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REVIEW 3 major objections 5 minor 133 references

The paper shows that a four-stage cleaning pipeline suppresses atmospheric 1/f noise by roughly four orders of magnitude in EoR-Spec timestreams, making the [C II]+CO line-intensity power spectrum detectable on small scales with one module

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2026-08-01 09:54 UTC pith:J3YREIKN

load-bearing objection A genuinely useful end-to-end simulation for EoR-Spec, but the headline detection threshold ignores the pipeline's own transfer function. the 3 major comments →

arxiv 2607.20404 v1 pith:J3YREIKN submitted 2026-07-22 astro-ph.GA astro-ph.IM

Spectral Data-cube Cleaning for CCAT Deep Spectroscopic Survey. I. Effect of correlated noise and filtering on the power spectrum

A. Dev , C. Karoumpis , Y. Okada , K. Basu , F. Bertoldi , D. Chung , J. Clarke , R. Freundt
show 3 more authors
T. Nikola T. Oak D. Riechers
This is my paper
classification astro-ph.GA astro-ph.IM
keywords line-intensity mapping[C II] emissionatmospheric 1/f noisepower spectrumfilter-and-bin pipelinetransfer functionEoR-Specsubmillimeter survey
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper asks whether atmospheric 1/f noise will stop the EoR-Spec spectrometer from measuring the cosmic [C II]+CO line-intensity power spectrum. Using end-to-end mock observations of the 330–370 GHz band, it shows that a four-stage filter-and-bin pipeline reduces low-frequency atmospheric noise by roughly four orders of magnitude and leaves detector timestreams close to white. A single EoR-Spec module at 50% observing efficiency should then detect the combined line power on shot-noise-dominated scales (wavenumber k > 0.1 Mpc^-1), and two modules at full efficiency should detect it across all probed scales (0.02–2 Mpc^-1). The same filtering, however, removes most large-scale clustering modes—the transfer function falls below 20% at k < 0.1 Mpc^-1—so the paper establishes that this pipeline is viable for the shot-noise regime but not yet for clustering measurements.

Core claim

The central result is that the filter-and-bin approach recovers the small-scale [C II]+CO power spectrum while suppressing atmospheric 1/f noise by about four orders of magnitude at temporal frequencies below 0.1 Hz. After polynomial de-trending, scan-synchronous correction, common-mode regression, and removal of the first three principal components, residual detector noise is nearly white and measured power-spectrum sensitivity tracks the white-noise forecast. In the nominal scenario (one module, 50% observing efficiency) the survey detects the combined signal for k > 0.1 Mpc^-1, the shot-noise regime set by discrete emitting galaxies; in the ideal scenario (two modules, full efficiency) it

What carries the argument

The load-bearing object is the Filter-and-Bin (F&B) pipeline. Each five-minute detector timestream is down-sampled and fit with a third-order polynomial to remove slow drifts; an elevation/azimuth model removes scan-synchronous pickup; a common-mode template across detectors in each spectral bin is regressed out; and the first few principal components of the detector covariance matrix are subtracted to remove residual correlated noise. The whitened timestreams are then inverse-variance weighted and binned into per-spectral-bin maps, which are co-added across the Fabry-Pérot steps. The transfer function is estimated by running identical signal-plus-noise and noise-only realizations through th

Load-bearing premise

The results assume the simulated atmosphere—a moving slab of Kolmogorov turbulence with the chosen wind speeds and length scales—behaves like the real sky noise at the telescope site; if it does not, the measured 1/f suppression and transfer function will not transfer to real data.

What would settle it

During commissioning, record blank-sky detector timestreams at the site and compute the average power spectral density and detector-to-detector correlation. If the low-frequency slope differs strongly from about f^-3 or the dominant noise is not shared as a common mode across the focal plane, the pipeline will not achieve the reported four-orders-of-magnitude suppression and the k-dependent transfer function will not match the simulations.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • With the filter-and-bin pipeline, a single EoR-Spec module at 50% observing efficiency can already detect the combined [C II]+CO power spectrum on shot-noise-dominated scales (k > 0.1 Mpc^-1).
  • Deploying two modules at 100% observing efficiency extends detection across all probed scales, 0.02 Mpc^-1 < k < 2 Mpc^-1.
  • Modes with k > 0.5 Mpc^-1 survive with at least 80% of their power, so shot-noise measurements can be corrected with a near-unity transfer function.
  • Modes with k < 0.1 Mpc^-1 keep less than 20% of their power, so large-scale clustering measurements require a different map-making approach than filter-and-bin.
  • Removing a fourth PCA component does not meaningfully improve noise suppression but does increase signal loss, making three the practical filter choice for this dataset.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The optimal number of PCA components is dataset-dependent, so the paper's signal-plus-noise / noise-only comparison could be reused on real commissioning timestreams to decide when to stop filtering.
  • Because the simulations omit gain fluctuations, ground pickup, glitches, and continuum foregrounds, the four-orders-of-magnitude suppression is plausibly an upper bound; blank-sky commissioning data is the direct test.
  • If the real atmosphere is multi-layered or departs from Kolmogorov statistics, both the suppression factor and the scale where the transfer function drops would shift, making site-specific noise measurements a cheap way to de-risk the survey.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. The paper presents end-to-end TOAST-based simulations of EoR-Spec observations for the CCAT Deep Spectroscopic Survey, covering 330–370 GHz with 5 of 15 FPI steps and ~500 detectors per spectral bin. The authors apply a Filter-and-Bin pipeline (polynomial de-trending, Az-El correction, common-mode regression, PCA filtering) to mock timestreams containing [CII]+CO signal, atmospheric 1/f noise, and white noise. They characterize the noise PSD at each pipeline stage, compute power-spectrum sensitivities for nominal (1 module, 50% efficiency) and ideal (2 modules, 100% efficiency) survey configurations, and estimate a pipeline transfer function. The central claims are that the pipeline suppresses atmospheric 1/f noise by ~4 orders of magnitude at low temporal frequencies, that the nominal survey detects the combined [CII]+CO power spectrum on scales k>0.1 Mpc^-1, that the ideal configuration detects all probed scales, and that the transfer function exceeds 80% at k≳0.5 Mpc^-1 while falling below 20% at k≲0.1 Mpc^-1.

