{"total":41,"items":[{"citing_arxiv_id":"2606.27853","ref_index":78,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"MSA-3D: Rotation Curves and Dark Matter Fractions at z~0.5-1.7 with JWST/NIRSpec","primary_cat":"astro-ph.GA","submitted_at":"2026-06-26T08:52:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New JWST data on 23 galaxies at 0.5<z<1.7 show median dark matter fraction of 0.63 at effective radius with 0.2 dex scatter, and a mix of rising, flat, and falling rotation curves.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.26445","ref_index":172,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Columba: isolated dwarf galaxy populations in diverse cosmological environments simulated with a cold interstellar medium","primary_cat":"astro-ph.GA","submitted_at":"2026-06-24T23:14:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New hydrodynamical simulations show that dwarf galaxy stellar mass-halo mass relations and star formation histories are more influenced by host halo concentration than by the 5 cMpc scale environment.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23790","ref_index":24,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Anisotropic quenching beyond $z=1$ and its implications for preprocessing around high-redshift galaxy clusters","primary_cat":"astro-ph.GA","submitted_at":"2026-06-22T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Anisotropic quenching is detected at the highest redshift yet and linked to preprocessing dominating over intrahalo effects by ~20% along the major axis in a delay-then-rapid quenching model informed by cluster accretion histories.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21651","ref_index":186,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Resolved Ages and Stellar Metallicities in Progenitors of Milky Way Analogs: A Closer Look at their Star Formation Histories since $z=5$","primary_cat":"astro-ph.GA","submitted_at":"2026-06-19T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Resolved stellar property gradients in Milky Way analog progenitors show inside-out assembly with minor, temporary disruption from major mergers.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.20809","ref_index":10,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"The Lifecycle and Emission Properties of PAHs in Cosmological Hydrodynamic Galaxy Formation Simulations","primary_cat":"astro-ph.GA","submitted_at":"2026-06-18T18:00:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Cosmological zoom-in simulations find that grain-grain shattering in diffuse ISM gas drives rising PAH mass fraction with time, naturally producing the observed PAH-metallicity relation and inverse qPAH-molecular gas trends.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"2000), and a temperature-dependent sticking coefficientS from Zhukovska et al. (2016) that reduces growth efficiency in warm gas. Thermal sputtering:In hot gas, collisions with thermal ions erode grain surfaces, at a rate: \u0012 da dt \u0013 sp =− a τsp (9) where the sputtering timescale follows the analytic approxi- mation of Tsai & Mathews (1995): τsp = 0.17 Gyr \u0012 a aref \u0013\u0012 10−27 g cm−3 ρg \u0013\u0014\u0012 T0 T \u0013ω + 1 \u0015 (10) witha ref = 0.1µm a reference grain radius,ρ g the lo- cal gas density,Tthe local gas temperature,ω= 2.5and T0 = 2×10 6 K, whereT 0 sets the temperature scale above which thermal sputtering becomes efficient andωcontrols the steepness of the sputtering rate with gas temperature. Supernova shock destruction:Dust grains swept up by supernova blast waves undergo partial or complete destruc-"},{"citing_arxiv_id":"2606.19463","ref_index":212,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"On the later evolution of observationally selected protocluster candidates at $z\\,{\\gtrsim}\\,5$","primary_cat":"astro-ph.GA","submitted_at":"2026-06-17T18:01:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations show observationally selected protocluster candidates at z ≳ 5 include significant interlopers, undergo 2-6 major mergers, and exhibit stronger clustering than observed, requiring total galaxy mass within 10 cMpc for reliable progenitor identification.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.19193","ref_index":3,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Solitary dwarf galaxy groups as tracers of primordial dark matter halos in the local Universe","primary_cat":"astro-ph.GA","submitted_at":"2026-06-17T15:34:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Discovery of 14 solitary dwarf galaxy groups with dynamical masses around 10^12 solar masses, interpreted as tracers of primordial dark matter halos.