Weekly issue

Week 26, 2025

Jun 23–29, 2025

Week 26, 2025 includes 6 curated papers, centered on high-z, spectroscopy, QSO.

2506.20896v1

Blowing star formation away in AGN Hosts (BAH) -- IV: Feeding and feedback in 3C 293 observed with JWST NIRSpec

Maitê S. Z. de Mellos, Rogemar A. Riffel, Gabriel L. Souza-Oliveira, Nadia L. Zakamska, Marina Bianchin, Thaisa Storchi-Bergmann, Rogério Riffel, José Henrique Costa-Souza

Theme match 5/5

Digest

JWST/NIRSpec IFU mapping of 3C 293’s inner ~2 kpc separates the gas into a rotating disk (σ ~100 km s−1), a blueshifted broad outflow (σ ~250 km s−1), and a very broad ionized outflow (σ ~640 km s−1). H2 2.12 μm, [Fe II] 1.64 μm, and Paα trace multiphase flows through heavy dust (A_V up to ~35), with H2 inflow along dust lanes at Ṁ_in ~4×10−4 M⊙ yr−1. Peak outflow rates reach 0.08±0.02 M⊙ yr−1 (hot H2) and 6.5±1.7 M⊙ yr−1 (ionized), and the jet-driven outflow carries ≈5% of the radio-jet power—sufficient to suppress star formation. The stellar field is a rotating disk whose kinematic center is offset by ~0.5 arcsec from the NIR continuum peak, consistent with a disturbed, post-merger nucleus.

Open paper page arXiv abstract arXiv PDF Highlighted PDF

Key figures to inspect

Fig. 1 composite + nuclear spectrum: verify strong H2, [Fe II], and Paα features and CO bandheads at the continuum peak; use to see the emission-line budget that motivates the multiphase kinematic decomposition.
Fig. 2 line-profile fits ([Fe II], Paα, H2): inspect the narrow/broad/very broad components and their σ values (~100/250/640 km s−1) and blueshifts, clarifying which phases host the fast outflow.
Fig. 3 stellar velocity/dispersion maps: confirm the rotating stellar disk and measure the ~0.5 arcsec offset between the kinematic center and continuum peak; check for central σ enhancements indicative of a disturbed nucleus.
Fig. 4 gas maps (flux/velocity/dispersion): compare narrow vs broad components to locate the jet-aligned outflow and identify H2 streaming along dust lanes (inflow) versus outflowing ionized gas, and relate high-velocity regions to obscured structures.

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2506.20634v1

The VLA Frontier Fields Survey: A 6GHz High-resolution Radio Survey of Abell 2744

Esteban A. Orozco, Eric F. Jiménez-Andrade, Eric J. Murphy, Ian Smail, Emmanuel Momjian, Ian Heywood, Miguel Vega-Gutierrez, Christa DeCoursey

Theme match 4/5

Digest

Ultra-deep 6 GHz VLA imaging of Abell 2744 (z=0.307) reaches ≈1 µJy beam−1 at 0.82″, yielding 93 detections, 46 with optical/NIR counterparts spanning z=0.15–3.55 (median z=0.93; median M⋆≈2.3×10^10 M⊙). Radio-inferred SFRs exceed UV–NIR estimates by roughly an order of magnitude, pointing to heavily obscured star formation missed by rest-UV/optical tracers. No individual radio counterparts are found for the z≈6 Little Red Dots; stacking sets a stringent 3σ limit of L6 GHz < 4.1×10^39 erg s−1. The survey also assembles 22 μ≳2 lensed systems, enabling sub-arcsecond probes of main-sequence galaxies at z∼1–2.

Open paper page arXiv abstract arXiv PDF Highlighted PDF

Key figures to inspect

Sensitivity/beam map of the 6 GHz mosaic: verify the ≈1 µJy beam−1 floor at the phase center, the 0.82″ synthesized beam, and how noise rises with radius across Abell 2744.
Radio–UV/NIR SFR comparison plot: inspect the ≈10× offset, trends with redshift or M⋆, and whether AGN-flagged sources drive outliers.
LRD stacking analysis: view the postage-stamp stack, radial profile, and flux-density limit that translates to L6 GHz < 4.1×10^39 erg s−1 at z≈6.
Lens-model/magnification distribution: check μ estimates and spatial locations for the 22 μ≳2 sources relative to the critical curves.
Postage stamps of representative lensed galaxies: compare 6 GHz contours with HST/NIR images to see alignment, sizes, and any evidence for compact star-forming knots.