Significance. This is a useful and timely methods paper for LIM with EoR-Spec. Its strengths are the realistic end-to-end simulation framework (including FPI spectral response, scan strategy, and atmospheric turbulence), the explicit transfer-function estimation via signal+noise-minus-noise simulations, and the honest listing of several simplifying assumptions in Sect. 5. If the sensitivity comparison is corrected, the paper provides a well-characterized baseline for early DSS data reduction and quantifies the expected large-scale signal loss due to filtering. However, the headline detection claim is currently undercut by an internal inconsistency between the sensitivity forecast and the paper's own transfer function, so the quantitative conclusions need revision.

major comments (3)
  1. [Sect. 4.2, Fig. 7, abstract] The detection claim compares σΔ2(k) from Eq. (18), which is computed from the filtered signal+noise cube, against the solid black curve representing the intrinsic input PS before beam/spectral response and before pipeline filtering. The actual observed signal after the pipeline is T(k)·Δ2_input(k), and Fig. 8 shows T<20% at k≲0.1 and T<80% for k<0.5. Thus the S/N for 0.1<k<0.5 is overestimated by at least 1/T, up to ~5x at k~0.1. Moreover, the abstract's 'shot-noise-dominated scales (k>0.1 Mpc^-1)' contradicts the paper's own statement (Sect. 5, finding 3) that the shot-noise regime is k>0.5 Mpc^-1, where T>80%. Please re-derive the detection threshold by plotting σΔ2(k) against T(k)·Δ2_input(k) (or at least the beam/spectral-convolved input) and revise the abstract, Sect. 4.2, and Sect. 5 accordingly.
  2. [Sect. 4.3, Fig. 8] The transfer function is estimated from (apparently) a single realization via Precovered = Psignal+noise − Pnoise. No error bars are shown on T(k). At large scales (k<0.2 Mpc^-1), the number of Fourier modes N_m is small and the subtraction of two noisy power spectra will produce large scatter. The specific claims '>80% at k⪆0.5' and '<20% at k⪅0.1' are not yet quantified with uncertainties. Please provide bootstrap or multiple-realization error bars and state how many realizations were used.
  3. [Sect. 2.3.2, Table D.1, Sect. 5] The quantitative conclusions — the ~4-orders-of-magnitude 1/f suppression and the TF shape — are derived from a single atmospheric realization drawn from a 3D Kolmogorov slab with the specific parameters of Table D.1 and a single gain rescale. If the real Cerro Chajnantor atmosphere has different statistics (e.g., multi-layer screens, non-Kolmogorov turbulence, variable wind), the reported suppression and TF could change. Section 5 lists other limitations but does not mention this atmospheric-model dependence. Please add a sensitivity test varying key atmospheric parameters (injection scale, wind speed, gain) or, at minimum, state explicitly that all quantitative claims are conditioned on this model.
minor comments (5)
  1. [Sect. 4.2 vs 4.3] The 'input signal' is used inconsistently: Fig. 7's black curve is the input PS 'before applying the instrumental beam and spectral response,' while Eq. (20) defines P_signal(k) as including the beam and spectral response. Please define distinct symbols (e.g., P_intrinsic vs P_signal) and use them consistently.
  2. [References] The Welch (1967) reference lists 'IEEE Transactions on AgriFood Electronics'; this should be 'IEEE Transactions on Audio and Electroacoustics'. Also, Appendix C contains a typo: 'Simons Ovservatory'.
  3. [Fig. 6 caption] The caption reads 'Fit: = 2.97, fknee = 2.23 Hz'; the spectral index symbol α is missing.
  4. [Sect. 3.4] The notation for the number of PCA components is inconsistent (ncomp, n_comp, n_comp). Please unify.
  5. [Sect. 4.1] The PSD fit reported (α=-2.97, fknee=2.23 Hz) is for a single observation; state whether this is representative across all observations and spectral bins.

Circularity Check

0 steps flagged

No circular derivation: the pipeline is validated by injection-recovery with a separate noise-only transfer function; the k>0.1 detection claim has a comparison-basis inconsistency that is a correctness issue, not a circularity.

full rationale

The derivation chain is not circular. A fiducial [CII]+CO signal from K22/K24 is injected into simulated TOD, processed through the F&B pipeline, and the recovered power is compared with the input via a transfer function T(k)=P_recovered/P_signal computed from independent noise-only simulations with identical noise realizations. This is the standard injection-recovery validation loop: the signal is not re-fit from the output, and the noise-only subtraction is a separate control. The choice n_comp=3 is a data-cleaning decision based on flattening the noise PSD and is explicitly tested against 2 and 4 components; it is not a parameter fit to the claimed detection. The self-citations to K22 and K24 are load-bearing only as stated, externally anchored simulation inputs (TNG300, V15 SFR-L[CII], CO SLED), and the detection claim is explicitly conditional on those fiducial models; no target result is imported from those papers as a black-box uniqueness or ansatz. The real problem in the skeptical note is an internal comparison inconsistency: Fig. 7 plots sigma_Delta2(k) from the filtered, beam- and spectral-convolved cube against the input PS 'before applying the instrumental beam and spectral response', while Sect. 4.3 defines the TF with the beam- and spectral-convolved signal and reports T(k)<20% at k<0.1 and >80% only at k>0.5. Thus the abstract's 'k>0.1' detection threshold is not supported by the paper's own transfer function. This is a significant scientific/interpretation error, but it is not circular: no equation or fitted parameter reduces to its own input by construction. The paper is otherwise self-contained and its pipeline conclusions are reproducible from the stated simulation ingredients.