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.16734","ref_index":151,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Edge-on Galaxies in the DESI survey (EGIDE): sample building and photometry","primary_cat":"astro-ph.GA","submitted_at":"2026-06-15T13:55:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"The EGIDE project releases a tenfold larger catalogue of edge-on galaxies with griz photometry, stellar masses, redshifts and star formation rates, finding that red-sequence galaxies are thicker than blue-cloud ones and show a mass-dependent increase in flattening ratio.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12249","ref_index":36,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Spatially Resolved Nebular-Stellar Reddening with JWST/NIRISS","primary_cat":"astro-ph.GA","submitted_at":"2026-06-10T15:52:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"JWST observations of high-redshift galaxies show no evolution in dust geometry to z~2.4 and yield an empirical calibration linking resolved differential reddening to SFR surface density.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10648","ref_index":52,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Star-formation variability on the star-forming main sequence during the Epoch of Reionization","primary_cat":"astro-ph.GA","submitted_at":"2026-06-09T09:57:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"PSD modeling of SFR scatter at six timescales shows dominant variability on 10-30 Myr scales, stronger in lower-mass galaxies at z=3-8.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10271","ref_index":87,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Multiphase images of a powerful supernova-driven wind in the early Universe","primary_cat":"astro-ph.GA","submitted_at":"2026-06-09T00:36:56+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Resolved multiphase observations reveal a supernova-driven wind in a z=5.3 galaxy removing gas at twice the star-formation rate, potentially quenching it within 100 Myr and matching local superwind properties.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10022","ref_index":126,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Learning the Universe with PRFM-vol: Introducing a new subgrid model for star formation in cosmological simulations","primary_cat":"astro-ph.GA","submitted_at":"2026-06-08T18:07:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"PRFM-vol is a new subgrid star formation model for cosmological simulations that computes SFR from ambient densities via PRFM theory and a modified effective EOS, producing taller stellar scale heights, slightly higher stellar mass, and morphology changes including Toomre-driven clumps compared to p","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10020","ref_index":252,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Manticore Project II: Bayesian digital twins of cosmic structure across the SDSS and BOSS volumes","primary_cat":"astro-ph.CO","submitted_at":"2026-06-08T18:07:40+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Manticore-Deep uses tiled Bayesian field-level inference on SDSS and BOSS data to produce posterior ensembles of 3D cosmic fields that are consistent with LCDM and validated by 7.4σ CMB lensing and 3.5σ kSZ detections.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.06609","ref_index":299,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"JWST absorption line spectroscopy with SPURS: ISM covering fractions and kinematics in individual galaxies at $z=5-9$","primary_cat":"astro-ph.GA","submitted_at":"2026-06-04T18:01:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"JWST spectra of six z=5-9 galaxies show low-ionization covering fractions of 0.2-0.9 and diverse kinematics including blueshifted outflows, indicating heterogeneous multiphase ISM.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.05151","ref_index":28,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Mapping the star formation peak with LIGO A# and Next-Generation detectors","primary_cat":"gr-qc","submitted_at":"2026-06-03T17:53:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Simulations show LIGO-A# constrains the peak redshift of binary black hole merger rate (tracing star formation) to ±0.1 in one year, improving to ±0.02 with next-generation detectors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.05237","ref_index":97,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"GREX-PLUS Science Book v2","primary_cat":"astro-ph.IM","submitted_at":"2026-06-03T04:42:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"GREX-PLUS is a proposed JAXA L-class mission with a 1m cooled telescope, wide-field 2-8um camera, and R=30000 spectrometer in 10-18um to enable studies of z>15 galaxies, protoplanetary snowlines, and related astrophysics.