CO (7−6), [C i] 370 μm, and [N ii] 205 μm Line Emission of the QSO BRI 1335-0417 at Redshift 4.407

Lu, N.; Cao, Tianwen; Díaz-Santos, T.; Zhao, Yi; Privon, George C.; Cheng, Cheng; Gao, Yu; Xu, C. K.; Charmandaris, V.; Rigopoulou, D.; Werf, P. P. van der; Huang, Jia-Sheng; Wang, Zhong; Evans, A. S.; Sanders, D. B.

doi:10.3847/1538-4357/aad3c9

Cited by 29 publications

(29 citation statements)

References 90 publications

(130 reference statements)

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“…To make the estimates for the QSO and SMG, we used the infrared luminosities from Salomé et al (2012). Other estimates from the literature are a few times higher (Wagg et al 2014;Lu et al 2018) and would yield values that have greater consistency with the best fit shown in the figure.…”

Section: H 2 O: Ir-pumping and Energy Dissipationmentioning

confidence: 99%

“…BR 1202-0725 is a well-studied, unlensed group composed of a quasi-stellar object (QSO), a sub-millimeter galaxy (SMG;McMahon et al 1994;Smail et al 1997), and two Lyα emitters (LAEs; e.g., Hu et al 1996). Both the QSO and SMG are very luminous IR emitters, ∼10 13 L , and the system has been observed in a wide range of molecular and atomic lines (Omont et al 1996;Benford et al 1999;Salomé et al 2012;Carilli et al 2013;Lu et al 2017aLu et al , 2018, and references therein). Based on an excess in the wing of the line profile of [CII], Carilli et al (2013) estimated an outflow rate in the atomic gas from the QSO ofṀ out ∼80 M yr −1 and concluded that the gas depletion time due to this outflow is ∼600 Myrs, a factor of 10 longer than the gas consumption time due to star formation.…”

Section: Introductionmentioning

confidence: 99%

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Etching glass in the early Universe: Luminous HF and H₂O emission in a QSO-SMG pair at z = 4.7

Lehnert

Yang

Emonts

et al. 2020

A&A

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We present ALMA observations of hydrogen fluoride, HF J = 1–0, water, H2O (220–211), and the 1.2 THz rest-frame continuum emission from the z = 4.7 system BR 1202-0725. System BR 1202-0725 is a galaxy group consisting of a quasi-stellar object (QSO), a sub-millimeter galaxy (SMG), and a pair of Lyα emitters. We detected HF in emission in the QSO and possibly in absorption in the SMG, while water was detected in emission in both the QSO and the SMG. The QSO is the most luminous HF J = 1–0 emitter that has yet been found and has the same ratio of HF emission-line to infrared luminosity, LHF/LIR, as a small sample of local active galactic nuclei and the Orion Bar. This consistency covers about ten orders of magnitude in LIR. Based on the conclusions of a study of HF emission in the Orion Bar and simple radiative transfer modeling, the HF emission in the QSO is excited either by collisions with electrons (and H2) in molecular plasmas irradiated by the AGN and intense star formation, or predominately by collisions with H2, with a modest contribution from electrons, in a relatively high temperature (∼120 K), dense (∼105 cm−3) medium. The high density of electrons necessary to collisionally excite the HF J = 1–0 line can be supplied in sufficient quantities by the estimated column density of C+. Although HF should be an excellent tracer of molecular outflows, we found no strong kinematic evidence for outflows in HF in either the QSO or the SMG. From a putative absorption feature in HF observed against the continuum emission from the SMG, we conducted a bootstrap analysis to estimate an upper limit on the outflow rate, Ṁoutflow ≲ 45 M⊙ yr−1. This result implies that the ratio of the molecular outflow rate to the star formation rate is Ṁoutflow/SFR ≲ 5% for the SMG. Both the QSO and the SMG are among the most luminous H2O (220–211) emitters currently known and are found to lie along the same relationship between LH2O (220 − 211)/LIR and LIR as a large sample of local and high-redshift star-forming galaxies. The kinematics of the H2O (220–211) line in the SMG is consistent with a rotating disk as found previously but the line profile appears broader than other molecular lines, with a full width at half maximum of ∼1020 km s−1. The broadness of the line, which is similar to the width of a much lower resolution observation of CO(2-1), may suggest that either the gas on large scales (≳4 kpc) is significantly more disturbed and turbulent due either to interactions and mass exchange with the other members of the group, or to the dissipation of the energy of the intense star formation, or both. Overall however, the lack of significant molecular outflows in either source may imply that much of the energy from the intense star formation and active galactic nucleus in this pair is being dissipated in their interstellar media.

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Section: H 2 O: Ir-pumping and Energy Dissipationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Etching glass in the early Universe: Luminous HF and H₂O emission in a QSO-SMG pair at z = 4.7

Lehnert

Yang

Emonts

et al. 2020

A&A

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“…At high-z, observations of the [Nii] 205 µm line is largely limited to z > 3.9, where the line is red-shifted to wavelengths longer than 1mm, making ground based observations possible due to the more transmissive and stable atmosphere, with lower receiver noise temperatures. The current sample where this emission line is detected consists of twelve highly star-forming galaxies (Decarli et al 2012(Decarli et al , 2014Combes et al 2012;Rawle et al 2014;Nagao et al 2012;Béthermin et al 2016;Pavesi et al 2016Pavesi et al , 2018bLu et al 2018), and there are at least five additional non-detections (see Walter et al 2009;Riechers et al 2013a).…”

Section: Introductionmentioning

confidence: 97%

The ‘Red Radio Ring’: ionized and molecular gas in a starburst/active galactic nucleus at z ∼ 2.55

