Big Three Dragons: A [N ii] 122 μm Constraint and New Dust-continuum Detection of a z = 7.15 Bright Lyman-break Galaxy with ALMA

Sugahara, Yuma; Inoue, Akio; Hashimoto, T.; Yamanaka, S.; Fujimoto, Seiji; Tamura, Motohide; Matsuo, Hiroshi; Binggeli, Christian; Zackrisson, Erik

doi:10.3847/1538-4357/ac2a36

Cited by 24 publications

(20 citation statements)

References 107 publications

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“…The L([O III] 88 )/SFR ratios of the z > 6 galaxies are comparable to or higher than the local dwarfs, despite their high SFR. These high L([O III] 88 )/SFR ratios at a given SFR are consistent with previous results of higher line-to-L FIR ratios at z > 1 than local line deficit at a given L FIR (e.g., Herrera-Camus et al 2018a;Sugahara et al 2021). The three SMGs exhibit lower L([O III] 88 )/SFR than the other z > 6 galaxies at a given L([C II] 158 )/SFR, implying that SMGs would be analogs of local U/LIRGs, which exhibit lower L([O III] 88 )/SFR than local dwarfs.…”

Section: Fir Sample: Z > 6 Galaxiessupporting

confidence: 92%

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Bridging Optical and Far-infrared Emission-line Diagrams of Galaxies from Local to the Epoch of Reionization: Characteristic High [O iii] 88 μm/SFR at z > 6

Sugahara

Inoue

Fudamoto

et al. 2022

ApJ

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We present photoionization modeling of galaxy populations at z ∼ 0, 2, and >6 to bridge optical and far-infrared (FIR) emission-line diagrams. We collect galaxies with measurements of optical and/or FIR ([O iii] 88 μm and [C ii] 158 μm) emission-line fluxes and plot them on the [O iii ]λ5007/Hβ–[N ii ]λ6585/Hα (BPT) and L([O iii]88)/SFR–L([C ii ]158)/SFR diagrams, where SFR is the star formation rate and L([O iii ]88) and L([C ii ]158) are the FIR line luminosities. We aim to explain the galaxy distributions on the two diagrams with photoionization models that employ three nebular parameters: the ionization parameter U, hydrogen density n H, and gaseous metallicity Z gas. Our models successfully reproduce the nebular parameters of local galaxies, and then predict the distributions of the z ∼ 0, 2, and >6 galaxies in the diagrams. The predicted distributions illustrate the redshift evolution on all the diagrams; e.g., [O iii ]/Hβ and [O iii ]88/[C ii]158 ratios continuously decrease from z > 6 to 0. Specifically, the z > 6 galaxies exhibit ∼0.5 dex higher U than low-redshift galaxies at a given Z gas and show predicted flat distributions on the BPT diagram at log [ O III ] / H β = 0.5–0.8. We find that some of the z > 6 galaxies exhibit high L([O iii]88)/SFR ratios. To explain these high ratios, our photoionization models require a low stellar-to-gaseous-metallicity ratio or bursty/increasing star formation history at z > 6. JWST will test the predictions and scenarios for the z > 6 galaxies proposed by our photoionization modeling.

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Section: Fir Sample: Z > 6 Galaxiessupporting

confidence: 92%

“…The following assumptions are adopted as fiducial models, which partly share the concepts with Nagao et al (2011Nagao et al ( , 2012, Harikane et al (2020b), andSugahara et al (2021). The adopted assumptions are summarized in Table 1.…”

Section: Fiducial Photoionization Modelsmentioning

confidence: 99%

Bridging Optical and Far-infrared Emission-line Diagrams of Galaxies from Local to the Epoch of Reionization: Characteristic High [O iii] 88 μm/SFR at z > 6

Sugahara

Inoue

Fudamoto

et al. 2022

ApJ

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“…The dust emissivities are assumed as β = 1.6 and 2.0. We also compare R0600-ID164 with galaxies at z ; 6 − 7 with normal dust temperatures (40-50 K; shown as green circles) confirmed with ALMA continuum detections in two bands at least, including J1211-0118, J0217-0208 (z = 6.03 and 6.20, respectively; Harikane et al 2020), A1689-zD1 (z = 7.13; Watson et al 2015;Knudsen et al 2017;Inoue et al 2020;Bakx et al 2021), and B14-65666 (z = 7.15;Hashimoto et al 2019;Sugahara et al 2021). Bakx et al (2020) showed that MACS0416 Y1, a lensed galaxy at z = 8.31 (black open squares in Figure 17; also Tamura et al 2019), exhibits abnormally warm dust temperature (T dust >80 K, 90% confidence) and/or steep dust emissivity index (β >2).…”

Section: Gas Depletion Timescalementioning

confidence: 54%

ALMA Lensing Cluster Survey: ALMA-Herschel Joint Study of Lensed Dusty Star-forming Galaxies across z ≃ 0.5 – 6