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.03667","ref_index":48,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Constraining AGN accretion physics with black hole mass-luminosity scaling relations","primary_cat":"astro-ph.GA","submitted_at":"2026-06-02T13:52:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Chaotic Cold Accretion reproduces the observed near-linear black hole mass-bolometric luminosity scaling (slope 0.91) in z>2 quasars while Bondi accretion underpredicts by ~2 dex.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02773","ref_index":102,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Why Little Red Dots Disappear at z < 3: Evolution of Number Density and Halo Mass","primary_cat":"astro-ph.GA","submitted_at":"2026-06-01T18:35:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"LRDs transition from underdense low-halo-mass environments at z>4 to typical galaxy conditions by z~3.5, with halo growth leading to larger sizes and SED changes that explain their disappearance at lower redshifts.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.23554","ref_index":192,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Inferring the role of binary neutron star mergers in r-process nucleosynthesis with multi-messenger observations using Cosmic Explorer and Einstein Telescope","primary_cat":"astro-ph.HE","submitted_at":"2026-05-22T12:19:56+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A new redshift-correlation technique with third-generation GW detectors can constrain the BNS contribution to cosmic r-process nucleosynthesis to 5-6% precision via Fisher forecasts on mock bright- and dark-siren data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.20590","ref_index":163,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Spider-Webb: enhanced star formation in low-mass galaxies within the Spiderweb protocluster revealed by JWST Pa$\\beta$ narrow-band imaging","primary_cat":"astro-ph.GA","submitted_at":"2026-05-20T00:55:56+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Low-mass Paβ emitters in the Spiderweb protocluster show enhanced star formation rates compared to field galaxies, with no significant deviation at higher masses.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.17253","ref_index":35,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"HI Observations of Baryon-Dominated Dwarf Galaxy Candidates","primary_cat":"astro-ph.GA","submitted_at":"2026-05-17T04:22:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Resolved HI observations of six baryon-dominated dwarf galaxy candidates show four are dark-matter deficient with high baryon efficiency, two in isolated environments without tidal signs.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16485","ref_index":5,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Halo-driven Origin and Suppression of Over-massive Black Holes and Little Red Dots","primary_cat":"astro-ph.GA","submitted_at":"2026-05-15T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Halo-driven transient rapid growth followed by thermodynamic suppression explains over-massive black holes and Little Red Dots as precursors to standard SMBH-galaxy coevolution.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15264","ref_index":93,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. II. Mass Mapping and Overdensity Characterization","primary_cat":"astro-ph.GA","submitted_at":"2026-05-14T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"First near-IR weak-lensing analysis of CANDELS fields detects 12 shear-selected overdensities with masses 0.2-2.2 x 10^14 solar masses at redshifts 0.22-0.9 and mean z=0.68.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.13966","ref_index":27,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Massive Galaxies Form Early and Gray: Stellar Assembly and Dust Attenuation at $\\mathbf{z>3.5}$ from CAPERS","primary_cat":"astro-ph.GA","submitted_at":"2026-05-13T18:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Massive galaxies at z>3.5 assembled stars earlier than theoretical models predict and exhibit gray dust attenuation, especially at the highest masses.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.08342","ref_index":4,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Satellite Metallicity Enhancement I: Suppressed Star Formation, Stellar Mass Loss, and Enriched Inflow of DESI and EAGLE Galaxies around Massive Clusters","primary_cat":"astro-ph.GA","submitted_at":"2026-05-08T18:00:10+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"The satellite metallicity enhancement profile around clusters declines steeply in the core, plateaus near the virial radius due to enriched inflow, and declines further out, with mass loss and quenching dominating the core.