Harrington¹,

Vishwas

Weiß

et al. 2019

Monthly Notices of the Royal Astronomical Society

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ABSTRACT We report the detection of the far-infrared (FIR) fine-structure line of singly ionized nitrogen, [N ii] 205 $\mu$m , within the peak epoch of galaxy assembly, from a strongly lensed galaxy, hereafter ‘The Red Radio Ring’; the RRR, at z = 2.55. We combine new observations of the ground-state and mid-J transitions of CO (Jup = 1, 5, 8), and the FIR spectral energy distribution (SED), to explore the multiphase interstellar medium (ISM) properties of the RRR. All line profiles suggest that the H ii regions, traced by [N ii] 205 $\mu$m , and the (diffuse and dense) molecular gas, traced by CO, are cospatial when averaged over kpc-sized regions. Using its mid-IR-to-millimetre (mm) SED, we derive a non-negligible dust attenuation of the [N ii] 205 $\mu$m line emission. Assuming a uniform dust screen approximation results a mean molecular gas column density >1024 cm−2, with a molecular gas-to-dust mass ratio of 100. It is clear that dust attenuation corrections should be accounted for when studying FIR fine-structure lines in such systems. The attenuation corrected ratio of $L_{\rm N\,{\small II}205} / L_{\rm IR(8\!-\!1000\, \mu m)} = 2.7 \times 10^{-4}$ is consistent with the dispersion of local and z > 4 SFGs. We find that the lower limit, [N ii] 205 $\mu$m -based star formation rate (SFR) is less than the IR-derived SFR by a factor of 4. Finally, the dust SED, CO line SED, and $L_{\rm N\,{\small II}205}$ line-to-IR luminosity ratio of the RRR is consistent with a starburst-powered ISM.

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“…[Cii]/[Nii] line luminosity ratios observed in high redshift galaxies to-date as a function of their FIR luminosityDe Breuck et al 2014;Béthermin et al 2016;Rawle et al 2014;Combes et al 2012;Riechers et al 2013Riechers et al , 2014Capak et al 2015;Wagg et al 2010;Umehata et al 2017;Lu et al 2018;Pavesi et al 2018b).For comparison we also show a sample of local ULIRGs from Farrah et al (2013) (using the [Nii] 122 µm line) and LIRGs with [Nii] (using the [Nii] 205 µm line) from Zhao et al (2016) and [Cii] from Díaz-Santos et al (2013). The range of ratios in dwarfs (Cormier et al 2015) (using the [Nii] 122 µm line) is shown as a cyan band.…”

mentioning

confidence: 99%

Low Star Formation Efficiency in Typical Galaxies at z = 5–6

Pavesi

Riechers

Faisst

et al. 2019

ApJ

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Using the VLA and ALMA, we have obtained CO(2-1), [Cii], [Nii] line emission and multiple dust continuum measurements in a sample of "normal" galaxies at z = 5−6. We report the highest redshift detection of low-J CO emission from a Lyman Break Galaxy, at z ∼ 5.7. The CO line luminosity implies a massive molecular gas reservoir of (1.3 ± 0.3)(α CO /4.5 M (K km s −1 pc 2 ) −1 ) × 10 11 M , suggesting low star formation efficiency, with a gas depletion timescale of order ∼1 Gyr. This efficiency is much lower than traditionally observed in z 5 starbursts, indicating that star forming conditions in Main Sequence galaxies at z ∼ 6 may be comparable to those of normal galaxies probed up to z ∼ 3 to-date, but with rising gas fractions across the entire redshift range. We also obtain a deep CO upper limit for a Main Sequence galaxy at z ∼ 5.3 with ∼ 3 times lower SFR, perhaps implying a high α CO conversion factor, as typically found in low metallicity galaxies. For a sample including both CO targets, we also find faint [Nii] 205 µm emission relative to [Cii] in all but the most IR-luminous "normal" galaxies at z = 5 − 6, implying more intense or harder radiation fields in the ionized gas relative to lower redshift. These radiation properties suggest that low metallicity may be common in typical ∼10 10 M galaxies at z = 5 − 6. While a fraction of Main Sequence star formation in the first billion years may take place in conditions not dissimilar to lower redshift, lower metallicity may affect the remainder of the population.

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CO (7−6), [C i] 370 μm, and [N ii] 205 μm Line Emission of the QSO BRI 1335-0417 at Redshift 4.407

Cited by 29 publications

References 90 publications

Etching glass in the early Universe: Luminous HF and H₂O emission in a QSO-SMG pair at z = 4.7

Etching glass in the early Universe: Luminous HF and H₂O emission in a QSO-SMG pair at z = 4.7

The ‘Red Radio Ring’: ionized and molecular gas in a starburst/active galactic nucleus at z ∼ 2.55

Low Star Formation Efficiency in Typical Galaxies at z = 5–6

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CO (7−6), [C i] 370 μm, and [N ii] 205 μm Line Emission of the QSO BRI 1335-0417 at Redshift 4.407

Cited by 29 publications

References 90 publications

Etching glass in the early Universe: Luminous HF and H2O emission in a QSO-SMG pair at z = 4.7

Etching glass in the early Universe: Luminous HF and H2O emission in a QSO-SMG pair at z = 4.7

The ‘Red Radio Ring’: ionized and molecular gas in a starburst/active galactic nucleus at z ∼ 2.55

Low Star Formation Efficiency in Typical Galaxies at z = 5–6

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Etching glass in the early Universe: Luminous HF and H₂O emission in a QSO-SMG pair at z = 4.7

Etching glass in the early Universe: Luminous HF and H₂O emission in a QSO-SMG pair at z = 4.7