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  • 1
    Online Resource
    Online Resource
    Accurate dust temperature determination in a z = 7.13 galaxy
    Oxford University Press (OUP) ; 2021
    In:  Monthly Notices of the Royal Astronomical Society: Letters Vol. 508, No. 1 ( 2021-09-22), p. L58-L63
    Details
    In: Monthly Notices of the Royal Astronomical Society: Letters, Oxford University Press (OUP), Vol. 508, No. 1 ( 2021-09-22), p. L58-L63
    Abstract: We report ALMA Band 9 continuum observations of the normal, dusty star-forming galaxy A1689-zD1 at z = 7.13, resulting in a ∼4.6 σ detection at 702 GHz. For the first time, these observations probe the far-infrared spectrum shortward of the emission peak of a galaxy in the Epoch of Reionization (EoR). Together with ancillary data from earlier works, we derive the dust temperature, Td, and mass, Md, of A1689-zD1 using both traditional modified blackbody spectral energy density fitting, and a new method that relies only on the [C ii] 158 μm line and underlying continuum data. The two methods give $T_{\rm d} = (42^{+13}_{-7}, 40^{+13}_{-7}$) K, and $M_{\rm d} = (1.7^{+1.3}_{-0.7}, 2.0^{+1.8}_{-1.0})\, \times {}\, 10^{7} \, \mathrm{ M}_{\odot }$. Band 9 observations improve the accuracy of the dust temperature (mass) estimate by ∼50 per cent (6 times). The derived temperatures confirm the reported increasing Td-redshift trend between z = 0 and 8; the dust mass is consistent with a supernova origin. Although A1689-zD1 is a normal UV-selected galaxy, our results, implying that ∼85 per cent of its star-formation rate is obscured, underline the non-negligible effects of dust in EoR galaxies.
    Type of Medium: Online Resource
    ISSN: 1745-3925 , 1745-3933
    URL: Article
    DOI: 10.1093/mnrasl/slab104
    Language: English
    Publisher: Oxford University Press (OUP)
    Publication Date: 2021
    detail.hit.zdb_id: 2190759-6
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  • 2
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    Quenching and the UVJ Diagram in the SIMBA Cosmological Simulation
    American Astronomical Society ; 2022
    In:  The Astrophysical Journal Vol. 929, No. 1 ( 2022-04-01), p. 94-
    Details
    In: The Astrophysical Journal, American Astronomical Society, Vol. 929, No. 1 ( 2022-04-01), p. 94-
    Abstract: Over the past decade, rest-frame color–color diagrams have become popular tools for selecting quiescent galaxies at high redshift, breaking the color degeneracy between quiescent and dust-reddened star-forming galaxies. In this work, we study one such color–color selection tool—the rest-frame U − V versus V − J diagram—by employing mock observations of cosmological galaxy formation simulations. In particular, we conduct numerical experiments assessing both trends in galaxy properties in UVJ space and the color–color evolution of massive galaxies as they quench at redshifts z ∼ 1–2. We find that our models broadly reproduce the observed UVJ diagram at z = 1–2, including (for the first time in a cosmological simulation) reproducing the population of extremely dust-reddened galaxies in the top right of the UVJ diagram. However, our models primarily populate this region with low-mass galaxies and do not produce as clear a bimodality between star-forming and quiescent galaxies as is seen in observations. The former issue is due to an excess of dust in low-mass galaxies and relatively gray attenuation curves in high-mass galaxies, while the latter is due to the overpopulation of the green valley in simba . When investigating the time evolution of galaxies on the UVJ diagram, we find that the quenching pathway on the UVJ diagram is independent of the quenching timescale, and instead dependent primarily on the average specific star formation rate in the 1 Gyr prior to the onset of quenching. Our results support the interpretation of different quenching pathways as corresponding to the divergent evolution of post-starburst and green valley galaxies.
