The [NII] 205 $\mu$m line emission from high-z SMGs and QSOs

Axel Weiss; Bram P. Venemans; Carl Ferkinhoff; Dominik A. Riechers; Emanuele Paolo Farina; Fabian Walter; Frank Bertoldi; Pierre Cox; Roberto Decarli; Roberto Neri

REVIEW 5 major objections 4 minor 114 references

The [NII] 205 $\mu$m line emission from high-z SMGs and QSOs

T0 review · 5 major / 4 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read At redshift 4–6, submillimeter galaxies and quasar hosts follow the [NII] line deficit, and AGN photoionization does not boost [NII] 205 μm emission.

desk verdict Useful new [NII] 205 um measurements, but the PDR fraction headline rests on a favorable normalization choice and should be revised. read the letter →

arxiv 2502.08984 v2 pith:YHBRRMMR submitted 2025-02-13 astro-ph.GA

Saimurali Kolupuri , Roberto Decarli , Roberto Neri , Pierre Cox , Carl Ferkinhoff , Frank Bertoldi , Axel Weiss , Bram P. Venemans

show 3 more authors

Dominik A. Riechers Emanuele Paolo Farina Fabian Walter

This is my paper · ORCID

classification astro-ph.GA

keywords [NII]205μmfine-structurelinehigh-redshiftgalaxiessubmillimeterquasarhost[CII]158deficitphoton-dominatedregionsinterstellarmediumdiagnostics

verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

The paper reports millimetre-interferometric observations of the $\mathrm{[NII]}\,205\,\mu$m fine-structure line toward six galaxies at redshift $4\lesssim z\lesssim 6$: three submillimeter galaxies (SMGs) and three quasar hosts. The line is detected in GN20, ID141, and PSSJ2322+1944, with upper limits for the other three sources. The authors argue that the $[\mathrm{NII}]$-to-infrared luminosity ratio follows the same 'line deficit' seen in local ultraluminous infrared galaxies, that the $[\mathrm{CII}]$-to-$[\mathrm{NII}]$ ratios imply most $[\mathrm{CII}]\,158\,\mu$m emission arises from neutral gas, and that the ratios are indistinguishable between SMGs and QSOs, so AGN photoionization contributes negligibly to $[\mathrm{NII}]\,205\,\mu$m emission. If correct, $[\mathrm{NII}]\,205\,\mu$m can serve as a star-formation tracer at early cosmic times without an AGN correction.

What carries the argument

The central diagnostic is the $[\mathrm{NII}]\,205\,\mu$m forbidden fine-structure line ($^3P_1\rightarrow {}^3P_0$), which arises almost exclusively from warm ionized gas. The analysis uses two ratios built on it: the line-to-infrared luminosity ratio, which measures how efficiently line cooling keeps pace with dust emission, and the $[\mathrm{CII}]\,158\,\mu$m-to-$[\mathrm{NII}]\,205\,\mu$m ratio, which separates neutral and ionized contributions to $[\mathrm{CII}]$. The PDR fraction is computed through the identity $f_{\mathrm{PDR}}\approx 1 - 3\,[\mathrm{NII}]_{205}/[\mathrm{CII}]_{158}$ (or with the factor 9 in place of 3). Supporting machinery consists of modified-blackbody dust SED fits that supply $L_{\mathrm{IR}}$, and gravitational magnification factors taken from $[\mathrm{CII}]$ or CO measurements that are assumed to apply unchanged to the $[\mathrm{NII}]$ emission.

What would settle it

Resolve the $[\mathrm{NII}]\,205\,\mu$m emission at sub-arcsecond scale in a strongly lensed source such as ID141 or PSSJ2322+1944 and compare the lensing magnification inferred from $[\mathrm{NII}]$ with that from $[\mathrm{CII}]$ or CO; additionally, measure the $[\mathrm{NII}]\,122\,\mu$m line in the same sources to obtain electron densities and a direct ionized-$[\mathrm{CII}]/[\mathrm{NII}]$ ratio. If the magnification factors disagree, or if the resulting ratios move the sources off the deficit trend, the paper's quantitative conclusions would need revision.

Watch

Extended reading notes

Core claim

On the paper's own terms, the $[\mathrm{NII}]\,205\,\mu$m line is detected in GN20, ID141, and PSSJ2322+1944, while HDF850.1, J2054-0005, and J2310+1855 yield 3$\sigma$ upper limits. Combining these with literature detections at $3<z<6$ and local samples, the authors find $L_{\mathrm{[NII]}}/L_{\mathrm{IR}}$ spans roughly $10^{-4}$ to $10^{-5}$ and decreases with infrared luminosity, matching the $[\mathrm{NII}]$ fine-structure line deficit. The $[\mathrm{CII}]$-to-$[\mathrm{NII}]$ luminosity ratios exceed 10 for most sources, placing them in the XDR/PDR/shock regime; assuming the ionized-$[\mathrm{CII}]/[\mathrm{NII}]$ ratio of about 3, this implies more than 75% of the $[\mathrm{CII}]\,158\,\mu$m emission arises from photon-dominated regions (with lower fractions of 27–62% if the newer ratio of about 9 is adopted). The same ratios show no offset between SMGs and QSOs, leading the authors to conclude that AGN photoionization has a negligible effect on $[\mathrm{NII}]\,205\,\mu$m emission.