Axiom & Free-Parameter Ledger

3 free parameters · 5 axioms · 0 invented entities

The central claims rest on simulated atmospheric and instrument models, not on new physics. The main hand-tuned inputs are the atmospheric scaling gains and the number of PCA components; the former sets the noise amplitude, the latter is a data-driven cleaning choice. No invented entities.

free parameters (3)
  • PCA components removed (n_comp) = 3 (nominal; cases 2 and 4 tested)
    Chosen from the mock dataset to whiten the residual noise spectrum; not determined a priori (Sect. 3.4).
  • Polynomial order for de-trending = 3
    Ad hoc choice for low-frequency drift removal (Sect. 3.1).
  • Atmospheric TOD gain rescale = 1e-4 (coarse), 4e-5 (fine)
    Hand-tuned scaling factors in Table D.1 to set atmospheric noise amplitude.
axioms (5)
  • domain assumption The atmosphere is a 3D Kolmogorov turbulent slab with parameters from Table D.1.
    Entered in Sect 2.3.2; if the real atmosphere differs (e.g., two-layer, non-Kolmogorov), the measured filter performance and TF may not transfer.
  • domain assumption After PCA filtering, the residual noise is uncorrelated and Gaussian, so the map-making noise covariance is diagonal (Eq. 13).
    Sect 3.5; underpins the F&B binning and the sensitivity estimates.
  • domain assumption The input [CII]+CO signal maps from K22/K24 (V15 fiducial) are representative of the true sky at z~4.45.
    Sect 2.3.1; detection forecasts are conditional on this model.
  • domain assumption The ideal FPI Lorentzian transmission model (Eq. 2, Appendix A) describes the real EoR-Spec spectral response.
    Sect 2.1; non-ideal bandpasses and cross-talk are excluded and may introduce mode mixing.
  • standard math Signal and noise are uncorrelated in the transfer-function estimation (P_signal+noise - P_noise).
    Sect 4.3, Eq. (20); holds because noise realisations are independent of the signal.

pith-pipeline@v1.3.0-alltime-deepseek · 27578 in / 11192 out tokens · 90222 ms · 2026-08-01T09:54:54.170503+00:00 · methodology

0 comments
read the original abstract

The Epoch of Reionization Spectrometer (EoR-Spec) on the Fred Young Submillimeter Telescope (FYST) will conduct the CCAT Deep Spectroscopic Survey (DSS) to perform line-intensity mapping of redshifted [C II] emission. Atmospheric $1/f$ noise and instrumental systematics affect power-spectrum recovery. We present realistic end-to-end simulations to quantify these effects and evaluate a Filter-and-Bin (F&B) pipeline. The simulated observations include instrument response, astrophysical emission, atmospheric noise, and observing strategy. The pipeline suppresses atmospheric $1/f$ noise by about four orders of magnitude at low temporal frequencies while leaving only minor residual correlated noise. For a single EoR-Spec module operating at 50% observing efficiency, the DSS is expected to detect the combined [C II] + CO power spectrum on shot-noise-dominated scales ($k > 0.1\,\mathrm{Mpc}^{-1}$). With two modules operating at full efficiency, detections are achievable over all targeted spatial scales. The transfer function exceeds 80% at $k \gtrsim 0.5\,\mathrm{Mpc}^{-1}$ but falls below 20% at $k \lesssim 0.1\,\mathrm{Mpc}^{-1}$, indicating significant suppression of large-scale modes. These results demonstrate that the F&B pipeline is effective for recovering the shot-noise regime, while improved map-making techniques will be required for accurate large-scale clustering measurements.

Figures

Figures reproduced from arXiv: 2607.20404 by A. Dev, C. Karoumpis, D. Chung, D. Riechers, F. Bertoldi, J. Clarke, K. Basu, R. Freundt, T. Nikola, T. Oak, Y. Okada.

Figure 1
Figure 1. Figure 1: Transmittance (T) showing the ideal spectral transmission profile, without accounting for losses and absorptance, for the 15 discrete FPI steps of EoR-Spec, is shown for normal incidence (θ = 0 ◦ ). Shaded regions indicate the spectral coverage at each FPI step due to the range of incident rays. Vertical dashed lines show the spectral binning for EoR-Spec (see Sect. 2.2). The low-frequency (LF) and high-fr… view at source ↗
Figure 2
Figure 2. Figure 2: EoR-Spec focal plane array layout projected onto the boresight coordinate plane. The cavity gap corresponds to the 5th FPI step, tuned to a resonance frequency of 235 GHz, associated with the second-order resonance at normal incidence. The layout shows two low-frequency ar￾rays (LFA: red – yellow), operating at the second-order resonance, and a single high-frequency array (HFA: blue – purple), targeting th… view at source ↗
Figure 3
Figure 3. Figure 3: A 2◦ × 2 ◦ cutout of the combined [C ii] and CO line-intensity mock map at the 365 GHz spectral bin (z[C ii] ∼ 4.2), based on K22 and K24. The map is convolved with the instrument beam and spec￾tral response, and projected onto the E-COSMOS field using the CAR projection. speed, producing realistic time-variable correlated patterns in the TOD that depend on detector angular separation, scan speed and wind … view at source ↗
Figure 4
Figure 4. Figure 4: Visualisation of TOD for simulated detectors for a single FPI step during ∼ 5 minutes of observation after successive stages of data cleaning. Panel (a) shows the TOD after polynomial de-trending, which removes the global drifts and leaves variations dominated by the telescope motion. Panel (b) displays the data after correcting for the telescope Az-El motion, after which the TOD is dominated by common mod… view at source ↗
Figure 5
Figure 5. Figure 5: A 2◦ × 2 ◦ cutout region of the final filtered and binned map for the 365 GHz spectral bin, obtained after co-adding the FPI steps contributing to this bin. The resulting map is dominated by white noise. The cutout region corresponds to the green-dashed region in Fig. C.2. presents the resulting co-added maps per spectral bin produced using this pipeline. We selected a 2◦ × 2 ◦ sub-region within each co-ad… view at source ↗
Figure 7
Figure 7. Figure 7: Spherically averaged and normalised power spectra sensitivi￾ties for the 330 − 370 GHz band of the EoR-Spec instrument at an average redshift of ⟨z⟩[C ii] = 4.45. The power spectra were calculated over a 4 deg2 survey area and spherically averaged with bins with ∆k = 0.12 Mpc−1 . Normalised power spectrum (∆ 2 (k)) for the input line-intensity signal with [C II] and CO line transitions is shown in solid bl… view at source ↗
Figure 8
Figure 8. Figure 8: Pipeline transfer function T(k) for the three cases of PCA-filter with two (Case I in orange), three (Case II in green) and four (case III in dashed magenta) leading principal components subtracted respectively, after processing the data with polynomial de-trending, Az-El correction and CM regression [PITH_FULL_IMAGE:figures/full_fig_p011_8.png] view at source ↗

discussion (0)