    Type of Medium: Online Resource
    ISSN: 0004-637X , 1538-4357
    URL: Article
    DOI: 10.3847/1538-4357/ac5d3a
    RVK:
    UA 1000
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2022
    detail.hit.zdb_id: 2207648-7
    detail.hit.zdb_id: 1473835-1
    SSG: 16,12
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  • 3
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    Online Resource
    Foliar fungicide application effects on whole plant BMR and floury corn varieties, and whole plant corn silage composition
    Elsevier BV ; 2019
    In:  Animal Feed Science and Technology Vol. 257 ( 2019-11), p. 114264-
    Details
    In: Animal Feed Science and Technology, Elsevier BV, Vol. 257 ( 2019-11), p. 114264-
    Type of Medium: Online Resource
    ISSN: 0377-8401
    URL: Article
    DOI: 10.1016/j.anifeedsci.2019.114264
    Language: English
    Publisher: Elsevier BV
    Publication Date: 2019
    detail.hit.zdb_id: 1495847-8
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  • 4
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    Broad Emission Lines in Optical Spectra of Hot, Dust-obscured Galaxies Can Contribute Significantly to JWST/NIRCam Photometry
    American Astronomical Society ; 2023
    In:  The Astrophysical Journal Letters Vol. 946, No. 2 ( 2023-04-01), p. L39-
    Details
    In: The Astrophysical Journal Letters, American Astronomical Society, Vol. 946, No. 2 ( 2023-04-01), p. L39-
    Abstract: Selecting the first galaxies at z 〉 7 − 10 from JWST surveys is complicated by z 〈 6 contaminants with degenerate photometry. For example, strong optical nebular emission lines at z 〈 6 may mimic JWST/NIRCam photometry of z 〉 7–10 Lyman-break galaxies (LBGs). Dust-obscured 3 〈 z 〈 6 galaxies in particular are potentially important contaminants, and their faint rest-optical spectra have been historically difficult to observe. A lack of optical emission line and continuum measures for 3 〈 z 〈 6 dusty galaxies now makes it difficult to test their expected JWST/NIRCam photometry for degenerate solutions with NIRCam dropouts. Toward this end, we quantify the contribution by strong emission lines to NIRCam photometry in a physically motivated manner by stacking 21 Keck II/NIRES spectra of hot, dust-obscured, massive ( log M * / M ⊙ ≳ 10 – 11 ) and infrared (IR) luminous galaxies at z ∼ 1–4. We derive an average spectrum and measure strong narrow (broad) [O iii ] 5007 and H α features with equivalent widths of 130 ± 20 Å (150 ± 50 Å) and 220 ± 30 Å (540 ± 80 Å), respectively. These features can increase broadband NIRCam fluxes by factors of 1.2 − 1.7 (0.2–0.6 mag). Due to significant dust attenuation ( A V ∼ 6), we find H α +[N ii ] to be significantly brighter than [O iii ]+H β and therefore find that emission-line dominated contaminants of high − z galaxy searches can only reproduce moderately blue perceived UV continua of S λ ∝ λ β with β 〉 − 1.5 and z 〉 4. While there are some redshifts ( z ∼ 3.75) where our stack is more degenerate with the photometry of z 〉 10 LBGs at λ rest ∼ 0.3–0.8 μ m , redder filter coverage beyond λ obs 〉 3.5 μ m and far-IR/submillimeter follow-up may be useful for breaking the degeneracy and making a crucial separation between two fairly unconstrained populations, dust-obscured galaxies at z ∼ 3–6 and LBGs at z 〉 10.
