional, Holler, Bryan Jason, additional, Hoppa, Jennifer Rose, additional, Horner, Scott, additional, Howard, Joseph M., additional, Howard, Richard J., additional, Huber, Jean M., additional, Hunkeler, Joseph S., additional, Hunter, Alexander, additional, Hunter, David Gavin, additional, Hurd, Spencer W., additional, Hurst, Brendan J., additional, Hutchings, John B., additional, Hylan, Jason E., additional, Ignat, Luminita Ilinca, additional, Illingworth, Garth, additional, Irish, Sandra M., additional, Isaacs III, John C., additional, Jackson Jr, Wallace C., additional, Jaffe, Daniel T., additional, Jahic, Jasmin, additional, Jahromi, Amir, additional, Jakobsen, Peter, additional, James, Bryan, additional, James, John C., additional, James, LeAndrea Rae, additional, Jamieson, William Brian, additional, Jandra, Raymond D., additional, Jayawardhana, Ray, additional, Jedrzejewski, Robert, additional, Jeffers, Basil S., additional, Jensen, Peter, additional, Joanne, Egges, additional, Johns, Alan T., additional, Johnson, Carl A., additional, Johnson, Eric L., additional, Johnson, Patricia, additional, Johnson, Phillip Stephen, additional, Johnson, Thomas K., additional, Johnson, Timothy W., additional, Johnstone, Doug, additional, Jollet, Delphine, additional, Jones, Danny P., additional, Jones, Gregory S., additional, Jones, Olivia C., additional, Jones, Ronald A., additional, Jones, Vicki, additional, Jordan, Ian J., additional, Jordan, Margaret E., additional, Jue, Reginald, additional, Jurkowski, Mark H., additional, Justis, Grant, additional, Justtanont, Kay, additional, Kaleida, Catherine C., additional, Kalirai, Jason S., additional, Kalmanson, Phillip Cabrales, additional, Kaltenegger, Lisa, additional, Kammerer, Jens, additional, Kan, Samuel K., additional, Kanarek, Graham Childs, additional, Kao, Shaw-Hong, additional, Karakla, Diane M., additional, Karl, Hermann, additional, Kassin, Susan A., additional, Kauffman, David D., additional, Kavanagh, Patrick, additional, Kelley, Leigh L., additional, Kelly, Douglas M., additional, Kendrew, Sarah, additional, Kennedy, Herbert V., additional, Kenny, Deborah A., additional, Keski-Kuha, Ritva A., additional, Keyes, Charles D., additional, Khan, Ali, additional, Kidwell, Richard C., additional, Kimble, Randy A., additional, King, James S., additional, King, Richard C., additional, Kinzel, Wayne M., additional, Kirk, Jeffrey R., additional, Kirkpatrick, Marc E., additional, Klaassen, Pamela, additional, Klingemann, Lana, additional, Klintworth, Paul U., additional, Knapp, Bryan Adam, additional, Knight, Scott, additional, Knollenberg, Perry J., additional, Knutsen, Daniel Mark, additional, Koehler, Robert, additional, Koekemoer, Anton M., additional, Kofler, Earl T., additional, Kontson, Vicki L., additional, Kovacs, Aiden Rose, additional, Kozhurina-Platais, Vera, additional, Krause, Oliver, additional, Kriss, Gerard A., additional, Krist, John, additional, Kristoffersen, Monica R., additional, Krogel, Claudia, additional, Krueger, Anthony P., additional, Kulp, Bernard A., additional, Kumari, Nimisha, additional, Kwan, Sandy W., additional, Kyprianou, Mark, additional, Labador, Aurora Gadiano, additional, Labiano, Álvaro, additional, Lafrenière, David, additional, Lagage, Pierre-Olivier, additional, Laidler, Victoria G., additional, Laine, Benoit, additional, Laird, Simon, additional, Lajoie, Charles-Philippe, additional, Lallo, Matthew D., additional, Lam, May Yen, additional, LaMassa, Stephanie Marie, additional, Lambros, Scott D., additional, Lampenfield, Richard Joseph, additional, Lander, Matthew Ed, additional, Langston, James Hutton, additional, Larson, Kirsten, additional, Larson, Melora, additional, LaVerghetta, Robert Joseph, additional, Law, David R., additional, Lawrence, Jon F., additional, Lee, David W., additional, Lee, Janice, additional, Lee, Yat-Ning Paul, additional, Leisenring, Jarron, additional, Leveille, Michael Dunlap, additional, Levenson, Nancy A., additional, Levi, Joshua S., additional, Levine, Marie B., additional, Lewis, Dan, additional, Lewis, Jake, additional, Lewis, Nikole, additional, Libralato, Mattia, additional, Lidon, Norbert, additional, Liebrecht, Paula Louisa, additional, Lightsey, Paul, additional, Lilly, Simon, additional, Lim, Frederick C., additional, Lim, Pey Lian, additional, Ling, Sai-Kwong, additional, Link, Lisa J., additional, Link, Miranda Nicole, additional, Lipinski, Jamie L., additional, Liu, XiaoLi, additional, Lo, Amy S., additional, Lobmeyer, Lynette, additional, Logue, Ryan M., additional, Long, Chris A., additional, Long, Douglas R., additional, Long, Ilana D., additional, Long, Knox S., additional, López-Caniego, Marcos, additional, Lotz, Jennifer M., additional, Love-Pruitt, Jennifer M., additional, Lubskiy, Michael, additional, Luers, Edward B., additional, Luetgens, Robert A., additional, Luevano, Annetta J., additional, G. Flores Lui, Sarah Marie, additional, Lund III, James M., additional, Lundquist, Ray A., additional, Lunine, Jonathan, additional, Lützgendorf, Nora, additional, Lynch, Richard J., additional, MacDonald, Alex J., additional, MacDonald, Kenneth, additional, Macias, Matthew J., additional, Macklis, Keith I., additional, Maghami, Peiman, additional, Maharaja, Rishabh Y., additional, Maiolino, Roberto, additional, Makrygiannis, Konstantinos G., additional, Malla, Sunita Giri, additional, Malumuth, Eliot M., additional, Manjavacas, Elena, additional, Marini, Andrea, additional, Marrione, Amanda, additional, Marston, Anthony, additional, Martel, André R, additional, Martin, Didier, additional, Martin, Peter G., additional, Martinez, Kristin L., additional, Maschmann, Marc, additional, Masci, Gregory L., additional, Masetti, Margaret E., additional, Maszkiewicz, Michael, additional, Matthews, Gary, additional, Matuskey, Jacob E., additional, McBrayer, Glen A., additional, McCarthy, Donald W., additional, McCaughrean, Mark J., additional, McClare, Leslie A., additional, McClare, Michael D., additional, McCloskey, John C., additional, McClurg, Taylore D., additional, McCoy, Martin, additional, McElwain, Michael W., additional, McGregor, Roy D., additional, McGuffey, Douglas B., additional, McKay, Andrew G., additional, McKenzie, William K., additional, McLean, Brian, additional, McMaster, Matthew, additional, McNeil, Warren, additional, De Meester, Wim, additional, Mehalick, Kimberly L., additional, Meixner, Margaret, additional, Meléndez, Marcio, additional, Menzel, Michael P., additional, Menzel, Michael T., additional, Merz, Matthew, additional, Mesterharm, David D., additional, Meyer, Michael R., additional, Meyett, Michele L., additional, Meza, Luis E., additional, Midwinter, Calvin, additional, Milam, Stefanie N., additional, Miller, Jay Todd, additional, Miller, William C., additional, Miskey, Cherie L., additional, Misselt, Karl, additional, Mitchell, Eileen P., additional, Mohan, Martin, additional, Montoya, Emily E., additional, Moran, Michael J., additional, Morishita, Takahiro, additional, Moro-Martín, Amaya, additional, Morrison, Debra L., additional, Morrison, Jane, additional, Morse, Ernie C., additional, Moschos, Michael, additional, Moseley, S. H., additional, Mosier, Gary E., additional, Mosner, Peter, additional, Mountain, Matt, additional, Muckenthaler, Jason S., additional, Mueller, Donald G., additional, Mueller, Migo, additional, Muhiem, Daniella, additional, Mühlmann, Prisca, additional, Mullally, Susan Elizabeth, additional, Mullen, Stephanie M., additional, Munger, Alan J, additional, Murphy, Jess, additional, Murray, Katherine T., additional, Muzerolle, James C., additional, Mycroft, Matthew, additional, Myers, Andrew, additional, Myers, Carey R., additional, R. Myers, Fred Richard, additional, Myers, Richard, additional, Myrick, Kaila, additional, Nagle, IV, Adrian F., additional, Nayak, Omnarayani, additional, Naylor, Bret, additional, Neff, Susan G., additional, Nelan, Edmund P., additional, Nella, John, additional, Nguyen, Duy Tuong, additional, Nguyen, Michael N., additional, Nickson, Bryony, additional, Nidhiry, John Joseph, additional, Niedner, Malcolm B., additional, Nieto-Santisteban, Maria, additional, Nikolov, Nikolay K., additional, Nishisaka, Mary Ann, additional, Noriega-Crespo, Alberto, additional, Nota, Antonella, additional, O’Mara, Robyn C., additional, Oboryshko, Michael, additional, O’Brien, Marcus B., additional, Ochs, William R., additional, Offenberg, Joel D., additional, Ogle, Patrick Michael, additional, Ohl, Raymond G., additional, Olmsted, Joseph Hamden, additional, Osborne, Shannon Barbara, additional, O’Shaughnessy, Brian Patrick, additional, Östlin, Göran, additional, O’Sullivan, Brian, additional, Otor, O. Justin, additional, Ottens, Richard, additional, Ouellette, Nathalie N.