Load-bearing premise

All corrected luminosities and ratios assume that the gravitational magnification measured from $[\mathrm{CII}]\,158\,\mu$m or CO emission applies unchanged to the $[\mathrm{NII}]\,205\,\mu$m emission; if the $[\mathrm{NII}]$-emitting region is more compact or differently lensed, the quantitative results and the SMG-versus-QSO comparison would change.

Editorial extensions

If this is right

If the conclusion holds, the $[\mathrm{NII}]\,205\,\mu$m line can be used as a star-formation-rate indicator at $z\sim4$–$6$ in both SMGs and quasar hosts without an AGN correction.
The $[\mathrm{NII}]$ line deficit is already in place within the first roughly one billion years of cosmic history, for both starbursting and AGN-host galaxies, implying its physical drivers are not unique to the local Universe.
For these infrared-bright sources, most of the $[\mathrm{CII}]\,158\,\mu$m emission traces the neutral medium, so $[\mathrm{CII}]$ remains a neutral-gas tracer even around luminous quasars.
The new upper limits are consistent with the deficit trend, so deeper integrations should detect $[\mathrm{NII}]\,205\,\mu$m in more high-redshift sources and tighten the comparison between populations.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

The stated magnification assumption could be tested directly: if high-resolution $[\mathrm{NII}]\,205\,\mu$m imaging shows the line is more compact than the $[\mathrm{CII}]$/CO emission in lensed sources, the corrected $[\mathrm{NII}]$ luminosities would shrink and the absolute ratios would shift.
The derived photon-dominated-region fractions depend on the adopted ionized-$[\mathrm{CII}]/[\mathrm{NII}]$ ratio; with the higher value of about 9, some sources would have only 27–62% of their $[\mathrm{CII}]$ from neutral gas, softening the claim that $[\mathrm{CII}]$ is neutral-dominated.
The absence of an AGN boost could mean AGN ionizing photons are absorbed by dust before reaching the [NII]-emitting gas, or that this gas is spatially decoupled from the nucleus; spatially resolved [NII] imaging in quasar hosts would distinguish these options.
A natural extension is to measure $[\mathrm{NII}]\,122\,\mu$m and $[\mathrm{OIII}]\,88\,\mu$m in the same sources, which would yield electron densities and ionization conditions and test whether the ionized-gas properties of SMGs and QSOs really are identical.

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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Desk Editor's Note

read the letter

Candid take: this paper is a solid, small-sample observational contribution: new [NII] 205 um measurements for six high-z sources, including three detections and three useful upper limits. The measurements and the comparison with local ULIRGs are the real value. The line deficit trend, with [NII]/IR dropping toward high L_IR, looks plausible and is consistent with earlier work. Credit where due: the data reduction is careful, the SED fitting is documented, and the authors explicitly state assumptions about magnification and the [CII]_ion/[NII] normalization. That transparency is why the paper is salvageable.

The main soft spot is the abstract's f_PDR>75% claim. Equation (2) and Table 3 show that this number comes from assuming [CII]_ion/[NII]=3. The authors themselves note that more recent estimates give ~9, which drops the derived fractions to 27-62%. The abstract and conclusions do not carry that caveat, so the headline "bulk of [CII] arises from the neutral medium" is an artifact of choosing the favorable normalization. That should be fixed before publication. Also, calling PSSJ2322 "well detected" at 2.4 sigma is generous; it's a low-S/N detection and the fitted flux should be treated with caution. The SMG/QSO comparison is based on a handful of sources with no statistical test, so "no significant differences" is not really established—better to say "no obvious differences in this small sample." The magnification assumption (same lensing for [NII] as for [CII]/CO) is stated clearly, but it is a systematic uncertainty that could shift the ratios; worth a sentence in the error budget.

Who is this for? People working on high-z ISM and fine-structure line diagnostics. The dataset is useful and the literature comparison is thorough. It deserves a serious referee, but the referee should require the PDR fraction caveat and the low-S/N language to be fixed. With those changes, it is a publishable contribution.

Referee Report

5 major / 4 minor

Summary. This paper presents IRAM PdBI/NOEMA observations of the [NII] 205 µm fine-structure line and underlying dust continuum in three submillimeter galaxies (GN20, ID141, HDF850.1) and three quasar hosts (PSSJ2322+1944, J2054-0005, J2310+1855) at 4≲z≲6. The authors report [NII] detections in GN20, ID141, and PSSJ2322+1944, upper limits for the other three sources, and new continuum measurements used to fit dust SEDs and derive infrared luminosities. From these data they compute L[NII]/L_IR and L[CII]/L[NII] ratios, place the sample on the [NII] fine-structure line deficit relation, and estimate the PDR fraction of [CII] using an assumed [CII]_ion/[NII] ratio. They conclude that the neutral medium dominates the [CII] emission and that AGN photoionization makes a negligible contribution to the [NII] 205 µm emission.