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2506.19589v1

Black Holes in the Red-sequence Elliptical Galaxies at Redshifts $\sim 0.7-2.5$: Not Dark Energy Source but Remanants of Little Red Dots

Lei Lei, Ze-Fan Wang, Yi-Ying Wang, Lei Feng, Yi-Zhong Fan

Theme match 4/5

Digest

Uses a JWST-selected set of very high‑z AGNs in red‑sequence ellipticals to test black‑hole cosmological coupling via the MBH–M* fundamental plane. The sample aligns with the local relation and yields a posterior on the coupling strength that rejects the “BHs as dark energy” scenario at >10σ, contradicting earlier claims of strong coupling. Simulations and data further show that low‑accretion Little Red Dots can evolve into the z≈0.7–2.5 red‑sequence ellipticals hosting relatively low‑mass BHs, eliminating the need for cosmological coupling. This links JWST LRD demographics to later ETG BH masses while removing BHs as a viable dark‑energy source.

Open paper page arXiv abstract arXiv PDF Highlighted PDF

Key figures to inspect

Figure 1: Compare JWST AGNs to the local MBH–M* relation and the blue dashed prediction for nonzero coupling; note that the high‑z points track the local plane rather than the coupled-growth track.
Figure 2: Inspect the posterior for the coupling parameter; quantify how far the peak and credible intervals lie from the strong‑coupling value and note the >10σ exclusion relative to previous claims.
Figure 3: Follow the simulated LRD evolutionary contours across redshift and see how they overlap both JWST LRD measurements and the red-/blue-point AGN samples, supporting an LRD→red‑sequence ETG pathway.

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2506.22416v1

Cosmology from Planck CMB Lensing and DESI DR1 Quasar Tomography

R. de Belsunce, A. Krolewski, S. Chiarenza, E. Chaussidon, S. Ferraro, B. Hadzhiyska, C. Ravoux, N. Sailer, G. Farren, A. Tamone, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. Cuceu, A. de la Macorra, J. Della Costa, Biprateep Dey, P. Doel, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, H. K. Herrera-Alcantar, K. Honscheid, M. Ishak, R. Joyce, S. Juneau, R. Kehoe, D. Kirkby, T. Kisner, A. Kremin, O. Lahav, A. Lambert, C. Lamman, M. Landriau, L. Le Guillou, M. E. Levi, M. Manera, P. Martini, A. Meisner, R. Miquel, S. Nadathur, G. Niz, N. Palanque-Delabrouille, W. J. Percival, F. Prada, I. Pérez-Ràfols, A. J. Ross, G. Rossi, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou

Theme match 2/5

Digest

Cross-correlating Planck PR4 (NPIPE) CMB lensing maps with 1.22M DESI DR1 spectroscopic quasars over 7,200 deg², the authors perform three-bin quasar–lensing tomography at z≈1.44, 2.27, and 2.75. A joint fit to quasar auto- and quasar×lensing power spectra, with an Ωm prior from DESI DR1 BAO, yields σ8=0.929(+0.059/−0.074) and S8=0.922(+0.059/−0.073), with detections of the cross and auto signals at S/N=21.7 and 27.2, respectively. The inferred growth amplitude is ≈1.5σ higher than ΛCDM predictions from Planck primary CMB, providing a high‑z, matter‑era check on structure formation. Combining with the Planck PR4 and ACT DR6 lensing auto-spectra, they obtain a sound-horizon-free H0=69.1(+2.2/−2.6) km s⁻¹ Mpc⁻¹ via sensitivity to the matter–radiation equality scale.

Open paper page arXiv abstract arXiv PDF Highlighted PDF

Key figures to inspect

Data maps: PR4 κ-convergence, DESI DR1 quasar density, and completeness mask—inspect sky overlap (Planck 67.1% vs DESI 20.3%) and spatial nonuniformities that could affect large-scale power.
Tomographic Cℓ(κ×q) per bin at z≈1.44, 2.27, 2.75 with best-fit model—check scale dependence, ℓ-ranges used, and per-bin S/N driving the joint constraints.
Quasar auto-power spectra and inferred bias vs redshift—verify consistency across bins and with mocks/analytic expectations used in the likelihood.
Posterior contours for σ8/S8 with the DESI-BAO Ωm prior—see the ≈1.5σ preference relative to Planck primary-CMB ΛCDM and how the tomographic bins combine.
Lensing-only H0 constraint figure (Planck PR4 + ACT DR6 autospectra plus this cross-correlation)—see how the equality-scale information yields H0 without a sound-horizon prior.