    Type of Medium: Online Resource
    ISSN: 2041-8205 , 2041-8213
    URL: Article
    DOI: 10.3847/2041-8213/acc322
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2023
    detail.hit.zdb_id: 2207648-7
    detail.hit.zdb_id: 2006858-X
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  • 5
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    Two Massive, Compact, and Dust-obscured Candidate z ≃ 8 Galaxies Discovered by JWST
    American Astronomical Society ; 2023
    In:  The Astrophysical Journal Vol. 956, No. 1 ( 2023-10-01), p. 61-
    Details
    In: The Astrophysical Journal, American Astronomical Society, Vol. 956, No. 1 ( 2023-10-01), p. 61-
    Abstract: We present a search for extremely red, dust-obscured, z 〉 7 galaxies with JWST/NIRCam+MIRI imaging over the first 20 arcmin 2 of publicly available Cycle 1 data from the COSMOS-Web, CEERS, and PRIMER surveys. Based on their red color in F277W−F444W (∼2.5 mag) and detection in MIRI/F770W (∼25 mag), we identify two galaxies, COS-z8M1 and CEERS-z7M1, that have best-fit photometric redshifts of z = 8.4 − 0.4 + 0.3 and 7.6 − 0.1 + 0.1 , respectively. We perform spectral energy distribution fitting with a variety of codes (including bagpipes , prospector , beagle , and cigale ) and find a 〉 95% probability that these indeed lie at z 〉 7. Both sources are compact ( R eff ≲ 200 pc) and highly obscured ( A V ∼ 1.5–2.5) and, at our best-fit redshift estimates, likely have strong [O iii ]+H β emission contributing to their 4.4 μ m photometry. We estimate stellar masses of ∼10 10 M ⊙ for both sources; by virtue of detection in MIRI at 7.7 μ m, these measurements are robust to the inclusion of bright emission lines, for example, from an active galactic nucleus. We identify a marginal (2.9 σ ) Atacama Large Millimeter/submillimeter Array detection at 2 mm within 0.″5 of COS-z8M1, which, if real, would suggest a remarkably high IR luminosity of ∼10 12 L ⊙ . These two galaxies, if confirmed at z ∼ 8, would be extreme in their stellar and dust masses and may be representative of a substantial population of highly dust-obscured galaxies at cosmic dawn.
    Type of Medium: Online Resource
    ISSN: 0004-637X , 1538-4357
    URL: Article
    DOI: 10.3847/1538-4357/acef21
    RVK:
    UA 1000
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2023
    detail.hit.zdb_id: 2207648-7
    detail.hit.zdb_id: 1473835-1
    SSG: 16,12
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  • 6
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    Quenching Timescales of Dwarf Satellites around Milky Way–mass Hosts
    American Astronomical Society ; 2021
    In:  The Astrophysical Journal Vol. 909, No. 2 ( 2021-03-01), p. 139-
    Details
    In: The Astrophysical Journal, American Astronomical Society, Vol. 909, No. 2 ( 2021-03-01), p. 139-
    Abstract: Observations of the low-mass satellites in the Local Group have shown high fractions of gas-poor, quiescent galaxies relative to isolated dwarfs, implying that the host halo environment plays an important role in the quenching of dwarf galaxies. In this work, we present measurements of the quenched fractions and quenching timescales of dwarf satellite galaxies in the DC Justice League suite of four high-resolution cosmological zoom-in simulations of Milky Way–mass halos. We show that these simulations accurately reproduce the satellite luminosity functions of observed nearby galaxies, as well as the variation in satellite quenched fractions from M * ∼ 10 5 M ⊙ to 10 10 M ⊙ . We then trace the histories of satellite galaxies back to z ∼ 15 and find that many satellites with M * ∼ 10 6 −10 8 M ⊙ quench within ∼2 Gyr of infall into the host halo, while others in the same mass range remain star-forming for as long as 5 Gyr. We show that this scatter can be explained by the satellite’s gas mass and the ram pressure it feels at infall. Finally, we identify a characteristic stellar mass scale of 10 8 M ⊙ above which infalling satellites are largely resistant to rapid environmental quenching.
    Type of Medium: Online Resource
    ISSN: 0004-637X , 1538-4357
    URL: Article
    DOI: 10.3847/1538-4357/abe2ab
    RVK:
    UA 1000
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2021
    detail.hit.zdb_id: 2207648-7
    detail.hit.zdb_id: 1473835-1
    SSG: 16,12
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  • 7
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    ALMA Reveals Extended Cool Gas and Hot Ionized Outflows in a Typical Star-forming Galaxy at Z = 7.13
    American Astronomical Society ; 2022
    In:  The Astrophysical Journal Vol. 934, No. 1 ( 2022-07-01), p. 64-
    Details
    In: The Astrophysical Journal, American Astronomical Society, Vol. 934, No. 1 ( 2022-07-01), p. 64-
    Abstract: We present spatially resolved morphological properties of [C II ] 158 μ m, [O III ] 88 μ m, dust, and rest-frame ultraviolet (UV) continuum emission for A1689-zD1, a strongly lensed, sub-L* galaxy at z = 7.13, by utilizing deep Atacama Large Millimeter/submillimeter Array (ALMA) and Hubble Space Telescope (HST) observations. While the [O III ] line and UV continuum are compact, the [C II ] line is extended up to a radius of r ∼ 12 kpc. Using multi-band rest-frame far-infrared continuum data ranging from 52 to 400 μ m, we find an average dust temperature and emissivity index of T dust = 41 − 14 + 17 K and β = 1.7 − 0.7 + 1.1 , respectively, across the galaxy. We find slight differences in the dust continuum profiles at different wavelengths, which may indicate that the dust temperature decreases with distance. We map the star formation rate (SFR) via IR and UV luminosities and determine a total SFR of 37 ± 1 M ⊙ yr −1 with an obscured fraction of 87%. While the [O III ] line is a good tracer of the SFR, the [C II ] line shows deviation from the local L [C II ] -SFR relations in the outskirts of the galaxy. Finally, we observe a clear difference in the line profile between [C II ] and [O III ], with significant residuals (∼5 σ ) in the [O III ] line spectrum after subtracting a single Gaussian model. This suggests a possible origin of the extended [C II ] structure from the cooling of hot ionized outflows. The extended [C II ] and high-velocity [O III ] emission may both contribute in part to the high L [O III ] / L [C II ] ratios recently reported in z 〉 6 galaxies.