Significance. If the results hold, they enlarge the small sample of high-redshift [NII] 205 µm detections and support the extension of the local [NII] fine-structure deficit to z∼4–6. The paper is also useful as a compilation of archival IRAM observations with documented SED fitting and explicit statements of assumptions. The body of the paper is largely honest about its systematics: Table 3 reports both normalizations of the [CII]_ion/[NII] ratio, the magnification assumption is stated in Table 1, and no parameter is tuned to force the key ratios. However, the abstract and conclusions do not carry these caveats, and the headline PDR-fraction claim is not robust to the adopted calibration.

major comments (5)

[§3.3, Eq. (2); Table 3; Abstract] The PDR-fraction headline is normalization-dependent and is overstated in the Abstract and Conclusions. Equation (2) adopts [CII]_ion/[NII]_205∼3, yielding f([CII]PDR)=76–87%, but the same section and Table 3 note that more recent estimates give a ratio of ∼9, for which the tabulated fractions become 42%±16% (ID141), >27% (HDF850.1), <35% (PSSJ2322+1944), >41% (J2054-0005), and >62% (J2310+1855). None of these reaches 75%, so the abstract's claim that 'the bulk of the [CII] 158 µm line emission (f([CII]PDR)>75%) arises from the neutral medium' is an artifact of choosing the more favorable normalization rather than a robust consequence of the data. Please revise the Abstract and Conclusions to state that >75% holds only under the ratio of 3, or to quote the range from both normalizations.
[Table 1, note (a)] All luminosity ratios and the subsequent deficit and SMG/QSO comparisons depend on the assumption that the gravitational magnification measured from [CII] or CO also applies to the [NII] 205 µm emission. The paper states this assumption but does not assess its impact. If the [NII]-emitting region is more compact or differently lensed than the [CII]/CO tracer, the corrected L[NII] values, L[NII]/L_IR, and L[CII]/L[NII] for ID141, HDF850.1, and PSSJ2322+1944 would shift systematically, potentially changing the quantitative conclusions. Please add a discussion of differential lensing or adopt conservative magnification uncertainties in the ratio analysis.
[§3.1 and Table 3] The detection significance of PSSJ2322+1944 is overstated. Table 3 reports F_line = 1.7 ± 0.7 Jy km/s, which is only a ∼2.4σ measurement, and GN20 is also only ∼3.3σ. Describing PSSJ2322+1944 as 'well detected' in Section 3.1 and stating in the Abstract that '[NII] emission is detected in three sources' overstates the confidence for this source. Please reclassify PSSJ2322+1944 as a tentative or marginal detection, or propagate it as an upper limit in the ratio analysis where appropriate.
[§3.3] The statement that 'for all of our sources, the [CII]/[NII] value is >10' is inconsistent with Table 3. PSSJ2322+1944 has a ratio quoted as an upper limit, <14.1, so the data do not constrain it to exceed 10, and GN20 has no [CII] measurement at all. The text should say 'most of our sources' and clearly treat PSSJ2322+1944 as an upper limit.
[§3.2 and §4] The conclusion that AGN photoionization has a 'negligible contribution' to [NII] 205 µm emission is stronger than the data support. The SMG/QSO comparison is based on six sources, three of which have only [NII] upper limits, and no statistical test is presented. The paper should state that no significant difference is detected in this small sample, rather than suggesting that the AGN contribution is negligible.

minor comments (4)

[§2.2] The text assigns 3.34 h on-source time to J2054-0005 and 3.45 h to J2310+1855, while Table 2 lists 3.45 h and 3.34 h, respectively; the assignment is reversed.
[§3.1] In the GN20 paragraph, 'Fline = 2.3±0.7 km s−1' should read 'Jy km s−1' to indicate the integrated line flux units.
[Reference list] The entry 'Sun, F., Helton, J. M., Egami, E., et al. (2024), ApJ, 961, 69' appears twice with identical bibliographic data; the duplicate should be removed.
[Table 3] The source label in column (1) truncates PSSJ2322+1944 to 'PSSJ2322'; please use the full source name for consistency with the rest of the paper.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: all derived ratios follow directly from observed fluxes, SED fitting, and stated literature assumptions; the key [CII] PDR fraction caveat is disclosed in the text.

full rationale

The paper's central quantities are measured luminosities and luminosity ratios. [NII] 205 micron luminosities are computed from integrated line fluxes via Eq. (1), which is a standard conversion; infrared luminosities come from independent SED fits to continuum photometry (Appendix B). The [NII]/IR and [CII]/[NII] ratios are therefore arithmetic combinations of observed or literature-based quantities, not parameters fitted to those target ratios. The [CII] PDR fraction in Eq. (2) does depend on an assumed [CII]_ion/[NII] ratio of ~3, taken from Oberst et al. (2006), but the paper explicitly states this assumption and simultaneously reports the lower fractions (27%-62%) obtained with the higher ratio ~9 from Decarli et al. (2023). This makes the 75% claim assumption-sensitive rather than circular: no quantity is defined in terms of the conclusion it is used to support. The magnification assumption in Table 1, note (a), is a clearly stated but unverified premise about source structure, not a restatement of any derived result, so it does not constitute circularity. Self-citations to Decarli et al. (2014, 2023) are used as comparative model/literature anchors, not as uniqueness theorems forcing the paper's choices. There is no fitted input renamed as a prediction, no load-bearing self-citation chain, and no derivation that reduces by construction to its own inputs.