-Q., additional, Outlaw, Daria J., additional, Owens, Beverly A., additional, Pacifici, Camilla, additional, Page, James Christophe, additional, Paranilam, James G., additional, Park, Sang, additional, Parrish, Keith A., additional, Paschal, Laura, additional, Patapis, Polychronis, additional, Patel, Jignasha, additional, Patrick, Keith, additional, Pattishall Jr, Robert A., additional, Paul, Douglas William, additional, Paul, Shirley J., additional, Pauly, Tyler Andrew, additional, Pavlovsky, Cheryl M., additional, Peña-Guerrero, Maria, additional, Pedder, Andrew H., additional, Peek, Matthew Weldon, additional, Pelham, Patricia A., additional, Penanen, Konstantin, additional, Perriello, Beth A., additional, Perrin, Marshall D., additional, Perrine, Richard F., additional, Perrygo, Chuck, additional, Peslier, Muriel, additional, Petach, Michael, additional, Peterson, Karla A., additional, Pfarr, Tom, additional, Pierson, James M., additional, Pietraszkiewicz, Martin, additional, Pilchen, Guy, additional, Pipher, Judy L., additional, Pirzkal, Norbert, additional, Pitman, Joseph T., additional, Player, Danielle M., additional, Plesha, Rachel, additional, Plitzke, Anja, additional, Pohner, John A., additional, Poletis, Karyn Konstantin, additional, Pollizzi, Joseph A., additional, Polster, Ethan, additional, Pontius, James T., additional, Pontoppidan, Klaus, additional, Porges, Susana C., additional, Potter, Gregg D., additional, Prescott, Stephen, additional, Proffitt, Charles R., additional, Pueyo, Laurent, additional, Quispe Neira, Irma Aracely, additional, Radich, Armando, additional, Rager, Reiko T., additional, Rameau, Julien, additional, Ramey, Deborah D., additional, Alarcon, Rafael Ramos, additional, Rampini, Riccardo, additional, Rapp, Robert, additional, Rashford, Robert A., additional, Rauscher, Bernard J., additional, Ravindranath, Swara, additional, Rawle, Timothy, additional, Rawlings, Tynika N., additional, Ray, Tom, additional, Regan, Michael W., additional, Rehm, Brian, additional, Rehm, Kenneth D., additional, Reid, Neill, additional, Reis, Carl A., additional, Renk, Florian, additional, Reoch, Tom B., additional, Ressler, Michael, additional, Rest, Armin W., additional, Reynolds, Paul J., additional, Richon, Joel G., additional, Richon, Karen V., additional, Ridgaway, Michael, additional, Riedel, Adric Richard, additional, Rieke, George H., additional, Rieke, Marcia J., additional, Rifelli, Richard E., additional, Rigby, Jane R., additional, Riggs, Catherine S., additional, Ringel, Nancy J., additional, Ritchie, Christine E., additional, Rix, Hans-Walter, additional, Robberto, Massimo, additional, Robinson, Gregory L., additional, Robinson, Michael S., additional, Robinson, Orion, additional, Rock, Frank W., additional, Rodriguez, David R., additional, del Pino, Bruno Rodríguez, additional, Roellig, Thomas, additional, Rohrbach, Scott O., additional, Roman, Anthony J., additional, Romelfanger, Frederick J., additional, Romo Jr, Felipe P., additional, Rosales, Jose J., additional, Rose, Perry, additional, Roteliuk, Anthony F., additional, Roth, Marc N., additional, Rothwell, Braden Quinn, additional, Rouzaud, Sylvain, additional, Rowe, Jason, additional, Rowlands, Neil, additional, Roy, Arpita, additional, Royer, Pierre, additional, Rui, Chunlei, additional, Rumler, Peter, additional, Rumpl, William, additional, Russ, Melissa L., additional, Ryan, Michael B., additional, Ryan, Richard M., additional, Saad, Karl, additional, Sabata, Modhumita, additional, Sabatino, Rick, additional, Sabbi, Elena, additional, Sabelhaus, Phillip A., additional, Sabia, Stephen, additional, Sahu, Kailash C., additional, Saif, Babak N., additional, Salvignol, Jean-Christophe, additional, Samara-Ratna, Piyal, additional, Samuelson, Bridget S., additional, Sanders, Felicia A., additional, Sappington, Bradley, additional, Sargent, B. A., additional, Sauer, Arne, additional, Savadkin, Bruce J., additional, Sawicki, Marcin, additional, Schappell, Tina M., additional, Scheffer, Caroline, additional, Scheithauer, Silvia, additional, Scherer, Ron, additional, Schiff, Conrad, additional, Schlawin, Everett, additional, Schmeitzky, Olivier, additional, Schmitz, Tyler S., additional, Schmude, Donald J., additional, Schneider, Analyn, additional, Schreiber, Jürgen, additional, Schroeven-Deceuninck, Hilde, additional, Schultz, John J., additional, Schwab, Ryan, additional, Schwartz, Curtis H., additional, Scoccimarro, Dario, additional, Scott, John F., additional, Scott, Michelle B., additional, Seaton, Bonita L., additional, Seely, Bruce S., additional, Seery, Bernard, additional, Seidleck, Mark, additional, Sembach, Kenneth, additional, Shanahan, Clare Elizabeth, additional, Shaughnessy, Bryan, additional, Shaw, Richard A., additional, Shay, Christopher Michael, additional, Sheehan, Even, additional, Sheth, Kartik, additional, Shih, Hsin-Yi, additional, Shivaei, Irene, additional, Siegel, Noah, additional, Sienkiewicz, Matthew G., additional, Simmons, Debra D., additional, Simon, Bernard P., additional, Sirianni, Marco, additional, Sivaramakrishnan, Anand, additional, Slade, Jeffrey E., additional, Sloan, G. C., additional, Slocum, Christine E., additional, Slowinski, Steven E., additional, Smith, Corbett T., additional, Smith, Eric P., additional, Smith, Erin C., additional, Smith, Koby, additional, Smith, Robert, additional, Smith, Stephanie J., additional, Smolik, John L., additional, Soderblom, David R., additional, Sohn, Sangmo Tony, additional, Sokol, Jeff, additional, Sonneborn, George, additional, Sontag, Christopher D., additional, Sooy, Peter R., additional, Soummer, Remi, additional, Southwood, Dana M., additional, Spain, Kay, additional, Sparmo, Joseph, additional, Speer, David T., additional, Spencer, Richard, additional, Sprofera, Joseph D., additional, Stallcup, Scott S., additional, Stanley, Marcia K., additional, Stansberry, John A., additional, Stark, Christopher C., additional, Starr, Carl W., additional, Stassi, Diane Y., additional, Steck, Jane A., additional, Steeley, Christine D., additional, Stephens, Matthew A., additional, Stephenson, Ralph J., additional, Stewart, Alphonso C., additional, Stiavelli, Massimo, additional, Jr, Hervey Stockman, additional, Strada, Paolo, additional, Straughn, Amber N., additional, Streetman, Scott, additional, Strickland, David Kendal, additional, Strobele, Jingping F., additional, Stuhlinger, Martin, additional, Stys, Jeffrey Edward, additional, Such, Miguel, additional, Sukhatme, Kalyani, additional, Sullivan, Joseph F., additional, Sullivan, Pamela C., additional, Sumner, Sandra M., additional, Sun, Fengwu, additional, Sunnquist, Benjamin Dale, additional, Swade, Daryl Allen, additional, Swam, Michael S., additional, Swenton, Diane F., additional, Swoish, Robby A., additional, Tam Litten, Oi In, additional, Tamas, Laszlo, additional, Tao, Andrew, additional, Taylor, David K., additional, Taylor, Joanna M., additional, Plate, Maurice te, additional, Van Tea, Mason, additional, Teague, Kelly K., additional, Telfer, Randal C., additional, Temim, Tea, additional, Texter, Scott C., additional, Thatte, Deepashri G., additional, Thompson, Christopher Lee, additional, Thompson, Linda M., additional, Thomson, Shaun R., additional, Thronson, Harley, additional, Tierney, C. M., additional, Tikkanen, Tuomo, additional, Tinnin, Lee, additional, Tippet, William Thomas, additional, Todd, Connor William, additional, Tran, Hien D., additional, Trauger, John, additional, Trejo, Edwin Gregorio, additional, Vinh Truong, Justin Hoang, additional, Tsukamoto, Christine L., additional, Tufail, Yasir, additional, Tumlinson, Jason, additional, Tustain, Samuel, additional, Tyra, Harrison, additional, Ubeda, Leonardo, additional, Underwood, Kelli, additional, Uzzo, Michael A., additional, Vaclavik, Steven, additional, Valenduc, Frida, additional, Valenti, Jeff A., additional, Van Campen, Julie, additional, van de Wetering, Inge, additional, Van Der Marel, Roeland P., additional, van Haarlem, Remy, additional, Vandenbussche, Bart, additional, van Dishoeck, Ewine F., additional, Vanterpool, Dona D., additional, Vernoy, Michael R., additional, Vila Costas, Maria Begoña, additional, Volk, Kevin, additional, Voorzaat, Piet, additional, Voyton, Mark F., additional, Vydra, Ekaterina, additional, Waddy, Darryl J., additional, Waelkens, Christoffel, additional, Wahlgren, Glenn Michael, additional, Walker Jr, Frederick E., additional, Wander, Michel, additional, Warfield, Christine K., additional, Warner, Gerald, additional, Wasiak, Francis C., additional, Wasiak, Matthew F., additional, Wehner, James, additional, Weiler, Kevin R., additional, Weilert, Mark, additional, Weiss, Stanley B., additional, Wells, Martyn, additional, Welty, Alan D., additional, Wheate, Lauren, additional, Wheeler, Thomas P., additional, White, Christy L., additional, Whitehouse, Paul, additional, Whiteleather, Jennifer Margaret, additional, Whitman, William Russell, additional, Williams, Christina C., additional, Willmer, Christopher N. A., additional, Willott, Chris J., additional, Willoughby, Scott P., additional, Wilson, Andrew, additional, Wilson, Debra, additional, Wilson, Donna V., additional, Windhorst, Rogier, additional, Wislowski, Emily Christine, additional, Wolfe, David J., additional, Wolfe, Michael A., additional, Wolff, Schuyler, additional, Wondel, Amancio, additional, Woo, Cindy, additional, Woods, Robert T., additional, Worden, Elaine, additional, Workman, William, additional, Wright, Gillian S., additional, Wu, Carl, additional, Wu, Chi-Rai, additional, Wun, Dakin D., additional, Wymer, Kristen B., additional, Yadetie, Thomas, additional, Yan, Isabelle C., additional, Yang, Keith C., additional, Yates, Kayla L., additional, Yeager, Christopher R., additional, Yerger, Ethan John, additional, Young, Erick T., additional, Young, Gary, additional, Yu, Gene, additional, Yu, Susan, additional, Zak, Dean S., additional, Zeidler, Peter, additional, Zepp, Robert, additional, Zhou, Julia, additional, Zincke, Christian A., additional, Zonak, Stephanie, additional, and Zondag, Elisabeth, additional
Published: 2023
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71. The ISM in the z = 6.9 Interacting Galaxies of SPT0311-58