    Type of Medium: Online Resource
    ISSN: 0004-637X , 1538-4357
    URL: Article
    DOI: 10.3847/1538-4357/ac795b
    RVK:
    UA 1000
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2022
    detail.hit.zdb_id: 2207648-7
    detail.hit.zdb_id: 1473835-1
    SSG: 16,12
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  • 8
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    COSMOS-Web: An Overview of the JWST Cosmic Origins Survey
    American Astronomical Society ; 2023
    In:  The Astrophysical Journal Vol. 954, No. 1 ( 2023-09-01), p. 31-
    Details
    In: The Astrophysical Journal, American Astronomical Society, Vol. 954, No. 1 ( 2023-09-01), p. 31-
    Abstract: We present the survey design, implementation, and outlook for COSMOS-Web, a 255 hr treasury program conducted by the James Webb Space Telescope in its first cycle of observations. COSMOS-Web is a contiguous 0.54 deg 2 NIRCam imaging survey in four filters (F115W, F150W, F277W, and F444W) that will reach 5 σ point-source depths ranging ∼27.5–28.2 mag. In parallel, we will obtain 0.19 deg 2 of MIRI imaging in one filter (F770W) reaching 5 σ point-source depths of ∼25.3–26.0 mag. COSMOS-Web will build on the rich heritage of multiwavelength observations and data products available in the COSMOS field. The design of COSMOS-Web is motivated by three primary science goals: (1) to discover thousands of galaxies in the Epoch of Reionization (6 ≲ z ≲ 11) and map reionization’s spatial distribution, environments, and drivers on scales sufficiently large to mitigate cosmic variance, (2) to identify hundreds of rare quiescent galaxies at z 〉 4 and place constraints on the formation of the universe’s most-massive galaxies ( M ⋆ 〉 10 10 M ⊙ ), and (3) directly measure the evolution of the stellar-mass-to-halo-mass relation using weak gravitational lensing out to z ∼ 2.5 and measure its variance with galaxies’ star formation histories and morphologies. In addition, we anticipate COSMOS-Web’s legacy value to reach far beyond these scientific goals, touching many other areas of astrophysics, such as the identification of the first direct collapse black hole candidates, ultracool subdwarf stars in the Galactic halo, and possibly the identification of z 〉 10 pair-instability supernovae. In this paper we provide an overview of the survey’s key measurements, specifications, goals, and prospects for new discovery.
    Type of Medium: Online Resource
    ISSN: 0004-637X , 1538-4357
    URL: Article
    DOI: 10.3847/1538-4357/acc2bc
    RVK:
    UA 1000
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2023
    detail.hit.zdb_id: 2207648-7
    detail.hit.zdb_id: 1473835-1
    SSG: 16,12
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  • 9
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    ALMA FIR View of Ultra-high-redshift Galaxy Candidates at z ∼ 11–17: Blue Monsters or Low-z Red Interlopers?