Assumptions & free parameters 4 free parameters · 4 assumptions · 0 invented entities

All free parameters are either fit to photometry (dust temperature, mass, beta) or adopted from the literature (the CII/NII ratio). The assumptions are standard in the field; no new physical entities are introduced.

free parameters (4)

Dust temperature per source = 32.9, 38.1, 30.7, 38.1, 59.7, 67.0 K
Fitted with MCMC to SED photometry; directly sets L_IR used in the L_NII/L_IR ratios (Table B.1).
Dust mass per source = 1.99, 7.67, 0.23, 2.51, 0.17, 0.43 x 10^9 Msun
Fitted in the same modified-blackbody SED model; contributes to L_IR and therefore to the reported ratios.
Dust emissivity index beta (QSOs only) = 1.84, 1.83, 1.88
Fitted for the two quasars and PSSJ2322; fixed for SMGs from literature. SED shape depends on this parameter (Table B.1).
Assumed [CII]_ion/[NII]_205 ratio = ~3 (Oberst 2006), ~9 (Decarli 2023)
Chosen from the literature; Eq. 2 converts [CII]/[NII] into f_PDR, so the neutral-medium fraction claim depends on this value (Section 3.3).

assumptions (4)

domain assumption Concordance cosmology with H0=70 km/s/Mpc, Omega_M=0.3, Omega_Lambda=0.7
Used to compute luminosity distances and line luminosities throughout (end of Section 1).
domain assumption Gravitational magnification factor measured from [CII] or CO applies to [NII] 205 um emission
Table 1 note (a) states the assumption; if [NII] has a different spatial distribution, all corrected luminosities shift.
domain assumption Modified blackbody dust SED model, optically thin for SMGs and optically thick for QSOs, with opacity law from Beelen et al. (2006)
Appendix B; L_IR values are outputs of this model, and the ratios inherit its uncertainties.
domain assumption [CII]_ion/[NII]_205 ratio of ~3 (Oberst 2006) or ~9 (Decarli 2023) characteristic of HII regions
Used in Eq. 2 to convert [CII]/[NII] to PDR fraction; the abstract favors the ~3 case while the paper also reports the ~9 case.

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Cite this review

Pith. "Pith review of The [NII] 205 $\mu$m line emission from high-z SMGs and QSOs." pith.science (2026). https://pith.science/paper/YHBRRMMR

@misc{pith2026250208984,
  author       = {Pith},
  title        = {Pith review of: The [NII] 205 $\mu$m line emission from high-z SMGs and QSOs},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/YHBRRMMR}},
  note         = {Machine review of arXiv:2502.08984}
}

abstract

We present [NII] 205 $\mu$m fine structure line observations of three submillimeter galaxies (SMGs) and three quasar host galaxies at 4$\lesssim$z$\lesssim$6 using the Institut de radioastronomie millim\'etrique (IRAM) interferometer. The [NII] emission is detected in three sources, and we report detections of the underlying dust continuum emission in all sources. The observed [NII]-to-infrared luminosity ratio spans at least 0.5 dex for our sources. Comparing our estimates with sources detected in the [NII] 205 $\mu$m at similar redshifts shows that the overall [NII]-to-IR luminosity ratio spans over a dex in magnitude from L$_{[NII]}$/L$_{IR}$ ~ 10$^{-4}$ - 10$^{-5}$ and follows the trend of the so-called [NII] fine structure line deficit observed in (ultra)-luminous infrared galaxies in the local Universe. The [CII]-to-[NII] luminosity ratio is >10 for most of our sources, indicating that the bulk of the [CII] 158 $\mu$m line emission (f([CII]$^{PDR}$)>75%) arises from the neutral medium. From our analysis, we do not find significant differences in the [NII] 205 $\mu$m emission and the respective ratios between SMGs and QSOs, suggesting a negligible contribution to the boosting of [NII] 205 $\mu$m emission due to the active galactic nucleus (AGN) photoionization. Future investigations involving other fine structure lines and optical diagnostics will provide further insight into a suite of ionized medium properties and reveal the diversity between AGN and non-AGN environments.

Figures

Figures reproduced from arXiv: 2502.08984 by the authors.

**Figure 1.** Observed [NII] 205 µm spectra of the sources in our sample. The orange histogram represents the 1-D spectra of submillimeter galaxies, while the red histogram represents the spectra of quasar hosts. The best Gaussian + continuum fit is shown in solid blue. The dashed blue line represents the mean dust continuum flux for sources undetected in the [NII] 205 µm emission. The gray bar represents the mean error (RMS) of… view at source ↗

**Figure 2.** The [NII]-to-IR ratio as a function of IR luminosity for [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗

**Figure 3.** The [CII]-to-[NII] ratio as a function of IR luminosity [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗

Discussion (0). Continue with ORCID to comment.

