
 We present a multiwavelength analysis using the Submillimeter Array (SMA), James Clerk Maxwell Telescope, NOEMA, JWST, the Hubble Space Telescope (HST), and the Spitzer Space Telescope of two dusty strongly star-forming galaxies, 850.1 and 850.2, seen through the massive cluster lens A 1489. These SMA-located sources both lie at z = 4.26 and have bright dust continuum emission, but 850.2 is a UV-detected Lyman-break galaxy, while 850.1 is undetected at ≲ 2 μm, even with deep JWST/NIRCam observations. We investigate their stellar, interstellar medium, and dynamical properties, including a pixel-level spectral energy distribution analysis to derive subkiloparsec-resolution stellar-mass and A
 
 V
 maps. We find that 850.1 is one of the most massive and highly obscured, A
 
 V
 ∼ 5, galaxies known at z > 4 with M
 * ∼1011.8
 M
 ⊙ (likely forming at z > 6), and 850.2 is one of the least massive and least obscured, A
 
 V
 ∼ 1, members of the z > 4 dusty star-forming population. The diversity of these two dust-mass-selected galaxies illustrates the incompleteness of galaxy surveys at z ≳ 3–4 based on imaging at ≲ 2 μm, the longest wavelengths feasible from HST or the ground. The resolved mass map of 850.1 shows a compact stellar-mass distribution, 
 


 
 
 
 R
 
 
 e
 
 
 mass
 
 
 
 
 ∼1 kpc, but its expected evolution means that it matches both the properties of massive, quiescent galaxies at z ∼ 1.5 and ultramassive early-type galaxies at z ∼ 0. We suggest that 850.1 is the central galaxy of a group in which 850.2 is a satellite that will likely merge in the near future. The stellar morphology of 850.1 shows arms and a linear bar feature that we link to the active dynamical environment it resides within.

Hidden Giants in JWST's PEARLS: An Ultramassive z = 4.26 Submillimeter Galaxy that Is Invisible to HST


 We report the ALMA Band 7 observations of 86 Herschel sources that likely contain gravitationally-lensed galaxies. These sources are selected with relatively faint 500 μm flux densities between 15 to 85 mJy in an effort to characterize the effect of lensing across the entire million-source Herschel catalogue. These lensed candidates were identified by their close proximity to bright galaxies in the near-infrared VISTA Kilo-Degree Infrared Galaxy Survey (VIKING) survey. Our high-resolution observations (0.15 arcsec) confirm 47 per cent of the initial candidates as gravitational lenses, while lensing cannot be excluded across the remaining sample. We find average lensing masses (log M/M⊙ = 12.9 ± 0.5) in line with previous experiments, although direct observations might struggle to identify the most massive foreground lenses across the remaining 53 per cent of the sample, particularly for lenses with larger Einstein radii. Our observations confirm previous indications that more lenses exist at low flux densities than expected from strong galaxy-galaxy lensing models alone, where the excess is likely due to additional contributions of cluster lenses and weak lensing. If we apply our method across the total 660 sqr. deg. H-ATLAS field, it would allow us to robustly identify 3000 gravitational lenses across the 660 square degree Herschel ATLAS fields.

FLASH: Faint lenses from Associated Selection with Herschel


 We present the deepest 850 μm map of the SSA22 field to date, utilizing a combination of new and archival observations taken with SCUBA-2, mounted at the James Clerk Maxwell Telescope (JCMT). The mapped area covers an effective region of approximately 0.34 deg2, achieving a boundary sensitivity of 2 mJy beam−1, with the deepest central coverage reaching a depth of σrms ∼ 0.79 mJy beam−1, the confusion noise is estimated to be ∼ 0.43 mJy beam−1. A catalogue of 850 μm sources in the SSA22 field is generated, identifying 390 sources with single-to-noise ratios above 3.5, out of which 92 sources exceed 5σ. The derived intrinsic number counts at 850 μm are found to be in excellent agreement with published surveys. Interestingly, the SSA22 number counts also exhibit an upturn in the brighter flux region, likely attributed to local emitters or lensing objects within the field. On the scale of ∼ 0.3 deg2, the 850 μm number counts are unaffected by cosmic variance and align with the blank field. In the deep region (σrms ≤ 1 mJy), the counts for fluxes below 8 mJy are consistent with the blank field, and the excess in the brighter regime is not significant. Due to the limited number of very bright sources and the insubstantial cosmic variance in our field, we attribute the fluctuations in the number counts primarily to Poisson noise. The SCUBA-2 850 μm detection in the SSA22 field does not exhibit indications of overdensity.

https://academic.oup.com/mnras/advance-article-pdf/doi/10.1093/mnras/stae017/55403926/stae017.pdf

Deep Submillimetre and Radio Observations in the SSA22 Field. II. Sub-millimetre source catalogue and number counts