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Reference graph

Works this paper leans on

133 extracted references · 2 canonical work pages

  1. [1]

    2014 , month = jan, volume =

    Starlink Cookbook , title =. 2014 , month = jan, volume =

    2014

  2. [2]

    Pearson, Karl , journal =. LIII. On Lines and Planes of Closest Fit to Systems of Points in Space , year =. doi:10.1080/14786440109462720 , groups =

    doi:10.1080/14786440109462720

  3. [3]

    Analysis of a Complex of Statistical Variables into Principal Components , year =

    Hotelling, Harold , journal =. Analysis of a Complex of Statistical Variables into Principal Components , year =. doi:10.1037/h0071325 , groups =

    doi:10.1037/h0071325

  4. [4]

    Principal Component Analysis , year =

    Jolliffe, Ian , editor =. Principal Component Analysis , year =. International Encyclopedia of Statistical Science , doi =

  5. [5]

    2011 , month = jan, number =

    , title =. 2011 , month = jan, number =. arXiv , doi =:1011.0691 , groups =

    Pith/arXiv arXiv 2011

  6. [6]

    2013 , month = apr, number =

    , title =. 2013 , month = apr, number =. arXiv , doi =:1301.3652 , groups =

    Pith/arXiv arXiv 2013

  7. [7]

    1997 , month = may, number =

    , title =. 1997 , month = may, number =. arXiv , doi =:astro-ph/9611130 , groups =

    Pith/arXiv arXiv 1997

  8. [8]

    2001 , month = jun, pages =

    , title =. 2001 , month = jun, pages =. arXiv , doi =:astro-ph/0101252 , groups =

    Pith/arXiv arXiv 2001

  9. [9]

    2013 , month = jan, number =

    , title =. 2013 , month = jan, number =. arXiv , doi =:1208.0050 , groups =

    Pith/arXiv arXiv 2013

  10. [10]

    2020 , month = dec, number =

    , title =. 2020 , month = dec, number =. arXiv , doi =:2007.07288 , groups =

    Pith/arXiv arXiv 2020

  11. [11]

    2025 , month = nov, number =

    , title =. 2025 , month = nov, number =. arXiv , doi =:2503.14451 , groups =

    Pith/arXiv arXiv 2025

  12. [12]

    2014 , month = nov, pages =

    , title =. 2014 , month = nov, pages =. arXiv , doi =:1303.5063 , groups =

    Pith/arXiv arXiv 2014

  13. [13]

    2016 , month = sep, pages =

    , title =. 2016 , month = sep, pages =. arXiv , doi =:1502.01585 , groups =

    Pith/arXiv arXiv 2016

  14. [14]

    1961 , month = jan, number =

    Physics Today , title =. 1961 , month = jan, number =. doi:10.1063/1.3057286 , groups =

    work page doi:10.1063/1.3057286 1961

  15. [15]

    1941 , month = jan, pages =

    Akademiia Nauk SSSR Doklady , title =. 1941 , month = jan, pages =

    1941

  16. [16]

    and Karoumpis, C

    Clarke, J. and Karoumpis, C. and Riechers, D. and Magnelli, B. and Okada, Y. and Dev, A. and Nikola, T. and Bertoldi, F. , journal =. [CII] luminosity models and large-scale image cubes based on COSMOS 2020 and ALPINE-ALMA [CII] data back to the epoch of reionisation , year =. arXiv , doi =:2404.05352 , groups =

    Pith/arXiv arXiv 2020

  17. [17]

    and Ade, P

    Errard, J. and Ade, P. A. R. and Akiba, Y. and Arnold, K. and Atlas, M. and Baccigalupi, C. and Barron, D. and Boettger, D. and Borrill, J. and Chapman, S. and Chinone, Y. and Cukierman, A. and Delabrouille, J. and Dobbs, M. and Ducout, A. and Elleflot, T. and Fabbian, G. and Feng, C. and Feeney, S. and Gilbert, A. and Goeckner-Wald, N. and Halverson, N. ...

    Pith/arXiv arXiv

  18. [18]

    Journal of Climate , title =

    Gelaro, Ronald and McCarty, Will and Su. Journal of Climate , title =. 2017 , month = jul, number =. doi:10.1175/JCLI-D-16-0758.1 , groups =

    doi:10.1175/jcli-d-16-0758.1 2017

  19. [19]

    ascl , author =:2307.022 , groups =

    TOAST: Time Ordered Astrophysics Scalable Tools , year =. ascl , author =:2307.022 , groups =

  20. [20]

    and Horton, Paul and Lee, Dennis and Mauskopf, Philip and Novak, Giles and Rodr

    Ma, Zhiyuan and McCrackan, Michael and DeNigris, Nat and Souccar, Kamal and Wilson, Grant and Golec, Joseph E. and Horton, Paul and Lee, Dennis and Mauskopf, Philip and Novak, Giles and Rodr. American Astronomical Society Meeting Abstracts \#241 , title =. 2023 , month = jan, pages =

