Redshift Dispersion Research Articles

Morphology of Galaxies in JWST Fields: Initial Distribution and Evolution of Galaxy Morphology

Abstract A recent study from the Horizon Run 5 (HR5) cosmological simulation has predicted that galaxies with log M * / M ⊙ ≲ 10 in the cosmic morning (10 ≳ z ≳ 4) dominantly have disk-like morphology in the ΛCDM universe, which is driven by the tidal torque in the initial fluctuations of matter. For a direct comparison with observation we identify a total of about 19,000 James Webb Space Telescope (JWST) galaxies with log M * / M ⊙ > 9 at z = 0.6–8.0 utilizing deep JWST/NIRCam images of publicly released fields, including North Ecliptic Pole Time-Domain Fields, Next Generation Deep Extragalactic Exploratory Public survey, Cosmic Evolution Early Release Science Survey, Cosmic Evolution Survey, UltraDeep Survey, and SMACS J0723-7327. We estimate their stellar masses and photometric redshifts with the redshift dispersion of σ NMAD = 0.009 and an outlier fraction of only about 6%. We classify galaxies into three morphological types, disks, spheroids, and irregulars, applying the same criteria used in the HR5 study. The morphological distribution of the JWST galaxies shows that disk galaxies account for 60%–70% at all redshift ranges. However, in the high-mass regime ( log M * / M ⊙ ≳ 11 ), spheroidal morphology becomes the dominant type. This implies that the mass growth of galaxies is accompanied by a morphological transition from disks to spheroids. The fraction of irregulars is about 20% or less at all masses and redshifts. All the trends in the morphology distribution are consistently found in the six JWST fields. These results are in close agreement with the results from the HR5 simulation, particularly confirming the prevalence of disk galaxies at small masses in the cosmic morning and noon.

An accurate cluster selection function for the J-PAS narrow-band wide-field survey

The impending Javalambre Physics of the accelerating universe Astrophysical Survey (J-PAS) will be the first wide-field survey of $\gtrsim$ 8500 deg$^2$ to reach the `stage IV' category. Because of the redshift resolution afforded by 54 narrow-band filters, J-PAS is particularly suitable for cluster detection in the range z$<$1. The photometric redshift dispersion is estimated to be only $\sim 0.003$ with few outliers $\lesssim$ 4\% for galaxies brighter than $i\sim23$ AB, because of the sensitivity of narrow band imaging to absorption and emission lines. Here we evaluate the cluster selection function for J-PAS using N-body+semi-analytical realistic mock catalogues. We optimally detect clusters from this simulation with the Bayesian Cluster Finder, and we assess the completeness and purity of cluster detection against the mock data. The minimum halo mass threshold we find for detections of galaxy clusters and groups with both $>$80\% completeness and purity is $M_h \sim 5 \times 10^{13}M_{\odot}$ up to $z\sim 0.7$. We also model the optical observable, $M^*_{\rm CL}$-halo mass relation, finding a non-evolution with redshift and main scatter of $\sigma_{M^*_{\rm CL} | M_{\rm h}}\sim 0.14 \,dex$ down to a factor two lower in mass than other planned broad-band stage IV surveys, at least. For the $M_{\rm h} \sim 1 \times 10^{14}M_{\odot}$ Planck mass limit, J-PAS will arrive up to $z\sim 0.85$ with a $\sigma_{M^*_{\rm CL} | M_{\rm h}}\sim 0.12 \, dex$. Therefore J-PAS will provide the largest sample of clusters and groups up to $z\sim 0.8$ with a mass calibration accuracy comparable to X-ray data.

Spectroscopic needs for imaging dark energy experiments

Large sets of objects with spectroscopic redshift measurements will be needed for imaging dark energy experiments to achieve their full potential, serving two goals:_training_, i.e., the use of objects with known redshift to develop and optimize photometric redshift algorithms; and_calibration_, i.e., the characterization of moments of redshift (or photo-z error) distributions. Better training makes cosmological constraints from a given experiment stronger, while highly-accurate calibration is needed for photo-z systematics not to dominate errors. In this white paper, we investigate the required scope of spectroscopic datasets which can serve both these purposes for ongoing and next-generation dark energy experiments, as well as the time required to obtain such data with instruments available in the next decade. Large time allocations on kilo-object spectrographs will be necessary, ideally augmented by infrared spectroscopy from space. Alternatively, precision calibrations could be obtained by measuring cross-correlation statistics using samples of bright objects from a large baryon acoustic oscillation experiment such as DESI. We also summarize the additional work on photometric redshift methods needed to prepare for ongoing and future dark energy experiments.

Locating the baryon acoustic peak

Forthcoming photometric redshift surveys should provide an accurate probe of the acoustic peak in the two-point galaxy correlation function, in the form of angular clustering of galaxies within a given shell in redshift space. We investigate the form of the anticipated signal, quantifying the distortions that arise due to projection effects, and, in particular, explore the validity of applying the Limber approximation. A single-integral prescription is presented, which provides an alternative to Limber's equation, and produces a significantly improved prediction in the regime of interest. The position of the acoustic peak within the angular correlation function relates to the angular diameter distance to the far side of the redshift bin. Thicker redshift bins therefore shift comoving features toward smaller angular scales. As a result, the value of the photometric redshift error acquires a greater significance, particularly at lower redshifts. In order to recover the dark energy equation of state to a level of 1 %, we find the total redshift dispersion must be determined to within Δ σz ≤ 10 -3 , which may prove challenging to achieve in practice.

A new statistic for redshift surveys: the redshift dispersion of galaxies

We present a new statistic - the redshift dispersion - which may prove useful for comparing next generation redshift surveys (e.g., the Sloan Digital Sky Survey) and cosmological simulations. Our statistic is specifically designed for the projection of phase space which is directly measured by redshift surveys. We find that the redshift dispersion of galaxies as a function of the projected overdensity has a strong dependence on the cosmological density parameter Ω. The redshift dispersion statistic is easy to compute and can be motivated by applying the cosmic virial theorem (CVT) to subsets of galaxies with the same local density. We show that the velocity dispersion of particles in these subsets is proportional to the product of Ω and the local density. Low resolution N-body simulations of several cosmological models (open/closed CDM, CDM + Λ, HDM) indicate that the proportionality between velocity dispersion, local density and Ω holds over redshift scales in the range 50 km s−1 to 500 km s−1. The redshift dispersion may provide an interesting means for comparing volume-limited subsamples of the Sloan Digital Sky Survey to equivalent N-body/hydrodynamics simulations.

Redshift dispersion in the X-ray cluster of galaxies A1367

Redshift dispersion in the X-ray cluster of galaxies A1367

On the dynamics of the Virgo cluster

view Abstract Citations (43) References (7) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS On the dynamics of the Virgo cluster Holmberg, Erik Abstract A detailed analysis of the observational material available for the Virgo cluster of galaxies leads to the conclusion that the high redshift dispersion can be satisfactorily explained as a result of orbital motions (especially orbital motions within the subgroups of the cluster), systematic errors in the measured redohifto, and disturbance by optical members. Each of these three sources may be responsible for about one-third of the observed square dispersion. Accordingly, there is no need to introduce any additional dispersion- increasing effects, such as a rapid expansion of the cluster, or a strong gravitational field due to nonluminous intergalactic matter. The results are applicable also to other clusters and agglomerations of galaxies. A detailed summary of the results, and of the conclusions to be reached, is given in Sec. 6. Publication: The Astronomical Journal Pub Date: December 1961 DOI: 10.1086/108474 Bibcode: 1961AJ.....66..620H full text sources ADS | data products NED (88)