Sun

Egami

Fujimoto

et al. 2022

ApJ

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We present an ALMA-Herschel joint analysis of sources detected by the ALMA Lensing Cluster Survey (ALCS) at 1.15 mm. Herschel/PACS and SPIRE data at 100–500 μm are deblended for 180 ALMA sources in 33 lensing cluster fields that are detected either securely (141 sources; in our main sample) or tentatively at S/N ≥ 4 with cross-matched HST/Spitzer counterparts, down to a delensed 1.15 mm flux density of ∼0.02 mJy. We performed far-infrared spectral energy distribution modeling and derived the physical properties of dusty star formation for 125 sources (109 independently) that are detected at >2σ in at least one Herschel band. A total of 27 secure ALCS sources are not detected in any Herschel bands, including 17 optical/near-IR-dark sources that likely reside at z = 4.2 ± 1.2. The 16th, 50th, and 84th percentiles of the redshift distribution are 1.15, 2.08, and 3.59, respectively, for ALCS sources in the main sample, suggesting an increasing fraction of z ≃ 1 − 2 galaxies among fainter millimeter sources (f 1150 ∼ 0.1 mJy). With a median lensing magnification factor of μ = 2.6 − 0.8 + 2.6 , ALCS sources in the main sample exhibit a median intrinsic star formation rate of 94 − 54 + 84 M ⊙ yr−1, lower than that of conventional submillimeter galaxies at similar redshifts by a factor of ∼3. Our study suggests weak or no redshift evolution of dust temperature with L IR < 1012 L ⊙ galaxies within our sample at z ≃ 0 − 2. At L IR > 1012 L ⊙, the dust temperatures show no evolution across z ≃ 1–4 while being lower than those in the local universe. For the highest-redshift source in our sample (z = 6.07), we can rule out an extreme dust temperature (>80 K) that was reported for MACS0416 Y1 at z = 8.31.

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“…We treat B14-65666 as a dust-temperature constrained sample. For our analysis, we use the flux density and the size measurements from Sugahara et al (2021).…”

Section: Datamentioning

confidence: 99%

“…Recently, Inoue et al (2020) (hereafter, I20) developed an alternative and simple analytical approach that enables to derive dust temperatures and IR luminosities using single-band dust continuum observations, dust emission sizes, and dust-to-stellar distribution geometry models. So far, the method is applied to a few examples (I20; Sugahara et al 2021), showing that the method constrains dust temperature of high-redshift galaxies well. In this paper, we further examined the applicability of the method developed in I20, calibrated the model using public data from the ALMA archive, and aimed to provide a simple method to derive dust temperature using single ALMA continuum measurements.…”

mentioning

confidence: 99%

Estimating Dust Temperature and Far-IR Luminosity of High-Redshift Galaxies using ALMA Continuum Observations

Fudamoto¹,

Inoue²,

Sugahara³

2022

Preprint

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We present a method that derives dust temperatures and infrared (IR) luminosities of high-redshift galaxies assuming the radiation equilibrium in a simple dust and stellar distribution geometry. Using public data in the Atacama Large Millimeter/submillimeter Array (ALMA) archive, we studied dust temperatures in a clumpy interstellar medium (ISM) model for high-redshift galaxies, and tested consistency of the results with what derived from other methods. We find the dust distribution model assuming clumpiness of log 𝜉 clp = −1.02 ± 0.41 can represent the ISM of high-redshift star-forming galaxies. By assuming the value of 𝜉 clp , our method enables to derive dust temperatures and IR luminosities of high-redshift galaxies from only a single-band ALMA observation that gives two ALMA measurements required for the method: the dust continuum flux and the dust continuum emission size. Using this method, we demonstrate to find the dust temperature (𝑇 d = 95 +13 −17 K) of a 𝑧 ∼ 8.3 star-forming galaxy, MACS0416-Y1. The method only requires a single-band dust observation to derive a dust temperature. It is more easily accessible than multi-band observations or emission line searches at high-redshift. Thus can be applicable to large samples of galaxies in future studies using high-resolution interferometers such as ALMA.

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Big Three Dragons: A [N ii] 122 μm Constraint and New Dust-continuum Detection of a z = 7.15 Bright Lyman-break Galaxy with ALMA

Cited by 24 publications

References 107 publications

Bridging Optical and Far-infrared Emission-line Diagrams of Galaxies from Local to the Epoch of Reionization: Characteristic High [O iii] 88 μm/SFR at z > 6

Bridging Optical and Far-infrared Emission-line Diagrams of Galaxies from Local to the Epoch of Reionization: Characteristic High [O iii] 88 μm/SFR at z > 6

ALMA Lensing Cluster Survey: ALMA-Herschel Joint Study of Lensed Dusty Star-forming Galaxies across z ≃ 0.5 – 6

Estimating Dust Temperature and Far-IR Luminosity of High-Redshift Galaxies using ALMA Continuum Observations

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