    2023

  21. [21]

    and Ashdown, M

    Natoli, P. and Ashdown, M. and Banerji, R. and Borrill, J. and Buzzelli, A. and de Gasperis, G. and Delabrouille, J. and Hivon, E. and Molinari, D. and Patanchon, G. and Polastri, L. and Tomasi, M. and Bouchet, F. R. and Henrot-Versill. , title =. 2018 , month = apr, number =. arXiv , doi =:1707.04224 , groups =

    Pith/arXiv arXiv 2018

  22. [22]

    , journal =

    Puglisi, Giuseppe and Keskitalo, Reijo and Kisner, Ted and Borrill, Julian D. , journal =. Simulating Calibration and Beam Systematics for a Future CMB Space Mission with the TOAST Package , year =. arXiv , doi =:2106.06005 , groups =

    Pith/arXiv arXiv

  23. [23]

    and Gudmundsson, Jon E

    Dachlythra, Nadia and Duivenvoorden, Adriaan J. and Gudmundsson, Jon E. and Hasselfield, Matthew and Coppi, Gabriele and Adler, Alexandre E. and Alonso, David and Azzoni, Susanna and Chesmore, Grace E. and Fabbian, Giulio and Ganga, Ken and Gerras, Remington G. and Jaffe, Andrew H. and Johnson, Bradley R. and Keating, Brian and Keskitalo, Reijo and Kisner...

    Pith/arXiv arXiv

  24. [24]

    , title =

    Pillepich, Annalisa and Springel, Volker and Nelson, Dylan and Genel, Shy and Naiman, Jill and Pakmor, R. , title =. 2018 , month = jan, number =. arXiv , doi =:1703.02970 , groups =

    Pith/arXiv arXiv 2018

  25. [25]

    The star formation activity of IllustrisTNG galaxies: main sequence, UVJ diagram, quenched fractions, and systematics , year =

    Donnari, Martina and Pillepich, Annalisa and Nelson, Dylan and Vogelsberger, Mark and Genel, Shy and Weinberger, Rainer and Marinacci, Federico and Springel, Volker and Hernquist, Lars , journal =. The star formation activity of IllustrisTNG galaxies: main sequence, UVJ diagram, quenched fractions, and systematics , year =. arXiv , doi =:1812.07584 , groups =

    Pith/arXiv arXiv

  26. [26]

    and Breysse, Patrick C

    Chung, Dongwoo T. and Breysse, Patrick C. and Cleary, Kieran A. and Ihle, H. , title =. 2022 , month = jul, number =. arXiv , doi =:2111.05931 , groups =

    Pith/arXiv arXiv 2022

  27. [27]

    Chung, D. T. and Breysse, P. C. and Cleary, K. A. and Dunne, D. A. and Lunde, J. G. S. and Padmanabhan, H. and Stutzer, N.-O. and Tolgay, D. and Bond, J. R. and Church, S. E. and Eriksen, H. K. and Gaier, T. and Gundersen, J. O. and Harper, S. E. and Harris, A. I. and Hobbs, R. and Ihle, H. T. and Kim, J. and Lamb, J. W. and Lawrence, C. R. and Murray, N....

    Pith/arXiv arXiv 2024

  28. [28]

    , title =

    B. , title =. 2022 , month = nov, pages =. arXiv , doi =:2204.12827 , groups =

    Pith/arXiv arXiv 2022

  29. [29]

    Ihle, H. T. and Bersanelli, M. and Franceschet, C. and Gjerl. , title =. 2023 , month = jul, pages =. arXiv , doi =:2011.06650 , groups =

    Pith/arXiv arXiv 2023

  30. [30]

    and Grainge, Keith and Harper, Stuart and Wang, Jingying , journal =

    Li, Yichao and Santos, Mario G. and Grainge, Keith and Harper, Stuart and Wang, Jingying , journal =. H I intensity mapping with MeerKAT: 1/f noise analysis , year =. arXiv , doi =:2007.01767 , groups =

    Pith/arXiv arXiv 2007

  31. [31]

    and Ponthieu, N

    Van Cuyck, M. and Ponthieu, N. and Lagache, G. and Beelen, A. and B. , title =. 2023 , issn =. arXiv , doi =:2306.01568 , groups =

    Pith/arXiv arXiv 2023

  32. [32]

    Ashdown, M. A. J. and Baccigalupi, C. and Balbi, A. and Bartlett, J. G. and Borrill, J. and Cantalupo, C. and de Gasperis, G. and G. , title =. 2007 , month = aug, number =. arXiv , doi =:astro-ph/0702483 , groups =

    Pith/arXiv arXiv 2007

  33. [33]

    2018 , month = jul, pages =

    Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy IX , title =. 2018 , month = jul, pages =. arXiv , doi =:1807.00058 , groups =

    Pith/arXiv arXiv 2018

  34. [34]

    Cosmic Star-Formation History , year =

    Madau, Piero and Dickinson, Mark , journal =. Cosmic Star-Formation History , year =. arXiv , doi =:1403.0007 , groups =

    Pith/arXiv arXiv

  35. [35]

    Gruppioni, C. and B. , title =. 2020 , month = nov, pages =. arXiv , doi =:2006.04974 , groups =

    Pith/arXiv arXiv 2020

  36. [36]

    , title =

    Bouwens, Rychard and Gonz. , title =. 2020 , month = oct, number =. arXiv , doi =:2009.10727 , groups =

    Pith/arXiv arXiv 2020

  37. [37]

    and Dunlop, J

    Bourne, N. and Dunlop, J. S. and Merlin, E. and Parsa, S. and Schreiber, C. and Castellano, M. and Conselice, C. J. and Coppin, K. E. K. and Farrah, D. and Fontana, A. and Geach, J. E. and Halpern, M. and Knudsen, K. K. and Micha. , title =. 2017 , month = may, number =. arXiv , doi =:1607.04283 , groups =

    Pith/arXiv arXiv 2017

  38. [38]

    Algera, Hiddo S. B. and Inami, Hanae and Oesch, Pascal A. and Sommovigo, Laura and Bouwens, Rychard J. and Topping, Michael W. and Schouws, Sander and Stefanon, Mauro and Stark, Daniel P. and Aravena, Manuel and Barrufet, Laia and da Cunha, Elisabete and Dayal, Pratika and Endsley, Ryan and Ferrara, Andrea and Fudamoto, Yoshinobu and Gonzalez, Valentino a...

