DNA barcoding is a powerful tool for species detection, identification and discovery. Metazoan DNA barcoding is primarily based upon a specific region of the cytochrome c oxidase subunit I gene that ...is PCR amplified by primers HCO2198 and LCO1490 (‘Folmer primers’) designed by Folmer et al. (Molecular Marine Biology and Biotechnology, 3, 1994, 294). Analysis of sequences published since 1994 has revealed mismatches in the Folmer primers to many metazoans. These sequences also show that an extremely high level of degeneracy would be necessary in updated Folmer primers to maintain broad taxonomic utility. In primers jgHCO2198 and jgLCO1490, we replaced most fully degenerated sites with inosine nucleotides that complement all four natural nucleotides and modified other sites to better match major marine invertebrate groups. The modified primers were used to amplify and sequence cytochrome c oxidase subunit I from 9105 specimens from Moorea, French Polynesia and San Francisco Bay, California, USA representing 23 phyla, 42 classes and 121 orders. The new primers, jgHCO2198 and jgLCO1490, are well suited for routine DNA barcoding, all‐taxon surveys and metazoan metagenomics.
The infall regions of galaxy clusters represent the largest gravitationally bound structures in a LambdaCDM universe. Measuring cluster mass profiles into the infall regions provides an estimate of ...the ultimate mass of these halos. We use the caustic technique to measure cluster mass profiles from galaxy redshifts obtained with the Hectospec Cluster Survey (HeCS), an extensive spectroscopic survey of galaxy clusters with MMT/Hectospec. We survey 58 clusters selected by X-ray flux at 0.1 < z < 0.3. The survey includes 22,680 unique MMT/Hectospec redshifts for individual galaxies; 10,145 of these galaxies are cluster members. For each cluster, we acquired high signal-to-noise spectra for ~200 cluster members and a comparable number of foreground/background galaxies. The cluster members trace out infall patterns around the clusters. The members define a very narrow red sequence. We demonstrate that the determination of velocity dispersion is insensitive to the inclusion of bluer members (a small fraction of the cluster population). We apply the caustic technique to define membership and estimate the mass profiles to large radii. The ultimate halo mass of clusters (the mass that remains bound in the far future of a LambdaCDM universe) is on average (1.99 + or - 0.11M sub(200), a new observational cosmological test in essential agreement with simulations. Summed profiles binned in M sub(200) on and in L sub(X) demonstrate that the predicted Navarro-Frenk-White form of the density profile is a remarkably good representation of the data in agreement with weak lensing results extending to large radius. The concentration of these summed profiles is also consistent with theoretical predictions.
Background
Luminal esophageal temperature (LET) monitoring is not associated with reduced esophageal injury following pulmonary vein isolation (PVI).
Objective
Detailed analysis of (the temporal and ...spatial gradients of) LET measurements may better predict the risk for esophageal injury.
Methods
Between January 2020 and December 2021, LET maxima, duration of LET rise above baseline, and area under the LET curve (AUC) were calculated offline and correlated with (endoscopy and endoscopic ultrasound detected) esophageal injury (i.e., mucosal esophageal lesions ELs, periesophageal edema, and gastric motility disorders) following PVI using moderate‐power moderate‐duration (MPMD 25–30 W/25–30s) and high‐power short‐duration (HPSD 50 W/13s) radiofrequency (RF) settings.
Results
63 patients (69 ± 9 years old, 32 male, 51 MPMD and 12 HPSD) were studied. The esophageal injury was frequent (40% in both groups), mucosal ELs were more common with MPMD, and edema was frequently observed following HPSD. RF‐duration, total RF‐energy at the left atrial (LA) posterior wall, and distance between LA and esophagus were not different between patients with/without esophageal injury. In contrast, to LET and LET duration above baseline, AUC was the best predictor and significantly increased in patients with esophageal injury (3422 vs. 2444 K.s).
Conclusion
For both ablation strategies, AUC of the LET curves best predicted esophageal injury. HPSD is associated with similar rates of esophageal injury when (mostly subclinical) periesophageal alterations (that are of unclear clinical relevance) are included. Whether integration of these calculated LET parameters is useful to prevent esophageal injury remains to be seen.