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"SF Suppression Fsfh Ffmd 4 6 8 10 12 t [Gyr] 0.0 0.1 0.2 0.3 0.4∆M∗(t) [10 9 M⊙] Mass-Loss ∆M∗ 4 6 8 10 12 t [Gyr] 8.4 8.6 8.8 ZISM 4 6 8 10 12 t [Gyr] 2 3 4η 3 4 5 M∗ [109 M⊙] 8.86 8.90 8.94 ZISM ∆M∗ ∆ZML Figure 3.The average stellar mass growth (left), star formation (middle), and mass loss (right) histories of relevant EAGLE galaxy samples atr scale=[0.2,0.4]. Left: Colored curves indicate the stellar mass evolution ofSAT(black),Fsfh(blue),Ffmd(red), andFobs(orange) samples. Red and orange horizontal dashed lines denote the formed and observed stellar masses of theSAT sample atz=0.1, respectively. Middle: Red and blue curves are the average SFHs ofFfmdandFsfhsamples, with the evolutions of their corresponding mass-loading factors and metallicities shown in the bottom-left and top-right inset panels, respectively."},{"citing_arxiv_id":"2605.04776","ref_index":7,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Redshift Evolution of the Ratio of Supermassive Black Hole Mass to Stellar Mass","primary_cat":"astro-ph.GA","submitted_at":"2026-05-06T11:22:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Simulations and analytic modeling predict that the supermassive black hole to stellar mass ratio peaks at several percent around redshift 7-10 before declining toward the present day.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Here we also estimate the relative growth rates of the black hole and stellar components in our simulation with analytical form. For the stellar mass, we assume M⋆ = Z SFR(t)dt,(6) The star formation rate (SFR) follows the empirical re- lation between halo accretion rate from Fakhouri et al. (2010): ˙Mhalo = 46.1M ⊙ yr−1 \u0012 Mhalo 1012M⊙ \u00131.1 ×(1 + 1.11z) \u0002 Ωm(1 +z) 3 + ΩΛ \u00031/2 , (7) SFR(Mhalo, z) =ϵ ⋆ Ωb Ωm ˙Mhalo(z).(8) 6 0.0 2.5 5.0 7.5 10.0 12.5 15.0 17.5 20.0 Redshift z 10 4 10 3 10 2 10 1 100 101 fduty q = 0.15, j = 0.15, Edd < 3 kinetic q = 0.15, j = 0.15, Edd < 3 mechanical q = 0.15, j = 0.15, Edd < 3 delay q = 0.15, j = 0.15, Edd < 3 kinESNII3e51 0.0004 (1 + z)3 M =9.75 M =10.25 M =10.75 M =11.25 Ren+25, 9.5<M <10.5"},{"citing_arxiv_id":"2605.04144","ref_index":77,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The galaxy-halo connection and the dynamical evolution of a giant disc in a massive node of the Cosmic Web at z~3","primary_cat":"astro-ph.GA","submitted_at":"2026-05-05T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The Big Wheel at z~3 has a stellar-to-halo mass ratio of 0.06, higher than expected, implying efficient stellar assembly without major mergers or instabilities.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.02999","ref_index":80,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Peering down the barrel with DESI DR2: 10 000+ inflows at $z$ < 0.6 reveal how galaxies accrete cold gas","primary_cat":"astro-ph.GA","submitted_at":"2026-05-04T18:00:00+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.27477","ref_index":3,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Critical Mass in Galaxy Evolution","primary_cat":"astro-ph.GA","submitted_at":"2026-04-30T06:19:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A simulation study finds that a hot gas halo at galaxy total mass ~10^12.5 solar masses suppresses cool gas accretion, driving a redshift-independent turnover in the stellar-to-total mass ratio via reduced in-situ star formation efficiency.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"observed cosmic star formation history, galaxy stellar mass function, and stellar mass-black hole mass relation. More details on the feedback prescriptions and parameters can be found in J. Lee et al. (2021). To compute the AGN energy injection rates for our sample galaxies, we query the relevant quantities at snapshots corresponding to redshiftsz= [0.625,0.873,0.995,1.985,2.336,2.395,2.98,3.111,3.608,4.074,4.946,5.989,6.96]. We then calculate the median energy injection rates for both the thermal-QSO and jet-AGN modes, as well as the median value ofχ, for the progenitors of our sample galaxies at each snapshot. Based on the medianχ, we determine which feedback mode is effective at a given redshift. The median trend of AGN energy injection rate as a function of redshift"},{"citing_arxiv_id":"2604.26022","ref_index":89,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Secondary Dependence of Baryonic Effects on the Density Profile of Dark Matter Halos","primary_cat":"astro-ph.CO","submitted_at":"2026-04-28T18:05:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Baryonic effects on dark matter halo density profiles exhibit strong secondary dependence on concentration (up to 15% variations at small scales for lower-mass halos) and weaker dependence on large-scale environment (~2%).","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"baryons on the halo mass function, bias, and cluster cosmology,Mon. Not. Roy. Astron. Soc. 500(2021) 2316 [2009.01775]. [88] J. Matthee, J. Schaye, R.A. Crain, M. Schaller, R. Bower and T. Theuns,The origin of scatter in the stellar