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Works this paper leans on

114 extracted references · 79 canonical work pages

[1]

P., Dudley, C., Fischer, J., et al

Abel, N. P., Dudley, C., Fischer, J., et al. (2009), ApJ, 701, 1147 Álvarez-Márquez, J., Colina, L., Crespo Gómez, A., et al. (2024), A&A, 686, A85

2009
[2]

A., Phillips, M

Baldwin, J. A., Phillips, M. M., & Terlevich, R. (1981), PASP, 93, 5

1981
[3]

J., et al

Beelen, A., Cox, P., Benford, D. J., et al. (2006), ApJ, 642, 694 Beirão, P., Armus, L., Appleton, P. N., et al. (2010), A&A, 518, L60

2006
[4]

(2003), A&A, 409, L47

Bertoldi, F., Cox, P., Neri, R., et al. (2003), A&A, 409, L47

2003
[5]

M., van der Werf, P

Butler, K. M., van der Werf, P. P., Topkaras, T., et al. (2023), ApJ, 944, 134 Béthermin, M., De Breuck, C., Gullberg, B., et al. (2016), A&A, 586, L7 Béthermin, M., Fudamoto, Y ., Ginolfi, M., et al. (2020), A&A, 643, A2

2023
[6]

J., Saxena, A., Bunker, A

Cameron, A. J., Saxena, A., Bunker, A. J., et al. (2023), A&A, 677, A115

2023
[7]

L., Bertoldi, F., Omont, A., et al

Carilli, C. L., Bertoldi, F., Omont, A., et al. (2001), AJ, 122, 1679

2001
[8]

L., Cox, P., Bertoldi, F., et al

Carilli, C. L., Cox, P., Bertoldi, F., et al. (2002), ApJ, 575, 145

2002

Show all 114 references

[10]

L., & Walter, F

Carilli, C. L., & Walter, F. (2013), ARA&A, 51, 105

2013
[11]

(2015), IAUGA, 29, 2247830

Carilli, C., & Walter, F. (2015), IAUGA, 29, 2247830

2015
[12]

L., Lewis, G

Carilli, C. L., Lewis, G. F., Djorgovski, S. G., et al. (2003), Sci, 300, 773

2003
[13]

L., Daddi, E., Riechers, D., et al

Carilli, C. L., Daddi, E., Riechers, D., et al. (2010), ApJ, 714, 1407

2010
[14]

L., Hodge, J., Walter, F., et al

Carilli, C. L., Hodge, J., Walter, F., et al. (2011), ApJL, 739, L33

2011
[15]

L., Pope, A., Scott, D., et al

Chapin, E. L., Pope, A., Scott, D., et al. (2009), MNRAS, 398, 1793

2009
[16]

(2020), ApJ, 898, 33

Cheng, C., Cao, X., Lu, N., et al. (2020), ApJ, 898, 33

2020
[17]

(2023), A&A, 673, L6

Colina, L., Crespo Gómez, A., Álvarez-Márquez, J., et al. (2023), A&A, 673, L6

2023
[18]

Cora, S. A. (2006), MNRAS, 368, 1540

2006
[19]

E., Valentino, F., et al

Cortzen, I., Magdis, G. E., Valentino, F., et al. (2020), A&A, 634, L14

2020
[20]

L., Barger, A

Cowie, L. L., Barger, A. J., Hsu, L.-Y ., et al. (2017), ApJ, 837, 139

2017
[21]

G., et al

Cox, P., Omont, A., Djorgovski, S. G., et al. (2002), A&A, 387, 406

2002
[22]

(2011), ApJ, 740, 63

Cox, P., Krips, M., Neri, R., et al. (2011), ApJ, 740, 63

2011
[23]

Cunningham, D. J. M., Chapman, S. C., Aravena, M., et al. (2020), MNRAS, 494, 4090

2020
[24]

(2009), ApJ, 694, 1517

Daddi, E., Dannerbauer, H., Stern, D., et al. (2009), ApJ, 694, 1517

2009
[25]

A., et al

Dannerbauer, H., Daddi, E., Riechers, D. A., et al. (2009), ApJL, 698, L178 De Looze, I., Cormier, D., Lebouteiller, V ., et al. (2014), A&A, 568, A62

2009
[26]

(2010), MNRAS, 402, 2453

Decarli, R., Falomo, R., Treves, A., et al. (2010), MNRAS, 402, 2453

2010
[27]

(2012), ApJ, 752, 2

Decarli, R., Walter, F., Neri, R., et al. (2012), ApJ, 752, 2

2012
[28]

(2014), ApJL, 782, L17

Decarli, R., Walter, F., Carilli, C., et al. (2014), ApJL, 782, L17

2014
[29]

P., et al

Decarli, R., Walter, F., Venemans, B. P., et al. (2018), ApJ, 854, 97

2018
[30]

(2022), A&A, 662, A60

Decarli, R., Pensabene, A., Venemans, B., et al. (2022), A&A, 662, A60

2022
[31]

(2023), A&A, 673, A157

Decarli, R., Pensabene, A., Diaz-Santos, T., et al. (2023), A&A, 673, A157

2023
[32]

