The radial acceleration relation persists at intermediate redshifts but with a characteristic acceleration scale that increases linearly with redshift.
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- other NGC 1068 094.B-0321(A) 64.6" x 63.8" 5.29 x 5.16 0.9" 2014-10-06 NGC 253 0102.B-0078(A) 87.4" x 87.2" 1.51 x 1.51 0.9" 2018-11-07 NGC 1320 108.229J.001 63.6" x 63.8" 12.51 x 12.55 0.7" 2022-01-07 13h25m30s 29s 28s 27s 26s 25s □43◦00′45′′ 01′00′′ 15′′ 30′′ RA DEC N 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 1" 200pc -17 -16.5 -16 -15.5 -15 log(F lux) [erg cm□2s□1] (a) Centaurus A, H α line map. 2h42m42s 41s 40s 39s □0◦00′15′′ 30′′ 45′′ 01′00′′ 15′′ RA DEC N 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17
- method analysis, as described in the following. Since all sources but one (J103853.29+392151.12) show only narrow emission lines, we used the stellar velocity dispersion (σ∗) found through the fitting of the stellar kinematic component to estimate the BH mass. To do this, we used the relation from McConnell & Ma (2013): log10 MBH M⊙ =(8.32±0.05)+(5.64±0.32) log 10 σ∗ 200 km s−1 . (1) Using these mass estimates, we derived the corresponding Eddington (1916) luminosity (LEdd) of each AGN in the 2
- method about these mechanisms in Appendix B. 1.3. Cluster relaxation and core-collapse Any gravitationally bound system undergoes dynamical relax- ation driven by the continuous dynamical interactions among its constituents. In a star cluster, this process occurs over a timescale (Spitzer 1969; Binney & Tremaine 2008): trel =4.2 Gyr 15 lnΛ c ! Rh,cl 4 pc ! s Mcl 107 M⊙ ,(1) called half-mass relaxation time, which depends on the cluster mass (Mcl) and the radius within which half of the cluster mass is
- method the star-galaxy separation by selecting objects that have a half- light radius larger than 0 .′′09. At the same time we removed faint galaxies with very large (and often non-physical) size es- timates, which can occur for very noisy objects. The magnitude- dependent selection that we adopted for this keeps objects with a half-light radius less than [−0 .′′1875 (IE − 24) + 1 .′′85]. This se- lection excludes all objects with a half-light radius larger than 1 .′′85 at IE = 24, but this limit incre
- method We follow the approach described by Leja et al. (2019a) with prior continuity. The continuity prior constrains the ratio of SFRs between the consecutive time-steps. This approach results in re- duced burstiness, that is, fewer rapid changes in SFR in time. The SFR changes follow the Student-t distribution, which is de- scribed by: PDF(x, ν)= Γ ν+1 2 √νπΓ ν 2 1+ (x/σt)2 ν !− ν+1 2 ,(1) whereΓis the Gamma function,νis the degree of freedom, and σt is the scale factor. Since with Student-t
- background covering the wavelength of the H 2 line of interest is shown in Figure 1. This data is yet to be corrected for tellurics or blaze; as such it has arbitrary flux units and displays an upward trend with wavelength. Article number, page 3 of 16 A&A proofs:manuscript no. aanda Table 1: Stellar and Disk Parameters for HD 131488 and HD 110058. Parameter HD 131488 References HD 110058 References Spectral Type A1 V [1] A0 V [2] R.A. (J2000) 14 55 08.03 [1] 12 39 46.14 [2] Decl. (J2000) -41 07 13.3 [1] -
co-cited works
representative citing papers
High-eccentricity tidal migration reproduces the Neptunian ridge as a density-dependent survival band and matches the desert boundary slope using one tidal encounter parameter.
Cold CGM clouds under quasar radiation follow optically thin ionization, radiation-shielded, or rocket-effect paths, with the latter increasing Lyα luminosity up to 10x and bright quasars fully ionizing the cold gas while faint ones drive rocket effects.
Four transiting sub-Neptunes with radii measured to <1.7% precision and masses >3 sigma for three planets, plus an outer non-transiting companion, discovered around TOI-5624 via TESS, CHEOPS photometry, and ground-based RV data.
Spectroscopic confirmation establishes the first intermediate-age RR Lyrae star as a member of open cluster Trumpler 5, with velocity and [Fe/H] matching the cluster but some element depletions.
Broad parameter study with detailed dust evolution code finds most outer dust traps leaky, producing long-lived O-rich inner discs with C/O < 1, while planetesimal formation is needed for strong blocking.
NLTE calculations indicate strontium is required to explain the onset of the 1μm feature at early times in AT2017gfo, while helium can dominate at later epochs with plausible masses.
Massive neutrinos leave distinct imprints on specific triangle configurations in the three-point correlation function of halos, with patterns that differ from sigma_8 variations and thus help break their degeneracy.
Galaxies at z>1 show N/O ratios elevated by a median 0.18 dex at fixed O/H relative to local trends, reaching 0.4-0.5 dex at low metallicity.
Multi-wavelength data on Aql X-1's 2024 outburst reveal an optical lead of up to 13 days over X-rays and a 12-hour hard-to-soft state transition.