Author: Litke, Katrina C., primary, Marrone, Daniel P., additional, Aravena, Manuel, additional, Archipley, Melanie, additional, Béthermin, Matthieu, additional, Burgoyne, James, additional, Cathey, Jared, additional, Chapman, Scott C., additional, Gonzalez, Anthony H., additional, Greve, Thomas R., additional, Gururajan, Gayathri, additional, Hayward, Christopher C., additional, Malkan, Matthew A., additional, Phadke, Kedar A., additional, Reuter, Cassie A., additional, Rotermund, Kaja M., additional, Spilker, Justin S., additional, Stark, Antony A., additional, Sulzenauer, Nikolaus, additional, Vieira, Joaquin D., additional, Vizgan, David, additional, and Weiß, Axel, additional
Published: 2023
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72. Life beyond 30:Probing the −20 < M UV < −17 Luminosity Function at 8 < z < 13 with the NIRCam Parallel Field of the MIRI Deep Survey

Author: Pérez-gonzález, Pablo G., Costantin, Luca, Langeroodi, Danial, Rinaldi, Pierluigi, Annunziatella, Marianna, Ilbert, Olivier, Colina, Luis, Nørgaard-nielsen, Hans Ulrik, Greve, Thomas R., Östlin, Göran, Wright, Gillian, Alonso-herrero, Almudena, Álvarez-márquez, Javier, Caputi, Karina I., Eckart, Andreas, Le Fèvre, Olivier, Labiano, Álvaro, García-marín, Macarena, Hjorth, Jens, Kendrew, Sarah, Pye, John P., Tikkanen, Tuomo, Van Der Werf, Paul, Walter, Fabian, Ward, Martin, Bik, Arjan, Boogaard, Leindert, Bosman, Sarah E. I., Gómez, Alejandro Crespo, Gillman, Steven, Iani, Edoardo, Jermann, Iris, Melinder, Jens, Meyer, Romain A., Moutard, Thibaud, Van Dishoek, Ewine, Henning, Thomas, Lagage, Pierre-olivier, Guedel, Manuel, Peissker, Florian, Ray, Tom, Vandenbussche, Bart, García-argumánez, Ángela, and María Mérida, Rosa
Published: 2023
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73. Life beyond 30: Probing the −20 < MUV < −17 Luminosity Function at 8 < z < 13 with the NIRCam Parallel Field of the MIRI Deep Survey

Author: Pérez-González, Pablo G., Costantin, Luca, Langeroodi, Danial, Rinaldi, Pierluigi, Annunziatella, Marianna, Ilbert, Olivier, Colina, Luis, Nørgaard-Nielsen, Hans Ulrik, Greve, Thomas R., Östlin, Göran, Wright, Gillian, Alonso-Herrero, Almudena, Álvarez-Márquez, Javier, Caputi, Karina I., Eckart, Andreas, Le Fèvre, Olivier, Labiano, Álvaro, García-Marín, Macarena, Hjorth, Jens, Kendrew, Sarah, and Guedel, Manuel
Abstract: We present the ultraviolet luminosity function and an estimate of the cosmic star formation rate density at 8 < z < 13 derived from deep NIRCam observations taken in parallel with the MIRI Deep Survey of the Hubble Ultra Deep Field (HUDF), NIRCam covering the parallel field 2. Our deep (40 hr) NIRCam observations reach an F277W magnitude of 30.8 (5σ), more than 2 mag deeper than JWST public data sets already analyzed to find high-redshift galaxies. We select a sample of 44 z > 8 galaxy candidates based on their dropout nature in the F115W and/or F150W filters, a high probability for their photometric redshifts, estimated with three different codes, being at z > 8, good fits based on χ2 calculations, and predominant solutions compared to z < 8 alternatives. We find mild evolution in the luminosity function from z ∼ 13 to z ∼ 8, i.e., only a small increase in the average number density of ∼0.2 dex, while the faint-end slope and absolute magnitude of the knee remain approximately constant, with values α = − 2.2 ± 0.1, and M* = − 20.8 ± 0.2 mag. Comparing our results with the predictions of state-of-the-art galaxy evolution models, we find two main results: (1) a slower increase with time in the cosmic star formation rate density compared to a steeper rise predicted by models; (2) nearly a factor of 10 higher star formation activity concentrated in scales around 2 kpc in galaxies with stellar masses ∼108M⊙ during the first 350 Myr of the universe, z ∼ 12, with models matching better the luminosity density observational estimations ∼150 Myr later, by z ∼ 9., The Astrophysical Journal Letters, 951 (1), ISSN:2041-8205, ISSN:1967-2014, ISSN:2041-8213
Published: 2023

74. Life beyond 30 : Probing the-20 < M (UV) <-17 Luminosity Function at 8 < z < 13 with the NIRCam Parallel Field of the MIRI Deep Survey