We use new Gaia measurements to explore the origin of the highest velocity stars in the hypervelocity star (HVS) survey. The measurements reveal a clear pattern in B-type stars. Halo stars dominate ...the sample at speeds of 100 km s−1 below Galactic escape velocity. Disk runaway stars have speeds up to 100 km s−1 above Galactic escape velocity, but most disk runaways are bound. Stars with speeds 100 km s−1 above Galactic escape velocity originate from the Galactic center. Two bound stars may also originate from the Galactic center. Future Gaia measurements will enable a large, clean sample of Galactic center ejections for measuring the massive black hole ejection rate of HVSs, and for constraining the mass distribution of the Milky Way dark matter halo.
We examine the mass-metallicity relation for z lap 1.6. The mass-metallicity relation follows a steep slope with a turnover, or "knee," at stellar masses around 10 super(10) M sub(middot in circle). ...At stellar masses higher than the characteristic turnover mass, the mass-metallicity relation flattens as metallicities begin to saturate. We show that the redshift evolution of the mass-metallicity relation depends only on the evolution of the characteristic turnover mass. The relationship between metallicity and the stellar mass normalized to the characteristic turnover mass is independent of redshift. We find that the redshift-independent slope of the mass-metallicity relation is set by the slope of the relationship between gas mass and stellar mass. The turnover in the mass-metallicity relation occurs when the gas-phase oxygen abundance is high enough that the amount of oxygen locked up in low-mass stars is an appreciable fraction of the amount of oxygen produced by massive stars. The characteristic turnover mass is the stellar mass, where the stellar-to-gas mass ratio is unity. Numerical modeling suggests that the relationship between metallicity and the stellar-to-gas mass ratio is a redshift-independent, universal relationship followed by all galaxies as they evolve. The mass-metallicity relation originates from this more fundamental universal relationship between metallicity and the stellar-to-gas mass ratio. We test the validity of this universal metallicity relation in local galaxies where stellar mass, metallicity, and gas mass measurements are available. The data are consistent with a universal metallicity relation. We derive an equation for estimating the hydrogen gas mass from measurements of stellar mass and metallicity valid for z lap 1.6 and predict the cosmological evolution of galactic gas masses.
ABSTRACT We examine the relation between stellar mass and central stellar velocity dispersion-the M* relation-for massive quiescent galaxies at z < 0.7. We measure the local relation from the Sloan ...Digital Sky Survey and the intermediate redshift relation from the Smithsonian Hectospec Lensing Survey. Both samples are highly complete (>85%) and we consistently measure the stellar mass and velocity dispersion for the two samples. The M* relation and its scatter are independent of redshift with for M* 1010.3 M . The measured slope of the M* relation is the same as the scaling between the total halo mass and the dark matter halo velocity dispersion obtained by N-body simulations. This consistency suggests that massive quiescent galaxies are virialized systems, where the central dark matter concentration is either a constant or negligible fraction of the stellar mass. The relation between the total galaxy mass (stellar + dark matter) and the central stellar velocity dispersion is consistent with the observed relation between the total mass of a galaxy cluster and the velocity dispersion of the cluster members. This result suggests that the central stellar velocity dispersion is directly proportional to the velocity dispersion of the dark matter halo. Thus, the central stellar velocity dispersion is a fundamental, directly observable property of galaxies, which may robustly connect galaxies to dark matter halos in N-body simulations. To interpret the results further in the context of ΛCDM, it would be useful to analyze the relationship between the velocity dispersion of stellar particles and the velocity dispersion characterizing their dark matter halos in high-resolution cosmological hydrodynamic simulations.
Abstract We examine the central stellar velocity dispersion of subhalos based on IllustrisTNG cosmological hydrodynamic simulations. The central velocity dispersion is a fundamental observable that ...links galaxies with their dark matter subhalos. We carefully explore simulated stellar velocity dispersions derived with different definitions to assess possible systematics. We explore the impact of variation in the identification of member stellar particles, the viewing axes, the velocity dispersion computation technique, and simulation resolution. None of these issues impact the velocity dispersion significantly; any systematic uncertainties are smaller than the random error. We examine the stellar mass–velocity dispersion relation as an observational test of the simulations. At fixed stellar mass, the observed velocity dispersions significantly exceed the simulation results. This discrepancy is an interesting benchmark for the IllustrisTNG simulations because the simulations are not explicitly tuned to match this relation. We demonstrate that the stellar velocity dispersion provides measures of the dark matter velocity dispersion and the dark matter subhalo mass.