    Pith/arXiv arXiv

  39. [39]

    and Narayanan, Desika and Cooray, Asantha , journal =

    Casey, Caitlin M. and Narayanan, Desika and Cooray, Asantha , journal =. Dusty star-forming galaxies at high redshift , year =. arXiv , doi =:1402.1456 , groups =

    Pith/arXiv arXiv

  40. [40]

    Zavala, J. A. and Casey, C. M. and Manning, S. M. and Aravena, M. and Bethermin, M. and Caputi, K. I. and Clements, D. L. and Cunha, E. da and Drew, P. and Finkelstein, S. L. and Fujimoto, S. and Hayward, C. and Hodge, J. and Kartaltepe, J. S. and Knudsen, K. and Koekemoer, A. M. and Long, A. S. and Magdis, G. E. and Man, A. W. S. and Popping, G. and Sand...

    Pith/arXiv arXiv

  41. [41]

    and Lidz, Adam and Bock, Jamie and Bradford, Charles M

    Kovetz, Ely and Breysse, Patrick C. and Lidz, Adam and Bock, Jamie and Bradford, Charles M. and Chang, Tzu-Ching and Foreman, Simon and Padmanabhan, Hamsa and Pullen, Anthony and Riechers, Dominik and Silva, Marta B. and Switzer, Eric , journal =. Astrophysics and Cosmology with Line-Intensity Mapping , year =. arXiv , doi =:1903.04496 , groups =

    Pith/arXiv arXiv 1903

  42. [42]

    and Viero, Marco P

    Kovetz, Ely D. and Viero, Marco P. and Lidz, Adam and Newburgh, Laura and Rahman, Mubdi and Switzer, Eric and Kamionkowski, Marc and Aguirre, James and Alvarez, Marcelo and Bock, James and Bond, J. Richard and Bower, Goeffry and Bradford, C. Matt and Breysse, Patrick C. and Bull, Philip and Chang, Tzu-Ching and Cheng, Yun-Ting and Chung, Dongwoo and Clear...

    Pith/arXiv arXiv 2017

  43. [43]

    Astrophysics & cosmology from line intensity mapping vs galaxy surveys , year =

    Schaan, Emmanuel and White, Martin , journal =. Astrophysics & cosmology from line intensity mapping vs galaxy surveys , year =. arXiv , doi =:2103.01971 , groups =

    Pith/arXiv arXiv

  44. [44]

    Line-Intensity Mapping , year =

    Chang, Tzu-Ching and Lidz, Adam , journal =. Line-Intensity Mapping , year =. arXiv , doi =:2602.03011 , groups =

    arXiv

  45. [45]

    , journal =

    Oxholm, Trevor M. , journal =. A Beginner's Guide to Line Intensity Mapping Power Spectra , year =. arXiv , doi =:2204.00685 , groups =

    Pith/arXiv arXiv

  46. [46]

    and Wang, Jingying and Carucci, Isabella P

    Cunnington, Steven and Li, Yichao and Santos, Mario G. and Wang, Jingying and Carucci, Isabella P. and Irfan, Melis O. and Pourtsidou, Alkistis and Spinelli, Marta and Wolz, Laura and Soares, Paula S. and Blake, Chris and Bull, Philip and Engelbrecht, Brandon and Fonseca, Jos. , title =. 2023 , month = feb, number =. arXiv , doi =:2206.01579 , groups =

    Pith/arXiv arXiv 2023

  47. [47]

    and Hinshaw, Gary and H

    Amiri, Mandana and Bandura, Kevin and Chakraborty, Arnab and Dobbs, Matt and Fandino, Mateus and Foreman, Simon and Gan, Hyoyin and Halpern, Mark and Hill, Alex S. and Hinshaw, Gary and H. , title =. 2024 , month = mar, number =. arXiv , doi =:2309.04404 , groups =

    Pith/arXiv arXiv 2024

  48. [48]

    Direct correlation of line intensity mapping and CMB lensing from evolution along the lightcone , year =

    Shen, Delon and Kokron, Nickolas and Schaan, Emmanuel , journal =. Direct correlation of line intensity mapping and CMB lensing from evolution along the lightcone , year =. arXiv , doi =:2507.17752 , groups =

    arXiv

  49. [49]

    2025 , month = nov, pages =

    arXiv e-prints , title =. 2025 , month = nov, pages =. arXiv , doi =:2511.19620 , groups =

    arXiv 2025

  50. [50]

    Masui, K. W. and Switzer, E. R. and Banavar, N. and Bandura, K. and Blake, C. and Calin, L.-M. and Chang, T.-C. and Chen, X. and Li, Y.-C. and Liao, Y.-W. and Natarajan, A. and Pen, U.-L. and Peterson, J. B. and Shaw, J. R. and Voytek, T. C. , journal =. Measurement of 21 cm Brightness Fluctuations at z. 2013 , month = jan, number =. arXiv , doi =:1208.03...

    Pith/arXiv arXiv 2013

  51. [51]

    and Alexander, Paul and Ali, Zaki S

    Abdurashidova, Zara and Aguirre, James E. and Alexander, Paul and Ali, Zaki S. and Balfour, Yanga and Beardsley, Adam P. and Bernardi, Gianni and Billings, Tashalee S. and Bowman, Judd D. and Bradley, Richard F. and Bull, Philip and Burba, Jacob and Carey, Steve and Carilli, Chris L. and Cheng, Carina and DeBoer, David R. and Dexter, Matt and de Lera Aced...