Author: Perez-Gonzalez, Pablo G., Costantin, Luca, Langeroodi, Danial, Rinaldi, Pierluigi, Annunziatella, Marianna, Ilbert, Olivier, Colina, Luis, Norgaard-Nielsen, Hans Ulrik, Greve, Thomas R., Östlin, Göran, Wright, Gillian, Alonso-Herrero, Almudena, Aalvarez-Marquez, Javier, Caputi, Karina I., Eckart, Andreas, Le Fevre, Olivier, Labiano, Alvaro, Garcia-Marin, Macarena, Hjorth, Jens, Kendrew, Sarah, Pye, John P., Tikkanen, Tuomo, van der Werf, Paul, Walter, Fabian, Ward, Martin, Bik, Arjan, Boogaard, Leindert, Bosman, Sarah E. I., Gomez, Alejandro Crespo, Gillman, Steven, Iani, Edoardo, Jermann, Iris, Melinder, Jens, Meyer, Romain A., Moutard, Thibaud, van Dishoek, Ewine, Henning, Thomas, Lagage, Pierre-Olivier, Guedel, Manuel, Peissker, Florian, Ray, Tom, Vandenbussche, Bart, Garcia-Argumanez, Angela, Merida, Rosa Maria, Perez-Gonzalez, Pablo G., Costantin, Luca, Langeroodi, Danial, Rinaldi, Pierluigi, Annunziatella, Marianna, Ilbert, Olivier, Colina, Luis, Norgaard-Nielsen, Hans Ulrik, Greve, Thomas R., Östlin, Göran, Wright, Gillian, Alonso-Herrero, Almudena, Aalvarez-Marquez, Javier, Caputi, Karina I., Eckart, Andreas, Le Fevre, Olivier, Labiano, Alvaro, Garcia-Marin, Macarena, Hjorth, Jens, Kendrew, Sarah, Pye, John P., Tikkanen, Tuomo, van der Werf, Paul, Walter, Fabian, Ward, Martin, Bik, Arjan, Boogaard, Leindert, Bosman, Sarah E. I., Gomez, Alejandro Crespo, Gillman, Steven, Iani, Edoardo, Jermann, Iris, Melinder, Jens, Meyer, Romain A., Moutard, Thibaud, van Dishoek, Ewine, Henning, Thomas, Lagage, Pierre-Olivier, Guedel, Manuel, Peissker, Florian, Ray, Tom, Vandenbussche, Bart, Garcia-Argumanez, Angela, and Merida, Rosa Maria
Abstract: We present the ultraviolet luminosity function and an estimate of the cosmic star formation rate density at 8 < z < 13 derived from deep NIRCam observations taken in parallel with the MIRI Deep Survey of the Hubble Ultra Deep Field (HUDF), NIRCam covering the parallel field 2. Our deep (40 hr) NIRCam observations reach an F277W magnitude of 30.8 (5 & sigma;), more than 2 mag deeper than JWST public data sets already analyzed to find high-redshift galaxies. We select a sample of 44 z > 8 galaxy candidates based on their dropout nature in the F115W and/or F150W filters, a high probability for their photometric redshifts, estimated with three different codes, being at z > 8, good fits based on & chi; (2) calculations, and predominant solutions compared to z < 8 alternatives. We find mild evolution in the luminosity function from z & SIM; 13 to z & SIM; 8, i.e., only a small increase in the average number density of & SIM;0.2 dex, while the faint-end slope and absolute magnitude of the knee remain approximately constant, with values & alpha; = - 2.2 & PLUSMN; 0.1, and M * = - 20.8 & PLUSMN; 0.2 mag. Comparing our results with the predictions of state-of-the-art galaxy evolution models, we find two main results: (1) a slower increase with time in the cosmic star formation rate density compared to a steeper rise predicted by models; (2) nearly a factor of 10 higher star formation activity concentrated in scales around 2 kpc in galaxies with stellar masses & SIM;10(8) M (& ODOT;) during the first 350 Myr of the universe, z & SIM; 12, with models matching better the luminosity density observational estimations & SIM;150 Myr later, by z & SIM; 9.
Published: 2023
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75. MINDS. The Detection of 13CO2 with JWST-MIRI Indicates Abundant CO2 in a Protoplanetary Disk

Author: Grant, Sierra L., van Dishoeck, Ewine F., Tabone, Benoît, Gasman, Danny, Henning, Thomas, Kamp, Inga, Güdel, Manuel, Lagage, Pierre-Olivier, Bettoni, Giulio, Perotti, Giulia, Christiaens, Valentin, Samland, Matthias, Arabhavi, Aditya M., Argyriou, Ioannis, Abergel, Alain, Absil, Olivier, Barrado, David, Boccaletti, Anthony, Bouwman, Jeroen, Caratti o Garatti, Alessio, Geers, Vincent, Glauser, Adrian M., Guadarrama, Rodrigo, Jang, Hyerin, Kanwar, Jayatee, Lahuis, Fred, Morales-Calderón, Maria, Mueller, Michael, Nehmé, Cyrine, Olofsson, Göran, Pantin, Eric, Pawellek, Nicole, Ray, Tom P., Rodgers-Lee, Donna, Scheithauer, Silvia, Schreiber, Jürgen, Schwarz, Kamber, Temmink, Milou, Vandenbussche, Bart, Vlasblom, Marissa, Waters, L. B. F. M., Wright, Gillian, Colina, Luis, Greve, Thomas R., Justannont, Kay, Östlin, Göran, Grant, Sierra L., van Dishoeck, Ewine F., Tabone, Benoît, Gasman, Danny, Henning, Thomas, Kamp, Inga, Güdel, Manuel, Lagage, Pierre-Olivier, Bettoni, Giulio, Perotti, Giulia, Christiaens, Valentin, Samland, Matthias, Arabhavi, Aditya M., Argyriou, Ioannis, Abergel, Alain, Absil, Olivier, Barrado, David, Boccaletti, Anthony, Bouwman, Jeroen, Caratti o Garatti, Alessio, Geers, Vincent, Glauser, Adrian M., Guadarrama, Rodrigo, Jang, Hyerin, Kanwar, Jayatee, Lahuis, Fred, Morales-Calderón, Maria, Mueller, Michael, Nehmé, Cyrine, Olofsson, Göran, Pantin, Eric, Pawellek, Nicole, Ray, Tom P., Rodgers-Lee, Donna, Scheithauer, Silvia, Schreiber, Jürgen, Schwarz, Kamber, Temmink, Milou, Vandenbussche, Bart, Vlasblom, Marissa, Waters, L. B. F. M., Wright, Gillian, Colina, Luis, Greve, Thomas R., Justannont, Kay, and Östlin, Göran
Abstract: We present JWST-MIRI Medium Resolution Spectrometer (MRS) spectra of the protoplanetary disk around the low-mass T Tauri star GW Lup from the MIRI mid-INfrared Disk Survey Guaranteed Time Observations program. Emission from 12CO2, 13CO2, H2O, HCN, C2H2, and OH is identified with 13CO2 being detected for the first time in a protoplanetary disk. We characterize the chemical and physical conditions in the inner few astronomical units of the GW Lup disk using these molecules as probes. The spectral resolution of JWST-MIRI MRS paired with high signal-to-noise data is essential to identify these species and determine their column densities and temperatures. The Q branches of these molecules, including those of hot bands, are particularly sensitive to temperature and column density. We find that the 12CO2 emission in the GW Lup disk is coming from optically thick emission at a temperature of ∼400 K. 13CO2 is optically thinner and based on a lower temperature of ∼325 K, and thus may be tracing deeper into the disk and/or a larger emitting radius than 12CO2. The derived / ratio is orders of magnitude higher than previously derived for GW Lup and other targets based on Spitzer-InfraRed-Spectrograph data. This high column density ratio may be due to an inner cavity with a radius in between the H2O and CO2 snowlines and/or an overall lower disk temperature. This paper demonstrates the unique ability of JWST to probe inner disk structures and chemistry through weak, previously unseen molecular features.
Published: 2023
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76. Sub-millimetre galaxies with Webb Near-infrared counterparts and multi-wavelength morphology

Author: Gillman, Steven, Gullberg, Bitten, Brammer, Gabe, Vijayan, Aswin P., Lee, Minju, Blánquez, David, Brinch, Malte, Greve, Thomas R., Jermann, Iris, Jin, Shuowen, Kokorev, Vasily, Liu, Lijie, Magdis, Georgios, Rizzo, Francesca, Valentino, Francesco, Gillman, Steven, Gullberg, Bitten, Brammer, Gabe, Vijayan, Aswin P., Lee, Minju, Blánquez, David, Brinch, Malte, Greve, Thomas R., Jermann, Iris, Jin, Shuowen, Kokorev, Vasily, Liu, Lijie, Magdis, Georgios, Rizzo, Francesca, and Valentino, Francesco
Published: 2023

77. The ISM in the z = 6.9 Interacting Galaxies of SPT0311-58

Author: Litke, Katrina C., Marrone, Daniel P., Aravena, Manuel, Archipley, Melanie, Béthermin, Matthieu, Burgoyne, James, Cathey, Jared, Chapman, Scott C., Gonzalez, Anthony H., Greve, Thomas R., Gururajan, Gayathri, Hayward, Christopher C., Malkan, Matthew A., Phadke, Kedar A., Reuter, Cassie A., Rotermund, Kaja M., Spilker, Justin S., Stark, Antony A., Sulzenauer, Nikolaus, Vieira, Joaquin D., Vizgan, David, Weiß, Axel, Litke, Katrina C., Marrone, Daniel P., Aravena, Manuel, Archipley, Melanie, Béthermin, Matthieu, Burgoyne, James, Cathey, Jared, Chapman, Scott C., Gonzalez, Anthony H., Greve, Thomas R., Gururajan, Gayathri, Hayward, Christopher C., Malkan, Matthew A., Phadke, Kedar A., Reuter, Cassie A., Rotermund, Kaja M., Spilker, Justin S., Stark, Antony A., Sulzenauer, Nikolaus, Vieira, Joaquin D., Vizgan, David, and Weiß, Axel
Abstract: SPT0311-58, a system of two interacting galaxies in the Epoch of Reionization, exists in one of the rarest, most massive dark matter halos theoretically possible in that era. Studying the interstellar medium (ISM) in these galaxies can illuminate the process of galaxy formation in the early Universe. In this work, we explore the multiphase ISM in this system, using ALMA observations of the [C ii] 158, [O i] 146, [N ii] 122, and [O iii] 88 fine-structure lines and dust continuum. We find wide variations in line ratios between the eastern and western galaxies, as well as across the western galaxy.
Published: 2023