G., Gal, R

Djorgovski, S. G., Gal, R. R., Mahabal, A., et al. (2000), AAS, 197, 116.07

2000
[33]

J., Geach, J

Doherty, M. J., Geach, J. E., Ivison, R. J., et al. (2020), ApJ, 905, 152

2020
[34]

(1999), A&A, 347, 809

Downes, D., Neri, R., Greve, A., et al. (1999), A&A, 347, 809

1999
[35]

(2018), MNRAS, 476, 4383

Dye, S., Furlanetto, C., Dunne, L., et al. (2018), MNRAS, 476, 4383

2018
[36]

A., Gomez, H

Dye, S., Eales, S. A., Gomez, H. L., et al. (2022), MNRAS, 510, 3734 Díaz-Santos, T., Armus, L., Charmandaris, V ., et al. (2017), ApJ, 846, 32

2022
[37]

(2010), PASP, 122, 499

Eales, S., Dunne, L., Clements, D., et al. (2010), PASP, 122, 499

2010
[38]

(2018), MNRAS, 475, 3467

Enia, A., Negrello, M., Gurwell, M., et al. (2018), MNRAS, 475, 3467

2018
[39]

Farrah, D., Lebouteiller, V ., Spoon, H. W. W., et al. (2013), ApJ, 776, 38

2013
[40]

J., Korista, K

Ferland, G. J., Korista, K. T., Verner, D. A., et al. (1998), PASP, 110, 761

1998
[41]

W., Lang, D., et al

Foreman-Mackey, D., Hogg, D. W., Lang, D., et al. (2013), PASP, 125, 306 Graciá-Carpio, J., Sturm, E., Hailey-Dunsheath, S., et al. (2011), ApJL, 728, L7

2013
[42]

K., et al

Harikane, Y ., Ouchi, M., Inoue, A. K., et al. (2020), ApJ, 896, 93

2020
[43]

K., Tamura, Y ., et al

Hashimoto, T., Inoue, A. K., Tamura, Y ., et al. (2019), PASJ, 71, 109

2019
[44]

J., Oesch, P

Herard-Demanche, T., Bouwens, R. J., Oesch, P. A., et al. (2023), MNRAS, sub- mitted [arXiv:2309.04525]

2023 arXiv
[45]

D., Wolfire, M

Herrera-Camus, R., Bolatto, A. D., Wolfire, M. G., et al. (2014), AAS, 223, 117.02

2014
[46]

D., Wolfire, M

Herrera-Camus, R., Bolatto, A. D., Wolfire, M. G., et al. (2015), ApJ, 800, 1

2015
[47]

D., et al

Herrera-Camus, R., Bolatto, A., Smith, J. D., et al. (2016), ApJ, 826, 175

2016
[48]

(2018), ApJ, 861, 95

Herrera-Camus, R., Sturm, E., Graciá-Carpio, J., et al. (2018), ApJ, 861, 95

2018
[49]

A., Carilli, C

Hodge, J. A., Carilli, C. L., Walter, F., et al. (2012), ApJ, 760, 11

2012
[50]

A., Riechers, D., Decarli, R., et al

Hodge, J. A., Riechers, D., Decarli, R., et al. (2015), ApJL, 798, L18

2015
[51]

Y .-Y ., Álvarez-Márquez, J., Coe, D., et al

Hsiao, T. Y .-Y ., Álvarez-Márquez, J., Coe, D., et al. (2024), ApJ, 973, 81

2024
[52]

H., Serjeant, S., Dunlop, J., et al

Hughes, D. H., Serjeant, S., Dunlop, J., et al. (1998), Natur, 394, 241

1998
[53]

(2024), PASJ..tmp,

Ishii, N., Hashimoto, T., Ferkinhoff, C., et al. (2024), PASJ..tmp,

2024
[54]

I., Stasi´nska, G., Meynet, G., et al

Izotov, Y . I., Stasi´nska, G., Meynet, G., et al. (2006), A&A, 448, 955

2006
[55]

(2009), AJ, 138, 305

Jiang, L., Fan, X., Bian, F., et al. (2009), AJ, 138, 305

2009
[56]

D., Fan, X., et al

Jiang, L., McGreer, I. D., Fan, X., et al. (2016), ApJ, 833, 222

2016
[57]

J., et al

Katz, H., Saxena, A., Cameron, A. J., et al. (2023), MNRAS, 518, 592

2023
[58]

P., Aller, L

Keenan, F. P., Aller, L. H., Bell, K. L., et al. (1996), MNRAS, 281, 1073

1996
[59]

J., Dopita, M

Kewley, L. J., Dopita, M. A., Sutherland, R. S., et al. (2001), ApJ, 556, 121

2001
[60]

(2022), A&A, 664, A39

Khusanova, Y ., Bañados, E., Mazzucchelli, C., et al. (2022), A&A, 664, A39

2022
[61]

(2018), A&A, 609, A130

Lagache, G., Cousin, M., & Chatzikos, M. (2018), A&A, 609, A130

2018
[62]

(2022), AAS, 54, 105.08

Lamarche, C., Smith, J.-D., Kreckel, K., et al. (2022), AAS, 54, 105.08

2022
[63]