 We investigate the constraints provided by the Euclid space observatory on the physical properties of dusty star-forming galaxies (DSFGs) at z ≳ 1.5 detected in wide area sub-millimetre surveys with Herschel. We adopt a physical model for the high-z progenitors of spheroidal galaxies, which form the bulk of DSFGs at z ≳ 1.5. We improve the model by combining the output of the equations of the model with a formalism for the spectral energy distribution (SED). After optimising the SED parameters to reproduce the measured infrared luminosity function and number counts of DFSGs, we simulated a sample of DSFGs over 100 deg2 and then applied a 5 σ detection limit of 37 mJy at 250 μm. We estimated the redshifts from the Euclid data and then fitted the Euclid+Herschel photometry with the code CIGALE to extract the physical parameters. We found that $100\%$ of the Herschel galaxies are detected in all 4 Euclid bands above 3 σ. For $87\%$ of these sources the accuracy on 1 + z is better than 15%. The sample comprises mostly massive, i.e. log (M⋆/M⊙) ∼ 10.5 − 12.9, highly star–forming, i.e. log (SFR/M⊙yr−1) ∼ 1.5 − 4, dusty, i.e. log (Mdust/M⊙) ∼ 7.5 − 9.9, galaxies. The measured stellar masses have a dispersion of 0.19 dex around the true value, thus showing that Euclid will provide reliable stellar mass estimates for the majority of the bright DSFGs at z ≳ 1.5 detected by Herschel. We also explored the effect of complementing the Euclid photometry with that from the Vera C. Rubin Observatory/LSST.

pdf/euclid-view-of-the-dusty-star-forming-galaxies-at-z-1-5-53akg6spev.pdf

Euclid view of the dusty star-forming galaxies at z ≳ 1.5 detected in wide area sub-millimetre surveys

Abstract We use the Atacama Large sub/Millimetre Array (ALMA) to efficiently observe spectral lines across Bands 3, 4, 5, 6, 7, and 8 at high-resolution (0.″5 – 0.″1) for 16 bright southern Herschel sources at 1.5 &amp;lt; z &amp;lt; 4.2. With only six and a half hours of observations, we reveal 66 spectral lines in 17 galaxies. These observations detect emission from CO (3–2) to CO(18–17), as well as atomic ([C i](1-0), (2-1), [O i] 145 μm and [N ii] 205 μm) lines. Additional molecular lines are seen in emission (H2O and H2O+) and absorption (OH+ and CH+). The morphologies based on dust continuum ranges from extended sources to strong lensed galaxies with magnifications between 2 and 30. CO line transitions indicate a diverse set of excitation conditions with a fraction of the sources (∼35 per cent) showcasing dense, warm gas. The resolved gas to star-formation surface densities vary strongly per source, and suggest that the observed diversity of dusty star-forming galaxies could be a combination of lensed, compact dusty starbursts and extended, potentially-merging galaxies. The predicted gas depletion timescales are consistent with 100 Myr to 1 Gyr, but require efficient fueling from the extended gas reservoirs onto the more central starbursts, referee in line with the Doppler-shifted absorption lines that indicate inflowing gas for two out of six sources. This pilot paper explores a successful new method of observing spectral lines in large samples of galaxies, supports future studies of larger samples, and finds that the efficiency of this new observational method will be further improved with the planned ALMA Wideband Sensitivity Upgrade. 

A novel high-z submm galaxy efficient line survey in ALMA bands 3 through 8 - an ANGELS pilot

We present 850um imaging of the XMM-LSS field observed for 170 hours as part of the James Clerk Maxwell Telescope SCUBA-2 Large eXtragalactic Survey (S2LXS). S2LXS XMM-LSS maps an area of 9 square degrees, reaching a moderate depth of 1-sigma ~ 4 mJy/beam. This is the largest contiguous area of extragalactic sky mapped by JCMT at 850um to date. The wide area of the S2LXS XMM-LSS survey allows us to probe the ultra-bright (S_850um>15 mJy), yet rare submillimetre population. We present the S2LXS XMM-LSS catalogue, which comprises 40 sources detected at>5-sigma significance, with deboosted flux densities in the range of 7 mJy to 48 mJy. We robustly measure the bright-end of the 850um number counts at flux densities>7 mJy, reducing the Poisson errors compared to existing measurements. The S2LXS XMM-LSS observed number counts show the characteristic upturn at bright fluxes, expected to be motivated by local sources of submillimetre emission and high-redshift strongly lensed galaxies. We find that the observed 850um number counts are best reproduced by model predictions that include either strong lensing or source blending from a 15 arcsec beam, indicating that both may make an important contribution to the observed over-abundance of bright single dish 850um selected sources. We make the S2LXS XMM-LSS 850um map and>5-sigma catalogue presented here publicly available.

/pdf/the-scuba-2-large-extragalactic-survey-850um-map-catalogue-2s3wb9js.pdf

The SCUBA-2 Large eXtragalactic Survey: 850um map, catalogue and the bright-end number counts of the XMM-LSS field

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The SCUBA-2 Large eXtragalactic Survey: 850um map, catalogue and the bright-end number counts of the XMM-LSS field