    Pith/arXiv arXiv 2022

  52. [52]

    and Baartman, Rushelle and Barkana, Rennan and Berkhout, Lindsay M

    Abdurashidova, Zuhra and Adams, Tyrone and Aguirre, James E. and Baartman, Rushelle and Barkana, Rennan and Berkhout, Lindsay M. and Bernardi, Gianni and Billings, Tashalee S. and Bizarria, Bruno B. and Bowman, Judd D. and Breitman, Daniela and Bull, Philip and Burba, Jacob and Byrne, Ruby and Carey, Steven and Chandra, Rajorshi Sushovan and Chen, Kai-Fen...

    arXiv 2026

  53. [53]

    Mertens, F. G. and Mevius, M. and Koopmans, L. V. E. and Offringa, A. R. and Mellema, G. and Zaroubi, S. and Brentjens, M. A. and Gan, H. and Gehlot, B. K. and Pandey, V. N. and Sardarabadi, A. M. and Vedantham, H. K. and Yatawatta, S. and Asad, K. M. B. and Ciardi, B. and Chapman, E. and Gazagnes, S. and Ghara, R. and Ghosh, A. and Giri, S. K. and Iliev,...

    Pith/arXiv arXiv 2020

  54. [54]

    and Amiri, Mandana and Bond, J

    Bandura, Kevin and Addison, Graeme E. and Amiri, Mandana and Bond, J. Richard and Campbell-Wilson, Duncan and Connor, Liam and Cliche, Jean-Fran. Ground-based and Airborne Telescopes V , title =. 2014 , editor =. arXiv , doi =:1406.2288 , groups =

    Pith/arXiv arXiv 2014

  55. [55]

    2025 , month = mar, number =

    , title =. 2025 , month = mar, number =. arXiv , doi =:2407.21626 , groups =

    Pith/arXiv arXiv 2025

  56. [56]

    and Parsons, Aaron R

    DeBoer, David R. and Parsons, Aaron R. and Aguirre, James E. and Alexander, Paul and Ali, Zaki S. and Beardsley, Adam P. and Bernardi, Gianni and Bowman, Judd D. and Bradley, Richard F. and Carilli, Chris L. and Cheng, Carina and de Lera Acedo, Eloy and Dillon, Joshua S. and Ewall-Wice, Aaron and Fadana, Gcobisa and Fagnoni, Nicolas and Fritz, Randall and...

    Pith/arXiv arXiv

  57. [57]

    and Parsons, Aaron R

    Pober, Jonathan C. and Parsons, Aaron R. and Aguirre, James E. and Ali, Zaki and Bradley, Richard F. and Carilli, Chris L. and DeBoer, Dave and Dexter, Matthew and Gugliucci, Nicole E. and Jacobs, Daniel C. and Klima, Patricia J. and MacMahon, Dave and Manley, Jason and Moore, David F. and Stefan, Irina I. and Walbrugh, William P. , journal =. Opening the...

    Pith/arXiv arXiv

  58. [58]

    and Cairns, Iver and Kaplan, David L

    Bowman, Judd D. and Cairns, Iver and Kaplan, David L. and Murphy, Tara and Oberoi, Divya and Staveley-Smith, Lister and Arcus, Wayne and Barnes, David G. and Bernardi, Gianni and Briggs, Frank H. and Brown, Shea and Bunton, John D. and Burgasser, Adam J. and Cappallo, Roger J. and Chatterjee, Shami and Corey, Brian E. and Coster, Anthea and Deshpande, Avi...

    Pith/arXiv arXiv

  59. [59]

    Nunhokee, C. D. and Null, D. and Trott, C. M. and Barry, N. and Qin, Y. and Wayth, R. B. and Line, J. L. B. and Jordan, C. H. and Pindor, B. and Cook, J. H. and Bowman, J. and Chokshi, A. and Ducharme, J. and Elder, K. and Guo, Q. and Hazelton, B. and Hidayat, W. and Ito, T. and Jacobs, D. and Jong, E. and Kolopanis, M. and Kunicki, T. and Lilleskov, E. a...

    Pith/arXiv arXiv 2025

  60. [60]

    Hollenbach, D. J. and Tielens, A. G. G. M. , journal =. Photodissociation regions in the interstellar medium of galaxies , year =. doi:10.1103/RevModPhys.71.173 , groups =

    doi:10.1103/revmodphys.71.173

  61. [61]

    Carilli, C. L. and Walter, F. , journal =. Cool Gas in High-Redshift Galaxies , year =. arXiv , doi =:1301.0371 , groups =

    Pith/arXiv arXiv

  62. [62]

    Stacey, G. J. and Geis, N. and Genzel, R. and Lugten, J. B. and Poglitsch, A. and Sternberg, A. and Townes, C. H. , journal =. The 158 Micron [C ii] Line: A Measure of Global Star Formation Activity in Galaxies , year =. doi:10.1086/170062 , groups =

    doi:10.1086/170062

  63. [63]

    and Kaufman, M

    Malhotra, S. and Kaufman, M. J. and Hollenbach, D. and Helou, G. and Rubin, R. H. and Brauher, J. and Dale, D. and Lu, N. Y. and Lord, S. and Stacey, G. and Contursi, A. and Hunter, D. A. and Dinerstein, H. , journal =. Far-Infrared Spectroscopy of Normal Galaxies: Physical Conditions in the Interstellar Medium , year =. arXiv , doi =:astro-ph/0106485 , groups =

    Pith/arXiv arXiv

  64. [64]

    and Boquien, M

    De Looze, Ilse and Cormier, Diane and Lebouteiller, Vianney and Madden, Suzanne and Baes, Maarten and Bendo, George J. and Boquien, M. , title =. 2014 , month = aug, pages =. arXiv , doi =:1402.4075 , groups =

    Pith/arXiv arXiv 2014

  65. [65]

    and Cousin, M

    Lagache, G. and Cousin, M. and Chatzikos, M. , journal =. The [CII] 158. 2018 , month = jan, pages =. arXiv , doi =:1711.00798 , groups =

    Pith/arXiv arXiv 2018

  66. [66]

    Stacey, G. J. and Hailey-Dunsheath, S. and Ferkinhoff, C. and Nikola, T. and Parshley, S. C. and Benford, D. J. and Staguhn, J. G. and Fiolet, N. , journal =. A 158. 2010 , month = dec, number =. arXiv , doi =:1009.4216 , groups =

    Pith/arXiv arXiv 2010

  67. [67]

    and Bolatto, A

    Herrera-Camus, R. and Bolatto, A. D. and Wolfire, M. G. and Smith, J. D. and Croxall, K. V. and Kennicutt, R. C. and Calzetti, D. and Helou, G. and Walter, F. and Leroy, A. K. and Draine, B. and Brandl, B. R. and Armus, L. and Sandstrom, K. M. and Dale, D. A. and Aniano, G. and Meidt, S. E. and Boquien, M. and Hunt, L. K. and Galametz, M. and Tabatabaei, ...