78. Revisiting the [C II]158µm line-intensity mapping power spectrum from the EoR using non-uniform line-luminosity scatter

Author: Murmu, Chandra Shekhar, Olsen, Karen P., Greve, Thomas R., Majumdar, Suman, Datta, Kanan K., Scott, Bryan R., Leung, T. K. Daisy, Dave, Romeel, Popping, Gergoe, Ochoa, Raul Ortega, Vizgan, David, Narayanan, Desika, Murmu, Chandra Shekhar, Olsen, Karen P., Greve, Thomas R., Majumdar, Suman, Datta, Kanan K., Scott, Bryan R., Leung, T. K. Daisy, Dave, Romeel, Popping, Gergoe, Ochoa, Raul Ortega, Vizgan, David, and Narayanan, Desika
Abstract: Detecting the line-intensity mapping (LIM) signal from the galaxies of the epoch of reionization is an emerging tool to constrain their role in reionization. Ongoing and upcoming experiments target the signal fluctuations across the sky to reveal statistical and astrophysical properties of these galaxies via signal statistics, e.g. the power spectrum. Here, we revisit the [C II](158 mu m) power spectrum under non-uniform line-luminosity scatter, which has a halo-mass variation of statistical properties. Line-luminosity scatter from a cosmological hydrodynamic and radiative transfer simulation of galaxies at z = 6 is considered in this study. We test the robustness of different model frameworks that interpret the impact of the line-luminosity scatter on the signal statistics. We use a simple power-law model to fit the scatter and demonstrate that the mean luminosity-halo mass correlation fit cannot preserve the mean intensity of the LIM signal (hence the clustering power spectrum) under non-uniform scatter. In our case, the mean intensity changes by similar to 48 per cent compared to the mean correlation fit in contrast to the general case with semi-analytical scatter. However, we find that the prediction for the mean intensity from the most-probable fit can be modelled robustly, considering the generalized and more realistic non-uniform scatter. We also explore the possibility of diminishing luminosity bias under non-uniform scatter, affecting the clustering power spectrum, although this phenomenon might not be statistically significant. Therefore, we should adopt appropriate approaches that can consistently interpret the LIM power spectrum from observations.
Published: 2023

79. Massive galaxy formation caught in action at z ∼ 5 with JWST

Author: Jin, Shuowen, Sillassen, Nikolaj B., Magdis, Georgios E., Vijayan, Aswin P., Brammer, Gabriel B., Kokorev, Vasily, Weaver, John R., Gobat, Raphael, Giménez-Arteaga, Clara, Valentino, Francesco, Brinch, Malte, Gómez-Guijarro, Carlos, Shuntov, Marko, Toft, Sune, Greve, Thomas R., Blanquez Sese, David, Jin, Shuowen, Sillassen, Nikolaj B., Magdis, Georgios E., Vijayan, Aswin P., Brammer, Gabriel B., Kokorev, Vasily, Weaver, John R., Gobat, Raphael, Giménez-Arteaga, Clara, Valentino, Francesco, Brinch, Malte, Gómez-Guijarro, Carlos, Shuntov, Marko, Toft, Sune, Greve, Thomas R., and Blanquez Sese, David
Abstract: We report the discovery of a compact group of galaxies, CGG-z5, at z ∼ 5.2 in the EGS field covered by the JWST/CEERS survey. CGG-z5 was selected as the highest overdensity of galaxies at z > 2 in recent JWST public surveys and it consists of six candidate members lying within a projected area of 1.5″ × 3″ (10×20 kpc2). All group members are HST/F435W and HST/F606W dropouts while securely detected in the JWST/NIRCam bands, yielding a narrow range of robust photometric redshifts 5.0 < z < 5.3. The most massive galaxy in the group has a stellar mass log(M*/M⊙)≈9.8, while the rest are low-mass satellites (log(M*/M⊙)≈8.4–9.2). While several group members were already detected in the HST and IRAC bands, the low stellar masses and the compactness of the structure required the sensitivity and resolution of JWST for its identification. To assess the nature and evolutionary path of CGG-z5, we searched for similar compact structures in the EAGLE simulations and followed their evolution with time. We find that all the identified structures merge into a single galaxy by z = 3 and form a massive galaxy (log(M*/M⊙)> 11) at z ∼ 1. This implies that CGG-z5 could be a “proto-massive galaxy” captured during a short-lived phase of massive galaxy formation.
Published: 2023

80. DEIMOS spectroscopy of z = 6 protocluster candidate in COSMOS – a massive protocluster embedded in a large-scale structure?

Author: Brinch, Malte, Greve, Thomas R, Sanders, David B, McPartland, Conor J R, Chartab, Nima, Gillman, Steven, Vijayan, Aswin P, Lee, Minju M, Brammer, Gabriel, Casey, Caitlin M, Ilbert, Olivier, Jin, Shuowen, Magdis, Georgios, McCracken, H J, Sillassen, Nikolaj B, Toft, Sune, and Zavala, Jorge A
Subjects: *SPECTRAL energy distribution, *STELLAR mass, *DARK matter, *LARGE scale structure (Astronomy), *GALACTIC redshift, *REDSHIFT, UNIVERSE
Abstract: We present the results of our Keck /DEep Imaging Multi-Object Spectrograph spectroscopic follow-up of candidate galaxies of i -band-dropout protocluster candidate galaxies at z ∼ 6 in the COSMOS field. We securely detect Lyman α emission lines in 14 of the 30 objects targeted, 10 of them being at z = 6 with a signal-to-noise ratio of 5–20; the remaining galaxies are either non-detections or interlopers with redshift too different from z = 6 to be part of the protocluster. The 10 galaxies at z ≈ 6 make the protocluster one of the riches at z > 5. The emission lines exhibit asymmetric profiles with high skewness values ranging from 2.87 to 31.75, with a median of 7.37. This asymmetry is consistent with them being Ly α, resulting in a redshift range of z = 5.85–6.08. Using the spectroscopic redshifts, we recalculate the overdensity map for the COSMOS field and find the galaxies to be in a significant overdensity at the 4σ level, with a peak overdensity of δ = 11.8 (compared to the previous value of δ = 9.2). The protocluster galaxies have stellar masses derived from Bagpipes spectral energy distribution fits of |$10^{8.29}\!-\!10^{10.28} \rm \, M_{\rm \odot }$| and star formation rates of |$2\!-\!39\, \rm M_{\rm \odot }\rm \, yr^{-1}$|⁠ , placing them on the main sequence at this epoch. Using a stellar-to-halo-mass relationship, we estimate the dark matter halo mass of the most massive halo in the protocluster to be |$\sim 10^{12}\rm M_{\rm \odot }$|⁠. By comparison with halo mass evolution tracks from simulations, the protocluster is expected to evolve into a Virgo- or Coma-like cluster in the present day. [ABSTRACT FROM AUTHOR]
Published: 2024
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81. First Light And Reionisation Epoch Simulations (FLARES) – XII: The consequences of star–dust geometry on galaxies in the EoR.

Author: Vijayan, Aswin P, Thomas, Peter A, Lovell, Christopher C, Wilkins, Stephen M, Greve, Thomas R, Irodotou, Dimitrios, Roper, William J, and Seeyave, Louise T C
Subjects: GALAXIES, STELLAR populations, STAR formation, STELLAR luminosity function, GALACTIC evolution, GEOMETRY
Abstract: Using the First Light And Reionisation Epoch Simulations, a suite of hydrodynamical simulations, we explore the consequences of a realistic model for star–dust geometry on the observed properties of galaxies. We find that the ultraviolet (UV) attenuation declines rapidly from the central regions of galaxies, and bright galaxies have spatially extended star formation that suffers less obscuration than their fainter counterparts, demonstrating a non-linear relationship between the UV luminosity and the UV attenuation, giving a double power-law shape to the UVLF. Spatially distinct stellar populations within galaxies experience a wide range of dust attenuation due to variations in the dust optical depth along their line of sight, which can range from completely dust obscured to being fully unobscured. The overall attenuation curve of a galaxy is then a complex combination of various lines of sight within the galaxy. We explore the manifestation of this effect to study the reliability of line ratios to infer galaxy properties, in particular, the Balmer decrement and the Baldwin, Phillips, and Terlevich (BPT) diagram. We find the Balmer decrement predicted Balmer-line attenuation to be higher (factor of 1 to ≳ 10) than expected from commonly used attenuation curves. The observed BPT line ratios deviate from their intrinsic values [median difference of 0.08 (0.02) and standard deviation of 0.2 (0.05) for log10([N |${\small II}]\lambda 6585/$| Hα) (log10([O iii ]λ5008/Hβ)]. Finally, we explore the variation in observed properties (UV attenuation, UV slope, and Balmer decrement) with viewing angle, finding average differences of ∼0.3 mag in the UV attenuation. [ABSTRACT FROM AUTHOR]
Published: 2024
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82. MINDS. The Detection of 13CO2 with JWST-MIRI Indicates Abundant CO2 in a Protoplanetary Disk

