Detection of [O iii] at z ∼ 3: A Galaxy Above the Main Sequence, Rapidly Assembling Its Stellar Mass

Vishwas, Amit; Ferkinhoff, Carl; Nikola, Thomas; Parshley, Stephen C.; Schoenwald, Justin; Stacey, G. J.; Higdon, Sarah J.U.; Higdon, James L.; Weiß, A.; Güsten, R.; Menten, K. M.

doi:10.3847/1538-4357/aab354

Cited by 13 publications

(17 citation statements)

References 76 publications

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“…The Cormier et al 2015). The ratio is as high as those found for z = 7-9 UV-selected galaxies, such as SXDF-NB1006- Ferkinhoff et al 2010;Ivison et al 2010;Valtchanov et al 2011;Vishwas et al 2018). All of the z > 7 galaxies, except for SPT0311−58 E/W, are assumed to have the dust temperature of T dust = 50 K; note that LIR decreases by a factor of 0.7 if assuming T dust = 40 K. The IR luminosities are corrected for magnification, if any.…”

Section: Blind Detection Of [O Iii] 88 µMmentioning

confidence: 59%

“…−3 , Carniani et al 2017), and A2744 YD4 at z = 8.38 (∼ 1 × 10 −3 , Laporte et al 2017), although SXDF-NB1006-2 and MACS1149-JD1 may have much higher values. The ratio of MACS0416 Y1, however, exhibits a sharp contrast to those found in local spirals, ultra-luminous IR galaxies (Herrera-Camus et al 2018a,b, see the gray open squares inFigure 4), z ∼ 2-7 submillimeter galaxies ( 1 × 10 −3 or less,Ferkinhoff et al 2010;Valtchanov et al 2011;Marrone et al 2018;Vishwas et al 2018), and an IR-luminous quasar APM 08279+5255 (3 × 10 −4 ,Ferkinhoff et al 2010).…”

mentioning

confidence: 91%

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Detection of the Far-infrared [O iii] and Dust Emission in a Galaxy at Redshift 8.312: Early Metal Enrichment in the Heart of the Reionization Era

Tamura

Mawatari

Hashimoto

et al. 2019

ApJ

216

229

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We present the Atacama Large Millimeter/submillimeter Array (ALMA) detection of the [O iii] 88 µm line and rest-frame 90 µm dust continuum emission in a Y -dropout Lyman break galaxy (LBG), MACS0416 Y1, lying behind the Frontier Field cluster MACS J0416.1−2403. This [O iii] detection confirms the LBG with a spectroscopic redshift of z = 8.3118 ± 0.0003, making this object one of the furthest galaxies ever identified spectroscopically. The observed 850 µm flux density of 137 ± 26 µJy corresponds to a de-lensed total infrared (IR) luminosity of L IR = (1.7±0.3)×10 11 L if assuming a dust temperature of T dust = 50 K and an emissivity index of β = 1.5, yielding a large dust mass of 4×10 6 M . The ultraviolet-to-far IR spectral energy distribution modeling where the [O iii] emissivity model is incorporated suggests the presence of a young (τ age ≈ 4 Myr), star-forming (SFR ≈ 60 M yr −1 ), moderately metal-polluted (Z ≈ 0.2Z ) stellar component with a mass of M star = 3 × 10 8 M . An analytic dust mass evolution model with a single episode of star-formation does not reproduce the metallicity and dust mass in τ age ≈ 4 Myr, suggesting a pre-existing evolved stellar component with M star ∼ 3 × 10 9 M and τ age ∼ 0.3 Gyr as the origin of the dust mass.

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Section: Blind Detection Of [O Iii] 88 µMmentioning

confidence: 59%

mentioning

confidence: 91%

Detection of the Far-infrared [O iii] and Dust Emission in a Galaxy at Redshift 8.312: Early Metal Enrichment in the Heart of the Reionization Era

Tamura

Mawatari

Hashimoto

et al. 2019

ApJ

216

229

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“…Both single dish submillimetre telescopes and interferometers have also detected the [NII] 122 µm and 205 µm lines at high redshift (Ferkinhoff et al 2011(Ferkinhoff et al , 2015Combes et al 2012;Nagao et al 2012;Decarli et al 2012Decarli et al , 2014Béthermin et al 2016;Pavesi et al 2016;Lu et al 2017;Tadaki et al 2019;Novak et al 2019). After a slow start, the [OIII] 88 µm line is quickly becoming a popular line to confirm redshifts of galaxies in the epoch of reionization (z 6), where it shifts into the submillimetre atmospheric windows below 500 GHz Inoue et al 2016;Carniani et al 2017;Marrone et al 2018;Vishwas, et al 2018;Hashimoto, et al 2018;Walter et al 2018;Tamura et al 2019;Tadaki et al 2019;Hashimoto et al 2019;Novak et al 2019). Deep Herschel/SPIRE spectroscopy has also revealed a number of FSL detections, either in individual objects (Valtchanov et al 2011;Coppin et al 2012;George et al 2013;Uzgil et al 2016;Rigopoulou et al 2018;Zhang et al 2018), or in stacked spectra (Wardlow et al 2017;Wilson et al 2017;Zhang et al 2018).…”

