A Comparison of the Stellar, CO, and Dust-continuum Emission from Three Star-forming HUDF Galaxies at z ∼ 2

Kaasinen, Melanie; Walter, Fabian; Novak, Mladen; Neeleman, Marcel; Smail, Ian; Boogaard, Leindert; Cunha, Elisabete da; Weiß, A.; Liu, Daizhong; Decarli, Roberto; Popping, Gergö; Díaz-Santos, T.; Cortés, Paulo C.; Aravena, M.; Werf, P. van der; Riechers, Dominik A.; Inami, Hanae; Hodge, J. A.; Rix, H. W.; Cox, P.

doi:10.3847/1538-4357/aba438

Cited by 47 publications

(61 citation statements)

References 128 publications

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“…The trend in Figure 13 can also be understood more fundamentally as a trend with molecular gas surface density, as a high surface density of gas would also drive the CO excitation upwards. 28 In that context, it is interesting to note that several of the galaxies at z≈2.5 are found to have a more compact dust distribution, compared to some of the sources at z≈1.5 (Rujopakarn et al 2019;Kaasinen et al 2020).…”

Section: Increasing Excitation With Redshiftmentioning

confidence: 99%

The ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: CO Excitation and Atomic Carbon in Star-forming Galaxies at z = 1–3

Boogaard

Werf

Weiß

et al. 2020

ApJ

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114

153

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We investigate the CO excitation and interstellar medium (ISM) conditions in a cold gas mass-selected sample of 22 star-forming galaxies at z=0.46-3.60, observed as part of the ALMA Spectroscopic Survey in the Hubble Ultra Deep Field (ASPECS). Combined with Very Large Array follow-up observations, we detect a total of 34 CO -J J 1 transitions with J=1 up to 8 (and an additional 21 upper limits, up to J=10) and 6 [ ] C I  P P 10 5 , comparable to the Milky Way and main-sequence galaxies at similar redshifts, and fairly high densities (10 4 cm −3), consistent with the low-J CO excitation. Our results imply a decrease in the cosmic molecular gas mass density at z2 compared to previous ASPECS measurements.

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Section: Increasing Excitation With Redshiftmentioning

confidence: 99%

The ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: CO Excitation and Atomic Carbon in Star-forming Galaxies at z = 1–3

Boogaard

Werf

Weiß

et al. 2020

ApJ

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114

153

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“…However, the resolved Schmidt-Kennicutt relation has not been tested for main-sequence galaxies at higher redshifts. There are resolved CO and dust observations of z ∼ 1 − 3 galaxies that indicate a different spatial distribution of molecular gas and dust compared to the stellar emission (e.g., Calistro Rivera et al 2018;Kaasinen et al 2020). These observations are typically limited to more massive and/or more actively star-forming galaxies than those in this work.…”

Section: Gas Mass Estimatesmentioning

confidence: 99%

IR SED and Dust Masses of Sub-solar Metallicity Galaxies at z~2.3

Shivaei,

Popping,

Rieke

et al. 2022

Preprint

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We present results from ALMA 1.2 mm continuum observations of a sample of 27 star-forming galaxies at z = 2.1 − 2.5 from the MOSFIRE Deep Evolution Field (MOSDEF) survey. These galaxies have gas-phase metallicity and star-formation rate measurements from Hβ, [Oiii], Hα, and [Nii]. Using stacks of Spitzer, Herschel, and ALMA photometry (rest-frame ∼ 8 − 400 µm), we examine the IR SED of high-redshift subsolar metallicity (∼ 0.5 Z ) LIRGs. We find that the data agree well with an average SED template of higher luminosity local low-metallicity dwarf galaxies (reduced χ 2 of 1.8). When compared with the commonly used templates for solar-metallicity local galaxies or highredshift LIRGs and ULIRGs, even in the most favorable case (with reduced χ 2 of 2.8), the templates are rejected at > 98% confidence level. The broader and hotter IR SED of both the local dwarfs and high-redshift subsolar metallicity galaxies may result from different grain properties, a clumpy dust geometry, or a harder/more intense ionizing radiation field that heats the dust to higher temperatures. The obscured SFR indicated by the FIR emission of the subsolar metallicity galaxies is only ∼ 60% of the total SFR, which is considerably lower than that of the local LIRGs with ∼ 96 − 97% obscured fractions. Due to the evolving IR SED shape, the local LIRG templates fit to mid-IR data can overestimate the Rayleigh-Jeans tail measurements at z ∼ 2 by a factor of 2 − 20, and these templates underestimate IR luminosities if fit to the observed ALMA fluxes by > 0.4 dex. At a given stellar mass or metallicity, dust masses at z ∼ 2.3 are an order of magnitude higher than those at z ∼ 0. Given the predicted molecular gas mass fractions, the observed z ∼ 2.3 dust-to-stellar mass ratios suggest lower dust-to-molecular gas masses than in local galaxies at the same metallicity. CO observations are necessary to better constrain the molecular gas content of sub-solar metallicity galaxies at z > 1.