Author: Grant, Sierra L., primary, van Dishoeck, Ewine F., additional, Tabone, Benoît, additional, Gasman, Danny, additional, Henning, Thomas, additional, Kamp, Inga, additional, Güdel, Manuel, additional, Lagage, Pierre-Olivier, additional, Bettoni, Giulio, additional, Perotti, Giulia, additional, Christiaens, Valentin, additional, Samland, Matthias, additional, Arabhavi, Aditya M., additional, Argyriou, Ioannis, additional, Abergel, Alain, additional, Absil, Olivier, additional, Barrado, David, additional, Boccaletti, Anthony, additional, Bouwman, Jeroen, additional, o Garatti, Alessio Caratti, additional, Geers, Vincent, additional, Glauser, Adrian M., additional, Guadarrama, Rodrigo, additional, Jang, Hyerin, additional, Kanwar, Jayatee, additional, Lahuis, Fred, additional, Morales-Calderón, Maria, additional, Mueller, Michael, additional, Nehmé, Cyrine, additional, Olofsson, Göran, additional, Pantin, Eric, additional, Pawellek, Nicole, additional, Ray, Tom P., additional, Rodgers-Lee, Donna, additional, Scheithauer, Silvia, additional, Schreiber, Jürgen, additional, Schwarz, Kamber, additional, Temmink, Milou, additional, Vandenbussche, Bart, additional, Vlasblom, Marissa, additional, Waters, L. B. F. M., additional, Wright, Gillian, additional, Colina, Luis, additional, Greve, Thomas R., additional, Justannont, Kay, additional, and Östlin, Göran, additional
Published: 2023
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83. The Mid-infrared Instrument for JWST and Its In-flight Performance

Author: Wright, Gillian S., primary, Rieke, George H., additional, Glasse, Alistair, additional, Ressler, Michael, additional, García Marín, Macarena, additional, Aguilar, Jonathan, additional, Alberts, Stacey, additional, Álvarez-Márquez, Javier, additional, Argyriou, Ioannis, additional, Banks, Kimberly, additional, Baudoz, Pierre, additional, Boccaletti, Anthony, additional, Bouchet, Patrice, additional, Bouwman, Jeroen, additional, Brandl, Bernard R., additional, Breda, David, additional, Bright, Stacey, additional, Cale, Steven, additional, Colina, Luis, additional, Cossou, Christophe, additional, Coulais, Alain, additional, Cracraft, Misty, additional, De Meester, Wim, additional, Dicken, Daniel, additional, Engesser, Michael, additional, Etxaluze, Mireya, additional, Fox, Ori D., additional, Friedman, Scott, additional, Fu, Henry, additional, Gasman, Danny, additional, Gáspár, András, additional, Gastaud, René, additional, Geers, Vincent, additional, Glauser, Adrian Michael, additional, Gordon, Karl D., additional, Greene, Thomas, additional, Greve, Thomas R., additional, Grundy, Timothy, additional, Güdel, Manuel, additional, Guillard, Pierre, additional, Haderlein, Peter, additional, Hashimoto, Ryan, additional, Henning, Thomas, additional, Hines, Dean, additional, Holler, Bryan, additional, Detre, Örs Hunor, additional, Jahromi, Amir, additional, James, Bryan, additional, Jones, Olivia C., additional, Justtanont, Kay, additional, Kavanagh, Patrick, additional, Kendrew, Sarah, additional, Klaassen, Pamela, additional, Krause, Oliver, additional, Labiano, Alvaro, additional, Lagage, Pierre-Olivier, additional, Lambros, Scott, additional, Larson, Kirsten, additional, Law, David, additional, Lee, David, additional, Libralato, Mattia, additional, Alverez, Jose Lorenzo, additional, Meixner, Margaret, additional, Morrison, Jane, additional, Mueller, Migo, additional, Murray, Katherine, additional, Mycroft, Matthew, additional, Myers, Richard, additional, Nayak, Omnarayani, additional, Naylor, Bret, additional, Nickson, Bryony, additional, Noriega-Crespo, Alberto, additional, Östlin, Göran, additional, O’Sullivan, Brian, additional, Ottens, Richard, additional, Patapis, Polychronis, additional, Penanen, Konstantin, additional, Pietraszkiewicz, Martin, additional, Ray, Tom, additional, Regan, Michael, additional, Roteliuk, Anthony, additional, Royer, Pierre, additional, Samara-Ratna, Piyal, additional, Samuelson, Bridget, additional, Sargent, Beth A., additional, Scheithauer, Silvia, additional, Schneider, Analyn, additional, Schreiber, Jürgen, additional, Shaughnessy, Bryan, additional, Sheehan, Evan, additional, Shivaei, Irene, additional, Sloan, G. C., additional, Tamas, Laszlo, additional, Teague, Kelly, additional, Temim, Tea, additional, Tikkanen, Tuomo, additional, Tustain, Samuel, additional, van Dishoeck, Ewine F., additional, Vandenbussche, Bart, additional, Weilert, Mark, additional, Whitehouse, Paul, additional, and Wolff, Schuyler, additional
Published: 2023
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84. Massive galaxy formation caught in action at z ∼ 5 with JWST

Author: Jin, Shuowen, primary, Sillassen, Nikolaj B., additional, Magdis, Georgios E., additional, Vijayan, Aswin P., additional, Brammer, Gabriel B., additional, Kokorev, Vasily, additional, Weaver, John R., additional, Gobat, Raphael, additional, Giménez-Arteaga, Clara, additional, Valentino, Francesco, additional, Brinch, Malte, additional, Gómez-Guijarro, Carlos, additional, Shuntov, Marko, additional, Toft, Sune, additional, Greve, Thomas R., additional, and Blanquez Sese, David, additional
Published: 2023
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85. COSMOS2020: Identification of High-z Protocluster Candidates in COSMOS

Author: Brinch, Malte, primary, Greve, Thomas R., additional, Weaver, John R., additional, Brammer, Gabriel, additional, Ilbert, Olivier, additional, Shuntov, Marko, additional, Jin, Shuowen, additional, Liu, Daizhong, additional, Giménez-Arteaga, Clara, additional, Casey, Caitlin M., additional, Davidson, Iary, additional, Fujimoto, Seiji, additional, Koekemoer, Anton M., additional, Kokorev, Vasily, additional, Magdis, Georgios, additional, McCracken, H. J., additional, McPartland, Conor J. R., additional, Mobasher, Bahram, additional, Sanders, David B., additional, Toft, Sune, additional, Valentino, Francesco, additional, Zamorani, Giovanni, additional, and Zavala, Jorge, additional
Published: 2023
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86. MINDS. The Detection of (CO2)-C-13 with JWST-MIRI Indicates Abundant CO2 in a Protoplanetary Disk

Author: Grant, Sierra L, van Dishoeck, Ewine F, Tabone, Benoit, Gasman, Danny, Henning, Thomas, Kamp, Inga, Guedel, Manuel, Lagage, Pierre-Olivier, Bettoni, Giulio, Perotti, Giulia, Christiaens, Valentin, Samland, Matthias, Arabhavi, Aditya M, Argyriou, Ioannis, Abergel, Alain, Absil, Olivier, Barrado, David, Boccaletti, Anthony, Bouwman, Jeroen, Garatti, Alessio Caratti O, Geers, Vincent, Glauser, Adrian M, Guadarrama, Rodrigo, Jang, Hyerin, Kanwar, Jayatee, Lahuis, Fred, Morales-Calderon, Maria, Mueller, Michael, Nehme, Cyrine, Olofsson, Goeran, Pantin, Eric, Pawellek, Nicole, Ray, Tom P, Rodgers-Lee, Donna, Scheithauer, Silvia, Schreiber, Juergen, Schwarz, Kamber, Temmink, Milou, Vandenbussche, Bart, Vlasblom, Marissa, Waters, LBFM, Wright, Gillian, Colina, Luis, Greve, Thomas R, Justannont, Kay, and Ostlin, Goeran
Subjects: Science & Technology, SPECTROSCOPY, PLANET-FORMING REGIONS, SPITZER SURVEY, Physical Sciences, WEBB-SPACE-TELESCOPE, WATER, LINE, MIDINFRARED MOLECULAR-EMISSION, SUBSTRUCTURES, LOW-MASS STARS, Astronomy & Astrophysics, YOUNG STELLAR OBJECTS
Abstract: ispartof: ASTROPHYSICAL JOURNAL LETTERS vol:947 issue:1 status: published
Published: 2023

87. Investigating the [C II]-to-H I Conversion Factor and the H I Gas Budget of Galaxies at z approximate to 6 with Hydrodynamic Simulations