Section: Introductionmentioning

confidence: 99%

A dense, solar metallicity ISM in the z = 4.2 dusty star-forming galaxy SPT 0418−47

Breuck

Weiß

Béthermin

et al. 2019

A&A

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We present a study of six far-infrared fine structure lines in the z=4.225 lensed dusty star-forming galaxy SPT 0418-47 to probe the physical conditions of its inter stellar medium (ISM). In particular, we report Atacama Pathfinder EXperiment (APEX) detections of the [OI] 145µm and [OIII] 88µm lines and Atacama Compact Array (ACA) detections of the [NII] 122 and 205µm lines. The [OI] 145µm / [CII] 158µm line ratio is ∼5× higher compared to the average of local galaxies. We interpret this as evidence that the ISM is dominated by photo-dissociation regions with high gas densities. The line ratios, and in particular those of [OIII] 88µm and [NII] 122µm imply that the ISM in SPT 0418-47 is already chemically enriched close to solar metallicity. While the strong gravitational amplification was required to detect these lines with APEX, larger samples can be observed with the Atacama Large Millimeter/submillimeter Array (ALMA), and should allow observers to determine if the dense, solar metallicity ISM is common among these highly star-forming galaxies.

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“…The [N ii] 205 µm line (or [N ii] 122 µm) and the [O iii] 88 µm line (or [O iii] 52 µm) emission both arise only from ionized gas as the ionization potential is higher than that of hydrogen (> 13.6 eV). In SMGs at z > 3, these lines have been detected with ground-based telescopes (e.g., Ferkinhoff et al 2010;Pavesi et al 2016;Lu et al 2017;Vishwas et al 2018;Marrone et al 2018;Pavesi et al 2018;Walter et al 2018) and with Herschel (e.g., Valtchanov et al 2011;Zhang et al 2018). The line ratio of nitrogen and oxygen can be used as an indicator of gas-phase metallicity, which is commonly estimated from observations of rest-frame optical lines (Pereira-Santaella et al 2017;Rigopoulou et al 2018).…”

Section: Introductionmentioning

confidence: 99%

CNO Emission of an Unlensed Submillimeter Galaxy at z = 4.3

Tadaki

Iono

Hatsukade

et al. 2019

ApJ

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We present the results from ALMA observations of [N ii] 205 µm, [C ii] 158 µm, and [O iii] 88 µm lines in an unlensed submillimeter galaxy at z = 4.3, COSMOS-AzTEC-1, hosting a compact starburst core with an effective radius of ∼1 kpc. The [C ii] and [N ii] emission are spatially-resolved in 0.3 ′′ -resolution (1 kpc in radius). The kinematic properties of the [N ii] emission are consistent with those of the CO(4-3) and [C ii] emission, suggesting that the ionized gas feels the same gravitational potential as the associated molecular gas and photodissociation regions (PDRs). On the other hand, the spatial extent is different among the lines and dust continuum: the [C ii] emitting gas is the most extended and the dust is the most compact, leading to a difference of the physical conditions in the interstellar medium. We derive the incident far-ultraviolet flux and the hydrogen gas density through PDR modeling by properly subtracting the contribution of ionized gas to the total [C ii] emission. The observed [C ii] emission is likely produced by dense PDRs with n PDR H = 10 5.5−5.75 cm −3 and G 0 = 10 3.5−3.75 in the central 1 kpc region and n PDR H = 10 5.0−5.25 cm −3 and G 0 = 10 3.25−3.5 in the central 3 kpc region. We have also successfully measured the line ratio of [O iii]/[N ii] in the central 3 kpc region of COSMOS-AzTEC-1 at z = 4.3, which is the highest redshift where both nitrogen and oxygen lines are detected. Under the most likely physical conditions, the measured luminosity ratio of L [OIII] /L [NII] = 6.4 ± 2.2 indicates a near solar metallicity with Z gas = 0.7 − 1.0 Z ⊙ , suggesting a chemically evolved system at z = 4.3.

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Detection of [O iii] at z ∼ 3: A Galaxy Above the Main Sequence, Rapidly Assembling Its Stellar Mass

Cited by 13 publications

References 76 publications

Detection of the Far-infrared [O iii] and Dust Emission in a Galaxy at Redshift 8.312: Early Metal Enrichment in the Heart of the Reionization Era

Detection of the Far-infrared [O iii] and Dust Emission in a Galaxy at Redshift 8.312: Early Metal Enrichment in the Heart of the Reionization Era

A dense, solar metallicity ISM in the z = 4.2 dusty star-forming galaxy SPT 0418−47

CNO Emission of an Unlensed Submillimeter Galaxy at z = 4.3

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