mass-halo mass relation of central galaxies in the EAGLE simulation, Mon. Not. Roy. Astron. Soc.465(2017) 2381 [1608.08218]. [89] P.S. Behroozi, R.H. Wechsler and C. Conroy,The Average Star Formation Histories of Galaxies in Dark Matter Halos from z = 0-8,Astrophys. J.770(2013) 57 [1207.6105]. [90] A. Kulier, N. Padilla, J. Schaye, R.A. Crain, M. Schaller, R.G. Bower et al.,The evolution of the baryon fraction in haloes as a cause of scatter in the galaxy stellar mass in the EAGLE"},{"citing_arxiv_id":"2604.25560","ref_index":24,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Massive black holes and their galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-04-28T12:31:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":0.0,"formal_verification":"none","one_line_summary":"A review summarizing detection methods, population statistics, and coevolution of supermassive black holes with host galaxies from early universe observations and simulations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.23236","ref_index":7,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The functional form of galaxy and halo luminosity and mass functions","primary_cat":"astro-ph.GA","submitted_at":"2026-04-25T10:19:56+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Exhaustive symbolic regression identifies low-complexity functional forms for luminosity and mass functions that outperform Schechter and Press-Schechter parametrizations while satisfying physical extrapolation and integration constraints.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"We denote the LF, SMF and HMF asϕ(L),ϕ(M ⋆)and n(Mh), respectively, giving the abundance of objects per unit volume and dex of the respective galaxy/halo quantity. We adopt the common approach of parametrising the HMF through the mass varianceσ(Mh)associated with haloes of massM h: n(Mh)d log(Mh) =f(σ) ¯ρm Mh |d ln(σ)|,(6) where σ2(Mh) = 1 2π2 Z ∞ 0 P(k) ˜W 2(kR)k 2 dk,(7) for linear matter power spectrumP(k), Fourier transform ˜Wof the top hat window function of radiusR( ˜W(kR) = 3(sin(kR)−kRcos(kR))/(kR) 3) and mean matter density ¯ρm. The smoothing scaleRis related to the halo mass by R= (3M h/(4π¯ρm))1/3. This parametrisation is useful be- cause most of the redshift and cosmology dependence of the HMF is already captured byσ, sof(σ)is more universal than"},{"citing_arxiv_id":"2604.19449","ref_index":37,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Cosmological constraints from the small scale clustering of Emission Line Galaxies","primary_cat":"astro-ph.CO","submitted_at":"2026-04-21T13:32:04+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"SHAMe-SF modeling of small-scale DESI ELG clustering delivers 6% precision on σ8 and Ωm h², matching full DR1 results with 1% volume.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.17963","ref_index":286,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"BEACON: JWST NIRCam Pure-parallel Imaging Survey. III. Constraints on the UV LF and the Clustering of z~7-14 Galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-04-20T08:45:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"New JWST pure-parallel imaging over 400 arcmin² yields UV luminosity functions at z~7.5-10 consistent with pre-JWST models and significant clustering of bright galaxies implying they occupy more massive halos than previously modeled.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.16597","ref_index":2,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Old Universe, Young SNe Ia: A Statistical Analysis of Type Ia Supernova Progenitor Age from 6,983 TITAN Host Galaxies, and Implications for Cosmology","primary_cat":"astro-ph.CO","submitted_at":"2026-04-17T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Large sample of SN Ia hosts shows young mean progenitor age of 3.5 Gyr and only 1.5 Gyr evolution, leading to negligible cosmological bias of 0.007 mag.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"The TITAN sample comprises 8,378 spectroscopically con- firmed SNe Ia with high-cadence, dual-band light curves obtained by the ATLAS all-sky survey (Tonry et al. 2018; Smith et al. 2020). Dedicated papers describ- 4Murakami & Tweddle et al. 103 104 105 106 λ[ ˚A] 2017hgz 2024vjb 2019yyv (rescaled) 10−20 10−19 10−18 10−17 10−16 10−15 10−14 10−13 Fλ[erg s −1 cm−2 ˚A−1] 0 2 4 6 8 10 12 Lookback time [Gyr] −12.5 −12.0 −11.5 −11.0 −10.5 −10.0 −9.5 −9.0 log10(SFR / M ∗ tot [yr−1]) Figure 1.Example best-fit SEDs and SFHs for the late-type host galaxy of SN 2017hgz, the early-type host galaxy of SN 2024vjb, and the irregular host galaxy of SN 2019yyv with clumpy star-forming regions, consistent with a disturbed system"},{"citing_arxiv_id":"2604.13866","ref_index":11,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Dark energy, spatial curvature, and star formation efficiency from JWST photometric and spectroscopic high-redshift galaxies","primary_cat":"astro-ph.CO","submitted_at":"2026-04-15T13:29:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Bayesian joint constraints show that elevated star formation efficiency accounts for JWST high-z galaxy excess in flat Lambda CDM, without requiring deviations in dark energy equation of state or curvature.