    Pith/arXiv arXiv 2015

  68. [68]

    , journal =

    Kennicutt, Jr., Robert C. , journal =. The Global Schmidt Law in Star-forming Galaxies , year =. arXiv , doi =:astro-ph/9712213 , groups =

    Pith/arXiv arXiv

  69. [69]

    Solomon, P. M. and Vanden Bout, P. A. , journal =. Molecular Gas at High Redshift , year =. arXiv , doi =:astro-ph/0508481 , groups =

    Pith/arXiv arXiv

  70. [70]

    and Evans, Neal J

    Kennicutt, Robert C. and Evans, Neal J. , journal =. Star Formation in the Milky Way and Nearby Galaxies , year =. arXiv , doi =:1204.3552 , groups =

    Pith/arXiv arXiv

  71. [71]

    and Wolfire, Mark and Leroy, Adam K

    Bolatto, Alberto D. and Wolfire, Mark and Leroy, Adam K. , journal =. The CO-to-H _. 2013 , month = aug, number =. arXiv , doi =:1301.3498 , groups =

    Pith/arXiv arXiv 2013

  72. [72]

    and Borowska, Jowita and Breysse, Patrick C

    Cleary, Kieran A. and Borowska, Jowita and Breysse, Patrick C. and Catha, Morgan and Chung, Dongwoo T. and Church, Sarah E. and Dickinson, Clive and Eriksen, Hans Kristian and Foss, Marie Kristine and Gundersen, Joshua Ott and Harper, Stuart E. and Harris, Andrew I. and Hobbs, Richard and Ihle, H. , title =. 2022 , month = jul, number =. arXiv , doi =:211...

    Pith/arXiv arXiv 2022

  73. [73]

    and Lunde, J

    Stutzer, N.-O. and Lunde, J. G. S. and Breysse, P. C. and Chung, D. T. and Cleary, K. A. and Dunne, D. A. and Eriksen, H. K. and Ihle, H. T. and Padmanabhan, H. and Tolgay, D. and Wehus, I. K. and Bond, J. R. and Church, S. E. and Gaier, T. and Gundersen, J. O. and Harris, A. I. and Harper, S. E. and Hobbs, R. and Kim, J. and Lamb, J. W. and Lawrence, C. ...

    Pith/arXiv arXiv 2024

  74. [74]

    Lunde, J. G. S. and Stutzer, N.-O. and Breysse, P. C. and Chung, D. T. and Cleary, K. A. and Dunne, D. A. and Eriksen, H. K. and Harper, S. E. and Ihle, H. T. and Lamb, J. W. and Pearson, T. J. and Philip, L. and Wehus, I. K. and Woody, D. P. and Bond, J. R. and Church, S. E. and Gaier, T. and Gundersen, J. O. and Harris, A. I. and Hobbs, R. and Kim, J. a...

    Pith/arXiv arXiv 2024

  75. [75]

    , title =

    Castellano, Marco and Fontana, Adriano and Treu, Tommaso and Merlin, Emiliano and Santini, Paola and Bergamini, Pietro and Grillo, Claudio and Rosati, Piero and Acebron, Ana and Leethochawalit, Nicha and Paris, Diego and Bonchi, Andrea and Belfiori, Davide and Calabr. , title =. 2023 , month = may, number =. arXiv , doi =:2212.06666 , groups =

    Pith/arXiv arXiv 2023

  76. [76]

    , title =

    B. , title =. 2020 , month = nov, pages =. arXiv , doi =:2002.00962 , groups =

    Pith/arXiv arXiv 2020

  77. [77]

    and Adelman, J

    York, Donald G. and Adelman, J. and Anderson, Jr., John E. and Anderson, Scott F. and Annis, James and Bahcall, Neta A. and Bakken, J. A. and Barkhouser, Robert and Bastian, Steven and Berman, Eileen and Boroski, William N. and Bracker, Steve and Briegel, Charlie and Briggs, John W. and Brinkmann, J. and Brunner, Robert and Burles, Scott and Carey, Larry ...

    Pith/arXiv arXiv 2000

  78. [78]

    and Whitaker, Katherine E

    Skelton, Rosalind E. and Whitaker, Katherine E. and Momcheva, Ivelina G. and Brammer, Gabriel B. and van Dokkum, Pieter G. and Labb. , title =. 2014 , month = oct, number =. arXiv , doi =:1403.3689 , groups =

    Pith/arXiv arXiv 2014

  79. [79]

    2025 , month = mar, pages =

    arXiv e-prints , title =. 2025 , month = mar, pages =. arXiv , doi =:2503.15302 , groups =

    Pith/arXiv arXiv 2025

  80. [80]

    and Marrone, Daniel P

    Keating, Garrett K. and Marrone, Daniel P. and Bower, Geoffrey C. and Leitch, Erik and Carlstrom, John E. and DeBoer, David R. , journal =. COPSS II: The Molecular Gas Content of Ten Million Cubic Megaparsecs at Redshift z. 2016 , month = oct, number =. arXiv , doi =:1605.03971 , groups =

    Pith/arXiv arXiv 2016

Showing first 80 references.