(2020), ApJ, 900, 131

Li, J., Wang, R., Cox, P., et al. (2020), ApJ, 900, 131

2020
[64]

(2018), ApJ, 864, 38

Lu, N., Cao, T., Díaz-Santos, T., et al. (2018), ApJ, 864, 38

2018
[65]

C., Cormier, D., Hony, S., et al

Madden, S. C., Cormier, D., Hony, S., et al. (2020), A&A, 643, A141

2020
[66]

E., Daddi, E., Elbaz, D., et al

Magdis, G. E., Daddi, E., Elbaz, D., et al. (2011), ApJL, 740, L15

2011
[67]

J., Hollenbach, D., et al

Malhotra, S., Kaufman, M. J., Hollenbach, D., et al. (2001), ApJ, 561, 766

2001
[68]

A., Walter, F., Cicone, C., et al

Meyer, R. A., Walter, F., Cicone, C., et al. (2022), ApJ, 927, 152

2022
[69]

X., et al

Neeleman, M., Kanekar, N., Prochaska, J. X., et al. (2017), Sci, 355, 1285

2017
[70]

X., et al

Neeleman, M., Kanekar, N., Prochaska, J. X., et al. (2019), ApJL, 870, L19

2019
[71]

(2014), A&A, 562, A35

Neri, R., Downes, D., Cox, P., et al. (2014), A&A, 562, A35

2014
[72]

(2019), ApJ, 881, 63

Novak, M., Bañados, E., Decarli, R., et al. (2019), ApJ, 881, 63

2019
[73]

E., Parshley, S

Oberst, T. E., Parshley, S. C., Stacey, G. J., et al. (2006), ApJL, 652, L125

2006
[74]

(2001), A&A, 374, 371 Orsi, Á., Padilla, N., Groves, B., et al

Omont, A., Cox, P., Bertoldi, F., et al. (2001), A&A, 374, 371 Orsi, Á., Padilla, N., Groves, B., et al. (2014), MNRAS, 443, 799

2001
[75]

A., Capak, P

Pavesi, R., Riechers, D. A., Capak, P. L., et al. (2016), ApJ, 832, 151

2016
[76]

A., Sharon, C

Pavesi, R., Riechers, D. A., Sharon, C. E., et al. (2018), ApJ, 861, 43

2018
[77]

A., Faisst, A

Pavesi, R., Riechers, D. A., Faisst, A. L., et al. (2019), ApJ, 882, 168

2019
[78]

(2020), A&A, 637, A84

Pensabene, A., Carniani, S., Perna, M., et al. (2020), A&A, 637, A84

2020
[79]

(2021), A&A, 652, A66

Pensabene, A., Decarli, R., Bañados, E., et al. (2021), A&A, 652, A66

2021
[80]

A., Chapin, E

Perera, T. A., Chapin, E. L., Austermann, J. E., et al. (2008), MNRAS, 391, 1227

2008
[81]

(2004), A&A, 428, L21

Pety, J., Beelen, A., Cox, P., et al. (2004), A&A, 428, L21

2004
[82]

(2006), MNRAS, 370, 1185

Pope, A., Scott, D., Dickinson, M., et al. (2006), MNRAS, 370, 1185

2006
[83]

A., Pavesi, R., Sharon, C

Riechers, D. A., Pavesi, R., Sharon, C. E., et al. (2019), ApJ, 872, 7

2019
[84]

A., Hodge, J

Rybak, M., Zavala, J. A., Hodge, J. A., et al. (2020), ApJL, 889, L11

2020
[85]

K., et al

Salak, D., Hashimoto, T., Inoue, A. K., et al. (2024), ApJ, 962, 1

2024
[86]

L., Shapley, A

Sanders, R. L., Shapley, A. E., Topping, M. W., et al. (2023), ApJ, 955, 54

2023
[87]

(2018), A&A, 611, A22

Schreiber, C., Labbé, I., Glazebrook, K., et al. (2018), A&A, 611, A22

2018
[88]

(2021), A&A, 646, A68

Schreiber, C., Glazebrook, K., Papovich, C., et al. (2021), A&A, 646, A68

2021
[89]

L., et al

Shao, Y ., Wang, R., Carilli, C. L., et al. 2019, ApJ, 876, 99

2019
[90]

M., & Vanden Bout, P

Solomon, P. M., & Vanden Bout, P. A. (2005), ARA&A, 43, 677

2005
[91]

R., McKean, J

Stacey, H. R., McKean, J. P., Robertson, N. C., et al. (2018), MNRAS, 476, 5075

2018
[92]

G., Kovács, A., Arendt, R

Staguhn, J. G., Kovács, A., Arendt, R. G., et al. (2014), ApJ, 790, 77

2014
[94]

M., Egami, E., et al

Sun, F., Helton, J. M., Egami, E., et al. (2024), ApJ, 961, 69

2024
[95]

A., Croxall, K

Sutter, J., Dale, D. A., Croxall, K. V ., et al. (2019), ApJ, 886, 60

2019
[96]