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“…Regarding the sizes of each component, observational evidence suggest that the background population will have a more compact dust component than the stellar component. This is true for both massive galaxies and intermediate mass galaxies (e.g., Fujimoto et al 2017;Kaasinen et al 2020). So if this was the case for the galaxies in our sample, it will drive larger magnifications for the gas component pushing the gas fraction to higher values, not lower.…”

Section: Lensed Galaxies In Contextmentioning

confidence: 76%

Molecular gas budget and characterization of intermediate-mass star-forming galaxies at z ≈ 2–3

Solimano

González-López²,

Barrientos³

et al. 2021

A&A

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Star-forming galaxies (SFGs) with stellar masses below 1010 M⊙ make up the bulk of the galaxy population at z > 2. The properties of the cold gas in these galaxies can only be probed in very deep observations or by targeting strongly lensed galaxies. Here we report the results of a pilot survey using the Atacama Compact Array of molecular gas in the most strongly magnified galaxies selected as giant arcs in optical data. The selection in rest-frame ultraviolet (UV) wavelengths ensures that sources are regular SFGs, without a priori indications of intense dusty starburst activity. We conducted Band 4 and Band 7 observations to detect mid-J CO, [C I] and thermal continuum as molecular gas tracers from four strongly lensed systems at z ≈ 2 − 3: our targets are SGAS J1226651.3+215220 (A and B), SGAS J003341.5+024217 and the Sunburst Arc. The measured molecular mass was then projected onto the source plane with detailed lens models developed from high resolution Hubble Space Telescope observations. Multiwavelength photometry was then used to obtain the intrinsic stellar mass and star formation rate via spectral energy distribution modeling. In only one of the sources are the three tracers robustly detected, while in the others they are either undetected or detected in continuum only. The implied molecular gass masses range from 4 × 109 M⊙ in the detected source to an upper limit of ≲109 M⊙ in the most magnified source. The inferred gas fraction and gas depletion timescale are found to lie approximately 0.5–1.0 dex below the established scaling relations based on previous studies of unlensed massive galaxies, but in relative agreement with existing literature about UV-bright lensed galaxies at these high redshifts. Our results indicate that the cold gas content of intermediate to low mass galaxies should not be extrapolated from the trends seen in more massive high-z galaxies. The apparent gas deficit is robust against biases in the stellar mass or star formation rate. However, we find that in this mass-metallicity range, the molecular gas mass measurements are severely limited by uncertainties in the current tracer-to-gas calibrations.

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A Comparison of the Stellar, CO, and Dust-continuum Emission from Three Star-forming HUDF Galaxies at z ∼ 2

Cited by 47 publications

References 128 publications

The ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: CO Excitation and Atomic Carbon in Star-forming Galaxies at z = 1–3

The ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: CO Excitation and Atomic Carbon in Star-forming Galaxies at z = 1–3

IR SED and Dust Masses of Sub-solar Metallicity Galaxies at z~2.3

Molecular gas budget and characterization of intermediate-mass star-forming galaxies at z ≈ 2–3

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