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2506.21658v1

Euclid and Roman with JWST Could Reveal Quasars at up to $z \sim$ 15

Muhammad A. Latif, Daniel J. Whalen

Theme match 2/5

Digest

Normalizing a thin-disk+corona spectrum to a J1120-like quasar grown in the Smidt et al. (2018) simulation, the authors predict continuum NIR AB magnitudes from z = 6–15 in Euclid, Roman, and JWST bands. They find Euclid can photometrically select such SMBHs to z ≈ 11 (Wide), z ≈ 13 (Deep), and z ≈ 14 (Ultra Deep), while Roman reaches z ≈ 14.5 in Y/J/H and its F213 band extends selection to z ≈ 18. JWST’s sensitivity enables spectroscopic redshift confirmation to z ≈ 15 and even detects ≳10^6 M⊙ BHs accreting near Eddington. This Euclid/Roman discovery plus JWST follow-up pipeline could inventory early SMBHs (including analogs of UHZ1 and GHZ9) and discriminate their growth channels beyond z > 10.

Open paper page arXiv abstract arXiv PDF Highlighted PDF

Key figures to inspect

Figure 1: Trace the bolometric luminosity versus redshift from the J1120-like simulation to see the 0.2–0.8 Eddington phases that set the normalization of the disk+corona SED used for all detectability forecasts.
Figure 2 (Euclid panel): Read where the H/J AB-magnitude curves intersect WS/DS/EUDS limits (24.5/26.0/27.7) to get z ≈ 11/13/14 reach; note why earlier times are cut off by the Lyman-limit absorption entering these filters.
Figure 2 (Roman panel): Compare Y/J/H curves to the HLSS 28 mag line to see Roman’s z ≈ 14.5 advantage and large-area yield; keep in mind the seven-filter coverage and F213 to 2.3 µm that supports z > 15 dropouts.
Figure 3: JWST NIRCam (2.5, 3.65, 4.44, 4.60 µm) AB magnitudes lie well above the m_AB ≈ 32 imaging limit, illustrating comfortable margins for NIRSpec confirmation and viability down to ~10^6 M⊙ at z ≈ 15.

Tags

2506.18993v1

Direct Collapse Pre-supermassive Black Hole Objects as Ly$α$ Emitters

Yang Luo, Isaac Shlosman

Theme match 2/5

Digest

The authors post-process a direct-collapse pre-SMBH inflow–outflow geometry with a Monte Carlo Lyα transfer that includes photon destruction and two-photon emission, finding that a radiatively driven shell plus a biconical polar funnel enables substantial escape. The emergent Lyα is highly anisotropic and line shapes depend on funnel opening angle and outer column density, yielding strong asymmetry with an extended red tail and measurable peak shifts/cuspiness. The escaping fraction can exceed 95% for a z=10 pre-SMBH object, with only the red wing detectable. Such sources are in principle reachable with NIRSpec/MOS in ~10^4 s at 10σ, and their line profiles provide a diagnostic to separate them from high-z galaxies and quasars.

Open paper page arXiv abstract arXiv PDF Highlighted PDF

Key figures to inspect

Figure 1: Use the schematic to locate the radiatively driven shell and the polar funnel relative to the disky and spherical inflows; this sets the sightlines where Lyα escape and strong anisotropy are expected.
Figure 2: Compare the Monte Carlo escape fractions against the Neufeld (1990) curves across column density and ionization fraction to see where f_esc > 0.95 occurs and how neutral vs. ionized gas controls the outcome.
Figure 3: Track how changing the funnel opening angle and the outer optical depth reshapes the profile—peak velocity shift, cuspiness, and the strength/extent of the red tail—highlighting signatures distinctive of pre-SMBH funnels.
Figure 4: Read off the fraction of intrinsic flux emerging in the red wing and the predicted integrated two-photon flux to gauge detectability and the balance between red-wing line emission and two-photon continuum.