The TNG300-1 run of the IllustrisTNG simulations includes 1697 clusters of galaxies with
M
200c
> 10
14
M
⊙
covering the redshift range 0.01 − 1.04. We built mock spectroscopic redshift catalogs ...of simulated galaxies within these clusters and applied the caustic technique to estimate the cumulative cluster mass profiles. We computed the total true cumulative mass profile from the 3D simulation data, calculated the ratio of caustic mass to total 3D mass as a function of cluster-centric distance, and identified the radial range where this mass ratio is roughly constant. The ratio of 3D to caustic mass on this plateau defines ℱ
β
. The filling factor, ℱ
β
= 0.41 ± 0.08, is constant on a plateau that covers a wide cluster-centric distance range, (0.6 − 4.2)
R
200c
. This calibration is insensitive to redshift. The calibrated caustic mass profiles are unbiased, with an average uncertainty of 23%. At
R
200c
, the average
M
C
/
M
3D
= 1.03 ± 0.22; at 2
R
200c
, the average
M
C
/
M
3D
= 1.02 ± 0.23. Simulated galaxies are unbiased tracers of the mass distribution. IllustrisTNG is a broad statistical platform for application of the caustic technique to large samples of clusters with spectroscopic redshifts for ≳200 members in each system. These observations will allow extensive comparisons with weak-lensing masses and will complement other techniques for measuring the growth rate of structure in the Universe.
Abstract
We use surveys covering the redshift range 0.05 <
z
< 3.8 to explore quiescent galaxy scaling relations and the redshift evolution of the velocity dispersion, size, and dynamical mass at ...fixed stellar mass. For redshift
z
< 0.6, we derive mass-limited samples and demonstrate that these large samples enhance constraints on the evolution of the quiescent population. The constraints include 2985 new velocity dispersions from the SHELS F2 survey. In contrast with the known substantial evolution of size with redshift, evolution in the velocity dispersion is negligible. The dynamical-to-stellar-mass ratio increases significantly as the universe ages, in agreement with recent results that combine high-redshift data with the Sloan Digital Sky Survey. Like other investigators, we interpret this result as an indication that the dark matter fraction within the effective radius increases as a result of the impact of the minor mergers that are responsible for size growth. We emphasize that dense redshift surveys covering the range 0.07 <
z
< 1 along with strong and weak lensing measurements could remove many ambiguities in evolutionary studies of the quiescent population.
We use 101 galaxies selected from the Nearby Field Galaxy Survey to investigate the effect of aperture size on the star formation rate, metallicity, and reddening determinations for galaxies. Our ...sample includes galaxies of all Hubble types except ellipticals with global star formation rates (SFRs) ranging from 0.01 to 100M
⊙yr−1, metallicities in the range
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, and reddening of
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. We compare the SFR, metallicity, and reddening derived from nuclear spectra to those derived from integrated spectra. For apertures capturing <20% of the
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light, the differences between nuclear and global metallicity, extinction, and SFR are substantial. Late‐type spiral galaxies show the largest systematic difference (∼0.14 dex), with nuclear metallicities greater than the global metallicities. The Sdm, Im, and Peculiar types have the largest scatter in nuclear/integrated metallicities, indicating a large range in metallicity gradients for these galaxy types, or clumpy metallicity distributions. We find little evidence for systematic differences between nuclear and global extinction estimates for any galaxy type. However, there is significant scatter between the nuclear and integrated extinction estimates for nuclear apertures containing <20% of the
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flux. We calculate an “expected” SFR using our nuclear spectra and apply the commonly used aperture correction method. The expected SFR overestimates the global value for early‐type spirals, with large scatter for all Hubble types, particularly late types. The differences between the expected and global SFRs probably result from the assumption that the distributions of the emission‐line gas and the continuum are identical. The largest scatter (error) in the estimated SFR occurs when the aperture captures <20% of the
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emission. We discuss the implications of these results for metallicity‐luminosity relations and star formation history studies based on fiber spectra. To reduce systematic and random errors from aperture effects, we recommend selecting samples with fibers that capture >20% of the galaxy light. For the Sloan Digital Sky Survey and the Two‐Degree Field Galaxy Redshift Survey, redshifts
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and 0.06 are required, respectively, to ensure a covering fraction >20% for galaxy sizes similar to the average size, type, and luminosity observed in our sample. Higher luminosity samples and samples containing many late‐type galaxies require a larger minimum redshift to ensure that >20% of the galaxy light is enclosed by the fiber.
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