First direct H2 measurements in two CO-rich exocometary belts yield CO/H2 lower limits of >1.35e-3 and >3.09e-5, showing the gas is H2-poor and supporting secondary exocometary origin.
Detection of 17.26-day eclipses in KQ Puppis reveals it as a hierarchical triple with dynamical masses of ~10 M⊙ for the RSG and ~14 M⊙ for the inner pair, plus the first orbital parallax for any red supergiant.
RX Gru is a pre-main-sequence eclipsing binary with twin components of mass ~1 solar mass each, age ~28 Myr, and a circumbinary companion of minimum mass 89 Mjup in a 23.8-year orbit.
Stellar mass functions in the peaks of the Hyperion protostructure at z~2.5 show a mass-dependent excess relative to the field, with ~10x enhancement at log(M*/M⊙)~11 versus ~3.5x at log(M*/M⊙)~9.5.
Euclid early release observations of Abell 2390 yield consistent weak lensing mass estimates from three shape catalogs and tomographic bins after contamination corrections.
EUV observations show hot prominence spicules generated by turbulence in cool solar filaments that may channel mass into the corona and aid filament evaporation.
FICO procedure yields average precisions of 2.3% mass, 0.82% radius, 6.9% age and 0.49% mean density for 95 solar-like stars, outperforming direct frequency fitting for stars above 1.15 solar masses or 6050 K.
In Auriga Superstars simulations, old stellar morphological lopsidedness correlates strongly with HI lopsidedness at z=0, with tidal interactions inducing coherent asymmetries in both while smooth accretion primarily affects gas and young stars.
Ultra-thick warm absorbers form a new subclass of AGN ionized outflows with exceptionally high column densities and moderate ionization that drive strong variability and may connect to ultra-fast outflows.
A vision transformer classifier trained on simulated and real Euclid data recovers all known strong lenses in test sets and finds 8 Grade A plus 26 Grade B new candidates in the Q1 data.
Hybrid deep learning models recover large frequency separation, frequency of maximum power, and dipole period spacing from low-resolution Gaia XP spectra with accuracy comparable to moderate-resolution spectroscopy.
Numerical models of neutron star atmospheres from fusion ashes show a radiation-pressure layer limiting flux and absorption edges tied to chemical composition, with fits to diluted blackbodies plus edges for X-ray burst interpretation.
Near-critical magnetic fields of 100-700 kG confined below the H-burning shell are inferred in eight Kepler red giants via non-perturbative modeling of mixed-mode frequencies, identifying components as m=0 and m=1 rather than m=±1.
Paschen jumps in Little Red Dots indicate their continua originate from free-bound recombination emission in low-temperature nebular gas rather than thermalized or AGN components.
citing papers explorer
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The imprints of massive neutrinos on the three-point correlation function of large-scale structures
Massive neutrinos leave distinct imprints on specific triangle configurations in the three-point correlation function of halos, with patterns that differ from sigma_8 variations and thus help break their degeneracy.
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Euclid: Early Release Observations. Weak gravitational lensing analysis of Abell 2390
Euclid early release observations of Abell 2390 yield consistent weak lensing mass estimates from three shape catalogs and tomographic bins after contamination corrections.
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SLICE -- Combining Strong Lensing and X-ray in AC 114. Further Insights into the Merger Scenario
Combined JWST lensing and X-ray analysis shows AC114 as the main cluster in a late post-collisional major merger with a gas-stripped companion AC114b located about 1 Mpc to the northwest.
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Towards an application of fourth-order shear statistics I. The information content of $\langle M_\mathrm{ap}^4 \rangle $
Derives filters for fourth-order aperture statistics, implements a numerical pipeline achieving 2% precision on Gaussian random fields, and forecasts only minimal extra cosmological constraining power when added to second- and third-order aperture statistics in a DES-Y3-like non-tomographic analysis
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Impact of Primordial Black Hole population on 21 cm observables at high redshift
X-ray heating from primordial black holes assumed to seed high-redshift AGNs shallows the global 21-cm absorption signal and suppresses its power amplitude at cosmic dawn, with strong dependence on the PBH mass function.
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Euclid. Populating a dark universe with galaxies using SciPIC
SciPICal calibrates galaxy properties in halo-based mocks for Euclid, delivering improved clustering predictions and a deep catalogue validated to 15 percent against observations.
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Euclid preparation. XCVI. Cosmology Likelihood for Observables in Euclid (CLOE). 3. Inference and Forecasts
CLOE pipeline produces forecasts showing Euclid can reach FoM >400 for dark energy w0 and wa by combining primary probes on synthetic data.
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The impact of strong feedback on galaxy group scaling relations
Highly ejective feedback models under-predict X-ray luminosity of galaxy groups at fixed mass by 5.7 sigma using direct observables from 44 XMM-Newton observed systems.
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Euclid preparation. XCVIII. Cosmology Likelihood for Observables in Euclid (CLOE). 5: Extensions beyond the standard modelling of theoretical probes and systematic effects
CLOE has been extended to model magnification bias, massive neutrinos, and modified gravity for Euclid probes and validated via posterior sampling on synthetic data.