Author: Vizgan, David, Heintz, Kasper E., Greve, Thomas R., Narayanan, Desika, Dave, Romeel, Olsen, Karen P., Popping, Gergo, and Watson, Darach
Subjects: NEUTRAL ATOMIC PHASES, DWARF GALAXIES, INTERSTELLAR-MEDIUM, LINE SURVEY, PHOTODISSOCIATION REGIONS, HIGH-REDSHIFT, HYDROGEN, EMISSION, MOLECULAR GAS, STAR-FORMATION
Abstract: One of the most fundamental baryonic matter components of galaxies is the neutral atomic hydrogen (H I). At low redshifts, this component can be traced directly through the 21 cm transition, but to infer the H I gas content of the most distant galaxies, a viable tracer is needed. We here investigate the fidelity of the fine-structure transition of the (P-2(3/2) - P-2(1/3)) transition of singly ionized carbon C II at 158 mu m as a proxy for H I in a set simulated galaxies at z approximate to 6, following the work by Heintz et al. We select 11,125 star-forming galaxies from the SIMBA simulations, with far-infrared line emissions postprocessed and modeled within the SIGAME framework. We find a strong connection between C II and H I, with the relation between this C I relation (beta([C II])) being anticorrelated with the gas-phase metallicity of the simulated galaxies. We further use these simulations to make predictions for the total baryonic matter content of galaxies at z approximate to 6, and specifically the H I gas mass fraction. We find mean values of M-H I/M-* = 1.4 and M-H I/ M-bar,M-tot = 0.45. These results provide strong evidence for H I being the dominant baryonic matter component by mass in galaxies at z approximate to 6.
Published: 2022
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88. Revisiting the [C ii] 158 μm line-intensity mapping power spectrum from the EoR using non-uniform line-luminosity scatter

Author: Murmu, Chandra Shekhar, primary, Olsen, Karen P, additional, Greve, Thomas R, additional, Majumdar, Suman, additional, Datta, Kanan K, additional, Scott, Bryan R, additional, Leung, T K Daisy, additional, Davé, Romeel, additional, Popping, Gergö, additional, Ochoa, Raul Ortega, additional, Vizgan, David, additional, and Narayanan, Desika, additional
Published: 2022
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89. A galaxy group candidate at z approximate to 3.7 in the COSMOS field

Author: Sillassen, Nikolaj B., Jin, Shuowen, Magdis, Georgios E., Daddi, Emanuele, Weaver, John R., Gobat, Raphael, Kokorev, Vasily, Valentino, Francesco, Finoguenov, Alexis, Shuntov, Marko, Gomez-Guijarro, Carlos, Coogan, Rosemary, Greve, Thomas R., Toft, Sune, Sese, David Blanquez, and Department of Physics
Subjects: Galaxy: evolution, Submillimeter: galaxies, Galaxies: high-redshift, Galaxies: clusters: general, 115 Astronomy, Space science
Abstract: We report a galaxy group candidate HPC1001 at z approximate to 3.7 in the COSMOS field. This structure was selected as a high galaxy overdensity at z > 3 in the COSMOS2020 catalog. It contains ten candidate members, of which eight are assembled in a 10 '' x 10 '' area with the highest sky density among known protoclusters and groups at z > 3. Four out of ten sources were also detected at 1.2mm with Atacama Large Millimeter Array continuum observations. Photometric redshifts, measured by four independent methods, fall within a narrow range of 3.5 < z < 3.9 and with a weighted average of z = 3.65 +/- 0.07. The integrated far-IR-to-radio spectral energy distribution yields a total UV and IR star formation rate SFR approximate to 900 M-circle dot yr(-1). We also estimated a halo mass of similar to 10(13) M-circle dot for the structure, which at this redshift is consistent with potential cold gas inflow. Remarkably, the most massive member has a specific star formation rate and dust to stellar mass ratio of M-dust/M-* that are both significantly lower than that of star-forming galaxies at this redshift, suggesting that HPC1001 could be a z approximate to 3.7 galaxy group in maturing phase. If confirmed, this would be the earliest structure in maturing phase to date, and an ideal laboratory to study the formation of the earliest quiescent galaxies as well as cold gas accretion in dense environments. Non
Published: 2022

90. Investigating the [C ii]-to-H i Conversion Factor and the H i Gas Budget of Galaxies at z ≈ 6 with Hydrodynamic Simulations

Author: Vizgan, David, primary, Heintz, Kasper E., additional, Greve, Thomas R., additional, Narayanan, Desika, additional, Davé, Romeel, additional, Olsen, Karen P., additional, Popping, Gergö, additional, and Watson, Darach, additional
Published: 2022
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91. A galaxy group candidate at z ≈ 3.7 in the COSMOS field

Author: Sillassen, Nikolaj B., primary, Jin, Shuowen, additional, Magdis, Georgios E., additional, Daddi, Emanuele, additional, Weaver, John R., additional, Gobat, Raphael, additional, Kokorev, Vasily, additional, Valentino, Francesco, additional, Finoguenov, Alexis, additional, Shuntov, Marko, additional, Gómez-Guijarro, Carlos, additional, Coogan, Rosemary, additional, Greve, Thomas R., additional, Toft, Sune, additional, and Blanquez Sese, David, additional
Published: 2022
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92. Life beyond 30: Probing the −20 < M UV < −17 Luminosity Function at 8 < z < 13 with the NIRCam Parallel Field of the MIRI Deep Survey.

Author: Pérez-González, Pablo G., Costantin, Luca, Langeroodi, Danial, Rinaldi, Pierluigi, Annunziatella, Marianna, Ilbert, Olivier, Colina, Luis, Nørgaard-Nielsen, Hans Ulrik, Greve, Thomas R., Östlin, Göran, Wright, Gillian, Alonso-Herrero, Almudena, Álvarez-Márquez, Javier, Caputi, Karina I., Eckart, Andreas, Le Fèvre, Olivier, Labiano, Álvaro, García-Marín, Macarena, Hjorth, Jens, and Kendrew, Sarah
Published: 2023
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93. Rapid build-up of the stellar content in the protocluster core SPT2349−56 at z = 4.3

Author: Chapman, Ryley Hill Scott, Phadke, Kedar A., Aravena, Manuel, Archipley, Melanie, Ashby, Matthew L N, Béthermin, Matthieu, Canning, Rebecca E A, Gonzalez, Anthony, Greve, Thomas R, Gururajan, Gayathri, Hayward, Christopher C, Hezaveh, Yashar, Jarugula, Sreevani, MacIntyre, Duncan, Marrone, Daniel P, Miller, Tim, Reuter, Cassie, Rotermund, Kaja M, Scott, Douglas, Spilker, Justin, Vieira, Joaquin D, Wang, George, Weiß, Axel, Chapman, Ryley Hill Scott, Phadke, Kedar A., Aravena, Manuel, Archipley, Melanie, Ashby, Matthew L N, Béthermin, Matthieu, Canning, Rebecca E A, Gonzalez, Anthony, Greve, Thomas R, Gururajan, Gayathri, Hayward, Christopher C, Hezaveh, Yashar, Jarugula, Sreevani, MacIntyre, Duncan, Marrone, Daniel P, Miller, Tim, Reuter, Cassie, Rotermund, Kaja M, Scott, Douglas, Spilker, Justin, Vieira, Joaquin D, Wang, George, and Weiß, Axel
Abstract: The protocluster SPT2349−56 at z=4.3 contains one of the most actively star-forming cores known, yet constraints on the total stellar mass of this system are highly uncertain. We have therefore carried out deep optical and infrared observations of this system, probing rest-frame ultraviolet to infrared wavelengths. Using the positions of the spectroscopically confirmed protocluster members, we identify counterparts and perform detailed source deblending, allowing us to fit spectral energy distributions in order to estimate stellar masses. We show that the galaxies in SPT2349−56 have stellar masses proportional to their high star formation rates, consistent with other protocluster galaxies and field submillimetre galaxies (SMGs) around redshift 4. The galaxies in SPT2349−56 have on average lower molecular gas-to-stellar mass fractions and depletion time-scales than field SMGs, although with considerable scatter. We construct the stellar-mass function for SPT2349−56 and compare it to the stellar-mass function of z=1 galaxy clusters, finding consistent shapes between the two. We measure rest-frame galaxy ultraviolet half-light radii from our HST-F160W imaging, finding that on average the galaxies in our sample are similar in size to typical star-forming galaxies at these redshifts. However, the brightest HST-detected galaxy in our sample, found near the luminosity-weighted centre of the protocluster core, remains unresolved at this wavelength. Hydrodynamical simulations predict that the core galaxies will quickly merge into a brightest cluster galaxy, thus our observations provide a direct view of the early formation mechanisms of this class of object.
Published: 2022