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"the data disagrees with our benchmark valuesϵ0 = 0.2,0.15, and0.1at the 2.8σ,3.8σ, and>5.0σlevels respectively. Our results still indicate that even in this rather general scenario the requirement for high star formation efficiency persists. On the other hand, the non-ΛCDM cosmological parameters remain rather weakly constrained, withw≳−1.23[w≳−1.86] andΩ K ≳0.12[Ω K ≳ −0.11]at68%C.L.[95%C.L.]. Wefindnostatisticallysignificantindicationsfor deviations from a cosmological constant and/or spatial flatness, with posterior probabilitiesp(w >−1) = 0.56andp(Ω K >0) = 0.86, confirming all earlier results. Thedegeneraciesbetweenϵ,w, andΩ K observedanddiscussedearlierpersist here, although at a weaker level, since they are now redistributed across the"},{"citing_arxiv_id":"2601.22213","ref_index":5,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Little Red Dots on FIRE: The Ability of Bursty Galaxies to Host an Abundant Population of High-Redshift AGN","primary_cat":"astro-ph.GA","submitted_at":"2026-01-29T19:00:00+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"FIRE-2 simulations with gravitational torque-driven and free-fall accretion models predict enough high-redshift AGN to explain little red dots, with a super-Eddington Eddington-limited scenario for M_BH >= 2e5 Msun in M_star >= 2e7 Msun galaxies reproducing key observations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.04362","ref_index":12,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"ELG$\\times$LRG distribution through dark matter halo dynamics","primary_cat":"astro-ph.GA","submitted_at":"2025-12-04T01:15:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A new halo occupation model called HOMe reproduces the anisotropic clustering of ELGs and LRGs down to 200 h^{-1} kpc scales by sampling satellites from dark matter particle positions and fitting parameters to two-point statistics.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.20430","ref_index":13,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"pop-cosmos: Star formation over 12 Gyr from generative modelling of a deep infrared-selected galaxy catalogue","primary_cat":"astro-ph.GA","submitted_at":"2025-09-24T18:00:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A score-based diffusion generative model on deep infrared galaxy photometry yields a star formation rate density peaking at z=1.3 and shows distinct non-parametric star formation histories plus AGN activity peaking during the quenching transition of massive galaxies.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1907.02977","ref_index":48,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Realistic simulations of galaxy formation in f(R) modified gravity","primary_cat":"astro-ph.CO","submitted_at":"2019-07-05T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Hydrodynamical simulations in f(R) gravity using Illustris-TNG find observable 20% effects on high-z HI and stellar power spectra exceeding SKA errors, plus changes in disc galaxy formation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1712.04452","ref_index":8,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Inferring the star-formation histories of massive quiescent galaxies with BAGPIPES: Evidence for multiple quenching mechanisms","primary_cat":"astro-ph.GA","submitted_at":"2017-12-12T19:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"BAGPIPES fitting of 9289 massive quiescent galaxies shows most SFHs rise gradually then quench in 1-2 Gyr, with faster quenching at z>1 and slower at z<1, interpreted as multiple AGN feedback and gas-supply mechanisms.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"The16thto84thpercentilerangefortheposteriorspectrumand photometry are shaded orange. A corner plot showing the posterior for fitted parameters is shown below, with posterior SFH information shown to the right. MNRAS000, 1-24 (2017) Inferring the SFHs of massive quiescent galaxies9 lnL\u0001 = −0.5 ∑︁ 𝑖 ln \u0010 2𝜋𝜎2 𝑖 \u0011 − 0.5 ∑︁ 𝑖 𝑓𝑖 − 𝑓 H 𝑖 (ΘΘΘ)\u00012 𝜎2 𝑖 (8) where 𝑓 H 𝑖 (ΘΘΘ) is the model prediction corresponding to the ob- served flux 𝑓𝑖, which is obtained by generating aBagpipesmodel as described in Section 3.1. 3.2.2 Nested Sampling implementation Bagpipesmakes use of the nested sampling algorithm of Skilling (2006) to obtain the posterior distribution and evidence value given some model, prior distribution and observational data."}],"limit":50,"offset":0}