    American Astronomical Society ; 2023
    In:  The Astrophysical Journal Vol. 955, No. 2 ( 2023-10-01), p. 130-
    Details
    In: The Astrophysical Journal, American Astronomical Society, Vol. 955, No. 2 ( 2023-10-01), p. 130-
    Abstract: We present Atacama Large Millimeter/submillimeter Array (ALMA) Band 7 observations of a remarkably bright galaxy candidate at z phot = 16.7 − 0.3 + 1.9 ( M UV = −21.6), S5-z17-1, identified in James Webb Space Telescope (JWST) Early Release Observation data of Stephen’s Quintet. We do not detect the dust continuum at 866 μ m, ruling out the possibility that S5-z17-1 is a low- z dusty starburst with a star formation rate of ≳30 M ⊙ yr −1 . We detect a 5.1 σ line feature at 338.726 ± 0.007 GHz exactly coinciding with the JWST source position, with a 2% likelihood of the signal being spurious. The most likely line identification would be [O iii ]52 μ m at z = 16.01 or [C ii ]158 μ m at z = 4.61, whose line luminosities do not violate the nondetection of the dust continuum in both cases. Together with three other z ≳ 11–13 candidate galaxies recently observed with ALMA, we conduct a joint ALMA and JWST spectral energy distribution (SED) analysis and find that the high- z solution at z ∼ 11–17 is favored in every candidate as a very blue (UV continuum slope of ≃−2.3) and luminous ( M UV ≃ [ − 24:−21]) system. Still, we find in several candidates that reasonable SED fits (Δ χ 2 ≲ 4) are reproduced by type II quasar and/or quiescent galaxy templates with strong emission lines at z ∼ 3–5, where such populations predicted from their luminosity functions and EW([O iii ]+H β ) distributions are abundant in survey volumes used for the identification of the z ∼ 11–17 candidates. While these recent ALMA observation results have strengthened the likelihood of the high- z solutions, lower- z possibilities are not completely ruled out in several of the z ∼ 11–17 candidates, indicating the need to consider the relative surface densities of the lower- z contaminants in the ultra-high- z galaxy search.
    Type of Medium: Online Resource
    ISSN: 0004-637X , 1538-4357
    URL: Article
    DOI: 10.3847/1538-4357/aceb67
    RVK:
    UA 1000
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2023
    detail.hit.zdb_id: 2207648-7
    detail.hit.zdb_id: 1473835-1
    SSG: 16,12
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  • 10
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    A solar metallicity galaxy at z 〉 7? Possible detection of the [N  ii ] 122 μm and [O  iii ] 52 μm lines
    Oxford University Press (OUP) ; 2023
    In:  Monthly Notices of the Royal Astronomical Society Vol. 521, No. 2 ( 2023-03-14), p. 2526-2534
    Details
    In: Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP), Vol. 521, No. 2 ( 2023-03-14), p. 2526-2534
    Abstract: We present the first detection of the [N ii] 122 $\mu$m and [O iii] 52 $\mu$m lines for a reionization-epoch galaxy. Based on these lines and previous [C ii] 158 $\mu$m and [O iii] 88 $\mu$m measurements, using two different radiative transfer models of the interstellar medium, we estimate an upper limit on electron density of ≲500 cm−3 and an approximate gas-phase metallicity of Z/Z⊙ ∼ 1.1 ± 0.2 for A1689-zD1, a gravitationally lensed dusty galaxy at z = 7.133. Other measurements or indicators of metallicity so far in galaxy interstellar media at z ≳ 6 are typically an order of magnitude lower than this. The unusually high metallicity makes A1689-zD1 inconsistent with the fundamental metallicity relation, although there is likely significant dust obscuration of the stellar mass, which may partly resolve the inconsistency. Given a solar metallicity, the dust-to-metals ratio is a factor of several lower than expected, hinting that galaxies beyond z ∼ 7 may have lower dust formation efficiency. Finally, the inferred nitrogen enrichment compared to oxygen, on which the metallicity measurement depends, indicates that star formation in the system is older than about 250 Myr, pushing the beginnings of this galaxy to z & gt; 10.
    Type of Medium: Online Resource
    ISSN: 0035-8711 , 1365-2966
    URL: Article
    DOI: 10.1093/mnras/stad687
    Language: English
    Publisher: Oxford University Press (OUP)
    Publication Date: 2023
    detail.hit.zdb_id: 2016084-7
    SSG: 16,12
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