A., Sandstrom, K., et al

Sutter, J., Dale, D. A., Sandstrom, K., et al. (2021), MNRAS, 503, 911

2021
[97]

ichi ., Iono, D., Hatsukade, B., et al

Tadaki, K.-. ichi ., Iono, D., Hatsukade, B., et al. (2019), ApJ, 876, 1

2019
[98]

ichi ., Tsujita, A., Tamura, Y ., et al

Tadaki, K.-. ichi ., Tsujita, A., Tamura, Y ., et al. (2022), PASJ, 74, L9

2022
[99]

(2014), A&A, 569, A98

Tan, Q., Daddi, E., Magdis, G., et al. (2014), A&A, 569, A98

2014
[100]

(2022), A&A, 665, A107

Tripodi, R., Feruglio, C., Fiore, F., et al. (2022), A&A, 665, A107

2022
[101]

(2024), A&A, 689, A220

Tripodi, R., Feruglio, C., Fiore, F., et al. (2024), A&A, 689, A220

2024
[102]

E., Daddi, E., et al

Valentino, F., Magdis, G. E., Daddi, E., et al. (2018), ApJ, 869, 27

2018
[103]

Veilleux, S., & Osterbrock, D. E. (1987), ApJS, 63, 295

1987
[104]

P., Walter, F., Neeleman, M., et al

Venemans, B. P., Walter, F., Neeleman, M., et al. (2020), ApJ, 904, 130

2020
[105]

(2018), ApJ, 856, 174

Vishwas, A., Ferkinhoff, C., Nikola, T., et al. (2018), ApJ, 856, 174

2018
[106]

E., Greve, T

Vizgan, D., Heintz, K. E., Greve, T. R., et al. (2022), ApJL, 939, L1

2022
[107]

L., Wilner, D

Wagg, J., Carilli, C. L., Wilner, D. J., et al. (2010), A&A, 519, L1

2010
[108]

A., et al

Walter, F., Weiß, A., Riechers, D. A., et al. (2009), ApJL, 691, L1

2009
[109]

(2012), Natur, 486, 233

Walter, F., Decarli, R., Carilli, C., et al. (2012), Natur, 486, 233

2012
[110]

(2022), ApJ, 927, 21

Walter, F., Neeleman, M., Decarli, R., et al. (2022), ApJ, 927, 21

2022
[111]

L., Wagg, J., et al

Wang, R., Carilli, C. L., Wagg, J., et al. (2008), ApJ, 687, 848

2008
[112]

L., et al

Wang, R., Wagg, J., Carilli, C. L., et al. (2013), ApJ, 773, 44

2013
[113]

(2023), A&A, 680, A95

Yang, C., Omont, A., Martín, S., et al. (2023), A&A, 680, A95

2023
[114]

A., Castellano, M., Akins, H

Zavala, J. A., Castellano, M., Akins, H. B., et al. (2024), NatAs.tmp..258Z

2024
[115]

K., et al

Zhao, Y ., Lu, N., Xu, C. K., et al. (2013), ApJL, 765, L13

2013
[116]

K., et al

Zhao, Y ., Lu, N., Xu, C. K., et al. (2016), ApJ, 819, 69 Article number, page 8 of 13 Kolupuri et al: The [NII] 205µm line emission from high-z SMGs and QSOs Appendix A: Line integrated and continuum maps We present the [NII] 205µm integrated emission line and continuum maps ...

2016

Pith tools

Reviewed August 7, 2026 · model on record in the stance chip above.

[1] [1]

P., Dudley, C., Fischer, J., et al

Abel, N. P., Dudley, C., Fischer, J., et al. (2009), ApJ, 701, 1147 Álvarez-Márquez, J., Colina, L., Crespo Gómez, A., et al. (2024), A&A, 686, A85

2009

[2] [2]

A., Phillips, M

Baldwin, J. A., Phillips, M. M., & Terlevich, R. (1981), PASP, 93, 5

1981

[3] [3]

J., et al

Beelen, A., Cox, P., Benford, D. J., et al. (2006), ApJ, 642, 694 Beirão, P., Armus, L., Appleton, P. N., et al. (2010), A&A, 518, L60

2006

[4] [4]

(2003), A&A, 409, L47

Bertoldi, F., Cox, P., Neri, R., et al. (2003), A&A, 409, L47

2003

[5] [5]

M., van der Werf, P

Butler, K. M., van der Werf, P. P., Topkaras, T., et al. (2023), ApJ, 944, 134 Béthermin, M., De Breuck, C., Gullberg, B., et al. (2016), A&A, 586, L7 Béthermin, M., Fudamoto, Y ., Ginolfi, M., et al. (2020), A&A, 643, A2

2023

[6] [6]

J., Saxena, A., Bunker, A

Cameron, A. J., Saxena, A., Bunker, A. J., et al. (2023), A&A, 677, A115

2023

[7] [7]

L., Bertoldi, F., Omont, A., et al

Carilli, C. L., Bertoldi, F., Omont, A., et al. (2001), AJ, 122, 1679

2001

[8] [8]

L., Cox, P., Bertoldi, F., et al

Carilli, C. L., Cox, P., Bertoldi, F., et al. (2002), ApJ, 575, 145

2002