94. Multiwavelength properties of 850-mu m selected sources from the North Ecliptic Pole SCUBA-2 survey

Author: Shim, Hyunjin, Lee, Dongseob, Kim, Yeonsik, Scott, Douglas, Serjeant, Stephen, Ao, Yiping, Barrufet, Laia, Chapman, Scott C., Clements, David L., Conselice, Christopher J., Goto, Tomotsugu, Greve, Thomas R., Hwang, Ho Seong, Im, Myungshin, Jeong, Woong-Seob, Kim, Helen K., Kim, Minjin, Kim, Seong Jin, Kong, Albert K. H., Koprowski, Maciej P., Malkan, Matthew A., Michalowski, Michal J., Pearson, Chris, Seo, Hyunjong, Takagi, Toshinobu, Toba, Yoshiki, White, Glenn J., Woo, Jong-Hak, Shim, Hyunjin, Lee, Dongseob, Kim, Yeonsik, Scott, Douglas, Serjeant, Stephen, Ao, Yiping, Barrufet, Laia, Chapman, Scott C., Clements, David L., Conselice, Christopher J., Goto, Tomotsugu, Greve, Thomas R., Hwang, Ho Seong, Im, Myungshin, Jeong, Woong-Seob, Kim, Helen K., Kim, Minjin, Kim, Seong Jin, Kong, Albert K. H., Koprowski, Maciej P., Malkan, Matthew A., Michalowski, Michal J., Pearson, Chris, Seo, Hyunjong, Takagi, Toshinobu, Toba, Yoshiki, White, Glenn J., and Woo, Jong-Hak
Abstract: We present the multiwavelength counterparts of 850-mu m selected submillimetre sources over a 2-deg(2) field centred on the North Ecliptic Pole. In order to overcome the large beam size (15 arcsec) of the 850-mu m images, deep optical to near-infrared (NIR) photometric data and arcsecond-resolution 20-cm images are used to identify counterparts of submillimetre sources. Among 647 sources, we identify 514 reliable counterparts for 449 sources (69 per cent in number), based either on probabilities of chance associations calculated from positional offsets or offsets combined with the optical-to-NIR colours. In the radio imaging, the fraction of 850-mu m sources having multiple counterparts is 7 percent. The photometric redshift, infrared luminosity, stellar mass, star formation rate (SFR), and the active galactic nucleus (AGN) contribution to the total infrared luminosity of the identified counterparts are investigated through spectral energy distribution fitting. The SMGs are infrared-luminous galaxies at an average < z > = 2.5 with log(10)(L-IR/L-circle dot) = 11.5-13.5, with a mean stellar mass of log(10)(M-star/M-circle dot) = 10.90 and SFR of log(10)(SFR/M-circle dot yr(-1)) = 2.34. The submillimetre galaxies (SMGs) show twice as large SFR as galaxies on the star-forming main sequence, and about 40 per cent of the SMGs are classified as objects with bursty star formation. At z >= 4, the contribution of AGN luminosity to total luminosity for most SMGs is larger than 30 per cent. The FIR-to-radio correlation coefficient of SMGs is consistent with that of main-sequence galaxies at z similar or equal to 2.
Published: 2022

95. Multiwavelength properties of 850-μm selected sources from the North Ecliptic Pole SCUBA-2 survey

Author: Shim, Hyunjin, primary, Lee, Dongseob, additional, Kim, Yeonsik, additional, Scott, Douglas, additional, Serjeant, Stephen, additional, Ao, Yiping, additional, Barrufet, Laia, additional, Chapman, Scott C, additional, Clements, David L, additional, Conselice, Christopher J, additional, Goto, Tomotsugu, additional, Greve, Thomas R, additional, Hwang, Ho Seong, additional, Im, Myungshin, additional, Jeong, Woong-Seob, additional, Kim, Helen K, additional, Kim, Minjin, additional, Kim, Seong Jin, additional, Kong, Albert K H, additional, Koprowski, Maciej P, additional, Malkan, Matthew A, additional, Michałowski, Michał J, additional, Pearson, Chris, additional, Seo, Hyunjong, additional, Takagi, Toshinobu, additional, Toba, Yoshiki, additional, White, Glenn J, additional, and Woo, Jong-Hak, additional
Published: 2022
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96. Chaotic and Clumpy Galaxy Formation in an Extremely Massive Reionization-era Halo

Author: Spilker, Justin S., primary, Hayward, Christopher C., additional, Marrone, Daniel P., additional, Aravena, Manuel, additional, Béthermin, Matthieu, additional, Burgoyne, James, additional, Chapman, Scott C., additional, Greve, Thomas R., additional, Gururajan, Gayathri, additional, Hezaveh, Yashar D., additional, Hill, Ryley, additional, Litke, Katrina C., additional, Lovell, Christopher C., additional, Malkan, Matthew A., additional, Murphy, Eric J., additional, Narayanan, Desika, additional, Phadke, Kedar A., additional, Reuter, Cassie, additional, Stark, Antony A., additional, Sulzenauer, Nikolaus, additional, Vieira, Joaquin D., additional, Vizgan, David, additional, and Weiß, Axel, additional
Published: 2022
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97. A census of the stellar content in the protocluster core SPT2349$-$56 at $z\,{=}\,4.3$

Author: Hill, Ryley, Chapman, Scott, Phadke, Kedar A., Aravena, Manuel, Archipley, Melanie, Bethermin, Matthieu, Canning, Rebecca E.A., Gonzalez, Anthony, Greve, Thomas R., Gururajan, Gayathri, Hayward, Christopher C., Hezaveh, Yashar, Jarugula, Sreevani, Marrone, Daniel P., Miller, Tim, Reuter, Cassie, Rotermund, Kaja, Scott, Douglas, Spilker, Justin, Vieira, Joaquin D., Wang, George, Weiss, Axel, Laboratoire d'Astrophysique de Marseille (LAM), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract: The protocluster core SPT2349$-$56 at $z\,{=}\,4.3$ is one of the most actively star-forming regions known, yet constraints on the total stellar mass of this system are highly uncertain. We have therefore carried out deep optical and infrared observations of this system, probing rest-frame ultraviolet to infrared wavelengths. Using the positions of the spectroscopically-confirmed protocluster members, we identify counterparts and perform detailed source deblending, allowing us to fit spectral energy distributions in order to estimate stellar masses. We show that the galaxies in SPT2349$-$56 have stellar masses proportional to their high star-formation rates, consistent with other protocluster galaxies and field submillimetre galaxies (SMGs) around redshift 4. The galaxies in SPT2349$-$56 have on average lower molecular gas-to-stellar mass fractions and depletion timescales than field SMGs, although with considerable scatter. We construct the stellar-mass function for SPT2349$-$56 and compare it to the stellar-mass function of $z\,{=}\,1$ galaxy clusters, finding both to be best described by a Schechter function. We measure rest-frame ultraviolet half-light radii from our {\it HST\/}-F160W imaging, finding that on average the galaxies in our sample are similar in size to typical star-forming galaxies around the same redshift. However, the brightest {\it HST\/}-detected galaxy in our sample, found near the luminosity-weighted centre of the protocluster core, remains unresolved at this wavelength. Hydrodynamical simulations predict that the core galaxies will quickly merge into a brightest cluster galaxy, thus our observations provide a direct view of the early formation mechanisms of this class of object.
Published: 2021

98. Rapid build-up of the stellar content in the protocluster core SPT2349−56 at z = 4.3

Author: Hill, Ryley, primary, Chapman, Scott, additional, Phadke, Kedar A, additional, Aravena, Manuel, additional, Archipley, Melanie, additional, Ashby, Matthew L N, additional, Béthermin, Matthieu, additional, Canning, Rebecca E A, additional, Gonzalez, Anthony, additional, Greve, Thomas R, additional, Gururajan, Gayathri, additional, Hayward, Christopher C, additional, Hezaveh, Yashar, additional, Jarugula, Sreevani, additional, MacIntyre, Duncan, additional, Marrone, Daniel P, additional, Miller, Tim, additional, Rennehan, Douglas, additional, Reuter, Cassie, additional, Rotermund, Kaja M, additional, Scott, Douglas, additional, Spilker, Justin, additional, Vieira, Joaquin D, additional, Wang, George, additional, and Weiß, Axel, additional
Published: 2021
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99. sígame v3: Gas Fragmentation in Postprocessing of Cosmological Simulations for More Accurate Infrared Line Emission Modeling

Author: Olsen, Karen Pardos, primary, Burkhart, Blakesley, additional, Mac Low, Mordecai-Mark, additional, Treß, Robin G., additional, Greve, Thomas R., additional, Vizgan, David, additional, Motka, Jay, additional, Borrow, Josh, additional, Popping, Gergö, additional, Davé, Romeel, additional, Smith, Rowan J., additional, and Narayanan, Desika, additional
Published: 2021
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100. Molecular Line Observations in Two Dusty Star-forming Galaxies at z = 6.9

Author: Jarugula, Sreevani, primary, Vieira, Joaquin D., additional, Weiss, Axel, additional, Spilker, Justin S., additional, Aravena, Manuel, additional, Archipley, Melanie, additional, Béthermin, Matthieu, additional, C. Chapman, Scott, additional, Dong, Chenxing, additional, Greve, Thomas R., additional, Harrington, Kevin, additional, Hayward, Christopher C., additional, Hezaveh, Yashar, additional, Hill, Ryley, additional, Litke, Katrina C., additional, Malkan, Matthew A., additional, Marrone, Daniel P., additional, Narayanan, Desika, additional, Phadke, Kedar A., additional, Reuter, Cassie, additional, and Rotermund, Kaja M., additional
Published: 2021
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